Author name code: jaeggli ADS astronomy entries on 2022-09-14 author:"Jaeggli, Sarah A." ------------------------------------------------------------------------ Title: A Publicly Available Multiobservatory Data Set of an Enhanced Network Patch from the Photosphere to the Corona Authors: Kobelski, Adam R.; Tarr, Lucas A.; Jaeggli, Sarah A.; Luber, Nicholas; Warren, Harry P.; Savage, Sabrina Bibcode: 2022ApJS..261...15K Altcode: 2022arXiv220501766K New instruments sensitive to chromospheric radiation at X-ray, UV, visible, IR, and submillimeter wavelengths have become available that significantly enhance our ability to understand the bidirectional flow of energy through the chromosphere. We describe the calibration, coalignment, initial results, and public release of a new data set combining a large number of these instruments to obtain multiwavelength photospheric, chromospheric, and coronal observations capable of improving our understanding of the connectivity between the photosphere and the corona via transient brightenings and wave signatures. The observations center on a bipolar region of enhanced-network magnetic flux near disk center on SOL2017-03-17T14:00-17:00. The comprehensive data set provides one of the most complete views to date of chromospheric activity related to small-scale brightenings in the corona and chromosphere. Our initial analysis shows a strong spatial correspondence between the areas of broadest width of the hydrogen-α spectral line and the hottest temperatures observed in Atacama Large Millimeter/submillimeter Array (ALMA) Band 3 radio data, with a linear coefficient of 6.12 × 10-5Å/K. The correspondence persists for the duration of cotemporal observations (≍60 m). Numerous transient brightenings were observed in multiple data series. We highlight a single, well-observed transient brightening in a set of thin filamentary features with a duration of 20 minutes. The timing of the peak intensity transitions from the cooler (ALMA, 7000 K) to the hotter (XRT, 3 MK) data series. Title: Ground-based instrumentation and observational techniques Authors: Rimmele, Thomas; Kuhn, Jeff; Woeger, Friedrich; Tritschler, . Alexandra; Lin, Haosheng; Casini, Roberto; Schad, Thomas; Jaeggli, Sarah; de Wijn, Alfred; Fehlmann, Andre; Anan, Tetsu; Schmidt, Dirk Bibcode: 2022cosp...44.2507R Altcode: We'll review the current state-of-the-art for ground-based instrumentation and techniques to achieve high-resolution observations. We'll use the 4m Daniel K. Inouye Solar Telescope (DKIST), the European Solar Telescope (EST) and other ground-based instrumentation as examples to demonstrate instrument designs and observing techniques. Using adaptive optics and post-facto image processing techniques, the recently completed DKIST provides unprecedented resolution and high polarimetric sensitivity that enables 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. Versatile ground-based instruments provide highly sensitive measurements of solar magnetic fields, that in the case of DKIST, also include measurements of the illusive magnetic field of the faint solar corona. Ground-based instruments produce large and diverse data sets that require complex calibration and data processing to provide science-ready to a broad community. We'll briefly touch on ongoing and future instrumentation developments, including multi-conjugate adaptive optics. Title: Science Commissioning of the Diffraction-Limited Near-IR Spectropolarimter for the Daniel K. Inouye Solar Telescope Authors: Lin, Haosheng; Schad, Thomas; Kramar, Maxim; Jaeggli, Sarah; Anan, Tetsu; Onaka, Peter Bibcode: 2022cosp...44.2508L Altcode: The Diffraction-Limited Near-IR Spectropolarimeter (DL-NIRSP) is one of the first-generation facility instruments of the Daniel K. Inouye Solar Telescope (DKIST, or The Inouye Solar Telescope). It is a near-IR spectropolarimeter optimized to study the magnetism of the dynamic solar atmosphere, from the photosphere to the corona. DL-NIRSP is equipped with two integral field units (IFUs) coupled to a high-resolution grating spectrograph, and is capable of simultaneous measurements of the full polarized spectra of a 2-dimensional spatial field without scanning. Large field of view observations are supported by mosaicking. DL-NIRSP observes simultaneously at three spectral windows, enabling simultaneous coverage of different atmospheric layers with carefully selected spectral lines. It can also observe the Sun with three resolution modes, from diffraction-limited observations with a spatial sampling of 0.03" to wide-field mode covering a 32"x15" instantaneous FOV with 0.5" sampling. This paper will present results from science commissioning observations conducted in late 2021. Title: Thomson Scattering above Solar Active Regions and an Ad Hoc Polarization Correction Method for the Emissive Corona Authors: Schad, Thomas A.; Jaeggli, Sarah A.; Dima, Gabriel I. Bibcode: 2022ApJ...933...53S Altcode: 2022arXiv220509808S Thomson-scattered photospheric light is the dominant constituent of the lower solar corona's spectral continuum viewed off-limb at optical wavelengths. Known as the K-corona, it is also linearly polarized. We investigate the possibility of using the a priori polarized characteristics of the K-corona, together with polarized emission lines, to measure and correct instrument-induced polarized crosstalk. First we derive the Stokes parameters of the Thomson scattering of unpolarized light in an irreducible spherical tensor formalism. This allows forward synthesis of the Thomson-scattered signal for the more complex scenario that includes symmetry-breaking features in the incident radiation field, which could limit the accuracy of our proposed technique. For this, we make use of an advanced 3D radiative magnetohydrodynamic coronal model. Together with synthesized polarized signals in the Fe XIII 10746 Å emission line, we find that an ad hoc correction of telescope- and instrument-induced polarization crosstalk is possible under the assumption of a nondepolarizing optical system. Title: A Model-based Technique for Ad Hoc Correction of Instrumental Polarization in Solar Spectropolarimetry Authors: Jaeggli, Sarah A.; Schad, Thomas A.; Tarr, Lucas A.; Harrington, David M. Bibcode: 2022ApJ...930..132J Altcode: 2022arXiv220403732J We present a new approach for correcting instrumental polarization by modeling the nondepolarizing effects of a complex series of optical elements to determine physically realizable Mueller matrices. Provided that the Mueller matrix of the optical system can be decomposed into a general elliptical diattenuator and general elliptical retarder, it is possible to model the crosstalk between both the polarized and unpolarized states of the Stokes vector and then use the acquired science observations to determine the best-fit free parameters. Here we implement a minimization for solar spectropolarimetric measurements containing photospheric spectral lines sensitive to the Zeeman effect using physical constraints provided by polarized line and continuum formation. This model-based approach is able to provide an accurate correction even in the presence of large amounts of polarization crosstalk and conserves the physically meaningful magnitude of the Stokes vector, a significant improvement over previous ad hoc techniques. Title: Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE). II. Flares and Eruptions Authors: Cheung, Mark C. M.; Martínez-Sykora, Juan; Testa, Paola; De Pontieu, Bart; Chintzoglou, Georgios; Rempel, Matthias; Polito, Vanessa; Kerr, Graham S.; Reeves, Katharine K.; Fletcher, Lyndsay; Jin, Meng; Nóbrega-Siverio, Daniel; Danilovic, Sanja; Antolin, Patrick; Allred, Joel; Hansteen, Viggo; Ugarte-Urra, Ignacio; DeLuca, Edward; Longcope, Dana; Takasao, Shinsuke; DeRosa, Marc L.; Boerner, Paul; Jaeggli, Sarah; Nitta, Nariaki V.; Daw, Adrian; Carlsson, Mats; Golub, Leon; The Bibcode: 2022ApJ...926...53C Altcode: 2021arXiv210615591C Current state-of-the-art spectrographs cannot resolve the fundamental spatial (subarcseconds) and temporal (less than a few tens of seconds) scales of the coronal dynamics of solar flares and eruptive phenomena. The highest-resolution coronal data to date are based on imaging, which is blind to many of the processes that drive coronal energetics and dynamics. As shown by the Interface Region Imaging Spectrograph for the low solar atmosphere, we need high-resolution spectroscopic measurements with simultaneous imaging to understand the dominant processes. In this paper: (1) we introduce the Multi-slit Solar Explorer (MUSE), a spaceborne observatory to fill this observational gap by providing high-cadence (<20 s), subarcsecond-resolution spectroscopic rasters over an active region size of the solar transition region and corona; (2) using advanced numerical models, we demonstrate the unique diagnostic capabilities of MUSE for exploring solar coronal dynamics and for constraining and discriminating models of solar flares and eruptions; (3) we discuss the key contributions MUSE would make in addressing the science objectives of the Next Generation Solar Physics Mission (NGSPM), and how MUSE, the high-throughput Extreme Ultraviolet Solar Telescope, and the Daniel K Inouye Solar Telescope (and other ground-based observatories) can operate as a distributed implementation of the NGSPM. This is a companion paper to De Pontieu et al., which focuses on investigating coronal heating with MUSE. Title: Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE): II. Flares and Eruptions Authors: Cheung, Chun Ming Mark; Martinez-Sykora, Juan; Testa, Paola; De Pontieu, Bart; Chintzoglou, Georgios; Rempel, Matthias; Polito, Vanessa; Kerr, Graham; Reeves, Katharine; Fletcher, Lyndsay; Jin, Meng; Nobrega, Daniel; Danilovic, Sanja; Antolin, Patrick; Allred, Joel; Hansteen, Viggo; Ugarte-Urra, Ignacio; DeLuca, Edward; Longcope, Dana; Takasao, Shinsuke; DeRosa, Marc; Boerner, Paul; Jaeggli, Sarah; Nitta, Nariaki; Daw, Adrian; Carlsson, Mats; Golub, Leon Bibcode: 2021AGUFMSH51A..08C Altcode: Current state-of-the-art spectrographs cannot resolve the fundamental spatial (sub-arcseconds) and temporal scales (less than a few tens of seconds) of the coronal dynamics of solar flares and eruptive phenomena. The highest resolution coronal data to date are based on imaging, which is blind to many of the processes that drive coronal energetics and dynamics. As shown by IRIS for the low solar atmosphere, we need high-resolution spectroscopic measurements with simultaneous imaging to understand the dominant processes. In this paper: (1) we introduce the Multi-slit Solar Explorer (MUSE), a spaceborne observatory to fill this observational gap by providing high-cadence (<20 s), sub-arcsecond resolution spectroscopic rasters over an active region size of the solar transition region and corona; (2) using advanced numerical models, we demonstrate the unique diagnostic capabilities of MUSE for exploring solar coronal dynamics, and for constraining and discriminating models of solar flares and eruptions; (3) we discuss the key contributions MUSE would make in addressing the science objectives of the Next Generation Solar Physics Mission (NGSPM), and how MUSE, the high-throughput EUV Solar Telescope (EUVST) and the Daniel K Inouye Solar Telescope (and other ground-based observatories) can operate as a distributed implementation of the NGSPM. This is a companion paper to De Pontieu et al. (2021, also submitted to SH-17), which focuses on investigating coronal heating with MUSE. Title: Chromospheric Heating Mechanisms in a Plage Region Constrained by Comparison of Magnetic Field and Mg II h & k Flux Measurements with Theoretical Studies Authors: Anan, Tetsu; Schad, Thomas; Kitai, Reizaburo; Dima, Gabriel; Jaeggli, Sarah; Tarr, Lucas; Collados, Manuel; Dominguez-Tagle, Carlos; Kleint, Lucia Bibcode: 2021AGUFMSH44A..05A Altcode: The strongest quasi-steady heating in the solar atmosphere from the photosphere through the corona occurs in plage regions. As many chromospheric heating mechanisms have been proposed, important discriminators of the possible mechanisms are the location of the heating and the correlation between the magnetic field properties in the chromosphere and the local heating rate. We observed a plage region with the He I 1083.0 nm and Si I 1082.7 nm lines on 2018 October 3 using the integral field unit mode of the GREGOR Infrared Spectrograph (GRIS) installed at the GREGOR telescope. During the GRIS observation, the Interface Region Imaging Spectrograph (IRIS) obtained spectra of the ultraviolet Mg II h & k doublet emitted from the same region. In the periphery of the plage region, within the limited field of view seen by GRIS, we find that the Mg II radiative flux increases with the magnetic field in the chromosphere. The positive correlation implies that magnetic flux tubes can be heated by Alfvén wave turbulence or by collisions between ions and neutral atoms relating to Alfvén waves. Within the plage region itself, the radiative flux was large between patches of strong magnetic field strength in the photosphere, or at the edges of magnetic patches. On the other hand, we do not find any significant spatial correlation between the enhanced radiative flux and the chromospheric magnetic field strength or the electric current. In addition to the Alfvén wave turbulence or collisions between ions and neutral atoms relating to Alfvén waves, other heating mechanisms related to magnetic field perturbations produced by interactions of magnetic flux tubes could be at work in the plage chromosphere. Title: Measurements of Photospheric and Chromospheric Magnetic Field Structures Associated with Chromospheric Heating over a Solar Plage Region Authors: Anan, Tetsu; Schad, Thomas A.; Kitai, Reizaburo; Dima, Gabriel I.; Jaeggli, Sarah A.; Tarr, Lucas A.; Collados, Manuel; Dominguez-Tagle, Carlos; Kleint, Lucia Bibcode: 2021ApJ...921...39A Altcode: 2021arXiv210807907A In order to investigate the relation between magnetic structures and the signatures of heating in plage regions, we observed a plage region with the He I 1083.0 nm and Si I 1082.7 nm lines on 2018 October 3 using the integral field unit mode of the GREGOR Infrared Spectrograph (GRIS) installed at the GREGOR telescope. During the GRIS observation, the Interface Region Imaging Spectrograph obtained spectra of the ultraviolet Mg II doublet emitted from the same region. In the periphery of the plage region, within the limited field of view seen by GRIS, we find that the Mg II radiative flux increases with the magnetic field in the chromosphere with a factor of proportionality of 2.38 × 104 erg cm-2 s-1 G-1. The positive correlation implies that magnetic flux tubes can be heated by Alfvén wave turbulence or by collisions between ions and neutral atoms relating to Alfvén waves. Within the plage region itself, the radiative flux was large between patches of strong magnetic field strength in the photosphere or at the edges of magnetic patches. On the other hand, we do not find any significant spatial correlation between the enhanced radiative flux and the chromospheric magnetic field strength or the electric current. In addition to the Alfvén wave turbulence or collisions between ions and neutral atoms relating to Alfvén waves, other heating mechanisms related to magnetic field perturbations produced by interactions of magnetic flux tubes could be at work in the plage chromosphere. 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: Magnetic field structures associated with chromospheric heating in a plage region Authors: Anan, T.; Schad, T.; Kitai, R.; Dima, G.; Jaeggli, S.; Collados, M.; Dominguez-Tagle, C.; Kleint, L. Bibcode: 2021AAS...23821222A Altcode: The strongest quasi-steady heating in the solar atmosphere occurs in the active chromosphere and in particular within plage regions. Our aim is to investigate the relation between magnetic structures and the signatures of heating in the plage regions so as to clarify what mechanisms are at work. We observed a plage region in NOAA active region 12723 in the near infrared He I triplet and Si I 1082.7 nm on 2018 October 3 using the Integral Field Unit mode of the GREGOR Infrared Spectrograph (GRIS) installed at the GREGOR telescope. At the same time, the Interface Region Imaging Spectrograph (IRIS) obtained spectra in the ultra-violet Mg II h & k doublet emitted from the same region. We applied the HAnle and ZEeman Light v2.0 inversion code (HAZEL v2.0) to the GRIS data to infer the photospheric and chromospheric magnetic field. We find that the radiative flux of the Mg II was large between patches of strong magnetic field strength in the photosphere, or at edges of the magnetic patches. On the other hand, the spatial correspondences between the Mg II flux and the magnetic field strength in the chromosphere and between the Mg II flux and the electric current are not so clear. In conclusion, chromospheric heatings in the plage region can be related to magnetic field perturbations produced by interactions of magnetic flux tubes. 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 Molecules to Investigate Cool Gas on the Sun with DKIST Authors: Jaeggli, Sarah Bibcode: 2021cosp...43E.970J Altcode: Simple molecules form in the solar atmosphere in regions of cool plasma. Molecules are physically interesting and provide critical diagnostics of cool plasma. They are sensitive to temperature and pressure, and some molecular lines are even magnetically sensitive. Strong absorption lines from molecules such as OH, CN, and CO are prominent in sunspot spectra. Molecular hydrogen, which has a noted absence of lines in the visible and infrared, may actually be the most abundant molecular species, comprising 10% of the total hydrogen population in very cool sunspot umbrae. CH, which is ubiquitous in the quiet-Sun, dissociates in hotter regions, revealing the features known as G-band bright points. The strongest lines of the fundamental band of CO at 4.6 um reveal what has been interpreted as a mix of hot and cool gas at the roots of the chromosphere. The U.S. National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST) will provide new observations of the Sun with unprecedented spatial and temporal resolution. DKIST instruments are designed to target atomic and molecular diagnostics to address a variety of science cases. Molecular diagnostics throughout the visible spectrum can be explored with the Visible Spectropolarimeter (ViSP). The Diffraction-Limited Near-Infrared Spectropolarimeter (DL-NIRSP) can be used to explore the dynamic behavior of OH in sunspots alongside sensitive magnetic field diagnostics of Fe I at 1565 nm using its integral field unit. The Cryogenic Near-Infrared Spectropolarimeter will provide the chance for detailed study of the 4.6 um CO lines on disk and at the limb. 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: Polarization modeling and predictions for Daniel K. Inouye Solar Telescope, part 6: fringe mitigation with polycarbonate modulators and optical contact calibration retarders Authors: Harrington, David M.; Jaeggli, Sarah A.; Schad, Tom A.; White, Amanda J.; Sueoka, Stacey R. Bibcode: 2020JATIS...6c8001H Altcode: Interference fringes are a major source of systematic error in astronomical spectropolarimeters. We apply the Berreman formalism with recent spatial fringe aperture averaging estimates to design and fabricate new fringe-suppressed polarization optics for several Daniel K. Inouye Solar Telescope (DKIST) use cases. We successfully performed an optical contact bond on a 120-mm-diameter compound crystal retarder for calibration with wavelength-dependent fringe suppression factors of one to three orders of magnitude. Special rotational alignment procedures were developed to minimize spectral oscillations, which we show here to represent our calibration stability limit under retarder thermal perturbation. We developed a fabrication technique to deliver low beam deflection for our large aperture polycarbonate (PC) retarders. Modulators are upgraded in two DKIST instruments with minimal beam deflection and bandpass-optimized antireflection coatings for fringe suppression factors of hundreds. We confirm that PC retarders do fringe as expected when low deflection is achieved. We show that increased retardance spatial variation from PC does not degrade modulation efficiency. Title: Observing Solar Plasma Environments with DKIST Authors: Jaeggli, Sarah Bibcode: 2020APS..DPPD02001J Altcode: The Sun displays diverse plasma environments structured by magnetic fields. The largely neutral photosphere is sprinkled with ∼1 kG magnetic fields rooted in the underlying convection zone. Just above this magneto-acoustic shocks and rapidly expanding magnetic fields create complex and dynamic structures interspersed with quiescent and eruptive phenomena in the chromosphere. The average temperature increases through the chromosphere abruptly jumps to >106 K in the solar corona. These different regimes are directly coupled by many processes that have been extensively studied using a combination of theory, simulations, and laboratory experiments: dynamos, waves, instabilities, and reconnection. The National Science Foundation's Daniel K. Inouye Solar Telescope is an unprecedented new facility that will allow for measurements of the highest spatial resolution and superb signal to noise on shorter timescales than ever before. First light instruments will provide simultaneous multi-wavelength observations with spectral and polarimetric capabilities on disk and above the limb. Coupled with radiative MHD modeling, this can provide 3D diagnosis of plasma parameters (e.g. magnetic field vector, temperature) over the plasma regimes found throughout the Sun's atmosphere. Title: Shock Heating Energy of Umbral Flashes Measured with Integral Field Unit Spectroscopy Authors: Anan, Tetsu; Schad, Thomas A.; Jaeggli, Sarah A.; Tarr, Lucas A. Bibcode: 2019ApJ...882..161A Altcode: 2019arXiv190710797A Umbral flashes are periodic brightness increases routinely observed in the core of chromospheric lines within sunspot umbrae and are attributed to propagating shock fronts. In this work we quantify the shock heating energy of these umbral flashes using observations in the near-infrared He I triplet obtained on 2014 December 7 with the SpectroPolarimetric Imager for the Energetic Sun, which is a novel integral field unit spectrograph at the Dunn Solar Telescope. We determine the shock properties (the Mach number and the propagation speed) by fitting the measured He I spectral profiles with a theoretical radiative transfer model consisting of two constant-property atmospheric slabs whose temperatures and macroscopic velocities are constrained by the Rankine-Hugoniot relations. From the Mach number, the shock heating energy per unit mass of plasma is derived to be 2 × 1010 erg g-1, which is insufficient to maintain the umbral chromosphere. In addition, we find that the shocks propagate upward with the sound speed and the Mach number does not depend on the temperature upstream of the shocks. The latter may imply suppression of the amplification of the Mach number due to energy loss of the shocks. Title: Optical Alignment of DL-NIRSP Spectrograph Authors: Jaeggli, Sarah A.; Anan, Tetsu; Kramar, Maxim; Lin, Haosheng Bibcode: 2019AAS...23410612J Altcode: The Diffraction-Limited Near-Infrared Spectropolarimeter (DL-NIRSP) will be delivered as part of the first light instrumentation for the Daniel K. Inouye Solar Telescope (DKIST) and is currently undergoing lab integration at the University of Hawai'i Institute for Astronomy's Advanced Technology Research Center on Maui. An off-axis hyperbolic mirror, with a focal length of 1250 mm, is used as both collimator and camera in the spectrograph, and makes this system particularly difficult to align. The optical axis, or vertex, of the parent surface is located approximately 260 mm from the center of the off-axis section of the mirror, but there is no direct physical or optical reference for the location and orientation of the optical axis. We have made use of vendor data and a coordinate measuring machine (CMM) arm to transfer coordinates from the back and perimeter surfaces of the mirror to locate the optical axis focus and place the other optical components in reference to this mechanical model. In coordination, we have conducted tests of the optical quality at various points during the alignment to ensure that the mechanical tolerances maintain the optical quality of the system so that the instrument will be able to achieve excellent spectral resolution limited by the spectrograph slit width (λ/Δλ 250,000), and preserve the diffraction limited spatial resolution provided by the telescope and feed optics (0.06" at 1 μm). Title: Transient dynamics and energy transfer from the photosphere to the low corona: initial results from a coordinated ALMA, DST, Hinode, IRIS, and SDO observation campaign Authors: Kobelski, Adam; Tarr, Lucas A.; Jaeggli, Sarah A.; Savage, Sabrina Bibcode: 2019AAS...23430702K Altcode: We present initial results from a coordinated observation campaign to study transient dynamics and energy transfer in the low solar atmosphere. The observations ran from approximately 2017-03-21 from 13UT to 19UT, and include data from Hinode, IRIS, DST, and ALMA. The target, a small, magnetically bipolar active area associated with a coronal bright point, was chosen for showing reasonable dynamics in the chromosphere (as dictated by AIA 304 data from the day prior), and being near disk center to better facilitate magnetic field measurement. The campaign was designed to capture the dynamics of the target with as rapid a timescale as possible for each instrument. Photospheric dynamics are available from broadband IBIS data and the HMI. New to this dataset, the chromospheric dynamics were observed in radio frequencies using ALMA (Band 3: 92-108GHz) at a 2s cadence. Additional chromospheric data are spectral H-α from the IBIS instrument at the DST, spectropolarimetic HeI 10830 from the FIRS instrument at the DST, and the medium linelist from IRIS; coronal data includes imaging from XRT and spectral data from EIS. In this first set of results, we discuss the frequency of transient brightenings observed in each set of imaging data and how the spatial distribution relates across each data channel and to the regions magnetic topology. Title: Shock heating energy in an umbra of a sunspot with integral field unit spectroscopy Authors: Anan, Tetsu; Schad, Thomas A.; Jaeggli, Sarah A.; Tarr, Lucas A. Bibcode: 2019AAS...23421705A Altcode: On 2014 December 7 we used new integral field spectroscopy techniques to observe umbral flashes, which are periodic brightness increases routinely observed in the core of chromospheric lines within sunspot umbrae and are attributed to propagating shock fronts. In this work we quantify the shock heating energy of these umbral flashes using observations in the near infrared HeI triplet obtained with the SpectroPolarimetric Imager for the Energetic Sun (SPIES), which is novel integral field unit spectrograph at the Dunn Solar Telescope. We determine the shock properties (the Mach number and the propagation speed) by fitting the measured HeI spectral profiles with a theoretical radiative transfer model using two constant property atmospheric slabs whose temperatures and macroscopic velocities are constrained by the Rankine-Hugoniot relations. From the Mach number, the shock heating energy per unit mass of plasma is derived as 2 x 1010 erg/g. We conclude that the estimated shock heating energy rate is less than the amount required to maintain the umbral chromosphere. Title: Shock Heating Energy in an umbra of a sunspot Authors: Anan, Tetsu; Schad, Tom; Jaeggli, Sarah Bibcode: 2019EGUGA..2113543A Altcode: In December 7, 2014, umbral flashes, which are periodic brightness increases in chromospheric spectral lines of the umbrae due to shocks, were observed in near infrared He I triplet with an integral-field-unit spectrometer, SPIES (SpectroPolarimetric Imager for the Energetic Sun) on the Dunn Solar Telescope with a cadence of 14 seconds. The SPIES is a prototype instruments of a facility instrument of the Daniel K. Inouye Solar Telescope. In order to determine Mach number at upstream of shock waves, we fit the measured spectral profiles in the He I 1083 nm triplet with theoretical profiles computed with a radiative transfer equation using an atmospheric model based on two constant property slabs, of which temperatures and macroscopic velocities are constrained by the Rankine-Hugoniot relations. From the Mach number and the temperature, shock heating energy per unit mass of plasma is derived as 2.0 x 10 ^ {10} erg/g. Finding a positive correlation between a spatial variation of the chromospheric temperature and shock speed, we concluded that prominent heating mechanism can be related with the shock, although estimated shock heating energy rate is less than the required amount of energy to maintain the umbral chromosphere. Title: VizieR Online Data Catalog: UV spectrum of molecular hydrogen in the Sun (Jaeggli+, 2018) Authors: Jaeggli, S. A.; Judge, P. G.; Daw, A. N. Bibcode: 2019yCat..18550134J Altcode: Ultraviolet (UV) lines of molecular hydrogen have been observed in solar spectra for almost four decades, but the behavior of the molecular spectrum and its implications for solar atmospheric structure are not fully understood. Data from the High-Resolution Telescope Spectrometer (HRTS) instrument revealed that H2 emission forms in particular regions, selectively excited by a bright UV transition region and chromospheric lines. We test the conditions under which H2 emission can originate by studying non-LTE models, sampling a broad range of temperature stratifications and radiation conditions. Stratification plays the dominant role in determining the population densities of H2, which forms in greatest abundance near the continuum photosphere. However, opacity due to the photoionization of Si and other neutrals determines the depth to which UV radiation can penetrate to excite the H2. Thus the majority of H2 emission forms in a narrow region, at about 650km in standard one-dimensional (1D) models of the quiet Sun, near the {tau}=1 opacity surface for the exciting UV radiation, generally coming from above. When irradiated from above using observed intensities of bright UV emission lines, detailed non-LTE calculations show that the spectrum of H2 seen in the quiet-Sun Solar Ultraviolet Measurement of Emitted Radiation atlas spectrum and HRTS light-bridge spectrum can be satisfactorily reproduced in 1D stratified atmospheres, without including three-dimensional or time-dependent thermal structures. A detailed comparison to observations from 1205 to 1550Å is presented, and the success of this 1D approach to modeling solar UV H2 emission is illustrated by the identification of previously unidentified lines and upper levels in HRTS spectra.

(3 data files). Title: Instrument Calibration of the Interface Region Imaging Spectrograph (IRIS) Mission Authors: Wülser, J. -P.; Jaeggli, S.; De Pontieu, B.; Tarbell, T.; Boerner, P.; Freeland, S.; Liu, W.; Timmons, R.; Brannon, S.; Kankelborg, C.; Madsen, C.; McKillop, S.; Prchlik, J.; Saar, S.; Schanche, N.; Testa, P.; Bryans, P.; Wiesmann, M. Bibcode: 2018SoPh..293..149W Altcode: The Interface Region Imaging Spectrograph (IRIS) is a NASA small explorer mission that provides high-resolution spectra and images of the Sun in the 133 - 141 nm and 278 - 283 nm wavelength bands. The IRIS data are archived in calibrated form and made available to the public within seven days of observing. The calibrations applied to the data include dark correction, scattered light and background correction, flat fielding, geometric distortion correction, and wavelength calibration. In addition, the IRIS team has calibrated the IRIS absolute throughput as a function of wavelength and has been tracking throughput changes over the course of the mission. As a resource for the IRIS data user, this article describes the details of these calibrations as they have evolved over the first few years of the mission. References to online documentation provide access to additional information and future updates. Title: Predictions of DKIST/DL-NIRSP Observations for an Off-limb Kink-unstable Coronal Loop Authors: Snow, B.; Botha, G. J. J.; Scullion, E.; McLaughlin, J. A.; Young, P. R.; Jaeggli, S. A. Bibcode: 2018ApJ...863..172S Altcode: 2018arXiv180704972S Synthetic intensity maps are generated from a 3D kink-unstable flux rope simulation using several DKIST/DL-NIRSP spectral lines to make a prediction of the observational signatures of energy transport and release. The reconstructed large field-of-view intensity mosaics and single tile sit-and-stare high-cadence image sequences show detailed, fine-scale structure and exhibit signatures of wave propagation, redistribution of heat, flows, and fine-scale bursts. These fine-scale bursts are present in the synthetic Doppler velocity maps and can be interpreted as evidence for small-scale magnetic reconnection at the loop boundary. The spectral lines reveal the different thermodynamic structures of the loop, with the hotter lines showing the loop interior and braiding and the cooler lines showing the radial edges of the loop. The synthetic observations of DL-NIRSP are found to preserve the radial expansion, and hence the loop radius can be measured accurately. The electron number density can be estimated using the intensity ratio of the Fe XIII lines at 10747 and 10798 Å. The estimated density from this ratio is correct to within ±10% during the later phases of the evolution; however, it is less accurate initially when line-of-sight density inhomogeneities contribute to the Fe XIII intensity, resulting in an overprediction of the density by ≈30%. The identified signatures are all above a conservative estimate for instrument noise and therefore will be detectable. In summary, we have used forward modeling to demonstrate that the coronal off-limb mode of DKIST/DL-NIRSP will be able to detect multiple independent signatures of a kink-unstable loop and observe small-scale transient features including loop braiding/twisting and small-scale reconnection events occurring at the radial edge of the loop. 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: Solar UV Molecular Hydrogen Fluorescence Authors: Daw, Adrian Nigel; Jaeggli, Sarah Amelia; Judge, Philip G.; Roueff, Evelyne; Abgrall, Hervé Bibcode: 2018tess.conf21706D Altcode: Solar observations of ultraviolet molecular hydrogen lines indicate that H2 emission forms in particular regions, selectively excited by bright UV transition region and chromospheric lines. IRIS frequently observes numerous H2 lines during flares and smaller energetic events, but the diagnostic value of these lines for probing the structure of the solar atmosphere has heretofore remained largely unexploited. We present a synthesis method for H2 emission, using 1-D non-LTE models sampling a broad range of temperature stratifications and input radiation conditions from the atmosphere above, and compare the results to observations by IRIS, SUMER and HRTS from 1205 to 1550 Å. Because opacity due to photoionization of silicon and other neutrals determines the depth to which UV radiation can penetrate to excite the H2, the majority of H2 emission forms in a narrow region near the tau=1 opacity surface for the exciting UV radiation, generally coming from above. The success of this 1-D approach to modeling solar UV H2 emission is illustrated by the identification of previously unidentified lines and upper levels. Applications of the observed emission and implications for solar atmospheric structure are discussed. Title: Formation of the UV Spectrum of Molecular Hydrogen in the Sun Authors: Jaeggli, S. A.; Judge, P. G.; Daw, A. N. Bibcode: 2018ApJ...855..134J Altcode: 2018arXiv180203779J Ultraviolet (UV) lines of molecular hydrogen have been observed in solar spectra for almost four decades, but the behavior of the molecular spectrum and its implications for solar atmospheric structure are not fully understood. Data from the High-Resolution Telescope Spectrometer (HRTS) instrument revealed that H2 emission forms in particular regions, selectively excited by a bright UV transition region and chromospheric lines. We test the conditions under which H2 emission can originate by studying non-LTE models, sampling a broad range of temperature stratifications and radiation conditions. Stratification plays the dominant role in determining the population densities of H2, which forms in greatest abundance near the continuum photosphere. However, opacity due to the photoionization of Si and other neutrals determines the depth to which UV radiation can penetrate to excite the H2. Thus the majority of H2 emission forms in a narrow region, at about 650 km in standard one-dimensional (1D) models of the quiet Sun, near the τ = 1 opacity surface for the exciting UV radiation, generally coming from above. When irradiated from above using observed intensities of bright UV emission lines, detailed non-LTE calculations show that the spectrum of H2 seen in the quiet-Sun Solar Ultraviolet Measurement of Emitted Radiation atlas spectrum and HRTS light-bridge spectrum can be satisfactorily reproduced in 1D stratified atmospheres, without including three-dimensional or time-dependent thermal structures. A detailed comparison to observations from 1205 to 1550 Å is presented, and the success of this 1D approach to modeling solar UV H2 emission is illustrated by the identification of previously unidentified lines and upper levels in HRTS spectra. Title: Formation of the UV Spectrum of Molecular Hydrogen in the Sun Authors: Jaeggli, S. A.; Judge, P. G.; Daw, A. N. Bibcode: 2017AGUFMSH52B..01J Altcode: UV lines of molecular hydrogen in the Sun have been observed for almost four decades, but the behavior of the spectra and their implications for solar atmospheric structure are not fully understood. Data from the HRTS instrument revealed that H2 emission forms in particular regions, selectively excited by bright UV transition region and chromospheric lines. We test the conditions under which H2 emission can originate by studying non-LTE models with increasingly complex temperature stratification. Stratification plays the dominant role in determining the population densities of H2, which can form in abundance only within about 700 km of the continuum photosphere where 3D and dynamic structure generally play secondary roles to stratification. When irradiated from above using observed intensities of bright UV emission lines, detailed non-LTE calculations show that the spectrum of H2 can be satisfactorily modeled in 1D stratified atmospheric models, with no need to invoke unusual 3D or time dependent thermal structures. 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: Large Scale Coordination of Small Scale Structures Authors: Kobelski, Adam; Tarr, Lucas A.; Jaeggli, Sarah A.; Savage, Sabrina Bibcode: 2017SPD....4820005K Altcode: Transient brightenings are ubiquitous features of the solar atmosphere across many length and energy scales, the most energetic of which manifest as large-class solar flares. Often, transient brightenings originate in regions of strong magnetic activity and create strong observable enhancements across wavelengths from X-ray to radio, with notable dynamics on timescales of seconds to hours.The coronal aspects of these brightenings have often been studied by way of EUV and X-ray imaging and spectra. These events are likely driven by photospheric activity (such as flux emergence) with the coronal brightenings originating largely from chromospheric ablation (evaporation). Until recently, chromospheric and transition region observations of these events have been limited. However, new observational capabilities have become available which significantly enhance our ability to understand the bi-directional flow of energy through the chromosphere between the photosphere and the corona.We have recently obtained a unique data set with which to study this flow of energy through the chromosphere via the Interface Region Imaging Spectrograph (IRIS), Hinode EUV Imaging Spectrometer (EIS), Hinode X-Ray Telescope (XRT), Hinode Solar Optical Telescope (SOT), Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA), SDO Helioseismic and Magnetic Imager (HMI), Nuclear Spectroscopic Telescope Array (NuStar), Atacama Large Millimeter Array (ALMA), and Interferometric BIdimensional Spectropolarimeter (IBIS) at the Dunn Solar Telescope (DST). This data set targets a small active area near disk center which was tracked simultaneously for approximately four hours. Within this region, many transient brightenings detected through multiple layers of the solar atmosphere. In this study, we combine the imaging data and use the spectra from EIS and IRIS to track flows from the photosphere (HMI, SOT) through the chromosphere and transition region (AIA, IBIS, IRIS, ALMA) into the corona (EIS, XRT, AIA). Title: An Update on the Diffraction-Limited Near Infrared Spectropolarimeter for the Daniel K. Inouye Solar Telescope Authors: Jaeggli, Sarah A.; Lin, Haosheng; Onaka, Peter; McGregor, Helen; Yamada, Hubert Bibcode: 2017SPD....4811704J Altcode: DL-NIRSP is an integral field imaging spectropolarimeter for photospheric, chromospheric, and coronal magnetic field studies which is currently under development by the University of Hawaii’s Institute for Astronomy as part of the first light instrument suite for DKIST. DL-NIRSP pairs a multi-slit fiber-optic image slicer with narrow bandpass isolation filters and large format detectors to achieve very high cadence observations in three simultaneous wavelength channels in the Visible-IR. Planned diagnostics at first light include Fe XI 789.2 nm, Ca II 854.2 nm, Fe XIII 1074.7 nm, Si I/He I 1083.0 nm, Si X 1430.0 nm, and Fe I 1565.0 nm. More spectral lines will be added in the future. As the last stop in the DKIST light distribution system, DL-NIRSP will receive an AO corrected beam and will be able to operate simultaneously with the other visible light instruments. We provide an update on the current challenges and rewards yet to come with DL-NIRSP. Title: The Magnetic Classification of Solar Active Regions 1992-2015 Authors: Jaeggli, S. A.; Norton, A. A. Bibcode: 2016ApJ...820L..11J Altcode: 2016arXiv160302552J The purpose of this Letter is to address a blindspot in our knowledge of solar active region (AR) statistics. To the best of our knowledge, there are no published results showing the variation of the Mount Wilson magnetic classifications as a function of solar cycle based on modern observations. We show statistics for all ARs reported in the daily Solar Region Summary from 1992 January 1 to 2015 December 31. We find that the α and β class ARs (including all sub-groups, e.g., βγ, βδ) make up fractions of approximately 20% and 80% of the sample, respectively. This fraction is relatively constant during high levels of activity however, an increase in the α fraction to about 35% and and a decrease in the β fraction to about 65% can be seen near each solar minimum and are statistically significant at the 2σ level. Over 30% of all ARs observed during the years of solar maxima were appended with the classifications γ and/or δ, while these classifications account for only a fraction of a percent during the years near the solar minima. This variation in the AR types indicates that the formation of complex ARs may be due to the pileup of frequent emergence of magnetic flux during solar maximum, rather than the emergence of complex, monolithic flux structures. Title: Multi-wavelength Study of a Delta-spot. I. A Region of Very Strong, Horizontal Magnetic Field Authors: Jaeggli, S. A. Bibcode: 2016ApJ...818...81J Altcode: 2015arXiv151208463J Active region NOAA 11035 appeared in 2009 December, early in the new solar activity cycle. This region achieved a delta sunspot (δ spot) configuration when parasitic flux emerged near the rotationally leading magnetic polarity and traveled through the penumbra of the largest sunspot in the group. Both visible and infrared imaging spectropolarimetry of the magnetically sensitive Fe I line pairs at 6302 and 15650 Å show large Zeeman splitting in the penumbra between the parasitic umbra and the main sunspot umbra. The polarized Stokes spectra in the strongest field region display anomalous profiles, and strong blueshifts are seen in an adjacent region. Analysis of the profiles is carried out using a Milne-Eddington inversion code capable of fitting either a single magnetic component with stray light or two independent magnetic components to verify the field strength. The inversion results show that the anomalous profiles cannot be produced by the combination of two profiles with moderate magnetic fields. The largest field strengths are 3500-3800 G in close proximity to blueshifts as strong as 3.8 km s-1. The strong, nearly horizontal magnetic field seen near the polarity inversion line in this region is difficult to understand in the context of a standard model of sunspot magnetohydrostatic equilibrium. Title: The Persistence of Apparent Non-Magnetostatic Equilibrium in NOAA 11035 Authors: Jaeggli, Sarah A. Bibcode: 2015IAUS..305...35J Altcode: 2015arXiv150401325J NOAA 11035 was a highly sheared active region that appeared in December 2009 early in the new activity cycle. The leading polarity sunspot developed a highly unusual feature in its penumbra, an opposite polarity pore with a strong magnetic field in excess of 3500 G along one edge, which persisted for several days during the evolution of the region. This region was well observed by both space- and ground-based observatories, including Hinode, FIRS, TRACE, and SOHO. These observations, which span wavelength and atmospheric regimes, provide a complete picture of this unusual feature which may constitute a force-free magnetic field in the photosphere which is produced by the reconnection of magnetic loops low in the solar atmosphere. Title: A very strong magnetic field region in NOAA 11035 Authors: Jaeggli, Sarah Amelia Bibcode: 2015TESS....111304J Altcode: NOAA 11035 was a fairly typical active region that emerged near the central meridian 13-14 December 2009, early in solar cycle 24. During the active region’s rapid emergence and evolution, a deeply-rooted magnetic bipole emerged into the pre-existing leading polarity with spectacular consequences. Multi-wavelength imaging and spectropolarimetry from FIRS, IBIS, Hinode, TRACE, and SOHO allow for a comprehensive investigation of the physical processes present in this region. Intrusion of the opposite polarity into the leading sunspot’s penumbra resulted in a region of highly concentrated horizontal magnetic field, with a peak field strength larger than 3600 G based on Milne-Eddington inversion of Fe I spectropolarimetry at 6302 and 15650 Å. Photospheric velocity measurements show blueshifts of 4 km/sec along the neutral line, which are coincident with a dark chromospheric structure in He I 10830 and H I 6563 Å. We conclude that these signatures are the result of continuous magnetic reconnection near photospheric heights. Title: Internetwork Chromospheric Bright Grains Observed With IRIS and SST Authors: Martínez-Sykora, Juan; Rouppe van der Voort, Luc; Carlsson, Mats; De Pontieu, Bart; Pereira, Tiago M. D.; Boerner, Paul; Hurlburt, Neal; Kleint, Lucia; Lemen, James; Tarbell, Ted D.; Title, Alan; Wuelser, Jean-Pierre; Hansteen, Viggo H.; Golub, Leon; McKillop, Sean; Reeves, Kathy K.; Saar, Steven; Testa, Paola; Tian, Hui; Jaeggli, Sarah; Kankelborg, Charles Bibcode: 2015ApJ...803...44M Altcode: 2015arXiv150203490M The Interface Region Imaging Spectrograph (IRIS) reveals small-scale rapid brightenings in the form of bright grains all over coronal holes and the quiet Sun. These bright grains are seen with the IRIS 1330, 1400, and 2796 Å slit-jaw filters. We combine coordinated observations with IRIS and from the ground with the Swedish 1 m Solar Telescope (SST) which allows us to have chromospheric (Ca ii 8542 Å, Ca ii H 3968 Å, Hα, and Mg ii k 2796 Å) and transition region (C ii 1334 Å, Si iv 1403 Å) spectral imaging, and single-wavelength Stokes maps in Fe i 6302 Å at high spatial (0\buildrel{\prime\prime}\over{.} 33), temporal, and spectral resolution. We conclude that the IRIS slit-jaw grains are the counterpart of so-called acoustic grains, i.e., resulting from chromospheric acoustic waves in a non-magnetic environment. We compare slit-jaw images (SJIs) with spectra from the IRIS spectrograph. We conclude that the grain intensity in the 2796 Å slit-jaw filter comes from both the Mg ii k core and wings. The signal in the C ii and Si iv lines is too weak to explain the presence of grains in the 1300 and 1400 Å SJIs and we conclude that the grain signal in these passbands comes mostly from the continuum. Although weak, the characteristic shock signatures of acoustic grains can often be detected in IRIS C ii spectra. For some grains, a spectral signature can be found in IRIS Si iv. This suggests that upward propagating acoustic waves sometimes reach all the way up to the transition region. Title: Homologous Helical Jets: Observations By IRIS, SDO, and Hinode and Magnetic Modeling With Data-Driven Simulations Authors: Cheung, Mark C. M.; De Pontieu, B.; Tarbell, T. D.; Fu, Y.; Tian, H.; Testa, P.; Reeves, K. K.; Martínez-Sykora, J.; Boerner, P.; Wülser, J. P.; Lemen, J.; Title, A. M.; Hurlburt, N.; Kleint, L.; Kankelborg, C.; Jaeggli, S.; Golub, L.; McKillop, S.; Saar, S.; Carlsson, M.; Hansteen, V. Bibcode: 2015ApJ...801...83C Altcode: 2015arXiv150101593C We report on observations of recurrent jets by instruments on board the Interface Region Imaging Spectrograph, Solar Dynamics Observatory (SDO), and Hinode spacecraft. Over a 4 hr period on 2013 July 21, recurrent coronal jets were observed to emanate from NOAA Active Region 11793. Far-ultraviolet spectra probing plasma at transition region temperatures show evidence of oppositely directed flows with components reaching Doppler velocities of ±100 km s-1. Raster Doppler maps using a Si iv transition region line show all four jets to have helical motion of the same sense. Simultaneous observations of the region by SDO and Hinode show that the jets emanate from a source region comprising a pore embedded in the interior of a supergranule. The parasitic pore has opposite polarity flux compared to the surrounding network field. This leads to a spine-fan magnetic topology in the coronal field that is amenable to jet formation. Time-dependent data-driven simulations are used to investigate the underlying drivers for the jets. These numerical experiments show that the emergence of current-carrying magnetic field in the vicinity of the pore supplies the magnetic twist needed for recurrent helical jet formation. Title: The 2014 March 29 X-flare: Subarcsecond Resolution Observations of Fe XXI λ1354.1 Authors: Young, Peter R.; Tian, Hui; Jaeggli, Sarah Bibcode: 2015ApJ...799..218Y Altcode: 2014arXiv1409.8603Y The Interface Region Imaging Spectrometer (IRIS) is the first solar instrument to observe ~10 MK plasma at subarcsecond spatial resolution through imaging spectroscopy of the Fe XXI λ1354.1 forbidden line. IRIS observations of the X1 class flare that occurred on 2014 March 29 at 17:48 UT reveal Fe XXI emission from both the flare ribbons and the post-flare loop arcade. Fe XXI appears at all of the chromospheric ribbon sites, although typically with a delay of one raster (75 s) and sometimes offset by up to 1''. 100-200 km s-1 blue-shifts are found at the brightest ribbons, suggesting hot plasma upflow into the corona. The Fe XXI ribbon emission is compact with a spatial extent of <2'', and can extend beyond the chromospheric ribbon locations. Examples are found of both decreasing and increasing blue-shift in the direction away from the ribbon locations, and blue-shifts were present for at least six minutes after the flare peak. The post-flare loop arcade, seen in Atmospheric Imaging Assembly 131 Å filtergram images that are dominated by Fe XXI, exhibited bright loop-tops with an asymmetric intensity distribution. The sizes of the loop-tops are resolved by IRIS at >=1'', and line widths in the loop-tops are not broader than in the loop-legs suggesting the loop-tops are not sites of enhanced turbulence. Line-of-sight speeds in the loop arcade are typically <10 km s-1, and mean non-thermal motions fall from 43 km s-1 at the flare peak to 26 km s-1 six minutes later. If the average velocity in the loop arcade is assumed to be at rest, then it implies a new reference wavelength for the Fe XXI line of 1354.106 ± 0.023 Å. Title: Venus' thermospheric temperature field using a refraction model at terminator : comparison with 2012 transit observations using SDO/HMI, VEx/SPICAV/SOIR and NSO/DST/FIRS Authors: Widemann, Thomas; Jaeggli, Sarah; Reardon, Kevin; Tanga, Paolo; Père, Christophe; Pasachoff, Jay M.; Vandaele, Ann Carine; Wilquet, Valerie; Mahieux, Arnaud; Wilson, Colin Bibcode: 2014DPS....4630206W Altcode: The transit of Venus in June 2012 provided a unique case study of the Venus' atmosphere transiting in front of the Sun, while at the same time ESA's Venus Express orbiter observed the evening terminator at solar ingress and solar egress.We report on mesospheric temperature at Venus' morning terminator using SDO/HMI aureole photometry and comparison with Venus Express. Close to ingress and egress phases, we have shown that the aureole photometry reflects the local density scale height and the altitude of the refracting layer (Tanga et al. 2012). The lightcurve of each spatially resolved aureole element is fit to a two-parameter model to constrain the meridional temperature gradient at terminator. Our measurements are in agreement with the VEx/SOIR temperatures obtained during orbit 2238 at evening terminator during solar ingress (46.75N - LST = 6.075PM) and solar egress (31.30N - LST = 6.047PM) captured from the Venus Express orbiter at the time Venus transited the Sun.We also performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption. Observations were taken during the first half of the transit using the Facility InfraRed Spectropolarimeter (FIRS) on the Dunn Solar Telescope (DST). Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric lines. Sun-subtracted Venus limb observations show intensity distribution of vibrational CO2 bands 221 2v+2v2+v3 at 1.571μm and 141 v1+4v2+v3 at 1.606μm. Title: Hot explosions in the cool atmosphere of the Sun Authors: Peter, H.; Tian, H.; Curdt, W.; Schmit, D.; Innes, D.; De Pontieu, B.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Martínez-Sykora, Juan; Kleint, L.; Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.; Kankelborg, C.; Jaeggli, S.; Carlsson, M.; Hansteen, V. Bibcode: 2014Sci...346C.315P Altcode: 2014arXiv1410.5842P The solar atmosphere was traditionally represented with a simple one-dimensional model. Over the past few decades, this paradigm shifted for the chromosphere and corona that constitute the outer atmosphere, which is now considered a dynamic structured envelope. Recent observations by the Interface Region Imaging Spectrograph (IRIS) reveal that it is difficult to determine what is up and down, even in the cool 6000-kelvin photosphere just above the solar surface: This region hosts pockets of hot plasma transiently heated to almost 100,000 kelvin. The energy to heat and accelerate the plasma requires a considerable fraction of the energy from flares, the largest solar disruptions. These IRIS observations not only confirm that the photosphere is more complex than conventionally thought, but also provide insight into the energy conversion in the process of magnetic reconnection. Title: The unresolved fine structure resolved: IRIS observations of the solar transition region Authors: Hansteen, V.; De Pontieu, B.; Carlsson, M.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Pereira, T. M. D.; De Luca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.; Kankelborg, C.; Jaeggli, S.; Kleint, L.; Martínez-Sykora, J. Bibcode: 2014Sci...346E.315H Altcode: 2014arXiv1412.3611H The heating of the outer solar atmospheric layers, i.e., the transition region and corona, to high temperatures is a long-standing problem in solar (and stellar) physics. Solutions have been hampered by an incomplete understanding of the magnetically controlled structure of these regions. The high spatial and temporal resolution observations with the Interface Region Imaging Spectrograph (IRIS) at the solar limb reveal a plethora of short, low-lying loops or loop segments at transition-region temperatures that vary rapidly, on the time scales of minutes. We argue that the existence of these loops solves a long-standing observational mystery. At the same time, based on comparison with numerical models, this detection sheds light on a critical piece of the coronal heating puzzle. Title: Evidence of nonthermal particles in coronal loops heated impulsively by nanoflares Authors: Testa, P.; De Pontieu, B.; Allred, J.; Carlsson, M.; Reale, F.; Daw, A.; Hansteen, V.; Martinez-Sykora, J.; Liu, W.; DeLuca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Tian, H.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kleint, L.; Kankelborg, C.; Jaeggli, S. Bibcode: 2014Sci...346B.315T Altcode: 2014arXiv1410.6130T The physical processes causing energy exchange between the Sun’s hot corona and its cool lower atmosphere remain poorly understood. The chromosphere and transition region (TR) form an interface region between the surface and the corona that is highly sensitive to the coronal heating mechanism. High-resolution observations with the Interface Region Imaging Spectrograph (IRIS) reveal rapid variability (~20 to 60 seconds) of intensity and velocity on small spatial scales (≲500 kilometers) at the footpoints of hot and dynamic coronal loops. The observations are consistent with numerical simulations of heating by beams of nonthermal electrons, which are generated in small impulsive (≲30 seconds) heating events called “coronal nanoflares.” The accelerated electrons deposit a sizable fraction of their energy (≲1025 erg) in the chromosphere and TR. Our analysis provides tight constraints on the properties of such electron beams and new diagnostics for their presence in the nonflaring corona. Title: Prevalence of small-scale jets from the networks of the solar transition region and chromosphere Authors: Tian, H.; DeLuca, E. E.; Cranmer, S. R.; De Pontieu, B.; Peter, H.; Martínez-Sykora, J.; Golub, L.; McKillop, S.; Reeves, K. K.; Miralles, M. P.; McCauley, P.; Saar, S.; Testa, P.; Weber, M.; Murphy, N.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kleint, L.; Kankelborg, C.; Jaeggli, S.; Carlsson, M.; Hansteen, V.; McIntosh, S. W. Bibcode: 2014Sci...346A.315T Altcode: 2014arXiv1410.6143T As the interface between the Sun’s photosphere and corona, the chromosphere and transition region play a key role in the formation and acceleration of the solar wind. Observations from the Interface Region Imaging Spectrograph reveal the prevalence of intermittent small-scale jets with speeds of 80 to 250 kilometers per second from the narrow bright network lanes of this interface region. These jets have lifetimes of 20 to 80 seconds and widths of ≤300 kilometers. They originate from small-scale bright regions, often preceded by footpoint brightenings and accompanied by transverse waves with amplitudes of ~20 kilometers per second. Many jets reach temperatures of at least ~105 kelvin and constitute an important element of the transition region structures. They are likely an intermittent but persistent source of mass and energy for the solar wind. Title: On the prevalence of small-scale twist in the solar chromosphere and transition region Authors: De Pontieu, B.; Rouppe van der Voort, L.; McIntosh, S. W.; Pereira, T. M. D.; Carlsson, M.; Hansteen, V.; Skogsrud, H.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; De Luca, E. E.; Golub, L.; McKillop, S.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.; Kankelborg, C.; Jaeggli, S.; Kleint, L.; Martinez-Sykora, J. Bibcode: 2014Sci...346D.315D Altcode: 2014arXiv1410.6862D The solar chromosphere and transition region (TR) form an interface between the Sun’s surface and its hot outer atmosphere. There, most of the nonthermal energy that powers the solar atmosphere is transformed into heat, although the detailed mechanism remains elusive. High-resolution (0.33-arc second) observations with NASA’s Interface Region Imaging Spectrograph (IRIS) reveal a chromosphere and TR that are replete with twist or torsional motions on sub-arc second scales, occurring in active regions, quiet Sun regions, and coronal holes alike. We coordinated observations with the Swedish 1-meter Solar Telescope (SST) to quantify these twisting motions and their association with rapid heating to at least TR temperatures. This view of the interface region provides insight into what heats the low solar atmosphere. Title: An Interface Region Imaging Spectrograph First View on Solar Spicules Authors: Pereira, T. M. D.; De Pontieu, B.; Carlsson, M.; Hansteen, V.; Tarbell, T. D.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Wülser, J. P.; Martínez-Sykora, J.; Kleint, L.; Golub, L.; McKillop, S.; Reeves, K. K.; Saar, S.; Testa, P.; Tian, H.; Jaeggli, S.; Kankelborg, C. Bibcode: 2014ApJ...792L..15P Altcode: 2014arXiv1407.6360P Solar spicules have eluded modelers and observers for decades. Since the discovery of the more energetic type II, spicules have become a heated topic but their contribution to the energy balance of the low solar atmosphere remains unknown. Here we give a first glimpse of what quiet-Sun spicules look like when observed with NASA's recently launched Interface Region Imaging Spectrograph (IRIS). Using IRIS spectra and filtergrams that sample the chromosphere and transition region, we compare the properties and evolution of spicules as observed in a coordinated campaign with Hinode and the Atmospheric Imaging Assembly. Our IRIS observations allow us to follow the thermal evolution of type II spicules and finally confirm that the fading of Ca II H spicules appears to be caused by rapid heating to higher temperatures. The IRIS spicules do not fade but continue evolving, reaching higher and falling back down after 500-800 s. Ca II H type II spicules are thus the initial stages of violent and hotter events that mostly remain invisible in Ca II H filtergrams. These events have very different properties from type I spicules, which show lower velocities and no fading from chromospheric passbands. The IRIS spectra of spicules show the same signature as their proposed disk counterparts, reinforcing earlier work. Spectroheliograms from spectral rasters also confirm that quiet-Sun spicules originate in bushes from the magnetic network. Our results suggest that type II spicules are indeed the site of vigorous heating (to at least transition region temperatures) along extensive parts of the upward moving spicular plasma. Title: Molecular absorption in transition region spectral lines Authors: Schmit, D. J.; Innes, D.; Ayres, T.; Peter, H.; Curdt, W.; Jaeggli, S. Bibcode: 2014A&A...569L...7S Altcode: 2014arXiv1409.1702S
Aims: We present observations from the Interface Region Imaging Spectrograph (IRIS) of absorption features from a multitude of cool atomic and molecular lines within the profiles of Si IV transition region lines. Many of these spectral lines have not previously been detected in solar spectra.
Methods: We examined spectra taken from deep exposures of plage on 12 October 2013. We observed unique absorption spectra over a magnetic element which is bright in transition region line emission and the ultraviolet continuum. We compared the absorption spectra with emission spectra that is likely related to fluorescence.
Results: The absorption features require a population of sub-5000 K plasma to exist above the transition region. This peculiar stratification is an extreme deviation from the canonical structure of the chromosphere-corona boundary. The cool material is not associated with a filament or discernible coronal rain. This suggests that molecules may form in the upper solar atmosphere on small spatial scales and introduces a new complexity into our understanding of solar thermal structure. It lends credence to previous numerical studies that found evidence for elevated pockets of cool gas in the chromosphere.

Movies associated to Figs. 1 and 2 are available in electronic form at http://www.aanda.org Title: The Interface Region Imaging Spectrograph (IRIS) Authors: De Pontieu, B.; Title, A. M.; Lemen, J. R.; Kushner, G. D.; Akin, D. J.; Allard, B.; Berger, T.; Boerner, P.; Cheung, M.; Chou, C.; Drake, J. F.; Duncan, D. W.; Freeland, S.; Heyman, G. F.; Hoffman, C.; Hurlburt, N. E.; Lindgren, R. W.; Mathur, D.; Rehse, R.; Sabolish, D.; Seguin, R.; Schrijver, C. J.; Tarbell, T. D.; Wülser, J. -P.; Wolfson, C. J.; Yanari, C.; Mudge, J.; Nguyen-Phuc, N.; Timmons, R.; van Bezooijen, R.; Weingrod, I.; Brookner, R.; Butcher, G.; Dougherty, B.; Eder, J.; Knagenhjelm, V.; Larsen, S.; Mansir, D.; Phan, L.; Boyle, P.; Cheimets, P. N.; DeLuca, E. E.; Golub, L.; Gates, R.; Hertz, E.; McKillop, S.; Park, S.; Perry, T.; Podgorski, W. A.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.; Weber, M.; Dunn, C.; Eccles, S.; Jaeggli, S. A.; Kankelborg, C. C.; Mashburn, K.; Pust, N.; Springer, L.; Carvalho, R.; Kleint, L.; Marmie, J.; Mazmanian, E.; Pereira, T. M. D.; Sawyer, S.; Strong, J.; Worden, S. P.; Carlsson, M.; Hansteen, V. H.; Leenaarts, J.; Wiesmann, M.; Aloise, J.; Chu, K. -C.; Bush, R. I.; Scherrer, P. H.; Brekke, P.; Martinez-Sykora, J.; Lites, B. W.; McIntosh, S. W.; Uitenbroek, H.; Okamoto, T. J.; Gummin, M. A.; Auker, G.; Jerram, P.; Pool, P.; Waltham, N. Bibcode: 2014SoPh..289.2733D Altcode: 2014arXiv1401.2491D; 2014SoPh..tmp...25D The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 - 0.4 arcsec spatial resolution, two-second temporal resolution, and 1 km s−1 velocity resolution over a field-of-view of up to 175 arcsec × 175 arcsec. IRIS was launched into a Sun-synchronous orbit on 27 June 2013 using a Pegasus-XL rocket and consists of a 19-cm UV telescope that feeds a slit-based dual-bandpass imaging spectrograph. IRIS obtains spectra in passbands from 1332 - 1358 Å, 1389 - 1407 Å, and 2783 - 2834 Å, including bright spectral lines formed in the chromosphere (Mg II h 2803 Å and Mg II k 2796 Å) and transition region (C II 1334/1335 Å and Si IV 1394/1403 Å). Slit-jaw images in four different passbands (C II 1330, Si IV 1400, Mg II k 2796, and Mg II wing 2830 Å) can be taken simultaneously with spectral rasters that sample regions up to 130 arcsec × 175 arcsec at a variety of spatial samplings (from 0.33 arcsec and up). IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by IRIS each day and made available for unrestricted use within a few days of the observation. Title: Detection of Supersonic Downflows and Associated Heating Events in the Transition Region above Sunspots Authors: Kleint, L.; Antolin, P.; Tian, H.; Judge, P.; Testa, P.; De Pontieu, B.; Martínez-Sykora, J.; Reeves, K. K.; Wuelser, J. P.; McKillop, S.; Saar, S.; Carlsson, M.; Boerner, P.; Hurlburt, N.; Lemen, J.; Tarbell, T. D.; Title, A.; Golub, L.; Hansteen, V.; Jaeggli, S.; Kankelborg, C. Bibcode: 2014ApJ...789L..42K Altcode: 2014arXiv1406.6816K Interface Region Imaging Spectrograph data allow us to study the solar transition region (TR) with an unprecedented spatial resolution of 0.''33. On 2013 August 30, we observed bursts of high Doppler shifts suggesting strong supersonic downflows of up to 200 km s-1 and weaker, slightly slower upflows in the spectral lines Mg II h and k, C II 1336, Si IV 1394 Å, and 1403 Å, that are correlated with brightenings in the slitjaw images (SJIs). The bursty behavior lasts throughout the 2 hr observation, with average burst durations of about 20 s. The locations of these short-lived events appear to be the umbral and penumbral footpoints of EUV loops. Fast apparent downflows are observed along these loops in the SJIs and in the Atmospheric Imaging Assembly, suggesting that the loops are thermally unstable. We interpret the observations as cool material falling from coronal heights, and especially coronal rain produced along the thermally unstable loops, which leads to an increase of intensity at the loop footpoints, probably indicating an increase of density and temperature in the TR. The rain speeds are on the higher end of previously reported speeds for this phenomenon, and possibly higher than the free-fall velocity along the loops. On other observing days, similar bright dots are sometimes aligned into ribbons, resembling small flare ribbons. These observations provide a first insight into small-scale heating events in sunspots in the TR. Title: Chromospheric Diagnostics from IRIS and DST Authors: Cauzzi, Gianna; Reardon, Kevin P.; Jaeggli, Sarah A.; Reid, Aaron Bibcode: 2014AAS...22430201C Altcode: Using data obtained during a coordinated observing campaign in September 2013, we compare the spectral and imaging diagnostics from IRIS and the instruments at the Dunn Solar Telescope (DST). We focus on a small active region observed for approximately one hour with IRIS (NUV, FUV, and SJI) in conjunction with IBIS, FIRS, and ROSA from the DST.In particular, we examine the line widths and intensities in the different chromospheric lines (H-alpha, Ca II 8542, Mg II) and the temporal evolution of these different diagnostics. This allows us to better relate the views from new window provided by IRIS to previous studies of the chromosphere. Title: Investigating Molecular Hydrogen in Active Regions with IRIS Authors: Jaeggli, Sarah A.; Saar, Steven H.; Daw, Adrian N.; Innes, Davina Bibcode: 2014AAS...22432306J Altcode: Molecular hydrogen should be the most abundant molecular species in sunspots, but recent observations with IRIS show that its florescent signature is absent from above the sunspot umbra, but appears brightly during flares. In this poster we continue the analysis of FUV observations of H2 in active regions, examining the correlation between the intensity of the H2 lines and the lines of C II and Si IV which are responsible for their excitation. We particularly focus on differentiating places where H2 is abundant, holes in the chromospheric opacity where FUV photons can enter more deeply into the solar atmosphere, and places where the FUV radiation field is intense, as in flares. Title: H2 Emission in the Sun and Stars: A New Window on Spots and Flares Authors: Saar, Steven H.; Jaeggli, Sarah A. Bibcode: 2014AAS...22412344S Altcode: Molecular H2 is likely important for the formation of sun and starspots, but has been difficult to observe in the past. H2 emission has been seen in solar FUV spectra of sunspots and flares, where it produced by fluorescent excitation driven (primarily) by Si IV and O IV. New observations with IRIS show that the emission is strong in flares, and in loops connected to pores or the boundaries of umbrae. We find evidence for H2 emission in the HST spectra of several magnetically active, flaring, spotted stars. Once the excitation process is better understood, observations of H2 emission should permit new insight into spot formation on the Sun and active stars. Title: Venus' thermospheric temperature field using a refraction model at terminator : comparison with 2012 transit observations using SDO/HMI and NSO/DST/FIRS Authors: Widemann, Thomas; Tanga, Paolo; Père, Christophe; Jaeggli, Sarah; Reardon, Kevin; Pasachoff, Jay M. Bibcode: 2014EGUGA..1612916W Altcode: The transit of Venus in June 2012 provided a unique case study of an Earth-size planet's atmosphere transiting in front of its parent star at 0.7AU, while at the same time ESA's Venus Express orbiter observed the evening terminator at solar ingress and solar egress. We report on mesospheric temperature at Venus' morning terminator using SDO/HMI aureole photometry and comparison with Venus Express. Close to ingress and egress phases, we have shown that the aureole photometry reflects the local density scale height and the altitude of the refracting layer (Tanga et al. 2012). The lightcurve of each spatial resolution element of the aureole is compared to a two-parameter model to constrain the meridional temperature gradient along the terminator. Our measurements are in agreement with the VEx/SOIR temperatures obtained during orbit 2238 at evening terminator during solar ingress (46.75N - LST = 6.075PM) and solar egress (31.30N - LST = 6.047PM) captured from the Venus Express orbiter at the time Venus transited the Sun for Earth-based observers. We also performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption. Observations were taken during the first half of the transit using the Facility InfraRed Spectropolarimeter on the Dunn Solar Telescope. Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric and molecular lines. Sun-subtracted Venus limb observations show intensity distribution of vibrational CO2 bands 221 2v + 2ν2 + ν3 at 1.571um and 141 ν1 + 4ν2 + ν3 at 1.606um. Data independently allow to constrain temperature as well as cross-terminator thermospheric winds. Title: High-resolution Observations of the Shock Wave Behavior for Sunspot Oscillations with the Interface Region Imaging Spectrograph Authors: Tian, H.; DeLuca, E.; Reeves, K. K.; McKillop, S.; De Pontieu, B.; Martínez-Sykora, J.; Carlsson, M.; Hansteen, V.; Kleint, L.; Cheung, M.; Golub, L.; Saar, S.; Testa, P.; Weber, M.; Lemen, J.; Title, A.; Boerner, P.; Hurlburt, N.; Tarbell, T. D.; Wuelser, J. P.; Kankelborg, C.; Jaeggli, S.; McIntosh, S. W. Bibcode: 2014ApJ...786..137T Altcode: 2014arXiv1404.6291T We present the first results of sunspot oscillations from observations by the Interface Region Imaging Spectrograph. The strongly nonlinear oscillation is identified in both the slit-jaw images and the spectra of several emission lines formed in the transition region and chromosphere. We first apply a single Gaussian fit to the profiles of the Mg II 2796.35 Å, C II 1335.71 Å, and Si IV 1393.76 Å lines in the sunspot. The intensity change is ~30%. The Doppler shift oscillation reveals a sawtooth pattern with an amplitude of ~10 km s-1 in Si IV. The Si IV oscillation lags those of C II and Mg II by ~3 and ~12 s, respectively. The line width suddenly increases as the Doppler shift changes from redshift to blueshift. However, we demonstrate that this increase is caused by the superposition of two emission components. We then perform detailed analysis of the line profiles at a few selected locations on the slit. The temporal evolution of the line core is dominated by the following behavior: a rapid excursion to the blue side, accompanied by an intensity increase, followed by a linear decrease of the velocity to the red side. The maximum intensity slightly lags the maximum blueshift in Si IV, whereas the intensity enhancement slightly precedes the maximum blueshift in Mg II. We find a positive correlation between the maximum velocity and deceleration, a result that is consistent with numerical simulations of upward propagating magnetoacoustic shock waves. Title: Characterization of a transiting exo-Venus : lessons from the 2012 Transit Authors: Widemann, Thomas; Jaeggli, S. A.; Reardon, K. P.; Tanga, P.; Pasachoff, J. M.; Schneider, G. Bibcode: 2013DPS....4511811W Altcode: The transit of Venus in June 2012 provided a unique chance to view a well studied planetary atmosphere as we might see that of a transiting exoplanet, through scattered and refracted illumination of its parent star. We report on mesospheric temperature at Venus' morning terminator using SDO/HMI aureole photometry and comparison with Venus Express. Close to ingress and egress phases, we have shown that the aureole photometry reflects the local density scale height and the altitude of the refracting layer (Tanga et al. 2012). The lightcurve of each spatial resolution element of the aureole is compared to a two-parameter model to constrain the meridional temperature gradient along the terminator. Our measurements are in agreement with the VEx/SOIR temperatures obtained during orbit 2238 at evening terminator during solar ingress (46.75N - LST = 6.075PM) and solar egress (31.30N - LST = 6.047PM) as seen from the orbiter. Imaging data using IBIS/ROSA on the Dunn Solar Telescope in the G-band (430 nm) are also presented. We also performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption. Observations were taken during the first half of the transit using the Facility InfraRed Spectropolarimeter on the Dunn Solar Telescope. Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric and molecular lines. Sun-subtracted Venus limb observations show intensity distribution of vibro-rotational CO2 band 221 2ν + 2ν2 + ν3 at 1.571μm allowing for an additional constraint on Venus' thermospheric temperature. Title: Testing Milne-Eddington Inversion Codes Against One-Dimensional Model Atmospheres Authors: Lastufka, Erica; Jaeggli, S. A.; Kankelborg, C.; Uitenbroek, H. Bibcode: 2013SPD....44..116L Altcode: Properties of solar vector magnetic fields can be determined by the inversion of polarization spectra. It is therefore important to have accurate inversion methods. Milne-Eddington inversions, used almost exclusively in the photosphere, assume a thin, flat atmosphere and are one of the most widely used inversion techniques. To investigate the potential weaknesses of parameterizing a stratified atmosphere using a single set of properties, we examine the consequences of using a Milne-Eddington inversion to invert spectra of complex atmospheres. Han Uitenbroek's Rybicki-Hummer radiative transfer and chemical equilibrium code was used to generate a series of one-dimensional model atmospheres with predetermined magnetic field configurations. Atmospheres at the quiet Sun temperature contained magnetic fields with strengths up 3000 G and inclination and azimuthal angles from 0 to 180 degrees. We examined the Stokes profiles of the Fe 15648.5 line, which with a Landé g-factor of 3.0 is very sensitive to the magnetic field. Using a simple Milne-Eddington inversion code, we examined the ranges in which the code accurately parameterized the magnetic field. To investigate the confidence intervals associated with the inverted parameters, we used the BayesME code developed by Andres Asensio Ramos. We discuss the key assumptions and limitations of a Milne-Eddington inversion. Title: Supernova 2013do in UGC 12137 = Psn J22395067+3812443 Authors: Elenin, L.; Molotov, I.; Rachubo, A. A.; Leonard, D. C.; Follette, K.; Sheehan, P.; McCarthy, D.; Moustakas, J.; Bailey, V.; Barrows, J.; Bosset, E.; Buckley, E.; Burd, D.; Calahan, J.; Ceesay, I.; Douglas, E.; Feeney, C.; Fornari, T.; Fox, A.; Fishwick, H.; Gano, H.; Green, C.; Griggs, J.; Hart, K.; Hart, S.; Hartman, K.; Holt, A.; Hooper, E.; Hume, S.; Jaeggli, S.; Lesser, D.; Kerr, M.; Kopans-Johnson, C.; Kumar, K.; Lackey, A.; Laube, S.; Marshall, E.; Martinez, M.; Mehta, G.; Melbourne, K.; Meshel, M.; Myers, C.; Puranen, E.; Schlingman, A.; Shen, K.; Stock, N.; Stillman, C.; Tinker, J.; Whitesell, B.; Tinyanont, S.; Cao, Y.; Kasliwal, M. M. Bibcode: 2013CBET.3571....2E Altcode: Additional CCD magnitudes for 2013do: 2013 June 1, [19.0 (Wang and Gao); 17.763, 17.0 (Joseph Brimacombe, Cairns, Australia; 41-cm telescope + infrared filter; bandpass > 700 nm; position end figures 50s.65, 43".5; image posted at URL http://www.flickr.com/photos/43846774@N02/9074451038/); 18.253, 18.1 (L. Elenin, Lyubertsy, Russia, and I. Molotov, Moscow; three 150-s images taken remotely with a 0.45-m f/2.8 telescope at the ISON-NM Observatory near Mayhill, NM, USA; position end figures 50s.54 +/- 0".18, 44".8 +/- 0".19; UCAC-4 reference stars; limiting mag about 18.8; image posted at website URL http://spaceobs.org/images/TOCP/PSNJ22395067+3812443-20130618.png); 21.832, 17.2 (Wang and Gao; position end figures 50s.69, 44".3); 22.819, 17.1 (Wang and Gao; position end figures 50s.70, 43".3). A. A. Rachubo and D. C. Leonard, San Diego State University; K. Follette, P. Sheehan, and D. McCarthy, University of Arizona; J. Moustakas, Siena College; V. Bailey, J. Barrows, E. Bosset, E. Buckley, D. Burd, J. Calahan, I. Ceesay, E. Douglas, C. Feeney, T. Fornari, A. Fox, H. Fishwick, H. Gano, C. Green, J. Griggs, K. Hart, S. Hart, K. Hartman, A. Holt, E. Hooper, S. Hume, S. Jaeggli, D. Lesser, M. Kerr, C. Kopans-Johnson, K. Kumar, A. Lackey, S. Laube, E. Marshall, M. Martinez, G. Mehta, K. Melbourne, M. Meshel, C. Myers, E. Puranen, A. Schlingman, W. Schlingman, W. M. Schlingman, K. Shen, N. Stock, C. Stillman, J. Tinker, and B. Whitesell, 2013 Advanced Teen Astronomy Camp, report that inspection of a low-dispersion optical spectrum (range 350-660 nm) of PSN J22395067+3812443 = SN 2013do, obtained with the 2.3-m Bok telescope (+ Boller & Chivens spectrograph) at Steward Observatory on June 26 UT, shows it to be a type-II supernova. Cross-correlation with a library of supernova spectra using the "Supernova Identification" code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) finds best matches with a number of normal type-IIP supernovae ranging in age from about one to two weeks after maximum light. Adopting the recession velocity for UGC 12137 of 4685 km/s (Wegner et al. 1993, A.J. 105, 1251; via the NASA/IPAC Extragalactic Database), an expansion velocity of 8900 km/s is derived from the position of the H_beta (rest wavelength 486.1 nm) minimum. S. Tinyanont, Harvey Mudd College; Y. Cao, California Institute of Technology; and M. M. Kasliwal, Observatories of the Carnegie Institution and Princeton University, report that spectroscopic observations (range 330-1000 nm) of PSN J22395067+3812443 = SN 2013do were obtained on June 27.27 UT with the Dual Imaging Spectrograph on the 3.5-m ARC telescope at Apache Point Observatory. The spectrum shows prominent H-alpha emission with a P-Cyg profile. The minimum of the H-alpha absorption is at 642.5 nm. Using the redshift z = 0.015627 for UGC 12137 (from Wegner et al. 1993, A.J. 105, 1251; via NED), this corresponds to a velocity of 11000 km/s. Running the SNID software, the spectrum resembles SN 2004et at fifteen days after maximum, indicating that 2013do is a type-II-P supernova. Title: Supernova 2013dq in UGC 525 = Psn J00513484+2943149 Authors: Howerton, S.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan, M.; Christensen, E.; Larson, S. M.; Rachubo, A. A.; Leonard, D. C.; Follette, K.; Sheehan, P.; Bailey, V.; McCarthy, D.; Moustakas, J.; Barrows, J.; Bosset, E.; Buckley, E.; Burd, D.; Calahan, J.; Ceesay, I.; Douglas, E.; Feeney, C.; Fornari, T.; Fox, A.; Fishwick, H.; Gano, H.; Green, C.; Griggs, J.; Hart, K.; Hart, S.; Hartman, K.; Holt, A.; Hooper, E.; Hume, S.; Jaeggli, S.; Lesser, D.; Kerr, M.; Kopans-Johnson, C.; Kumar, K.; Lackey, A.; Laube, S.; Marshall, E.; Martinez, M.; Mehta, G.; Melbourne, K.; Meshel, M.; Myers, C.; Puranen, E.; Schlingman, A.; Shen, K.; Stock, N.; Stillman, C.; Tinker, J.; Whitesell, B. Bibcode: 2013CBET.3573....1H Altcode: 2013CBET.3573A...1H S. Howerton, Arkansas City, KS, U.S.A.; A. J. Drake, S. G. Djorgovski, A. Mahabal, M. J. Graham, and R. Williams, California Institute of Technology; J. L. Prieto, Princeton University; M. Catelan, Pontificia Universidad Catolica de Chile; and E. Christensen and S. M. Larson, Lunar and Planetary Laboratory, University of Arizona, report the Catalina Real-time Transient Survey discovery of an apparent supernova in public images from the Catalina Sky Survey (CSS). SN 2013 UT R.A. (2000.0) Decl. Mag. Offset 2013dq June 27.44 0 51 34.84 +29 43 14.9 16.8 4".3 E, 15".6 N The variable was designated PSN J00513484+2943149 when it was posted at the Central Bureau's TOCP webpage and is here designated SN 2013dq based on the spectroscopic confirmation reported below. Additional CCD magnitudes for 2013dq: Feb. 8.14 UT, [19.5 (CSS); June 28.814, 17.2 (Joseph Brimacombe, Cairns, Australia; 41-cm telescope + infrared filter; bandpass > 700 nm; position end figures 35s.02, 13".8; image posted at website URL http://www.flickr.com/photos/43846774@N02/9174594184/). A. A. Rachubo and D. C. Leonard, San Diego State University; K. Follette, P. Sheehan, V. Bailey, and D. McCarthy, University of Arizona; J. Moustakas, Siena College; J. Barrows, E. Bosset, E. Buckley, D. Burd, J. Calahan, I. Ceesay, E. Douglas, C. Feeney, T. Fornari, A. Fox, H. Fishwick, H. Gano, C. Green, J. Griggs, K. Hart, S. Hart, K. Hartman, A. Holt, E. Hooper, S. Hume, S. Jaeggli, D. Lesser, M. Kerr, C. Kopans-Johnson, K. Kumar, A. Lackey, S. Laube, E. Marshall, M. Martinez, G. Mehta, K. Melbourne, M. Meshel, C. Myers, E. Puranen, A. Schlingman, W. Schlingman, W. M. Schlingman, K. Shen, N. Stock, C. Stillman, J. Tinker, and B. Whitesell, 2013 Advanced Teen Astronomy Camp, report that inspection of a low-dispersion optical spectrogram (range 370-680 nm) of PSN J00513484+2943149 = SN 2013dq, obtained in heavy twilight with the 2.3-m Bok telescope (+ Boller & Chivens spectrograph) at Steward Observatory on June 28 UT, shows it to be an aging type-Ia supernova. After correcting for a redshift of 4931 km/s for the assumed host galaxy, UGC 525 (Falco et al. 1999, PASP 111, 438; via NED), reasonable matches are found with normal type-Ia supernovae at epochs ranging between 40 and 65 days after maximum light, although there is a notable absence of emission in 2013dq near 500.0 nm (attributed to Fe II; Branch et al. 2008, PASP 120, 135) that is usually seen at this phase. The most convincing individual spectral match is made with SN 1999gp at 50 days post-maximum (Matheson et al. 2008, A.J. 135, 1598), which exhibited a broad, 1991T-like light-curve (dm15[B] = 0.80; Hicken et al. 2009, Ap.J. 700, 331), a "shallow silicon" maximum-light spectrum (Jha et al. 2000, IAUC 7341; Branch et al. 2009, PASP 121, 238), and somewhat-muted 500.0-nm emission at this phase. Title: 1565 nm Observations of the transit of Venus, Proxy for a Transiting Exoplanet Authors: Jaeggli, Sarah A.; Reardon, K. P.; Pasachoff, J. M.; Schneider, G.; Widemann, T.; Tanga, P. Bibcode: 2013SPD....44..150J Altcode: The transit of Venus in June 2012 provided a unique chance to view its atmosphere as we might see that of a transiting Cytherean exoplanet, through scattered and refracted illumination from its parent star. We performed spectroscopy and polarimetry during the transit of Venus focusing on extracting signatures of CO2 absorption of Venus from the solar spectrum. Although the predicted CO2 transmission spectrum of Venus was not particularly strong at 1565 nm, this region of the H-band often used in magnetic-field studies of the Sun's photosphere provides a particularly flat solar continuum with few atmospheric and molecular lines. Observations of Venus were taken throughout first contact and on the solar disk using the Facility InfraRed Spectropolarimeter on the Dunn Solar Telescope at the National Solar Observatory. The transit also provided a unique opportunity to investigate instrumental effects. In this poster we discuss initial results from the transit, including estimates for an exoplanet detection of this kind, preliminary comparison with atmospheric models, and the stray light properties of the instrument. This work was performed in collaboration with the Williams College Venus transit expedition, which was sponsored by Natl Geog/Comm for Research and Exploration. Title: National Student Solar Spectrograph Competition Overview and Results Authors: Des Jardins, Angela C.; Larimer, R.; Shaw, J. A.; Kankelborg, C.; Palmer, C.; Key, J. S.; Nakagawa, W.; Springer, L.; Knighton, W.; Repasky, K. S.; Pust, N. J.; Babbitt, W.; Jaeggli, S. A.; Hobish, M. K.; Wilson, E. W.; Anderson, M.; Boger, J.; McCrady, N.; Naylor, J.; Turcotte, S.; Lines, T.; Strobel, N.; Cooper, W.; Darke, R.; Head, R.; Kimball, D.; Kissel, G.; Buck, K.; Lawrence, L.; Wragg, J.; Runyon, C. J.; Spacher, P.; Dumitriu, I.; Nollenberg, J. G.; Estaban, R. Bibcode: 2013SPD....44..160D Altcode: The yearly National Student Solar Spectrograph Competition (NSSSC) is Montana Space Grant Consortium's Education and Public Outreach (EP/O) Program for NASA's Interface Region Imaging Spectrograph (IRIS) mission. The NSSSC is designed to give institutions with less aerospace activity such as Minority Serving Institutions and Community Colleges an opportunity for hands on real world research experience. The NSSSC provides students from across the country the opportunity to work as part of an undergraduate interdisciplinary team to design, build and test a ground based solar spectrograph. Over the course of nine months, teams come up with their own science goals and then build an instrument to collect data in support of their goals. Teams then travel to Bozeman, MT to demonstrate their instruments and present their results in a competitive science fair environment. This poster will present the 2012-2013 competition results.Abstract (2,250 Maximum Characters): The yearly National Student Solar Spectrograph Competition (NSSSC) is Montana Space Grant Consortium's Education and Public Outreach (EP/O) Program for NASA's Interface Region Imaging Spectrograph (IRIS) mission. The NSSSC is designed to give institutions with less aerospace activity such as Minority Serving Institutions and Community Colleges an opportunity for hands on real world research experience. The NSSSC provides students from across the country the opportunity to work as part of an undergraduate interdisciplinary team to design, build and test a ground based solar spectrograph. Over the course of nine months, teams come up with their own science goals and then build an instrument to collect data in support of their goals. Teams then travel to Bozeman, MT to demonstrate their instruments and present their results in a competitive science fair environment. This poster will present the 2012-2013 competition results. Title: Spectroscopy of PSN J00513484+2943149 in UGC 525 Authors: Rachubo, A. A.; Leonard, D. C.; Follette, K.; Sheehan, P.; Bailey, V.; McCarthy, D.; Moustakas, J.; Barrows, J.; Bosset, E.; Buckley, E.; Burd, D.; Calahan, J.; Ceesay, I.; Douglas, E.; Feeney, C.; Fornari, T.; Fox, A.; Fishwick, H.; Gano, H.; Green, C.; Griggs, J.; Hart, K.; Hart, S.; Hartman, K.; Holt, A.; Hooper, E.; Hume, S.; Jaeggli, S.; Lesser, D.; Kerr, M.; Kopans-Johnson, C.; Kumar, K.; Lackey, A.; Laube, S.; Marshall, E.; Martinez, M.; Mehta, G.; Melbourne, K.; Meshel, M.; Myers, C.; Puranen, E.; Schlingman, A.; Schlingman, W.; Schlingman, W. M.; Shen, K.; Stock, N.; Stillman, C.; Tinker, J.; Whitesell, B. Bibcode: 2013ATel.5176....1R Altcode: We report that inspection of a low-dispersion optical spectrum (range 370-680 nm) of PSN J00513484+2943149 (CBAT TOCP), obtained in heavy twilight with the 2.3-m Bok telescope (+ Boller & Chivens spectrograph) at Steward Observatory on June 28 UT, shows it to be an aging type-Ia supernova. After correcting for a redshift of 4931 km/s for the assumed host galaxy, UGC 525 (Falco et al. 1999, PASP, 111, 438; via NED), reasonable matches are found with normal SNe Ia at epochs ranging between 40 and 65 days after maximum light, although there is a notable absence of emission in PSN J00513484+2943149 near 5000 Angstrom (attributed to Fe II; Branch et al. Title: Transit Observations of Venus's Atmosphere in 2012 from Terrestrial and Space Telescopes as Exoplanet Analogs Authors: Pasachoff, Jay M.; Schneider, G.; Babcock, B. A.; Lu, M.; Penn, M. J.; Jaeggli, S. A.; Galayda, E.; Reardon, K. P.; Widemann, T.; Tanga, P.; Ehrenreich, D.; Vidal-Madjar, A.; Nicholson, P. D.; Dantowitz, R. Bibcode: 2013AAS...22221701P Altcode: We extensively observed the 8 June 2012 transit of Venus from several sites on Earth; we provide this interim status report about this and about two subsequent ToVs observed from space. From Haleakala Obs., we observed the entire June transit over almost 7 h with a coronagraph of the Venus Twilight Experiment B filter) and with a RED Epic camera to compare with simultaneous data from ESA's Venus Express, to study the Cytherean mesosphere; from Kitt Peak, we have near-IR spectropolarimetry at 1.6 µm from the aureole and during the disk crossing that compare well with carbon dioxide spectral models; from Sac Peak/IBIS we have high-resolution imaging of the Cytherean aureole for 22 min, starting even before 1st contact; from Big Bear, we have high-resolution imaging of Venus's atmosphere and the black-drop effect through 2nd contact; and we had 8 other coronagraphs around the world. For the Sept 21 ToV as seen from Jupiter, we had 14 orbits of HST to use Jupiter's clouds as a reflecting surface to search for an 0.01% diminution in light and a differential drop that would result from Venus's atmosphere by observing in both IR/UV, for which we have 170 HST exposures. As of this writing, preliminary data reduction indicates that variations in Jovian clouds and the two periods of Jupiter's rotation will be too great to allow extraction of the transit signal. For the December 20 ToV as seen from Saturn, we had 22 hours of observing time with VIMS on Cassini, for which we are looking for a signal of the 10-hr transit in total solar irradiance and of Venus's atmosphere in IR as an exoplanet-transit analog. Our Maui & Sac Peak expedition was sponsored by National Geographic Society's Committee for Research and Exploration; HST data reduction by NASA: HST-GO-13067. Some of the funds for the carbon dioxide filter for Sac Peak provided by NASA through AAS's Small Research Grant Program. We thank Rob Ratkowski of Haleakala Amateur Astronomers; Rob Lucas, Aram Friedman, Eric Pilger, Stan Truitt, and Steve Bisque/Software Bisque for Haleakala support/operations; Vasyl Yurchyshyn and Joseph Gangestad '06 of The Aerospace Corp. at Big Bear Solar Obs; LMSAL and Hinode science/operations team. Title: Multi-height Spectropolarimetry Of Sunspots With Firs And Ibis Authors: Jaeggli, Sarah A.; Lin, H.; Tritschler, A. Bibcode: 2012AAS...22020606J Altcode: The effects of radiative transfer prevent the characterization of the magnetic field at a single geometric height in the photosphere of a sunspot. Therefore, a full 3D characterization of the magnetic field is necessary to understand many properties of sunspots, such as the true state of hydrostatic equilibrium. Many current and proposed solar spectropolarimeters are capable of taking near-simultaneous observations at multiple wavelengths. Combining these rich datasets provides a welcome problem to the community. We present the first joint observations of the magnetically sensitive photospheric Fe I lines at 630 and 1565 nm taken with the Facility Infrared Spectropolarimeter (FIRS); and the chromospheric Ca II line at 854 nm taken with the Interferometric Bi-Dimensional Spectrometer (IBIS); both instruments operated at the Dunn Solar Telescope. These wavelengths allow us to probe the magnetic field over a broad range of heights, from the bottom of the photosphere to the chromosphere. We investigate the magnetic field topologies of several sunspots of different size and magnetic complexity. Title: Comparison of Multi-Height Observations with a 3D MHD Sunspot Model Authors: Jaeggli, S. A.; Lin, H.; Uitenbroek, H.; Rempel, M. Bibcode: 2012ASPC..456...67J Altcode: In sunspots the contribution to the horizontal pressure support from the curvature force and the geometrical height of formation which magnetic field measurements sample are poorly constrained observationally due to the effect of radiative transfer. In cool atmospheres, observations of the sunspot photosphere probe geometrically deeper layers, information on the magnetic field gradients cannot be easily derived even using multi-wavelength, multi-height observations. Recent MHD atmosphere models of sunspots analyzed with the Rybiki-Hummer radiative transfer code allow for direct comparison with simultaneous multi-height observations of the Fe I magnetic field diagnostics at 1565 and 630.2 nm in sunspots observed using the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope. Title: Spies - Spectral Polarimetric Imager For The Energetic Sun Authors: Lin, Haosheng; Jaeggli, S. Bibcode: 2012AAS...22012306L Altcode: Spectropolarimetric observation with uncompromised spatial, spectral, and temporal resolution simulatneously over a substantial 2D field and multiple spectral lines is the key to the resolution of many important questions in modern solar physics. While 2D imaging spectroscopy based on fiber optics integral field unit and image slicer has a long history nighttime astronomy, adaptation for solar observation occured only recently. This paper will present preliminary results of magnetic field observation in the HeI 1083 nm and FeI 1565 nm lines obtained with SPIES --- a true imaging spectropolarimeter based on a large format (64 x 32 fibers input array) fiber-optic array optimized for the study of evolution of magnetic and thermodynamic properties of energetic and dynamic phenomena of the sun. We will also discuss considerations for the use of fiber-optic array for solar spectropolarimetric applications, as well as the design of SPIES. Title: Non-Stationary Deconvolution for the IRIS NUV Slit-Jaw Imager Authors: Jaeggli, Sarah A.; Kankelborg, Charles C.; IRIS Team Bibcode: 2012decs.confE..49J Altcode: High spatial resolution context imaging is essential to linking spatial structures with spectral signatures in the chromosphere, a critical part of the science requirements for IRIS (Interface Region Imaging Spectrograph). Measurements of the optical figure of the Solc filter indicate that the NUV slit-jaw imager on IRIS will have a somewhat broader PSF than the other instrument channels. We have developed an advanced deconvolution technique which combines measured PSFs sampled over the image plane to achieve the best correction for each pixel. We have conducted an analysis of this technique on synthetic data, and we assess the quality of the resulting images containing a variety of simulated effects, including cosmic ray hits, photon counting noise, discrete energetic solar events (flares), and saturation and overflow artifacts. Title: On Molecular Hydrogen Formation and the Magnetohydrostatic Equilibrium of Sunspots Authors: Jaeggli, S. A.; Lin, H.; Uitenbroek, H. Bibcode: 2012ApJ...745..133J Altcode: 2011arXiv1110.0575J We have investigated the problem of sunspot magnetohydrostatic equilibrium with comprehensive IR sunspot magnetic field survey observations of the highly sensitive Fe I lines at 15650 Å and nearby OH lines. We have found that some sunspots show isothermal increases in umbral magnetic field strength which cannot be explained by the simplified sunspot model with a single-component ideal gas atmosphere assumed in previous investigations. Large sunspots universally display nonlinear increases in magnetic pressure over temperature, while small sunspots and pores display linear behavior. The formation of molecules provides a mechanism for isothermal concentration of the umbral magnetic field, and we propose that this may explain the observed rapid increase in umbral magnetic field strength relative to temperature. Existing multi-component sunspot atmospheric models predict that a significant amount of molecular hydrogen (H2) exists in the sunspot umbra. The formation of H2 can significantly alter the thermodynamic properties of the sunspot atmosphere and may play a significant role in sunspot evolution. In addition to the survey observations, we have performed detailed chemical equilibrium calculations with full consideration of radiative transfer effects to establish OH as a proxy for H2, and demonstrate that a significant population of H2 exists in the coolest regions of large sunspots. Title: An Observational Study of the Formation and Evolution of Sunspots Authors: Jaeggli, Sarah A.; Lin, H.; Uitenbroek, H. Bibcode: 2011SPD....42.0302J Altcode: 2011BAAS..43S.0302J It is well known that the thermal-magnetic relation in sunspots can be non-linear. Previous investigations ascribe the non-linearity of the relation to changing geometrical height of the measurement due to radiative transfer effects (Wilson Depression) and the poorly determined magnetic field curvature force. However, the very coolest regions of some sunspots show a rapid increase in umbral magnetic field strength relative to temperature which cannot be explained by the simplified sunspot model with single-component ideal gas atmosphere which has been previously assumed. This represents a fundamental flaw in our understanding of the sunspot equilibrium problem. Existing multiple-component sunspot atmospheric models predict that a large amount of molecular hydrogen (H2) exists in the sunspot umbra. The formation of molecules provides a mechanism for isothermal concentration of the umbral magnetic field which may explain the observed rapid increase in umbral magnetic field strength relative to temperature. We have characterized the equilibrium forces in sunspots using simultaneous visible and IR sunspot magnetic field survey observations of the highly sensitive Fe I lines at 6302 and 15650 Angstroms and nearby OH lines which have been conducted with the new Facility Infrared Spectropolarimeter (FIRS) at the Dunn Solar Telescope. We have performed detailed chemical equilibrium calculations with full consideration of radiative transfer effects to establish OH as a proxy for H2, and demonstrate that a significant population of H2 exists in the coolest regions of large and more mature sunspots. We further point out that the formation of H2 can significantly alter the thermodynamic properties of the sunspot atmosphere and may play a significant role in sunspot evolution. Title: Spectropolarimetry of Chromospheric Magnetic and Velocity Structure Above Active Regions Authors: Schad, T. A.; Jaeggli, S. A.; Lin, H.; Penn, M. J. Bibcode: 2011ASPC..437..483S Altcode: 2011arXiv1101.0631S Active regions often host large-scale gas flows in the chromosphere presumably directed along curved magnetic field lines. Spectropolarimetric observations of these flows are critical to understanding the nature and evolution of their anchoring magnetic structure. We discuss recent work with the Facility Infrared Spectropolarimeter (FIRS) located at the Dunn Solar Telescope in New Mexico to achieve high-resolution imaging-spectropolarimetry of the Fe I lines at 630 nm, the Si I line at 1082.7 nm, and the He I triplet at 1083 nm. We present maps of the photospheric and chromospheric magnetic field vector above a sunspot as well as discuss characteristics of surrounding chromospheric flow structures. Title: Molecule Formation and Magnetic Field Evolution in Sunspots Authors: Jaeggli, S. A.; Lin, H.; Uitenbroek, H. Bibcode: 2011ASPC..437..473J Altcode: In a sunspot the magnetic field provides horizontal support to keep the warm, high pressure photosphere from intruding into the cool, low pressure sunspot atmosphere. In the very coolest regions of the umbra a rapid increase in magnetic field strength relative to temperature has been observed by many authors although its origins have remained unknown. In these regions the magnetic and gas pressure forces have found a different state which the current simplified theory of magnetohydrostatic equilibrium cannot quantitatively describe. It is well known that molecules form in sunspots. The formation of a large molecular fraction would alter the physical characteristic of the gas, providing a mechanism for concentrating the umbral magnetic field. The formation of molecules may be responsible for the observed rapid increase of the magnetic field strength observed in the coolest regions of the sunspots and may play a significant role in sunspot evolution. We investigate this problem with atmospheric models and present preliminary results from observations taken with the new Facility Infrared Spectropolarimeter on the Dunn Solar Telescope. Title: An observational study of the formation and evolution of sunspots Authors: Jaeggli, Sarah A. Bibcode: 2011PhDT........97J Altcode: This dissertation focuses on the problem of molecules and the horizontal balance of forces in sunspots. Sunspots are quasi-static features on the solar surface and can be considered to be in a state of equilibrium. The weaker gas pressure of the cool sunspot interior is horizontally supported against the higher pressure of the hotter quiet-Sun by a strong vertical magnetic field. However, some sunspots show a rapid increase in magnetic pressure relative to the temperature of the gas in the coolest regions of the sunspot, implying that an isothermal decrease in the gas pressure must have occurred. The current model of sunspots is unable to describe this deviation from the assumed equilibrium state of the magnetic field and thermal gas pressure observed in these sunspots. Another method of altering the pressure of the gas must be occurring. The formation of molecules in sunspots may be the key to solving this puzzle. The sunspot interior provides a cool environment where molecules can form in abundance. As atoms become bound into molecules the total particle number of the gas is decreased. A sufficiently large molecular fraction could significantly alter the properties of the sunspot plasma, and specifically provide a mechanism for concentrating the magnetic field by non-thermally lowering the gas pressure. I have investigated the equilibrium condition of sunspots of different sizes and in a variety of evolutionary phases through a Milne-Eddington inversion of spectropolarimetric observations of the Zeeman-split Fe I lines at 6302 and 15650 A to obtain their thermal and magnetic topology. I carried out a calculation of the detailed radiative transfer and chemical equilibrium of model sunspot atmospheres to determine the molecular gas fraction. Several sunspots show unambiguous cases of isothermal magnetic field intensification, which can only be explained by the formation or destruction of a large molecular population. All sunspots with magnetic fields stronger than 2500 G and temperatures cooler than 5800 K consistently show a signature of magnetic field over-concentration, consistent with molecular hydrogen formation of a few percent of the total gas fraction. The formation of this large molecular population has widespread implications for sunspot physics. Title: Magnetic Field Measurements at the Photosphere and Coronal Base Authors: Judge, P. G.; Centeno, R.; Tritschler, A.; Uitenbroek, H.; Jaeggli, S.; Lin, H. Bibcode: 2010AGUFMSH31A1783J Altcode: We have obtained vector polarimetric measurements in lines of Fe I (630nm), Ca II (854nm) and He I (1083nm) of several active regions during 3-14 June 2010. The measurements were made at the Dunn Solar Telescope at Sacramento Peak Observatory, using the FIRS and IBIS instruments simultaneously. We discuss these and SDO data for NOAA 11076. The seeing was very good or excellent and the adaptive optics system functioned well. In this preliminary analysis we compare extrapolations of photospheric fields with the constraints available from Stokes polarimetry, including the morphology and kinematic properties of fibrils. Connections to the corona will also be discussed. The implications for field extrapolations from photospheric measurements will be discussed. We will make the reduced data freely available on the web for interested researchers. Title: Utilization of redundant polarized solar spectra to infer the polarization properties of the new generation of large aperture solar telescopes Authors: Elmore, David F.; Lin, Haosheng; Socas Navarro, Héctor; Jaeggli, Sarah A. Bibcode: 2010SPIE.7735E..4EE Altcode: 2010SPIE.7735E.147E Spectro-polarimetry plays an important role in the study of solar magnetism and strongly influences the design of the new generation of solar telescopes. Calibration of the polarization properties of the telescope is a critical requirement needed to use these observations to infer solar magnetic fields. However, the large apertures of these new telescopes make direct calibration with polarization calibration optics placed before all the telescope optical elements impractical. It is therefore desirable to be able to infer the polarization properties of the telescope optical elements utilizing solar observations themselves. Taking advantage of the fact that the un-polarized, linearly, and circularly polarized spectra originating from the Sun are uncorrelated, we have developed techniques to utilize observations of solar spectra with redundant combination of the polarization states measured at several different telescope configurations to infer the polarization properties of the telescope as a whole and of its optical elements. We show results of these techniques applied to spectro-plarimetric data obtained at the Dunn Solar Telescope. Title: Magnetic field measurements at the photosphere and coronal base Authors: Judge, Philip; Centeno, R.; Tritschler, A.; Uitenbroek, H.; Jaeggli, S.; Lin, H. Bibcode: 2010shin.confE..56J Altcode: We have obtained vector polarimetric measurements in lines of Fe I (630nm), Ca II (854nm) and He I (1083) of several active regions during 3-14 June 2010. The measurements were made at the Dunn Solar Telescope at Sacramento Peak Observatory, using the FIRS and IBIS instruments simultaneously. We discuss data for NOAA 11076 observed on 4 June 2010. The seeing was very good or excellent and the adaptive optics system functioned well. In this preliminary analysis we compare linear extrapolations of photospheric fields with the constraints available from Stokes polarimetry, including the morphology and kinematic properties of fibrils. The implications for field extrapolations from photospheric measurements will be discussed. We will make the reduced data freely available on the web for interested researchers. 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 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: Erratum: ``Localized Enhancements of Fe+10 Density in the Corona as Observed in Fe XI 789.2 nm during the 2006 March 29 Total Solar Eclipse'' (ApJ, 663, 598 [2007]) Authors: Habbal, Shadia Rifai; Morgan, Huw; Johnson, Judd; Arndt, Martina Belz; Daw, Adrian; Jaeggli, Sarah; Kuhn, Jeff; Mickey, Don Bibcode: 2007ApJ...670.1521H Altcode: The eclipse image of Figure 3 was provided to the authors by Jackob Strikis of the Elizabeth Observatory, Athens, who claimed authorship. However, shortly after publication the authors discovered that this eclipse image was in fact a preliminary version of an image belonging to Prof. Miloslav Druckmüller, taken during the 2006 total solar eclipse from Libya at 30°56.946' N, 24°14.301' E, and at an altitude of 158 m. This image can be found at ApJ, 663, 598 [2007]. We extend our gratitude to Prof. Druckmüller, from Brno University of Technology, Czech Republic, who brought this incident to our attention, and who has graciously accepted our apology for this unintentional mishap. A forthcoming article in collaboration with Prof. Druckmüller is in preparation. 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: Localized Enhancements of Fe+10 Density in the Corona as Observed in Fe XI 789.2 nm during the 2006 March 29 Total Solar Eclipse Authors: Habbal, Shadia Rifai; Morgan, Huw; Johnson, Judd; Arndt, Martina Belz; Daw, Adrian; Jaeggli, Sarah; Kuhn, Jeff; Mickey, Don Bibcode: 2007ApJ...663..598H Altcode: The first ever image of the full solar corona in the Fe XI 789.2 nm spectral line was acquired during the total solar eclipse of 2006 March 29. Several striking features stand out in the processed image: (1) The emission extended out to at least 3 Rsolar in streamers. (2) A bubble-like structure, occupying a cone of about 45° and reaching out to 1 Rsolar above the limb, was observed southward of a bright active region complex close to the limb. (3) Localized intensity enhancements were found in different parts of the corona at heights ranging from 1.2 to 1.5 Rsolar. (4) Striations extended out to the edge of the field of view above an almost north-south-oriented prominence. Comparison with the corresponding white-light image taken simultaneously during the eclipse showed no evidence for these localized enhancements, and the bubble-like structure and striations, while present, did not stand out in the same manner. The extent of the Fe XI emission is attributed to the dominance of radiative over collisional excitation in the formation of that spectral line. The localized intensity enhancements, observed only in Fe XI and not in white light, are a signature of localized increases in Fe+10 density relative to electron density. These are the first observations to show direct evidence of localized heavy ion density enhancements in the extended corona. They point to the importance of implementing observations of the Fe XI 789.2 nm line with existing or future coronagraphs for the exploration of the physical processes controlling the behavior of heavy ions in different source regions of the solar wind. Title: The Starburst-AGN Connection: Integral Field Spectroscopy of Merging and Seyfert 2 Galaxies Authors: Jaeggli, Sarah A.; Joseph, R. D. Bibcode: 2007AAS...210.1207J Altcode: 2007BAAS...39..109J Luminous galaxies can be powered by two different mechanisms, accretion of matter onto a super-massive black hole at the nucleus, and a rapid burst of star formation that produces many luminous young stars, a "starburst." Both events occur inside a large optical depth of dust: a Seyfert 2 through its dusty torus and starbursts through their dusty cocoons. Using the UIST integral field unit on the United Kingdom Infrared Telescope we make observations in the K-band where obscuration due to dust is ten times less than at visible wavelengths. With a resolution of 900 and a field of 6 x 3.3 square arcseconds, the integral field unit allows us to use infrared spectral diagnostics for a sample of galaxies identified as merging starbursts and another sample identified as Seyfert 2s to investigate the presence of both starbursts and AGNs in both samples, and look for evidence of the starburst-AGN connection. 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: 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: Penumbral Moving Magnetic Features Authors: Penn, M. J.; Jaeggli, S. A.; Henney, C. J.; Luszcz, S.; Walton, S. R. Bibcode: 2006ASPC..358...31P Altcode: Moving magnetic features are observed in the penumbrae of two sunspots with time sequences of vector magnetic field measurements taken in the infrared Fe I 1565 nm spectral line (g=3). These features move with similar radial velocities as previously observed continuum and G-band features, and confirm a short sequence of penumbral magnetic observations in the visible. These features move with similar speeds to the moving magnetic features seen outside sunspot penumbrae, and in some cases they are seen to cross the penumbral boundary and move across the sunspot moat. Magnetic and flow parameters are briefly compared with predictions from the moving flux tube model. 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: 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: Searching for Moving Magnetic Features at 1565 nm Authors: Jaeggli, S. A.; Penn, M. J.; Henney, C. J. Bibcode: 2005AGUSMSP41B..01J Altcode: Spectropolarimetric data of the active region 10663 was taken with the CSUN-NSO IR camera and the McMath-Pierce telescope on August 26, 2004 from 16:35 to 21:02 UT. Utilizing the Zeeman split Fe I line near 1565 nm, the data is processed to remove instrumental polarization and a Milne-Eddington inversion technique is applied. The results of the inversion are used to examine the physical properties and radial motions of moving magnetic features which appear to originate in the sunspot penumbra. Title: Moving Magnetic Features Inside the Penumbra of NOAO 10008 Authors: Luszcz, S. H.; Penn, M. J.; Jaeggli, S. A.; Henney, C. J. Bibcode: 2005AGUSMSP11A..05L Altcode: Over 30 years of observations and theories comprise the study of moving magnetic features (MMFs). MMFs, which often occur in opposite polarity pairs, migrate radially outward through the sunspot moat at speeds of about 1 km~s-1. A sequence of sixteen scans of the active region NOAO 10008 were taken using the NSO-CSUN IR camera at the NSO McMath-Pierce Solar Telescope on 24 June 2002 17:38-21:59. Using the Fe I absorption line at 1564.8nm, magnetogram images and maps of the magnetic field vector were produced, revealing magnetic features within the penumbra that appear to move radially outward at similar velocities and azimuth angles as those of MMFs in the moat. We use polar time slice images to measure the radial velocities of both types of features. This work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. Title: The 1564.6nm CN Line in Sunspots Authors: Penn, M. J.; Jaeggli, S. A. Bibcode: 2005AGUSMSP11A..02P Altcode: The line strength of CN absorption has been observed to vary with the continuum intensity within sunspots, and the Doppler shift of the CN line at 1564.6nm has been shown to reveal fast Evershed flows in the penumbra. We examine several sunspots observed from 2002-2005 using intensity spectroscopy and spectropolarimetry to determine the line strength, plasma flow velocity, and the local magnetic field configuration as functions of position in these sunspots. Title: IR Vector Magnetic Fields I: Instrumental Polarization Correction Authors: Jaeggli, S. A.; Penn, M. J. Bibcode: 2004AAS...204.3706J Altcode: 2004BAAS...36R.709J Instrumental polarization is evident in the spectra of active region 10008 taken with the CSUN-NSO IR camera at the McMath-Pierce telescope on June 24, 2002. Several iron lines near 15650 Å in the spectra exhibit Zeeman splitting. Using a technique described by Kuhn et. al. (1994) the original polarization is restored. For all Zeeman split lines in the spectra the corrected Stokes profiles for the Q and U components show symmetry, while Stokes V is made antisymmetric with no central component.

The observed Stokes vector is related to the true Stokes vector through the formula Strue = M-1 Sobs where M-1 is the inverse Mueller matrix. The correction coefficients from the Kuhn method are used to compute the inverse Mueller matrix for light path of the entire system. The expected inverse Mueller matrix is computed for the telescope at each scan time using a simple model described by Bernasconi (1997) but assuming the n and k values of the index of refraction are the same for each mirror surface. A least squares technique is used to fit this telescope model to the measured inverse Mueller matrix for the system. The telescope model can account for most of the measured cross-talk except for the observed Stokes Q to Stokes V cross-talk which is thought to occur in the polarimeter. Title: IR Vector Magnetic Fields II: Atomic and Molecular Line Polarization in a Sunspot Authors: Penn, M. J.; Jaeggli, S. A.; Henney, C. J.; Walton, S. R.; Ceja, J. A. Bibcode: 2004AAS...204.3705P Altcode: 2004BAAS...36..709P Full Stokes I,Q,U and V measurements of the active region NOAA 10008 were taken from 21-27 June 2002 at the NSO Kitt Peak McMath/Pierce solar telescope using the CSUN/NSO HgCdTe IR camera and polarimeter at 1565nm. The data is corrected for instrumental polarization as discussed in Paper I. Here the initial analysis of the atomic and molecular line polarization data is presented.

Inversion of the Fe I g=3 1564.8nm line data with a modified Skumanich and Lites Milne-Eddington technique is used to measure photospheric magnetic field parameters. A sequence of scans covering several hours of time shows evolution of the magnetic field. Examination of the linear polarization of the OH 1565.2nm shows curious temporal variation which results in a magnetic azimuth radically different from that measured using the photospheric lines. (Similar OH polarization behavior is seen in data from the CSUN San Fernando Observatory vacuum telescope taken with the CSUN/NSO camera in active region NOAA 10069 on 12 Aug 2002.) Finally, maps of the CN 1564.6nm Stokes I line shift show rapid penumbral Evershed flows and a curious signal in the sunspot umbra.

Some of this work is carried out through the National Solar Observatory Research Experiences for Undergraduate (REU) site program, which is co-funded by the Department of Defense in partnership with the National Science Foundation REU Program. Title: An Online Astronomy Course VS. A Interactive Classroom Authors: Slater, Timothy F.; Bailey, Janelle M.; Jaeggli, Sarah A.; Jones, Lauren V.; Lee, Ariane C. Bibcode: 2003IAUSS...4E..27S Altcode: Contemporary science education reforms emphasize building instruction around students’ pre-instructional beliefs fostering a learning environment where students interact with information and phenomena and providing students with frequent feedback to help them monitor their own learning. Recently personal computers and the Internet have given students access to scientific data sets and visualization tools that only professional scientists could use a few years before. With these things in mind we designed a hypermedia learning experience for introductory astronomy (Astronomy Online) that matches Internet technology with how people learn. Astronomy Online was used as the sole delivery system for courses offered during the Fall 2002 semester. The courses are run online. In one manifestation the course was delivered to middle and secondary school teachers spread across the globe. In another version the course was delivered to college undergraduate non-science majors where the only class meetings were a single orientation session and three on-campus exams. We compare these with on-campus courses that use highly interactive teaching techniques by studying common examination questions the Astronomy Diagnostic Test an attitude survey and interviews with students Title: An Online Interactive Astronomy Course for Non-Science Majors Authors: Slater, T. F.; Jones, L. V.; Bailey, J. M.; Jaeggli, S. A.; Lee, A. C. Bibcode: 2002AAS...201.8803S Altcode: 2002BAAS...34.1249S Contemporary science education reforms emphasize the need to build instruction around students' pre-instructional beliefs, to foster a productive learning environment for students to interact with information and phenomena, and to provide students with frequent feedback to help them monitor their own learning. Over the last five years, personal computers and the Internet have given students the opportunity to explore actual scientific data sets and use scientific visualization tools in ways that only professional scientists could only a few years before. Taken together, the authors have created a hypermedia learning experience for introductory astronomy that matches Internet technology with how people learn. This course weaves multimedia visualizations into a structured learning environment by dividing complex concepts into bite-size pieces. Each cognitive piece contains hyperlinks explaining all terms as well as illustrated using high-resolution images, animations, and videos which students manipulate to answer questions. Each module helps students engage in the pursuit of astronomy by providing activities where students make astronomical observations. Learners are required to answer pre-module questions, not as multiple-choice questions, but as written narratives, about the concept under study to make their knowledge explicit. At the conclusion, students compare new ideas with their initial answers and evaluate various alternative explanations. Astronomy Online was used as the sole delivery system for a course offered during the Fall 2002 semester. The course was run online; the only class meetings were a single orientation session and three on-campus exams. We compare this with on-campus courses that use highly interactive teaching techniques by studying common examination questions, the Astronomy Diagnostic Test, an attitude survey, and interviews with students.