Author name code: kuhn ADS astronomy entries on 2022-09-14 author:"Kuhn, Jeffrey Richard" ------------------------------------------------------------------------ Title: The National Science Foundation's Daniel K. Inouye Solar Telescope — Status Update Authors: Rimmele, T.; Woeger, F.; Tritschler, A.; Casini, R.; de Wijn, A.; Fehlmann, A.; Harrington, D.; Jaeggli, S.; Anan, T.; Beck, C.; Cauzzi, G.; Schad, T.; Criscuoli, S.; Davey, A.; Lin, H.; Kuhn, J.; Rast, M.; Goode, P.; Knoelker, M.; Rosner, R.; von der Luehe, O.; Mathioudakis, M.; Dkist Team Bibcode: 2021AAS...23810601R Altcode: The National Science Foundation's 4m Daniel K. Inouye Solar Telescope (DKIST) on Haleakala, Maui is now the largest solar telescope in the world. DKIST's superb resolution and polarimetric sensitivity will enable astronomers to unravel many of the mysteries the Sun presents, including the origin of solar magnetism, the mechanisms of coronal heating and drivers of flares and coronal mass ejections. Five instruments, four of which provide highly sensitive measurements of solar magnetic fields, including the illusive magnetic field of the faint solar corona. The DKIST instruments will produce large and complex data sets, which will be distributed through the NSO/DKIST Data Center. DKIST has achieved first engineering solar light in December of 2019. Due to COVID the start of the operations commissioning phase is delayed and is now expected for fall of 2021. We present a status update for the construction effort and progress with the operations commissioning phase. Title: DKIST First-light Instrumentation Authors: Woeger, F.; Rimmele, T.; Casini, R.; von der Luehe, O.; Lin, H.; Kuhn, J.; Dkist Team Bibcode: 2021AAS...23810602W Altcode: The NSF's Daniel K. Inouye Solar Telescope's (DKIST) four meter aperture and state-of-the-art wavefront correction system and instrumentation will facilitate new insights into the complexities of the solar atmosphere. We will describe the details and status of the diverse first light instruments, including the high order adaptive optics system, that are being commissioned: The Visible Spectro-Polarimeter (ViSP), the Visible Broadband Imager (VBI), the Visible Tunable Filter (VTF), the Diffraction-Limited Spectro-Polarimeter (DL-NIRSP) and the Cryogenic Spectro-Polarimeter (Cryo-NIRSP). We will present first data demonstrating the telescope's instrument systems performance. Title: Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST) Authors: Rast, Mark P.; Bello González, Nazaret; Bellot Rubio, Luis; Cao, Wenda; Cauzzi, Gianna; Deluca, Edward; de Pontieu, Bart; Fletcher, Lyndsay; Gibson, Sarah E.; Judge, Philip G.; Katsukawa, Yukio; Kazachenko, Maria D.; Khomenko, Elena; Landi, Enrico; Martínez Pillet, Valentín; Petrie, Gordon J. D.; Qiu, Jiong; Rachmeler, Laurel A.; Rempel, Matthias; Schmidt, Wolfgang; Scullion, Eamon; Sun, Xudong; Welsch, Brian T.; Andretta, Vincenzo; Antolin, Patrick; Ayres, Thomas R.; Balasubramaniam, K. S.; Ballai, Istvan; Berger, Thomas E.; Bradshaw, Stephen J.; Campbell, Ryan J.; Carlsson, Mats; Casini, Roberto; Centeno, Rebecca; Cranmer, Steven R.; Criscuoli, Serena; Deforest, Craig; Deng, Yuanyong; Erdélyi, Robertus; Fedun, Viktor; Fischer, Catherine E.; González Manrique, Sergio J.; Hahn, Michael; Harra, Louise; Henriques, Vasco M. J.; Hurlburt, Neal E.; Jaeggli, Sarah; Jafarzadeh, Shahin; Jain, Rekha; Jefferies, Stuart M.; Keys, Peter H.; Kowalski, Adam F.; Kuckein, Christoph; Kuhn, Jeffrey R.; Kuridze, David; Liu, Jiajia; Liu, Wei; Longcope, Dana; Mathioudakis, Mihalis; McAteer, R. T. James; McIntosh, Scott W.; McKenzie, David E.; Miralles, Mari Paz; Morton, Richard J.; Muglach, Karin; Nelson, Chris J.; Panesar, Navdeep K.; Parenti, Susanna; Parnell, Clare E.; Poduval, Bala; Reardon, Kevin P.; Reep, Jeffrey W.; Schad, Thomas A.; Schmit, Donald; Sharma, Rahul; Socas-Navarro, Hector; Srivastava, Abhishek K.; Sterling, Alphonse C.; Suematsu, Yoshinori; Tarr, Lucas A.; Tiwari, Sanjiv; Tritschler, Alexandra; Verth, Gary; Vourlidas, Angelos; Wang, Haimin; Wang, Yi-Ming; NSO and DKIST Project; DKIST Instrument Scientists; DKIST Science Working Group; DKIST Critical Science Plan Community Bibcode: 2021SoPh..296...70R Altcode: 2020arXiv200808203R The National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to measure, understand, and model the basic physical processes that control the structure and dynamics of the Sun and its atmosphere. The first-light DKIST images, released publicly on 29 January 2020, only hint at the extraordinary capabilities that will accompany full commissioning of the five facility instruments. With this Critical Science Plan (CSP) we attempt to anticipate some of what those capabilities will enable, providing a snapshot of some of the scientific pursuits that the DKIST hopes to engage as start-of-operations nears. The work builds on the combined contributions of the DKIST Science Working Group (SWG) and CSP Community members, who generously shared their experiences, plans, knowledge, and dreams. Discussion is primarily focused on those issues to which DKIST will uniquely contribute. Title: Using long baseline radial velocities and direct imaging to make 13-sigma dynamical mass measurements for the components of the HD 104304 stellar binary. Authors: Nagpal, V.; Blunt, S.; Howard, A.; Hirsch, L.; Liu, M.; Isaacson, H.; Morales, F.; Kuhn, J. Bibcode: 2021AAS...23753003N Altcode: Combining direct imaging astrometry and long-baseline radial velocity (RV) measurements of stellar binaries can provide precise constraints on their 3D orbits and yield dynamical masses for both components. We applied the combination of these methods to study HD104304, a binary system with a decades-long orbit containing a G8IV subgiant and a recently-discovered M dwarf companion. Using radial velocities collected over a timespan of two decades by Keck/HIRES and astrometry calculated from adaptive optics images taken by Keck/NIRC2, we explored models to jointly fit the astrometric orbital motion and RV trend. Previous studies of this system (Howard & Fulton, 2016) were unable to distinguish between two and three body solutions using RVs alone. However, we are able to break this degeneracy by incorporating images into the fit. We make 13-sigma dynamical mass measurements of the primary and secondary, and find that a slightly eccentric solution (e=0.4) is required. However, the dynamical mass we measure for the primary (~1.8 solar masses) is significantly higher than its well constrained spectroscopic mass of 1.02 solar masses. This hints at the need for a three-body solution to accurately model the observed trend in the HD 104304 system. Title: The Daniel K. Inouye Solar Telescope - Observatory Overview Authors: Rimmele, Thomas R.; Warner, Mark; Keil, Stephen L.; Goode, Philip R.; Knölker, Michael; Kuhn, Jeffrey R.; Rosner, Robert R.; McMullin, Joseph P.; Casini, Roberto; Lin, Haosheng; Wöger, Friedrich; von der Lühe, Oskar; Tritschler, Alexandra; Davey, Alisdair; de Wijn, Alfred; Elmore, David F.; Fehlmann, André; Harrington, David M.; Jaeggli, Sarah A.; Rast, Mark P.; Schad, Thomas A.; Schmidt, Wolfgang; Mathioudakis, Mihalis; Mickey, Donald L.; Anan, Tetsu; Beck, Christian; Marshall, Heather K.; Jeffers, Paul F.; Oschmann, Jacobus M.; Beard, Andrew; Berst, David C.; Cowan, Bruce A.; Craig, Simon C.; Cross, Eric; Cummings, Bryan K.; Donnelly, Colleen; de Vanssay, Jean-Benoit; Eigenbrot, Arthur D.; Ferayorni, Andrew; Foster, Christopher; Galapon, Chriselle Ann; Gedrites, Christopher; Gonzales, Kerry; Goodrich, Bret D.; Gregory, Brian S.; Guzman, Stephanie S.; Guzzo, Stephen; Hegwer, Steve; Hubbard, Robert P.; Hubbard, John R.; Johansson, Erik M.; Johnson, Luke C.; Liang, Chen; Liang, Mary; McQuillen, Isaac; Mayer, Christopher; Newman, Karl; Onodera, Brialyn; Phelps, LeEllen; Puentes, Myles M.; Richards, Christopher; Rimmele, Lukas M.; Sekulic, Predrag; Shimko, Stephan R.; Simison, Brett E.; Smith, Brett; Starman, Erik; Sueoka, Stacey R.; Summers, Richard T.; Szabo, Aimee; Szabo, Louis; Wampler, Stephen B.; Williams, Timothy R.; White, Charles Bibcode: 2020SoPh..295..172R Altcode: We present an overview of the National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST), its instruments, and support facilities. The 4 m aperture DKIST provides the highest-resolution observations of the Sun ever achieved. The large aperture of DKIST combined with state-of-the-art instrumentation provide the sensitivity to measure the vector magnetic field in the chromosphere and in the faint corona, i.e. for the first time with DKIST we will be able to measure and study the most important free-energy source in the outer solar atmosphere - the coronal magnetic field. Over its operational lifetime DKIST will advance our knowledge of fundamental astronomical processes, including highly dynamic solar eruptions that are at the source of space-weather events that impact our technological society. Design and construction of DKIST took over two decades. DKIST implements a fast (f/2), off-axis Gregorian optical design. The maximum available field-of-view is 5 arcmin. A complex thermal-control system was implemented in order to remove at prime focus the majority of the 13 kW collected by the primary mirror and to keep optical surfaces and structures at ambient temperature, thus avoiding self-induced local seeing. A high-order adaptive-optics system with 1600 actuators corrects atmospheric seeing enabling diffraction limited imaging and spectroscopy. Five instruments, four of which are polarimeters, provide powerful diagnostic capability over a broad wavelength range covering the visible, near-infrared, and mid-infrared spectrum. New polarization-calibration strategies were developed to achieve the stringent polarization accuracy requirement of 5×10−4. Instruments can be combined and operated simultaneously in order to obtain a maximum of observational information. Observing time on DKIST is allocated through an open, merit-based proposal process. DKIST will be operated primarily in "service mode" and is expected to on average produce 3 PB of raw data per year. A newly developed data center located at the NSO Headquarters in Boulder will initially serve fully calibrated data to the international users community. Higher-level data products, such as physical parameters obtained from inversions of spectro-polarimetric data will be added as resources allow. Title: High dynamic-range observation using a 1.8-m off-axis telescope PLANETS: feasibility study and telescope design Authors: Kagitani, Masato; Sakanoi, Takeshi; Kasaba, Yasumasa; Hirahara, Yasuhiro; Kurita, Mikio; Kuhn, Jeffrey R.; Berdyugina, Svetlana V.; Emilio, Marcelo Bibcode: 2020SPIE11445E..43K Altcode: PLANETS will be a 1.8-m off-axis telescope combined with contrast enhancement techniques, enabling us to observe faint emissions in the vicinity of bright objects. This "high dynamic-range" capability is largely dependent upon precision of telescope optics as well as atmospheric distortion. We present feasibility study of monitoring water plumes on Europa, neutral torus close to Enceladus, and ionosphere on Mars using PLANETS telescope. To test feasibility of high dynamic-range observation under actual conditions of wavefront error, we modeled propagation of light though the system based on Fraunhofer calculation taking into account for wavefront error made by atmospheric distortion and by primary mirror figure error. Then point spread function is calculated for several cases of figure errors under use of adaptive optics. The modeling result predicts that the moderate or high-precision primary mirror is mandatory to accomplish the high dynamic-range observation. We also present the latest design of PLANETS, especially focus on the support structures of primary mirror. We employ 36-point whiffletrees with 33 warping harnesses for axial support, and 24-point Schwesinger support for lateral support. The active support system is expected to reduce pre-polished RMS error from 1.51 μm to 0.66 μm corresponding to 70% reduction in total volume of final polish. The laboratory experiment using one third part of prototype whiffletrees shows supporting force RMS repeatability < 0.005 kgf, and drive hysteresis < 0.7% of load range, which are precise enough to control or to keep the primary mirror figure. Title: Advanced 3D-printed EAP actuator applied to high precision large optical-quality surface fabrication: first results Authors: Thetpraphi, K.; Moretto, G.; Kuhn, J. R.; Cottinet, P. J.; Le, M. Q.; Audigier, D.; Petit, L.; Capsal, J. F. Bibcode: 2020SPIE11375E..1XT Altcode: LiveMetaOptics presented the Exo-life finder (ELF) telescope combined with the hybrid dynamic structure of live and light active mirror named as "Live-mirror". Recently we reported the idea of active optical surface correction using the advantage of an electromechanical stimulator to deform mirror surface in a significant correction scale. An effort to develop a conventional electroactive polymer (EAP) actuator through Live-mirror application has been taken the new approach, assembling EAP actuator via additive manufacturing or 3D printing technology. The approach of next-generation mirror leaned on 3D printing technological advancement is able to unlock the principles of a potentially new actuator manufacturing technique. Full 3D print of modified EAP was formulated with plasticized terpolymer for an active layer and terpolymer/CB composite for printed electrodes. Though rudimentary of electroactive polymer, the full-printed actuator could transfer its transversal stress or shear force to shape the mirror surface under low applied electric fields. We described here as well creating multilayer structures with capabilities well beyond those of the individual actuator components. Our various configurations of printed actuators could achieve glass surface deformation in a range of 50 nm to 2 µm considering the maximum glass deformation. As a result of material modification coupled with 3D printing technology, we can increase productivity while enabling a mass and cost reduction and an increase of the parts functionality in terms of the real application. Title: SPHERE+: Imaging young Jupiters down to the snowline Authors: Boccaletti, A.; Chauvin, G.; Mouillet, D.; Absil, O.; Allard, F.; Antoniucci, S.; Augereau, J. -C.; Barge, P.; Baruffolo, A.; Baudino, J. -L.; Baudoz, P.; Beaulieu, M.; Benisty, M.; Beuzit, J. -L.; Bianco, A.; Biller, B.; Bonavita, B.; Bonnefoy, M.; Bos, S.; Bouret, J. -C.; Brandner, W.; Buchschache, N.; Carry, B.; Cantalloube, F.; Cascone, E.; Carlotti, A.; Charnay, B.; Chiavassa, A.; Choquet, E.; Clenet, Y.; Crida, A.; De Boer, J.; De Caprio, V.; Desidera, S.; Desert, J. -M.; Delisle, J. -B.; Delorme, P.; Dohlen, K.; Doelman, D.; Dominik, C.; Orazi, V. D; Dougados, C.; Doute, S.; Fedele, D.; Feldt, M.; Ferreira, F.; Fontanive, C.; Fusco, T.; Galicher, R.; Garufi, A.; Gendron, E.; Ghedina, A.; Ginski, C.; Gonzalez, J. -F.; Gratadour, D.; Gratton, R.; Guillot, T.; Haffert, S.; Hagelberg, J.; Henning, T.; Huby, E.; Janson, M.; Kamp, I.; Keller, C.; Kenworthy, M.; Kervella, P.; Kral, Q.; Kuhn, J.; Lagadec, E.; Laibe, G.; Langlois, M.; Lagrange, A. -M.; Launhardt, R.; Leboulleux, L.; Le Coroller, H.; Li Causi, G.; Loupias, M.; Maire, A. L.; Marleau, G.; Martinache, F.; Martinez, P.; Mary, D.; Mattioli, M.; Mazoyer, J.; Meheut, H.; Menard, F.; Mesa, D.; Meunier, N.; Miguel, Y.; Milli, J.; Min, M.; Molliere, P.; Mordasini, C.; Moretto, G.; Mugnier, L.; Muro Arena, G.; Nardetto, N.; Diaye, M. N; Nesvadba, N.; Pedichini, F.; Pinilla, P.; Por, E.; Potier, A.; Quanz, S.; Rameau, J.; Roelfsema, R.; Rouan, D.; Rigliaco, E.; Salasnich, B.; Samland, M.; Sauvage, J. -F.; Schmid, H. -M.; Segransan, D.; Snellen, I.; Snik, F.; Soulez, F.; Stadler, E.; Stam, D.; Tallon, M.; Thebault, P.; Thiebaut, E.; Tschudi, C.; Udry, S.; van Holstein, R.; Vernazza, P.; Vidal, F.; Vigan, A.; Waters, R.; Wildi, F.; Willson, M.; Zanutta, A.; Zavagno, A.; Zurlo, A. Bibcode: 2020arXiv200305714B Altcode: SPHERE (Beuzit et al,. 2019) has now been in operation at the VLT for more than 5 years, demonstrating a high level of performance. SPHERE has produced outstanding results using a variety of operating modes, primarily in the field of direct imaging of exoplanetary systems, focusing on exoplanets as point sources and circumstellar disks as extended objects. The achievements obtained thus far with SPHERE (~200 refereed publications) in different areas (exoplanets, disks, solar system, stellar physics...) have motivated a large consortium to propose an even more ambitious set of science cases, and its corresponding technical implementation in the form of an upgrade. The SPHERE+ project capitalizes on the expertise and lessons learned from SPHERE to push high contrast imaging performance to its limits on the VLT 8m-telescope. The scientific program of SPHERE+ described in this document will open a new and compelling scientific window for the upcoming decade in strong synergy with ground-based facilities (VLT/I, ELT, ALMA, and SKA) and space missions (Gaia, JWST, PLATO and WFIRST). While SPHERE has sampled the outer parts of planetary systems beyond a few tens of AU, SPHERE+ will dig into the inner regions around stars to reveal and characterize by mean of spectroscopy the giant planet population down to the snow line. Building on SPHERE's scientific heritage and resounding success, SPHERE+ will be a dedicated survey instrument which will strengthen the leadership of ESO and the European community in the very competitive field of direct imaging of exoplanetary systems. With enhanced capabilities, it will enable an even broader diversity of science cases including the study of the solar system, the birth and death of stars and the exploration of the inner regions of active galactic nuclei. Title: Surface Imaging of Proxima b and Other Exoplanets: Albedo Maps, Biosignatures, and Technosignatures Authors: Berdyugina, S. V.; Kuhn, J. R. Bibcode: 2019AJ....158..246B Altcode: Seeing oceans, continents, quasi-static weather, and other surface features on exoplanets may allow for detecting and characterizing life outside the solar system. The Proxima b exoplanet resides within the stellar habitable zone, possibly allowing for liquid water on its surface, as on Earth. However, even the largest planned telescopes will not be able to resolve its surface features directly. Here we demonstrate an inversion technique to indirectly image exoplanet surfaces using observed unresolved reflected light variations over the course of the exoplanet’s orbital and axial rotation: ExoPlanet Surface Imaging (EPSI). We show that the reflected light curve contains enough information to detect both longitudinal and latitudinal structures and to map exoplanet surface features. We demonstrate this using examples of solar system planets and moons, as well as simulated planets with Earth-like life and artificial structures. We also describe how it is possible to infer the planet and orbit geometry from light curves. Then, we show how albedo maps of Proxima b can be successfully reconstructed for tidally locked, resonance, and unlocked axial and orbital rotation. Such albedo maps obtained in different wavelength passbands can provide “photographic” views of distant exoplanets. We estimate the signal-to-noise ratio necessary for successful inversions and analyze telescope and detector requirements necessary for the first surface image reconstructions of Proxima b and other nearby exoplanets using EPSI. This is a significant challenge, but the success of such measurements depends heavily on large-aperture diffraction-limited telescope performance—a feat that may be achieved on the ground before it is in space. Title: State of the Profession Considerations for Laboratory Astrophysics Authors: Savin, Daniel Wolf; Babb, James F.; Barklem, Paul; Bellan, Paul M.; Betancourt-Martinez, Gabriele; Blum, Jürgen; Boersma, Christiaan; Boryta, Mark D.; Brisset, Julie; Brogan, Crystal; Cami, Jan; Caselli, Paola; Chutjian, Ara; Corrales, Lia; Crabtree, Kyle; Dominguez, Gerardo; Federman, Steven R.; Fontes, Christopher J.; Freedman, Richard; Gavilan-Marin, Lisseth; Gibson, Brad; Golub, Leon; Gorczyca, Thomas W.; Hahn, Michael; Hartmann, Dieter; Hörst, Sarah M.; Hudson, Reggie L.; Ji, Hantao; Kreckel, Holger; Kuhn, Jeffrey; Lawler, James E.; Lee, Timothy J.; Leutenegger, Maurice A.; Mancini, Roberto; Marler, Joan P.; Mashonkina, Lyudmila I.; McCarthy, Michael C.; McCoustra, Martin; McGuire, Brett A.; Milam, Stefanie N.; Montgomery, Mike; Murphy, Nicholas A.; Nave, Gillian; Nelson, Robert M.; Nollett, Kenneth M.; Norton, Aimee A.; Novotný, Oldřich; Papol, Anthony; Raymond, John C.; Salama, Farid; Sciamma-O'Brien, Ella M.; Smith, Randall; Sosolik, Chad; Sousa-Silva, Clara; Spyrou, Artemis; Stancil, Phillip C.; Sung, Keeyoon; Tennyson, Jonathan; Timmes, Frank; Trimble, Virginia L.; Venot, Olivia; Wahlgren, Glenn; Wargelin, Bradford J.; Winget, Don; Wood, Michael P. Bibcode: 2019BAAS...51g...7S Altcode: 2019astro2020U...7S Astrophysics advances, in part, through laboratory astrophysics studies of the underlying processes controlling the observed properties of the Cosmos. These studies encompass both theoretical and experimental research. Robust support for laboratory astrophysics is critically needed to maximize the scientific return of astronomical observations. Title: Coronagraphic Observations of Si X λ14301 and Fe XIII λ10747 Linearly Polarized Spectra Using the SOLARC Telescope Authors: Dima, Gabriel I.; Kuhn, Jeffrey R.; Schad, Thomas A. Bibcode: 2019ApJ...877..144D Altcode: The forbidden Si X emission line at 14301 Å has been identified as a potentially valuable polarized diagnostic for solar coronal magnetic fields; however, the only polarized Si X measurements achieved to date have been during eclipses and at comparatively low spatial and spectral resolution. Here we report spectropolarimetric observations of both the Si X 14301 Å and more well-established Fe XIII 10747 Å coronal lines acquired with the 0.45 m aperture SOLARC coronagraph atop Haleakalā. Using its fiber-based integral field spectropolarimeter, we derive observations sampled at radial intervals of 0.05 {R} (i.e., ∼50″) with a spectral resolving power of ≈36,000. Results for both lines, which represent averages over different active and nonactive regions of the corona, indicate a relatively flat radial variation for the line widths and line centers and a factor of ≈2-3 decrease in polarized brightness between 1.05 and 1.45 {R}. Averaging over all the measurements the mean and standard deviations of line properties for Si X 14301 Å and Fe XIII 10747 Å are, respectively, FWHM of 3.0 ± 0.4 Å and 1.6 ± 0.1 Å, line-integrated polarized brightness of 0.07 ± 0.03 and 0.3 ± 0.3 erg s-2 cm-2 sr-1, where the uncertainty quoted reflects a large sample variance, and line center wavelengths 14300.7 ± 0.2 Å and 10746.3 ± 0.1 Å. The polarized brightness for both lines may be underestimated by up to a factor of 5 due to limitations in the photometric calibration. When accounting for this uncertainty we find consistency between our observations and previous measurements of the two lines as well as theoretical calculations and affirm the potential of the Si X line as a polarized diagnostic of the solar corona. Title: Polarimetric observations of the SiX and Fe XIII infrared coronal emission lines using the SOLARC telescope Authors: Dima, Gabriel; Kuhn, Jeffrey Richard; Schad, Thomas A. Bibcode: 2019AAS...23411704D Altcode: The forbidden Si X emission line at 14301 Å has been identified as a potentially valuable polarized diagnostic for solar coronal magnetic fields; however, the only polarized Si X measurements achieved to date have been during eclipses and at comparatively low spatial and spectral resolution. Here we report spectropolarimetric observations of both the Si X 14301 Å and more well-established FeXIII 10747 Å coronal lines acquired with the 0.45 m aperture SOLARC coronagraph atop Haleakala. Results for both lines, which represent averages over different active and non-active regions of the corona, indicate a relatively flat radial variation for the line widths and line centers and a factor of 2-3 decrease in polarized brightness between 1.05 and 1.45 R. Averaging over all the measurements the mean and standard deviations of line properties for Si X 14301 Å and Fe XIII 10747 Å are respectively: FWHM of 3.0±0.4 Å and 1.6±0.1, line-integrated polarized brightness of 0.07±0.03 and 0.3±0.3 erg s-2 cm-2 sr-1 where the uncertainty quoted reflects a large sample variance, and line center wavelengths 14300.7±0.2 Å and 10746.3±0.1 Å. The polarized brightness for both lines may be underestimated by up to a factor of 5 due to limitations in the photometric calibration. When accounting for this uncertainty we find consistency between our observations and previous measurements of the two lines as well as theoretical calculations and affirm the potential of the Si X line as a polarized diagnostic of the solar corona. Title: Hanle Coronal Magnetometry Using Permitted He I 1083 nm and Forbidden Si X 1430 nm IR Emission Lines Authors: Dima, G. I.; Kuhn, J. R.; Berdyugina, S. V. Bibcode: 2019ASPC..526..199D Altcode: With a model of the coronal Hanle effect, and by measuring the linear polarization of permitted and forbidden lines, it is possible to determine the magnetic field in the emission region of the considered lines. This technique may be applicable in the corona because of the discovery of faint He I emission, possibly due to a non-equilibrium population of He I atoms originating on coronal dust grains. He I 1083 nm lies in the unsaturated Hanle regime for field strengths below 8 G, so that the polarization amplitude and orientation are sensitive to both the orientation and strength of the magnetic field. To break this degeneracy we can use one of several coronal infrared forbidden lines, like Fe XIII 1075 nm or Si X 1430 nm. These forbidden lines are sensitive to different coronal temperature regimes, and provide additional constraints on the orientation of the magnetic field. We discuss magnetic field uncertainties inherent to this measurement technique, and present the first polarized measurements of the Si X 1430 nm line, obtained using the SOLARC telescope on Haleakalā. Title: Astrophysical Science enabled by Laboratory Astrophysics Studies in Atomic, Molecular, and Optical (AMO) Physics Authors: Savin, Daniel Wolf; Babb, James F.; Bellan, Paul M.; Brogan, Crystal; Cami, Jan; Caselli, Paola; Corrales, Lia; Dominguez, Gerardo; Federman, Steven R.; Fontes, Chris J.; Freedman, Richard; Gibson, Brad; Golub, Leon; Gorczyca, Thomas W.; Hahn, Michael; Hartmann, Dieter; Hörst, Sarah M.; Hudson, Reggie L.; Kuhn, Jeffrey; Lawler, James E.; Leutenegger, Maurice A.; Marler, Joan P.; McCarthy, Michael C.; McGuire, Brett A.; Milam, Stefanie N.; Murphy, Nicholas A.; Nave, Gillian; Norton, Aimee A.; Papol, Anthony; Raymond, John C.; Salama, Farid; Sciamma-O'Brien, Ella M.; Smith, Randall; Sosolik, Chad; Sousa-Silva, Clara; Stancil, Phillip C.; Timmes, Frank; Trimble, Virginia L.; Wargelin, Bradford J. Bibcode: 2019BAAS...51c..96S Altcode: 2019astro2020T..96S We highlight a few of the many astrophysical advances that will become possible with advances in AMO laboratory astrophysics. This submission supersedes the previous submission. Title: Measurements of Solar Oblateness during the SDO Mission Authors: Bush, R. I.; Emilio, M.; Scholl, I.; Kuhn, J. R.; Sommers, J. Bibcode: 2018csc..confE...5B Altcode: Beginning in April 2010, the Helioseismic and Magnetic Imager (HMI) instrument on the Solar Dynamics Observatory (SDO) spacecraft has been making periodic measurements of the solar shape. The primary observations are 4096 by 4096 pixel full Sun images taken in the continuum of the 617.3 nm Fe I absorption line in 4 linear polarizations. It is necessary to determine the instrument optical distortion in order to extract the solar shape from the full Sun images. This is accomplished during a roll maneuver of the SDO spacecraft in which the spacecraft is rotated 360 degrees around the Sun-spacecraft line while taking a series of images at 32 uniformly spaced roll angles. Measurements of the solar oblateness are typically obtained twice per year, and eighteen roll maneuvers have been performed by the SDO spacecraft to date. Initially these observations were taken in April and October from 2011 to 2014. During the April 2015 roll, however, the spacecraft maneuver was aborted due to a pointing anomaly. This error condition was identified, but subsequent roll maneuvers were shifted to January and July of the following years. The mean equator to pole radius difference over the nine years of observations is 6.0 +/- 1.0 milli-arcseconds. The higher order (hexadecapole) term is consistent with 0. The long term trend of the solar oblateness does not show a correlation with the current solar sunspot cycle. Details of the measurements and trending will be discussed. Title: Perspectives on Astrophysics Based on Atomic, Molecular, and Optical (AMO) Techniques Authors: Savin, Daniel Wolf; Babb, James F.; Bellan, Paul M.; Brogan, Crystal; Cami, Jan; Caselli, Paola; Corrales, Lia; Dominguez, Gerardo; Federman, Steven R.; Fontes, Chris J.; Freedman, Richard; Gibson, Brad; Golub, Leon; Gorczyca, Thomas W.; Hahn, Michael; Hörst, Sarah M.; Hudson, Reggie L.; Kuhn, Jeffrey; Lawler, James E.; Leutenegger, Maurice A.; Marler, Joan P.; McCarthy, Michael C.; McGuire, Brett A.; Milam, Stefanie N.; Murphy, Nicholas A.; Nave, Gillian; Norton, Aimee A.; Papol, Anthony; Raymond, John C.; Salama, Farid; Sciamma-O'Brien, Ella M.; Smith, Randall; Sosolik, Chad; Sousa-Silva, Clara; Stancil, Phillip C.; Timmes, Frank; Trimble, Virginia L.; Wargelin, Bradford J. Bibcode: 2018arXiv181106157S Altcode: About two generations ago, a large part of AMO science was dominated by experimental high energy collision studies and perturbative theoretical methods. Since then, AMO science has undergone a transition and is now dominated by quantum, ultracold, and ultrafast studies. But in the process, the field has passed over the complexity that lies between these two extremes. Most of the Universe resides in this intermediate region. We put forward that the next frontier for AMO science is to explore the AMO complexity that describes most of the Cosmos. Title: Review of high-contrast imaging systems for current and future ground- and space-based telescopes I: coronagraph design methods and optical performance metrics Authors: Ruane, G.; Riggs, A.; Mazoyer, J.; Por, E. H.; N'Diaye, M.; Huby, E.; Baudoz, P.; Galicher, R.; Douglas, E.; Knight, J.; Carlomagno, B.; Fogarty, K.; Pueyo, L.; Zimmerman, N.; Absil, O.; Beaulieu, M.; Cady, E.; Carlotti, A.; Doelman, D.; Guyon, O.; Haffert, S.; Jewell, J.; Jovanovic, N.; Keller, C.; Kenworthy, M. A.; Kuhn, J.; Miller, K.; Sirbu, D.; Snik, F.; Wallace, J. Kent; Wilby, M.; Ygouf, M. Bibcode: 2018SPIE10698E..2SR Altcode: 2018arXiv180707042R The Optimal Optical Coronagraph (OOC) Workshop at the Lorentz Center in September 2017 in Leiden, the Netherlands gathered a diverse group of 25 researchers working on exoplanet instrumentation to stimulate the emergence and sharing of new ideas. In this first installment of a series of three papers summarizing the outcomes of the OOC workshop, we present an overview of design methods and optical performance metrics developed for coronagraph instruments. The design and optimization of coronagraphs for future telescopes has progressed rapidly over the past several years in the context of space mission studies for Exo-C, WFIRST, HabEx, and LUVOIR as well as ground-based telescopes. Design tools have been developed at several institutions to optimize a variety of coronagraph mask types. We aim to give a broad overview of the approaches used, examples of their utility, and provide the optimization tools to the community. Though it is clear that the basic function of coronagraphs is to suppress starlight while maintaining light from off-axis sources, our community lacks a general set of standard performance metrics that apply to both detecting and characterizing exoplanets. The attendees of the OOC workshop agreed that it would benefit our community to clearly define quantities for comparing the performance of coronagraph designs and systems. Therefore, we also present a set of metrics that may be applied to theoretical designs, testbeds, and deployed instruments. We show how these quantities may be used to easily relate the basic properties of the optical instrument to the detection significance of the given point source in the presence of realistic noise. Title: The Exo-Life Finder Telescope (ELF): design and beam synthesis concepts Authors: Kuhn, J. R.; Berdyugina, S. V.; Capsal, J. -F.; Gedig, M.; Langlois, M.; Moretto, G.; Thetpraphi, K. Bibcode: 2018SPIE10700E..15K Altcode: Currently planned massively segmented telescopes like the European Extremely Large Telescope (EELT)1 or the Thirty Meter Telescope (TMT)2, use "Keck-era" optics. Their mirror subapertures create a dynamically rigid primary optical surface from 100's of 1m-scale few-cm thick mirrors. We suggest that a dedicated telescope for distinguishing reflected exoplanet light from its host star may not follow these design principles. To reduce moving mass and telescope-scattered light, a post-Keck era large telescope could use new technologies that replace this opto-mechanical stiffness with massively parallel active electro-optics and interferometric concepts. This opens the intriguing possibility of building a dedicated ground-based exoplanet telescope with an aperture of 20m at a cost-scale of $100M. This is a compelling reason for exploring what we call "synthetic aperture" or "hybrid optical telescopes." Even larger apertures that could be an order of magnitude less costly per square meter than comparable Keck-like optics are possible. Here we consider an optical system built from a relatively "floppy" optical structure and scalable interferometrically phased, moderate size (5m diameter), subapertures. This ExoLife Finder (ELF) telescope is sensitive to optical biomarker signals and has the power to map the surfaces of nearby M-dwarf exoplanets on subcontinental scales. Title: The Exo-Life Finder (ELF) telescope: New strategies for direct detection of exoplanet biosignatures and technosignatures Authors: Berdyugina, S. V.; Kuhn, J. R.; Langlois, M.; Moretto, G.; Krissansen-Totton, J.; Catling, D.; Grenfell, J. L.; Santl-Temkiv, T.; Finster, K.; Tarter, J.; Marchis, F.; Hargitai, H.; Apai, D. Bibcode: 2018SPIE10700E..4IB Altcode: The Exo-Life Finder (ELF) will be an optical system with the resolving power of a >=20m telescope optimized for characterizing exoplanets and detecting exolife. It will allow for direct detection of Earth-size planets in commonlyconsidered water-based habitable zones (WHZ) of nearby stars and for generic exolife studies. Here we discuss capabilities of the ELF to detect biosignatures and technosignatures in exoplanetary atmospheres and on their surfaces in the visual and near infrared. We evaluate sensitivity limits for mid- and low-resolution spectral, photometric and polarimetric measurements, analyzed using atmosphere models and light-curve inversions. In particular, we model and estimate integration times required to detect O2, O3, CO2, CH4, H2O and other biosignature gases and habitability markers. Disequilibrium biosignature pairs such as O2+CH4 or CO2+CH4-CO are also explored. Photosynthetic and nonphotosynthetic pigments are other important biosignatures that ELF will search for in atmospheres and on resolved surfaces of exoplanets, in the form of bioaerosols and colonies of organisms. Finally, possible artificial structures on exoplanet surfaces and in near-exoplanet space can be detected. Practical instrument requirements are formulated for detecting these spectral and structural biosignatures and technosignatures. It is imperative that such a study is applied first to characterize the nearest exoplanet Proxima b, then to search for exo-Earths in the Alpha Cen A and B system and other near-Sun stars, and finally to explore larger exoplanets around more distant stars. Title: Status of the Daniel K. Inouye Solar Telescope: unraveling the mysteries the Sun. Authors: Rimmele, Thomas R.; Martinez Pillet, Valentin; Goode, Philip R.; Knoelker, Michael; Kuhn, Jeffrey Richard; Rosner, Robert; Casini, Roberto; Lin, Haosheng; von der Luehe, Oskar; Woeger, Friedrich; Tritschler, Alexandra; Fehlmann, Andre; Jaeggli, Sarah A.; Schmidt, Wolfgang; De Wijn, Alfred; Rast, Mark; Harrington, David M.; Sueoka, Stacey R.; Beck, Christian; Schad, Thomas A.; Warner, Mark; McMullin, Joseph P.; Berukoff, Steven J.; Mathioudakis, Mihalis; DKIST Team Bibcode: 2018AAS...23231601R Altcode: The 4m Daniel K. Inouye Solar Telescope (DKIST) currently under construction on Haleakala, Maui will be the world’s largest solar telescope. Designed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the sun, this facility will perform key observations of our nearest star that matters most to humankind. DKIST’s superb resolution and sensitivity will enable astronomers to address many of the fundamental problems in solar and stellar astrophysics, including the origin of stellar magnetism, the mechanisms of coronal heating and drivers of the solar wind, flares, coronal mass ejections and variability in solar and stellar output. DKIST will also address basic research aspects of Space Weather and help improve predictive capabilities. In combination with synoptic observations and theoretical modeling DKIST will unravel the many remaining mysteries of the Sun.The construction of DKIST is progressing on schedule with 80% of the facility complete. Operations are scheduled to begin early 2020. DKIST will replace the NSO facilities on Kitt Peak and Sac Peak with a national facility with worldwide unique capabilities. The design allows DKIST to operate as a coronagraph. Taking advantage of its large aperture and infrared polarimeters DKIST will be capable to routinely measure the currently illusive coronal magnetic fields. The state-of-the-art adaptive optics system provides diffraction limited imaging and the ability to resolve features approximately 20 km on the Sun. Achieving this resolution is critical for the ability to observe magnetic structures at their intrinsic, fundamental scales. Five instruments will be available at the start of operations, four of which will provide highly sensitive measurements of solar magnetic fields throughout the solar atmosphere - from the photosphere to the corona. The data from these instruments will be distributed to the world wide community via the NSO/DKIST data center located in Boulder. We present examples of science objectives and provide an overview of the facility and project status, including the ongoing efforts of the community to develop the critical science plan for the first 2-3 years of operations. Title: Using a New Infrared Si X Coronal Emission Line for Discriminating between Magnetohydrodynamic Models of the Solar Corona During the 2006 Solar Eclipse Authors: Dima, Gabriel I.; Kuhn, Jeffrey R.; Mickey, Don; Downs, Cooper Bibcode: 2018ApJ...852...23D Altcode: During the 2006 March 29 total solar eclipse, coronal spectropolarimetric measurements were obtained over a 6 × 6 R field of view with a 1-2 μm spectral range. The data yielded linearly polarized measurements of the Fe XIII 1.075 μm, He I 1.083 μm, and for the first time, of the Si X 1.430 μm emission lines. To interpret the measurements, we used forward-integrated synthetic emission from two magnetohydrodynamic models for the same Carrington rotation with different heating functions and magnetic boundary conditions. Observations of the Fe XIII 1.075/Si X 1.430 line ratio allowed us to discriminate between two models of the corona, with the observations strongly favoring the warmer model. The observed polarized amplitudes for the Si X 1.430 μm line are around 7%, which is three times higher than the predicted values from available atomic models for the line. This discrepancy indicates a need for a closer look at some of the model assumptions for the collisional coefficients, as well as new polarized observations of the line to rule out any unknown systematic effect in the present data. All but two near-limb fibers show correlated bright He I 1.083 μm and H I 1.282 μm emission, which likely indicates cool prominence emission that is non-localized by the strongly defocused optics. One of the distant fibers located at 1.5 R detected a weak He I 1.083 μm intensity signal consistent with previous eclipse measurements around 3 × 10-7 {B}. However, given the limitations of these observations, it is not possible to completely remove contamination that is due to emission from prominence material that is not obscured by the lunar limb. Title: Constraining Line-of-sight Confusion in the Corona Using Linearly Polarized Observations of the Infrared FeXIII 1075nm and SiX 1430nm Emission Lines Authors: Dima, G. I.; Kuhn, J. R.; Berdyugina, S. Bibcode: 2017AGUFMSH54A..03D Altcode: Measurements of the coronal magnetic field are difficult because of the intrinsically faint emission of coronal plasma and the large spurious background due to the bright solar disk. This work addresses the problem of resolving the confusion of the line-of-sight (LOS) integration through the optically-thin corona being observed. Work on developing new measuring techniques based on single-point inversions using the Hanle effect has already been described (Dima et al. 2016). It is important to develop a technique to assess when the LOS confusion makes comparing models and observations problematic. Using forward integration of synthetic emission through magnetohydrodynamic (MHD) models together with simultaneous linearly polarized observations of the FeXIII 1075nm and SiX 1430nm emission lines allows us to assess LOS confusion. Since the lines are both in the Hanle saturated regime their polarization angles are expected to be aligned as long as the gas is sampling the same magnetic field. If significant contributions to the emission is taking place from different regions along the LOS due to the additive nature of the polarized brightness the measured linear polarization between the two lines will be offset. The size of the resolution element is important for this determination since observing larger coronal regions will confuse the variation along the LOS with that in the plane-of-sky. We also present comparisons between synthetic linearly polarized emission through a global MHD model and observations of the same regions obtained using the 0.5m Scatter-free Observatory for Limb Active Regions and Coronae (SOLARC) telescope located on Haleakala, Maui. This work is being done in preparation for the type of observations that will become possible when the next generation 4m DKIST telescope comes online in 2020. Title: Space Weathering of Super-Earths: Model Simulations of Exospheric Sodium Escape from 61 Virgo b Authors: Yoneda, M.; Berdyugina, S.; Kuhn, J. Bibcode: 2017AJ....154..139Y Altcode: Rocky exoplanets are expected to be eroded by space weather in a similar way as in the solar system. In particular, Mercury is one of the dramatically eroded planets whose material continuously escapes into its exosphere and further into space. This escape is well traced by sodium atoms scattering sunlight. Due to solar wind impact, micrometeorite impacts, photo-stimulated desorption and thermal desorption, sodium atoms are released from surface regolith. Some of these released sodium atoms are escaping from Mercury’s gravitational-sphere. They are dragged anti-Sun-ward and form a tail structure. We expect similar phenomena on exoplanets. The hot super-Earth 61 Vir b orbiting a G3V star at only 0.05 au may show a similar structure. Because of its small separation from the star, the sodium release mechanisms may be working more efficiently on hot super-Earths than on Mercury, although the strong gravitational force of Earth-sized or even more massive planets may be keeping sodium atoms from escaping from the planet. Here, we performed model simulations for Mercury (to verify our model) and 61 Vir b as a representative super-Earth. We have found that sodium atoms can escape from this exoplanet due to stellar wind sputtering and micrometeorite impacts, to form a sodium tail. However, in contrast to Mercury, the tail on this hot super-Earth is strongly aligned with the anti-starward direction because of higher light pressure. Our model suggests that 61 Vir b seems to have an exo-base atmosphere like that of Mercury. Title: Partially Filled Aperture Interferometric Telescopes: Achieving Large Aperture and Coronagraphic Performance Authors: Moretto, G.; Kuhn, J.; Langlois, M.; Berdugyna, S.; Tallon, M. Bibcode: 2017EPSC...11..893M Altcode: Telescopes larger than currently planned 30-m class instruments must break the mass-aperture scaling relationship of the Keck-generation of multi-segmented telescopes. Partially filled aperture, but highly redundant baseline interferometric instruments may achieve both large aperture and high dynamic range. The PLANETS FOUNDATION group has explored hybrid telescope-interferometer concepts for narrow-field optical systems that exhibit coronagraphic performance over narrow fields-of-view. This paper describes how the Colossus and Exo-Life Finder telescope designs achieve 10x lower moving masses than current Extremely Large Telescopes. Title: First Detection of a Strong Magnetic Field on a Bursty Brown Dwarf: Puzzle Solved Authors: Berdyugina, S. V.; Harrington, D. M.; Kuzmychov, O.; Kuhn, J. R.; Hallinan, G.; Kowalski, A. F.; Hawley, S. L. Bibcode: 2017ApJ...847...61B Altcode: 2017arXiv170902861B We report the first direct detection of a strong, 5 kG magnetic field on the surface of an active brown dwarf. LSR J1835+3259 is an M8.5 dwarf exhibiting transient radio and optical emission bursts modulated by fast rotation. We have detected the surface magnetic field as circularly polarized signatures in the 819 nm sodium lines when an active emission region faced the Earth. Modeling Stokes profiles of these lines reveals the effective temperature of 2800 K and log gravity acceleration of 4.5. These parameters place LSR J1835+3259 on evolutionary tracks as a young brown dwarf with the mass of 55+/- 4{M}{{J}} and age of 22 ± 4 Myr. Its magnetic field is at least 5.1 kG and covers at least 11% of the visible hemisphere. The active region topology recovered using line profile inversions comprises hot plasma loops with a vertical stratification of optical and radio emission sources. These loops rotate with the dwarf in and out of view causing periodic emission bursts. The magnetic field is detected at the base of the loops. This is the first time that we can quantitatively associate brown dwarf non-thermal bursts with a strong, 5 kG surface magnetic field and solve the puzzle of their driving mechanism. This is also the coolest known dwarf with such a strong surface magnetic field. The young age of LSR J1835+3259 implies that it may still maintain a disk, which may facilitate bursts via magnetospheric accretion, like in higher-mass T Tau-type stars. Our results pave a path toward magnetic studies of brown dwarfs and hot Jupiters. Title: Critical Infrared Science with the Daniel K. Inouye Solar Telescope Authors: Schad, Thomas A.; Fehlmann, Andre; Jaeggli, Sarah A.; Kuhn, Jeffrey Richard; Lin, Haosheng; Penn, Matthew J.; Rimmele, Thomas R.; Woeger, Friedrich Bibcode: 2017SPD....4811703S Altcode: Critical science planning for early operations of the Daniel K. Inouye Solar Telescope is underway. With its large aperture, all-reflective telescope design, and advanced instrumentation, DKIST provides unprecedented access to the important infrared (IR) solar spectrum between 1 and 5 microns. Breakthrough IR capabilities in coronal polarimetry will sense the coronal magnetic field routinely for the first time. The increased Zeeman resolution near the photospheric opacity minimum will provide our deepest and most sensitive measurement of quiet sun and active region magnetic fields to date. High-sensitivity He I triplet polarimetry will dynamically probe the chromospheric magnetic field in fibrils, spicules, and filaments, while observations of molecular CO transitions will characterize the coolest regions of the solar atmosphere. When combined with the longer timescales of good atmospheric seeing compared with the visible, DKIST infrared diagnostics are expected to be mainstays of solar physics in the DKIST era. This paper will summarize the critical science areas addressed by DKIST infrared instrumentation and invite the community to further contribute to critical infrared science planning. Title: The Cryogenic Near Infrared Spectropolarimeter for the Daniel K. Inouye Solar Telescope Authors: Fehlmann, Andre; Giebink, Cindy; Kuhn, Jeffrey Richard; Mickey, D. L.; Scholl, Isabelle Bibcode: 2017SPD....4811702F Altcode: The Cryogenic Near Infrared Spectropolarimeter is one of the first light instruments for the Daniel K. Inouye Solar Telescope. This dual-beam instrument, which is currently characterized at the University of Hawaii’s Institute for Astronomy, is designed to sensitively measure the solar spectrum at wavelengths from 1 to 5 μm. The high dynamic range of the spectrograph and its context imager will provide sensitive data of the solar disk in the CO bands; unique observations of the low corona and unprecedented measurements of the coronal magnetic field. Observations near the limb and in the corona will greatly benefit from DKIST’s limb occulting system. The initial suite of filters includes selecting filters for the spectrograph at He I / Fe XIII 1080 nm, Si X 1430 nm, Si IX 3934 nm and CO 4651 nm as well as narrow band filters for the context imager at Fe XIII 1074.7 nm, He I 1083.0, Si X 1430.0 nm and J band 1250 nm. In this paper we will present an update on the ongoing instrument characterization and CryoNIRSP’s capabilities. Title: Daytime sky polarization calibration limitations Authors: Harrington, David M.; Kuhn, Jeffrey R.; Ariste, Arturo López Bibcode: 2017JATIS...3a8001H Altcode: 2016arXiv161200538H The daytime sky has recently been demonstrated as a useful calibration tool for deriving polarization cross-talk properties of large astronomical telescopes. The Daniel K. Inouye Solar Telescope and other large telescopes under construction can benefit from precise polarimetric calibration of large mirrors. Several atmospheric phenomena and instrumental errors potentially limit the technique's accuracy. At the 3.67-m AEOS telescope on Haleakala, we performed a large observing campaign with the HiVIS spectropolarimeter to identify limitations and develop algorithms for extracting consistent calibrations. Effective sampling of the telescope optical configurations and filtering of data for several derived parameters provide robustness to the derived Mueller matrix calibrations. Second-order scattering models of the sky show that this method is relatively insensitive to multiple-scattering in the sky, provided calibration observations are done in regions of high polarization degree. The technique is also insensitive to assumptions about telescope-induced polarization, provided the mirror coatings are highly reflective. Zemax-derived polarization models show agreement between the functional dependence of polarization predictions and the corresponding on-sky calibrations. Title: Daniel K. Inouye Solar Telescope: High-resolution observing of the dynamic Sun Authors: Tritschler, A.; Rimmele, T. R.; Berukoff, S.; Casini, R.; Kuhn, J. R.; Lin, H.; Rast, M. P.; McMullin, J. P.; Schmidt, W.; Wöger, F.; DKIST Team Bibcode: 2016AN....337.1064T Altcode: The 4-m aperture Daniel K. Inouye Solar Telescope (DKIST) formerly known as the Advanced Technology Solar Telescope (ATST) is currently under construction on Haleakalā (Maui, Hawai'i) projected to start operations in 2019. At the time of completion, DKIST will be the largest ground-based solar telescope providing unprecedented resolution and photon collecting power. The DKIST will be equipped with a set of first-light facility-class instruments offering unique imaging, spectroscopic and spectropolarimetric observing opportunities covering the visible to infrared wavelength range. This first-light instrumentation suite will include: a Visible Broadband Imager (VBI) for high-spatial and -temporal resolution imaging of the solar atmosphere; a Visible Spectro-Polarimeter (ViSP) for sensitive and accurate multi-line spectropolarimetry; a Fabry-Pérot based Visible Tunable Filter (VTF) for high-spatial resolution spectropolarimetry; a fiber-fed Diffraction-Limited Near Infra-Red Spectro-Polarimeter (DL-NIRSP) for two-dimensional high-spatial resolution spectropolarimetry (simultaneous spatial and spectral information); and a Cryogenic Near Infra-Red Spectro-Polarimeter (Cryo-NIRSP) for coronal magnetic field measurements and on-disk observations of, e.g., the CO lines at 4.7 μm. We will provide an overview of the DKIST's unique capabilities with strong focus on the first-light instrumentation suite, highlight some of the additional properties supporting observations of transient and dynamic solar phenomena, and touch on some operational strategies and the DKIST critical science plan. Title: Cryogenic near infrared spectropolarimeter for the Daniel K. Inouye Solar Telescope Authors: Fehlmann, Andre; Giebink, Cynthia; Kuhn, Jeffrey R.; Messersmith, Ernesto J.; Mickey, Donald L.; Scholl, Isabelle F.; James, Don; Hnat, Kirby; Schickling, Greg; Schickling, Richard Bibcode: 2016SPIE.9908E..4DF Altcode: The Cryogenic Near Infrared Spectropolarimeter for the Daniel K Inouye Solar Telescope is designed to measure polarized light from 0.5 to 5 μm. It uses an almost all reflective design for high throughput and an R2 echelle grating to achieve the required resolution of up to R = 100,000. The optics cooled to cryogenic temperatures reduce the thermal background allowing for IR observations of the faint solar corona. Both the spectrograph and its context imager use H2RG detector arrays with a newly designed controller to allow synchronized exposures at frame rates up to 10 Hz. All hardware has been built and tested and the key components met their design goals. 1) The cryogenic system uses mechanical closed cycle coolers which introduce vibrations. Our design uses a two stage approach with a floating mounting disk and flexible cold links to reduce these. The vibration amplitudes on all critical stages were measured and are smaller than 1μm. 2) The grating stage of the spectrograph uses a double stack of harmonic drives and an optical encoder to provide sub-arcsecond resolution and a measured repeatability of better than 0.5 arcsec. Title: Daytime sky polarization calibration limitations Authors: Harrington, David M.; Kuhn, Jeffrey R.; López Ariste, Arturo Bibcode: 2016SPIE.9912E..6SH Altcode: The daytime sky has been recently demonstrated as a useful calibration tool for deriving polarization cross-talk properties of large astronomical telescopes. The Daniel K Inouye Solar Telescope (DKIST) and other large telescopes under construction can benefit from precise polarimetric calibration of large off-axis mirrors. Several atmospheric phenomena and instrumental errors potentially limit the techniques accuracy. At the 3.67m AEOS telescope on Haleakala, we have performed a large observing campaign with the HiVIS spectropolarimeter to identify limitations and develop algorithms for extracting consistent calibrations. Effective sampling of the telescope optical configurations and filtering of data for several derived parameters provide robustness to the derivedMueller matrix calibrations. Second-order scattering models of the sky show that this method is relatively insensitive to assumptions about telescope induced polarization provided the mirror coatings are highly reflective. Zemax-derived polarization models show agreement between predictions and on-sky calibrations. Title: IR heterodyne spectrometer MILAHI for continuous monitoring observatory of Martian and Venusian atmospheres at Mt. Haleakalā, Hawaii Authors: Nakagawa, Hiromu; Aoki, Shohei; Sagawa, Hideo; Kasaba, Yasumasa; Murata, Isao; Sonnabend, Guido; Sornig, Manuela; Okano, Shoichi; Kuhn, Jeffrey R.; Ritter, Joseph M.; Kagitani, Masato; Sakanoi, Takeshi; Taguchi, Makoto; Takami, Kosuke Bibcode: 2016P&SS..126...34N Altcode: A new Mid-Infrared Laser Heterodyne Instrument (MILAHI) with >106 resolving power at 7-12 μm was developed for continuous monitoring of planetary atmospheres by using dedicated ground-based telescopes for planetary science at Mt. Haleakalā, Hawaii. Room-temperature-type quantum cascade lasers (QCLs) that cover wavelength ranges of 7.69-7.73, 9.54-9.59, and 10.28-10.33 μm have been newly installed as local oscillators to allow observation of CO2, CH4, H2O2, H2O, and HDO. Modeling and predictions by radiative transfer code gave the following scientific capabilities and measurement sensitivities of the MILAHI. (1) Temperature profiles are achieved at altitudes of 65-90 km on Venus, and the ground surface to 30 km on Mars. (2) New wind profiles are provided at altitudes of 75-90 km on Venus, and 5-25 km on Mars. (3) Direct measurements of the mesospheric wind and temperature are obtained from the Doppler-shifted emission line at altitudes of 110 km on Venus and 75 km on Mars. (4) Detections of trace gases and isotopic ratios are performed without any ambiguity of the reproducing the terrestrial atmospheric absorptions in the observed wavelength range. A HDO measurement of twice the Vienna Standard Mean Ocean Water (VSMOW) can be obtained by 15-min integration, while H2O of 75 ppm is provided by 3.62-h integration. The detectability of the 100 ppb-CH4 on Mars corresponds to an integration time of 32 h. Title: The SCExAO high contrast imager: transitioning from commissioning to science Authors: Jovanovic, N.; Guyon, O.; Lozi, J.; Currie, T.; Hagelberg, J.; Norris, B.; Singh, G.; Pathak, P.; Doughty, D.; Goebel, S.; Males, J.; Kuhn, J.; Serabyn, E.; Tuthill, P.; Schworer, G.; Martinache, F.; Kudo, T.; Kawahara, H.; Kotani, T.; Ireland, M.; Feger, T.; Rains, A.; Bento, J.; Schwab, C.; Coutts, D.; Cvetojevic, N.; Gross, S.; Arriola, A.; Lagadec, T.; Kasdin, J.; Groff, T.; Mazin, B.; Minowa, Y.; Takato, N.; Tamura, M.; Takami, H.; Hayashi, M. Bibcode: 2016SPIE.9909E..0WJ Altcode: SCExAO is the premier high-contrast imaging platform for the Subaru Telescope. It offers high Strehl ratios at near-IR wavelengths (y-K band) with stable pointing and coronagraphs with extremely small inner working angles, optimized for imaging faint companions very close to the host. In the visible, it has several interferometric imagers which offer polarimetric and spectroscopic capabilities. A recent addition is the RHEA spectrograph enabling spatially resolved high resolution spectroscopy of the surfaces of giant stars, for example. New capabilities on the horizon include post-coronagraphic spectroscopy, spectral differential imaging, nulling interferometry as well as an integral field spectrograph and an MKID array. Here we present the new modules of SCExAO, give an overview of the current commissioning status of each of the modules and present preliminary results. Title: Construction Status and Early Science with the Daniel K. Inouye Solar Telescope Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Warner, Mark; Martinez Pillet, Valentin; Craig, Simon; Woeger, Friedrich; Tritschler, Alexandra; Berukoff, Steven J.; Casini, Roberto; Goode, Philip R.; Knoelker, Michael; Kuhn, Jeffrey Richard; Lin, Haosheng; Mathioudakis, Mihalis; Reardon, Kevin P.; Rosner, Robert; Schmidt, Wolfgang Bibcode: 2016SPD....4720101M Altcode: The 4-m Daniel K. Inouye Solar Telescope (DKIST) is in its seventh year of overall development and its fourth year of site construction on the summit of Haleakala, Maui. The Site Facilities (Utility Building and Support & Operations Building) are in place with ongoing construction of the Telescope Mount Assembly within. Off-site the fabrication of the component systems is completing with early integration testing and verification starting.Once complete this facility will provide the highest sensitivity and resolution for study of solar magnetism and the drivers of key processes impacting Earth (solar wind, flares, coronal mass ejections, and variability in solar output). The DKIST will be equipped initially with a battery of first light instruments which cover a spectral range from the UV (380 nm) to the near IR (5000 nm), and capable of providing both imaging and spectro-polarimetric measurements throughout the solar atmosphere (photosphere, chromosphere, and corona); these instruments are being developed by the National Solar Observatory (Visible Broadband Imager), High Altitude Observatory (Visible Spectro-Polarimeter), Kiepenheuer Institute (Visible Tunable Filter) and the University of Hawaii (Cryogenic Near-Infrared Spectro-Polarimeter and the Diffraction-Limited Near-Infrared Spectro-Polarimeter). Further, a United Kingdom consortium led by Queen's University Belfast is driving the development of high speed cameras essential for capturing the highly dynamic processes measured by these instruments. Finally, a state-of-the-art adaptive optics system will support diffraction limited imaging capable of resolving features approximately 20 km in scale on the Sun.We present the overall status of the construction phase along with the current challenges as well as a review of the planned science testing and the transition into early science operations. Title: Infrared Dual-line Hanle diagnostic of the Coronal Vector Magnetic Field Authors: Dima, Gabriel; Kuhn, Jeffrey; Berdyugina, Svetlana Bibcode: 2016FrASS...3...13D Altcode: Measuring the coronal vector magnetic field is still a major challenge in solar physics. This is due to the intrinsic weakness of the field (e.g. ~4G at a height of 0.1Rsun above an active region) and the large thermal broadening of coronal emission lines. We propose using concurrent linear polarization measurements of near-infrared forbidden and permitted lines together with Hanle effect models to calculate the coronal vector magnetic field. In the unsaturated Hanle regime both the direction and strength of the magnetic field affect the linear polarization, while in the saturated regime the polarization is insensitive to the strength of the field. The relatively long radiative lifetimes of coronal forbidden atomic transitions implies that the emission lines are formed in the saturated Hanle regime and the linear polarization is insensitive to the strength of the field. By combining measurements of both forbidden and permitted lines, the direction and strength of the field can be obtained. For example, the SiX 1.4301 um line shows strong linear polarization and has been observed in emission over a large field-of-view (out to elongations of 0.5 Rsun. Here we describe an algorithm that combines linear polarization measurements of the SiX 1.4301 um forbidden line with linear polarization observations of the HeI 1.0830 um permitted coronal line to obtain the vector magnetic field. To illustrate the concept we assume the emitting gas for both atomic transitions is located in the plane of the sky. The further development of this method and associated tools will be a critical step towards interpreting the high spectral, spatial and temporal infrared spectro-polarimetric measurements that will be possible when the Daniel K. Inouye Solar Telescope (DKIST) is completed in 2019. Title: Haleakalā Sky Polarization: Full-Sky Observations and Modeling Authors: Swindle, R.; Kuhn, J. R. Bibcode: 2015PASP..127.1061S Altcode: No abstract at ADS Title: Discovery of a Low-mass Companion Around HR 3549 Authors: Mawet, D.; David, T.; Bottom, M.; Hinkley, S.; Stapelfeldt, K.; Padgett, D.; Mennesson, B.; Serabyn, E.; Morales, F.; Kuhn, J. Bibcode: 2015ApJ...811..103M Altcode: 2015arXiv150905689M We report the discovery of a low-mass companion to HR 3549, an A0V star surrounded by a debris disk with a warm excess detected by WISE at 22 μm (10σ significance). We imaged HR 3549 B in the L band with NAOS-CONICA, the adaptive optics infrared camera of the Very Large Telescope, in January 2013 and confirmed its common proper motion in 2015 January. The companion is at a projected separation of ≃80 AU and position angle of ≃157°, so it is orbiting well beyond the warm disk inner edge of r > 10 AU. Our age estimate for this system corresponds to a companion mass in the range 15-80 MJ, spanning the brown dwarf regime, and so HR 3549 B is another recent addition to the growing list of brown dwarf desert objects with extreme mass ratios. The simultaneous presence of a warm disk and a brown dwarf around HR 3549 provides interesting empirical constraints on models of the formation of substellar companions. Title: The Subaru Coronagraphic Extreme Adaptive Optics System: Enabling High-Contrast Imaging on Solar-System Scales Authors: Jovanovic, N.; Martinache, F.; Guyon, O.; Clergeon, C.; Singh, G.; Kudo, T.; Garrel, V.; Newman, K.; Doughty, D.; Lozi, J.; Males, J.; Minowa, Y.; Hayano, Y.; Takato, N.; Morino, J.; Kuhn, J.; Serabyn, E.; Norris, B.; Tuthill, P.; Schworer, G.; Stewart, P.; Close, L.; Huby, E.; Perrin, G.; Lacour, S.; Gauchet, L.; Vievard, S.; Murakami, N.; Oshiyama, F.; Baba, N.; Matsuo, T.; Nishikawa, J.; Tamura, M.; Lai, O.; Marchis, F.; Duchene, G.; Kotani, T.; Woillez, J. Bibcode: 2015PASP..127..890J Altcode: 2015arXiv150700017J The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is a multipurpose high-contrast imaging platform designed for the discovery and detailed characterization of exoplanetary systems and serves as a testbed for high-contrast imaging technologies for ELTs. It is a multi-band instrument which makes use of light from 600 to 2500nm allowing for coronagraphic direct exoplanet imaging of the inner 3 lambda/D from the stellar host. Wavefront sensing and control are key to the operation of SCExAO. A partial correction of low-order modes is provided by Subaru's facility adaptive optics system with the final correction, including high-order modes, implemented downstream by a combination of a visible pyramid wavefront sensor and a 2000-element deformable mirror. The well corrected NIR (y-K bands) wavefronts can then be injected into any of the available coronagraphs, including but not limited to the phase induced amplitude apodization and the vector vortex coronagraphs, both of which offer an inner working angle as low as 1 lambda/D. Non-common path, low-order aberrations are sensed with a coronagraphic low-order wavefront sensor in the infrared (IR). Low noise, high frame rate, NIR detectors allow for active speckle nulling and coherent differential imaging, while the HAWAII 2RG detector in the HiCIAO imager and/or the CHARIS integral field spectrograph (from mid 2016) can take deeper exposures and/or perform angular, spectral and polarimetric differential imaging. Science in the visible is provided by two interferometric modules: VAMPIRES and FIRST, which enable sub-diffraction limited imaging in the visible region with polarimetric and spectroscopic capabilities respectively. We describe the instrument in detail and present preliminary results both on-sky and in the laboratory. Title: Correcting Systematic Polarization Effects in Keck LRISp Spectropolarimetry to < 0.05% Authors: Harrington, David M.; Berdyugina, Svetlana V.; Kuzmychov, Oleksii; Kuhn, Jeffrey R. Bibcode: 2015PASP..127..757H Altcode: 2015arXiv150503916H Spectropolarimetric measurements at moderate spectral resolutions are effective tracers of stellar magnetic fields and circumstellar environments when signal to noise ratios (SNRs) above 2000 can be achieved. The LRISp spectropolarimeter is capable of achieving these SNRs on faint targets with the 10m aperture of the Keck telescope, provided several instrumental artifacts can be suppressed. We describe here several methods to overcome instrumental error sources that are required to achieve these high SNRs on LRISp. We explore high SNR techniques such as defocusing and slit-stepping during integration with high spectral and spatial oversampling. We find that the instrument flexure and interference fringes introduced by the achromatic retarders create artificial signals at 0.5\% levels in the red channel which mimic real stellar signals and limit the sensitivity and calibration stability of LRISp. Careful spectral extraction and data filtering algorithms can remove these error sources. For faint targets and long exposures, cosmic ray hits are frequent and present a major limitation to the upgraded deep depletion red-channel CCD. These must be corrected to the same high SNR levels, requiring careful spectral extraction using iterative filtering algorithms. We demonstrate here characterization of these sources of instrumental polarization artifacts and present several methods used to successfully overcome these limitations. We have measured the linear to circular cross-talk and find it to be roughly 5\%, consistent with the known instrument limitations. We show spectropolarimetric signals on brown dwarfs are clearly detectable at 0.2\% amplitudes with sensitivities better than 0.05\% at full spectral sampling in atomic and molecular bands. Future LRISp users can perform high sensitivity observations with high quality calibration when following the described algorithms. Title: Calibrating and stabilizing spectropolarimeters with charge shuffling and daytime sky measurements Authors: Harrington, D.; Kuhn, J. R.; Nevin, R. Bibcode: 2015A&A...578A.126H Altcode: 2015arXiv150306744H Well-calibrated spectropolarimetry studies at resolutions of R > 10 000 with signal-to-noise ratios (S/Ns) better than 0.01% across individual line profiles, are becoming common with larger aperture telescopes. Spectropolarimetric studies require high S/N observations and are often limited by instrument systematic errors. As an example, fiber-fed spectropolarimeters combined with advanced line-combination algorithms can reach statistical error limits of 0.001% in measurements of spectral line profiles referenced to the continuum. Calibration of such observations is often required both for cross-talk and for continuum polarization. This is not straightforward since telescope cross-talk errors are rarely less than ~1%. In solar instruments like the Daniel K. Inouye Solar Telescope (DKIST), much more stringent calibration is required and the telescope optical design contains substantial intrinsic polarization artifacts. This paper describes some generally useful techniques we have applied to the HiVIS spectropolarimeter at the 3.7 m AEOS Telescope on Haleakala. HiVIS now yields accurate polarized spectral line profiles that are shot-noise limited to 0.01% S/N levels at our full spectral resolution of 10 000 at spectral sampling of ~100 000. We show line profiles with absolute spectropolarimetric calibration for cross-talk and continuum polarization in a system with polarization cross-talk levels of essentially 100%. In these data the continuum polarization can be recovered to one percent accuracy because of synchronized charge-shuffling model now working with our CCD detector. These techniques can be applied to other spectropolarimeters on other telescopes for both night and daytime applications such as DKIST, TMT, and ELT which have folded non-axially symmetric foci. Title: Measuring the Solar Radius from Space during the 2012 Venus Transit Authors: Emilio, M.; Couvidat, S.; Bush, R. I.; Kuhn, J. R.; Scholl, I. F. Bibcode: 2015ApJ...798...48E Altcode: We report in this work the determination of the solar radius from observations by the Helioseismic and Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) instruments on board the Solar Dynamics Observatory during the 2012 June Venus transit of the Sun. Two different methods were utilized to determine the solar radius using images of Sun taken by the HMI instrument. The first technique fit the measured trajectory of Venus in front of the Sun for seven wavelengths across the Fe I absorption line at 6173 Å. The solar radius determined from this method varies with the measurement wavelength, reflecting the variation in the height of line formation. The second method measured the area of the Sun obscured by Venus to determine the transit duration from which the solar radius was derived. This analysis focused on measurements taken in the continuum wing of the line, and applied a correction for the instrumental point spread function (PSF) of the HMI images. Measurements taken in the continuum wing of the 6173 Å line, resulted in a derived solar radius at 1 AU of 959.''57 ± 0.''02 (695, 946 ± 15 km). The AIA instrument observed the Venus transit at ultraviolet wavelengths. Using the solar disk obscuration technique, similar to that applied to the HMI images, analysis of the AIA data resulted in values of R = 963.''04 ± 0.''03 at 1600 Å and R = 961.''76 ± 0.''03 at 1700 Å. Title: DKIST: Observing the Sun at High Resolution Authors: Tritschler, A.; Rimmele, T. R.; Berukoff, S.; Casini, R.; Craig, S. C.; Elmore, D. F.; Hubbard, R. P.; Kuhn, J. R.; Lin, H.; McMullin, J. P.; Reardon, K. P.; Schmidt, W.; Warner, M.; Woger, F. Bibcode: 2015csss...18..933T Altcode: The 4-m aperture Daniel K. Inouye Solar Telescope (DKIST) formerly known as the Advanced Technology Solar Telescope (ATST) and currently under construction on Haleakalā (Maui, Hawai'i) will be the largest solar ground-based telescope and leading resource for studying the dynamic Sun and its phenomena at high spatial, spectral and temporal resolution. Accurate and sensitive polarimetric observations at high-spatial resolution throughout the solar atmosphere including the corona is a high priority and a major science driver. As such the DKIST will offer a combination of state-of-the-art instruments with imaging and/or spectropolarimetric capabilities covering a broad wavelength range. This first-light instrumentation suite will include: a Visible Broadband Imager (VBI) for high-spatial and -temporal resolution imaging of the solar atmosphere; a Visible Spectro-Polarimeter (ViSP) for sensitive and accurate multi-line spectropolarimetry; a double Fabry-Pérot based Visible Tunable Filter (VTF) for high-spatial resolution spectropolarimetry; a fiber-fed 2D Diffraction-Limited Near Infra-Red Spectro-Polarimeter (DL-NIRSP); and a Cryogenic Near Infra-Red Spectro-Polarimeter (Cryo-NIRSP) for coronal magnetic field measurements and on-disk observations of e.g. the CO lines at 4.7 microns. We will provide a brief overview of the DKIST's unique capabilities to perform spectroscopic and spectropolarimetric measurements of the solar atmosphere using its first-light instrumentation suite, the status of the construction project, and how facility and data access is provided to the US and international community. Title: Microarsecond Solar Limb Astrometry from Space Authors: Kuhn, J. R.; Cunnyngham, I.; Bush, R. I.; Emilio, M.; Scholl, I. F. Bibcode: 2014AGUFMSH41C4157K Altcode: The solar limb astrometry program for HMI has accumulated several years of precise limb brightness and shape measurements. From above the Earth's atmosphere, with the stable SDO/HMI instrument platform, individual limb measurements are accurate to the 10's of milliarcsecond level. The combined timeseries of solar limb shape is sensitive to solar shape perturbations at the submicroarcsecond level. Oscillatory phenomena (like solar g- and r-modes) may be detected at low frequencies with effective velocity amplitudes of 10's of microns per second. We describe here the low frequency shape and limb brightness oscillations observed by HMI from 1 - 3000 microHz. Title: Combining Linear Polarization Measurements of both Forbidden/Permitted Coronal Emission Lines for measuring the Vector Magnetic Field in the Solar Corona Authors: Dima, G. I.; Kuhn, J. R.; Mickey, D. Bibcode: 2014AGUFMSH23C..03D Altcode: Measuring the coronal vector magnetic field is still a major challenge in solar physics. This is due to the intrinsic weakness of the field (~4 G at a height of 0.1 Rsun above an active region) and the large thermal broadening of coronal emission lines. Current methods deduce either the direction of the magnetic field or the magnetic flux density. We propose using concurrent linear polarization measurements in the near IR of forbidden and permitted lines to calculate the coronal vector magnetic field. The effect of the magnetic field on the polarization properties of emitted light is encapsulated in the Hanle effect. In the unsaturated Hanle regime both the direction and strength of the magnetic field affect the linear polarization, while for saturated Hanle the polarization is insensitive to the strength of the field. Coronal forbidden lines are always in the saturated Hanle regime so the linear polarization holds no information on the strength of the field. By pairing measurements of both forbidden and permitted lines we would be able to obtain both the direction and strength of the field. The near-IR region of the spectrum offers the opportunity to study this problem from the ground. The FeXIII 1.075 um and SiX 1.431 um forbidden lines are strongly polarizable and are sufficiently bright over a large field of view (out to 1.5 Rsun). Measurements of both these lines can be paired up with the recently observed coronal HeI 1.083 um permitted line. The first data set used to test this technique was taken during the March 29, 2006 total solar eclipse and consisted of near-IR spectra covering the spectral region 0.9-1.8 um, with a field of view of 3 x 3 Rsun. The data revealed unexpectedly strong SiX emission compared to FeXIII. Using the HAO FORWARD suite of codes we produced simulated emission maps from a global HMD model for the day of the eclipse. Comparing the intensity variation of the measurements and the model we predict that SiX emission is more extended for this day that the model would suggest, further supporting the possible usefulness of SiX polarimetry. The development of this method and associated tools will be critical in interpreting the high spectral, spatial and temporal IR measurements that will be possible when the Daniel K. Inouye Solar Telescope (DKIST) is completed in a few years time. Title: A Mach-Zender Holographic Microscope for Quantifying Bacterial Motility Authors: Niraula, B.; Nadeau, J. L.; Serabyn, E.; Wallace, J. K.; Liewer, K.; Kuhn, J.; Graff, E.; Lindensmith, C. Bibcode: 2014AGUFM.P53A4004N Altcode: New microscopic techniques have revolutionized cell biology over the past two decades. However, there are still biological processes whose details elude us, especially those involving motility: e.g. feeding behavior of microorganisms in the ocean, or migration of cancer cells to form metastases. Imaging prokaryotes, which range in size from several hundred nm to a few microns, is especially challenging. An emerging technique to address these issues is Digital Holographic Microscopy (DHM). DHM is an imaging technique that uses the interference of light to record and reproduce three-dimensional magnified images of objects. This approach has several advantages over ordinary brightfield microscopy for fieldwork: a larger depth of field, hands-off operation, robustness regarding environmental conditions, and large sampling volumes with quantitative 3D records of motility behavior. Despite these promising features, real-time DHM was thought to be impractical for technological and computational reasons until recently, and there has so far been very limited application of DHM to biology. Most existing instruments are limited in performance by their particular (e.g. in-line, lens-less, phase-shifting) approach to holography. These limitations can be mitigated with an off-axis dual-path configuration. Here we describe the design and implementation of a design for a Mach-Zehnder-type holographic microscope with diffraction-limited lateral resolution, with intended applications in environmental microbiology. We have achieved sub-micron resolution and three-dimensional tracking of prokaryotic and eukaryotic test strains designed to represent different modes and speeds of microbial motility. Prokaryotes are Escherichia coli, Vibrio alginolyticus, and Bacillus subtilis. Each shows a characteristic motility pattern, as we illustrate in holographic videos in sample chambers 0.6 mm in depth. The ability to establish gradients of attractants with bacterial taxis towards the attractant is also established. The eukaryotic strains are Euglena gracilis, which demonstrates both phototaxis and geotaxis, and Paramecium micromultinucleatum. The challenges of optimizing resolution vs. field of view, and of handling the large volumes of data generated during holographic imaging, are discussed. Title: Bacterial Motility As a Biosignature: Tests at Icy Moon Analogue Sites Authors: Nadeau, J. L.; Lindensmith, C.; Deming, J. W.; Stocker, R.; Graff, E.; Serabyn, E.; Wallace, J. K.; Liewer, K.; Kuhn, J. Bibcode: 2014AGUFM.P53A4005N Altcode: Extraterrestrial life in our Solar System, if present, is almost certain to be microbial. Methods and technologies for unambiguous detection of living or extinct microorganisms are needed for life-detection missions to the Jovian and Saturnian moons, where liquid water is known to exist. Our research focuses specifically on microbial meaningful motion as a biosignature—"waving crowds" at the micron scale. Digital Holographic Microscopy (DHM) is an excellent tool for unambiguous identification of bacterial and protozoal swimming, even in the presence of turbidity, drift, and currents. The design of a holographic instrument with bacteria scale resolution was described in the previous talk. In this presentation, we will illustrate the design challenges for construction of a field instrument for extreme environments and space, and present plans for scientific investigations at analogue sites for the coming season. The challenges of creating a field instrument involve performance trade-offs, the ability to operate at extreme temperatures, and handling large volumes of data. A fully autonomous instrument without external cables or power is also desirable, and this is something that previous holographic instruments have not achieved. The primary issues for space exploration are identification of a laser and drive electronics that are qualified for the expected radiation environments of the moons around gas giant planets. Tests in Earth analogue environments will establish performance parameters as well as answer scientific questions that traditional microscopic techniques cannot. Specifically, we will visit a Greenland field site to determine whether or not microorganisms are motile within the brine-filled interior network of sea ice, and if they can be autonomously tracked using the instrument. Motility within the liquid phase of a frozen matrix has been hypothesized to explain how bacteria contribute to the biogeochemical signatures detected in ice, but observational evidence of motility in natural samples at subzero temperatures does not exist. Complementing tests for bacterial motility in ice-brines, we will also test for motility in the subzero waters directly beneath the ice, where motility has long been suspected but also never observed. Title: The Daniel K. Inouye Solar Telescope: A Project Update. Authors: Rimmele, T.; Berger, T.; McMullin, J.; Warner, M.; Casinsi, R.; Kuhn, J.; Lin, H.; Woeger, F.; Schmidt, W.; Tritschler, A.; Inouye, Daniel K.; Solar Telescope Team Bibcode: 2014amos.confE..43R Altcode: The Advanced Technology Solar Telescope will be the largest solar facility ever built. Designed and developed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the sun, this facility will support key experiments for the study of solar magnetism and its influence on the solar wind, flares, coronal mass ejections and solar irradiance variability. The 4-meter diameter facility will operate over a broad wavelength range (0.35 to 28 microns), using state-of-the-art adaptive optics systems to provide diffraction limited imaging and the ability to resolve features approximately 20 km on the Sun. Five first light instruments will be available at the start of operations. Key subsystems have been designed and fabrication is well underway, including the site construction, which began in December 2012. We provide an update on the development of the facilities both on site at the Haleakala Observatories in Maui and the development of components around the world. We present the overall construction and integration schedule leading to the start of operations in mid-2019 and touch on operations aspects. Title: Construction status of the Daniel K. Inouye Solar Telescope Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Martínez Pillet, Valentin; Berger, Thomas E.; Casini, Roberto; Craig, Simon C.; Elmore, David F.; Goodrich, Bret D.; Hegwer, Steve L.; Hubbard, Robert P.; Johansson, Erik M.; Kuhn, Jeffrey R.; Lin, Haosheng; McVeigh, William; Schmidt, Wolfgang; Shimko, Steve; Tritschler, Alexandra; Warner, Mark; Wöger, Friedrich Bibcode: 2014SPIE.9145E..25M Altcode: The Daniel K. Inouye Solar Telescope (DKIST, renamed in December 2013 from the Advanced Technology Solar Telescope) will be the largest solar facility built when it begins operations in 2019. Designed and developed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the Sun, the observatory will enable key research for the study of solar magnetism and its influence on the solar wind, flares, coronal mass ejections and solar irradiance variations. The 4-meter class facility will operate over a broad wavelength range (0.38 to 28 microns, initially 0.38 to 5 microns), using a state-of-the-art adaptive optics system to provide diffraction-limited imaging and the ability to resolve features approximately 25 km on the Sun. Five first-light instruments will be available at the start of operations: Visible Broadband Imager (VBI; National Solar Observatory), Visible SpectroPolarimeter (ViSP; NCAR High Altitude Observatory), Visible Tunable Filter (VTF; Kiepenheuer Institut für Sonnenphysik), Diffraction Limited Near InfraRed SpectroPolarimeter (DL-NIRSP; University of Hawai'i, Institute for Astronomy) and the Cryogenic Near InfraRed SpectroPolarimeter (Cryo-NIRSP; University of Hawai'i, Institute for Astronomy). As of mid-2014, the key subsystems have been designed and fabrication is well underway, including the site construction, which began in December 2012. We provide an update on the development of the facilities both on site at the Haleakalā Observatories on Maui and the development of components around the world. We present the overall construction and integration schedule leading to the handover to operations in mid 2019. In addition, we outline the evolving challenges being met by the project, spanning the full spectrum of issues covering technical, fiscal, and geographical, that are specific to this project, though with clear counterparts to other large astronomical construction projects. Title: Development and recent results from the Subaru coronagraphic extreme adaptive optics system Authors: Jovanovic, N.; Guyon, O.; Martinache, F.; Clergeon, C.; Singh, G.; Kudo, T.; Newman, K.; Kuhn, J.; Serabyn, E.; Norris, B.; Tuthill, P.; Stewart, P.; Huby, E.; Perrin, G.; Lacour, S.; Vievard, S.; Murakami, N.; Fumika, O.; Minowa, Y.; Hayano, Y.; White, J.; Lai, O.; Marchis, F.; Duchene, G.; Kotani, T.; Woillez, J. Bibcode: 2014SPIE.9147E..1QJ Altcode: The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) instrument is one of a handful of extreme adaptive optics systems set to come online in 2014. The extreme adaptive optics correction is realized by a combination of precise wavefront sensing via a non-modulated pyramid wavefront sensor and a 2000 element deformable mirror. This system has recently begun on-sky commissioning and was operated in closed loop for several minutes at a time with a loop speed of 800 Hz, on ~150 modes. Further suppression of quasi-static speckles is possible via a process called "speckle nulling" which can create a dark hole in a portion of the frame allowing for an enhancement in contrast, and has been successfully tested on-sky. In addition to the wavefront correction there are a suite of coronagraphs on board to null out the host star which include the phase induced amplitude apodization (PIAA), the vector vortex, 8 octant phase mask, 4 quadrant phase mask and shaped pupil versions which operate in the NIR (y-K bands). The PIAA and vector vortex will allow for high contrast imaging down to an angular separation of 1 λ/D to be reached; a factor of 3 closer in than other extreme AO systems. Making use of the left over visible light not used by the wavefront sensor is VAMPIRES and FIRST. These modules are based on aperture masking interferometry and allow for sub-diffraction limited imaging with moderate contrasts of ~100-1000:1. Both modules have undergone initial testing on-sky and are set to be fully commissioned by the end of 2014. Title: Looking beyond 30m-class telescopes: the Colossus project Authors: Kuhn, J. R.; Berdyugina, S. V.; Langlois, M.; Moretto, G.; Thiébaut, E.; Harlingten, C.; Halliday, D. Bibcode: 2014SPIE.9145E..1GK Altcode: The exponential growth in exoplanet studies is a powerful reason for developing very large optical systems optimized for narrow-field science. Concepts which cross the boundary between fixed aperture telescopes and interferometers, combined with technologies that decrease the system moving mass, can violate the cost and mass scaling laws that make conventional large-aperture telescopes relatively expensive. Here we describe a concept which breaks this scaling relation in a large optical/IR system called "Colossus"1. Title: L'-band AGPM vector vortex coronagraph's first light on LBTI/LMIRCam Authors: Defrère, D.; Absil, O.; Hinz, P.; Kuhn, J.; Mawet, D.; Mennesson, B.; Skemer, A.; Wallace, K.; Bailey, V.; Downey, E.; Delacroix, C.; Durney, O.; Forsberg, P.; Gomez, C.; Habraken, S.; Hoffmann, W. F.; Karlsson, M.; Kenworthy, M.; Leisenring, J.; Montoya, M.; Pueyo, L.; Skrutskie, M.; Surdej, J., Bibcode: 2014SPIE.9148E..3XD Altcode: 2014arXiv1410.6244D We present the first observations obtained with the L'-band AGPM vortex coronagraph recently installed on LBTI/LMIRCam. The AGPM (Annular Groove Phase Mask) is a vector vortex coronagraph made from diamond subwavelength gratings. It is designed to improve the sensitivity and dynamic range of high-resolution imaging at very small inner working angles, down to 0.09 arcseconds in the case of LBTI/LMIRCam in the L' band. During the first hours on sky, we observed the young A5V star HR8799 with the goal to demonstrate the AGPM performance and assess its relevance for the ongoing LBTI planet survey (LEECH). Preliminary analyses of the data reveal the four known planets clearly at high SNR and provide unprecedented sensitivity limits in the inner planetary system (down to the diffraction limit of 0.09 arcseconds). Title: The Constant Size and Shape of the Sun Authors: Bush, Rock; Emilio, Marcelo; Kuhn, Jeffrey Richard Bibcode: 2014AAS...22421833B Altcode: Over the last four years, the Helioseismic and Magnetic Imager (HMI) instrument on the Solar Dynamics Observatory spacecraft has been measuring the radius and oblateness of the Sun. The primary observations for the solar radius are full Sun images taken twice per day in the continuum wing of the 617.3 nm Fe I absorption line. The solar radius is defined as the mean distance from the center of the Sun to the inflection point of the limb darkening function. After correcting for the varying Sun-spacecraft distance and temperature variation of the optics, the measured solar radius is essentially constant over the rising phase of the solar cycle.Measurements of the solar oblateness are obtained twice per year in April and October when the spacecraft is rotated 360 degrees around the Sun-spacecraft line. HMI observations taken during these roll maneuvers allow the instrument distortion to be separated from the solar shape. There is an apparent spring to fall change which maybe due to seasonal variation of the measurements which have not been corrected. The long term trend of the solar oblateness, however, does not show a correlation with the current solar sunspot cycle. Title: Enabling Technologies for Detecting Life in the Universe: The Colossus Project Authors: Kuhn, J.; Berdyugina, S.; Halliday, D.; Harlingten, C.; Langlois, M.; Moretto, G. Bibcode: 2014ebi..conf.4.19K Altcode: An international consortium of scientists, engineers, and private interests formed two in 2012 to develope a large telescope with the capability of detecting life signatures, and potentially even Earth-like civilizations, on hundreds of nearby exoplanets. This "Colossus Telescope" departs from all currently planned large optical telescope designs in order to achieve the required coronagraphic performance, angular resolution, and flux sensitivity. As a nearly filled-aperture, highly redundant-baseline optical and IR imaging instrument, it has several advantages for studying exoplanets. This presentation introduces the instrument concept and some strategies for finding life within about 25pc of the Sun. Title: L'-band AGPM vector vortex coronagraph's first light on LBTI/LMIRCAM Authors: Defrère, D.; Absil, O.; Hinz, P.; Mawet, D.; Kuhn, J.; Mawet, D.; Mennesson, B.; Skemer, A.; Wallace, K.; Bailey, V.; Downey, E.; Delacroix, C.; Durney, O.; Forsberg, P.; Gomez, C.; Habraken, S.; Karlsson, M.; Kenworthy, M.; Leisenring, J.; Montoya, M.; Pueyo, L.; Skrutskie, M.; Surdej, J. Bibcode: 2014ebi..confP4.75D Altcode: We present the first science observations obtained with the L'-band AGPM coronagraph recently installed on LBTI/LMIRCAM. The AGPM (Annular Groove Phase Mask) is a vector vortex coronagraph made from diamond sub-wavelength gratings tuned to the L'-band. It is designed to improve the sensitivity and dynamic range of high-resolution imaging at very small inner working angles, down to 0.09 arcseconds in the case of LBTI/LMIRCAM in the L'- band.

During the first hours on sky, we observed the young A5V star HR8799 with the goal to obtain the best sensitivity/contrast ever in the inner region (<1") of the planetary system. Preliminary analyses of the data reveal the four known planets clearly at high SNR. The performance of the instrument in this mode will be presented and compared to straight imaging (without coronagraph) which is used for the ongoing LBTI planet survey (LEECH, see abstract by A. Skemer). Title: Detecting extraterrestrial life with the Colossus telescope using photosynthetic biosignatures Authors: Berdyugina, S.; Kuhn, J.; Harrington, D.; Moretto, G.; Langlois, M.; Halliday, D.; Harlingten, C. Bibcode: 2014ebi..confP4.89B Altcode: We propose to search for life on Earth-like planets in habitable zones using photosynthesis biosignatures. Many life forms on Earth process the solar light and utilize it to support their own activity and to provide a valuable energy source for other life forms. We expect therefore that photosynthesis is very likely to arise on another planet and can produce conspicuous biosignatures. We have recently identified biological polarization effects, e.g., selective light absorption or scattering by photosynthetic molecules which can be used for remote detection of extraterrestrial life. Here we present synthetic spectra and polarization of Earth-like planets with photosynthetic life and evaluate the sensitivity of the Colossus telescope for their remote detection in the solar neighborhood. Title: Submicron-AlGaN/GaN MMICs for space applications Authors: Quay, R.; Waltereit, P.; Kuhn, J.; Bruckner, P.; van Heijningen, M.; Jukkala, P.; Hirche, K.; Ambacher, O. Bibcode: 2013imsd.conf97533Q Altcode: No abstract at ADS Title: Investigating the magnetism of brown dwarfs Authors: Kuzmychov, O.; Berdyugina, S. V.; Harrington, D.; Kuhn, J. Bibcode: 2013MmSAI..84.1127K Altcode: 2013arXiv1309.4617K We model the spectra of two brown dwarfs observed with the low resolution spectropolarimeter LRIS (R ∼ 3000, Keck observatory) during several rotational phases in order to infer their magnetic properties. The spectra modeled include the intensity signal (Stokes I/I_c) as well as the polarimetric signals (Stokes Q/I_c, U/I_c and V/I_c), all coming from the 0-0 vibrational band of the CrH molecule at ≈ 8610 Å. In order to model the Stokes profiles, we solve a set of the radiative transfer equations for the CrH transitions in the presence of an external magnetic field. We present here the upper limits for the magnetic field strengths for the objects observed, based on the modeling of the intensity signal I/I_c and the signal-to-noise information only. The proper modeling of the polarimetric signals, that requires more careful data reduction, is underway. Nevertheless, our preliminary results show a hint for kG magnetic fields for both brown dwarfs, that is in a good agreement with the result obtained from the simultaneous radio, Halpha and X-Ray observations of one another radio pulsating brown dwarf. Title: Solar Dark Matter and Dark Energy: How can CryoNIRSP Help? Authors: Kuhn, J. R.; Scholl, I. F.; Mickey, D. L. Bibcode: 2012ASPC..463..207K Altcode: ATST will be the world's most expensive optical telescope ever built and provide the largest jump in our ground-based solar observing capability since Galileo. It is more than “just a solar telescope” as it will dominate the solar and stellar science landscape for many years to come. Given the telescope's ground-breaking new capabilities we should expect its initial instrumentation to have comparable revolutionary performance and to expect “discovery” science from the ATST soon after first light. The CryoNIRSP instrument is one such facility and the only explicitly coronal instrument designed to take advantage of the full ATST photometric dynamic range, from typical daytime to night-time light flux levels. This brief paper summarizes its design and capabilities. Title: Construction of the Advanced Technology Solar Telescope - A Progress Report. Authors: Rimmele, T. R.; Keil, S.; McMullin, J.; Goode, P. R.; Knoelker, M.; Kuhn, J. R.; Rosner, R.; ATST Team Bibcode: 2012IAUSS...6E.206R Altcode: The 4m Advance Technology Solar Telescope (ATST) will be the most powerful solar telescope and the world's leading ground-based resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and variability in the Sun's output. The ATST will provide high resolution and high sensitivity observations of the dynamic solar magnetic fields throughout the solar atmosphere, including the corona at infrared wavelengths. With its 4 m aperture, ATST will resolve magnetic features at their intrinsic scales. A high order adaptive optics system delivers a corrected beam to the initial set of five state-of-the-art, facility class instrumentation located in the coude laboratory facility. Photopheric and chromospheric magnetometry is part of the key mission of four of these instruments. Coronal magnetometry and spectroscopy will be performed by two of these instruments at infrared wavelengths. The ATST project has transitioned from design and development to its construction phase. Site construction is expected to begin in the first half of 2012. The project has awarded design and fabrication contracts for major telescope subsystems. A robust instrument program has been established and all instruments have passed preliminary design reviews or critical design reviews. A brief summary of the science goals and observational requirements of the ATST will be given, followed by a summary of the project status of the telescope and discussion of the approach to integrating instruments into the facility. Title: Construction of the Advanced Technology Solar Telescope Authors: Rimmele, T. R.; Keil, S.; McMullin, J.; Knölker, M.; Kuhn, J. R.; Goode, P. R.; Rosner, R.; Casini, R.; Lin, H.; Tritschler, A.; Wöger, F.; ATST Team Bibcode: 2012ASPC..463..377R Altcode: The 4m Advance Technology Solar Telescope (ATST) will be the most powerful solar telescope and the world's leading ground-based resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and variability in the Sun's output. The project has entered its construction phase. Major subsystems have been contracted. As its highest priority science driver ATST shall provide high resolution and high sensitivity observations of the dynamic solar magnetic fields throughout the solar atmosphere, including the corona at infrared wavelengths. With its 4m aperture, ATST will resolve features at 0.″03 at visible wavelengths and obtain 0.″1 resolution at the magnetically highly sensitive near infrared wavelengths. A high order adaptive optics system delivers a corrected beam to the initial set of state-of-the-art, facility class instrumentation located in the Coudé laboratory facility. The initial set of first generation instruments consists of five facility class instruments, including imagers and spectro-polarimeters. The high polarimetric sensitivity and accuracy required for measurements of the illusive solar magnetic fields place strong constraints on the polarization analysis and calibration. Development and construction of a four-meter solar telescope presents many technical challenges, including thermal control of the enclosure, telescope structure and optics and wavefront control. A brief overview of the science goals and observational requirements of the ATST will be given, followed by a summary of the design status of the telescope and its instrumentation, including design status of major subsystems, such as the telescope mount assembly, enclosure, mirror assemblies, and wavefront correction Title: Eclipse Spectropolarimetry of the ɛ Aurigae System Authors: Geise, K.; Stencel, R. E.; Manset, N.; Harrington, D.; Kuhn, J. Bibcode: 2012JAVSO..40..767G Altcode: The recent eclipse of the enigmatic binary star system, epsilon Aurigae, offered a special opportunity to explore the role of spectropolarimetry in discovery of unknown facets of the objects involved. Here we present spectropolarimetric results for H-alpha, H-beta, Ca I (422.6 nm), and K I (769.9 nm) based on more than 50 epochs of high dispersion spectra obtained with the ESPaDOnS instrument at CFHT during 2006-2012. Title: The Precise Solar Shape and Its Variability Authors: Kuhn, J. R.; Bush, R.; Emilio, M.; Scholl, I. F. Bibcode: 2012Sci...337.1638K Altcode: The precise shape of the Sun has not been convincingly determined, despite half a century of modern photoelectric observations. The expected deviation of the solar-limb shape from a perfect circle is very small, but such asphericity is sensitive to the Sun’s otherwise invisible interior conditions, as well as the solar atmosphere. We use evidence from a long-running experiment based in space to show that, when analyzed with sufficiently high spatial resolution, the Sun’s oblate shape is distinctly constant and almost completely unaffected by the solar-cycle variability seen on its surface. The solar oblateness is significantly lower than theoretical expectations by an amount that could be explained by a slower differential rotation in the outer few percent of the Sun. Title: Advanced Technology Solar Telescope Construction: Progress Report Authors: Rimmele, Thomas R.; McMullin, J.; Keil, S.; Goode, P.; Knoelker, M.; Kuhn, J.; Rosner, R.; ATST Team Bibcode: 2012AAS...22012202R Altcode: The 4m Advance Technology Solar Telescope (ATST) on Haleakala will be the most powerful solar telescope and the world’s leading ground-based resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and variability in the Sun’s output. The ATST will provide high resolution and high sensitivity observations of the dynamic solar magnetic fields throughout the solar atmosphere, including the corona at infrared wavelengths. With its 4 m aperture, ATST will resolve magnetic features at their intrinsic scales. A high order adaptive optics system delivers a corrected beam to the initial set of five state-of-the-art, facility class instrumentation located in the coude laboratory facility. Photopheric and chromospheric magnetometry is part of the key mission of four of these instruments. Coronal magnetometry and spectroscopy will be performed by two of these instruments at infrared wavelengths. The ATST project has transitioned from design and development to its construction phase. Site construction is expected to begin in April 2012. The project has awarded design and fabrication contracts for major telescope subsystems. A robust instrument program has been established and all instruments have passed preliminary design reviews or critical design reviews. A brief overview of the science goals and observational requirements of the ATST will be given, followed by a summary of the project status of the telescope and discussion of the approach to integrating instruments into the facility.

The National Science Foundation (NSF) through the National Solar Observatory (NSO) funds the ATST Project. The NSO is operated under a cooperative agreement between the Association of Universities for Research in Astronomy, Inc. (AURA) and NSF. Title: A RHESSI and SDO Campaign Measuring Latitude-dependent Limb Profiles and Oblateness of the Optical Solar Disk II Authors: Fivian, Martin; Hudson, H. S.; Lin, R. P.; Bush, R. I.; Emilio, M.; Kuhn, J. R.; Scholl, I. F. Bibcode: 2012AAS...22020511F Altcode: The SDO spacecraft conducts special roll maneuvers every 6 months. These SDO maneuvers enable its HMI instrument to obtain precise observations of the global structure of the limb. During the SDO roll on 2011 April 6 05:50-12:30 UT, we also successfully obtained RHESSI optical observations at very high cadence, 128 samples per sec for each of the three linear CCDs. A second coordinated observation with optimized parameter settings for RHESSI is planned for the time of the SDO roll maneuver in April 2012. The data from the two instruments (RHESSI/SAS and SDO/HMI), give different means for the investigation of the variation of the solar limb properties as a function of position angle (latitude). At the normal RHESSI cadence very long integrations (of order 3 months) are needed to obtain precise limb measurements, but in this case we are able to report results within the exact time frame of the SDO roll maneuver. The special RHESSI data rate was about 10,000 times larger than the standard rate and will achieve high precision in a relatively short time. We will compare these results with our earlier RHESSI observations (Fivian et al., 2008) and those obtained by Kuhn et al. (1998) and Emilio et al. (2007) with the earlier MDI roll maneuvers, and as well as with the most recent analysis of HMI data. Title: Measuring the Solar Radius from Space during the 2003 and 2006 Mercury Transits Authors: Emilio, M.; Kuhn, J. R.; Bush, R. I.; Scholl, I. F. Bibcode: 2012ApJ...750..135E Altcode: 2012arXiv1203.4898E The Michelson Doppler Imager (MDI) aboard the Solar and Heliospheric Observatory observed the transits of Mercury on 2003 May 7 and 2006 November 8. Contact times between Mercury and the solar limb have been used since the seventeenth century to derive the Sun's size but this is the first time that high-quality imagery from space, above the Earth's atmosphere, has been available. Unlike other measurements, this technique is largely independent of optical distortion. The true solar radius is still a matter of debate in the literature as measured differences of several tenths of an arcsecond (i.e., about 500 km) are apparent. This is due mainly to systematic errors from different instruments and observers since the claimed uncertainties for a single instrument are typically an order of magnitude smaller. From the MDI transit data we find the solar radius to be 960farcs12 ± 0farcs09 (696, 342 ± 65 km). This value is consistent between the transits and consistent between different MDI focus settings after accounting for systematic effects. Title: High Resolution Spectropolarimetry of the Hα Line: Obscured Stars and Absorptive Polarization Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2011ASPC..449..295H Altcode: The near-star environment around obscured stars is very dynamic. Many classes of stars show evidence for winds, disks, inflows and outflows with many phenomena occurring simultaneously. These processes are involved in stellar evolution, star and planet formation, and influence the formation and habitability of planets around host stars. Even for the nearest stars, this region will not be imaged even after the completion of the next generation of telescopes. Other methods for measuring the physical properties of circumstellar material must be developed. The polarization of light across spectral lines is a signature that contains information about the circumstellar material on these small spatial scales. We used the HiVIS (R=13 000 to 50 000) and ESPaDOnS (R=68 000) spectropolarimeters to monitor several classes of stars on over a hundred nights of observing from 2004-2008. In 10/30 classical Be stars, the traditional broad depolarization morphology is reproduced, but with some additional absorptive effects in 4 of these 10 stars. In Herbig Ae/Be stars roughly 2/3 of the stars (14/20) with strong absorptive components (either central or blue-shifted) showed clear spectropolarimetric signatures typically centered on absorptive components of the spectral lines. They were typically 0.3% to 2% with some signatures being variable in time. Post-AGB and RV Tau type evolved stars showed very strong absorptive polarimetric effects (5/6 PAGB and 4/4 RV Tau) very similar to the Herbig Ae/Be stars. These observations were inconsistent with the traditional scattering models and inspired the development of a new explanation of the observed polarization. This new model, based on optical-pumping, has the potential to provide direct measurements of the circumstellar gas properties. Title: Does the sun change its shape? Authors: Kuhn, J. R.; Bush, R. I.; Emilio, M.; Scholl, I. Bibcode: 2011sdmi.confE..39K Altcode: Its not easy to change the radius or the shape of the Sun. It must come with a large energy cost and will be difficult to disentangle from the complicated physics at the boundary between the radiatively opaque and transparent solar atmosphere. HMI offers great advantages for measuring the limb physics which we're using to look for solar cycle variations that could be clues to how the interior changes. This talk will update the ongoing effort to understand the solar limb better. Title: Deriving Telescope Mueller Matrices Using Daytime Sky Polarization Observations Authors: Harrington, David M.; Kuhn, J. R.; Hall, Shannon Bibcode: 2011PASP..123..799H Altcode: 2011arXiv1105.2615H Telescopes often modify the input polarization of a source so that the measured circular or linear output state of the optical signal can be significantly different from the input. This mixing, or polarization “cross talk,” is defined by the optical system Mueller matrix. We describe an efficient method here for recovering the input polarization state of the light and the full 4 × 4 Mueller matrix of the telescope with an accuracy of a few percent without external masks or telescope hardware modification. Observations of the bright, highly polarized daytime sky using the Haleakala 3.7 m AEOS telescope and a coudé spectropolarimeter demonstrate the technique. Title: A RHESSI And SDO Campaign Measuring Latitude-dependent Limb ProfilesAnd Oblateness Of The Optical Solar Disk Authors: Fivian, Martin; Hudson, H. S.; Lin, R. P.; Bush, R. I.; Emilio, M.; Kuhn, J. R.; Scholl, I. F. Bibcode: 2011SPD....42.1706F Altcode: 2011BAAS..43S.1706F The SDO spacecraft conducted a special roll maneuver, 2011 April 6 05:50-12:30 UT, to enable its HMI instrument to obtain precise observations of the global structure of the limb. Similar maneuvers had been carried out with SOHO for MDI in the past. On this occasion we also successfully obtained RHESSI optical observations at very high cadence, 128 samples per sec for each of the three linear CCDs. The data from the two instrument (RHESSI/SAS and SDO/HMI), give different means for the investigation of the variation of the solar limb properties as a function of position angle (latitude). At the normal RHESSI cadence very long integrations (of order 3 months) are needed to obtain precise limb measurements, but in this case we expect to be able to report results within the exact time frame of the SDO roll maneuver. The special RHESSI data rate was about 10,000 times larger than the standard rate and will achieve high precision in a relatively short time. We will compare these results with our earlier RHESSI observations (Fivian et al., 2008) and those obtained by Kuhn et al. (1998) and Emilio et al. (2007) with the earlier MDI roll maneuvers. Title: Extreme Limb Polarization Measurement From HMI: A Progress Report Authors: Scholl, I. F.; Kuhn, J. R.; Bush, R. I.; Emilio, M. Bibcode: 2011ASPC..437..201S Altcode: We have obtained the first direct measurement of the continuum polarization near the extreme limb using the Helioseismic Imager (HMI) on board the Solar Dynamics Observatory (SDO). The polarization is small (much less than 1%) but easily distinguished from statistical and systematic noise sources. These measurements differ from previous attempts to measure small continuum polarization that depended on a model of line polarization to infer the continuum (cf. Stenflo 2005) polarization. Title: Using Absorptive Linear Polarization Spectroscopy to Understand Imbedded Stars Authors: Kuhn, J. R.; Geiss, B.; Harrington, D. M. Bibcode: 2011ASPC..437..245K Altcode: 2010arXiv1010.0705K Sensitive measurements of the linearly polarized spectra of stars can be used to deduce geometric properties of their otherwise unresolved circumstellar environments. This paper describes some of the evidence for optical pumping and absorptive linear polarization and explores some interesting applications of linear spectropolarimetry for obtaining spatial information from imbedded stars. Title: Solar Polarization Workshop 6 Authors: Kuhn, J. R.; Harrington, D. M.; Lin, H.; Berdyugina, S. V.; Trujillo-Bueno, J.; Keil, S. L.; Rimmele, T. Bibcode: 2011ASPC..437.....K Altcode: No abstract at ADS Title: Precision and Resolution in Stellar Spectropolarimetry Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2011ASPC..437..257H Altcode: 2010arXiv1010.0704H Stellar spectropolarimetry is a relatively new remote sensing tool for exploring stellar atmospheres and circumstellar environments. We present the results of our HiVIS survey and a multi-wavelength ESPaDOnS follow-up campaign showing detectable linear polarization signatures in many lines for most obscured stars. This survey shows polarization at and below 0.1% across many lines are common in stars with often much larger Hα signatures. These smaller signatures are near the limit of typical systematic errors in most night-time spectropolarimeters. In an effort to increase our precision and efficiency for detecting small signals we designed and implemented the new HiVIS bi-directionally clocked detector synchronized with the new liquid-crystal polarimeter package. We can now record multiple independent polarized spectra in a single exposure on identical pixels and have demonstrated 10-4 relative polarimetric precision. The new detector allows for the movement of charge on the device to be synchronized with phase changes in the liquid-crystal variable retarders at rates of > 5Hz. It also allows for more efficient observing on bright targets by effectively increasing the pixel well depth. With the new detector, low and high resolution modes and polarization calibrations for the instrument and telescope, we substantially reduce limitations to the precision and accuracy of this new spectropolarimetric tool. Title: The Search for Molecular Hydrogen in the IR Second Solar Spectrum Authors: White, Amanda; Kuhn, J. R. Bibcode: 2011AAS...21743602W Altcode: 2011BAAS...4343602W Molecular hydrogen in sunspots should be a dominant molecular species and an important factor in spot dynamics. The rotational and vibrational transitions of molecular hydrogen are extremely weak in comparison to the overall intensity spectrum of the sun making the molecule difficult to observe. Molecular lines, however, are prominent in the linearly polarized spectrum of the sun, also called the Second Solar Spectrum. Using the Scatter-free Observatory for Limb Active Regions and Coronae (SOLAR-C) located on the summit of Haleakala and a spectropolarimeter, we have observed the linear polarized spectrum of the sun near the 2.128 micron line of molecular hydrogen and begun to catalog the second solar spectrum in the IR.

This work was conducted as part of a Research Experience for Undergraduates (REU) position at the University of Hawai'i's Institute for Astronomy and funded by the NSF. Title: Properties of the Diffuse Neutral Helium in the Inner Heliosphere Authors: Moise, E.; Raymond, J.; Kuhn, J. R. Bibcode: 2010ApJ...722.1411M Altcode: Sensitive SOLARC imaging spectropolarimetric observations from Haleakala reveal a diffuse coronal surface brightness in the He I 1083 nm line. A series of observations suggests that this signal originates from an "inner source" of neutral helium atoms in the solar corona. Here, we explore the possibility that this cold coronal component originates from helium ions that are neutralized by the near-Sun dust and subsequently excited to the metastable 1s2s 3 S state, which then scatters photons from the solar disk. This picture suggests a deficit of coronal dust inside about 2-4 R sun in order to account for both the flat radial brightness distribution and the small velocity line width of the observations. We find a strong correlation between the polarized He brightness and coronal white light brightness that supports the argument that electronic collisional excitation of the metastable helium triplet level is responsible for our polarization signal. Title: The Lyot Project Direct Imaging Survey of Substellar Companions: Statistical Analysis and Information from Nondetections Authors: Leconte, Jérémy; Soummer, Rémi; Hinkley, Sasha; Oppenheimer, Ben R.; Sivaramakrishnan, Anand; Brenner, Douglas; Kuhn, Jeffrey; Lloyd, James P.; Perrin, Marshall D.; Makidon, Russell; Roberts, Lewis C., Jr.; Graham, James R.; Simon, Michal; Brown, Robert A.; Zimmerman, Neil; Chabrier, Gilles; Baraffe, Isabelle Bibcode: 2010ApJ...716.1551L Altcode: 2010arXiv1006.3409L The Lyot project used an optimized Lyot coronagraph with extreme adaptive optics at the 3.63 m Advanced Electro-Optical System telescope to observe 86 stars from 2004 to 2007. In this paper, we give an overview of the survey results and a statistical analysis of the observed nondetections around 58 of our targets to place constraints on the population of substellar companions to nearby stars. The observations did not detect any companion in the substellar regime. Since null results can be as important as detections, we analyzed each observation to determine the characteristics of the companions that can be ruled out. For this purpose, we use a Monte Carlo approach to produce artificial companions and determine their detectability by comparison with the sensitivity curve for each star. All the non-detection results are combined using a Bayesian approach and we provide upper limits on the population of giant exoplanets and brown dwarfs for this sample of stars. Our nondetections confirm the rarity of brown dwarfs around solar-like stars and we constrain the frequency of massive substellar companions (M>40 M J) at orbital separation between and 10 and 50 AU to be lsim20%. Title: On the Constancy of the Solar Radius. III. Authors: Bush, R. I.; Emilio, M.; Kuhn, J. R. Bibcode: 2010ApJ...716.1381B Altcode: The Michelson Doppler Imager on board the Solar and Heliospheric Observatory satellite has operated for over a sunspot cycle. This instrument is now relatively well understood and provides a nearly continuous record of the solar radius in combination with previously developed algorithms. Because these data are obtained from above Earth's atmosphere, they are uniquely sensitive to possible long-term changes of the Sun's size. We report here on the first homogeneous, highly precise, and complete solar-cycle measurement of the Sun's radius variability. Our results show that any intrinsic changes in the solar radius that are synchronous with the sunspot cycle must be smaller than 23 mas peak to peak. In addition, we find that the average solar radius must not be changing (on average) by more than 1.2 mas yr-1. If ground- and space-based measurements are both correct, the pervasive difference between the constancy of the solar radius seen from space and the apparent ground-based solar astrometric variability can only be accounted for by long-term changes in the terrestrial atmosphere. Title: Achromatizing a Liquid-Crystal Spectropolarimeter: Retardance vs. Stokes-Based Calibration of HiVIS Authors: Harrington, D. M.; Kuhn, J. R.; Sennhauser, C.; Messersmith, E. J.; Thornton, R. J. Bibcode: 2010PASP..122..420H Altcode: 2010arXiv1002.1409H Astronomical spectropolarimeters can be subject to many sources of systematic error that limit the precision and accuracy of the instrument. We present a calibration method for observing high-resolution polarized spectra using chromatic liquid-crystal variable retarders (LCVRs). These LCVRs allow for polarimetric modulation of the incident light without any moving optics at frequencies ≥10 Hz. We demonstrate a calibration method using pure Stokes input states that enables an achromatization of the system. This Stokes-based deprojection method reproduces input polarization even though highly chromatic instrument effects exist. This process is first demonstrated in a laboratory spectropolarimeter where we characterize the LCVRs and show example deprojections. The process is then implemented on the newly upgraded HiVIS spectropolarimeter on the 3.67 m Advanced Electro-Optical System (AEOS) telescope. The HiVIS spectropolarimeter has also been expanded to include broadband full-Stokes spectropolarimetry using achromatic wave plates in addition to the tunable full-Stokes polarimetric mode using LCVRs. These two new polarimetric modes in combination with a new polarimetric calibration unit provide a much more sensitive polarimetric package with greatly reduced systematic error. Title: FIRS: a new instrument for photospheric and chromospheric studies at the DST. Authors: Jaeggli, S. A.; Lin, H.; Mickey, D. L.; Kuhn, J. R.; Hegwer, S. L.; Rimmele, T. R.; Penn, M. J. Bibcode: 2010MmSAI..81..763J Altcode: The simultaneous observation of select spectral lines at optical and infrared wavelengths allows for the determination of the magnetic field at several photospheric and chromospheric heights and thus the 3D magnetic field gradient in the solar atmosphere. The Facility Infrared Spectropolarimeter (FIRS) is a newly completed, multi-slit, dual-beam spectropolarimeter installed at the Dunn Solar Telescope (DST) at Sacramento Peak (NSO/SP). Separate optics and polarimeters simultaneously observe two band-passes at visible and infrared wavelengths with a choice of two modes: the Fe I 6302 Å and 15648 Å lines in the photosphere; or the Fe I 6302 Å and He I 10830 Å line in the photosphere and high chromosphere, respectively. FIRS can also operate simultaneously with a white light camera, G-band imager, and the Interferometric Bi-dimensional Spectrometer (IBIS) observing the mid-chromospheric Ca II 8542 Å line. The instrument uses four parallel slits to sample four slices of the solar surface simultaneously to achieve fast, diffraction-limited precision imaging spectropolarimetry, enabling the study of MHD phenomena with short dynamic time scales. Title: The Near-Star Environment: Spectropolarimetry of Herbig Ae/Be Stars Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2009ASPC..420...77H Altcode: 2007arXiv0711.2604H The near-star environment around young stars is very dynamic with winds, disks, and outflows. These processes are involved in star and planet formation, and influence the formation and habitability of planets around host stars. Even for the closest young stars, this will not be imaged even after the completion of the next generation of telescopes decades from now and other proxies must be used. The polarization of light across individual spectral lines is such a proxy that contains information about the geometry and density of circumstellar material on these small spatial scales. We have recently built a high-resolution spectropolarimeter (R 13000 to 50000) for the HiVIS spectrograph on the 3.67m AEOS telescope. We used this instrument to monitor several young intermediate-mass stars over many nights. These observations show clear spectropolarimetric signatures typically centered on absorptive components of the spectral lines, with some signatures variable in time. The survey also confirms the large spectroscopic variability in these stars on timescales of minutes to months, and shows the dynamic bullets and streamers in the stellar winds. These observations were largely inconsistent with the traditional scattering models and inspired the development of a new explanation of their polarization, based on optical-pumping, that has the potential to provide direct measurements of the circumstellar gas properties. Title: Line-profile Variability from Tidal Flows in Alpha Virginis (Spica) Authors: Harrington, David; Koenigsberger, Gloria; Moreno, Edmundo; Kuhn, Jeffrey Bibcode: 2009ApJ...704..813H Altcode: 2009arXiv0908.3336H We present the results of high precision, high-resolution (R ~ 68,000) optical observations of the short-period (4 days) eccentric binary system Alpha Virginis (Spica) showing the photospheric line-profile variability that in this system can be attributed to non-radial pulsations driven by tidal effects. Although scant in orbital-phase coverage, the data provide signal-to-noise ratio > 2000 line profiles at full spectral resolution in the wavelength range Δλ4000-8500 Å, allowing a detailed study of the night-to-night variability as well as changes that occur on ~2 hr timescale. Using an ab initio theoretical calculation, we show that the line-profile variability can arise as a natural consequence of surface flows that are induced by the tidal interaction. Title: New Solar System Researches expected by a New Telescope Project at Mt. Haleakala, Hawaii Authors: Kagitani, Masato; Okano, S.; Kasaba, Y.; Kuhn, J.; Berdyugina, S. Bibcode: 2009DPS....41.4509K Altcode: We Tohoku University starts the project for the new ground-based telescope dedicated to planets and exoplanets, in collaboration with the Institute for Astronomy of University of Hawaii(IfA/UH) and ETH Zurich.

The summit of Mt. Haleakala in Maui, Hawaii is one of the best sites with clear skies, good seeing, and low humidity conditions as well as good accessibility despite its high altitude (elv. 3,000m). Haleakala High Altitude Observatory is operated by IfA/UH, and we have been making observation of planets there since 2000.

Currently, our observation facility consists of a 40cm telescope. We have been making observations of faint atmospheric and plasma features around bright planets, Io plasma torus, Mercury and Lunar sodium tail, and so on. Atmospheric escapes from Mars and Venus, the exoplanets close to mother stars are also possible future important topics. When we try to observe those faint emissions surrounding the bright objects, intense scattered light causes a serious problem. The new telescope shall avoid the diffraction due to a spider structure that holds a secondary mirror and to minimize the scattered light from mirror surfaces as far as possible. Such telescope with a wide dynamic range dedicated to planetary and exoplanetary sciences does not exist yet.

The project, called PLANETS (Poralized Light from Atmospheres of Nearby Extra Terrestrial Planets), develops a new telescope (tentatively named as JHET; Japan Hawaii Europe Telescope) which consists of an off-axis primary mirror with a diameter of 1.8m, and Gregorian optics on an equatorial mount. State-of-art adaptive optics and masking technologies will also be adopted to eliminate the scattering light. This telescope will enables us to do spectro-polarimetric observations and faint plasma and atmospheres around the bright bodies.

We will introduce the progress of our ground-based observations and the future plan involving the wide area of the international communities. Title: Speckle Suppression Through Dual Imaging Polarimetry, and a Ground-based Image of the HR 4796A Circumstellar Disk Authors: Hinkley, Sasha; Oppenheimer, Ben R.; Soummer, Rémi; Brenner, Douglas; Graham, James R.; Perrin, Marshall D.; Sivaramakrishnan, Anand; Lloyd, James P.; Roberts, Lewis C., Jr.; Kuhn, Jeffrey Bibcode: 2009ApJ...701..804H Altcode: 2009arXiv0906.3010H We demonstrate the versatility of a dual imaging polarimeter working in tandem with a Lyot coronagraph and adaptive optics to suppress the highly static speckle noise pattern—the greatest hindrance to ground-based direct imaging of planets and disks around nearby stars. Using a double difference technique with the polarimetric data, we quantify the level of speckle suppression, and hence improved sensitivity, by placing an ensemble of artificial faint companions into real data, with given total brightness and polarization. For highly polarized sources within 0farcs5, we show that we achieve 3 to 4 mag greater sensitivity through polarimetric speckle suppression than simply using a coronagraph coupled to a high-order adaptive optics system. Using such a polarimeter with a classical Lyot coronagraph at the 3.63 m Advanced Electro-Optical System telescope, we have obtained a 6.5σ detection in the H band of the 76 AU diameter circumstellar debris disk around the star HR 4796A. Our data represent the first definitive ground-based near-IR polarimetric image of the HR 4796A debris disk and clearly show the two outer ansae of the disk, evident in Hubble Space Telescope NICMOS/STIS imaging. Comparing our peak linearly polarized flux with the total intensity in the lobes as observed by NICMOS, we derive a lower limit to the fractional linear polarization of >29% caused by dust grains in the disk. In addition, we fit simple morphological models of optically thin disks to our data allowing us to constrain the dust disk scale height (2.5+5.0 -1.3 AU) and scattering asymmetry parameter (g = langcos θrang = 0.20+.07 -.10). These values are consistent with several lines of evidence suggesting that the HR 4796A disk is dominated by a micron-sized dust population, and are indeed typical of disks in transition between those surrounding the Herbig Ae stars to those associated with Vega-like stars. Title: Ubiquitous Hα-Polarized Line Profiles: Absorptive Spectropolarimetric Effects and Temporal Variability in Post-AGB, Herbig Ae/Be, and Other Stellar Types Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2009ApJ...695..238H Altcode: 2008arXiv0812.2598H We show here that the absorptive Hα polarized line profile previously seen in many Herbig Ae/Be (HAeBe) stars is a nearly ubiquitous feature of other types of embedded or obscured stars. This characteristic 1% linear polarization variation across the absorptive part of the Hα line is seen in post-AGB stars as well as RV Tau, δ Scuti, and other types. Each of these stars shows evidence of obscuration by intervening circumstellar hydrogen gas and the polarization effect is in the absorptive component, consistent with an optical pumping model. We present ESPaDOnS spectropolarimetric observations of nine post-AGB and RV Tau types in addition to many multi-epoch HiVIS observations of these targets. We find significant polarization changes across the Hα line in 8/9 stars with polarization amplitudes of 0.5% to over 3% (5/6 post-AGB and 3/3 RV Tau). In all but one of these, the polarization change is dominated by the absorptive component of the line profile. There is no evidence that subclasses of obscured stars showing stellar pulsations (RV Tau for post-AGB stars and δ Scuti for Herbig Ae/Be stars) show significant spectropolarimetric differences from the main class. Significant temporal variability is evident from both HiVIS and ESPaDOnS data for several stars presented here: 89 Her, AC Her, SS Lep, MWC 120, AB Aurigae, and HD144668. The morphologies and temporal variability are comparable to existing large samples of Herbig Ae/Be and Be type stars. Since post-AGB stars have circumstellar gas that is very different from Be stars, we discuss these observations in the context of their differing environments. Title: Spectropolarimetric Observations of Herbig Ae/Be Stars. II. Comparison of Spectropolarimetric Surveys: Haebe, Be and Other Emission-Line Stars Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2009ApJS..180..138H Altcode: 2008arXiv0809.3849H The polarization of light across individual spectral lines contains information about the circumstellar environment on very small spatial scales. We have obtained a large number of high-precision, high-resolution spectropolarimetric observations of Herbig Ae/Be, Classical Be and other emission-line stars collected on 117 nights of observations with the Hi-Resolution Visible spectropolarimeter at a resolution of R = 13, 000 on the 3.67 m Advanced Electro-Optical System telescope. We also have many observations from the ESPaDOnS spectropolarimeter at a resolution of R = 68, 000 on the 3.6 m Canada-France-Hawaii Telescope. In roughly ~2/3 of the so-called "windy" or "disky" Herbig Ae/Be stars, the detected Hα linear polarization varies from our typical detection threshold near 0.1% to over 2%. In all but one HAe/Be star, the detected polarization effect is not coincident with the Hα emission peak but is detected in and around the obvious absorptive part of the line profile. The qu-loops are dominated by the polarization in this absorptive region. In several stars, the polarization varies in time mostly in the absorptive component and is not necessarily tied to corresponding variations in intensity. This is a new result not seen at lower resolution. In the Be and emission-line stars, ten out of a sample of 30 show a typical broad depolarization effect but four of these ten show weaker effects only visible at high resolution. Another five of 30 show smaller amplitude, more complex signatures. Six stars of alternate classification showed large amplitude (1%-3%) absorptive polarization effects. These detections are largely inconsistent with the traditional disk-scattering and depolarization models. Title: Spectropolarimetry of the Deep Impact Target Comet 9P/Tempel 1 with HiVIS Authors: Harrington, D. M.; Meech, K. J.; Kolokolova, L.; Kuhn, J. R.; Whitman, K. Bibcode: 2009diwo.conf..155H Altcode: 2007astro.ph..3335H Spectropolarimetry of the Deep Impact target, comet 9P/ Tempel 1, was performed during the impact event on July 4th, 2005 with the HiVIS Spectropolarimeter and the AEOS 3.67-m telescope on Haleakala, Maui. We observed atypical polarization spectra that changed significantly in the few hours after the impact. The polarization is sensitive to the geometry, size and composition of the scattering particles. Our first measurement, beginning 8 minutes after impact and centered at 6:30UT, showed a polarization of 4% at 650 nm falling to 3% at 950 nm. The next observation, centered an hour later, showed a polarization of 7% at 650 nm falling to 2% at 950nm. This corresponds to a spectropolarimetric gradient, or slope, of -0.9% per 1000Å 40 minutes after impact, decreasing to a slope of -2.3% per 1000Å 75 minutes after impact. Both are atypical blue polarization slopes. The polarization values of 4 and 7% at 650 nm are typical for comets at this scattering angle, whereas the low polarization of 2 and 3% at 950 nm is not. This, combined with the IR spectroscopy performed by a number of observers during the event, suggests an increase in size, number, and crystallinity of the individual silicate particles (monomers) that are a constituant of the dust particles (aggregates) in the ejecta. Title: Spectropolarimetric Observations of the Helium 10830 Å Line: A Search for the Signature of Optical Pumping Authors: Goldbaum, Nathan Jonathan; Kuhn, J. R. Bibcode: 2009AAS...21349204G Altcode: 2009BAAS...41..472G In order to characterize the center-to-limb and latitudinal variation of the polarization of the He I 10830 Å line we observed the limb of the sun at several position angles using the Scatter-Free Observatory for Limb Active Regions and Coronae (SOLARC), an imaging spectropolarimeter located on the summit of Haleakala, Maui. The data was reduced and analyzed to produce profiles of the magnitude of the Stokes Q/I and U/I signals as a function of latitude and solar radius. Modeling of the observed profiles should allow us to detect whether the observed linear polarization signal is due entirely to scattering polarization or possibly includes absorptively polarized light transmitted through an optically pumped gas. This work was conducted as part of a Research Experience for Undergraduates (REU) position at the University of Hawaii's Institute for Astronomy and funded by the NSF Title: Measuring Electron Temperature and Flow Speed using Thomson Scattered Emission from the Corona Observed with the Solar-C Coronagraph Authors: Davila, J. M.; Reginald, N.; St. Cyr, O. C.; Kuhn, J. Bibcode: 2008AGUFMSH11A..05D Altcode: A method for measuring the density, temperature, and velocity of coronal electrons was proposed by Reginald and Davila (2000) based on an extension the Thomson scattering theory of Cram (1976) to include flows. In this method the electron density is measured in the usual way (e.g. in LASCO or MkIV coronagraph images) by observing the total coronal intensity. The electron temperature and flow speed are obtained by obtaining ratios of spectral intensity measured in 50 A passbands or by fitting a portion of the spectrum to coronal models. Observations during the total solar eclipse of 2000 near Lusaka, Zambia demonstrated the feasibility of the method (Reginald et. al., 2003) using the first generation Multi-Aperture Coronal Spectrometer (MACS-1) instrument, and with the second-generation MACS in Libya in 2006 reasonable temperature and flow speeds were obtained. In this paper we continue this work by reporting on the results of new observations taken from the ground at the Solar-C coronagraph. Although eclipse measurements provide the best observation (nearly free of scattered light but with limited duration), the Solar-C coronagraph observations allowed several days of nearly continuous observation from which the repeatability and accuracy of the measurement could be determined. To deal with the increased atmospheric scatter, observations at Solar-C were done in polarized brightness (pB). Results will be reported in this talk. Title: Electroexcitation of the Roper resonance for 1.7<Q2<4.5GeV2 in e→p→enπ+ Authors: Aznauryan, I. G.; Burkert, V. D.; Kim, W.; Park, K.; Adams, G.; Amaryan, M. J.; Ambrozewicz, P.; Anghinolfi, M.; Asryan, G.; Avakian, H.; Bagdasaryan, H.; Baillie, N.; Ball, J. P.; Baltzell, N. A.; Barrow, S.; Batourine, V.; Battaglieri, M.; Bedlinskiy, I.; Bektasoglu, M.; Bellis, M.; Benmouna, N.; Berman, B. L.; Biselli, A. S.; Blaszczyk, L.; Bonner, B. E.; Bookwalter, C.; Bouchigny, S.; Boiarinov, S.; Bradford, R.; Branford, D.; Briscoe, W. J.; Brooks, W. K.; Bültmann, S.; Butuceanu, C.; Calarco, J. R.; Careccia, S. L.; Carman, D. S.; Casey, L.; Cazes, A.; Chen, S.; Cheng, L.; Cole, P. L.; Collins, P.; Coltharp, P.; Cords, D.; Corvisiero, P.; Crabb, D.; Crede, V.; Cummings, J. P.; Dale, D.; Dashyan, N.; de Masi, R.; de Vita, R.; de Sanctis, E.; Degtyarenko, P. V.; Denizli, H.; Dennis, L.; Deur, A.; Dhamija, S.; Dharmawardane, K. V.; Dhuga, K. S.; Dickson, R.; Djalali, C.; Dodge, G. E.; Donnelly, J.; Doughty, D.; Dugger, M.; Dytman, S.; Dzyubak, O. P.; Egiyan, H.; Egiyan, K. S.; Fassi, L. El; Elouadrhiri, L.; Eugenio, P.; Fatemi, R.; Fedotov, G.; Feldman, G.; Feuerbach, R. J.; Forest, T. A.; Fradi, A.; Funsten, H.; Gabrielyan, M. Y.; Garçon, M.; Gavalian, G.; Gevorgyan, N.; Gilfoyle, G. P.; Giovanetti, K. L.; Girod, F. X.; Goetz, J. T.; Gohn, W.; Golovatch, E.; Gonenc, A.; Gordon, C. I. O.; Gothe, R. W.; Graham, L.; Griffioen, K. A.; Guidal, M.; Guillo, M.; Guler, N.; Guo, L.; Gyurjyan, V.; Hadjidakis, C.; Hafidi, K.; Hafnaoui, K.; Hakobyan, H.; Hakobyan, R. S.; Hanretty, C.; Hardie, J.; Hassall, N.; Heddle, D.; Hersman, F. W.; Hicks, K.; Hleiqawi, I.; Holtrop, M.; Hyde, C. E.; Ilieva, Y.; Ireland, D. G.; Ishkhanov, B. S.; Isupov, E. L.; Ito, M. M.; Jenkins, D.; Jo, H. S.; Johnstone, J. R.; Joo, K.; Juengst, H. G.; Kalantarians, N.; Keller, D.; Kellie, J. D.; Khandaker, M.; Kim, K. Y.; Klein, A.; Klein, F. J.; Klimenko, A. V.; Kossov, M.; Krahn, Z.; Kramer, L. H.; Kubarovsky, V.; Kuhn, J.; Kuhn, S. E.; Kuleshov, S. V.; Kuznetsov, V.; Lachniet, J.; Laget, J. M.; Langheinrich, J.; Lawrence, D.; Lee, T.; Li, Ji; Lima, A. C. S.; Livingston, K.; Lu, H. Y.; Lukashin, K.; MacCormick, M.; Markov, N.; Mattione, P.; McAleer, S.; McKinnon, B.; McNabb, J. W. C.; Mecking, B. A.; Mehrabyan, S.; Melone, J. J.; Mestayer, M. D.; Meyer, C. A.; Mibe, T.; Mikhailov, K.; Minehart, R.; Mirazita, M.; Miskimen, R.; Mokeev, V.; Morand, L.; Moreno, B.; Moriya, K.; Morrow, S. A.; Moteabbed, M.; Mueller, J.; Munevar, E.; Mutchler, G. S.; Nadel-Turonski, P.; Nasseripour, R.; Niccolai, S.; Niculescu, G.; Niculescu, I.; Niczyporuk, B. B.; Niroula, M. R.; Niyazov, R. A.; Nozar, M.; O'Rielly, G. V.; Osipenko, M.; Ostrovidov, A. I.; Park, S.; Pasyuk, E.; Paterson, C.; Pereira, S. Anefalos; Philips, S. A.; Pierce, J.; Pivnyuk, N.; Pocanic, D.; Pogorelko, O.; Polli, E.; Popa, I.; Pozdniakov, S.; Preedom, B. M.; Price, J. W.; Prok, Y.; Protopopescu, D.; Qin, L. M.; Raue, B. A.; Riccardi, G.; Ricco, G.; Ripani, M.; Ritchie, B. G.; Rosner, G.; Rossi, P.; Rowntree, D.; Rubin, P. D.; Sabatié, F.; Saini, M. S.; Salamanca, J.; Salgado, C.; Santoro, J. P.; Sapunenko, V.; Schott, D.; Schumacher, R. A.; Serov, V. S.; Sharabian, Y. G.; Sharov, D.; Shaw, J.; Shvedunov, N. V.; Skabelin, A. V.; Smith, E. S.; Smith, L. C.; Sober, D. I.; Sokhan, D.; Stavinsky, A.; Stepanyan, S. S.; Stepanyan, S.; Stokes, B. E.; Stoler, P.; Strakovsky, I. I.; Strauch, S.; Suleiman, R.; Taiuti, M.; Takeuchi, T.; Tedeschi, D. J.; Tkabladze, A.; Tkachenko, S.; Todor, L.; Tur, C.; Ungaro, M.; Vineyard, M. F.; Vlassov, A. V.; Watts, D. P.; Weinstein, L. B.; Weygand, D. P.; Williams, M.; Wolin, E.; Wood, M. H.; Yegneswaran, A.; Yun, J.; Yurov, M.; Zana, L.; Zhang, B.; Zhang, J.; Zhao, B.; Zhao, Z. W. Bibcode: 2008PhRvC..78d5209A Altcode: 2008arXiv0804.0447A The helicity amplitudes of the electroexcitation of the Roper resonance are extracted for 1.7<Q2<4.5GeV2 from recent high precision JLab-CLAS cross section and longitudinally polarized beam asymmetry data for π+ electroproduction on protons at W=1.15-1.69 GeV. The analysis is made using two approaches, dispersion relations and a unitary isobar model, which give consistent Q2 behavior of the helicity amplitudes for the γ*p→N(1440)P11 transition. It is found that the transverse helicity amplitude A1/2, which is large and negative at Q2=0, becomes large and positive at Q2≃2GeV2, and then drops slowly with Q2. The longitudinal helicity amplitude S1/2, which was previously found from CLAS e→p→epπ0,enπ+ data to be large and positive at Q2=0.4,0.65GeV2, drops with Q2. Available model predictions for γ*p→N(1440)P11 allow us to conclude that these results provide strong evidence in favor of N(1440)P11 as a first radial excitation of the 3q ground state. The results of the present paper also confirm the conclusion of our previous analysis for Q2<1 GeV2 that the presentation of N(1440)P11 as a qG3 hybrid state is ruled out. Title: High Resolution Spectropolarimetry of the H-alpha Line: Obscured Stars and Absorptive Polarization Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2008arXiv0809.3297H Altcode: The near-star environment around obscured stars is very dynamic. Many classes of stars show evidence for winds, disks, inflows and outflows with many phenomena occurring simultaneously. These processes are involved in stellar evolution, star and planet formation, and influence the formation and habitability of planets around host stars. Even for the nearest stars, this region will not be imaged even after the completion of the next generation of telescopes. Other methods for measuring the physical properties of circumstellar material must be developed. The polarization of light across spectral lines is a signature that contains information about the circumstellar material on these small spatial scales. We used the HiVIS (R=13000 to 50000) and ESPaDOnS (R=68000) spectropolarimeters to monitor several classes of stars on over a hundred nights of observing from 2004-2008. In 10/30 classical Be stars, the traditional broad depolarization morphology is reproduced, but with some additional absorptive effects in 4 of these 10 stars. In Herbig Ae/Be stars roughly 2/3 of the stars (14/20) with strong absorptive components (either central or blue-shifted) showed clear spectropolarimetric signatures typically centered on absorptive components of the spectral lines. They were typically 0.3% to 2% with some signatures being variable in time. Post-AGB and RV-Tau type evolved stars showed very strong absorptive polarimetric effects (5/6 PAGB and 4/4 RVTau) very similar to the Herbig Ae/Be stars. These observations were inconsistent with the traditional scattering models and inspired the development of a new explanation of the observed polarization. This new model, based on optical-pumping, has the potential to provide direct measurements of the circumstellar gas properties. Title: Inner Source Diffuse Helium Observations Authors: Moise, E.; Kuhn, J.; Raymond, J.; Armstrong, J. D. Bibcode: 2008ESPM...12.2.88M Altcode: Sensitive SOLARC imagining spectropolarimetric observations from Haleakala reveal a diffuse coronal surface brightness in the He I 1083nm line. A series of observations obtained during the last two years suggests that this signal originates from an "inner source" of neutral helium atoms in the solar corona. We argue here that this cold coronal component is likely to originate from the near-sun dust, and that there is a deficit of coronal dust close to the Sun. Title: The Solar-System-Scale Disk around AB Aurigae Authors: Oppenheimer, Ben R.; Brenner, Douglas; Hinkley, Sasha; Zimmerman, Neil; Sivaramakrishnan, Anand; Soummer, Remi; Kuhn, Jeffrey; Graham, James R.; Perrin, Marshall; Lloyd, James P.; Roberts, Lewis C., Jr.; Harrington, David M. Bibcode: 2008ApJ...679.1574O Altcode: 2008arXiv0803.3629O The young star AB Aurigae is surrounded by a complex combination of gas-rich and dust-dominated structures. The inner disk, which has not been studied previously at sufficient resolution and imaging dynamic range, seems to contain very little gas inside a radius of least 130 AU from the star. Using adaptive optics coronagraphy and polarimetry, we have imaged the dust in an annulus between 43 and 302 AU from the star, a region never seen before. An azimuthal gap in an annulus of dust at a radius of 102 AU, along with a clearing at closer radii inside this annulus, suggests the formation of at least one small body at an orbital distance of ~100 AU. This structure seems consistent with crude models of mean motion resonances or accumulation of material at two of the Lagrange points relative to the putative object and the star. We also report a low significance detection of a point source in this outer annulus of dust. This source may be an overdensity in the disk due to dust accreting onto an unseen companion. An alternate interpretation suggests that the object's mass is between 5 and 37 times the mass of Jupiter. The results have implications for circumstellar disk dynamics and planet formation. Title: The Facility IR Spectropolarimeter for the Dunn Solar Telescope Authors: Jaeggli, S. A.; Lin, H.; Mickey, D. L.; Kuhn, J. R.; Hegwer, S. L.; Rimmele, T. R.; Penn, M. J. Bibcode: 2008AGUSMSH31A..11J Altcode: The Facility IR Spectropolarimeter(FIRS) is a multi-slit spectropolarimeter designed for the Dunn Solar Telescope (DST) at the National Solar Observatory on Sacramento Peak (NSO/SP) in New Mexico to study magnetism on the solar surface. The instrument samples adjacent slices of the solar surface using four parallel slits to achieve high cadence, diffraction-limited, precision imaging-spectropolarimetry. Due to the versatile, multi-armed design of the spectrograph, up to four spectral lines at visible and infrared wavelengths, covering four different heights in the solar atmosphere, can be observed simultaneously. In this poster-paper we will describe the design, capabilities, and performance of the instrument. Title: First Direct Detection of Magnetic Fields in Starspots and Stellar Chromospheres Authors: Berdyugina, S. V.; Fluri, D. M.; Afram, N.; Suwald, F.; Petit, P.; Arnaud, J.; Harrington, D. M.; Kuhn, J. R. Bibcode: 2008ASPC..384..175B Altcode: 2008csss...14..175B; 2007astro.ph..3559B Here we report on the first detection of circular polarization in molecular lines formed in cool magnetic regions (starspots) and in chromospheric emission lines formed in hot plages on the surfaces of active stars.

Our survey of G-K-M stars included young main-sequence dwarfs and RS~CVn-type giants and subgiants. All stars were found to possess surface magnetic fields producing Stokes V LSD signals in atomic lines of 0.05% to 0.5%. Several stars clearly showed circular polarization in molecular lines of 0.1% to 1%. The molecular Stokes V signal is reminiscent of that observed in sunspots. Chromospheric magnetic fields were detected on most active targets in Stokes~V profiles of emission lines with peak polarization up to 2%. The observed molecular circular polarization on M dwarfs indicates single-polarity magnetic fields covering at least 10% of the stellar disk. Smaller signals on K stars imply that their magnetic fields are apparently weaker, more entangled than on M dwarfs, or more diluted by the bright photosphere. Title: Spectropolarimetric Observations of Herbig Ae/Be Stars. I. HiVIS Spectropolarimetric Calibration and Reduction Techniques Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2008PASP..120...89H Altcode: 2007arXiv0711.2327H Using the High-Resolution Visible Spectrograph (HiVIS) spectropolarimeter built for the Haleakala 3.7 m Advanced Electro-optical System (AEOS) telescope in Hawaii, we are collecting a large number of high precision spectropolarimetric observations of stars. In order to precisely measure very small polarization changes, we have performed a number of polarization calibration techniques on the AEOS telescope and HiVIS spectrograph. We have extended our dedicated IDL reduction package and have performed some hardware upgrades to the instrument. We have also used the ESPaDOnS spectropolarimeter on CFHT to verify the HiVIS results with back-to-back observations of MWC 361 and HD 163296. Comparison of this and other HiVIS data with stellar observations from the Intermediate-dispersion Spectroscopic and Imaging System (ISIS) and William-Wehlau (WW) spectropolarimeters in the literature further shows the usefulness of this instrument. Title: Curvature adaptive optics and low light imaging Authors: Ftaclas, C.; Chun, M.; Kuhn, J.; Ritter, J. Bibcode: 2008amos.confE..20F Altcode: We review the basic approach of curvature adaptive optics (AO) and show how its many advantages arise. A curvature wave front sensor (WFS) measures exactly what a curvature deformable mirror (DM) generates. This leads to the computational and operational simplicity of a nearly diagonal control matrix. The DM automatically reconstructs the wave front based on WFS curvature measurements. Thus, there is no formal wave front reconstruction. This poses an interesting challenge to post-processing of AO images. Physical continuity of the DM and the reconstruction of phase from wave front curvature data assure that each actuated region of the DM corrects local phase, tip-tilt and focus. This gain in per-channel correction efficiency, combined with the need for only one pixel per channel detector reads in the WFS allows the use of photon counting detectors for wave front sensing. We note that the use of photon counting detectors implies penalty-free combination of correction channels either in the WFS or on the DM. This effectively decouples bright and faint source performance in that one no longer predicts the other. The application of curvature AO to the low light moving target detection problem, and explore the resulting challenges to components and control systems. Rapidly moving targets impose high-speed operation posing new requirements unique to curvature components. On the plus side, curvature wave front sensors, unlike their Shack-Hartmann counterparts, are tunable for optimum sensitivity to seeing and we are examining autonomous optimization of the WFS to respond to rapid changes in seeing. Title: Observing Interstellar Neutral Helium from the Ground Authors: Moise, E.; Kuhn, J. Bibcode: 2007AGUFMSH14A1698M Altcode: Cool neutral Helium is now being observed near the Sun. Routinely from sensitive IR spectropolarimetry data using SOLARC at Haleakala and from eclipses, observations reveal scattered photospheric light at 1083nm from He I far above the solar limb. Here we report on observations of this transient coronal constituent that help to understand whether this comes from the coronal "inner source" or from the interstellar Helium wind. Title: Detection of an Extended Near-Sun Neutral Helium Cloud from Ground-based Infrared Coronagraph Spectropolarimetry Authors: Kuhn, J. R.; Arnaud, J.; Jaeggli, S.; Lin, H.; Moise, E. Bibcode: 2007ApJ...667L.203K Altcode: Sensitive spectropolarimetric observations from the Haleakala SOLARC coronagraph and infrared imaging spectropolarimeter have detected an extended diffuse surface brightness flux at the 1083 nm wavelength of neutral helium (He I). This has the polarization signature of light scattered by an extended He I cloud in the vicinity of the Sun. The He I scattered surface brightness appears to be consistent with a previous eclipse measurement and satellite observations of the local interstellar medium (LISM) helium wind (LISW), obtained using observations of the He I UV resonance line at 58.4 nm. The sensitivity of the infrared coronagraphic method suggests that the LISW interaction with the local solar wind can have observable consequences that may yield a useful ground-based technique for studying the coronal and interplanetary plasma. Title: A New Mechanism for Polarizing Light from Obscured Stars Authors: Kuhn, J. R.; Berdyugina, S. V.; Fluri, D. M.; Harrington, D. M.; Stenflo, J. O. Bibcode: 2007ApJ...668L..63K Altcode: 2007arXiv0708.0599K Recent spectropolarimetric observations of Herbig Ae/Be stellar systems show linear polarization variability with wavelength and epoch near their obscured Hα emission. Surprisingly, this polarization is not coincident with the Hα emission peak but is variable near the absorptive part of the line profile. With a new and novel model, we show here that this is evidence of optical pumping-anisotropy of the incident radiation that leads to a linear polarization-dependent optical depth within the intervening hydrogen wind or disk cloud. This effect can yield a larger polarization signal than scattering polarization in these systems. Title: Spectropolarimetry of the Hα Line in Herbig Ae/Be Stars Authors: Harrington, D. M.; Kuhn, J. R. Bibcode: 2007ApJ...667L..89H Altcode: 2007arXiv0708.0601H Using the HiVIS spectropolarimeter built for the Haleakala 3.7 m AEOS telescope, we have obtained a large number of high-precision spectropolarimetrc observations (284) of Herbig AeBe stars collected over 53 nights totaling more than 300 hr of observing. Our sample of five HAeBe stars, AB Aurigae, MWC 480, MWC 120, MWC 158, and HD 58647, all show systematic variations in the linear polarization amplitude and direction as a function of time and wavelength near the Hα line. In all our stars, the Hα line profiles show evidence of an intervening disk or outflowing wind, evidenced by strong emission with an absorptive component. The linear polarization varies by 0.2%-1.5% with the change typically centered in the absorptive part of the line profile. These observations are inconsistent with a simple disk-scattering model or a depolarization model that produce polarization changes centered on the emissive core. We speculate that polarized absorption via optical pumping of the intervening gas may be the cause. Title: The Lyot Project: Status and Results Authors: Sivaramakrishnan, A.; Oppenheimer, B. R.; Soummer, R.; Hinkley, S.; Brenner, D.; Leconte, J.; Roberts, L. C.; Perrin, M. D.; Lloyd, J. P.; Makidon, R. B.; Kuhn, J. R. Bibcode: 2007lyot.confE..21S Altcode: The Lyot Project near-IR coronagraph, operating behind the AEOS 3.6m 941-channel adaptive optics system, has opened up new search areas in the mass-separation parameter space of faint companions to nearby stars brighter than V=7. As the first so-called extreme AO system on sky, often operating at a 90% Strehl ratio at H with an upgraded AEOS AO system, its use has uncovered some hitherto unforeeseen difficulties in the search for faint companions. The coronagraph possesses a simultaneous dual-polarization mode and a novel technique for precision relative astrometry and photometry. We have also developed a refinement of the angular differential imaging technique in order to suppress the static and quasi-static speckles that limit our dynamic range. We are about to explore newer coronagraph designs, and place an Integral Field Unit spectrograph behind the coronagraph. Title: The Lyot Project: Survey Analysis Authors: Leconte, J.; Soummer, R.; Oppenheimer, B. R.; Hinkley, S.; Brenner, D.; Sivaramakrishnan, A.; Kuhn, J.; Perrin, M. D.; Roberts, L. C., Jr.; Simon, M.; Brown, R. A.; Chabrier, G.; Baraffe, I. Bibcode: 2007lyot.confE..44L Altcode: The Lyot project survey has observed 57 stars so far. We have developed some image processing and analysis tools to reduce speckle noise with Angular Differential Imaging, and to estimate the detection sensitivity (dynamic range) from the data. We apply these techniques to each star of the survey, and give a general overview of the instrument sensitivity. We use a Monte-Carlo based approach to define the possible population of companions around these stars, and we determine the completeness of each observation as a function of mass and semi-major axis, according to the measured dynamic range for each star. We use the overall survey non-detection results to constrain the possible population of companions. Title: Mees Imaging Solar Spectrometer Authors: Lin, Haosheng; Li, J.; Kuhn, J. R.; Mickey, D.; Habbal, S. R.; Jaeggli, S. S. Bibcode: 2007AAS...210.9215L Altcode: 2007BAAS...39R.210L We propose the construction of a new instrument, the Mees Imaging Solar Spectrometer (MISS), optimized for spectroscopic study of energetic solar events such as filament eruptions and solar flares, and their relationship to coronal mass ejections. MISS is a fiber-optics-based imaging spectrograph. It will be able to perform simultaneous spectroscopic observations of selected spectral lines and continuum over an extended field with high spatial and spectral resolution and high cadence. It will operate nominally in a low-resolution (20" per pixel), full-disk patrol mode, and can be rapidly switched to a high-resolution (1" per pixel) region-of-interest mode of observation when energetic events are detected. Several spectral lines, from CaII H & K to HeI 1083 nm can be recorded in rapid succession. These advanced imaging spectroscopic capabilities make it an ideal instrument for the study of the rapid change of the physical conditions of the solar atmosphere during these energetic events. Title: Observing Interstellar Neutral Helium from the Ground Authors: Moise, Elena; Kuhn, J. Bibcode: 2007AAS...21012007M Altcode: 2007BAAS...39..246M Cool neutral Helium is now being observed near the Sun. Routine observations by SOLARC at Haleakala Observatory (by means of IR spectropolarimetry) reveal the existence of scattered photospheric light at 1083nm from HeI far above the solar limb. Here we report on recent observations of this transient coronal constituent that help us understand whether this cool HeI comes from the coronal "inner source" or from the interstellar Helium wind. Title: A Changing Solar Shape Authors: Kuhn, Jeffrey R.; Emilio, M.; Bush, R.; Scherrer, P. Bibcode: 2007AAS...21012001K Altcode: 2007BAAS...39..245K The Sun's shape is sensitive to the influence of gravity, rotation, and local turbulence and magnetic fields in its outer atmosphere. In 1997 the Michelson Doppler Imager (MDI) aboard the Solar and Heliospheric Observatory (SOHO) allowed a precise measurement of the oblateness from above the atmosphere. In 2001 this technique was repeated and we report here on the detection of a time-variable solar shape from these data. Title: What Makes The Advanced Technology Solar Telescope (ATST) So Advanced? Authors: Kuhn, Jeffrey R.; Rimmele, T.; ATST Design Team Bibcode: 2007AAS...210.6701K Altcode: 2007BAAS...39..175K -- Its the science! While its true that we haven't advanced ground-based solar astronomy by a leap as big as this since Galileo, its the qualitatively new insights that we expect with ATST that drive its design. ATST isn't so much a telescope as much as it is a sensitive magnetometer, and a high dynamic range imaging spectropolarimeter. In this talk we'll try to draw the lines between the questions you've always wanted to ask about the Sun, and this unique optical and infrared instrument. Title: Molecular Hydrogen Dynamics in the Cool Photosphere Authors: Downs, Cooper; Kuhn, J. Bibcode: 2007AAS...210.2501D Altcode: 2007BAAS...39..131D Molecular hydrogen can be a major component of the cool solar photosphere in magnetic regions. The steep dependence in the abundance fraction of the molecular species with temperature can produce strong relative density gradients that can dominate the local hydrostatic pressure. These pressure gradients can produce "diffusive" shock fronts that may have important dynamical consequences on, for example, sunspot penumbrae formation. We explore some simple analytic and numerical multi-fluid models that illustrate these dynamical effects. Title: A Changing Solar Shape Authors: Emilio, M.; Bush, R. I.; Kuhn, J.; Scherrer, P. Bibcode: 2007ApJ...660L.161E Altcode: The Sun's shape is sensitive to the influence of gravity, rotation, and local turbulence and magnetic fields in its outer atmosphere. A careful measurement of this shape has long been sought to better understand the solar structure and its change during the 11 yr solar cycle. Numerous disparate measurements of the solar oblateness or the fractional difference between equatorial and polar radii have been difficult to interpret, in part because this quantity is much smaller than terrestrial atmospheric seeing and most instrumental noise sources. In 1997 the Michelson Doppler Imager (MDI) aboard the Solar and Heliospheric Observatory (SOHO) obtained a precise measurement of the oblateness from above the atmosphere by utilizing a spacecraft roll procedure to remove instrumental influences. In 2001 this technique was repeated, and we report here on the detection of a time-variable solar shape from these data. The changing oblateness we find from 1997 to 2001 is smaller than the apparent discrepancy between earlier ground-based observations, but is significantly larger than MDI's astrometric measurement uncertainty. The shape change appears to be anticorrelated with the observed helioseismic variability. This fact and our MDI measurements suggest that the outer solar atmosphere expands nonhomologously during the cycle. It is possible that solar cycle changes in the turbulent pressure in the outer atmosphere can account for both the optical limb change and the helioseismic acoustic global solar shape change. Title: The Lyot Project: status and results Authors: Sivaramakrishnan, Anand; Oppenheimer, Ben R.; Hinkley, Sasha; Brenner, Douglas; Soummer, Rémi; Mey, Jacob L.; Lloyd, James P.; Perrin, Marshall D.; Graham, James R.; Makidon, Russell B.; Roberts, Lewis C.; Kuhn, Jeffrey R. Bibcode: 2007CRPhy...8..355S Altcode: We present a retrospective on, and some new imaging data from The Lyot Project JHK coronagraph which is used behind the 3.6 m AEOS 941-channel AO telescope on Mt. Haleakala, on the island of Maui in Hawaii. This instrument is the first ‘extreme adaptive optics’ (ExAO) coronagraph ever; it opens up new scientific search spaces in direct imaging of faint companions of nearby stars. It also blazed a trail for current ExAO systems being developed for ESO-VLT and Gemini telescopes. Amongst other things, the Lyot Project has been used to demonstrate a device for precision coronagraphic astrometry and photometry using the novel technique of placing a wire grid over the pupil to create stable fiducial ghost images, to show the effects of frozen actuators on a deformable mirror, to refine angular differential imaging for use on the Coudé focus of Alt-Az telescopes, and to develop a coronagraphic data reduction pipeline. To cite this article: A. Sivaramakrishnan et al., C. R. Physique 8 (2007). Title: Spectropolarimetry of the Deep Impact target Comet 9P/Tempel 1 with HiVIS Authors: Harrington, D. M.; Meech, K.; Kolokolova, L.; Kuhn, J. R.; Whitman, K. Bibcode: 2007Icar..187..177H Altcode: High resolution spectropolarimetry of the Deep Impact target, Comet 9P/Tempel 1, was performed during the impact event on July 4th, 2005 with the HiVIS spectropolarimeter and the AEOS 3.67-m telescope on Haleakala, Maui. We observed atypical polarization spectra that changed significantly in the few hours after the impact. The polarization of scattered light as a function of wavelength is very sensitive to the size and composition (complex refractive index) of the scattering particles as well as the scattering geometry. As opposed to most observations of cometary dust, which show an increase in the linear polarization with the wavelength (at least in the visible domain and for phase angles greater than about 30, a red polarization spectrum) observations of 9P/Tempel 1 at a phase angle of 41° beginning 8 min after impact and centered at 6:30 UT showed a polarization of 4% at 650 nm falling to 3% at 950 nm. The next observation, centered an hour later showed a polarization of 7% at 650 nm falling to 2% at 950 nm. This corresponds to a spectropolarimetric gradient, or slope, of -0.9% per 1000 Å 40 min after impact, decreasing to a slope of -2.3% per 1000 Å an hour and a half after impact. This is an atypical blue polarization slope, which became more blue 1 h after impact. The polarization values of 4 and 7% at 650 nm are typical for comets at this scattering angle, whereas the low polarization of 2 and 3% at 950 nm is not. We compare observations of Comet 9P/Tempel 1 to that of a typical comet, C/2004 Machholz, at a phase angle of 30° which showed a typical red slope, rising from 2% at 650 nm to 3% at 950 nm in two different observations (+1.0 and +0.9% per 1000 Å). Title: Temporal Evolution of Coronagraphic Dynamic Range and Constraints on Companions to Vega Authors: Hinkley, Sasha; Oppenheimer, Ben R.; Soummer, Rémi; Sivaramakrishnan, Anand; Roberts, Lewis C., Jr.; Kuhn, Jeffrey; Makidon, Russell B.; Perrin, Marshall D.; Lloyd, James P.; Kratter, Kaitlin; Brenner, Douglas Bibcode: 2007ApJ...654..633H Altcode: 2006astro.ph..9337H The major obstacle to the direct detection of companions to nearby stars is the overwhelming brightness of the host star. Current instruments employing the combination of adaptive optics (AO) and coronagraphy can typically detect objects within 2" of the star that are ~104-105 times fainter. Correlated speckle noise is one of the biggest obstacles limiting such high-contrast imaging. We have obtained a series of 284 8 s, AO-corrected, coronagraphically occulted H-band images of the star Vega at the 3.63 m AEOS telescope located on Haleakala, Hawaii. This data set is unique for studying the temporal behavior of speckle noise and represents the first time such a study on highly corrected coronagraphic AO images has been carried out in a quantitative way. We find the speckle pattern to be highly stable in both position and time in our data. This is due to the fact that the AO system corrects disturbances to the stellar wave front at the level where the instrumental wave front errors dominate. Because of this, we find that our detection limit is not significantly improved simply with increased exposure time alone. However, we are able to improve our dynamic range by 1.5-2 mag through subtraction of static/quasi-static speckles in two rotating frames: the telescope pupil frame and the deformable mirror frame. The highly stable nature of speckles will exist for any program using coronagraphy and high-order AO. Furthermore, from our data, we are able to constrain the mass of any purported companion to Vega to be less than ~45MJ at 8 AU and less than ~30MJ at 16 AU, radii not previously probed at these sensitivities. Title: Spectropolarimetry of the Deep Impact target Comet 9P/Tempel 1 with HiVIS Authors: Harrington, D. M.; Meech, K.; Kolokolova, L.; Kuhn, J. R.; Whitman, K. Bibcode: 2007Icar..191S.381H Altcode: 2007Icar..191..381H; 2006astro.ph..8676H High resolution spectropolarimetry of the Deep Impact target, Comet 9P/Tempel 1, was performed during the impact event on July 4th, 2005 with the HiVIS spectropolarimeter and the AEOS 3.67-m telescope on Haleakala, Maui. We observed atypical polarization spectra that changed significantly in the few hours after the impact. The polarization of scattered light as a function of wavelength is very sensitive to the size and composition (complex refractive index) of the scattering particles as well as the scattering geometry. As opposed to most observations of cometary dust, which show an increase in the linear polarization with the wavelength (at least in the visible domain and for phase angles greater than about 30, a red polarization spectrum) observations of 9P/Tempel 1 at a phase angle of 41° beginning 8 min after impact and centered at 6:30 UT showed a polarization of 4% at 650 nm falling to 3% at 950 nm. The next observation, centered an hour later showed a polarization of 7% at 650 nm falling to 2% at 950 nm. This corresponds to a spectropolarimetric gradient, or slope, of -0.9% per 1000 Å 40 min after impact, decreasing to a slope of -2.3% per 1000 Å an hour and a half after impact. This is an atypical blue polarization slope, which became more blue 1 h after impact. The polarization values of 4 and 7% at 650 nm are typical for comets at this scattering angle, whereas the low polarization of 2 and 3% at 950 nm is not. We compare observations of Comet 9P/Tempel 1 to that of a typical comet, C/2004 Machholz, at a phase angle of 30° which showed a typical red slope, rising from 2% at 650 nm to 3% at 950 nm in two different observations (+1.0 and +0.9% per 1000 Å). Title: Broadband Spectroscopy of the Corona during the Total Solar Eclipse of March 29, 2006 Authors: Jaeggli, Sarah A.; Habbal, S. R.; Kuhn, J. R.; Nayfeh, M. H. Bibcode: 2006AAS...209.1601J Altcode: 2006BAAS...38..918J We present coronal observations from the total solar eclipse of 29 March 2006 taken near Waw al Namus, Libya. During the 4 minutes and 6 seconds of totality, observations were made with a tracking collecting mirror and fiber-fed spectrograph. The spectrograph used is a high quantum efficiency commercial Ocean Optics QE65000 Spectrometer with a wavelength range of 350 to 1100 nm, and spectral resolution of about 0.75 nm. High quantum efficiency allowed for many short exposures of the inner (100 msec) and outer (10,000 msec) corona during the eclipse. Important spectral features, and the difference in color between the inner and outer corona are identified. Atmospheric contributions are discussed. Likely candidates for the nature of dust grains contributing to the F-corona measurements are also presented. These are compared with laboratory spectra of silicon nanoparticles. Title: Osmotically Driven Neutral Sunspot Winds Authors: Kuhn, J. R.; Morgan, H. Bibcode: 2006ASPC..354..230K Altcode: The low ionization state in parts of a sunspot may play an important role in its evolution and dynamical state. The cool magnetic interior region of the umbra develops a substantial neutral atomic and molecular hydrogen osmotic pressure which can drive a wind outward from the umbra. Ambipolar diffusion against the magnetically pinned ionized plasma component can also distort the umbral magnetic field into a filamentary penumbral structure. This wind can contribute to the development of the sunspot penumbra and the Evershed flow. Title: Polarimetric Imaging and Spectroscopy of the Corona from 400 to 2000 nm during the Total Solar Eclipse of 29 March 2006 Authors: Habbal, S. R.; Kuhn, J.; Mickey, D.; Morgan, H.; Jaeggli, S.; Johnson, J.; Daw, A.; Arndt, M. B.; Nayfeh, M.; Roussev, I. Bibcode: 2006AGUFMSH44A..06H Altcode: Total solar eclipses continue to offer unique opportunities for exploring the solar corona, in particular for validating new concepts, and testing new instrumentation. We report on the results of the observations taken during the total solar eclipse of 29 March 2006. The eclipse was observed from Waw AnNamous, Libya, under perfect seeing conditions. A complement of imaging and spectroscopic polarization measurements, covering the wavelength range from 400 to 2000 nm, were used. Among the highlights of the observations were the unexpected radial extent of the emission from the Fe XI 789.2 nm spectral line, which has proven to have significant potential for future coronagraphic measurements, and the appearance of presently unidentified spectral lines in the visible and near infrared part of the spectrum. The implications of these results for the coronal magnetic field, and the near-Sun dust environment will be discussed. Title: The Coronal Solar Magnetic Observatory (COSMO) Authors: Tomczyk, S.; Zurbuchen, T.; Kuhn, J.; Lin, H.; Judge, P.; Burkepile, J.; Casini, R. Bibcode: 2006AGUFMSM12A..03T Altcode: Measurement of magnetic fields in the corona is arguably the most important observable required for advances in our understanding of the emergence of magnetic flux into the solar atmosphere and the processes responsible for the production of solar activity, coronal heating and coronal dynamics. We discuss plans for the COronal Solar Magnetic Observatory (COSMO), which is a proposed ground-based suite of instruments designed to routinely study coronal magnetic fields and their environment. The core of the facility includes a meter-class coronagraph with instrumentation dedicated to measuring the coronal magnetic field using the polarization of forbidden emission lines in the infrared. Supporting instruments focus on prominence magnetometry and the dynamics of the electron-scattered corona (K-corona) and chromosphere. In addition to acquiring routine synoptic observations of coronal magnetic fields, the COSMO project will include the establishment of a community-based user advisory panel to accept observational campaigns submitted by members of the scientific community at-large. COSMO will enhance the value of existing and new observatories on the ground (SOLIS, ATST, FASR) and in space (SOHO, TRACE, GOES, Solar-B, STEREO and SDO) by providing unique and crucial observations of the global coronal magnetic field and its evolution and dynamics. Title: The Challenges of Coronagraphic Astrometry Authors: Digby, Andrew P.; Hinkley, Sasha; Oppenheimer, Ben R.; Sivaramakrishnan, Anand; Lloyd, James P.; Perrin, Marshall D.; Roberts, Lewis C., Jr.; Soummer, Rémi; Brenner, Douglas; Makidon, Russell B.; Shara, Michael; Kuhn, Jeffrey; Graham, James; Kalas, Paul; Newburgh, Laura Bibcode: 2006ApJ...650..484D Altcode: A coronagraph in conjunction with adaptive optics provides an effective means to image faint companions of nearby stars from the ground. The images from such a system are complex, however, and need to be fully characterized and understood before planets or disks can be detected against the glare from the host star. Using data from the Lyot Project coronagraph, we investigate the difficulties of astrometric measurements in diffraction-limited coronagraphic images and consider the principal problem of determining the precise location of the occulted star. We demonstrate how the image structure varies when the star is decentered from the optical axis and show how even small offsets (0.05λ/D or 5 mas) give rise to false sources in the image. We consider methods of determining the star position from centroiding, instrument feedback, and analysis of point-spread function symmetry and conclude that internal metrology is the most effective technique.

Based on observations made at the Maui Space Surveillance System operated by Detachment 15 of the US Air Force Research Laboratory's Directed Energy Directorate. Title: Progress on the 1.6-meter New Solar Telescope at Big Bear Solar Observatory Authors: Denker, C.; Goode, P. R.; Ren, D.; Saadeghvaziri, M. A.; Verdoni, A. P.; Wang, H.; Yang, G.; Abramenko, V.; Cao, W.; Coulter, R.; Fear, R.; Nenow, J.; Shoumko, S.; Spirock, T. J.; Varsik, J. R.; Chae, J.; Kuhn, J. R.; Moon, Y.; Park, Y. D.; Tritschler, A. Bibcode: 2006SPIE.6267E..0AD Altcode: 2006SPIE.6267E..10D The New Solar Telescope (NST) project at Big Bear Solar Observatory (BBSO) now has all major contracts for design and fabrication in place and construction of components is well underway. NST is a collaboration between BBSO, the Korean Astronomical Observatory (KAO) and Institute for Astronomy (IfA) at the University of Hawaii. The project will install a 1.6-meter, off-axis telescope at BBSO, replacing a number of older solar telescopes. The NST will be located in a recently refurbished dome on the BBSO causeway, which projects 300 meters into the Big Bear Lake. Recent site surveys have confirmed that BBSO is one of the premier solar observing sites in the world. NST will be uniquely equipped to take advantage of the long periods of excellent seeing common at the lake site. An up-to-date progress report will be presented including an overview of the project and details on the current state of the design. The report provides a detailed description of the optical design, the thermal control of the new dome, the optical support structure, the telescope control systems, active and adaptive optics systems, and the post-focus instrumentation for high-resolution spectro-polarimetry. Title: The New HiVIS Spectropolarimeter and Spectropolarimetric Calibration of the AEOS Telescope Authors: Harrington, D. M.; Kuhn, J. R.; Whitman, K. Bibcode: 2006PASP..118..845H Altcode: 2006astro.ph..6503H We have designed, built, and calibrated a new spectropolarimeter for the HiVIS spectrograph (R ~ 12,000-49,000) on the Advanced Electro-Optical System (AEOS) telescope. We have also conducted a polarization calibration of the telescope and instrument. In this paper, we introduce the design and use of the spectropolarimeter, in addition to a new data-reduction package we have developed, and then discuss the polarization calibration of the spectropolarimeter and the AEOS telescope. We used observations of unpolarized standard stars at many pointings to measure the telescope-induced polarization and compare it with a Zemax model. The telescope induces polarization of 1%-6%, with a strong variation with wavelength and pointing, consistent with the expected altitude and azimuth variation. We then used scattered sunlight as a linearly polarized source to measure the telescope's spectropolarimetric response to linearly polarized light. Finally, we made an all-sky map of the telescope's polarization response to calibrate future spectropolarimetry. Title: Site testing for the Advanced Technology Solar Telescope Authors: Hill, F.; Beckers, J.; Brandt, P.; Briggs, J.; Brown, T.; Brown, W.; Collados, M.; Denker, C.; Fletcher, S.; Hegwer, S.; Horst, T.; Komsa, M.; Kuhn, J.; Lecinski, A.; Lin, H.; Oncley, S.; Penn, M.; Radick, R.; Rimmele, T.; Socas-Navarro, H.; Streander, K. Bibcode: 2006SPIE.6267E..1TH Altcode: 2006SPIE.6267E..59H The Advanced Solar Technology Telescope (ATST) is a 4-m solar telescope being designed for high spatial, spectral and temporal resolution, as well as IR and low-scattered light observations. The overall limit of performance of the telescope is strongly influenced by the qualities of the site at which it is located. Six sites were tested with a seeing monitor and a sky brightness instrument for 1.5 to 2 years. The sites were Big Bear (California), Haleakala (Hawaii), La Palma (Canary Islands, Spain), Panguitch Lake (Utah), Sacramento Peak (New Mexico), and San Pedro Martir (Baja California, Mexico). In this paper we will describe the methods and results of the site survey, which chose Haleakala as the location of the ATST. Title: Using Polarimetric Imaging and Spectroscopy of the Corona from 400 to 1800 nm for Exploring the near Sun Plasma Authors: Habbal, S. Rifai; Kuhn, J.; Mickey, D.; Jaeggli, S.; Morgan, H.; Roussev, I.; Johnson, J.; Arndt, M. B.; Daw, A.; Nayfeh, M. H. Bibcode: 2006spse.conf...27H Altcode: No abstract at ADS Title: Infrared Coronal Polarimetry: Magnetometry and More Authors: Kuhn, J.; Lin, H.; Jaeggli, S.; Arnaud, J.; Mickey, D. Bibcode: 2006cosp...36.1643K Altcode: 2006cosp.meet.1643K Near-infrared spectropolarimetry of the solar corona is a powerful tool for measuring the coronal magnetic field and even the local interstellar wind Here we describe how sensitive imaging spectropolarimetric observations are being obtained from the worlds largest coronagraph -- a reflecting off-axis telescope -- from the summit of Haleakala Hawai i Title: The Lyot project coronagraph: data processing and performance analysis Authors: Soummer, R.; Oppenheimer, B. R.; Hinkley, S.; Sivaramakrishnan, A.; Makidon, R. B.; Digby, A.; Brenner, D.; Kuhn, J.; Perrin, M. D.; Roberts, L. C., Jr.; Kratter, K. Bibcode: 2006EAS....22..199S Altcode: In this communication we illustrate the main steps required for the preprocessing of the Lyot Project Coronagraph data, starting from the raw data to the reduced data. We then discuss the estimation of the performance on direct, unocculted data, by measuring the Strehl Ratio on these images. We show that Strehl Ratios of the order of 80% can be obtained for the best images in the H Band, using the AEOS telescope adaptive optics, and the Kermit infrared camera. We then present a few methods to estimate the dynamic range in coronagraphic images, and their results are discussed. Title: Scattered Light Suppression and IR Polarimetry Authors: Kuhn, J. R. Bibcode: 2005ASPC..343...22K Altcode: Dual-beam polarimetry is an effective tool for high dynamic range imaging of circumstellar regions. We have achieved scattered light suppression exceeding 5 magnitudes over angular scales where current adaptive optics systems are not useful. This paper describes some techniques and algorithms that are generally helpful for detecting faint circumstallar scattered light associated with disk systems. Title: Using Imaging Infrared Coronal Spectropolarimetry to Measure the Near-Sun Plasma Authors: Kuhn, J.; Lin, H.; Arnaud, J.; Jaeggli, S. Bibcode: 2005AGUFMSH44A..08K Altcode: A moderate aperture ground-based coronagraph and an imaging infrared spectropolarimeter have provided our first direct longitudinal coronal magnetograms. This talk will describe the advantages and subtleties of these techniques for direct coronal magnetometry. We also summarize some of the diagnostic potential of current and likely future IR spectropolarimetric instruments (like the Advanced Technology Solar Telescope) for measuring the properties of the near-solar plasma. Title: Solar Site Survey for the Advanced Technology Solar Telescope. I. Analysis of the Seeing Data Authors: Socas-Navarro, H.; Beckers, J.; Brandt, P.; Briggs, J.; Brown, T.; Brown, W.; Collados, M.; Denker, C.; Fletcher, S.; Hegwer, S.; Hill, F.; Horst, T.; Komsa, M.; Kuhn, J.; Lecinski, A.; Lin, H.; Oncley, S.; Penn, M.; Rimmele, T.; Streander, K. Bibcode: 2005PASP..117.1296S Altcode: 2005astro.ph..8690S The site survey for the Advanced Technology Solar Telescope concluded recently after more than 2 years of data gathering and analysis. Six locations, including lake, island, and continental sites, were thoroughly probed for image quality and sky brightness. The present paper describes the analysis methodology employed to determine the height stratification of the atmospheric turbulence. This information is crucial, because daytime seeing is often very different between the actual telescope aperture (~30 m) and the ground. Two independent inversion codes have been developed to simultaneously analyze data from a scintillometer array and a solar differential image monitor. We show here the results of applying them to a sample subset of data from 2003 May that was used for testing. Both codes retrieve a similar seeing stratification through the height range of interest. A quantitative comparison between our analysis procedure and actual in situ measurements confirms the validity of the inversions. The sample data presented in this paper reveal a qualitatively different behavior for the lake sites (dominated by high-altitude seeing) and the rest (dominated by near-ground turbulence). Title: Exploring Halo Substructure with Giant Stars: The Velocity Dispersion Profiles of the Ursa Minor and Draco Dwarf Spheroidal Galaxies at Large Angular Separations Authors: Muñoz, Ricardo R.; Frinchaboy, Peter M.; Majewski, Steven R.; Kuhn, Jeffrey R.; Chou, Mei-Yin; Palma, Christopher; Sohn, Sangmo Tony; Patterson, Richard J.; Siegel, Michael H. Bibcode: 2005ApJ...631L.137M Altcode: 2005astro.ph..4035M We analyze velocity dispersion profiles for the Draco and Ursa Minor (UMi) dwarf spheroidal (dSph) galaxies based on published and new Keck HIRES spectra for stars in the outer UMi field. Washington + DDO51 filter photometric catalogs provide additional leverage on membership of individual stars and, beyond 0.5 King limiting radii (rlim), identify bona fide dSph members up to 4.5 times more efficiently than simple color-magnitude diagram selections. Previously reported ``cold populations'' at rlim are not obvious in the data and appear only with particular binning; more or less constant and platykurtic dispersion profiles are characteristic of these dSphs to large radii. We report the discovery of UMi stars to at least 2.7rlim (i.e., 210' or 4 kpc). Even with conservative assumptions, a UMi mass of M>4.9×108 Msolar is required to bind these stars, implying an unlikely global mass-to-light ratio of M/L>900 (M/L)solar. We conclude that we have found stars tidally stripped from UMi. Title: Are Neutral Sunspot Winds Important for Penumbral Dynamics and the First Ionization Potential Effect? Authors: Kuhn, J. R.; Lin, H.; Morgan, H. Bibcode: 2005astro.ph..9862K Altcode: The low ionization state in parts of a sunspot may play an important role in its evolution and dynamical state. The cool magnetic interior region of the sunspot develops a substantial neutral atomic and molecular hydrogen osmotic pressure which can drive a wind outward from the umbra. Ambipolar diffusion against the magnetically pinned ionized plasma component can also distort the umbral magnetic field into a filamentary penumbral structure. This may be important for explaining the development of the sunspot penumbra and the Evershed flow. This fractionation process may also be important for the ``First Ionization Potential'' (FIP) effect seen in the solar wind. In support of this mechanism we find evidence for such ionization fractionization in UV observations of molecular hydrogen in a sunspot umbra and penumbra. Title: High precision polarimetry with the Advanced Technology Solar Telescope Authors: Socas-Navarro, Hector; Elmore, David F.; Keller, Christoph U.; Seagraves, Paul H.; Streander, Kim V.; Card, Gregory L.; Warner, Mark; Kuhn, Jeffrey R.; Mickey, Donald L. Bibcode: 2005SPIE.5901...52S Altcode: This paper addresses the issue of calibrating the Advanced Technology Solar Telescope for high-precision polarimetry, in particular of the optical train above the Gregorian station (where suitable calibration optics will be placed). Conventional techniques would not be adequate for this telescope given its large aperture. Here we explore two different methods that are currently being considered by the design team. The first one is the "sub-aperture" method, which uses small calibration optics above the primary mirror to calibrate a small sub-aperture of the system. This calibration is then extended to the full aperture by means of actual observations. The second method is based on analyzing the polarization observed in a spectral line with a peculiar Zeeman pattern, such as the FeII 614.9 nm line, which does not produce any intrinsic linear polarization. Numerical simulations are presented that show the robustness of both techniques and their respective advantages and disadvantages are discussed. Title: Spectropolarimetry of the dust coma of Deep Impact target 9P/Tempel 1 Authors: Harrington, D. M.; Meech, K. J.; Kuhn, J.; Kolokolova, L.; Pittichova, J.; Harrington, D. M.; Meech, K. J.; Kuhn, J.; Kolokolova, L.; Pittichova, J. Bibcode: 2005DPS....37.4402H Altcode: 2005BAAS...37Q.715H Spectropolarimetry can be used to measure polarization of cometary continua as a function of wavelength and phase angle to learn about the dust properties. The wavelength dependence of the polarization is mainly controlled by the complex refractive index of the material making up the particles, and the spectral dependence of the intensity is also sensitive to the size of the particles. We will use the new IfA-designed high-resolution spectropolarimeter (R 12000 to 49000, from 5400 to 9900 Angstroms) mounted on the AEOS 3.7m telescope on Haleakala, Maui to characterize the size and composition of dust grains ejected from the comets. We will combine optical measurements of dust comae, Finson-Probstein dust-dynamical models (to get particle size distributions), and polarization spectra to study the composition of the dust grains in comet 9P/Tempel 1 both pre- and post impact to look for dust compositional changes between the pristine interior materials and the surface dust on the nucleus.

Support for this work was provided through University of Maryland and University of Hawaii subcontract Z667702, which was awarded under prime contract NASW-00004 from NASA. Title: Radial Alignment of Cluster Galaxies Authors: Pereira, M. J.; Kuhn, J. R. Bibcode: 2005ApJ...627L..21P Altcode: 2004astro.ph.11710P We report the discovery of a statistically significant radial alignment of cluster galaxies in a sample of 85 X-ray-selected clusters observed in the Sloan Digital Sky Survey. The tendency for alignment is a robust feature of our sample and does not vary significantly with individual cluster or galaxy properties. We use dynamical arguments to show that a significant fraction of cluster galaxies should be undergoing a parametric tidal resonance that can cause their long axes to orient themselves toward the center of the cluster potential, and therefore tentatively ascribe the observed radial alignment to this dynamical effect. Title: The ATST Site Survey Authors: Hill, F.; Beckers, J.; Brandt, P.; Briggs, J. W.; Brown, T.; Brown, W.; Collados, M.; Denker, C.; Fletcher, S.; Hegwer, S.; Horst, T.; Komsa, M.; Kuhn, J.; Lecinski, A.; Lin, H.; Oncley, S.; Penn, M.; Radick, R.; Rimmele, T.; Socas-Navarro, H.; Soltau, D.; Streander, K. Bibcode: 2005AGUSMSP34A..04H Altcode: The Advanced Technology Solar Telescope (ATST) will be the world's largest aperture solar telescope, and is being designed for high resolution, IR, and coronal research. It must be located at a site that maximizes the scientific return of this substantial investment. We present the instrumentation, analysis and results of the ATST site survey. Two instrumentation sets were deployed at each of six sites to measure seeing as a function of height, and sky brightness as a function of wavelength and off-limb position. Analysis software was developed to estimate the structure function Cn2 as a function of height near the ground, and the results were verified by comparison with in-situ measurements. Additional software was developed to estimate the sky brightness. The statistics of the conditions at the sites were corrected for observing habits and the annualized hours of specific observing conditions were estimated. These results were used to identify three excellent sites suitable to host the ATST: Haleakala, Big Bear and La Palma. Among them, Haleakala is proposed as the optimal location of the ATST, La Palma and Big Bear being viable alternative sites. Title: The New Solar Telescope at Big Bear Solar Observatory - A Progress Report Authors: Denker, C.; Cao, W.; Chae, J.; Coulter, R.; Kuhn, J. R.; Marquette, W. H.; Moon, Y.; Park, Y.; Ren, D.; Tritschler, A.; Varsik, J. R.; Wang, H.; Yang, G.; Shoumko, S.; Goode, P. R. Bibcode: 2005AGUSMSP43A..07D Altcode: The New Solar Telescope (NST) is a new 1.6-meter, off-axis telescope for the Big Bear Solar Observatory (BBSO) in California. The NST is collaboration between BBSO, the Korean Astronomical Observatory (KAO) and Institute for Astronomy (IfA) at the University of Hawaii. BBSO is an ideal site for high-spatial resolution observations, since this mountain-lake site provides consistent seeing conditions with extended periods of excellent seeing from sunrise to sunset. These unique seeing characteristics make BBSO ideally suited for combined high-resolution campaigns and synoptic observations, which are essential for studies of solar activity and space weather. In this progress report, we present the latest information on the optical design, the optical support structure, the telescope control system and the requisite instrumentation for the telescope. Acknowledgements: This work has been supported by NSF under grants ATM-0236945, ATM-0342560, MRI-0320540, and Air Force DURIP F-49620-03-1-0271. Title: First-Light Instrumentation for the Advanced Technology Solar Telescope Authors: Rimmele, T.; Balasubramaniam, K.; Berger, T.; Elmore, D.; Gary, A.; Keller, C.; Kuhn, J.; Lin, H.; Mickey, D.; Pevtsov, A.; Robinson, B.; Sigwarth, M.; Soccas-Navarro, H. Bibcode: 2005AGUSMSP34A..03R Altcode: The 4m Advanced Technology Solar Telescope (ATST) is the next generation ground based solar telescope. In this paper we provide an overview of the ATST post-focus instrumentation. The majority of ATST instrumentation is located in an instrument Coude lab facility, where a rotating platform provides image de-rotation. A high order adaptive optics system delivers a corrected beam to the Coude lab facility. Alternatively, instruments can be mounted at the Nasmyth focus. For example, instruments for observing the faint corona preferably will be mounted at Nasmyth where maximum throughput is achieved. In addition, the Nasmyth focus has minimum telescope polarization and minimum stray light. We give an overview of the initial set of first generation instruments: the Visible-Light Broadband Imager (VLBI), the Visible Spectro-Polarimeter (ViSP), the Near-IR Spectro-Polarimeter (NIRSP), which includes a coronal module, and the Visible Tunable Filter. We also discuss the unique and efficient approach to the ATST instrumentation, which builds on the use of common components such as detector systems, polarimetry packages and various opto-mechanical components. For example, the science requirement for polarimetric sensitivity (10-5 relative to intensity) and accuracy (5'10-4 relative to intensity) place strong constraints on the polarization analysis and calibration units. Consequently, these systems are provided at the facility level, rather than making it part of the requirement for each instrument. Title: Improving Ocean Analyses and ENSO Forecasts at NOAA Using the Global Ocean Data Assimilation System and Altimetric Sea Level Authors: Lillibridge, J.; Behringer, D.; Xue, Y.; Kuhn, J. Bibcode: 2005ESASP.572E.139L Altcode: 2005eers.sympE.139L No abstract at ADS Title: Light-Weight Local Group Dwarf Spheroidal Galaxies Authors: Kuhn, J. R.; Kocevski, D.; Fleck, J. -J. Bibcode: 2004ASPC..327..150K Altcode: 2003astro.ph..9207K A simple and natural explanation for the dynamics and morphology of the Local Group Dwarf Spheroidal galaxies, Draco (Dra) and Ursa Minor (UMi), is that they are weakly unbound stellar systems with no significant dark matter component. A gentle, but persistent, Milky Way (MW) tide has left them in their current kinematic and morphological state. This short paper reviews the parametric tidal interaction model which accounts for their behavior and discusses new statistical evidence from the observed stellar distribution in Dra which implies that its total mass is not dominated by collisionless dark matter (DM). Title: The Lyot project: toward exoplanet imaging and spectroscopy Authors: Oppenheimer, Ben R.; Digby, Andrew P.; Newburgh, Laura; Brenner, Douglas; Shara, Michael; Mey, Jacob; Mandeville, Charles; Makidon, Russell B.; Sivaramakrishnan, Anand; Soummer, Remi; Graham, James R.; Kalas, Paul; Perrin, Marshall D.; Roberts, Lewis C., Jr.; Kuhn, Jeffrey R.; Whitman, Kathryn; Lloyd, James P. Bibcode: 2004SPIE.5490..433O Altcode: Among the adaptive optics systems available to astronomers, the US Air Force Advanced Electro-Optical System (AEOS) is unique because it delivers very high order wave front correction. The Lyot Project includes the construction and installation of the world"s first diffraction-limited, optimized coronagraph that exploits the full astronomical potential of AEOS and represents a critical step toward the long-term goal of directly imaging and studying extrasolar planets (a.k.a. "exoplanets"). We provide an update on the Project, whose coronagraph saw first light in March 2004. The coronagraph is operating at least as well as predicted by simulations, and a survey of nearby stars has begun. Title: On the Constancy of the Solar Diameter. II. Authors: Kuhn, J. R.; Bush, R. I.; Emilio, M.; Scherrer, P. H. Bibcode: 2004ApJ...613.1241K Altcode: The Michelson Doppler Imager instrument on board SOHO has operated for most of a solar cycle. Here we present a careful analysis of solar astrometric data obtained with it from above the Earth's turbulent atmosphere. These data yield the most accurate direct constraint on possible solar radius variations on timescales from minutes to years and the first accurate determination of the solar radius obtained in the absence of atmospheric seeing. Title: Coronal Magnetic Field Measurements Authors: Lin, H.; Kuhn, J. R.; Coulter, R. Bibcode: 2004ApJ...613L.177L Altcode: A long-standing solar problem has been to measure the coronal magnetic field. We believe it determines the coronal structure and dynamics from the upper chromosphere out into the heliospheric environment. It is only recently that Zeeman splitting observations of infrared coronal emission lines have been successfully used to deduce the coronal magnetic flux density. Here we extend this technique and report first results from a novel coronal magnetometer that uses an off-axis reflecting coronagraph and optical fiber-bundle imaging spectropolarimeter. We determine the line-of-sight magnetic flux density and transverse field orientation in a two-dimensional map with a sensitivity of about 1 G with 20" spatial resolution after 70 minutes of integration. These full-Stokes spectropolarimetric measurements of the forbidden Fe XIII 1075 nm coronal emission line reveal the line-of-sight coronal magnetic field 100" above an active region to have a flux density of about 4 G. Title: Evidence for Light-weight Local Group Dwarf Spheroidal Galaxies Authors: Kuhn, J. R.; Kocevski, D. Bibcode: 2004IAUS..220..365K Altcode: Local Group dwarf spheroidal (dS) galaxies are a testing ground for dark matter dominated models of galaxy structure formation and dynamical evolution. Using Keck HIRES kinematic data CFHT deep wide-field photometry and a new analysis of a Mathieu equation description of parametric tidal interactions we demonstrate that these galaxies are unlikely to be in dynamical equilibrium. The data and models imply that dS dynamics and morphology are controlled by multiple perigalacticon orbit passes in mildly elliptical Milky Way orbits. Title: Latest Results from the ATST Site Survey Authors: Hill, F.; Collados, M.; Navarro, H.; Beckers, J.; Brandt, P.; Briggs, J.; Brown, T.; Denker, C.; Hegwer, S.; Horst, T.; Komsa, M.; Kuhn, J.; Lin, H.; Oncley, S.; Penn, M.; Rimmele, T.; Soltau, D.; Streander, K. Bibcode: 2004AAS...204.6909H Altcode: 2004BAAS...36..795H We present the latest results and current status of the site survey portion of the Advanced Technology Solar Telescope (ATST) project. The ATST will provide high resolution solar data in the visible and IR. The site is a major factor determining the performance of the telescope. The most critical site characteristics are the statistics of daytime seeing quality and sky clarity. These conditions are being measured by a suite of instruments at three sites (Big Bear, Haleakala, La Palma). These sites were chosen from a set of six that have been tested starting in November 2001. The instrumentation includes a solar differential image motion monitor, an array of scintillometers, a miniature coronagraph, a dust monitor, and a weather station. The analysis of the data provides an estimate of the seeing as a function of height near the ground. We will present the latest results of the analysis of the survey data set. Title: On the Constancy of the Solar Diameter Authors: Kuhn, J. R.; Bush, R.; Emilio, M.; Scherrer, P. Bibcode: 2004AAS...204.8801K Altcode: 2004BAAS...36..819K The solar radius and its variation have now been measured during most of a solar cycle from the Solar and Heliospheric Observatory, using the Michelson Doppler Imager. These instruments provide unique astrometric data from above the Earth's atmosphere. A new analysis based on MDI data yields a refined measurement of the solar radius and no evidence of secular or solar cycle size variations. Title: The New Solar Telescope at Big Bear Solar Observatory Authors: Denker, C.; Marquette, W. H.; Varsik, J.; Wang, H.; Goode, P. R.; Moretto, G.; Kuhn, J.; Coulter, R. Bibcode: 2004AAS...204.6908D Altcode: 2004BAAS...36R.795D The New Solar Telescope (NST) at Big Bear Solar Observatory is the replacement of the current 65 cm vacuum telescope. We present the optical design of this novel off-axis telescope with a 1.6 m clear aperture. The NST has been designed to exploit the excellent seeing conditions at a lake-site observatory and provide data with a spatial resolution close the telescope's diffraction limit from the visible to the near-infrared (NIR) wavelength region. The post-focus instrumentation is located in the Coudé-room, a new optical laboratory below the observing floor, which also hosts a high-order adaptive optics system. The main instruments are two imaging spectro-polarimeters for visible and NIR observations and a real-time image reconstruction system for visible-light multi-color photometry. This unique combination of instruments will realize its full potential in the studies of active region evolution and space weather forecasts. Title: Title Requested Authors: Lin, H.; Kuhn, J. R.; Coulter, R. Bibcode: 2004AAS...204.9807L Altcode: 2004BAAS...36Q.985L A critical problem for understanding the solar corona has been to measure its magnetic field that we believe determines its structure and dynamics from the upper chromosphere out into the heliospheric environment. The direct measurement of this field has been a longstanding problem. Only recently have Zeeman splitting observations of infrared coronal emission lines (Lin et al. 2000) been used to deduce the coronal magnetic flux density. We have extended this technique and report here our first results from a novel coronal magnetometer that uses an off-axis reflecting coronagraph (SOLARC) and optical fiber-bundle imaging spectropolarimeter (OFIS). Our results reveal the line-of-sight magnetic flux density with a sensitivity of a few gauss with 20 arcsec spatial resolution and approximately 60min temporal resolution. These full Stokes spectropolarimetric data of the forbidden FeXIII emission line at 1075nm imply a line-of-sight coronal magnetic field above an active region with a flux density of 9G. Although these first results from SOLARC/OFIS have relatively coarse resolution, they have potential for solving our coronal "dark energy" problem with infrared magnetometry. This research has been supported by the Multidisciplinary University Research Initiative (MURI) of the DOD, NASA, and the National Science Foundation Atmospheric Research Program. Title: Irradiance and solar cycle variability: clues in cycle phase properties Authors: Kuhn, J. R. Bibcode: 2004AdSpR..34..302K Altcode: We see solar cycle-related variations in almost every coronal, chromospheric, and photospheric measurement obtained over a several-years timescale. With such an abundant observational foundation, we should expect our physical models of the solar cycle to be overconstrained. In fact this is not the case and the "standard dynamo model" is not predictive. This paper describes some new thoughts on how solar irradiance variations may provide clues to the solar cycle regulation mechanism near the radiative-convection zone boundary. Title: Fundamentals of the Solar Interior and Atmosphere Authors: Kuhn, Jeffrey R.; McCormack, John Bibcode: 2004GMS...141....3K Altcode: The practical, and immediately useful, questions related to predicting how terrestrial climate may change are completely dependent on the theoretical (and perhaps more fundamental) questions about how the solar cycle varies—what causes it, and how it changes the solar outputs which affect the Earth. For example, we obviously don't have a chance of accurately predicting whether the next solar cycle will be dangerously high or low if we don't have a useful physical model for it.

As we have learned from decades of solar-terrestrial research, it is not easy to find a "useful physical" model of the solar cycle. Here "useful" is synonymous with "predictive." Until recently we've only been able to view the cycle using magnetic observables with retrospective models. Interestingly, over about the last cycle, we have developed new accurate photometric and helioseismic tools. These photometric and acoustic observables hold the promise of finally elucidating the solar cycle physics. Title: Solar Variability and its Effects on Climate. Geophysical Monograph 141 Authors: Pap, Judit M.; Fox, Peter; Frohlich, Claus; Hudson, Hugh S.; Kuhn, Jeffrey; McCormack, John; North, Gerald; Sprigg, William; Wu, S. T. Bibcode: 2004GMS...141.....P Altcode: This monograph presents a state-of-the-art description of the most recent results on solar variability and its possible influence on the Earth's climate and atmosphere. Our primary goal in doing so is to review solar energy flux variations (both electromagnetic and particle) and understand their relations to solar magnetic field changes and global effects, their impact on different atmospheric layers, and—as a collaboration of scientists working on solar-terrestrial physics—to note unresolved questions on an important interdisciplinary area.

One of the highest-level questions facing science today is whether the Earth's atmosphere and climate system changes in a way that we can understand and predict. The Earth's climate is the result of a complex and incompletely understood system of external inputs and interacting parts. Climate change can occur on various time scales as a consequence of natural variability—including solar variability—or anthropogenic causes, or both. The Sun's variability in the form of sunspots and related magnetic activity has been the subject of careful study ever since the earliest telescopic observations. High precision photometric observations of solar-type stars clearly show that year-to-year brightness variations connected with magnetic activity are a widespread phenomenon among such stars. As our nearest star, the Sun is the only star where we can observe and identify a variety of structures and processes which lead to variations in the solar energy output, in both radiative and particle fluxes. Studying event tiny changes in solar energy flux variations may teach us about internal processes taking place in the Sun's convective zone and below. Title: Solar variability and climate changes Authors: Labitzke, K.; Pap, J.; Kuhn, J. R.; Shea, M. A. Bibcode: 2004AdSpR..34..227L Altcode: No abstract at ADS Title: On the constancy of the solar radius Authors: Kuhn, J.; Bush, R.; Emilio, M.; Scherrer, P. Bibcode: 2004cosp...35.1918K Altcode: 2004cosp.meet.1918K The MDI experiment aboard SOHO has operated for most of a solar cycle. From it we have obtained the most sensitive constraints on possible solar radius variations and changes in the solar limb darkening function over a solar cycle timescale. Here we describe the new measurements and their implications for our understanding of the mechanisms of solar cycle variability. Title: Preface Authors: Pap, Judit M.; Fox, Peter; Fröhlich, Claus; Hudson, Hugh S.; Kuhn, Jeffrey; McCormack, John; North, Gerald; Sprigg, William; Wu, S. T. Bibcode: 2004GMS...141D...7P Altcode: This monograph presents a state-of-the-art description of the most recent results on solar variability and its possible influence on the Earth's climate and atmosphere. Our primary goal in doing so is to review solar energy flux variations (both electromagnetic and particle) and understand their relations to solar magnetic field changes and global effects, their impact on different atmospheric layers, and—as a collaboration of scientists working on solar-terrestrial physics—to note unresolved questions on an important interdisciplinary area.

One of the highest-level questions facing science today is whether the Earth's atmosphere and climate system changes in a way that we can understand and predict. The Earth's climate is the result of a complex and incompletely understood system of external inputs and interacting parts. Climate change can occur on various time scales as a consequence of natural variability—including solar variability—or anthropogenic causes, or both. The Sun's variability in the form of sunspots and related magnetic activity has been the subject of careful study ever since the earliest telescopic observations. High precision photometric observations of solar-type stars clearly show that year-to-year brightness variations connected with magnetic activity are a widespread phenomenon among such stars. As our nearest star, the Sun is the only star where we can observe and identify a variety of structures and processes which lead to variations in the solar energy output, in both radiative and particle fluxes. Studying even tiny changes in solar energy flux variations may teach us about internal processes taking place in the Sun's convective zone and below. Title: Mechanisms of Solar Irradiance Variations Authors: Kuhn, J. R.; Armstrong, J. D. Bibcode: 2004GMS...141...87K Altcode: This section discusses how measurements of the Sun's surface brightness may be used to determine its total emergent flux. We explore how solar luminosity and irradiance changes are related but distinct phenomena, which are not well treated in one-dimensional or diffusive solar convection zone models. Efforts to improve our knowledge of the solar luminosity are essential, since a refined understanding of the variability of the total solar luminosity, or even of the net emergent energy flux from isolated parts of the photosphere are critical tools for understanding the physics of the convection zone and for probing deeper into the solar interior. In combination with magnetic, helioseismic, and numerical simulation observations and tools, the global solar luminosity and irradiance variability can reveal much about the mechanisms of the solar cycle. Title: The HAWAII-2 2048×2048 HgCdTe Detector Arrays Authors: Hodapp, K. W.; Kuhn, J.; Thornton, R.; Irwin, E.; Yamada, H.; Waterson, M.; Kozlowski, L.; Montroy, J. T.; Haas, A.; Vural, K.; Cabelli, C. Bibcode: 2004ASSL..300..501H Altcode: 2004sdab.conf..501H This paper discusses the design and testing of the new HAWAII-2 devices. The HAWAII-2 design is largely based on the very successful HAWAII-1 devices developed by Rockwell, but with an extended detector array size of 2048×2048. The device was designed for use in the AEOS spectrograph, a cross-dispersed spectrograph intended to cover a large spectral range in a single exposure, therefore, array size was of paramount importance. Title: The New 1.7 m Off-Axis Solar Telescope (NST) Project: a Path to Better Solar Science Authors: Goode, P. R.; Didkovsky, L. V.; Kuhn, J. Bibcode: 2003AGUFMSH42B0532G Altcode: Big Bear Solar Observatory (BBSO) of New Jersey Institute of Technology is upgrading its 65 cm aperture vacuum telescope with a modern, off-axis 1.6 m clear aperture instrument - New Solar Telescope (NST). The NST offers a significant incremental improvement in ground-based infrared and visible light high angular resolution capabilities. It will fully utilize the optical and dynamical range advantages of its unobstructed (off-axis) pupil. The NST enhances our continuing program to understand photospheric magneto-convection and chromospheric dynamics. This new telescope will be the largest aperture solar telescope, and the largest aperture off-axis telescope located in one of the best observing sites. It will enable new, cutting edge science. Title: The Lyot Project: Toward Exoplanet and Circumstellar Disk Imaging and Spectroscopy Authors: Oppenheimer, B. R.; Digby, A. P.; Shara, M.; Brenner, D.; Newburgh, L.; Makidon, R. B.; Sivaramakrishnan, A.; Soummer, R.; Graham, J. R.; Kalas, P.; Perrin, M.; Kuhn, J. R.; Whitman, K.; Lloyd, J. P. Bibcode: 2003AAS...20313604O Altcode: 2004BAAS...36Q.583O We present the opto-mechanical design, expected performance, and a progress report on the Lyot Project's new near-infrared coronagraph designed and optimized to operate in tandem with the Advanced Electro-Optical System at the Maui Space Surveilance System. This coronagraph includes a number of novel features, such as active optical alignment and a second stage tip/tilt loop. The in-lab construction is nearly complete. We expect first light in March 2004, when we will commence a survey for extremely faint objects, such as brown dwarfs and large planets, and disks orbiting nearby stars. This instrument will be more sensitive, by almost a factor of ten, than any other existing instrument in the .2 to 1.5 arcsec range of separations from the target stars.

The Lyot Project is funded by two grants from the National Science Foundation. The US Air Force provides telescope time, on-site support and 80% of the research funds for one of the grants. The Project also benefits from the generosity of the American Museum of Natural History's patrons. Title: Thermal IR Prospects for Coronal Magnetic Field Measurement Authors: Kuhn, J. R.; Coulter, R. Bibcode: 2003AGUFMSH41D..06K Altcode: The SOLARC Haleakala reflecting coronagraph was designed and built for studying the IR solar corona. High dynamic range imaging and spectroscopy in the thermal IR offers unique prospects for coronal field measurements. Here we summarize the interesting opportunities, our progress and results toward this goal. Title: Solar Radius Observer Satellite (SoROS) Authors: Emilio, M.; Leister, N. V.; Teixeira, R.; Benevides-Soares, P.; Kuhn, J. Bibcode: 2003ala..conf..177E Altcode: It is known a long time ago that the Sun presents variations. The most obvious of the manifestations is the variation of the solar spots in his surface. With the invention of the telescope around 1600 regular observations, but no systematic, of the solar surface began to be done by several observatories in Europe. The manifestations of the activity cycle in the production of solar energy are associated to the solar wind, to the emission of particles and the magnetic fields on the solar surface. While the energy of the solar wind is negligible compared to the energy in the ultraviolet and in the visible, the relative variations are significantly larger. But can those small fluctuations of energy affect the climate? This mission aim to measure solar shape and radius to test models to explain the variation of solar energy, help to determine Sun's gravitational potential and its internal rotational and for the first time, measure gmodes oscillations frequencies. Title: Um satélite brasileiro para observação do diâmetro solar Authors: Emilio, M.; Leister, N. V.; Benevides Soares, P.; Teixeira, R.; Kuhn, J. Bibcode: 2003BASBr..23..198E Altcode: Propomos uma missão espacial para medir a forma e o diâmetro solar com o objetivo de ajudar a determinar o potencial gravitacional do Sol e a sua rotação com precisão, testar modelos teóricos de variação de energia e pela primeira vez medir os modos g de oscilação. As observações serão obtidas através do instrumento denominado APT (Astrometric and Photometric Telescope) descrito por Kuhn(1983). A sensibilidade do instrumento é de 0,2 mas em 27 dias para as observações do diâmetro solar feitas a cada minuto. Esta é uma missão de três anos de duração e pode complementar as medidas que serão feitas pelo satélite PICARD (a ser lançado em 2007). Outros parâmetros físicos podem ser obtidos com as mesmas imagens o que certamente interessará à comunidade de física solar. Um primeiro contato foi realizado com a agência espacial brasileira que pretende lançar um satélite científico a cada dois anos. Title: Parametric Dwarf Spheroidal Tidal Interaction Authors: Fleck, Jean-Julien; Kuhn, J. R. Bibcode: 2003ApJ...592..147F Altcode: 2003astro.ph..2463F The time-dependent tidal interaction of the Local Group dwarf spheroidal (dSph) galaxies with the Milky Way (MW) can fundamentally affect their dynamical properties. The model developed here extends earlier numerical descriptions of dSph-MW tidal interactions. We explore the dynamical evolution of dSph systems in circular or elliptical MW orbits in the framework of a parametric oscillator. An analytic model is developed and compared with more general numerical solutions and N-body simulation experiments. Title: 1.6 M Solar Telescope in Big Bear -- The NST Authors: Goode, Philip R.; Denker, Carsten. J.; Didkovsky, Leonid I.; Kuhn, J. R.; Wang, Haimin Bibcode: 2003JKAS...36S.125G Altcode: No abstract at ADS Title: High Dynamic Range and the Search for Planets Authors: Tokunaga, A. T.; Ftaclas, C.; Kuhn, J. R.; Baudoz, P. Bibcode: 2003IAUS..211..487T Altcode: 2002astro.ph..8328T General arguments for optimized coronagraphy in the search for planets are presented. First, off-axis telescopes provide the best telescopic platforms for use with coronagraphy, and telescope fabrication technology now allows the fabrication of such telescopes with diameters of up to 6.5 m. We show that in certain circumstances a smaller telescope with an off-axis primary has a signal-to-noise advantage compared with larger Cassegrain telescopes. Second, to fully exploit the advantages of the coronagraph for suppressing stray light, it is necessary to use a high Strehl ratio adaptive optics system. This can be best achieved initially with modest aperture telescopes of 3--4 m in diameter. Third, application of simultaneous differential imaging and simultaneous polarimetric techniques are required to reach the photon-limit of coronagraphic imaging. These three developments, if pursued together, will yield significant improvements in the search for planets. Title: The J- and K-Band Brightness of the Solar F Corona Observed during the Solar Eclipse on 1998 February 26 Authors: Ohgaito, R.; Mann, I.; Kuhn, J. R.; MacQueen, R. M.; Kimura, H. Bibcode: 2002ApJ...578..610O Altcode: We analyze J- and K-band observations of the 1998 solar eclipse and derive the F-corona brightness in the K band between 3 and 7 Rsolar from the center of the Sun and in the J band out to 5 Rsolar. The falloff in the K-band brightness from 3 to 7 Rsolar is fitted with a radial power law with exponent -2.4+/-0.1 at the solar equator and with exponent -2.9+0.2-0.1 at the solar pole. This slope is gentler than that derived from observations in 1983 but is steeper than that derived from observations for the 1991 eclipse. The radial profiles agree well with models that explain the F corona with weakly absorbing dust particles. Comparison of the J- and K-band brightness at 3 Rsolar from the center of the Sun indicates a reddening of the F corona with respect to the solar spectrum. The reddening is, however, less pronounced compared to the F corona observed during the 1983 total solar eclipse. This fact may be attributed to a change in the composition of dust near the Sun. As with the radial profiles, the reddening in 1998 is better explained with models that assume weakly absorbing rather than strongly absorbing dust particles in the solar corona. Similar to recent eclipse observations, we do not detect an excess emission feature of near-solar dust in the F corona. We hence can reject the hypothesis that suggests a correlation between the detection of an emission feature and the solar activity cycle. Title: Sunspot bright rings - a probe into thermal conduction in the solar convection zone Authors: Armstrong, J. D.; Kuhn, J. R. Bibcode: 2002AAS...200.9102A Altcode: 2002BAAS...34..953A The conductivity derived from mixing length theory has often been used as an arguement that energy which one might consider "blocked" by a sunspot, is quickly distributed through out the convection zone and radiated over the thermal times scale of the convection zone. In a complimentary view, facular regions are thought of as bright regions which draw upon the thermal reserves of the entire convection zone. We examine the bright rings seen around sunspots, and by comparing to simple conductive models show that thermal perterbations in convective regions do not behave in this manner. Title: Solar Irradiance Variations over Solar Cycles 21 to 23 Authors: Pap, J. M.; Kuhn, J.; Jones, H.; Turmon, M.; Arge, N.; Schmutz, W.; Floyd, L. Bibcode: 2002AAS...200.2803P Altcode: 2002BAAS...34..679P In this paper we describe the science requirements and a new measurement strategy to better understand solar variability and its potential effect on climate. We study the relation between the variations in solar total and UV irradiances and solar magnetic fields as observed within the last three decades. The results of our analysis raise important questions: (1) is there a significant non-magnetic component in the observed irradiance variations?; (2) may polar magnetic fields play a role in irradiance changes?; (3) is there a strict linear relationship between solar variability and irradiance variations as the current irradiance models used in climate studies assume? The results presented in this paper underscore the need to further develop new measurement and analysis techniques to study and predict the climate impact of solar variability. Title: The Solar Cycle as a Delayed Oscillator Authors: Kuhn, J. R.; Armstrong, J. D. Bibcode: 2002AAS...200.8905K Altcode: 2002BAAS...34R.791K Solar luminosity and irradiance variations provide an important constraint on the physics of the solar cycle. Starting from magnetic flux-transport models of the solar cycle it is possible to reproduce many of the features of the magnetic, irradiance, and acoustic solar cycle observables. This talk will describe how a ``delayed oscillator" model could explain the magnetic cycle. Title: Long-term solar irradiance variations: results and perspectives Authors: Pap, J.; Fleck, B.; Frohlich, C.; Jones, H.; Kuhn, J.; Schmutz, W. Bibcode: 2002cosp...34E.553P Altcode: 2002cosp.meetE.553P In this paper we show the recent result on irradiance variations and their relation to solar magnetic activity over solar cycles 21 to 23. Comparison of the multi-decade long irradiance and magnetic field measurements indicates that the shape and magnitude of irradiance variations are different from that of magnetic indices. Specifically, while magnetic indices show that solar cycle 23 is weaker than the two previous cycles, the long-term variation of total solar irradiance over solar cycles 21 to 23 is rather symmetrical, showing that its maximum and minimum levels were about the same within their measuring uncertainties. These results raise questions like: (1) is there a strict linear relationship between solar variability and irradiance variations as the current irradiance models used in climate studies assume?; (2) what is the role of polar magnetic fields in irradiance changes?; (3) is there a significant non-magnetic component in the observed irradiance variations? The results presented in this paper underscore the need to further develop new measurement and analysis techniques to study and predict the climate impact of solar variability. Title: Solar radius variations over the solar cycle: ground and space experiments Authors: Emilio, M.; Leister, N.; Kuhn, J.; Bush, R.; Benevides-Soares, P. Bibcode: 2002cosp...34E2798E Altcode: 2002cosp.meetE2798E An astrolabe observational program at São Paulo measures the solar radius since 1974. Several ground experiments, including astrolabes, show correlations between solar radius and solar magnetic activit. A curious fact is that some measures in the ground show amplitude of the order of 0.1 sec during the solar cycle. Theoretical forecasts, heliosismologic observations and measurements made with SOHO satellite shows that the amplitude of the radius variation must be of at least one magnitude order lower. Would be these instruments measuring a variation of the terrestrial atmosphere instead variation of the solar radius? Errors of atmospheric refraction using astrolabes are of second order. Theoretically, the first order errors vanish doing the subtraction of the zenithal distances between upper and lower solar limbs. Those of second order include possible variations of atmospheric refraction in the interval of contact of each limb that are about of 4 minutes. Could the atmospheric turbulence vary during the solar cycle and explain the amplitude of the variation observed in the radius made by the ground experiments? It is known that the solar magnetic cycle intervenes with our atmosphere but still there is not a model describing in details how this variation happens. We present hear a study about the divergences among the space and ground experiments. Title: Physical mechanisms of the irradiance solar cycle Authors: Kuhn, J.; Armstrong, J. Bibcode: 2002cosp...34E.695K Altcode: 2002cosp.meetE.695K Despite more than two decades of satellite solar irradiance observations we are unable to answer important questions like, could the next solar cycle be three times larger than the current? Basic questions like, is the cycle phase-amplitude variability a consequence of strongly non-linear chaotic behavior or does the cycle result from stochastic driving of a weakly non-linear system? (as Babcock and Leighton suggested many years ago), have not been resolved. Finding a physical model which simultaneously accounts for the Sun's photometric and magnetic variability may be key to answering these questions. This paper explores the physical connections between the global solar cycle and the physical mechanisms of irradiance and magnetic variability. Title: Concepts for a Large-Aperture, High Dynamic Range Telescope Authors: Kuhn, J. R.; Moretto, G.; Racine, R.; Roddier, F.; Coulter, R. Bibcode: 2001PASP..113.1486K Altcode: This paper summarizes concept studies for a large telescope capable of wide-field imaging and of the highest possible dynamic range for photometry and angular resolution. Point-spread functions (PSFs) and scattered light levels at large offsets are computed and compared for four telescopes of the same light-gathering power but with different pupil functions:1. a reference monolithic mirror telescope with a 17.4 m primary,2. a segmented mirror telescope (SMT) with a hexagonally segmented primary,3. a hexagonal off-axis telescope (HOT) with a distributed aperture made of 6×6.5 m unobstructed circular mirrors that are identical off-axis sections of a parent 20 m mirror, and4. a square off-axis telescope (SOT) whose aperture is made of 4×8 m off-axis mirrors. The characteristics of the PSFs are examined in the diffraction- and seeing-limited regimes, assuming (1) perfect mirror figure and (2) realistic figure errors (edge defects). The implications of field rotation with an altitude-azimuth mounting are discussed in each case. The implementation of adaptive optics (AO) and the properties of AO-compensated PSFs having a Strehl ratio of 0.5, and of coronagraphic imaging, are also discussed for the four configurations. It is shown that, in the seeing-limited regime and as intuitively expected, the optical performance of all four telescopes is comparable. With higher order adaptive optics and for coronagraphic observations, the SOT and HOT are superior to the SMT. This distinction becomes larger with relaxed constraints on mirror edge-polishing requirements. A full optical design is presented for the novel HOT configuration, and optical fabrication issues are briefly addressed. Finally, science programs and possible instrumentation layouts with the HOT are briefly explored for different modes of operation. It appears that the natural ``optical bench'' configuration of the HOT can provide a remarkably versatile and convenient environment for instrument deployment. Title: Solar Radius Observations by the Michelson Doppler Imager Authors: Bush, R. I.; Chu, K.; Kuhn, J. R. Bibcode: 2001AGUFMSH11B0715B Altcode: The Michelson Doppler Imager (MDI) instrument on the SOHO spacecraft is approaching the completion of six years of observing the Sun. During this period, full disk continuum images with 4 arc-second resolution have been taken at a cadence of at least four images per day. Because of the absence of atmospheric blurring and the stable environment of the L1 halo orbit, these images provide a long term measurement of the solar limb. The determination of changes in the solar radius from these images is affected by both an annual thermal variation in the MDI front entrance window and by a slow shift in the instrument focus due to aging of the entrance bandpass filter. These effects are being modeled in order to determine an estimate of the solar cycle variation in the solar radius. This research is supported by NASA grant NAG5-10483 at Stanford University. Title: Erratum: He I 10830 Å Line Polarimetry: A New Tool to Probe the Filament Magnetic Fields Authors: Lin, Haosheng; Penn, Matt J.; Kuhn, Jeffrey R. Bibcode: 2001ApJ...560..534L Altcode: In the paper ``He I 10830 Å Line Polarimetry: A New Tool to Probe the Filament Magnetic Fields'' by Haosheng Lin, Matt J. Penn, and Jeffrey R. Kuhn (ApJ, 493, 978 [1998]), several mathematical and typographical errors escaped the authors' attention. These are mostly errors in the scaling factor of the expressions, however, and they did not affect the results of the paper. 1. There was an error in the scaling factor in the right-hand side of equation (4). The correct expression for equation (4) should be ES(r,ω,t)=-e(ω/c)2 (e-i(ωt-k˙r))/r × r×x(ω) . This error propagated into the paper and affected several equations derived later on. First, the correct expression for equation (33) (and eq. [A24]) should be N(ω)~((ω0)/2m)(e/c)21)/ (ω0-ω)+iΓ/2) Accordingly, the correction expressions for equations (34), (35), and (36) are NN*=1/4((ω0)/m)2(e/c)4 1/(ω0-ω)2+(Γ/2)2), Re(iNN*)=1/4((ω0)/m)2 ((e/c)4Γ/2)/[(ω0-ω)2+ (Γ/2)2]2, Im(iNN*)=1/4((ω0)/m)2 (e/c)40-ω)/[(ω0- ω)2+(Γ/2)2]2 Similarly, this correction should be applied to the coefficient of equations (A25), (A26), and (A37). That is, the factor (eω0/2m)2 in equations (A25), (A25), and (A37) should be replaced by (1/4)(ω0/m)2(e/c)4. Finally, the correct expressions for the Doppler-broadened profiles h(a,v), k(a,v), and f(a,v) in equations (39), (40), and (41) should be h(a,v)=3/8(sqrt(π)e2)/mc 1/(▵ωD) a/πΣ-∞ (e-y^2dy)((v-y)2+a2) = 3/8(sqrt(π)e2)/mc 1/(▵ωD) H(a,v), k(a,v)=3/4(sqrt(π)e2)/mc 1/(▵ω2D) (a2)/πΣ-∞ (e-y^2dy)([(v-y)2+a2]2), f(a,v)=3/4(sqrt(π)e2)/mc 1/(▵ω2D) πΣ-∞ ((v-y)e-y^2dy)([(v-y)2+a2]2. 2. The h2 factor in equations (17), (22), and (23) should be removed. 3. The sentence after equation (7) should read ``The oscillator solution can be written as X(ω)=e-1(ω/c)-2NEI.'' Title: Imaging Polarimetric Observations of a New Circumstellar Disk System Authors: Kuhn, J. R.; Potter, D.; Parise, B. Bibcode: 2001ApJ...553L.189K Altcode: 2001astro.ph..5239K Few circumstellar disks have been observed directly. Here we use sensitive differential polarimetric techniques to overcome atmospheric speckle noise in order to image the circumstellar material around HD 169142. The detected envelope or disk is considerably smaller than expectations based on the measured strength of the far-IR excess from this system. Title: Physical Mechanisms of Solar Irradiance and Luminosity Variations Authors: Kuhn, J. R. Bibcode: 2001AGUSM..SP31B05K Altcode: The solar irradiance and luminosity changes observed over the last two decades measure distinct physical mechanisms, each triggered differently by solar magnetic fields. The irradiance fluctuations, associated with sunspots and bright faculae, are more aptly described as extremes from a range of magnetic perturbations which includes the magnetic network. We use accurate photometry from the ground and space to illustrate this and to show how proxy measurements using CaII K or magnetic flux density data can go awry while trying to identify the mechanisms of solar variability. Very precise, spatially resolved, solar surface brightness observations are a critical tool for understanding stellar convection, and in particular how the base of the convection zone evolves with the solar magnetic cycle. It is likely that our understanding and ability to predict the importance of solar irradiance variations, for example, for the terrestrial climate system, will depend on future surface brightness data of similar and improved accuracy. Title: Coronagraphy with the AEOS High Order Adaptive Optics System Authors: Lloyd, J. P.; Graham, J. R.; Kalas, P.; Oppenheimer, B. R.; Sivaramakrishnan, A.; Makidon, R. B.; Macintosh, B. A.; Max, C. E.; Baudoz, P.; Kuhn, J. R.; Potter, D. Bibcode: 2001AAS...198.7703L Altcode: 2001BAAS...33Q.902L Adaptive Optics has recently become a widely used technique to acquire sensitive, diffraction limited images in the near infrared with large ground based telescopes. Most astronomical targets are faint; driving astronomical AO systems towards large subapertures; resulting in a compromise between guide star brightness, observing wavelength, resolution and Strehl ratio. Space surveilance systems have recently been developed that exploit high order adaptive optics systems to take diffraction limited images in visible light on 4 meter class telescopes on bright (V<8) targets. There is, however, a particular niche that can be exploited by turning these visible light space surveillance systems to astronomical use at infrared wavelengths. At the longer wavelengths, the strehl ratio rises dramatically, thus placing more light into the diffracted Airy pattern at the expense of the atmospheric halo. A coronagraph can be used to suppress the diffracted light, and observe faint companions and debris disks around nearby, bright stars. Observations of these very high contrast objects benefit greatly from much higher order adaptive optics systems than are presently available to the astronomical commnunity. The National Science Foundation and Air Force Office of Scientific Research is sponsoring a program to conduct astronomical observations at the AEOS facility. We are presently developing an astronomical coronagraph to be deployed at the Air Force AEOS facility. We describe the coronagraph, and discuss the advantages and limitations of ground based high order AO for high contrast imaging. Title: An Off-axis Telescope Concept for High Contrast Imaging Authors: Tokunaga, A. T.; Kuhn, J.; Baudoz, P.; Coulter, R.; Rayner, J.; Toomey, D.; Moretto, G. Bibcode: 2001AAS...198.7710T Altcode: 2001BAAS...33..903T A telescope concept is proposed to undertake studies of Kuiper Belt Objects, Near-Earth Objects, and circumstellar disks and extra-solar planets. These diverse scientific objectives require capabilities ranging over wide-field imaging, high angular resolution, high sensitivity in the optical and thermal infrared, and superb photometric dynamic range. It is possible to achieve all of these performance requirements using a 6.5m unobstructed, off-axis telescope. Unique features include optimization for unprecedented low scattered light and high dynamic range astronomy, extremely low infrared emissivity, and innovative instruments uniquely designed to take full advantage of these capabilities, such as coronagraphic instruments. Title: Limits on Lyot coronagraphy with AEOS adaptive optics telescope Authors: Sivaramakrishnan, A.; Makidon, R. B.; Lloyd, J. P.; Oppenheimer, B. R.; Graham, J. R.; Kalas, P. G.; Macintosh, B. A.; Max, C. E.; Baudoz, P.; Kuhn, J.; Potter, D. Bibcode: 2001AAS...198.7705S Altcode: 2001BAAS...33..902S The 3.6m Air Force Electo-Optical System telescope is the most advanced adaptive optics (AO) system available to the astronomical community. Its 941-channel AO system feeds several stable instrument platforms at a very slow Cassegrain focus. Its small secondary obscuration makes it ideal for AO coronagraphy. We present estimates of current and theoretical limits on dynamic range using a diffraction-limited Lyot coronagraph optimized for the 3.6m AEOS telescope. We incorporate both the effects of imperfect AO correction of the wavefront and telescope guiding errors in our simulations. We calculate limits on faint companion detection (in the H-band) for this system at separations between 0.36 and 1.3 arcseconds. Title: One solar cycle later: reflections and speculations on directions in helio- and asteroseismology in a new millennium Authors: Kuhn, J. R. Bibcode: 2001ESASP.464....7K Altcode: 2001soho...10....7K This talk reflects on our progress since the last helioseismology symposium held here in Tenerife over one solar cycle ago. While even a superficial inspection shows that the last decade of seismic investigation of the Sun and other stars has been enormously revealing - it appears that new observations are generating new questions at a faster rate than our ability to solve old problems. Here we briefly review some of this progress, and highlight questions and research directions that might possibly be described at the next Tenerife helioseismology meeting. Title: MDI-SOHO Measures of Solar Radius Variation Authors: Emilio, M.; Kuhn, J. R.; Bush, R. I.; Scherrer, P. Bibcode: 2001IAUS..203..101E Altcode: Why does the solar luminosity vary and could it change on human timescales by enough to affect terrestrial climate? As important as these questions are, we lack answers because we do not understand the physical mechanisms which are responsible for the solar irradiance cycle. Progress here depends on discovering how changes in the solar interior affect energy flow from the radiative and convection zones out through the photosphere. Measurements of small changes in the solar radius are a critical probe of the Sun's interior stratification and can tell us how and where the solar luminosity is gated or stored. Here we report results from a sensitive 3 year satellite experiment designed to detect solar diameter fluctuations. Title: Tidal Disruptions of the Ursa Minor and Draco Dwarf Spheroidal Galaxies Authors: Kocevski, D. D.; Kuhn, J. R. Bibcode: 2000AAS...197.3004K Altcode: 2000BAAS...32.1446K Several of the local group dwarf spheroidal (dS) galaxies show evidence of inflated velocity dispersions. A likely model for Ursa Minor, Carina, and Draco is that their tidal interaction with the Milky Way has pushed them far from virial equilibrium. We have obtained wide-field V and I band photometry of the Ursa Minor and Draco dS galaxies using the 12K CCD mosaic detector on the Canada-France-Hawaii telescope. We present here the results of a sensitive search for extratidal stars out to distances of 4 degrees from the centers of these galaxies. We discuss the implications of these results for dark matter and Milky Way tidal interaction models. Title: Using Precise Solar Limb Shape Measurements to Study the Solar Cycle Authors: Kuhn, J. R.; Floyd, L.; Fröhlich, C.; Pap, J. M. Bibcode: 2000SSRv...94..169K Altcode: Despite 20 years of total solar irradiance measurements from space, the lack of high precision spatially resolved observations limits definitive answers to even simple questions like ``Are the solar irradiance changes caused solely by magnetic fields perturbing the radiative flux at the photosphere?" More subtle questions like how the aspheric structure of the sun changes with the magnetic cycle are only now beginning to be addressed with new tools like p-mode helioseismology. Solar 5-min oscillation studies have yielded precise information on the mean radial interior solar structure and some knowledge about the rotational and thermal solar asphericity. Unfortunately this progress has not been enough to generate a self-consistent theory for why the solar irradiance and luminosity vary with the magnetic cycle. We need sharper tools to describe and understand the sun's global aspheric response to its internal dynamo, and we need to be able to measure the solar cycle manifestation of the magnetic cycle on entropy transport from the interior to the photosphere in much the same way that we study the fundamentally more complex problem of magnetic flux transport from the solar interior. A space experiment called the Solar Physics Explorer for Radius, Irradiance and Shape (SPHERIS) and in particular its Astrometric and Photometric Telescope (APT) component will accomplish these goals. Title: A Least-squares Solution for the Effective Conductivity of the Solar Convection Zone Authors: Kuhn, J. R.; Georgobiani, D. Bibcode: 2000SSRv...94..161K Altcode: Here we show how realistic numerical simulations of solar convection can be parameterized with an effective thermal conductivity tensor. We show that this diffusive approximation yields an accurate statistical (in the sense of the χ^2 test) description of the thermal transport properties of a perturbed solar convection zone. This parameterization will allow more accurate large scale solar irradiance and luminosity calculations. Title: On the Constancy of the Solar Diameter Authors: Emilio, M.; Kuhn, J. R.; Bush, R. I.; Scherrer, P. Bibcode: 2000ApJ...543.1007E Altcode: Why does the solar luminosity vary and could it change on human timescales by enough to affect terrestrial climate? As important as these questions are, we lack answers because we do not understand the physical mechanisms responsible for the solar irradiance cycle. Progress here depends on discovering how changes in the solar interior affect energy flow from the radiative and convection zones out through the photosphere. Measurements of small changes in the solar radius are a critical probe of the Sun's interior stratification; they can tell us how and where the solar luminosity is gated or stored. Here we report results from a sensitive 3 yr satellite experiment designed to detect solar diameter fluctuations. Title: Physical Causes of Solar Variability - Discussion Session 1b Authors: Kuhn, J. R.; Schüssler, M. Bibcode: 2000SSRv...94..177K Altcode: This report is divided into three parts: Section 1 gives a short introduction and a summary of the topics discussed. Section 2 is a position statement by J. Kuhn on the interpretation of the irradiance measurements, while Section 3 gives a position statement by M. Schüssler discussing observations of stars that could be useful for understanding solar variability. Title: Solar Interior: Solar Diameter, Oblateness and Temperature Authors: Kuhn, J. Bibcode: 2000eaa..bookE2245K Altcode: The visible edge of the Sun is called the LIMB and is almost circular, but very small deviations from a spherical Sun are measurable. The largest deviation is a `flattening' of the polar radius in comparison to the equatorial solar radius. The Sun's surface temperature is also not spherically symmetric but has a tiny asphericity in the form of a latitudinal temperature variation. The radius, sha... Title: Global Solar Corona Revealed by Time Series Observations Authors: Li, Jing; Kuhn, J.; LaBonte, B.; Raymond, J. C.; Acton, L. W. Bibcode: 2000ApJ...538..415L Altcode: Time series observations at UV (Extreme Ultraviolet Imaging Telescope/Solar and Heliospheric Observatory) and X-ray (Soft X-Ray Telescope/Yohkoh) wavelengths reveal properties of the global solar corona that are not easily identified in a single image. A median-filtering technique that rejects features varying with time is used to isolate background corona. The coronal hole boundaries, polar plumes, and polar rays in the inner corona are clearly seen in Extreme Ultraviolet Imaging Telescope data over 5 months during the last solar minimum (1996 January through May). For the first time, we provide physical evidence for coronal hole boundaries in the inner corona. The observations show clearly that the polar coronal holes expand divergently with height. A simple latitudinal and radial electron density distribution for the inner corona is found. Title: Rossby waves on the Sun as revealed by solar `hills' Authors: Kuhn, J. R.; Armstrong, J. D.; Bush, R. I.; Scherrer, P. Bibcode: 2000Natur.405..544K Altcode: It is a long-standing puzzle that the Sun's photosphere-its visible surface-rotates differentially, with the equatorial regions rotating faster than the poles. It has been suggested that waves analogous to terrestrial Rossby waves, and known as r-mode oscillations, could explain the Sun's differential rotation: Rossby waves are seen in the oceans as large-scale (hundreds of kilometres) variations of sea-surface height (5-cm-high waves), which propagate slowly either east or west (they could take tens of years to cross the Pacific Ocean). Calculations show that the solar r-mode oscillations have properties that should be strongly constrained by differential rotation. Here we report the detection of 100-m-high `hills' in the photosphere, spaced uniformly over the Sun's surface with a spacing of (8.7 +/- 0.6) × 104km. If convection under the photosphere is organized by the r-modes, the observed corrugated photosphere is a probable surface manifestation of these solar oscillations. Title: Development Status of the Microshutter Arrays for the NGST MOS. Authors: Moseley, S. H.; Fettig, R. K.; Kuhn, J.; Kutyrev, A. S.; Li, M.; Mott, D. B.; Schwinger, D. S.; Wesenberg, R. P.; Woodgate, B. E. Bibcode: 2000AAS...196.3216M Altcode: 2000BAAS...32..722M We are developing a two-dimensional array of microshutters that can be used as a high efficiency, high contrast field selection device for a multi-object spectrometer for the Next Generation Space Telescope (NGST). The device is a close-packed array of randomly selectable shutters with a cell size of 100 microns square and area filling factor of about 80% produced in a 100 micrometer thick silicon wafer. Each shutter, made of silicon nitride with an appropriate optical coating, pivots on a torsion flexure along one edge. A CMOS circuit embedded in the frame around the shutters allows independent individual selection. An original double-shutter mechanism is employed for actuation. It has been tested on a small size three by three shutter array. Processing includes anisotropic back etching for wafer thinning, an Inductive Coupled Plasma (ICP) back etch through the silicon to the mechanical active nitride membrane and a Reactive Ion Etching (RIE) to produce the shutters out of the nitride membrane. The layout is based on a detailed mechanical analysis for which we determined crucial material parameters experimentally. Our current array size is 128x128. We expect to have working arrays by the end of this year. This project has been supported by NASA grants. Title: Microshutter Arrays for the Multi-Object Spectrometer on NGST Authors: Moseley, S. H.; Bowers, C. W.; Fettig, R. K.; Gardner, J. P.; Kimble, R. A.; Kuhn, J.; Kutyrev, A. S.; Malumuth, E. M.; Mentzell, E. E.; Mott, D. B.; Schwinger, D. S.; Teplitz, H. I.; Wesenberg, R. P.; Woodgate, B. E. Bibcode: 2000AAS...196.2302M Altcode: 2000BAAS...32R.705M We present a concept for a high-efficiency, wide-band, multi-object near-infrared spectrograph for the NGST. The spectrograph will simultaneously cover the wavelength range of 0.6-5 microns with a 4K by 4K mosaic array of InSb detectors and will offer low resolution spectroscopy (R=25 - 100) of thousands of objects simultaneously, higher resolution spectroscopy (R ~1500) of about a thousand objects simultaneously, and an imaging mode for initial target acquisition and configuration of a high transmission entrance aperture mask. The key component of the spectrometer is the entrance aperture mask, a programmable microshutter array. We have demonstrated basic mechanical and electrostatic cell operation of a 3 by 3 array. We are currently in the process of scaling it up to large arrays. The first working large size arrays are expected to be tested by the end of this year. Our spectrograph conceptual design includes two principal features to address the demanding scientific requirements of the NGST, whose primary targets will typically be highly redshifted and extremely faint: 1) our lowest resolution spectrograph design is based on refractive dispersing elements (prisms) that permit us to obtain spectra over the entire near-IR range of 0.6-5 microns ( 3 octaves) simultaneously for all objects observed, rather than the 1 octave of coverage (to avoid order confusion) available with a typical grating spectrograph. The use of prisms as the only transmissive or dispersing elements, provides both substantially higher throughput than grating/order sorter combinations as well as the significant multiplexing advantage of complete wavelength coverage in one exposure, 2) for higher resolutions than those available to prisms, we evaluate the trade-off between using 3 or first order gratings for R ~1500 and a prism cross-dispersed echelle for R ~5000. Title: A Least-Squares Solution for the Effective Conductivity of the Solar Convection Zone Authors: Kuhn, J. R.; Georgobiani, D. Bibcode: 2000svc..book..161K Altcode: No abstract at ADS Title: Using Precise Solar Limb Shape Measurements to Study the Solar Cycle Authors: Kuhn, J. R.; Floyd, L.; Fröhlich, C.; Pap, J. M. Bibcode: 2000svc..book..169K Altcode: No abstract at ADS Title: Tunable Filters on NGST Authors: Satyapal, S.; Greenhouse, M. A.; Barclay, R.; Amato, D.; Arritt, B.; Barry, R.; Holt, C.; Kuhn, J.; Higelman, T.; Fonneland, N.; Lesyna, L. Bibcode: 2000ASPC..207..212S Altcode: 2000ngst.conf..212S No abstract at ADS Title: Physical Causes of Solar Variability Authors: Kuhn, J. R.; Schussler, M. Bibcode: 2000svc..book..177K Altcode: No abstract at ADS Title: The Tunable Filter Program for NGST Authors: Satyapal, S.; Greenhouse, M. A.; Barclay, R.; Amato, D.; Arritt, B.; Barry, R.; Holt, C.; Kuhn, J.; Higeiman, T.; Fonneland, N.; Lesnya, L. Bibcode: 2000ASPC..195..437S Altcode: 2000iutd.conf..437S No abstract at ADS Title: A New Planetary Telescope Concept Authors: Joseph, R. D.; Kuhn, J. R.; Tokunaga, A.; Coulter, R.; Ftaclas, C.; Graves, J. E.; Hull, C.; Jewitt, D.; Mickey, D.; Moretto, G.; Neill, D.; Northcott, M.; Roddier, F.; Roddier, C.; Siegmund, W.; Owen, T. Bibcode: 1999DPS....31.5943J Altcode: 1999BAAS...31.1591J The NASA IRTF is arguably the only ground-based telescope in the world dedicated to planetary astronomy. Two decades of improvement in infrared array technology, adaptive optics, and large mirror fabrication techniques now make it imperative that the future needs of NASA's Planetary Astronomy program be considered in the context of the capabilities now possible for a modern telescope. In response to a suggestion from NASA Headquarters we have developed an innovative telescope concept which provides unique and unsurpassed scientific capabilities to the planetary community. We call this facility the New Planetary Telescope (NPT). We have assumed that the main objectives for the NPT are studies of Kuiper Belt Objects, Near-Earth Objects, studies of circumstellar disks and extra-solar planets, and ground-based support for NASA flight missions. These diverse scientific objectives require capabilities ranging over wide-field imaging, high angular resolution, high sensitivity in the optical and thermal infrared, and superb photometric dynamic range. This study shows that it is possible to achieve all of these performance requirements using a 6.5m unobstructed, off-axis telescope. This concept has compelling natural advantages for adaptive optics, coronagraphic astronomical imaging, and thermal infrared imaging. Unique features of the NPT include wide-field imaging capability, with a field-of-view of at least two degrees, optimization for unprecedented low scattered light and high dynamic range astronomy, extremely low infrared emissivity, and innovative instruments uniquely designed to take full advantage of these capabilities. This telescope concept breaks new ground in telescope technology, and it is therefore an ideal technical development project for NASA. NASA is currently at the forefront of development in interferometry using the Keck telescopes. The NPT complements and enhances this program since it provides an important baseline to add to those already planned on Mauna Kea. Moreover, the NPT is the ideal telescope for a full-fledged optical/infrared array of interferometric telescopes. Title: Tunable Filters for NGST Authors: Satyapal, S.; Greenhouse, M.; Barry, R.; Barclay, R.; Amato, D.; Arritt, B.; Harvey, V.; Holt, C.; Kuhn, J.; Fonneland, N.; Lesyna, L. Bibcode: 1999AAS...195.8606S Altcode: 1999BAAS...31Q1501S Tunable filters will enhance the spectral resolution, sensitivity, and field of view capabilities of a number of potential science instruments on NGST. They will : 1) provide flexibility in wavelength and bandwidth choice compared with a fixed inventory of filters in convential cameras, 2) improve the sensitivity of Fourier Transform Spectrometers when full wavelength coverage imaging is not needed, and 3) provide a greater multiplex advantage to multiobject spectrographs when limited spectral coverage is desired. We display work in progress on a near-infrared tunable bandpass filter for the wide field camera of the Next Generation Space Telescope (NGST) Integrated Science Instrument Module (ISIM). This Demonstration Unit for Low Order Cryogenic Etalon (DULCE), is designed to demonstrate a high efficiency scanning Fabry-Perot etalon operating in interference orders 1-4 at 30 K with a high stability DSP based servo control system. DULCE is currently the only available tunable filter for low order cryogenic operation in the near-infrared. In this application, scanning etalons will illuminate the focal plane arrays with a single order of interference to enable wide field low resolution (50 < R < 200) hyperspectral imaging over a wide range of redshifts. Title: Interpreting the Solar Limb Shape Distortions Authors: Armstrong, James; Kuhn, J. R. Bibcode: 1999ApJ...525..533A Altcode: Accurate measurements of the solar oblateness have recently been obtained from the SOHO/MDI satellite experiment. The new data are sufficiently accurate to measure nonnegligible multipole shape terms of higher order than the oblateness. Here we extend earlier solar limb shape calculations and compare the new data with the helioseismic evidence for a complex internal solar rotation profile. We find that the quadrupole (l=2) and hexadecapole (l=4) shape terms are marginally inconsistent with the solar rotation data. Title: The J- and K-Band brightness of the solar F-corona observed during the solar eclipse on February 26, 1998. Authors: Ohgaito, R.; Mann, I.; Kuhn, J. R.; MacQueen, R. M.; Lin, H.; Edmunds, D. Bibcode: 1999BAAS...31.1159O Altcode: No abstract at ADS Title: The J- and K-Band Brightness of the Solar F-Corona Observed During the Solar Eclipse on February 26, 1998 Authors: Ohgaito, R.; Mann, I.; Kuhn, J. R.; MacQueen, R. M.; Lin, H.; Edmunds, D. Bibcode: 1999DPS....31.5502O Altcode: The solar eclipse on February 26 1998 was observed from an open flying aircraft at an altitude of almost 6 km above the Pacific about 800 km southwest from Panama City. The solar F-corona, produced by light scattering and thermal emission from dust around the Sun, was observed with a low atmospheric straylight level in the J and K-band over a field of view of 7 degrees. The data show no indication for the existence of pronounced brightness features in the solar F-corona, such as often discussed as evidence for the existence of dust rings. The shape of the corona is slightly elliptic but symmetric in the north-south direction. The data show a reddening of the coronal brightness compared to the solar spectrum. The color of the F-corona is influenced by the temperature of dust particles, by their spatial distribution, as well as by their size distribution that influences especially the forward scattering that is seen in the corona from dust particles close to the observer. We will discuss the color variation from the solar equator to the solar pole and with distances from the Sun and compare it to models of dust light scattering and thermal emission. Title: Probable Detection of a Bright Infrared Coronal Emission Line of Si IX near 3.93 Microns Authors: Kuhn, J. R.; MacQueen, R. M.; Streete, J.; Tansey, G.; Mann, I.; Hillebrand, P.; Coulter, R.; Lin, H.; Edmunds, D.; Judge, P. Bibcode: 1999ApJ...521..478K Altcode: We report here the probable detection of an emission line of Si IX that was observed from an open C130 aircraft over the Pacific Ocean during the 1998 total solar eclipse. Although the IR data themselves are inconclusive because of the uncertainty in the precise central wavelengths of the narrowband filters during the eclipse, the consistency of the measured IR limb excess with simultaneous EUV emission measured by SOHO/Coronal Diagnostic Spectrometer and the EUV Imager Telescope support our detection claim. This line appears to be the brightest IR coronal line yet observed, and its existence may significantly improve future prospects for obtaining optical coronal magnetic field measurements. Title: Some Astronomical Performance Advantages of Off-Axis Telescopes Authors: Kuhn, J. R.; Hawley, S. L. Bibcode: 1999PASP..111..601K Altcode: Measurements requiring very high photometric dynamic range, like astronomical observations of faint objects near bright sources (e.g., extrasolar planet detection), are often limited by the scattered light characteristics of the telescope. Although the light-gathering power of recently built telescopes has increased dramatically, their scattered light performance has not. We compare models and measurements of telescope scattered light and discuss some of the scientific and technical issues that suggest how a low scattered light design could extend the scientific capabilities of moderate (4 m aperture) telescopes. Title: The Tunable Filter Program for NGST Authors: Satyapal, S.; Greenhouse, M. A.; Barclay, R.; Amato, D.; Arritt, B.; Barry, R.; Holt, C.; Irish, S.; Kuhn, J.; Kutyrev, A.; Morrel, A.; Higelman, T.; Fonneland, N.; Lesyna, L. Bibcode: 1999AAS...194.9109S Altcode: 1999BAAS...31..984S We display work in progress on a near-infrared tunable bandpass filter for the wide field camera of the Next Generation Space Telescope (NGST) Integrated Science Instrument Module (ISIM). This Demonstration Unit for Low Order Cryogenic Etalon (DULCE), is designed to demonstrate a high efficiency scanning Fabry-Perot etalon operating in interference orders 1-4 at 30 K with a high stability DSP based servo control system. DULCE has heritage in a Northrop Grumman system designed for 1st order operation at 300 K, and is being developed jointly by GSFC and NGC as an option to satisfy NGST requirements. In this application, scanning etalons will illuminate the focal plane arrays with a single order of interference to enable wide field low resolution (50 << R << 200) hyperspectral imaging over a wide range of redshifts. We discuss specific science applications that will be enabled by near-infrared tunable filters. Title: What can irradiance measurements tell us about the solar magnetic cycle? Authors: Kuhn, J. R.; Lin, H.; Coulter, R. Bibcode: 1999AdSpR..24..185K Altcode: New full-disk satellite and ground-based experiments operating at visible wavelengths can routinely produce solar photometric data of sufficient accuracy to directly observe the photospheric signature of total irradiance variations. Such data are likely to directly test causal (as opposed to statistical) models of the irradiance mechanisms. This is an important step, since without a physical understanding of these changes we can neither predict nor rule out the possibility of future (or past) large solar influences on the earth's climate variability. Title: Near-Infrared Tunable Bandpass Filters for the NGST ISIM Authors: Satyapal, S.; Greenhouse, M. A.; Barclay, R.; Amato, D.; Arritt, B.; Barry, R.; Irish, S.; Kuhn, J.; Kutyrev, A.; Morell, A.; Hilgeman, T.; Lesyna, L.; Fonneland, N. Bibcode: 1998AAS...193.3505S Altcode: 1998BAAS...30.1296S We display work in progress on a near-infrared tunable bandpass filter for the wide field camera of the Next Generation Space Telescope (NGST) Integrated Science Instrument Module (ISIM). This Demonstration Unit for Low Order Cryogenic Etalon (DULCE), is designed to demonstrate a high efficiency scanning Fabry-Perot etalon operating in interference orders 1-4 at 30 K with a high stability DSP based servo control system. DULCE has heritage in a Northrop Grumman system designed for 1st order operation at 300 K, and is being developed jointly by GSFC and NGC as an option to satisfy NGST requirements. In this application, scanning etalons will illuminate the focal plane arrays with a single order of interference to enable wide field low resolution (50 < R < 200) hyperspectral imaging over a wide range of redshifts. Title: The sun's shape and brightness Authors: Kuhn, J. R.; Bush, R. I.; Scherrer, P.; Scheick, X. Bibcode: 1998Natur.392..155K Altcode: We present satellite data that show that the sun's shape and temperature vary with latitude in an unexpectedly complex way. Although the solar oblateness shows no evidence of varying with the solar cycle, we find a significant hexadecapole shape term which may vary. We also see a variation of about 1.5 K in the surface temperature with latitude. Based on these results, we suggest that sensitive observations of brightness variations be used as a record of the surface 'shadow' of cyclical changes in the solar interior. Title: He i 10830 Angstrom Line Polarimetry: A New Tool to Probe the Filament Magnetic Fields Authors: Lin, Haosheng; Penn, Matt J.; Kuhn, Jeffrey R. Bibcode: 1998ApJ...493..978L Altcode: In this paper, we present a new Stokes polarization observation of a solar filament using the neutral helium line at 10830 Å. Similar to the prominence Hanle effect, the polarization of the filament is due to the resonant scattering and magnetic depolarization of the photospheric radiation; it differs only in the scattering geometry. Since this represents one of the first filament polarization observations, we also present a classical derivation of a set of diagnostic formulae that relate the filament polarization signals to the vector magnetic field.

We measured the full Stokes profiles (I, Q, U, V) by scanning the slit of the spectrograph parallel to the axis of a small filament. In one section of the filament, the polarization signals showed that the axial component of the magnetic field reverses direction on either side of the filament axis. This axial field reversal is not predicted by any of the existing magnetic field models of the filament, nor was it observed by previous prominence Hanle effect observations. We propose that a tilted magnetic field loop across the filament axis can explain the observed axial field reversal.

This observation also serves to demonstrate that measurements of the polarization of the He I 10830 Å radiation from filaments is a useful new tool for the diagnostics of filament magnetic field structures. Title: On the Origin of the Helioseismic Solar Cycle Variations Authors: Kuhn, J. R. Bibcode: 1998ESASP.418..871K Altcode: 1998soho....6..871K With more than one solar cycle's worth of measurements of helioseismic variations, can we make sense of these changes? How much of the solar cycle mechanism do we really understand -- particularly as to how it affects the global acoustic, irradiance/luminosity, and outward magnetic appearance of the sun? In combination with all of the solar observables, what does the helioseismic data reveal (if anything) about solar interior changes? This paper will highlight some of the relevant measurements while attempting to illuminate the physical connections between the local and global solar observations (as inferred from helioseismic, photometric, and numerical experiments). Title: Importance of Monitoring Solar Global Properties: Luminosity, Radius and Oscillations Authors: Pap, J. M.; Kuhn, J. R.; Fröhlich, C.; Ulrich, R.; Jones, A.; Rozelot, J. P. Bibcode: 1998ESASP.417..267P Altcode: 1998cesh.conf..267P No abstract at ADS Title: Space-based near infrared coronal observations Authors: Mann, I.; Kuhn, J. R. Bibcode: 1998AdSpR..21..315M Altcode: We propose a set of observations of the near infrared coronal brightness. Such a study allows unique measurements of the near solar dust dynamics and material properties. In addition, recent suggestions for a cool gas component in the corona will be investigated by observations of the infrared neutral helium line. These observations are difficult and require an upper atmospheric or satellite platform to reduce the noise background. Title: Heat Transport in the Convective Zone and Deviations from the Mixing Length Models Authors: Georgobiani, D.; Kuhn, J. R.; Nordlund, AA.; Stein, R. F. Bibcode: 1998ESASP.418..771G Altcode: 1998soho....6..771G For several decades, the heat transport in the solar convective zone has been thought to be isotropic. Attempts to describe it in terms of the mixing length theory seemed to be quite successful. In contradiction with such an idealized picture, recent numerical and observational data have demonstrated a highly non-isotropic, inhomogeneous structure of the convective zone. This work presents the results of calculations of the thermal conductivity in the convective zone, using the numerical model of Stein-Nordlund. Thermal conductivity is assumed to be a 3D tensor. Its vertical and horizontal diagonal components differ in magnitudes for each given depth. Moreover, the horizontal component stays negative, while increasing with depth. Both features are naturally explained by the physical properties of the solar convective zone. Implications for global questions of solar convection are considered. Title: We must Choose the Simplest Physical Theory: LEVIN-LI-VITÁNYI Theorem and its Potential Physical Applications Authors: Fox, D.; Schmidt, M.; Koshelev, M.; Kreinovich, V.; Longpré, L.; Kuhn, J. Bibcode: 1998mebm.conf..239F Altcode: No abstract at ADS Title: Sound speed variations near the photosphere due to entropy perturbations in 3d numerical experiments Authors: Georgobiani, D.; Kuhn, J. R.; Stein, R. F. Bibcode: 1997ASSL..225..127G Altcode: 1997scor.proc..127G Results on how the temperature distribution near the solar photosphere is altered by perturbing the entropy of rising fluid in the convection zone several megameters below the surface, are presented. Effects on the emergent intensity and implications for helioseismic observations are described. Title: HE I 10830 A Line Polarimetry: A New Tool to Probe the Filament Magnetic Fields Authors: Lin, Haosheng; Penn, Matt J.; Kuhn, Jeffrey R. Bibcode: 1997STIN...9822262L Altcode: In this paper, we present a new Stokes polarization observation of a solar filament using the neutral Helium line at 10830 A. Similar to the prominence Hanle effect, the polarization of the filament is due to the resonant scattering and magnetic depolarization of the photospheric radiation; it differs only in the scattering geometry. Since this represents one of the first filament polarization observations, we also present a classical derivation of a set of diagnostic formulae that relate the filament polarization signals to the vector magnetic field. We measured the full Stokes profiles (I, Q, U, V) by scanning the slit of the spectrograph parallel to the axis of a small filament. In one section of the filament, the polarization signals showed that the axial component of the magnetic field reverses direction on either side of the filament axis. This axial field reversal is not predicted by any of the existing magnetic field models of the filament, nor was it observed by previous prominence Hanle effect observations. We propose that a tilted magnetic field loop across the filament axis can explain the observed axial field reversal. This observation also serves to demonstrate that measurements of the polarization of the He I 10830 A radiation from filaments is a useful new tool for the diagnostics of filament magnetic field structures. Title: Solar Oblateness Measurements by the MDI Instrument on SOHO Authors: Bush, R. I.; Kuhn, J. R.; Scheick, X. Bibcode: 1997SPD....28.0202B Altcode: 1997BAAS...29Q.893B The Michelson Doppler Imager instrument on the SOHO spacecraft provides high precision measurements of the solar limb brightness because of the absence of atmospheric blurring. This paper will describe the solar oblateness determined from MDI observations during a roll maneuver of the SOHO spacecraft performed on 20 March 1997. This maneuver was requested by the SOI-MDI team in order to obtain precise measurements of the solar limb and consisted of two 360 degree rolls of the SOHO spacecraft about the axis pointing to the center of the sun.. By observing the solar limb during the spacecraft roll, the static solar shape can be extracted from the distortion caused by the MDI optics. The primary observable for this activity was the full-disk computed continuum using 1.96" pixels. The first complete roll was performed in increments of 30 degrees, and a second roll was performed in the opposite direction in increments of 90 degrees. The dwell time at each roll position was nominally 25 minutes, with about 10 minutes required to roll the spacecraft 30 degrees and precisely determine the new location. The calibration and analysis of these continuum images to determine the solar oblateness will be detailed Title: Precision solar astrometry from SoHO/MDI Authors: Kuhn, J. R.; Bogart, R.; Bush, R.; Sá, L.; Scherrer, P.; Scheick, X. Bibcode: 1997IAUS..181..103K Altcode: No abstract at ADS Title: Tidal Streams from the Carina and Draco Dwarf Galaxies Authors: Smith, H. A.; Kuhn, J. R.; Hawley, S. L. Bibcode: 1997ASPC..127..163S Altcode: 1997pmga.conf..163S No abstract at ADS Title: Tidal Disruption and Tails from the Carina Dwarf Spheroidal Galaxy Authors: Kuhn, J. R.; Smith, Horace A.; Hawley, Suzanne L. Bibcode: 1996ApJ...469L..93K Altcode: New photometry of regions beyond the classical tidal radius of Carina exposes a Carina-like stellar distribution that is about 1% of the central surface density and which extends at least as far as 2 deg (3.5 kpc) from Carina's center. The detections of a spatially extended RR Lyrae distribution, and a significant Carina-like stellar population at large central distances confirm predictions of the time-dependent tidal interaction model and suggest that Carina is not in virial equilibrium. Title: Accounting for the Solar Acoustic and Luminosity Variations from the Deep Convection Zone Authors: Kuhn, J. R.; Stein, R. F. Bibcode: 1996ApJ...463L.117K Altcode: Recent helioseismic observations (Duvall et al.) have demonstrated how new data analysis techniques can determine local changes in the acoustic properties beneath the photosphere. The recent results provide compelling evidence of a latitudinal sound speed variation. Using results from numerical simulations, we show here how this acoustic variation has the correct form and amplitude needed to account for the previously observed solar photometric changes. In this picture, both the acoustic and irradiance changes may be caused by magnetically induced entropy fluctuations near the base of the solar convection zone. Title: Infrared lines as probes of solar magnetic features. XII. Magnetic flux tubes: evidence of convective collapse? Authors: Solanki, S. K.; Zufferey, D.; Lin, H.; Rueedi, I.; Kuhn, J. R. Bibcode: 1996A&A...310L..33S Altcode: The magnetic field in the solar photosphere is mainly composed of magnetic flux tubes. Their formation is not well understood, largely due to an absence of observational tests of theoretical predictions. Here we use infrared polarimetric data to test and confirm the prediction that whereas the field strength of large flux tubes is almost independent of their magnetic flux, small flux tubes show a strong dependence. Our work thus strengthens the case for convective collapse as the source of concentrated solar magnetic fields. We also present the first direct measurement of the intrinsic field strength of typical intranetwork elements. A significant fraction of them is in equipartition with the kinetic energy of convection. Nevertheless, our results suggest that as far as their internal structure is concerned intranetwork magnetic features are better described by flux tubes than by turbulent fields. Title: The Precision Solar Photometric Telescopes Authors: Coulter, R. L.; Kuhn, J. R.; Lin, H. Bibcode: 1996AAS...188.5604C Altcode: 1996BAAS...28..912C The Precision Solar Photometric Telescopes Program (PSPT) is a community based activity to develop a network of 2 or 3 small aperture telescopes for obtaining accurate solar differential photometry. This effort is centered at the National Solar Observatory (Sunspot, NM) and is funded by the NSF Atmospheric Radiative Inputs of the Sun to Earth (RISE) program and the Astronomy Division. The PSPT is a small, low-scattered-light refracting telescope consisting of a 15-cm doublet objective, a magnetostrictive tip-tilt mirror for fast guiding, a .25nm band-pass CaK filter (393.3nm), two continuum filters and a 2048x2048 CCD camera. The PSPTs will provide full-disk images at 0.1% photometric precision to allow detailed study of the total solar irradiance variation at various temporal scales. These instruments will operate as a multiple station network to allow occasional long unbroken time-series of photometry. The network will produce photometrically calibrated solar images sufficient for detailed study of photospheric features such as limb-darkening, faculae, sunspots and plages. RISE/PSPT will also provide precise measurements of sunspot coordinates, umbral and penumbral areas, and contrasts. The overall design of the PSPT will be described. Recent developments, test results, and an outline of expected data products will be presented. Title: The precision solar photometric telescopes. Authors: Coulter, R. L.; Kuhn, J. R.; Lin, H. Bibcode: 1996BAAS...28R.911C Altcode: No abstract at ADS Title: He I 10830 Angstroms Polarimetry of Filament Authors: Lin, H.; Kuhn, J. R.; Penn, M. Bibcode: 1996AAS...188.8001L Altcode: 1996BAAS...28..956L Full Stokes parameters (IQUV) were obtained from a filament at the He I 10830 Angstroms wavelength. These observations provide information on the vector magnetic field configuration of the filaments, which, up-to-date, were mostly infered from indirect observations like the photospheric magnetograms and Hα images. We will present the instrumentation, as well as the magnetic field configuration of the filament derived from these data, and discuss their implications to filament models. Title: Observations of Tidal Disruption of the Carina Dwarf Spheroidal Galaxy Authors: Kuhn, J. R.; Smith, H. A.; Hawley, S. L. Bibcode: 1996AAS...188.7705K Altcode: 1996BAAS...28S.954K New observations of the Carina dwarf spheroidal galaxy have been obtained at angular distances as far as 2 degrees from its center. Along the Carina major axis we detect RR Lyraes at Carina's MW distance, but well beyond its classical tidal radius. Color-magnitude observations show the existence of a surface density of Carina-population stars which is a few percent of the central density as far as 3.5kpc away from the dS center along its major axis. These measurements support the model of Carina as a tidally disrupting galaxy with no excess dark matter. Title: Earth-Based Observations of the Galileo Probe Entry Site Authors: Orton, G.; Ortiz, J. L.; Baines, K.; Bjoraker, G.; Carsenty, U.; Colas, F.; Dayal, A.; Deming, D.; Drossart, P.; Frappa, E.; Friedson, J.; Goguen, J.; Golisch, W.; Griep, D.; Hernandez, C.; Hoffmann, W.; Jennings, D.; Kaminski, C.; Kuhn, J.; Laques, P.; Limaye, S.; Lin, H.; Lecacheux, J.; Martin, T.; McCabe, G.; Momary, T.; Parker, D.; Puetter, R.; Ressler, M.; Reyes, G.; Sada, P.; Spencer, J.; Spitale, J.; Stewart, S.; Varsik, J.; Warell, J.; Wild, W.; Yanamandra-Fisher, P.; Fazio, G.; Hora, J.; Deutsch, L. Bibcode: 1996Sci...272..839O Altcode: Earth-based observations of Jupiter indicate that the Galileo probe probably entered Jupiter's atmosphere just inside a region that has less cloud cover and drier conditions than more than 99 percent of the rest of the planet. The visual appearance of the clouds at the site was generally dark at longer wavelengths. The tropospheric and stratospheric temperature fields have a strong longitudinal wave structure that is expected to manifest itself in the vertical temperature profile. Title: Sound Speed Variations Near the Photosphere due to Entropy Perturbations in 3D Numerical Experiments Authors: Georgobiani, D.; Kuhn, J. R.; Stein, R. F. Bibcode: 1996AAS...188.6910G Altcode: 1996BAAS...28..937G Results on how the temperature distribution near the solar photosphere is altered by perturbing the entropy of fluid in the convection zone several megameters below the surface are presented. Effects on the emergent intensity and implications for helioseismic observations are described. Title: Observations of tidal disruption of the Carina dwarf spheroidal galaxy. Authors: Kuhn, J. R.; Smith, H. A.; Hawley, S. L. Bibcode: 1996BAAS...28..954K Altcode: No abstract at ADS Title: The Near-Infrared Coronal Spectrum Authors: Kuhn, J. R.; Penn, M. J.; Mann, I. Bibcode: 1996ApJ...456L..67K Altcode: Sensitive measurements of the near-infrared coronal spectrum were obtained from the 1994 total solar eclipse. A new [S IX] emission line at 1.25249 +/- 0.00003 mu m has been detected, and a bright, potentially important diagnostic, [Si X] line at 1.43 mu m has been confirmed. Upper limits on the intensity of several other predicted IR emission lines have been established. Also, diffuse He I emission, perhaps geocoronal, has been observed with a significant heliocentric redshift. Title: Infrared Spectroscopic Observations of Neutral Helium during the 1994 Eclipse Authors: Mann, I.; Kuhn, J. R.; Penn, M. J. Bibcode: 1996ASPC..104..345M Altcode: 1996pcdi.conf..345M; 1996IAUCo.150..345M No abstract at ADS Title: Global changes in the Sun. Authors: Kuhn, J. R. Bibcode: 1996stsu.conf..231K Altcode: The following topics were dealt with: some interesting non-acoustic observables (global observations, solar neutrino variations? another solar mode?); interpreting velocity and shape data; interpreting brightness data; experimenting below the photosphere; numerical experiments, deep questions? Title: Using Scintillation Measurements to Achieve High Spatial Resolution in Photometric Solar Observations Authors: Coulter, R.; Kuhn, J. R.; Rimmele, T. Bibcode: 1996SoPh..163....7C Altcode: The RISE/PSPT (`Radiative Inputs from the Sun to the Earth/Precision Solar Photometric Telescopes') experiment will attain high differential photometric precision in full-disk solar images with 1 arc sec pixels. To achieve this spatial resolution it will be necessary to use frame selection techniques to minimize the effects of atmospheric `seeing'. We report here on experiments to use a simple scintillation monitor as a trigger or `veto' for imaging observations. Title: Preliminary Results of the Analysis of CAII K Spectroheliograms Authors: Kariyappa, R.; Pap, J. M.; Balasubramaniam, K. S.; Kuhn, J. R. Bibcode: 1995ESASP.376b.429K Altcode: 1995help.confP.429K; 1995soho....2..429K No abstract at ADS Title: Mapping Prominence Magnetic Fields: New He I 1083 nm Data Authors: Penn, M.; Kuhn, J. Bibcode: 1995SPD....26..618P Altcode: 1995BAAS...27..965P No abstract at ADS Title: Imaging Spectropolarimetry of the He i 1083 Nanometer Line in a Flaring Solar Active Region Authors: Penn, M. J.; Kuhn, J. R. Bibcode: 1995ApJ...441L..51P Altcode: Slit spectra, simultaneously measuring left and right circular polarization of the solar spectrum at 1082.9 +/- 0.4 nm, were taken using the National Solar Observatory (NSO) Vacuum Tower Telescope (VTT) at Sacramento Peak with a 128 x 128 pixel HgCdTe IR camera. By moving the slit the solar active region NOAA 7629 was scanned with a cadence of 246 s from 1724 to 1902 UT on 1993 December 6. The region was in the decay phase of a C9.7 flare. Intensity, velocity and longitudinal magnetic field in both the Si I (photospheric) and He I (chromospheric) lines are computed from fits to the line profiles in left and right polarizations. Analysis of these quantities show: (1) He I line emission in three decaying flare kernels, (2) Zeeman splitting of the He I emission measuring the longitudinal magnetic field inside the flare kernels; (3) dark He I active region filaments avoid strong longitudinal chromospheric magnetic field, and an active filament (with a transverse speed of 9 km/s) produces fluctuations in the strength of the longitudinal magnetic fields, and (4) bipolar moving magnetic features (MMFs) and emerging active region bipoles (EARBs) are observed at photospheric but not chromospheric heights. Title: The Near Infrared Coronal Spectrum: Results from the 1994 Eclipse Authors: Kuhn, J.; Penn, M.; Mann, I. Bibcode: 1995SPD....26..609K Altcode: 1995BAAS...27..963K No abstract at ADS Title: CLEAR : A Concept for a "Coronagraph and Low Emissivity Astronomical Reflector" for Solar and Nighttime Observations Authors: Beckers, J. M.; Kuhn, J.; Neidig, D.; Rabin, R.; Rimmele, T.; Smartt, R. N. Bibcode: 1995SPD....26..722B Altcode: 1995BAAS...27..971B No abstract at ADS Title: Using Eclipse Observations to Test Scintillation Models Authors: Georgobiani, D.; Kuhn, J. R.; Beckers, J. M. Bibcode: 1995SoPh..156....1G Altcode: Near second and third contact during a solar eclipse the spatial spectrum of the solar illumination changes as the relative power at high spatial frequencies increases strongly. Since groundlevel atmospheric scintillation depends on a weighted integral of the image power spectrum, we can expect to see a measureable time dependence to solar scintillation during an eclipse. This effect was observed during an annular solar eclipse and quantitatively compared with a scintillation model. Title: Solar Variability in Irradiance and Oscillations Authors: Kuhn, J. R. Bibcode: 1995ESASP.376a.145K Altcode: 1995heli.conf..145K; 1995soho....1..145K The signature of the solar cycle appears clearly in helioseismic frequencies and splittings. We have learned that it is the changing outer superadiabatic region of the Sun that is responsible, but can we learn about the deeper solar-cycle mechanism from the surface changes? In particular, how do magnetic fields perturb the global modes, the solar irradiance, and the luminosity? One-dimensional models do not capture the physics of this problem. The author shows that progress will follow from numerical experiments, helioseismic inference, and accurate solar photometry. Title: Infrared tools for solar astrophysics: What's next? Authors: Kuhn, Jeffrey R.; Penn, Matthew J. Bibcode: 1995itsa.conf.....K Altcode: No abstract at ADS Title: Infrared Coronal Magnetic Field Measurements Authors: Kuhn, J. R. Bibcode: 1995itsa.conf...89K Altcode: No abstract at ADS Title: Polarimetric IR Array Observations of a Flare Authors: Penn, M. J.; Kuhn, J. R. Bibcode: 1995itsa.conf..393P Altcode: No abstract at ADS Title: Ground-based Detection of an Infrared [Si x] Coronal Emission Line and Improved Wavelengths for the Infrared [Fe xiii] Emission Lines Authors: Penn, M. J.; Kuhn, J. R. Bibcode: 1994ApJ...434..807P Altcode: The wavelength of an infrared (Si X) coronal emission line is measured to be 1430.084 +/- 0.006 nm with a coronagraph of the National Solar Observatory at Sacramento Peak (NSOINP). New measurements of the infrared (Fe XIII) emission lines locate the central wavelengths at 1074.617 +/- 0.005 nm and 1079.783 +/- 0.006 nm. The slit-averaged line center intensities were 4.5, 27.8, and 5.2 (in units of 10-6 B(solar)) for the 1430 nm, 1075 nm, and 1080 nm emission lines, repectively. The spatial distribution of (Si X) emission is correlated with the coronal electron density as determined from the (Fe XIII) line ratio. Upper limits are set for coronal emission near 1266 nm and 1523 nm. Title: Coronal electron density measurements using the near-ir [Fe XIII] emission lines Authors: Penn, M. J.; Kuhn, J. R.; Arnaud, J.; Mickey, D. L.; Labonte, B. J. Bibcode: 1994SSRv...70..185P Altcode: Observations made during the 1991 total solar eclipse and recent observations from NSO/Sac Peak are discussed. The ground-based density measurements will be complimentary to SOHO observations, particularly SOHO electron density measurements. Title: Removing Instrumental Polarization from Infrared Solar Polarimetric Observations Authors: Kuhn, J. R.; Balasubramaniam, K. S.; Kopp, G.; Penn, M. J.; Dombard, A. J.; Lin, H. Bibcode: 1994SoPh..153..143K Altcode: Full Stokes polarimetry is obtained using the National Solar Observatory Vacuum Tower Telescope at Sacramento Peak while observing the magnetically sensitive infrared FeI line at wavelength of 1.56μ. A technique is described which makes use of the high magnetic resolution in this spectral range to remove instrumental polarization from observed StokesQ, U, andV line profiles. Title: How bright is the [Si X] 1431 nm coronal emission line? Authors: Penn, M. J.; Kuhn, J. R. Bibcode: 1994SoPh..151...51P Altcode: Airborne eclipse observations of the [SiX] 1430.5 nm coronal emission line are reviewed, and new ground-based out-of-eclipse coronagraph observations obtained at NSO/Sacramento Peak are reported. We find that the [SiX] 1430.5 nm coronal emission line brightness is less than 8 × 10−6B⊙ in small active region corona which showed [FeXIII] 1074.7 nm emission (corrected for sky background) of about 20 × 10−6B⊙. Title: Diffuse Light in A2670: Smoothly Distributed? Authors: Scheick, Xania; Kuhn, Jeffrey R. Bibcode: 1994ApJ...423..566S Altcode: We report R- and V-band observations of the rich cluster of galaxies A2670. A measurement of the circular component of the diffuse light or halo of the cD follows a smooth de Vaucouleurs profile out to 230/h kpc. Measurements of the fluctuation per pixel indicate that the diffuse light is likely to be composed of numerous low-luminosity objects. Autocorrelations of the residual images allow us to probe the small-scale fluctuations to a sensitivity of 0.05% of the diffuse light. A differential luminosity function of the central 160/h kpc suggests real differences in the luminosity function within the cluster center from a universal cluster luminosity function. We measure the V - R color of the cD and cluster galaxies and the color gradient across the halo. Also, we report results from a search for detecting evidence of the visible results of dynamical friction, that is, the wakes associated with galaxies passing through a diffuse medium. Title: Solar Irradiance and Luminosity Variations from Active Regions Authors: Kuhn, J. R. Bibcode: 1994ASPC...68...43K Altcode: 1994sare.conf...43K No abstract at ADS Title: Brightness Observations of the Sun Authors: Kuhn, J. R. Bibcode: 1994svsp.coll..130K Altcode: 1994IAUCo.143P.130K No abstract at ADS Title: RISE/PSPT as an Experiment to Study Active Region Irradiance and Luminosity Evolution Authors: Coulter, Roy L.; Kuhn, J. R. Bibcode: 1994ASPC...68...37C Altcode: 1994sare.conf...37C No abstract at ADS Title: IR Observations of the K and F Corona During the 1991 Eclipse Authors: Kuhn, J. R.; Lin, H.; Lamy, P.; Koutchmy, S.; Smartt, R. N. Bibcode: 1994IAUS..154..185K Altcode: No abstract at ADS Title: Simultaneous IR and Visible Light Measurements of the Solar Granulation Authors: Keil, S.; Kuhn, J.; Lin, H.; Reardon, K. Bibcode: 1994IAUS..154..251K Altcode: No abstract at ADS Title: The Precision Solar Photometric Telescope Project Authors: Kuhn, J. R.; Coulter, R. Bibcode: 1993AAS...183.0809K Altcode: 1993BAAS...25.1302K The National Solar Observatory has begun an NSF funded program to obtain precise differential surface photometry of the sun. This experiment is directed at understanding the source of the long (yearly) and short (daily) solar luminosity and irradiance fluctuations. The project will generate full-disk data over wavelengths from 393 nm to 800 nm with 1 arcsecond/pixel spatial resolution. The relative photometric precision of the instrument will be 0.1% /pixel with time resolution of about 1 hour. Two stations will allow occasional 24 hour continuous datasets to be obtained. The current status of the program and scientific focus of the experiment are reviewed in this paper. Title: Dynamical Friction Wake Candidates in A2029 and Diffuse Light in Binary Nucleus Clusters Authors: Scheick, Xania; Kuhn, Jeffrey R. Bibcode: 1993AAS...183.8713S Altcode: 1993BAAS...25R1428S We present R-band observations of candidate wakes associated with five galaxies in A2029. The shapes of the wakes are very similar to the results of Weinberg's 1989 numerical simulations (MNRAS 239 549). We can use the wakes' characteristics (luminosity, size, curvature, local diffuse light level) and the parent galaxies' characteristics (luminosity, radial velocity) to constrain the parent galaxies' mass and transverse velocity with N-body simulations. We also present results of an analysis of the diffuse light in two binary nucleus clusters. Diffuse light has previously been measured in some cD galaxies to supply up to one third of the total cluster light. With two clusters having two distinct but interacting central galaxies, we will address the issue of diffuse light separate from the halos of these galaxies. The results of this analysis have direct bearing on cluster evolution models which suggest that cD galaxies and their large-scale envelopes are formed by mergers. Title: The RISE Precision Solar Photometric Telescope Project Authors: Kuhn, J. R.; Foukal, P. V. Bibcode: 1993BAAS...25.1184K Altcode: No abstract at ADS Title: Unbound Dwarf Spheroidal Galaxies and the Mass of the Milky Way Authors: Kuhn, Jeffrey R. Bibcode: 1993ApJ...409L..13K Altcode: There are reasonable dynamical arguments to support the claim that at least some of the Local Group dwarf spheroidal (dSph) galaxies are not internally bound collections of stars. There are now even a few observations that bolster this view. This Letter points out that the lifetimes of these systems may be longer than is commonly appreciated, and that (as unbound systems) dynamical observations of the dSph may tell us much more about the mass and dark matter content of the Milky Way (MW) than they do about the dark matter content of the dwarf spheroidal. Title: What Causes Cycle-Related Global Solar Changes Authors: Kuhn, J. R. Bibcode: 1993ASPC...42...27K Altcode: 1993gong.conf...27K No abstract at ADS Title: Precision Infrared and Visible Solar Photometry - Part One Authors: Lin, H.; Kuhn, J. R. Bibcode: 1992SoPh..141....1L Altcode: A precision Solar Photometric Telescope (SPT) was constructed to study the large-scale thermal structure of the solar photosphere. This instrument does full-disk, broad-band (10 nm FWHM), two-color (500 and 650 nm) imaging of the solar photosphere. Data obtained by the SPT reveals network structures correlated with the supergranulation velocity field, and the CaK network of the chromosphere. Infrared array photometry extends these measurements to 1.6 and 2.2 micron. The observed correlation of the network brightness signal with the CaK network is positive at visible wavelengths. The correlation between the network at the opacity minimum (1.6 micron) and in the higher photosphere (2.2 micron) is positive also. The root-mean-square (r.m.s.) amplitude of the contrast at disk center is (2.34 ± 0.38) × 10-3, (1.83 ± 0.51) × 10-3, (1.02 ± 0.21) × 10-3, and (1.11 ± 0.21) × 10-3 for the green, red, H, and K band, respectively. It is consistent with a brightness temperature modulation of 2.9 K. The r.m.s. amplitude of the contrast of active region network shows a large increase toward the limb, and the quiet region network shows little center-to-limb variation (CLV). Power-spectrum analysis shows that the bright facular points in the active regions appear in the form of enhanced network. Title: No Evidence of a Circumsolar Dust Ring from Infrared Observations of the 1991 Solar Eclipse Authors: Lamy, P.; Kuhn, J. R.; Lin, H.; Koutchmy, S.; Smartt, R. N. Bibcode: 1992Sci...257.1377L Altcode: During the past 25 years there have been many attempts to detect a possible dust ring around the sun, with contradictory results. Before the 1991 eclipse, infrared eclipse experiments used single-element detectors to scan the corona along the ecliptic for excess surface brightness peaks. The availability of relatively large-format infrared array detectors now provides a considerable observational advantage: two-dimensional mapping of the brightness and polarization of the corona with high photometric precision. The 1991 eclipse path included the high-altitude Mauna Kea Observatory, a further advantage to measure the corona out to large angular distances from the sun. Results are reported from an experiment conducted on Mauna Kea with a HgCdTe-array detector sensitive to wavelengths between 1 and 2.5 micrometers, using broad-band J, H, and K filters. Although the sky conditions were not ideal, the H- and K-band surface brightnesses clearly show the inhomogeneous structure in the K-corona and the elliptical flattening of the F-corona, but no evidence of a circumsolar, local dust component out to 15 solar radii. Title: Infrared Array Measurements of Sunspot Magnetic Fields Authors: McPherson, M. R.; Lin, H.; Kuhn, J. R. Bibcode: 1992SoPh..139..255M Altcode: We have used a 128 × 128 format HgCdTl infrared array with the Sacramento Peak Observatory Vacuum Telescope (VTT) and Echelle spectrograph to obtain two-dimensional observations of the true magnetic field strength in a sunspot. The system we describe retains all of the spectral information contained in the unpolarized IR Fraunhofer line profile with time resolution of about a minute (depending on the scan area and spatial resolution). Unlike previous optical observations (cf. Adam, 1990), infrared observations readily allow direct field strength measurements out to the outer edge of the penumbra. Our data suggest that the magnetic flux density in the outer penumbra is not well described by an extrapolation of the quadratic polynomial, in normalized central distance, that describes the umbral field. We measure a relatively high field strength of 800 G at the penumbra-quiet-Sun boundary, which is consistent with the `return-flux' model of Osherovich and Garcia (1989). Title: Infrared Determinations of Magnetic Profiles in Sunspots Authors: Kopp, G.; Kuhn, J.; Lin, H.; Rabin, D. Bibcode: 1992AAS...180.1202K Altcode: 1992BAAS...24R.747K We present measurements of a sunspot using unpolarized observations of the magnetically-sensitive (Lande g=3) Fe I line at lambda =1.5649 microns (6388.6 cm(-1) ). We compare the magnetic field profile from this fairly symmetric spot with model profiles. Splittings in this infrared line are nearly a factor of 3 greater than in a comparable visible line, since Zeeman splitting as a fraction of linewidth increases linearly with wavelength. The infrared is also less affected by stray light than the visible, because the intensity contrast is reduced, decreasing the effects of stray light, and because instrumental scatter is lower in the infrared. The combination of the magnetic and stray light advantages of the infrared and the recent availability of ``large'' infrared arrays has made possible more sensitive determinations of the magnetic field profile throughout sunspots. From observations of several sunspots, we find that the magnetic field strength, determined in the strong field regime, is not a smooth function of radius from spot center, and that single radial parameter models do not accurately describe the observed spots. Title: Nonfacular Solar Luminosity Variations Authors: Kuhn, J. R.; Libbrecht, K. G. Bibcode: 1991ApJ...381L..35K Altcode: Solar limb photometry data obtained in 1990 shows a decline in the active region facular contribution to the solar irradiance from the previous year - in accord with the maximum in the sunspot cycle occurring in late 1989. In contrast, the nonfacular and nonsunspot contribution to the solar flux increased compared to 1989. This third component of the irradiance variation is consistent with a significant increase in the total mean solar irradiance from the value observed near the time of sunspot maximum. Evidently, the irradiance maximum, like other solar activity indices, exhibits a phase lag with respect to the solar activity maximum as measured by the sunspot number. Title: Gain calibrating NonUniform Image-Array Data Using Only the Image Data Authors: Kuhn, J. R.; Lin, H.; Loranz, D. Bibcode: 1991PASP..103.1097K Altcode: An algorithm is developed for calibrating the spatial nonuniformity of image-array (CCD-type) detectors. Like other techniques this approach uses multiple, spatially displaced images. In circumstances where high-precision flat fields are not available by other means (i.e., sky flats) this technique is advantageous as it uses the data frames for gain calibration even when the array images extended, nonuniform, sources. Numerical experiments and direct observations with intrinsically uniform and quite nonuniform detectors show that this algorithm is useful when data frames are crowded with sources - circumstance where 'median filtering' flatfielding techniques often fail. The algorithm described is robust and efficiently uses information from multiple data frames to determine pixel gain variations, using visible and IR array observations of extended sources. Title: Short-Term Changes in Solar Oscillation Frequencies and Solar Activity Authors: Woodard, M. F.; Kuhn, J. R.; Murray, N.; Libbrecht, K. G. Bibcode: 1991ApJ...373L..81W Altcode: It is shown that the frequencies of solar rho-mode oscillations change significantly over periods as short as one month. These changes correlate significantly with variations in the strength of surface solar activity as measured by the average, over the sun's visible surface, of the magnitude of the line-of-sight magnetic field component from magnetograms. The frequency and mean magnetic variations are found to obey a linear relationship. It is seen that the mean frequency shift at any time depends on the history of solar activity over an interval of, at most, several months prior to the measurement and conclude that the dominant mechanism of the frequency shift is correlated with surface magnetic activity. Title: Precision visible and infrared solar photometry. Authors: Haosheng, Lin; Kuhn, J. R. Bibcode: 1991BAAS...23.1069H Altcode: No abstract at ADS Title: Diffuse Light in Dense Clusters of Galaxies. I. R-Band Observations of Abell 2029 Authors: Uson, Juan M.; Boughn, Stephen P.; Kuhn, Jeffrey R. Bibcode: 1991ApJ...369...46U Altcode: We have developed an observing technique that uses a CCD detector, multiple overlapping exposures, and a tesselating algorithm that allows us to do reliable differential photometry over a large (about 0.6^deg^) field of view to a precision of 2 x 10^-4^ of the night-sky level, limited only by statistical noise. We have measured the point-spread function of the telescope-detector combination out to 20' from the nominal pointing position. We have found that it is necessary to correct the data for the contamination from the extended halos of stars brighter than m_R_ = 15.5 in order to measure diffuse light at levels below μ ~ 26, or about 1% of the average night-sky level. We present R-band observations of the very dense cluster of galaxies Abell 2029. We detect an elliptical component of diffuse light-extended halo of the cD galaxy-with constant eccentricity of 0.9 that follows a de Vaucouleurs profile out to a distance of 425h^1^ kpc [measured as d = (r_min_ r_max_)^1/2^]. The integrated luminosity of the cD galaxy with this halo is 5 x 10^11^h^-2^ L_sun_ (R band). The ratio of the diffuse light to the total cluster light in the elliptical annulus between d = 250h^-1^ kpc and d = 425h^-1^ kpc is 0.10 +/- 0.005, where the uncertainty comes mainly from the estimate of the contribution of the galaxies. We place an upper limit of 5% to the ratio of diffuse light to total cluster light in the elliptical annulus between d = 425h^-1^ kpc and d = 850h^-1^ kpc. Title: Precision Visible and Infrared Solar Photometry Authors: Lin, H.; Kuhn, J. R. Bibcode: 1991BAAS...23.1069L Altcode: No abstract at ADS Title: Inferring solar structure variations from photometric and helioseismic observations Authors: Kuhn, J. R. Bibcode: 1991AdSpR..11d.171K Altcode: 1991AdSpR..11..171K Present large scale photometric and helioseismic data may be related to spatial and temporal deviations from an otherwise static, spherical solar convection zone (SCZ). New space experiments combine precise photometric, helioseismic, and magnetic observational capabilities (like SOHO and MDI) and will provide data needed to understand the interaction of magnetic fields and global scale circulation in the SCZ. Even simple physical arguments make it clear that the anticipated accuracy of these new experiments virtually guarantees new constraints on models of the SCZ. Title: The Variability of the Solar Diameter Authors: Ribes, E.; Beardsley, B.; Brown, T. M.; Delache, Ph.; Laclare, F.; Kuhn, J. R.; Leister, N. V. Bibcode: 1991suti.conf...59R Altcode: It is argued here that most of the variation in observations of the solar radius of over three centuries measure properties of the sun's limb darkening function and are affected by many sources of degradation of the solar image. They do not directly measure a true solar radius. From a long series of visual observations made by a single observer as well as recent photoelectric observations, evidence is found for periodicities in the apparent radius that occur in both modern and historical records. The magnitude of the observed variations is quite different in visual and photoelectric observations, suggesting that the process responsible for the periodicities is either one that modifies the solar limb darkening function or one that causes systematic variations in image blurring by the earth's atmosphere. A connection between solar magnetic activity an apparent radius seems likely, with evidence for such a relation dating back as fast as the Maunder minimum. Title: The Central Galaxy in Abell 2029: An Old Supergiant Authors: Uson, Juan M.; Boughn, Stephen P.; Kuhn, Jeffrey R. Bibcode: 1990Sci...250..539U Altcode: A mosaic of images shows the extended structure of the cD galaxy that resides at the center of the rich cluster of galaxies Abell 2029. After correcting for the scattered light of nearby stars and galaxies, the faint halo of this giant can be traced out to a distance of more than 1 megaparsec, making it one of the largest and most luminous galaxies known. The smoothness of this halo suggests that it was formed early in the history of the cluster. Title: Consistency in Trends in Helioseismic Data and Photospheric Temperature Data through the Solar Cycle Authors: Goode, Philip R.; Kuhn, J. R. Bibcode: 1990ApJ...356..310G Altcode: Inversion confirms the apparent correlation between trends in the helioseismic data and the photospheric temperature data. Although the helioseismic data are noisy, the radial dependence in the results appear to support a model of a cold or hot thermal shadow arising from, perhaps, the dynamo magnetic field seated near the base of the convection zone. Title: Dwarf Spheroidal Galaxies and the Outer Milky Way Potential Authors: Kuhn, J. R.; Hipple, R. Bibcode: 1990BAAS...22..867K Altcode: No abstract at ADS Title: CCD Observation of Diffuse Light in the Rich Cluster A:2029 Authors: Boughn, S. P.; Kuhn, J. R.; Uson, J. M. Bibcode: 1990IAUS..139..357B Altcode: By mosaicking many CCD frames together, a large-scale (1/2 deg) R-band map of the cD cluster Abell 2029 has been constructed. The map was flat from one edge to the other to about 0.05 percent of the night sky, which corresponds to v(R) 30 mag sq arcsec. A novel technique involving the pixel distribution function, was used to measure diffuse light in the cluster out to 450 arcsec (500/h Kpc) along the minor axis of the cluster. In the elliptical region from minor radius 100 arcsec to minor radius 300 arcsec, the diffuse light corresponds to roughly 8 percent of the total cluster light. Data in other optical bands and on other clusters are in the process of being reduced. The applicability of the above technique to measurements of the fluctuations in the extragalactic background light is discussed. Title: Measuring Solar Structure Variations from Helioseismic and Photometric Observations Authors: Kuhn, J. R. Bibcode: 1990LNP...367..157K Altcode: 1990psss.conf..157K There has been some discussion at this meeting of small changes in frequencies and frequency splittings observed during the solar cycle. Previous observations of frequency changes at the level of 10-4 have been convincingly confirmed by several observations presented at this meeting (Jefferies et al. 1990; Libbrecht and Woodard 1990; Pallé et al. 1990). It has been noted that solar photometric (differential and absolute) observations are of comparable accuracy and show similar solar cycle variations. I will summarize here how the latest photometric and helioseismic data may be accounted for by changes in the the convection zone during a solar cycle. Some of these data and this model have been further described elsewhere (Kuhn 1989; Goode and Kuhn 1990). Title: An imaging, tunable magneto-optical filter Authors: Lin, H.; Kuhn, J. R. Bibcode: 1989SoPh..122..365L Altcode: The Imaging, Tunable Magneto-Optical Filter (ITMOF) is a one- or two-cell magnetic birefringence filter designed to measure the Doppler shift of the solar potassium line (770 nm) with respect to a laboratory standard. Two gas vapor cells contain isotopically refined potassium and operate at temperature near 393 K. Hot cell windows are employed in a carefully controlled thermal environment to limit spurious birefringence in the pyrex cell and prevent condensation in the light path. Electromagnets provide a variable strength and direction longitudinal magnetic field of up to 5000 G on each cell. There is no rotating quarter-wave plate or other moving parts. The final image is detected with a CCD camera system. Title: Dwarf Spheroidal Galaxies and Resonant Orbital Coupling Authors: Kuhn, J. R.; Miller, R. H. Bibcode: 1989ApJ...341L..41K Altcode: The structural properties of the dwarf spheroidal satellite galaxies of the Milky Way may be strongly affected by their time-dependent interactions with the "tidal" field of the Milky Way. A low Q resonance of the tidal driving force with collective oscillation modes of the dwarf system can produce many of the observed properties of the Local Group dwarf spheroidal galaxies, including large velocity dispersions that would normally be interpreted as indicating large dynamical masses. Title: Helioseismic Observations of the Solar Cycle Authors: Kuhn, J. R. Bibcode: 1989ApJ...339L..45K Altcode: Satellite and limb photometry observations of the sun yield a consistent picture of a changing effective temperature distribution in the photosphere. Those observations are used to show that a large change in helioseismic splitting coefficients and mode centroid frequencies should be observed in helioseismic data obtained in 1988. Title: Calculating the Internal Solar Asphericity from Frequency Splitting Measurements Authors: Kuhn, J. R. Bibcode: 1989SoPh..123....1K Altcode: Considerable effort and progress has been made in measuring the internal solar rotation from observations of the odd-order helioseismological splitting coefficients (cf. Brown and Morrow, 1987, and references therein). Less progress has been made in using the even coefficients to measure the internal solar structure (cf. Duvall, Harvey, and Pomerantz, 1986; Gough and Taylor, 1984; Dziembowski and Goode, 1984, and references). Yet, small deviations from spherical symmetry in the internal solar structure may be inferred from the helioseismological splitting observations. Spherical-harmonic decomposition and first-order perturbation theory provide a convenient formalism for describing the distortion. Here I describe the formalism and a new, computationally efficient, method for calculating the kernel functions that are needed to invert the splitting data to obtain the structural asphericity. Title: Resonant Orbital Tidal Interactions: Dwarf Spheroidal Morphology and Dynamics Authors: Kuhn, J. R.; Miller, R. H. Bibcode: 1989BAAS...21..767K Altcode: No abstract at ADS Title: Convection and Waves Authors: Stein, R. F.; Nordlund, Å.; Kuhn, J. R. Bibcode: 1989ASIC..263..381S Altcode: 1989ssg..conf..381S No abstract at ADS Title: CCD Observations of Variable Stars in Globular Clusters Authors: Smith, H. A.; Kuhn, J. R.; Curtis, J. Bibcode: 1989upsf.conf..285S Altcode: 1989IAUCo.111..285S No abstract at ADS Title: Convection and p-mode oscillations. Authors: Stein, R. F.; Nordlund, A.; Kuhn, J. R. Bibcode: 1988ESASP.286..529S Altcode: 1988ssls.rept..529S The authors have simulated the upper 2.5 Mm of the solar convection zone using a three-dimensional, compressible, hydrodynamic computer code. Preliminary results show that convection excites p-mode oscillations. The frequencies of the modes in the numerical simulation agree well with the eigenfrequencies of our computational box calculated for the time averaged mean atmosphere. The agreement is excellent at low frequencies, and diverges at higher frequencies in a manner similar to the difference between observed and theoretical frequencies for the sun. Title: Radial and temporal structure of the internal solar asphericity. Authors: Kuhn, J. R. Bibcode: 1988ESASP.286...87K Altcode: 1988ssls.rept...87K There are large systematic differences between the measured even-order splitting coefficients obtained from different helioseismic observations. These data were obtained by several groups, starting about 6 years ago, and used different observing techniques (e.g. Doppler vs. Intensity full disk solar observations) to derive the m-dependence of mode frequencies. Given the wide variation between the observation techniques it may not be surprising that the results differ - yet, the author argued that the variation between datasets may be physically significant and directly related to solar cycle variations in the aspheric structure of the sun. This asphericity is not confined to the photosphere and is related to the solar cycle luminosity variations measured by ACRIM and the solar limb brightness observations. Title: The Surface Temperature of the Sun and Changes in the Solar Constant Authors: Kuhn, J. R.; Libbrecht, K. G.; Dicke, R. H. Bibcode: 1988Sci...242..908K Altcode: The solar distortion telescope has been used to measure the limb shape and latitude dependence of the limb brightness during the summer months for a 5-year period--a time base sufficient to detect solar cycle trends in the data. Comparison of these observations with spaceborne measurements of the solar constant suggests that a significant part of the solar cycle variation in irradiance is a result of temporal changes in the latitude-dependent surface temperature of the sun. Title: Helioseismological Splitting Measurements and the Nonspherical Solar Temperature Structure Authors: Kuhn, J. R. Bibcode: 1988ApJ...331L.131K Altcode: Helioseismological observations continue to yield new information on the structure of the solar interior. Measurements of the splitting of the frequency degeneracy of modes of a given spherical harmonic order already provide a measure of the internal solar radial differential rotation. It is shown here how the even-order terms may be related to an internal nonspherical solar temperature structure. In addition, the apparent inconsistency of the different splitting measurements may be understood from the time dependence observed in the limb observations, which, as shown here, imply a corresponding temporal variation in the splitting data. Title: Non-Newtonian Forces and the Observed Solar Oscillation Spectrum Authors: Kuhn, J. R. Bibcode: 1988IAUS..123..119K Altcode: No abstract at ADS Title: Solar 5-MIN Oscillation Amplitude Anisotropy and Doppler Velocity Systematics Authors: Kuhn, J. R.; O'Neill, C. M.; Gilliam, L. B. Bibcode: 1988IAUS..123...63K Altcode: Several measurements of 5-min velocity amplitudes have yielded confusing and conflicting information on the l and m dependence of the modal excitation (Kuhn and O'hanlon, 1983 - henceforth KO; Deubner, 1985; and Hill et al. 1985). The authors have obtained considerably more data than was described in KO using similar observing techniques. Additional analysis has illuminated a systematic effect related to the finite spatial resolution, and line asymmetry of the data that can lead to errors in inferred velocity amplitudes. Title: Measuring the Solar Limb Brightness Authors: Kuhn, J. Bibcode: 1988srov.proc..217K Altcode: No abstract at ADS Title: An Imaging Tunable Magneto-Optical Filter for Stable Solar Doppler Observations Authors: Lin, H. -S.; Kuhn, J. R. Bibcode: 1987BAAS...19.1097L Altcode: No abstract at ADS Title: Cluster Diffuse Light Measurements Authors: Kuhn, J. R.; Boughn, S. P.; Uson, J. M. Bibcode: 1987BAAS...19.1105K Altcode: No abstract at ADS Title: Observations of a Solar Latitude-dependent Limb Brightness Variation: Erratum Authors: Kuhn, J. R.; Libbrecht, K. G.; Dicke, R. H. Bibcode: 1987ApJ...319.1010K Altcode: No abstract at ADS Title: Is the Solar Oblateness Variable? Measurements of 1985 Authors: Dicke, R. H.; Kuhn, J. R.; Libbrecht, K. G. Bibcode: 1987ApJ...318..451D Altcode: The solar oblateness measured in 1985 is Δr = req-rp = 14.6±2.2 arc ms, where the error is only a formal standard deviation assuming normally distributed and uncorrelated errors. The above result is significantly greater than the 1984 value which, in turn, is significantly less than the 1983 and 1966 values. The differences may be physically significant and are consistent with the hypothesis that the oblateness oscillates with the 11.14 yr period of the solar cycle. The data at present only weakly support this hypothesis. Title: Evidence of global circulation currents from solar-limb temperature variations Authors: Kuhn, J. R.; Libbrecht, K. G.; Dicke, R. H. Bibcode: 1987Natur.328..326K Altcode: The temperature distribution in a turbulent rotating photosphere is non-spherical. Dimensional arguments for the Sun suggest that such a temperature modulation may have an amplitude ΔT~ Tv2/Φ~0.1 K, where T is an average temperature (5,700 K) and v2/Φ is the ratio of the rotational kinetic and potential energy density of the photosphere. Detailed calculations1-3 generally support this expectation. Here we report new observations that should help to understand the solar global dynamics problem. From about 1,400 h of solar-limb data obtained during the summers of 1983-85 we find that the solar-limb temperature variation is not spherically symmetric and is ~1 K. Our results also indicate that the limb temperature departs from its expected l = 2 spatial harmonic form and has, at most, a weak dependence on solar cycle. Title: Solar distortion measurements Authors: Dicke, R. H.; Kuhn, J. R. Bibcode: 1987prnc.rept.....D Altcode: Highly accurate solar limb temperature and shape observations were obtained from Mt Wilson using a highly specialized telescope. The solar oblateness appears to fluctuate on a time scale of years. A latitude dependent solar limb temperature variation exists with a temperature amplitude of about 0.6k. This temperature variation is independent of the solar cycle. Oblateness of the Sun in 1983 and Relativity; On the Facular Contrast Near the Solar Limb; Brightness Variation; Another Reason to Search for Solar g-Modes and New Limits from Solar Ellipticity Measurements; Solar Ellipticity Fluctuations Yield No Evidence of g-Modes; The Variable Oblateness of the Sun: Measurements of 1984; Is the Solar Oblateness Variable? Measurements of 1985; More Evidence for a Solar Latitude Dependent Limb Temperature Variation. Title: Non-Newtonian Forces and the Invisible Mass Problem Authors: Kuhn, J. R.; Kruglyak, L. Bibcode: 1987ApJ...313....1K Altcode: Experimental or observational tests of the 1/r-squared gravitational force law are weak or nonexistent at length scales beyond the solar system. This is because at long distances all astrophysical estimates of mass density based on dynamics give larger values than corresponding measurements based on observed luminosity and local mass-to-luminosity ratios. The discrepancy generally increases with increasing distance, from galactic lengths to at least cluster scales near 10 Mpc, and is usually interpreted as evidence for missing mass. From an empirical perspective that does not recognize the existence of dark matter unless it is nondynamically confirmed, it could be concluded that there are no significant constraints on possible spatial variations in Newton's constant at large distances. The implications of a simple force law correction to Newtonian gravity from planetary to cosmological distances are discussed. Title: Limits on a stochastic gravitational wave background from observations of Earth normal modes. Authors: Boughn, S. P.; Kuhn, J. R. Bibcode: 1987txra.symp...31B Altcode: No abstract at ADS Title: More Evidence for a Solar Latitude Dependent Limb Temperature Variation Authors: Kuhn, J. R. Bibcode: 1987ASSL..137...51K Altcode: 1987isav.symp...51K A preliminary analysis of solar limb data obtained during 1983, 1984 and 1985 supports the observation that the sun has a 0.6°K effective limb temperature variation with a temperature minimum near 50° north and south latitude and no detectible solar cycle time scale variability. Title: The Variable Oblateness of the Sun: Measurements of 1984 Authors: Dicke, R. H.; Kuhn, J. R.; Libbrecht, K. G. Bibcode: 1986ApJ...311.1025D Altcode: The solar oblateness measured in 1984 appears to be significantly less than the 1983 value. This is in turn substantially less than the 1966 value. The observations of 1983 and 1984 were made with a modified and improved version of the Princeton Solar Distortion Telescope used in 1966. Its design is discussed. The sources of error and the analysis technique are discussed. The observed changes in oblateness of the sun are believed to be real and significant. Title: A Search for Extragalactic Background Light Using the Dark Cloud L134 Authors: Boughn, S. P.; Kuhn, J. R. Bibcode: 1986ApJ...309...33B Altcode: CCD surface photometry at 0.65 micron and single-aperture photometry at 2.2 microns on the dark molecular cloud, L134, and on nearby blank sky, were carried out at levels of 0.001 and less than 0.0001 of the brightness of the night sky, respectively. Presumably because of the reflected Galactic light, the cloud appeared bright compared to the reference sky at both these wavelengths. Relative to blank fields, the darkest positions on the cloud had intensities of 1 x 10 to the -5th erg s/sq cm/s/sr at 0.65 micron and 4 x 10 to the -5th ergs/sq cm/s/sr at 2.2 microns. Since the magnitude of the reflected light is unknown, one cannot deduce the level of the extragalactic background light (EBL); however, either the EBL is on the order of or smaller than these values, or the reflected light and the EBL fortuitously cancel. Title: Alternatives to a Galactic Dark Matter Distribution Authors: Kuhn, J. R. Bibcode: 1986BAAS...18.1024K Altcode: No abstract at ADS Title: Solar ellipticity fluctuations yield no evidence of g-modes Authors: Kuhn, J. R.; Libbrecht, K. G.; Dicke, R. H. Bibcode: 1986Natur.319..128K Altcode: Although there have been several claims for the detection of solar g-modes with periods between 2 and 10 hours1-3 and although the present sensitivity of the Princeton Solar Distortion Telescope should allow these low frequency modes to be observed, solar oblateness data from the summers of 1983 and 1984 show no evidence of such oscillations with periods between 1 and 5 hours. In about 250 days (nearly 1,000 hours) of observations, we find no evidence for significant spectral power associated with g-modes. In particular, there is no evidence of a 160.01-min period solar oscillation. Title: Another reason to search for solar g-modes and new limits from solar ellipticity measurements. Authors: Kuhn, J. R. Bibcode: 1986ASIC..169...63K Altcode: 1986ssds.proc...63K Observations of solar g-modes will teach us some gravitational physics. The present sensitivity of the Princeton Solar Distortion Telescope and other recent claims of solar g-modes suggest that these low frequency modes should be observable in shape measurements. From about 250 days and nearly 1000 hours of observations the author finds no evidence for significant spectral power that can be associated with g-modes and no sign of the elusive 160.01 min period solar oscillation. Title: Dark matter in clusters? Authors: Kuhn, J. R. Bibcode: 1986NRAOW..16..291K Altcode: The missing dynamical mass in clusters is still missing (i.e. undetected by nondynamical means). The author shows how a simple relationship accounts for the required dynamical mass in terms of one parameter and only the visible mass distribution. The simplicity of the model argues for its physical interest and the single parametrization may be a clue to the form of the dark matter (henceforth denoted DM) constituents. It is also interesting that the effect of DM in clusters is in detail formally equivalent to adding another long range force that couples to visible mass - although the model provides, equivalently, a statement about the distribution of the DM. It is formulated below in terms of only the visible mass density of a cluster and an additional "effective" long range interaction. Title: On the facular contrast near the solar limb Authors: Libbrecht, K. G.; Kuhn, J. R. Bibcode: 1985ApJ...299.1047L Altcode: Libbrecht and Kuln (1984) have conducted measurements of the continuum contrast of solar faculae in wavelength bands centered at 800 and 525 nm. Some of the obtained results did not agree with observations reported by Chapman and Klabunde (1982). The present paper has the objective to provide new data, taking into account a demonstration of a procedure for obtaining the facular contrast near the solar limb on the basis of a simple analysis. The findings confirm the results of Libbrecht and Kuln that the contrast in the region near the extreme solar limb decreases with decreasing distance to the limb. Attention is given to exposed limbs and flux ratios for three occulting disks, seasonal average normalized flux profiles Delta F/I for the three disks in two colors, and excess facular signal Delta F/I plotted for various disks using 1984 data. Title: Oblateness of the Sun in 1983 and relativity Authors: Dicke, R. H.; Kuhn, J. R.; Libbrecht, K. G. Bibcode: 1985Natur.316..687D Altcode: Measurements of the solar oblateness obtained during 1983 from Mount Wilson, California, yield a value with an upper bound only half of that observed in 1966. This difference may support the conjecture that the solar quadrupole moment slowly oscillates. A knowledge of the character of such an oscillation, if it occurs, would be needed to test Einstein's relativity theory using Mercury's orbital motion. Title: Observations of a Solar Latitude-dependent Limb Brightness Variation Authors: Kuhn, J. R.; Libbrecht, K. G.; Dicke, R. H. Bibcode: 1985ApJ...290..758K Altcode: A small latitude-dependent photospheric excess brightness variation has been observed from 131 days of data obtained with the Princeton Solar Distortion Telescope. Using an analytic model to separate the influence of faculae from the brightness signal, a temperature difference of 0.6 + or - 0.1 K between the poles and the regions at + or - 53 solar latitude was obtained for the summer of 1983, a temperature difference of 0.6 + or - 0.1 K between the poles and the regions at + or - 53 deg solar latitude was obtained for the summer of 1983, with the polar regions being hotter. Title: Spectral information from gapped data: a comparison of techniques. Authors: Kuhn, J. R. Bibcode: 1984sses.nasa..293K Altcode: 1984sss..conf..293K The fast Fourier transformations (FFT) is used to estimate power spectra of continuous signals evenly sampled on discrete domains. The problem of finding power spectra on unevenly sampled domains, in particular a regularly spaced domain with gaps is discussed. The analysis of the ACRIM solar bolometric intensity data, obtained with a 3/5 on and 2/5 off duty cycle of approximately 100 minutes, would benefit from the techniques. The comparative effectiveness of three different analysis techniques applied to synthetic data generated on gapped domain is reported. Title: Limits on a stochastic gravitational wave background from observations of terrestrial and solar oscillations Authors: Boughn, S. P.; Kuhn, J. R. Bibcode: 1984ApJ...286..387B Altcode: Realistic models of the Earth and Sun are used to calculate their respective responses to a homogeneous, isotropic background of gravitational radiation. Solar velocity data constrain the energy density of such a background at a frequency of 4 x 10-4 Hz to be less than 102, times the closure density of the universe, as does Earth seismic data at frequencies of 2 x 10-3 Hz and 2 x 10-2 Hz. With improved data soon to be available it is likely that both of these limits will be lowered to below closure density. Errors in previous analyses of the Earth are pointed out. Title: Anisotropy and amplitude structure of low-l 5-min solar oscillations Authors: Kuhn, J. R. Bibcode: 1984MmSAI..55...69K Altcode: Line-center Doppler-shift data has been obtained from CCD-spectrograph observations. The 5-hour time series yields useful information at spatial wavelengths near one solar radius along both the solar north-south and east-west orientations. At these wavelengths the 5-min-oscillation velocity field is not isotropic and not well described by modes of uniform excitation. The velocity power density per spherical harmonic increases with decreasing l to 1100 sq cm/sq sec per 350-microhertz angular-frequency bandwidth at l = 4. It is interesting that the calculated low-l dependence in the growth rate of p-modes due to the kappa mechanism shows a similar behavior. Title: Observations of a Solar Latitude Dependent Photospheric Brightness Variation Authors: Kuhn, J. R.; Libbrecht, K. G.; Dicke, R. H. Bibcode: 1984BAAS...16..451K Altcode: No abstract at ADS Title: Limits on a Stochastic Gravitational Wave Background from Observations of Terrestrial &Solar Oscillations Authors: Boughn, S. P.; Kuhn, J. R. Bibcode: 1984BAAS...16..452B Altcode: No abstract at ADS Title: Random Walk Statistics Applied to Large Scale Galaxy Maps Authors: Wolpert, D. H.; Kuhn, J. R. Bibcode: 1984BAAS...16..488W Altcode: No abstract at ADS Title: Gravitational wave excitation of the 160-min solar oscillation? Authors: Kuhn, J. R.; Boughn, S. P. Bibcode: 1984Natur.308..164K Altcode: Recent γ-ray observations1 of the, apparently, nearby source Geminga suggest the possibility that it is a close binary pair of compact stellar objects orbiting with a period of 160 or perhaps 320 min (Delache1 speculates that a 160-min periodicity in the γ-ray flux might still be a signature of a 320-min orbital period). The coincidence of this period with the observed 160-min periodicity in the full disk solar velocity data has led G. Isaak (personal communication) and others to speculate that the gravitational waves emitted by the binary pair are exciting a normal mode of the Sun. Solar velocity data2-4 confirm the existence of an approximately 50 cm s-1 oscillation in integrated Doppler shift observations that has been phase coherent for ~9 yr. We report here a calculation of the solar cross-section for gravitational wave excitation and discuss why such a mechanism is an extremely unlikely explanation of the observed solar oscillation. Title: A new measurement of the facular contrast near the solar limb Authors: Libbrecht, K. G.; Kuhn, J. R. Bibcode: 1984ApJ...277..889L Altcode: Photometer measurements of solar faculae taken at 525 nm and 800 nm over a five-month period in the summer of 1982 are presented. They reveal a contrast function which decreases with decreasing mu near the extreme limb, in striking disagreement with the result of Chapman and Klabunde (1982). It is shown that systematic errors in the Chapman-Klabunde data analysis could account for the discrepancy. The instrument and observing program of this study and the procedure used to identify faculae near the limb are described. The effectiveness of different analysis programs for determining the contrast function from photometer data is discussed and the analysis procedure used on the presented data is described in detail. The results are in good agreement with the facular model of Spruit (1976). Title: Center-to-Limb Variation of the Convective Line Shift Authors: Kuhn, J. R. Bibcode: 1984ssdp.conf..381K Altcode: Full disk Fraunhofer line core shifts have been analysed for evidence of a latitude dependence to the residual convective blue shift, and temporal variability greater than expected from the low-l 5 min oscillations. The author finds no evidence for a latitude dependence to the mean convective shift at the two sigma level of 105 m s-1. The global symmetric line shift profile shows temporal variability in the 5-min band which is larger than expected based on estimates of the 5-min mode amplitudes. Title: Using Solar Oscillations to Search for Gravitational Radiation Authors: Kuhn, J. R.; Boughn, S. P. Bibcode: 1984LIACo..25..224K Altcode: 1984tpss.conf..224K; 1984trss.conf..224K No abstract at ADS Title: Low-l 5-min oscillation observations. Authors: Kuhn, J. R.; Ohanlon, M. Bibcode: 1983SoPh...87..207K Altcode: 1983SoPh...87..207O Medium resolution CCD-spectrograph observations have been obtained that are suitable for studying long spatial wavelength 5-min oscillations. We find evidence that at wavelengths of order one solar radius the oscillation field is not isotropic. It is also not well described by modes of uniform excitation. The velocity power density per spherical harmonic increases with decreasing l to 1.1 × 103 cm2 s−2 per 3.5 × 10−4 Hz angular frequency bandwidth at l = 4. These results are inconsistent with the data of Fossat and Ricort (1975) as analyzed by Christensen-Dalsgaard and Gough (1982), who found a substantially constant modal amplitude at intermediate l values. It is interesting that other calculations have seen a similar dependence at small l in the growth rate of p-modes due to the κ-mechanism. Title: Facular influences on the apparent solar shape Authors: Dicke, R. H.; Kuhn, J. R.; Libbrecht, K. G. Bibcode: 1983Natur.304..326D Altcode: Schatten and Sofia1 have recently reconsidered the question of whether the 1966 solar ellipticity measurements2 were seriously contaminated by excess brightness of faculae near the solar limb3-7. They considered several different functions for the variations of the facular contrast with position relative to the solar limb. With their own facular contrast function, Schatten and Sofia obtain only a small contribution of faculae to the 1966 apparent solar ellipticity, but with the Chapman function they obtain a substantial contribution. New observations of faculae during the summer of 1982 and a novel analytical technique determine a facular contrast which is constant or decreasing towards the limb, consistent with the Schatten and Sophia function but inconsistent with Chapman's function. We show here that the statistical analysis of the 1966 data8 supports this result. We disagree with the earlier conclusion1, that with an acceptable facular contrast function one can obtain ``an acceptable fit to the oblateness measurements'' as a purely facular effect. For 20-30% of the observational days in 1966 only a few small, weak facular patches were present at the limb, but the ellipticity signal was present and it was not reduced in magnitude for those days. Title: Low-1 5-min Oscillation Observations Authors: Kuhn, J. R. Bibcode: 1983BAAS...15Q.705K Altcode: No abstract at ADS Title: A New Measurement of the Facular Contrast Near the Solar Limb Authors: Libbrecht, K. G.; Kuhn, J. R. Bibcode: 1983BAAS...15..717L Altcode: No abstract at ADS Title: Observations of global-scale photospheric Fraunhofer line shifts Authors: Kuhn, J. R. Bibcode: 1983ApJ...264..689K Altcode: Transform techniques have been applied to a 1 yr sequence of solar photospheric Fraunhofer line shift data. In agreement with earlier studies, no evidence is found of large-scale structure in mean spatial power spectra near the level of 12 m/s. It is argued that such spectra are easily dominated by random supergranule noise, and that these data may even be used to estimate supergranule characteristics. By considering a rotation signal in the temporal transformed data, statistical evidence (at the 3 sigma level) is found of a large-scale, long-lived, photospheric line shift field. A simple model suggests spatial scales of 100,000-1,000,000 km, with lifetimes of at least 3 days and line shifts corresponding to velocity amplitudes near 2 m/s. While the interpretation of the residual line shift is not unambiguous, it is suggested that this is the Doppler velocity signature of large-scale convective cells. Title: Filamentary structure in the Shane-Wirtanen galaxy distribution. Authors: Kuhn, J. R.; Uson, J. M. Bibcode: 1982ApJ...263L..47K Altcode: The paper considers a statistic that is sensitive to differences in the galaxy distribution of the Shane-Wirtanen catalog and similar random catalogs with the same low-order galaxy autocorrelation functions. It has been indicated by numerical experiments that this statistic is a measure of the filamentary structure in these catalogs. The present results show that there is significantly more filamentary structure in the Shane-Wirtanen galaxy distribution than in model catalogs without added chainlike structure. Title: Does the Shane-Wirtanen Galaxy Distribution have Filamentary Structure? Authors: Kuhn, J. R.; Uson, J. M. Bibcode: 1982BAAS...14..631K Altcode: No abstract at ADS Title: Recovering spectral information from unevenly sampled data - Two machine-efficient solutions Authors: Kuhn, J. R. Bibcode: 1982AJ.....87..196K Altcode: Astronomical data are often unevenly sampled. The problem of recovering a discrete Fourier transform is discussed, and two procedures for recovering an approximation to the transform are presented. Numerical examples suggest that the approach may be useful for many types of sample domains. Title: Possible radio flaring activity on a late-type giant star, alf Cet. Authors: Boice, D. C.; Kuhn, J. R.; Robinson, R. D.; Worden, S. P. Bibcode: 1981ApJ...245L..71B Altcode: A search is made for radio flare events on 15 late-type stars using the Arecibo radio telescope at 430 MHz. About 50 hr of interference-free data are obtained and one impulsive event is detected for the M2 III star Alpha Cet. The observed radio event is consistent with the hypothesis that it originated in a solar-flare-type disturbance in the stellar atmosphere. Title: Flare activity on T Tau stars. Authors: Worden, S. P.; Schneeberger, T. J.; Kuhn, J. R.; Africano, J. L. Bibcode: 1981ApJ...244..520W Altcode: Observations of short-period photometric fluctuations in T Tauri stars show flarelike events. These events are consistent with the superposition of many solar-like flare events and have a power-spectrum frequency dependence of ∼f-2. This dependence is the same as that observed on UV Ceti stars. The flare events are very powerful, and the expected proton flux from these events may explain early solar system abundance anomalies without recourse to nearby supernovae. The flare events are consistent with the observations of mass loss in these stars. Title: Global Scale Photospheric Velocity Fields: Probes of the Solar Interior. Authors: Kuhn, J. R. Bibcode: 1981PhDT.........2K Altcode: The integrity of the theory of stellar evolution depends on agreement between the sun and its models. There are inconsistencies, though, which will only be resolved by a more complete understanding of the solar interior. This will likely come from photospheric measurements of parameters that are sensitive to the interior conditions. Large scale photospheric velocity fields are one such probe. This work describes an attempt to measure the long term behavior of global scale fields, with an eye toward understanding the conditions below the surface that largely determine these velocity patterns. This paper reports on: (1) a 4-sigma detection of convective eddies rotating at the photospheric rate with transverse spatial scales of order 10('5)km, (2) a 3m/s bound to the amplitude of long period global photospheric velocity oscillations, and (3) a new method for Fourier analysing unevenly sampled data. Title: Global scale photospheric velocity fields: probes of the solar interior Authors: Kuhn, Jeffrey Richard Bibcode: 1981PhDT.......160K Altcode: No abstract at ADS Title: Large Scale Solar Velocity Features Authors: Kuhn, J. R.; Worden, S. P. Bibcode: 1980BAAS...12..473K Altcode: No abstract at ADS Title: Evidence of long-period velocity fluctuations. Authors: Kuhn, J. R.; Worden, S. P. Bibcode: 1979ApJ...228L.119K Altcode: Evidence of a solar fluctuation with a period of 17 days is observed in spectroscopic differential-rotation data by using a technique developed to look at long time sequences of unevenly spaced data. Both spectroscopic observations and sunspot drift-velocity measurements indicate a possible periodicity between 184 and 364 days. The sunspot data marginally show fluctuations with periods which are multiples of 4.2 days. Title: Evidence of Long Period Solar Velocity Fluctuations Authors: Kuhn, J. R.; Worden, S. P. Bibcode: 1978BAAS...10..639K Altcode: No abstract at ADS