Author name code: jones ADS astronomy entries on 2022-09-14 author:"Jones, Harrison P." ------------------------------------------------------------------------ Title: Results from the WINCS Ion Energy Analyzer on the NASA Green Propellant Infusion Mission Authors: Nicholas, A. C.; Herrero, F. A.; Finne, T. T.; Jones, H.; Aalami, D. Bibcode: 2020AGUFMSA023..12N Altcode: The instrument suite WINCS (Wind Ion/Neutral Composition Suite) is operating on the NASA GPIM (Green Propellant Infusion Mission). The miniaturized charged-particle spectrometers measurements are: neutral wind, temperature and composition - and ion-drift, ion temperature and ion composition; the WINCS size being 3x3x3 inches3 having a mass of 650g and consuming power of 1.7W. This presentation will focus on the data from the ion energy analyzer during the latter phase of the GPIM mission when the orbit was eccentric, ~300 km x 700km. The data have been analyzed using the Levenberg-Marquart algorithm via discrete inverse theory to simultaneously fit the observed peaks from ionospheric constituents in energy spectra. This analysis will provide ion temperature and composition over the course of the orbit. Title: Site Selection and Instrument Considerations for Micro-Rover Exploration of Lunar Polar Ice: The MoonRanger Mission Authors: Schweitzer, L.; Elphic, R. C.; Jones, H.; Wettergreen, D. S.; Whittaker, W. Bibcode: 2020AGUFMP023.0012S Altcode: Lunar ice holds the prospect of water for drinking, growing food, generating oxygen, and producing propellants. Successful ice utilization relies heavily on yet-undetermined knowledge of accessible concentrations at useful scales. This can only be achieved by surface missions. Some explorations will be undertaken by MER-scale rovers (e.g. VIPER in 2023), but a capable new class of micro-rovers may provide complementary coverage over multiple landing sites. Micro-rovers present, however, unique considerations of siting, instrumentation, and operations for high-return missions.

Small rovers can cost less, weigh less, and fly more frequently; however, they also have lower energy storage and more limited slope capability for probing into darkness and reaching stable ice. They likely offer less range from their landers and no direct-to-Earth communication to provide human oversight. Additionally, the small landers that deliver small rovers may provide less precision in landing site targeting and less tolerance of landing slopes and hazards. They require full sunlight and line of sight to Earth. We present a methodology and results for search and site selection based on these considerations. Favorable sites are found to be a minor subset of those acceptable for VIPER-scale roving. Several most-favorable sites are profiled and compared. Title: SEE: The 2017 Solar Eclipse Excursion, Mt. San Antonio College Edition Authors: Boryta, M. D.; Jones, H. P.; Lawlor, E.; Webb, C.; Hood, M.; Bray-Ali, J.; Draper, J. Bibcode: 2020AGUFMSY0140004B Altcode: Mt. SAC is a large single-campus two-year college in the greater Los Angeles area. Our Department of Earth Sciences and Astronomy has a strong education and outreach program that includes a busy planetarium and astronomical observatory. Four Mt SAC faculty and staff led a group of 19 students to Krupp Scout Hollow (KSH; Rigby, Idaho) to view the 2017 Solar Eclipse.

Our 7-day trip was designed to be affordable and educational for students. With college support for vehicles and gas we were able to keep costs down to $160 per student, using department telescopes and camping gear. We camped in low-cost areas including National Parks, and everyone took part in cooking meals at the campsite.

We attracted students by offering a program of geological adventure and cultural significance in addition to the eclipse experience. Geology and Anthropology faculty researched and planned excursions along the trek to and from the final eclipse destination. Students who attended got training in telescope operating to prepare for the eclipse and to facilitate viewing by the public. Astronomers planned activities for the 800+ drop-in guests during the event. KSH arranged for other groups to be present; e.g., NASA meteorologists carefully measured the drop in temperature (11°C!) as a function of eclipse. We were able to live-stream the entire eclipse, including footage from our solar telescope, back to our Planetarium, where another 4000+ students and community members were able to participate.

We have already begun planning a similar excursion for the 2024 eclipse. We suggest looking for and securing a viable spot far ahead of time - one with the least chance of rain/cloudy weather for that time of year. Check on electrical and internet connections, parking, bathroom and cooking facilities for your group. Allow participants to take part as much as possible in planning meals, duties, travel, etc. Plan too for an exponential surge in interest and applicants close to the event! Title: Lunar Pit Exploration via Autonomous Micro-Rover Authors: Ford, J.; Jones, H.; Wong, U.; Sharif, K.; Whittaker, W. Bibcode: 2020AGUFMP084...01F Altcode: Lunar pits are compelling destinations for surface mission exploration. They could access lava tubes with prospects of haven from the extreme temperatures, radiation exposures and micrometeorite hazards of the surface. Their walls offer direct observation of the only geologic columns not obscured by regolith, and they are scientifically interesting in their own right. The required vantages and proximities for these inquiries are not possible from orbit and motivate robotic surface exploration.

This paper presents an autonomous micro-rover a pproach to exploration and mapping of lunar pits by in-situ modeling via imagery gathered from their rims. The mission concept incorporates a commercial lander, rover forays around the rim, autonomous acquisition of a vast image dataset, and incremental photogrammetric construction of a pit model from the imagery. We develop the requisite autonomy, modeling, computing, and mobility technologies and present results from a case study performed at a terrestrial analog pit. We demonstrate the coverage and accuracy achievable by this method and conclude with progress toward a fully integrated rover for this important new class of mission. The rover incorporates telephoto lensing to achieve the requisite resolution for observing detail across vast pit dimensions. For frequent, affordable, commercial landing opportunities, the rover must be small and solar powered. To complete a long range mission before the onset of lunar night, the rover requires unprecedented autonomy, steep-slope mobility, high performance computing and state-of-the-art photogrammetry algorithms. We present a case study applying micro-rover imaging, computing, and photogrammetry to a terrestrial pit. This acquires 10,000 high resolution, high dynamic range images from 26 poses around the rim of the West Desert Sinkhole which is a terrestrial pit with diameter, depth, and stratification analogous to known lunar mare pits. Results are compared to ground truth LIDAR with error below 10cm across 90% of the pit surface. Title: Erratum: The first planet detected in the WTS: an inflated hot-Jupiter in a 3.35 day orbit around a late F-star Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.; Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.; Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.; Martín, E. L.; Snellen, I.; Barnes, J.; Campbell, D.; Catalan, S.; Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk, O.; Jones, H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.; Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.; Steele, P.; Stoev, H.; Tata, R.; Zendejas, J. Bibcode: 2020MNRAS.497..916C Altcode: No abstract at ADS Title: Preliminary Results from the WINCS sensor on the NASA Green Propellant Infusion Mission Authors: Nicholas, A. C.; Herrero, F. A.; Finne, T. T.; Aalami, D.; Jones, H. Bibcode: 2019AGUFMSA33B3144N Altcode: The instrument suite WINCS (Wind Ion/Neutral Composition Suite) is operating on the NASA GPIM (Green Propellant Infusion Mission). The miniaturized charged-particle spectrometers measurements are: neutral wind, temperature and composition - and ion-drift, ion temperature and ion composition; the WINCS size being 3x3x3 inches3 having a mass of 650g and consuming power of 1.7W. Since the neutrals entering WINCS are not affected by spacecraft charging, the combined neutral and ion measurements provide a method to measure the spacecraft potential in the ionosphere. Preliminary results will be presented to illustrate this method of monitoring spacecraft charging. In addition it will be possible to detect distortions of ion trajectories by unwanted electric fields in the vicinity of WINCS. Understanding these instrumental effects would then clear the way to obtain the six basic parameters of the ionosphere/ thermosphere fluid, consisting of bulk velocity vectors (neutral wind and ion-drift), temperatures, and compositions of the neutrals and ions in the ionosphere/thermosphere system. Preliminary determinations of these parameters will be presented. Title: Extraordinary rocks from the peak ring of the Chicxulub impact crater: P-wave velocity, density, and porosity measurements from IODP/ICDP Expedition 364 Authors: Christeson, G. L.; Gulick, S. P. S.; Morgan, J. V.; Gebhardt, C.; Kring, D. A.; Le Ber, E.; Lofi, J.; Nixon, C.; Poelchau, M.; Rae, A. S. P.; Rebolledo-Vieyra, M.; Riller, U.; Schmitt, D. R.; Wittmann, A.; Bralower, T. J.; Chenot, E.; Claeys, P.; Cockell, C. S.; Coolen, M. J. L.; Ferrière, L.; Green, S.; Goto, K.; Jones, H.; Lowery, C. M.; Mellett, C.; Ocampo-Torres, R.; Perez-Cruz, L.; Pickersgill, A. E.; Rasmussen, C.; Sato, H.; Smit, J.; Tikoo, S. M.; Tomioka, N.; Urrutia-Fucugauchi, J.; Whalen, M. T.; Xiao, L.; Yamaguchi, K. E. Bibcode: 2018E&PSL.495....1C Altcode: Joint International Ocean Discovery Program and International Continental Scientific Drilling Program Expedition 364 drilled into the peak ring of the Chicxulub impact crater. We present P-wave velocity, density, and porosity measurements from Hole M0077A that reveal unusual physical properties of the peak-ring rocks. Across the boundary between post-impact sedimentary rock and suevite (impact melt-bearing breccia) we measure a sharp decrease in velocity and density, and an increase in porosity. Velocity, density, and porosity values for the suevite are 2900-3700 m/s, 2.06-2.37 g/cm3, and 20-35%, respectively. The thin (25 m) impact melt rock unit below the suevite has velocity measurements of 3650-4350 m/s, density measurements of 2.26-2.37 g/cm3, and porosity measurements of 19-22%. We associate the low velocity, low density, and high porosity of suevite and impact melt rock with rapid emplacement, hydrothermal alteration products, and observations of pore space, vugs, and vesicles. The uplifted granitic peak ring materials have values of 4000-4200 m/s, 2.39-2.44 g/cm3, and 8-13% for velocity, density, and porosity, respectively; these values differ significantly from typical unaltered granite which has higher velocity and density, and lower porosity. The majority of Hole M0077A peak-ring velocity, density, and porosity measurements indicate considerable rock damage, and are consistent with numerical model predictions for peak-ring formation where the lithologies present within the peak ring represent some of the most shocked and damaged rocks in an impact basin. We integrate our results with previous seismic datasets to map the suevite near the borehole. We map suevite below the Paleogene sedimentary rock in the annular trough, on the peak ring, and in the central basin, implying that, post impact, suevite covered the entire floor of the impact basin. Suevite thickness is 100-165 m on the top of the peak ring but 200 m in the central basin, suggesting that suevite flowed downslope from the collapsing central uplift during and after peak-ring formation, accumulating preferentially within the central basin. Title: Long-Term Recovery of Life in the Chicxulub Crater Authors: Lowery, C.; Jones, H.; Bralower, T. J.; Smit, J.; Rodriguez-Tovar, F. J.; Whalen, M. T.; Owens, J. D.; Expedition 364 Science Party, I. I. Bibcode: 2017AGUFM.P23H..07L Altcode: The Chicxulub Crater on the Yucatán Peninsula of Mexico was formed by the impact of an asteroid 66 Ma that caused the extinction of 75% of genera on Earth. Immediately following the impact, the decimated ecosystem began the long process of recovery, both in terms of primary productivity and species diversity. This well-documented process was heterogeneous across the world ocean, but until the present time it has been inaccessible at ground zero of the impact. IODP/ICDP Exp. 364 recovered 9.5 m of pelagic limestone spanning the entire Paleocene, including a continuous section spanning the first 5 myr following the impact. The Chicxulub Crater is the largest known marine impact crater on Earth, and the recovery of the ecosystem presented here is the first such record of long-term primary succession in the sterile zone of a large impact crater. Planktic and benthic foraminifera, calcareous nannoplankton, calcispheres, bioturbation, and geochemical proxies all indicate that export productivity in the Chicxulub Crater recovered rapidly (within 30 kyr) following the impact. Recovery in terms of diversity and species abundance took much longer, and varied between groups. Planktic foraminifera quickly diversified, with all common Paleocene tropical/subtropical species appearing roughly when expected. Trace fossils appear rapidly after the event, with a progressive recovery through the lowermost Paleocene. Calcareous nannoplankton took much longer to recover, and disaster taxa like Braarudosphaera dominated the assemblage well into the late Paleocene. Paleoecology and geochemistry relate these trends to oceanographic conditions within the Chicxulub Crater. Planktic foraminifera from known depth habitats, including Morozovellids, Acarininids, Chiloguembelinids, and Subbotinids, track changes in the water column structure and paleoredox conditions within the crater. Diverse and abundant macro- and microbenthic organisms indicate food availability and good oxygen conditions on the seafloor. The latest Paleocene, just prior to the onset of the PETM, is characterized by a typical and diverse assemblage of foraminifera and calcareous nannoplankton; a normal open-marine assemblage with no trace of long-term negative effects from the impact. Title: Terrestrial Palynology of Paleocene and Eocene Sediments Above the Chicxulub Impact Crater Authors: Smith, V.; Warny, S.; Bralower, T. J.; Jones, H.; Lowery, C. M.; Smit, J.; Vajda, V.; Vellekoop, J.; 364 Scientists, E. Bibcode: 2017AGUFM.P33D2906S Altcode: International Ocean Discovery Program (IODP) Expedition 364, with support from the International Continental Scientific Drilling Program, cored through Paleocene and Eocene sediments and into the impact structure of the Chicxulub impact crater. Three palynological studies of the post-impact section are currently underway. The two other studies are investigating the dinoflagellate palynology and terrestrial palynology of the K/Pg boundary section, while this study focuses on the early Eocene terrestrial palynology of the IODP 364 core, which has yielded a diverse and well preserved pollen assemblage. A few samples from the Early Paleocene have also been examined but organic microfossil preservation is quite poor. Samples from this core are the oldest palynological record from the Yucatan peninsula. Sample preparation and detailed abundance counts of sixty samples throughout the post-impact section are in progress, with a particular focus on the Paleocene-Eocene Thermal Maximum (PETM) and the Early Eocene Climatic Optimum (EECO). Terrestrial palynomorph assemblages will be used to reconstruct paleoclimatological conditions throughout this time period. Floral response to hyperthermal events in the IODP 364 core will be compared with records from other Gulf of Mexico and Caribbean sections. In addition to the biological and paleoclimatological implications of this research, age control from foraminiferal and nannofossil biostratigraphy, paleomagnetism, and radiometric dating will provide a chronological framework for the terrestrial pollen biostratigraphy, with applications to hydrocarbon exploration in the Wilcox Formation and age equivalent sections in the Gulf of Mexico. Title: The Recovery of Life in the Chicxulub Crater Following the End Cretaceous Mass Extinction Authors: Lowery, C. M.; Jones, H.; Smit, J.; Bralower, T. J.; Owens, J. D.; IODP-ICDP Expedition 364 Science Party Bibcode: 2017LPI....48.2156L Altcode: We present the first record of the recovery of life in a large impact crater. Zoo- and phytoplankton follow diveregent trends for millions of years post-impact. Title: IODP/ICDP Expedition 364-Drilling the Cretaceous-Paleogene Chicxulub impact crater: Insights into large craters formation and their effect on life. Authors: Gulick, S. P. S.; Morgan, J. V.; Fucugauchi, J. U.; Bralower, T. J.; Chenot, É.; Christeson, G. L.; Claeys, P.; Cockell, C. S.; Collins, G. S.; Coolen, M.; Gebhardt, C.; Goto, K.; Kring, D. A.; Xiao, L.; Lowery, C.; Mellett, C.; Ocampo-Torres, R.; Osinski, G. R.; Perez-Cruz, L. L.; Pickersgill, A.; Poelchau, M.; Rae, A.; Rasmussen, C.; Rebolledo-Vieyra, M.; Riller, U. P.; Sato, H.; Schmitt, D. R.; Smit, J.; Tikoo, S.; Tomioka, N.; Whalen, M. T.; Zylberman, W.; Jones, H.; Gareth, C.; Wittmann, A.; Lofi, J.; Yamaguchi, K. E.; Ferrière, L. Bibcode: 2016AGUFM.P31E..05G Altcode: An international project to drill the Chicxulub impact crater was conducted in April and May, 2016 as Expedition 364 of the International Ocean Discovery Program (IODP) and International Continental Scientific Drilling Project (ICDP). Site M0077 is located offshore Yucatan in the southern Gulf of Mexico. The target was to core the only pristine terrestrial peak ring and to measure physical properties of the entire borehole. Specific questions included: What rocks comprise a topographic peak ring? How are peak rings formed? How are rocks weakened during large impacts to allow them to collapse and form relatively wide, flat craters? What insights arise from biologic recovery in the Paleogene within a potentially "toxic" ocean basin? Are impact craters (including peak rings) habitats for life? Coring occurred from 503 - 1334.7 mbsf with nearly 100% recovery. Wireline logs were collected from ultra slimline tools to total depth including gamma ray, magnetic susceptibility, sonic, borehole fluid temperature and conductivity, resistivity data, borehole images, and a finely spaced vertical seismic profile. Stratigraphy cored included 110 m of Eocene and Paleocene carbonates, 130 m of allochthonous impactites, and 590 m of crustal basement with dikes. All cores were measured using a shipboard core logger (density, gamma ray, magnetic susceptibility and resistivity) and shorebased dual energy, 0.3 mm resolution CT scanner. These data allow us to: 1) refine numerical models of the formation of the Chicxulub impact structure; 2) place constraints on environmental perturbations that led to the K-Pg mass extinction; 3) improve simulations of impact craters on other planetary bodies; 4) examine deformation mechanisms for insights into how rocks weaken during impacts; 5) study impact generated hydrothermal systems and 6) understand the effects of impacts on the deep biosphere including as a habitat for microbial life with implications for evolution on Earth and astrobiology. Key results are that the Chicxulub peak ring is formed from fractured basement rocks that may host a subsurface biosphere. The impactite layer overlying the peak ring in turn provides insight into resurge and tsunami processes, while the Paleogene sediments contain the record of the recovery of life after the mass extinction event. Title: Route Planning Software for Lunar Polar Missions Authors: Cunningham, C.; Jones, H.; Amato, J.; Holst, I.; Otten, N.; Kitchell, F.; Whittaker, W.; Horchler, A. Bibcode: 2016LPICo1960.5062C Altcode: Rover mission planning on the lunar poles is challenging due to the long, time-varying shadows. This abstract presents software for efficiently planning traverses while balancing competing demands of science goals, rover energy constraints, and risk. Title: Quantitative Evaluation of a Planetary Renderer for Terrain Relative Navigation Authors: Amoroso, E.; Jones, H.; Otten, N.; Wettergreen, D.; Whittaker, W. Bibcode: 2016LPICo1960.5037A Altcode: A ray-tracing computer renderer tool is presented based on LOLA and LROC elevation models and is quantitatively compared to LRO WAC and NAC images for photometric accuracy. We investigated using rendered images for terrain relative navigation. Title: Results of Lunar Rover Drivetrain TRL-6 Environmental Testing Authors: Visscher, P.; Edmundson, P.; Ghafoor, N.; Jones, H.; Kleinhenz, J.; Picard, M. Bibcode: 2016LPICo1960.5027V Altcode: Latest results of work performed by Ontario Drive and Gear Ltd., Canadensys Aerospace Corporation, and partners on Canadian lunar rover development activities for the Canadian Space Agency, including "dirty" thermal vacuum testing of drivetrain unit. Title: Ca II 854.2 nm Spectromagnetograms: A Powerful Chromospheric Diagnostic Authors: Harvey, J. W.; Bertello, Luca; Branston, D.; Britanik, J.; Bulau, S.; Cole, L.; Gosain, Sanjay; Harker, Brian; Jones, Harrison P.; Marble, A.; Martinez Pillet, V.; Pevtsov, A.; Schramm, K.; Streander, Kim; Villegas, H. Bibcode: 2016SPD....4710106H Altcode: The transition from physical dominance by plasma flows in the photosphere to magnetic pressure in the solar chromosphere motivates as many diagnostic observations as possible across this important region. Among the few ground-accessible spectral lines formed within the chromosphere, the Ca II 854.2 nm line has the desirable properties of presence everywhere on the solar disk, Zeeman sensitivity, and narrow line width. Mapped observations of circular polarization within this line (spectromagnetograms) have been made at NSO infrequently since 1974, with regular daily full-disk observations starting in August 1996. Full-disk spectral observations of the complete Stokes polarization vector are now being made regularly since November 2015. It is not easy to estimate chromospheric magnetic field properties from the 854.2 nm line profile polarization. To provide rough quick-look vector field maps we found that the weak-field approximation provides a fair first estimate of the line-of-sight component but appears to be too simple to interpret the transverse magnetic field from frequently asymmetric, linearly-polarized line profiles. More realistic estimates of the chromospheric vector field, short of extremely lengthy, full 3D, non-local radiative transfer inversions, are being investigated. We briefly introduce recent instrumental modifications and observational characteristics, sample observations, and results concerning the expansion of the chromospheric field with increasing height, the presence of large areas of weak, nearly horizontal fields, and field estimates in plages, sunspots, flares, filaments, and filament channels. The Stokes spectra will be freely available to the community.This work utilizes SOLIS data obtained by the NSO Integrated Synoptic Program (NISP), managed by the National Solar Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA), Inc. under a cooperative agreement with the National Science Foundation. Title: The EChO science case Authors: Tinetti, Giovanna; Drossart, Pierre; Eccleston, Paul; Hartogh, Paul; Isaak, Kate; Linder, Martin; Lovis, Christophe; Micela, Giusi; Ollivier, Marc; Puig, Ludovic; Ribas, Ignasi; Snellen, Ignas; Swinyard, Bruce; Allard, France; Barstow, Joanna; Cho, James; Coustenis, Athena; Cockell, Charles; Correia, Alexandre; Decin, Leen; de Kok, Remco; Deroo, Pieter; Encrenaz, Therese; Forget, Francois; Glasse, Alistair; Griffith, Caitlin; Guillot, Tristan; Koskinen, Tommi; Lammer, Helmut; Leconte, Jeremy; Maxted, Pierre; Mueller-Wodarg, Ingo; Nelson, Richard; North, Chris; Pallé, Enric; Pagano, Isabella; Piccioni, Guseppe; Pinfield, David; Selsis, Franck; Sozzetti, Alessandro; Stixrude, Lars; Tennyson, Jonathan; Turrini, Diego; Zapatero-Osorio, Mariarosa; Beaulieu, Jean-Philippe; Grodent, Denis; Guedel, Manuel; Luz, David; Nørgaard-Nielsen, Hans Ulrik; Ray, Tom; Rickman, Hans; Selig, Avri; Swain, Mark; Banaszkiewicz, Marek; Barlow, Mike; Bowles, Neil; Branduardi-Raymont, Graziella; du Foresto, Vincent Coudé; Gerard, Jean-Claude; Gizon, Laurent; Hornstrup, Allan; Jarchow, Christopher; Kerschbaum, Franz; Kovacs, Géza; Lagage, Pierre-Olivier; Lim, Tanya; Lopez-Morales, Mercedes; Malaguti, Giuseppe; Pace, Emanuele; Pascale, Enzo; Vandenbussche, Bart; Wright, Gillian; Ramos Zapata, Gonzalo; Adriani, Alberto; Azzollini, Ruymán; Balado, Ana; Bryson, Ian; Burston, Raymond; Colomé, Josep; Crook, Martin; Di Giorgio, Anna; Griffin, Matt; Hoogeveen, Ruud; Ottensamer, Roland; Irshad, Ranah; Middleton, Kevin; Morgante, Gianluca; Pinsard, Frederic; Rataj, Mirek; Reess, Jean-Michel; Savini, Giorgio; Schrader, Jan-Rutger; Stamper, Richard; Winter, Berend; Abe, L.; Abreu, M.; Achilleos, N.; Ade, P.; Adybekian, V.; Affer, L.; Agnor, C.; Agundez, M.; Alard, C.; Alcala, J.; Allende Prieto, C.; Alonso Floriano, F. J.; Altieri, F.; Alvarez Iglesias, C. A.; Amado, P.; Andersen, A.; Aylward, A.; Baffa, C.; Bakos, G.; Ballerini, P.; Banaszkiewicz, M.; Barber, R. J.; Barrado, D.; Barton, E. J.; Batista, V.; Bellucci, G.; Belmonte Avilés, J. A.; Berry, D.; Bézard, B.; Biondi, D.; Błęcka, M.; Boisse, I.; Bonfond, B.; Bordé, P.; Börner, P.; Bouy, H.; Brown, L.; Buchhave, L.; Budaj, J.; Bulgarelli, A.; Burleigh, M.; Cabral, A.; Capria, M. T.; Cassan, A.; Cavarroc, C.; Cecchi-Pestellini, C.; Cerulli, R.; Chadney, J.; Chamberlain, S.; Charnoz, S.; Christian Jessen, N.; Ciaravella, A.; Claret, A.; Claudi, R.; Coates, A.; Cole, R.; Collura, A.; Cordier, D.; Covino, E.; Danielski, C.; Damasso, M.; Deeg, H. J.; Delgado-Mena, E.; Del Vecchio, C.; Demangeon, O.; De Sio, A.; De Wit, J.; Dobrijévic, M.; Doel, P.; Dominic, C.; Dorfi, E.; Eales, S.; Eiroa, C.; Espinoza Contreras, M.; Esposito, M.; Eymet, V.; Fabrizio, N.; Fernández, M.; Femenía Castella, B.; Figueira, P.; Filacchione, G.; Fletcher, L.; Focardi, M.; Fossey, S.; Fouqué, P.; Frith, J.; Galand, M.; Gambicorti, L.; Gaulme, P.; García López, R. J.; Garcia-Piquer, A.; Gear, W.; Gerard, J. -C.; Gesa, L.; Giani, E.; Gianotti, F.; Gillon, M.; Giro, E.; Giuranna, M.; Gomez, H.; Gomez-Leal, I.; Gonzalez Hernandez, J.; González Merino, B.; Graczyk, R.; Grassi, D.; Guardia, J.; Guio, P.; Gustin, J.; Hargrave, P.; Haigh, J.; Hébrard, E.; Heiter, U.; Heredero, R. L.; Herrero, E.; Hersant, F.; Heyrovsky, D.; Hollis, M.; Hubert, B.; Hueso, R.; Israelian, G.; Iro, N.; Irwin, P.; Jacquemoud, S.; Jones, G.; Jones, H.; Justtanont, K.; Kehoe, T.; Kerschbaum, F.; Kerins, E.; Kervella, P.; Kipping, D.; Koskinen, T.; Krupp, N.; Lahav, O.; Laken, B.; Lanza, N.; Lellouch, E.; Leto, G.; Licandro Goldaracena, J.; Lithgow-Bertelloni, C.; Liu, S. J.; Lo Cicero, U.; Lodieu, N.; Lognonné, P.; Lopez-Puertas, M.; Lopez-Valverde, M. A.; Lundgaard Rasmussen, I.; Luntzer, A.; Machado, P.; MacTavish, C.; Maggio, A.; Maillard, J. -P.; Magnes, W.; Maldonado, J.; Mall, U.; Marquette, J. -B.; Mauskopf, P.; Massi, F.; Maurin, A. -S.; Medvedev, A.; Michaut, C.; Miles-Paez, P.; Montalto, M.; Montañés Rodríguez, P.; Monteiro, M.; Montes, D.; Morais, H.; Morales, J. C.; Morales-Calderón, M.; Morello, G.; Moro Martín, A.; Moses, J.; Moya Bedon, A.; Murgas Alcaino, F.; Oliva, E.; Orton, G.; Palla, F.; Pancrazzi, M.; Pantin, E.; Parmentier, V.; Parviainen, H.; Peña Ramírez, K. Y.; Peralta, J.; Perez-Hoyos, S.; Petrov, R.; Pezzuto, S.; Pietrzak, R.; Pilat-Lohinger, E.; Piskunov, N.; Prinja, R.; Prisinzano, L.; Polichtchouk, I.; Poretti, E.; Radioti, A.; Ramos, A. A.; Rank-Lüftinger, T.; Read, P.; Readorn, K.; Rebolo López, R.; Rebordão, J.; Rengel, M.; Rezac, L.; Rocchetto, M.; Rodler, F.; Sánchez Béjar, V. J.; Sanchez Lavega, A.; Sanromá, E.; Santos, N.; Sanz Forcada, J.; Scandariato, G.; Schmider, F. -X.; Scholz, A.; Scuderi, S.; Sethenadh, J.; Shore, S.; Showman, A.; Sicardy, B.; Sitek, P.; Smith, A.; Soret, L.; Sousa, S.; Stiepen, A.; Stolarski, M.; Strazzulla, G.; Tabernero, H. M.; Tanga, P.; Tecsa, M.; Temple, J.; Terenzi, L.; Tessenyi, M.; Testi, L.; Thompson, S.; Thrastarson, H.; Tingley, B. W.; Trifoglio, M.; Martín Torres, J.; Tozzi, A.; Turrini, D.; Varley, R.; Vakili, F.; de Val-Borro, M.; Valdivieso, M. L.; Venot, O.; Villaver, E.; Vinatier, S.; Viti, S.; Waldmann, I.; Waltham, D.; Ward-Thompson, D.; Waters, R.; Watkins, C.; Watson, D.; Wawer, P.; Wawrzaszk, A.; White, G.; Widemann, T.; Winek, W.; Wiśniowski, T.; Yelle, R.; Yung, Y.; Yurchenko, S. N. Bibcode: 2015ExA....40..329T Altcode: 2015ExA...tmp...67T; 2015arXiv150205747T The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune—all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10-4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest spectral resolving power is needed, with R ~ 300 for wavelengths less than 5 μm and R ~ 30 for wavelengths greater than this. The transit spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m2 is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m2 telescope, diffraction limited at 3 μm has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate than current observations. This would enable the detection of molecular abundances three orders of magnitude lower than currently possible and a fourfold increase from the handful of molecules detected to date. Combining these data with estimates of planetary bulk compositions from accurate measurements of their radii and masses would allow degeneracies associated with planetary interior modelling to be broken, giving unique insight into the interior structure and elemental abundances of these alien worlds. EChO would allow scientists to study exoplanets both as a population and as individuals. The mission can target super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300-3000 K) of F to M-type host stars. The EChO core science would be delivered by a three-tier survey. The EChO Chemical Census: This is a broad survey of a few-hundred exoplanets, which allows us to explore the spectroscopic and chemical diversity of the exoplanet population as a whole. The EChO Origin: This is a deep survey of a subsample of tens of exoplanets for which significantly higher signal to noise and spectral resolution spectra can be obtained to explain the origin of the exoplanet diversity (such as formation mechanisms, chemical processes, atmospheric escape). The EChO Rosetta Stones: This is an ultra-high accuracy survey targeting a subsample of select exoplanets. These will be the bright "benchmark" cases for which a large number of measurements would be taken to explore temporal variations, and to obtain two and three dimensional spatial information on the atmospheric conditions through eclipse-mapping techniques. If EChO were launched today, the exoplanets currently observed are sufficient to provide a large and diverse sample. The Chemical Census survey would consist of > 160 exoplanets with a range of planetary sizes, temperatures, orbital parameters and stellar host properties. Additionally, over the next 10 years, several new ground- and space-based transit photometric surveys and missions will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Title: Lunar Rover Drivetrain Development to TRL-6 Authors: Visscher, P.; Edmundson, P.; Ghafoor, N.; Jones, H.; Kleinhenz, J.; Picard, M. Bibcode: 2015LPICo1863.2009V Altcode: The LRPDP and SPRP rovers are designed to provide high mobility and robustness in a lunar working environment and are compatible with various lunar surface activities. TRL-6 testing is scheduled for late 2015 on the rover drivetrain components. Title: Rover Traverse Planning to Support a Lunar Polar Volatiles Mission Authors: Heldmann, J. L.; Colaprete, A. C.; Elphic, R. C.; Bussey, B.; McGovern, A.; Beyer, R.; Lees, D.; Deans, M. C.; Otten, N.; Jones, H.; Wettergreen, D. Bibcode: 2015LPICo1863.2007H Altcode: We present notional traverse plans for NASA’s Resource Prospector mission for a lunar polar rover and utilize this mission architecture and associated constraints to evaluate whether a suitable landing site exists to support an RP flight mission. Title: The SAMI Galaxy Survey: cubism and covariance, putting round pegs into square holes Authors: Sharp, R.; Allen, J. T.; Fogarty, L. M. R.; Croom, S. M.; Cortese, L.; Green, A. W.; Nielsen, J.; Richards, S. N.; Scott, N.; Taylor, E. N.; Barnes, L. A.; Bauer, A. E.; Birchall, M.; Bland-Hawthorn, J.; Bloom, J. V.; Brough, S.; Bryant, J. J.; Cecil, G. N.; Colless, M.; Couch, W. J.; Drinkwater, M. J.; Driver, S.; Foster, C.; Goodwin, M.; Gunawardhana, M. L. P.; Ho, I. -T.; Hampton, E. J.; Hopkins, A. M.; Jones, H.; Konstantopoulos, I. S.; Lawrence, J. S.; Leslie, S. K.; Lewis, G. F.; Liske, J.; López-Sánchez, Á. R.; Lorente, N. P. F.; McElroy, R.; Medling, A. M.; Mahajan, S.; Mould, J.; Parker, Q.; Pracy, M. B.; Obreschkow, D.; Owers, M. S.; Schaefer, A. L.; Sweet, S. M.; Thomas, A. D.; Tonini, C.; Walcher, C. J. Bibcode: 2015MNRAS.446.1551S Altcode: 2014arXiv1407.5237S We present a methodology for the regularization and combination of sparse sampled and irregularly gridded observations from fibre-optic multiobject integral field spectroscopy. The approach minimizes interpolation and retains image resolution on combining subpixel dithered data. We discuss the methodology in the context of the Sydney-AAO multiobject integral field spectrograph (SAMI) Galaxy Survey underway at the Anglo-Australian Telescope. The SAMI instrument uses 13 fibre bundles to perform high-multiplex integral field spectroscopy across a 1° diameter field of view. The SAMI Galaxy Survey is targeting ∼3000 galaxies drawn from the full range of galaxy environments. We demonstrate the subcritical sampling of the seeing and incomplete fill factor for the integral field bundles results in only a 10 per cent degradation in the final image resolution recovered. We also implement a new methodology for tracking covariance between elements of the resulting data cubes which retains 90 per cent of the covariance information while incurring only a modest increase in the survey data volume. Title: Erratum: The first planet detected in the WTS: an inflated hot-Jupiter in a 3.35 d orbit around a late F star Authors: Cappetta, M.; Saglia, R. P.; Birkby, J. L.; Koppenhoefer, J.; Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, B.; Barrado, D.; Nefs, B.; Pavlenko, Y. V.; Fossati, L.; del Burgo, C.; Martín, E. L.; Snellen, I.; Barnes, J.; Campbell, D.; Catalan, S.; Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C.; Ivanyuk, O.; Jones, H.; Kuznetsov, M.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.; Napiwotzki, R.; Palle, E.; Pollacco, D.; Sarro Baro, L.; Solano, E.; Steele, P.; Stoev, H.; Tata, R.; Zendejas, J. Bibcode: 2014MNRAS.444.3150C Altcode: 2014arXiv1410.3235C We report the discovery of WTS-1b, the first extrasolar planet found by the WFCAM Transit Survey, which began observations at the 3.8-m United Kingdom Infrared Telescope (UKIRT) in August 2007. Light curves comprising almost 1200 epochs with a photometric precision of better than 1 per cent to J ~ 16 were constructed for ~60000 stars and searched for periodic transit signals. For one of the most promising transiting candidates, high-resolution spectra taken at the Hobby-Eberly Telescope (HET) allowed us to estimate the spectroscopic parameters of the host star, a late-F main sequence dwarf (V=16.13) with possibly slightly subsolar metallicity, and to measure its radial velocity variations. The combined analysis of the light curves and spectroscopic data resulted in an orbital period of the substellar companion of 3.35 days, a planetary mass of 4.01 +- 0.35 Mj and a planetary radius of 1.49+0.16-0.18 Rj. WTS-1b has one of the largest radius anomalies among the known hot Jupiters in the mass range 3-5 Mj. The high irradiation from the host star ranks the planet in the pM class. Title: Radial Velocity Studies of M Dwarfs Authors: Jones, H. Bibcode: 2014hwat.confE..23J Altcode: Our current view of exoplanets is one derived primarily from Solar-like stars with a strong focus on understanding our Solar System. Our knowledge about the properties of exoplanets around the dominant stellar population by number, the so called low-mass stars or M dwarfs is much more cursory. Based on combining radial velocities of nearby M dwarfs obtained with UVES and HARPS we find 8 new M dwarf planets and 2 previous known from a sample of 41 stars. By computing the estimated detection probability function the occurrence rate of planets less than 10 Earth masses around nearby M dwarfs is found to be of the order of one planet per star and that of habitable zone planets between 3 and 10 Earth masses around 20 percent. The mass of radial velocity M dwarf planets is relatively much lower than the expected mass dependency based on stellar mass and thus it is inferred that planet formation efficiency around low mass stars is relatively impaired. Techniques to overcome the practical issue of obtaining good quality radial velocity data for M dwarfs are considered: (1) the wavelength sensitivity of radial velocity signals, (2) the combination of radial velocity data from different experiments for robust detection of small amplitude signals and (3) optimum selection of targets. Title: Meeting the Challenge of Affordable Lunar Exploration - Heritage Systems, Flexible Partnerships, New Flight Opportunities Authors: Ghafoor, N.; Jones, H.; Jessen, S.; McCoubrey, R.; Fulford, P.; McCarthy, T.; Chappell, L.; Lackner, D.; Tadros, A. Bibcode: 2013LPICo1748.7058G Altcode: No abstract at ADS Title: Realistic limitations of detecting planets around young active stars Authors: Jeffers, S. V.; Barnes, J. R.; Jones, H.; Pinfield, D. Bibcode: 2013EPJWC..4709002J Altcode: Current planet hunting methods using the radial velocity method are limited to observing middle-aged main-sequence stars where the signatures of stellar activity are much less than on young stars that have just arrived on the main-sequence. In this work we apply our knowledge from the surface imaging of these young stars to place realistic limitations on the possibility of detecting orbiting planets. In general we find that the magnitude of the stellar jitter is directly proportional to the stellar vsini. For G and K dwarfs, we find that it is possible, for models with high stellar activity and low stellar vsini, to be able to detect a 1 MJupiter mass planet within 50 epochs of observations and for the M dwarfs it is possible to detect a habitable zone Earth-like planet in 10s of observational epochs. Title: The 2MASS Tully-Fisher Survey: Mapping the mass in the Universe Authors: Hong, T.; Staveley-Smith, L.; Masters, K.; Springob, C.; Macri, L.; Koribalski, B.; Jones, H.; Jarrett, T. Bibcode: 2013IAUS..289..312H Altcode: 2012arXiv1212.2090H The 2MASS Tully-Fisher Survey (2MTF) aims to measure Tully-Fisher (TF) distances for all bright, inclined spirals in the 2MASS Redshift Survey (2MRS) using high-quality HI widths and 2MASS photometry. Compared with previous peculiar-velocity surveys, the 2MTF survey provides more accurate width measurements and more uniform sky coverage, combining observations with the Green Bank, Arecibo, and Parkes telescopes. With this new redshift-independent distance database, we will significantly improve our understanding of the mass distribution in the local Universe. Title: VVV high proper motion survey . Authors: Gromadzki, M.; Kurtev, R.; Folkes, S.; Beamín, J. C.; Peña Ramírez, K.; Borissova, J.; Pinfield, D.; Jones, H.; Minniti, D.; Ivanov, V. D. Bibcode: 2013MmSAI..84..980G Altcode: 2013arXiv1310.4072G Here we present survey of proper motion stars towards the Galactic Bulge and an adjacent plane region base on VISTA-VVV data. The searching method is based on cross-matching photometric K_s-band CASU catalogs. The most interesting discoveries are shown. Title: A new UKIDSS proper motion survey and key early results, including new benchmark systems Authors: Smith, L.; Lucas, P.; Burningham, B.; Jones, H.; Pinfield, D.; Smart, R.; Andrei, A. Bibcode: 2013MmSAI..84..976S Altcode: We present a proper motion catalogue for the 1500 deg2 of 2 epoch J-band UKIDSS Large Area Survey (LAS) data, which includes 120,000 stellar sources with motions detected above the 5sigma level. Our upper limit on proper motion detection is 3\farcs3 yr-1 and typical uncertainties are of order 10 mas yr-1 for bright sources from data with a modest 1.8-7.0 year epoch baseline. We developed a bespoke proper motion pipeline which applies a source-unique second order polynomial transformation to UKIDSS array coordinates to counter potential local non-uniformity in the focal plane. Our catalogue agrees well with the proper motion data supplied in the current WFCAM Science Archive (WSA) tenth data release (DR10) catalogue where there is overlap, and in various optical catalogues, but it benefits from some improvements, such as a larger matching radius and relative to absolute proper motion correction. We present proper motion results for 128 T dwarfs in the UKIDSS LAS and key early results of projects utilising our catalogue, in particular searches for brown dwarf benchmark systems through cross matches with existing proper motion catalogues. We report the discovery of two new T dwarf benchmark systems. Title: First T dwarfs in the VISTA Hemisphere Survey Authors: Lodieu, N.; Burningham, B.; Day-Jones, A.; Scholz, R. -D.; Marocco, F.; Koposov, S.; Barrado y Navascués, D.; Lucas, P. W.; Cruz, P.; Lillo, J.; Jones, H.; Perez-Garrido, A.; Ruiz, M. T.; Pinfield, D.; Rebolo, R.; Béjar, V. J. S.; Boudreault, S.; Emerson, J. P.; Banerji, M.; González-Solares, E.; Hodgkin, S. T.; McMahon, R.; Canty, J.; Contreras, C. Bibcode: 2012A&A...548A..53L Altcode: 2012arXiv1210.5148L
Aims: The aim of the project is to improve our current knowledge of the density of T dwarfs and the shape of the substellar initial mass function by identifying a magnitude-limited sample of T dwarfs in the full southern sky.
Methods: We present the results of a photometric search aimed at discovering cool brown dwarfs in the southern sky imaged at infrared wavelengths by the Visible and Infrared Survey Telescope for Astronomy (VISTA) and the Wide Infrared Survey Explorer (WISE) satellite mission. We combined the first data release (DR1) of the VISTA Hemisphere Survey (VHS) and the WISE preliminary data release to extract candidates with red mid-infrared colours and near- to mid-infrared colours characteristics of cool brown dwarfs.
Results: The VHS DR1 vs. WISE search returned tens of T dwarf candidates, 13 of which are presented here, including two previously published in the literature and five new ones confirmed spectroscopically with spectral types between T4.5 and T8. We estimate that the two T6 dwarfs lie within 16 pc and the T4.5 within 25 pc. The remaining three are 30-50 pc distant. The only T7 dwarf in our sample is the faintest of its spectral class with J = 19.28 mag. The other six T dwarf candidates remain without spectroscopic follow-up. We also improve our knowledge on the proper motion accuracy for three bright T dwarfs by combining multi-epoch data from public databases (DENIS, 2MASS, VHS, WISE, Spitzer).

Based on observations made with the Calar Alto 3.5-m telescope, the Magellan telescope at Las Campanas, the ESO Very Large Telescope at the Paranal Observatory, and the IAC80 at Teide Observatory.Figures 1 and 2 are available in electronic form at http://www.aanda.org Title: Towards an Imaging Mid-Infrared Heterodyne Spectrometer Authors: Hewagama, T.; Aslam, S.; Jones, H.; Kostiuk, T.; Villanueva, G.; Roman, P.; Shaw, G. B.; Livengood, T.; Allen, J. E. Bibcode: 2012LPICo1683.1125H Altcode: We will discuss efforts in developing a compact, low-mass, low-power, mid-infrared imaging heterodyne spectrometer for planetary science applications. Title: Physical parameters of the binary star CM draconis components Authors: Kuznetsov, M. K.; Pavlenko, Ya. V.; Pinfield, D.; Jones, H. Bibcode: 2012KPCB...28..137K Altcode: No abstract at ADS Title: Mapping the Dark Matter with 6dFGS Authors: Mould, Jeremy R.; Magoulas, C.; Springob, C.; Colless, M.; Jones, H.; Lucey, J.; Erdogdu, P.; Campbell, L. Bibcode: 2012AAS...22032101M Altcode: Fundamental plane distances from the 6dF Galaxy Redshift Survey are fitted to a model of the density field within 200/h Mpc. Likelihood is maximized for a single value of the local galaxy density, as expected in linear theory for the relation between overdensity and peculiar velocity. The dipole of the inferred southern hemisphere early type galaxy peculiar velocities is calculated within 150/h Mpc, before and after correction for the individual galaxy velocities predicted by the model. The former agrees with that obtained by other peculiar velocity studies (e.g. SFI++). The latter is only of order 150 km/sec and consistent with the expectations of the standard cosmological model and recent forecasts of the cosmic mach number, which show linearly declining bulk flow with increasing scale. Title: The 6dF Galaxy Survey: Baryon Acoustic Oscillations and the Local Hubble Constant Authors: Beutler, Florian; Blake, C.; Colless, M.; Staveley-Smith, L.; Jones, H. Bibcode: 2012AAS...21940201B Altcode: The large-scale correlation function of the 6dF Galaxy Survey (6dFGS) allows the detection of a Baryon Acoustic Oscillation (BAO) signal. The low effective redshift of 6dFGS makes it a competitive and independent alternative to Cepheids and low-z supernovae in constraining the Hubble constant. It also depends on very different (and arguably smaller) systematic uncertainties. We found a Hubble constant of H0 = 67 +/- 3.2 km/s/Mpc in agreement with the current standard cosmological model LCDM. Title: A Search for Extreme Ultracool Objects in UKIDSS+VISTA Authors: Zhang, Z.; Pinfield, D.; Day-Jones, A.; Burningham, B.; Jones, H.; Lucas, P.; Gomes, J.; Ruiz, M. T.; Gallardo, J.; Jenkins, J. Bibcode: 2011ASPC..448.1411Z Altcode: 2011csss...16.1411Z Brown dwarfs with thick water cloud atmospheres, ancient population III brown dwarfs, and nearby free-floating planetary mass objects are targets in our new discovery space. We have developed a candidate selection process that identifies near infrared sources without optical counterparts whose infrared/optical fluxes are not consistent with stars, and whose infrared colors are not like those of known L and T dwarf populations. We plan to carry out this programme over the next 3-4 years, and effectively give UKIDSS and VISTA the capability to measure proper motions of unusual objects in 14000 sq degs of infrared sky. High proper motion discoveries will be fast-tracked for spectroscopy through our ongoing 8m class telescopes initiatives. Title: Age patterns in a sample of spiral galaxies Authors: Sánchez-Gil, M. C.; Jones, H.; Pérez, E.; Bland-Hawthorn, J.; Alfaro, E. J.; O'Byrne, J. Bibcode: 2011hsa6.conf..345S Altcode: 2011arXiv1103.4147S We present the burst ages for young stellar populations in a sample of 6 nearby spiral galaxies using a differential pixel-by-pixel analysis of the ionized gas emission. We explore a new approach for connecting large-scale dynamical mechanisms with star formation processes in disk galaxies, based on burst ages derived from the Hα to far UV (FUV) flux ratio. Images of each galaxy in Hα were taken with Taurus Tunable Filter (TTF) and matched to FUV imaging from GALEX. The resulting flux ratio provides a robust measure of relative age across the disk which we discuss in terms of the large-scale dynamical motions. Systematic effects, such as a variable initial mass function (IMF), non-solar metallicities, variable star-formation history (SFHs), and dust attenuation, have been considered insofar as the models have permitted. The resulting age maps show age gradients along the spiral arms, in addition to circumnuclear regions (M94) or in HII complexes (IC 2574) in specific cases. Remarkably, in the case of M51 we find evidence for a stellar age gradient along short spurs of dust lane branching off the main spiral arms. We find that a comparison of the Hα and FUV observations of nearby spiral galaxies is a relatively direct way to probe burst age variations in spirals. Title: Do Disk Galaxies Have Different Central Velocity Dispersions At A Given Rotation Velocity? Authors: Danilovich, Taissa; Jones, H.; Mould, J.; Taylor, E.; Tonini, C.; Webster, R. Bibcode: 2011AAS...21840802D Altcode: 2011BAAS..43G40802D Hubble's classification of spiral galaxies was one dimensional. Actually it was 1.5 dimensional, as he distinguished barred spirals. Van den Bergh's was two dimensional: spirals had luminosity classes too. Other schemes are summarized at http://www.daviddarling.info/encyclopedia/G/galaxyclassification.html

A more quantitative approach is to classify spiral galaxies by rotation velocity. Their central velocity dispersion (bulge) tends to be roughly one half of their rotation velocity (disk). There is a trend from σ/W = 0.8 to σ/W = 0.2 as one goes from W = 100 to 500 km/s, where W is twice the rotation velocity. But some fraction of spirals have a velocity dispersion up to a factor of two larger than that.

In hierarchical galaxy formation models, the relative contributions of σ and W depend on the mass accretion history of the galaxy, which determines the mass distribution of the dynamical components such as disk, bulge and dark matter halo. The wide variety of histories that originate in the hierarchical mass assembly produce at any value of W a wide range of σ/W, that reaches high values in more bulge- dominated systems.

In a sense the two classifiers were both right: spirals are mostly one dimensional, but σ/W (bulge to disk ratio) is often larger than average. Is this a signature of merger history? Title: Reduction of SOLIS/VSM Intensity, Line Depth, and Equivalent Width Images Authors: Jones, Harrison P. Bibcode: 2011SPD....42.1515J Altcode: 2011BAAS..43S.1515J Most user interest in the SOLIS Vector Spectromagnetograph (VSM) centers on full-disk vector and longitudinal magnetograms which are used for many purposes including flare prediction, field extrapolation, and studies of the solar cycle. However, pseudo-continuum intensity, line-depth, and equivalent-width images, which are perfectly registered both in time and space with their corresponding magnetograms, are carried with the standard SOLIS data analysis to Level 1 (flat-fielding and sorting of individual scan lines into "raw" images). These quantities potentially provide important thermodynamic information which improve feature identification and inform models of photospheric and chromospheric structures, but the raw images contain many defects which prevent their direct use. Least-squares spline and polynomial algorithms are presented for compputing contrast images which are free of both these defects and center-to-limb variation. Title: Spectral Investigations of CM Dra Authors: Kuznetsov, M. K.; Pavlenko, Y. V.; Pinfield, D.; Jones, H. Bibcode: 2010OAP....23...74K Altcode: We present an analysis of a high resolution (R=47000) echelle spectra of the low-mass eclipsing binary CM Draconis, which were obtained on the 4.2-m William Herschel Telescope. Spectra were obtained for various phases of the orbit. There are some difficulties in echelle spectra processing of cool stars, since it is hard to get energy distribution in a large scale in such spectra. We proposed an efficient method for making the continuum of spectrum of cool stars. We refined the parameters (effective temperature, rotational velocity and metallicity) of the components of the system CM Dra using the method of stellar atmospheres. The data that we obtained are in good agreement with the results obtained by other authors. It is indicate on efficiency of our technique. The errors of temperature and metallicity determinations is about 100 K and 0.3 dex respectively. Title: Scaling relations of early-type galaxies in the 6dF Galaxy Survey Authors: Magoulas, C.; Colless, M.; Jones, H.; Mould, J.; Springob, C. Bibcode: 2010HiA....15...84M Altcode: Over 10,000 early-type galaxies from the 6dF Galaxy Survey (6dFGS) (Jones, D. H. et al. (2009), Jones et al. (2004)) have been used to determine the Fundamental Plane at optical and near-infrared wavelengths. We find that a maximum likelihood fit to an explicit three-dimensional Gaussian model for the distribution of galaxies in size, surface brightness and velocity dispersion can precisely account for selection effects, censoring and observational errors, leading to precise and unbiased parameters for the Fundamental Plane and its intrinsic scatter. Title: Other SOLIS Data: Intensity, Line Depth, and Equivalent Width from the VSM Authors: Jones, Harrison P. Bibcode: 2010shin.confE.149J Altcode: Most user interest in the SOLIS Vector Spectromagnetograph (VSM) has centered on full-disk vector and longitudinal magnetograms which are used for many purposes including flare prediction, field extrapolation, and studies of the solar cycle. However, additional thermodynamic information, is available which can potentially extend and improve the usefulness of VSM observations for tasks such as feature identification and informing models of photospheric and chromospheric structures. Pseudo-continuum intensity, line-depth, and equivalent-width images, which are perfectly registered both in time and space with their corresponding magnetograms, are carried with the standard SOLIS data analysis to Level 1 (flat-fielding and sorting of individual scan lines into Title: Statistical Feature Recognition for Multidimensional Solar Imagery Authors: Turmon, Michael; Jones, Harrison P.; Malanushenko, Olena V.; Pap, Judit M. Bibcode: 2010SoPh..262..277T Altcode: 2010SoPh..tmp...52T A maximum a posteriori (MAP) technique is developed to identify solar features in cotemporal and cospatial images of line-of-sight magnetic flux, continuum intensity, and equivalent width observed with the NASA/National Solar Observatory (NSO) Spectromagnetograph (SPM). The technique facilitates human understanding of patterns in large data sets and enables systematic studies of feature characteristics for comparison with models and observations of long-term solar activity and variability. The method uses Bayes' rule to compute the posterior probability of any feature segmentation of a trio of observed images from per-pixel, class-conditional probabilities derived from independently-segmented training images. Simulated annealing is used to find the most likely segmentation. New algorithms for computing class-conditional probabilities from three-dimensional Gaussian mixture models and interpolated histogram densities are described and compared. A new extension to the spatial smoothing in the Bayesian prior model is introduced, which can incorporate a spatial dependence such as center-to-limb variation. How the spatial scale of training segmentations affects the results is discussed, and a new method for statistical separation of quiet Sun and quiet network is presented. Title: Analysis of Ca II 8542 Å scanning spectroscopy for statistical feature recognition. Authors: Malanushenko, O.; Jones, H.; Turmon, M.; Pap, J. Bibcode: 2010MmSAI..81..801M Altcode: Previously, we used Bayesian methods to recognize active regions (AR), enhanced magnetic network (EN), and sunspots (SS) in National Solar Observatory/Kitt Peak Vacuum Telescope synoptic observations. In this paper we study imaging spectroscopy of the chromospheric Ca II 8542 Å and photospheric Fe I 8688 Å lines to improve separation of ARs and EN. We find that correlation plots between Ca line-center and ± 0.45 Å line-wing intensities show two identifiable but overlapping distributions. The first includes ARs (bright and faint) and the second includes ENs, network, and moat (``quiet Sun''). Active and Quiet distributions overlap in areas of EN and faint AR, so that feature identification using thresholds is unreliable. The statistical methodology of our previous work, however, is particularly well suited for distinguishing features with such partially overlapping distributions. Additionally, we find features in the Ca line which are not visible in the Fe observations, including a dark moat around an AR and narrow dark points associated with network and strong line-of-sight flows. Title: Solar Irradiance Variations Related to Intensity and Magnetic Flux of Solar Features Authors: Pap, Judit M.; Jones, H.; Parker, D.; Chapman, G.; Floyd, L. Bibcode: 2010cosp...38.1783P Altcode: 2010cosp.meet.1783P Solar total and spectral irradiance have been measured since late 1978. These measurements have demonstrated that solar irradiance changes from minutes to the 11-year solar cycle. Con-sidering the astrophysical and climate importance of irradiance variations, considerable efforts have been put forward to develop irradiance models to explain the origin of irradiance varia-tions and have information for those time intervals when measurements don't exist. However, most of the current models are simple empirical models, using the Photometric Sunspot Index to describe the darkening effect of sunspots and either the CaK index or the Mg II h k core-to wing ratio to describe the facular excess flux. While these models can explain reasonably well the short-term variations, long-term variations over years to the cycle are not well-accounted. Since the SOHO era we have combined the MDI intensity images and magnetograms to ac-count for the effect and the role of active region evolution to irradiance variations. Similar studies have been done routinely at the San Fernando Observatory, California State University. More recently we have used the SPM data from NSO Kitt Peak to deduct various activity components, and new efforts at UCLA are in progress to develop a sophisticated method to identify various features. Using observations by SDO/HMI we will have further insight into active region evolution, especially during the rising portion of cycle 24, following the long and deep minimum of cycle 23. In this paper we compare data derived from various images and compare them to irradiance variations. One of the main goals is to identify weak magnetic fields and estimate their contribution to irradiance changes. We will study cycle 23 in detail, and will discuss how the used methods and techniques can be applied to HMI on SDO. Title: Comparison of Independent Feature Recognition Method for Time Series Analysis of Irradiance Variations Based on Statistical Feature Recognition Authors: Pap, Judit M.; Bertello, L.; Chapman, G.; Floyd, L. E.; Jones, H.; Malanushenko, E.; Preminger, D.; Turmon, M. Bibcode: 2009SPD....41.0934P Altcode: Solar total and UV irradiances have been observed over three decades, and recently spectral irradiance data are available from the Solar Irradiance Monitor (SIM) on the SORCE Mission. Results of these measurements show that irradiance varies on various time scales from minutes to decades. To better understand the origin of irradiance changes, we need to use spatially resolved data rather than full disk indices. For this purpose various automated image processing and analyses techniques have been developed. Using these image processing techniques, we separated quiet-sun, network, faculae and sunspots. On one hand, we compare the area data of these features derived from various images to validate results and discuss future efforts needed to coordinate efforts between various groups working on image analysis. Another goal is to compare the variations of the identified features with total solar and UV irradiances to establish to what degree

the identified images explain short and long-term irradiance variations. Title: Experimental and Theoretical Characterization of the ANDE Wind and Temperature Spectrometer (WATS) Authors: Fenn, D.; Syrstad, E. A.; Dyer, J. S.; Vancil, B.; Roman, P.; Jones, H.; Herrero, F.; Finne, T. T.; Nicholas, A. C. Bibcode: 2009AGUFMSA23A1463F Altcode: The Wind and Temperature Spectrometer (WATS), developed at NASA-GSFC and NRL, is currently flying aboard the Atmospheric Neutral Density Experiment (ANDE). The primary mission objective of ANDE is validation and improvement of spacecraft drag and thermospheric models by measurement of the total atmospheric density. Drag determination also requires accurate measurements of neutral wind, temperature, and composition (O/N2 ratio). WATS provides the unprecedented capability to simultaneously measure all of these parameters in situ, by analyzing the angular and energy distribution of the gas stream passing its entrance aperture. WATS imposes very low power and size requirements on the host spacecraft, and is suitable for integration with small satellite platforms such as CubeSat. After passing through a pair of mutually-perpendicular collimating slits, neutrals are ionized by electron impact and energy analyzed by a crossed Small Deflection Energy Analyzer (SDEA) pair. The angular distribution of ions exiting the SDEA pair is measured by a microchannel plate (MCP) detector with linear spatial readout. The peak of this distribution indicates the neutral stream velocity vector in spectrometer coordinates, while the energy distribution yields the magnitude of this vector. Specification of the full neutral wind follows from knowledge of the satellite pointing angle. The width and shape of the angular distribution allows determination of the neutral temperature. Additionally, the high satellite velocity allows mass separation of the major thermospheric constituents by energy analysis. For example, at 7500 m/s, O and N2 have kinetic energies of 4.7 and 8.2 eV, respectively, and are readily resolved by the SDEA. This paper describes theoretical and experimental efforts aimed to characterize WATS performance, validate instrument and component functionality, augment sensor calibration, and improve data analysis. Much of this work has involved ion trajectory simulations (SIMION 3D) to characterize the operational parameters and performance of the crossed SDEA pair. Due to the intersecting SDEA volume and resulting potential field perturbations, energy analysis of low-angle ions traveling near the instrument axis requires greater voltages than predicted for a single SDEA. Additionally, the SDEA configuration in WATS includes an open drift region between the ion source aperture and analyzer entrance, which promotes ion beam divergence and yields less-than-ideal energy resolution. We present a promising deflection lens design predicted to collimate incident ion beams and significantly improve energy resolution. Also presented is experimental performance data for a novel low-power thermionic cathode (BaO-coated tungsten wire) that acts as the source of ionizing electrons in WATS. Additionally, ongoing laboratory experiments aim to characterize angle-dependent SDEA performance testing using a monoenergetic ion beam. Title: GAMA: towards a physical understanding of galaxy formation Authors: Driver, Simon P.; Norberg, Peder; Baldry, Ivan K.; Bamford, Steven P.; Hopkins, Andrew M.; Liske, Jochen; Loveday, Jon; Peacock, John A.; Hill, D. T.; Kelvin, L. S.; Robotham, A. S. G.; Cross, N. J. G.; Parkinson, H. R.; Prescott, M.; Conselice, C. J.; Dunne, L.; Brough, S.; Jones, H.; Sharp, R. G.; van Kampen, E.; Oliver, S.; Roseboom, I. G.; Bland-Hawthorn, J.; Croom, S. M.; Ellis, S.; Cameron, E.; Cole, S.; Frenk, C. S.; Couch, W. J.; Graham, A. W.; Proctor, R.; De Propris, R.; Doyle, I. F.; Edmondson, E. M.; Nichol, R. C.; Thomas, D.; Eales, S. A.; Jarvis, M. J.; Kuijken, K.; Lahav, O.; Madore, B. F.; Seibert, M.; Meyer, M. J.; Staveley-Smith, L.; Phillipps, S.; Popescu, C. C.; Sansom, A. E.; Sutherland, W. J.; Tuffs, R. J.; Warren, S. J. Bibcode: 2009A&G....50e..12D Altcode: 2009arXiv0910.5123D Simon P Driver, Peder Norberg, Ivan K Baldry, Steven P Bamford, Andrew M Hopkins, Jochen Liske, Jon Loveday, John A Peacock and the GAMA Survey Team (Galaxy and Mass Assembly) review progress on the latest large galaxy redshift survey now underway on the 3.9 m Anglo-Australian Telescope. Title: Training Sets for Statistical Feature Recognition in Multidimensional Solar Imagery Authors: Jones, Harrison P.; Turmon, M. J.; Malanushenko, O. V.; Pap, J. M. Bibcode: 2009SPD....40.1518J Altcode: We have previously reported the multi-dimensional extension of a statistical maximum likelihood algorithm for segmenting images into different feature classes developed by Turmon, Pap, and Mukhtar (2002, ApJ 568, p. 396). The method works best for features which have overlapping but nonetheless distinct distributions of observed variables. Developing these empirical class-conditional distributions from independently classified training sets depends sensitively on the match of spatial scales between the training segmentations and the desired feature classes. We discuss recent progress in extracting well-posed class distributions even when the training segmentations are mixtures of the classes which we wish to identify. For example, in addition to large-scale labelings, Harvey and White (1999, ApJ 515, p. 812) provide finely grained information which we use to help isolate areas of pure quiet Sun. Quiet Sun distributions of observed quantities can then be separated from distributions derived from areas labeled as network which also include quiet Sun. Similarly, these distributions can then be isolated from those mixed with active regions and/or sunspots. This research is funded by a NASA Supporting Research and Technology grant. Title: Galaxy And Mass Assembly (GAMA) Authors: Driver, Simon P.; GAMA Team; Baldry, I. K.; Bamford, S.; Bland-Hawthorn, J.; Bridges, T.; Cameron, E.; Conselice, C.; Couch, W. J.; Croom, S.; Cross, N. J. G.; Driver, S. P.; Dunne, L.; Eales, S.; Edmondson, E.; Ellis, S. C.; Frenk, C. S.; Graham, A. W.; Jones, H.; Hill, D.; Hopkins, A.; van Kampen, E.; Kuijken, K.; Lahav, O.; Liske, J.; Loveday, J.; Nichol, B.; Norberg, P.; Oliver, S.; Parkinson, H.; Peacock, J. A.; Phillipps, S.; Popescu, C. C.; Prescott, M.; Proctor, R.; Sharp, R.; Staveley-Smith, L.; Sutherland, W.; Tuffs, R. J.; Warren, S. Bibcode: 2009IAUS..254..469D Altcode: 2008arXiv0807.0376D The GAMA survey aims to deliver 250,000 optical spectra (3-7 Å resolution) over 250 sq. degrees to spectroscopic limits of rAB < 19.8 and KAB < 17.0 mag. Complementary imaging will be provided by GALEX, VST, UKIRT, VISTA, HERSCHEL and ASKAP to comparable flux levels leading to a definitive multi-wavelength galaxy database. The data will be used to study all aspects of cosmic structures on 1kpc to 1Mpc scales spanning all environments and out to a redshift limit of z ≈ 0.4. Key science drivers include the measurement of: the halo mass function via group velocity dispersions; the stellar, HI, and baryonic mass functions; galaxy component mass-size relations; the recent merger and star-formation rates by mass, types and environment. Detailed modeling of the spectra, broad SEDs, and spatial distributions should provide individual star formation histories, ages, bulge-disc decompositions and stellar bulge, stellar disc, dust disc, neutral HI gas and total dynamical masses for a significant subset of the sample (~ 100k) spanning both the giant and dwarf galaxy populations. The survey commenced March 2008 with 50k spectra obtained in 21 clear nights using the Anglo Australian Observatory's new multi-fibre-fed bench-mounted dual-beam spectroscopic system (AAΩ). Title: Darwin-A Mission to Detect and Search for Life on Extrasolar Planets Authors: Cockell, C. S.; Léger, A.; Fridlund, M.; Herbst, T. M.; Kaltenegger, L.; Absil, O.; Beichman, C.; Benz, W.; Blanc, M.; Brack, A.; Chelli, A.; Colangeli, L.; Cottin, H.; Coudé du Foresto, V.; Danchi, W. C.; Defrère, D.; den Herder, J. -W.; Eiroa, C.; Greaves, J.; Henning, T.; Johnston, K. J.; Jones, H.; Labadie, L.; Lammer, H.; Launhardt, R.; Lawson, P.; Lay, O. P.; LeDuigou, J. -M.; Liseau, R.; Malbet, F.; Martin, S. R.; Mawet, D.; Mourard, D.; Moutou, C.; Mugnier, L. M.; Ollivier, M.; Paresce, F.; Quirrenbach, A.; Rabbia, Y. D.; Raven, J. A.; Rottgering, H. J. A.; Rouan, D.; Santos, N. C.; Selsis, F.; Serabyn, E.; Shibai, H.; Tamura, M.; Thiébaut, E.; Westall, F.; White, G. J. Bibcode: 2009AsBio...9....1C Altcode: 2008arXiv0805.1873C The discovery of extrasolar planets is one of the greatest achievements of modern astronomy. The detection of planets that vary widely in mass demonstrates that extrasolar planets of low mass exist. In this paper, we describe a mission, called Darwin, whose primary goal is the search for, and characterization of, terrestrial extrasolar planets and the search for life. Accomplishing the mission objectives will require collaborative science across disciplines, including astrophysics, planetary sciences, chemistry, and microbiology. Darwin is designed to detect rocky planets similar to Earth and perform spectroscopic analysis at mid-infrared wavelengths (6-20 μm), where an advantageous contrast ratio between star and planet occurs. The baseline mission is projected to last 5 years and consists of approximately 200 individual target stars. Among these, 25-50 planetary systems can be studied spectroscopically, which will include the search for gases such as CO2, H2O, CH4, and O3. Many of the key technologies required for the construction of Darwin have already been demonstrated, and the remainder are estimated to be mature in the near future. Darwin is a mission that will ignite intense interest in both the research community and the wider public. Title: The application of Gaussian Mixture and Histogram-based Bayesian methods to NSO/Kitt Peak VT data. Authors: Malanushenko, O.; Jones, H. P.; Turmon, M.; Pap, J. Bibcode: 2008AGUFMSH13A1519M Altcode: We applied Gaussian Mixture and Histogram-based Bayesian methods to recognize several solar features using Kitt Peak Vacuum Telescope (VT) observations from 1992-2003. We used 5D observations in the 868.8 nm line including LoS magnetic field, continuum intensity, radial velocity, line depth, and EqW. We applied the analysis for recognition of active regions, magnetic network, and sunspots, for the purpose of automatic recognition of solar activity, and linking solar activity to irradiance changes. The success of such a feature recognition process strongly depends on separation and sensitivity of observable and derivative parameters for different features. For some features it works very well for two kind of data, but in some other cases the probability of correct recognition of a feature is low without the adding complementary data. We discuss the advantages and limitations of these statistical methods, review the importance and possibility of using the complementary data, and compare our results with other methods which derive feature areas. This methodological review will help to create the strategy for new SDO/HMI analysis. Title: Spectral Irradiance Variations and Magnetic Field Changes During Solar Cycle 23. Authors: Pap, J. M.; Bertello, L.; Chapman, G.; Floyd, L. E.; Harder, J.; Jones, H.; Malanuskenko, O.; Preminger, D.; Turmon, M. Bibcode: 2008AGUFMSH13A1504P Altcode: Both total irradiance and the Mg core-to-wing ratio was high at the maximum of weak solar cycle 23. However, photometric observations from the San Fernando Observatory show that both the number and size of active regions (spots and faculae) were low at the maximum of solar cycle 23 which points to the importance of the role of weak magnetic fields in irradiance variations. The purpose of this paper is to use new SOLIS spectromagnetograph observations in conjunction with a newly developed image analysis technique to compare irradiance time series as function of wavelengths with various surface magnetic features. One major goal is to compare features derived from the SOLIS images using the new technique with well-established features from SFO. Another important goal is to determine the contribution of active regions/weak fields to irradiance variations at various wavelengths, using the SOHO/VIRGO and SORCE/SIM data. A third goal is to determine the extent of irradiance variations not explained by magnetic structures. To do this, we use a new analysis technique to evaluate SOLIS spectromagnetograph observations. Title: Using SPICA Space Telescope to characterize Exoplanets Authors: Goicoechea, J. R.; Swinyard, B.; Tinetti, G.; Nakagawa, T.; Enya, K.; Tamura, M.; Ferlet, M.; Isaak, K. G.; Wyatt, M.; Aylward, A. D.; Barlow, M.; Beaulieu, J. P.; Boccaletti, A.; Cernicharo, J.; Cho, J.; Claudi, R.; Jones, H.; Lammer, H.; Leger, A.; Martín-Pintado, J.; Miller, S.; Najarro, F.; Pinfield, D.; Schneider, J.; Selsis, F.; Stam, D. M.; Tennyson, J.; Viti, S.; White, G. Bibcode: 2008arXiv0809.0242G Altcode: We present the 3.5m SPICA space telescope, a proposed Japanese-led JAXA-ESA mission scheduled for launch around 2017. The actively cooled (<5 K), single aperture telescope and monolithic mirror will operate from ~3.5 to ~210 um and will provide superb sensitivity in the mid- and far-IR spectral domain (better than JWST at lambda > 18 um). SPICA is one of the few space missions selected to go to the next stage of ESA's Cosmic Vision 2015-2025 selection process. In this White Paper we present the main specifications of the three instruments currently baselined for SPICA: a mid-infrared (MIR) coronagraph (~3.5 to ~27 um) with photometric and spectral capabilities (R~200), a MIR wide-field camera and high resolution spectrometer (R~30,000), and a far-infrared (FIR ~30 to ~210 um) imaging spectrometer - SAFARI - led by a European consortium. We discuss their capabilities in the context of MIR direct observations of exo-planets (EPs) and multiband photometry/high resolution spectroscopy observations of transiting exo-planets. We conclude that SPICA will be able to characterize the atmospheres of transiting exo-planets down to the super-Earth size previously detected by ground- or space-based observatories. It will also directly detect and characterize Jupiter/Neptune-size planets orbiting at larger separation from their parent star (>5-10 AU), by performing quantitative atmospheric spectroscopy and studying proto-planetary and debris disks. In addition, SPICA will be a scientific and technological precursor for future, more ambitious, IR space missions for exo-planet direct detection as it will, for example, quantify the prevalence exo-zodiacal clouds in planetary systems and test coronographic techniques, cryogenic systems and lightweight, high quality telescopes. (abridged) Title: Feature Classification of NSO/Kitt Peak Magnetograms Authors: Malanushenko, O.; Jones, H. P.; Pap, J. M.; Turmon, M. Bibcode: 2008AGUSMSP31B..04M Altcode: We present new segmentations of daily NASA/NSO Spectromagnetograph (SPM) multidimensional magnetograms obtained at the NSO/Kitt Peak Vacuum Telescope from 1992-2003. Full-disk images are divided into areas of quiet Sun, network, active regions, and sunspots using a three-dimensional adaptation of a statistical image classification method developed by Turmon, Pap, and Mukhtar (ApJ 568:396-407, 2002). Probability distributions for each feature class are derived from a training set of images independently segmented using thresholds in magnetic flux and continuum intensity. We summarize our analysis procedures and compare segmentations derived from class-conditional probabilities computed with Gaussian mixture models and histogram interpolation. We also compare our segmentations with features identified by other methods and with solar irradiance variation. Title: A Comparison of Feature Classification Methods for Modeling Solar Irradiance Variation Authors: Jones, H. P.; Chapman, G. A.; Harvey, K. L.; Pap, J. M.; Preminger, D. G.; Turmon, M. J.; Walton, S. R. Bibcode: 2008SoPh..248..323J Altcode: Physical understanding of total and spectral solar irradiance variation depends upon establishing a connection between the temporal variability of spatially resolved solar structures and spacecraft observations of irradiance. One difficulty in comparing models derived from different data sets is that the many ways for identifying solar features such as faculae, sunspots, quiet Sun, and various types of "network" are not necessarily consistent. To learn more about classification differences and how they affect irradiance models, feature "masks" are compared as derived from five current methods: multidimensional histogram analysis of NASA/National Solar Observatory/Kitt Peak spectromagnetograph data, statistical pattern recognition applied to SOHO/Michelson Doppler Imager photograms and magnetograms, threshold masks allowing for influence of spatial surroundings applied to NSO magnetograms, and "one-trigger" and "three-trigger" algorithms applied to California State University at Northridge Cartesian Full Disk Telescope intensity observations. In general all of the methods point to the same areas of the Sun for labeling sunspots and active-region faculae, and available time series of area measurements from the methods correlate well with each other and with solar irradiance. However, some methods include larger label sets, and there are important differences in detail, with measurements of sunspot area differing by as much as a factor of two. The methods differ substantially regarding inclusion of fine spatial scale in the feature definitions. The implications of these differences for modeling solar irradiance variation are discussed. Title: The Southern 2MASS Red AGN Survey: Spectroscopic Observations with 6dF Authors: Masci, Franco; Cutri, R.; Francis, P.; Nelson, B.; Huchra, J.; Jones, H.; Colless, M.; Saunders, W. Bibcode: 2008AAS...21115709M Altcode: Following the success of The Two Micron All-Sky Survey (2MASS) in revealing large numbers of new optically red AGN and QSOs, we report on an extension of this search in the Southern equatorial sky using the Six Degree Field (6dF) multifibre spectrograph. Near-IR selected samples are more sensitive to objects whose optical emission may be reddened by dust, or is intrinsically weak. Our sample of red AGN candidates was selected using a single color cut of J-Ks > 2 mag and a galactic latitude |b| > 30 deg. For comparison, most optical/UV-selected QSOs and (quiescent) galaxies at redshifts z< 0.4 have colors of J-Ks < 2 mag. A subsample of 6386 candidates with Bj < 19 and rF < 18 were selected as auxiliary targets for the 6dF Galaxy Redshift Survey. Spectra were obtained for 1182 objects. Approximately 700 are of sufficient quality to enable a reliable identification. We present the results of the classification of the 6dF spectra, making use of Bj, R (SuperCOSMOS) and J, H, Ks (2MASS) images to assist in the identification process. We quantify the AGN content, types, host morphologies (i.e., whether point-like or extended), and compare their properties to those of AGN discovered at other wavelengths. Title: Physical and orbital properties of the Trojan asteroids Authors: Melita, M. D.; Licandro, J.; Jones; C., D.; Williams, I. P. Bibcode: 2008arXiv0801.2497M Altcode: All the Trojan asteroids orbit about the Sun at roughly the same heliocentric distance as Jupiter. Differences in the observed visible reflection spectra range from neutral to red, with no ultra-red objects found so far. Given that the Trojan asteroids are collisionally evolved, a certain degree of variability is expected. Additionally, cosmic radiation and sublimation are important factors in modifying icy surfaces even at those large heliocentric distances. We search for correlations between physical and dynamical properties, we explore relationships between the following four quantities; the normalised visible reflectivity indexes ($S'$), the absolute magnitudes, the observed albedos and the orbital stability of the Trojans. We present here visible spectroscopic spectra of 25 Trojans. This new data increase by a factor of about 5 the size of the sample of visible spectra of Jupiter Trojans on unstable orbits. The observations were carried out at the ESO-NTT telescope (3.5m) at La Silla, Chile, the ING-WHT (4.2m) and NOT (2.5m) at Roque de los Muchachos observatory, La Palma, Spain. We have found a correlation between the size distribution and the orbital stability. The absolute-magnitude distribution of the Trojans in stable orbits is found to be bimodal, while the one of the unstable orbits is unimodal, with a slope similar to that of the small stable Trojans. This supports the hypothesis that the unstable objects are mainly byproducts of physical collisions. The values of $S'$ of both the stable and the unstable Trojans are uniformly distributed over a wide range, from $0 %/1000Å$ to about $15 %/1000Å$. The values for the stable Trojans tend to be slightly redder than the unstable ones, but no significant statistical difference is found. Title: The PRVS Pathfinder Authors: Ramsey, Lawrence W.; Redman, S.; Wolszczan, A.; Jones, H.; Barnes, J. Bibcode: 2007AAS...211.1118R Altcode: 2007BAAS...39..747R The Precision Radial Velocity Spectrometer (PRVS) is a fiber coupled near infrared (NIR) spectrometer being designed for the Gemini International Observatory specifically to search for planets around M stars. These stars emit most of their flux at wavelengths between 1 and 2 microns. These low mass stars are the most likely place where PRV techniques will allow detection of earth mass planets in the so called "Habitable Zone". The pathfinder instrument has become a significant tool in mitigating design, performance and cost risks for the PRVS. Last year we demonstrated the ability to detect radial velocity variations at the 10-15 meter/sec level. Since then, we have made significant progress in our understanding of the limitations of the PRVS in the NIR. In particular, we present the latest improvements we have made to the calibration spectra, as well as the characterization and suppression of the modal noise in the optical fibers. Title: Application of Statistical Image Segmentation to Recognition of Solar Magnetic Network Authors: Jones, H. P.; Malanushenko, O. V.; Pap, J. M.; Turmon, M. J. Bibcode: 2007AGUFMSH13A1096J Altcode: We have developed a statistical method for feature identification in NSO multidimensional imagery which requires a training set of independently determined image segmentations. The large spatial scale of our initial training set determined by the algorithm of Harvey and White (1999, ApJ 515, p. 812) mixes the details of magnetic network which are contained in the observations with quiet Sun and other features. We have found it difficult to reproduce this large scale in models of conditional and prior probabilities and are in fact interested in marking smaller scale structures for comparison with variation of total and spectral solar irradiance. We describe in this paper the performance of our technique with finer scale training sets determined by observations from other instruments and independently for the NSO data. Title: 2MTF - The 2MASS Tully-Fisher Survey Authors: Masters, Karen L.; Huchra, J. P.; Crook, A. C.; Macri, L. M.; Jarrett, T.; Koribalski, B.; Staveley-Smith, L.; Jones, H.; Springob, C. M. Bibcode: 2007AAS...210.8403M Altcode: 2007BAAS...39..193M The 2MASS Tully-Fisher survey (2MTF) is making use of existing high quality rotations widths, new HI widths and 2MASS photometry to measure Tully-Fisher (TF) distances/peculiar velocities for all bright inclined spirals in the 2MASS redshift survey (2MRS). 2MRS has already provided the best nearby galaxy density field, so we know where the baryons are. The local universe is the only place where peculiar velocity measurements are sufficiently accurate to compare this with the distribution of mass. In the linear regime peculiar velocities are directly proportional to the underlying gravity. Previous peculiar velocity surveys have struggled to meet their potential because of large errors on individual measurements, poor statistics and uneven sky coverage. A survey based on 2MRS will provide significantly more uniform sky coverage than has previously been available, providing a qualitatively better sample for velocity--density field reconstructions. Better coverage in the ZoA will also aid in studies of the "Great Attractor'' region. We provide a progress report on the 2MTF survey including a first look at over 300 hours of HI observations at GBT, a report on ongoing southern hemisphere observations with the Parkes Radio Telescope and a preview of a universal 2MASS Tully-Fisher relation. KLM is supported by NSF grant AST-0406906. Title: Statistical Feature Recognition for Multidimensional NSO Imagery Authors: Malanushenko, Elena; Jones, H. P.; Pap, J. M.; Turmon, M. J. Bibcode: 2007AAS...210.2406M Altcode: 2007BAAS...39..129M Turmon, Pap, and Mukhtar (2002: Astrophysical Journal 568, 396) present a statistical method for identifying sunspots, faculae, and quiet Sun region classes in co-registered SOHO/MDI magnetograms and intensity images. This paper describes progress toward an extension of this method for finding a more complete region classification using multidimensional images (magnetic flux, line-of-sight velocity, intensity, equivalent width, and central line depth) obtained from 1992-2003 with the NASA/NSO Spectromagnetograph (SPM) and since 2003 with the NSO/SOLIS Vector Spectromagnetograph (VSM). We discuss the selection of the feature set, training images, and the temporal and spatial consistency of the NSO data. We determine class-conditional probability densities using both Gaussian mixture models and direct histogram interpolation, and compare feature labelings driven by both methods. Title: Bayesian Feature Recognition for Multidimensional NSO Imagery Authors: Jones, H. P.; Pap, J. M.; Turmon, M. J. Bibcode: 2006AGUFMSH23B0372J Altcode: Turmon, Pap, and Mukhtar (2002: Astrophysical Journal 568, 396) present a statistical method for identifying sunspots, faculae, and quiet Sun in SOHO/MDI magnetograms and intensity images. This paper describes progress toward an extension of this method for identifying more complete feature sets using the multidimensional images (magnetic flux, line-of-sight velocity, intensity, equivalent width, and central line depth) obtained from 1992-2003 with the NASA/NSO Spectromagnetograph (SPM) and since 2003 with the NSO/SOLIS Vector Spectromagnetograph (VSM). We discuss the selection of the feature set and training images, and the temporal and spatial consistency of the NSO data. We determine the class-conditional (Bayesian prior) probability densities using both Gaussian mixture models and direct histogram interpolation, and show projections of the multidimensional probability densities derived from SPM observations. Finally, we compare various feature identification methods driven by these two types of prior. Title: High Spectral Resolution Study of the He 10830 Spectral Region Authors: Malanushenko, O.; Livingston, W.; Jones, H.; Malanushenko, V. P. Bibcode: 2005ASPC..346..389M Altcode: The He 1083 nm line, formed in the upper chromosphere, is used for observations of coronal holes (CHs) near their origins at the solar surface. The weak He profiles in CHs show some peculiarities such as asymmetry, broadening, and different ratios between spectral components. These effects are small and the influence of disturbing noise and approximations in reductions may be crucial for their definition. In the present work we used low noise and high spectral resolution observations carried out at the Kitt Peak McMath-Pierce telescope to establish the key characteristics of He profile. The shape of He profile is affected by telluric water line and we suggest a method for its correction. Also there are solar lines that lie between the main and second He components and overlap with both. If the He line is weak and blue shifted, as in a CH and in cell centers, the blends distort the visual shape of the main component and obscure the second component. As an example we analyze two integral spectra of CH and quiet Sun and confirm the broadening and minor blue shift of the He line in a CH. This result must be considered to be preliminary and the work is in progress. Title: Magnetic Fields and Flows in Open Magnetic Structures Authors: Jones, H. P. Bibcode: 2005ASPC..346..229J Altcode: Open magnetic structures connect the solar surface to the heliosphere and are thus of great interest in solar-terrestrial physics. This paper is a selective observational review of what is known about magnetic fields and outward flows in such regions with special focus on coronal holes and origins of the fast solar wind. First evidence of the connection between these two features was seen in Skylab data after the discovery of coronal holes whose solar roots are now known to be in unipolar photospheric regions. Subsequently many observations of have been made, ranging from oscillations in the underlying photosphere and chromosphere, to possible beginnings of the solar wind as observed by Doppler shifts in high chromospheric and transition-region lines, to coronagraphic time-lapse studies of outward-moving material which perhaps trace elements of solar-wind plasma. Some of the many unresolved and controversial issues regarding details of these observations and their association with the solar wind will be discussed. Title: New high eccentricity planets from the AAT Authors: Jones, H.; Anglo-Australian Planet Search Team Bibcode: 2005DPS....37.2801J Altcode: 2005BAAS...37..671J The Anglo-Australian Planet Search is a long-term programme being carried out on the Anglo-Australian Telescope to search for giant planets around nearby Solar type stars. We began observing in January 1998 observing 200 target stars over 20 nights per year, and have very recently grown to more than 60 nights per year targetting an expanded sample. Twenty planet candidates with M sin i values ranging from 0.2 to 10 Mjup have been found from the programme, four planet candidates have been confirmed using our data and several found by other programmes disputed. Our precision Doppler velocity measurements are made with the an echelle spectrograph with an iodine absorption cell. The iodine cell enables us to achieve measured long-term velocity stability of 2 m/s (for suitably stable stars) down to our survey magnitude limit. This stability will be discussed in the context of our latest results which include the discovery of two highly elliptical planets.

We acknowledge support for this programme by the partners of the Anglo-Australian Telescope agreement as well as from NSF and NASA. Title: The 6dF Galaxy Survey: First Data Release Authors: Jones, H.; Saunders, W.; Colless, M.; Read, M.; Parker, Q.; Watson, F.; Campbell, L. Bibcode: 2005ASPC..329...11J Altcode: The 6dF Galaxy Survey (6dFGS) is currently measuring the redshifts of around 170 000 galaxies and the peculiar velocities of a 15 000-member sub-sample. It will be the largest redshift survey of the local universe and more than an order of magnitude larger than any peculiar velocity survey to date. When complete, it will cover essentially the entire southern sky around a mean redshift of z = 0.05. Central to the survey is the Six-Degree Field (6dF) multi-fibre spectrograph, an instrument able to record 150 simultaneous spectra over the 5.7°-field of the UK Schmidt Telescope. Targets have been drawn from the 2MASS Extended Source Catalog (XSC) to include all galaxies brighter than Ktot = 12.75, supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J, rF, bJ) = (13.05, 13.75, 15.6, 16.75). Here we describe the implementation of the survey and the procedures used to select sources and determine redshifts. We also describe early results utilising the First Data Release of ∼ 45 000 redshifts. There is an online database of 6dFGS data accessible from the 6dFGS web site (http://www.mso.anu.edu.au/6dFGS). Title: Reduction of SOLIS/Vector Spectromagnetograph He I 1083 nm Observations Authors: Jones, H. P.; Malanushenko, O. V.; Harvey, J. W.; Henney, C. J.; Keller, C. U. Bibcode: 2005AGUSMSP51A..02J Altcode: The SOLIS/Vector Spectromagnetograph (VSM) now continues the three-decade record of full-disk He I 1083 nm spectroheliograms from NSO/Kitt Peak (see poster by Henney et al.). Although the sensitivity of the VSM interim cameras at 1083 nm is far greater than that of previous NSO/KP instruments, the observations are compromised by strong interference fringes produced within the detectors. We discuss in some detail the extent to which this difficulty is overcome in the simple algorithm used to produce the synoptic observations and explore methods for removing remaining fringe effects for true imaging spectroscopy. These techniques include Fourier and Wavelet filtering, the flat-fielding algorithm used for earlier NASA/NSO Spectromagnetograph (SPM) observations, and physical modeling of the detector fringe pattern. Title: The He I 1083 nm line in Coronal Holes, a study with high spectral resolution. Authors: Malanushenko, O.; Jones, H. P.; Livingston, W.; Malanushenko, V. P. Bibcode: 2005AGUSMSP51B..08M Altcode: The He 1083 nm line (He), formed in the upper chromosphere, is used for observations of coronal holes (CH) near their origins at the solar surface. Weak He 1083 nm profiles in CHs show some peculiarities such as asymmetry, broadening, and a different ratio between the spectral components. These effects are small so that the influence of disturbing noise and approximations in reduction processes are important for the results. In this research we have used low noise and high spectral resolution observations carried out at the Kitt Peak McMath-Pierce telescope to establish the key characteristics of the He profile in CHs. For accurate reduction we corrected the He profile for spectral blending from water vapor and weak solar lines. We confirm our previous result, based on imaging-spectroscopy data from the Kitt Peak Vacuum Telescope, regarding broadening of the He line in CHs and explain previous instability of CH contrast in our procedure for CH recognition as an influence of hidden photospheric lines. Title: Differentiating Coronal Holes from the Quiet Sun by He 1083 nm Imaging Spectroscopy Authors: Malanushenko, O. V.; Jones, H. P. Bibcode: 2005SoPh..226....3M Altcode: The locations of coronal holes are usually based on equivalent-width images in the He I 1083 nm line. However, it is difficult to differentiate coronal holes from the centers of quiet chromospheric network without complementary data and the skill of an experienced observer. Analysis of imaging spectroscopy shows that line half-width and central intensity are correlated differently in coronal holes and a quiet Sun. This fact can be used to form linear combinations of these images in which coronal holes are better separated from the quiet Sun. Coronal hole borders agree well with SOHO/EIT data but can show significant differences from National Solar Observatory maps. Title: The 6dF Galaxy Survey: Mass and Motions in the Local Universe Authors: Colless, M.; Jones, H.; Campbell, L.; Burkey, D.; Taylor, A.; Saunders, W. Bibcode: 2005IAUS..216..180C Altcode: 2003IAUS..216E..28C The 6dF Galaxy Survey will provide 167000 redshifts and about 15000 peculiar velocities for galaxies over most of the southern sky out to about cz = 30000 km/s. The survey is currently almost half complete, with the final observations due in mid-2005. An initial data release was made public in December 2002; the first third of the dataset will be released at the end of 2003, with the remaining thirds being released at the end of 2004 and 2005. The status of the survey, the survey database and other relevant information can be obtained from the 6dFGS web site at http://www.mso.anu.edu.au/6dFGS.

In terms of constraining cosmological parameters, combining the 6dFGS redshift and peculiar velocity surveys will allow us to: (1) break the degeneracy between the redshift-space distortion parameter beta = Omega_m0.6b/b and the galaxy-mass correlation parameter rg; (2) measure the four parameters Ag, Gamma, beta and rg with precisions of between 1% and 3%; (3) measure the variation of rg and b with scale to within a few percent over a wide range of scales. Title: Helicity and the SOLIS Vector-Spectromagnetograph Authors: Keller, Christoph U.; Harvey, John W.; Henney, Carl. J.; Jones, Harrison P. Bibcode: 2005HiA....13..126K Altcode: SOLIS (Synoptic Optical Long-term Investigations of the Sun) is a suite of three innovative instruments that greatly improve ground-based synoptic solar observations. The main instrument the Vector Spectro-Magnetograph (VSM) is a compact high-throughput vector-polarimeter that measures the magnetic field strength and direction over the full solar disk within 15 minutes. Helicity can be directly calculated from the full-disk vector field data provided by the Stokes inversion of the observed polarized line profiles. We present an anlysis of the difficulties and problems that one faces when interpreting the the helicity derived from VSM data. Title: Analysis of He I 1083 nm Imaging Spectroscopy Using a Spectral Standard Authors: Malanushenko, O. V.; Jones, H. P. Bibcode: 2004SoPh..222...43M Altcode: We develop a technique for the analysis of He i 1083 nm spectra which addresses several difficulties through determination of a continuum background by comparison with a well-calibrated standard and through removal of nearby solar and telluric blends by differential comparison to an average spectrum. The method is compared with earlier analysis of imaging spectroscopy obtained at the National Solar Observatory/Kitt Peak Vacuum Telescope (NSO/KPVT) with the NASA/NSO Spectromagnetograph (SPM). We examine distributions of Doppler velocity and line width as a function of central intensity for an active region, filament, quiet Sun, and coronal hole. For our example, we find that line widths and central intensity are oppositely correlated in a coronal hole and quiet Sun. Line widths are comparable to the quiet Sun in the active region, are systematically lower in the filament, and extend to higher values in the coronal hole. Outward velocities of ≈ 2-4 km s−1 are typically observed in the coronal hole. The sensitivity of these results to analysis technique is discussed. Title: SOLIS-VSM Longitudinal Magnetogram Calibration Authors: Henney, C. J.; Harvey, J. W.; Keller, C. U.; Jones, H. P. Bibcode: 2004AAS...204.3702H Altcode: 2004BAAS...36..709H The VSM (Vector SpectroMagnetograph) instrument started recording daily full-disk magnetograms during August, 2003 at a temporary site in Tucson, Arizona. Along with the other instruments that constitute the SOLIS (Synoptic Optical Long-term Investigations of the Sun) project, the VSM will be relocated to Kitt Peak in April, 2004. The VSM instrument provides a unique record of solar full-disk vector magnetograms along with the high sensitivity photospheric and chromospheric longitudinal magnetograms. In addition, the VSM takes daily full-disk He I 1083 nm equivalent width observations. These parameter-grams are constructed from individual scans in declination of the projected solar image on the entrance slit with a relatively large field angle of over a half of a degree in the spectrograph. The calibration of the VSM longitudinal magnetic observations is reviewed, along with a comparison between the VSM mean field, sun-as-a-star, measurements with those by the Wilcox Solar Observatory. In addition, the making of synoptic maps derived from the VSM magnetograms is discussed, including the filling of data gaps in polar regions and the use of accompanying weight maps. VSM magnetograms and synoptic maps are available via the Internet at: http://solis.nso.edu/. This research was supported in part by the Office of Naval Research Grant N00014-91-J-1040. The National Solar Observatory is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. Title: Early Results from SOLIS Authors: Harvey, J.; Giampapa, M.; Henney, C.; Keller, C.; Jones, H. Bibcode: 2004AAS...204.3701H Altcode: 2004BAAS...36..708H SOLIS (Synoptic Optical Long-Term Investigations of the Sun) is a project that is replacing antiquated synoptic observing equipment at the National Solar Observatory. SOLIS consists of a suite of three instruments on an equatorial mount that will be installed on Kitt Peak in April 2004. The major SOLIS instrument is a vector spectromagnetograph (VSM) that maps magnetic fields across the full solar disk using a slit spectrograph and one arc sec pixels. Limited daily observations started at a temporary site in August, 2003 and include line-of-sight component magnetograms in the photosphere and chromosphere and, for the first time, full-disk vector magnetograms. At a medium scan speed ( ∼ 10 minutes for the full disk) noise is less than 1 Mx/cm2. This low noise, combined with negligible instrumental polarization and well resolved spectral line profiles, yields moderate resolution magnetograms of unprecedented quality. Observations show magnetic flux nearly everywhere in the photosphere from the disk center to the solar limb. Weak, intranetwork fields are now routinely observed and show a tendency to be of opposite polarity to the stronger surrounding fields. Diffuse fields surround decaying active regions and appear to be distinct from canopy fields. Vector magnetograms easily show the radial orientation of network fields, and the diffuse component surrounding decaying active regions. Near the disk center, the transverse magnetic fields of network elements change on a time scale of minutes. Detailed quantitative calibration of the observations is in progress. Good results have been obtained from the other SOLIS instruments: a full-disk filter imager at several narrow wavelengths and a double-pass grating spectrograph that provides high-accuracy line spectra of integrated sunlight. SOLIS data are freely available via the Internet and users are invited to submit observing time requests for special observations. The National Solar Observatory is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. Additional support for the development of SOLIS from NASA and ONR is gratefully acknowledged. Title: Differentiating Coronal Holes from the Quiet Sun by He 1083 nm imaging spectroscopy. Authors: Malanushenko, O. V.; Jones, H. P. Bibcode: 2004AAS...204.7105M Altcode: 2004BAAS...36R.797M We applied our new analysis technique to several examples of He I 1083 nm imaging spectroscopy obtained with the NASA/NSO Spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope. We studied correlations of intensity vs width and Doppler velocity in several coronal holes and areas of chromospheric network in the quiet Sun. We confirm our previous result, which was based on a single example, that the correlation of line width and central intensity is opposite in coronal holes and quiet Sun. Suitably normalized linear combinations of width and intensity can be used to distinguish between quiet Sun and coronal holes. Title: Measurement Scale of the SOLIS Vector Spectromagnetograph Authors: Jones, H. P.; Harvey, J. W.; Henney, C. J.; Keller, C. U.; Malanushenko, O. M. Bibcode: 2004AAS...204.3703J Altcode: 2004BAAS...36Q.709J Longitudinal magnetograms obtained with the SOLIS Vector Spectromagnetograph (VSM) during a cross-calibration period are compared with similar data from the NASA/NSO Spectromagnetograph (SPM) at the NSO/Kitt Peak Vacuum Telescope as well as with SOHO/MDI and GONG magnetograms. The VSM began observations at the University of Arizona agricultural test site and collaborative observations were obtained with both the VSM and SPM from 2003 Aug 05 through 2003 Sep 21 when the SPM was officially retired. The VSM replaces the SPM and continues the 30-year NSO/Kitt Peak synoptic magnetogram record. Magnetograms are compared by equating histograms and, for selected examples, by pixel-by-pixel comparison of coregistered images. The VSM was not corrected for polarization crosstalk and was operated without fast guiding. Solar activity was at best moderate during this period. Over the range of observed fields, the VSM magnetograms show greatly improved sensitivity but are otherwise virtually identical with "raw" SPM magnetograms. GONG magnetograms are also closely comparable with the SPM while MDI flux values tend to be stronger by a factor of 1.2 - 1.4. Dependence of the results on seeing will be discussed. Partial funding for this work was provided through Solar and Heliospheric Research Supporting Research and Technology grants from NASA's Office of Space Sciences. Title: DASL--Data and Activities for Solar Learning Authors: Hill, F.; Gearen, M.; Henney, C.; Jones, H.; Stagg, T. Bibcode: 2004AAS...204.7703H Altcode: 2004BAAS...36..808H Data and Activities for Solar Learning (DASL) provides a classroom learning environment based on a twenty-five year record of solar magnetograms from the National Solar Observatory (NSO) at Kitt Peak, AZ. The data, together with image processing software for Macs or PCs, can be used to learn basic facts about the Sun and astronomy at the middle school level. At the high school level, students can study properties of the Sun's magenetic cycle with classroom excercises emphasizing data and error analysis and can participate in a new scientific study, Research in Active Solar Longitudes (RASL), in collaboration with classrooms throughout the country and scientists at NSO and NASA. We will have available a compact disc with the data and software, and a web site for uploading the RASL results. Title: Imaging the Chromosphere using Photospheric Mn 539.4 nm Authors: Malanushenko, Olena; Jones, H. P.; Livingston, W. Bibcode: 2004IAUS..223..645M Altcode: 2005IAUS..223..645M Archival full disk observations of the central depth of Mn 539.467, a photospheric line, have been found to correlate with chromospheric Ca K intensity. In this paper we present spectroheliograms taken in Mn I 539.467 and 542.32 nm lines and other nearby lines to see if the other photospheric lines show chromospheric structures. We see both Mn images and also Si I 542.118 mimic magnetograms the similar way, while strong Fe and Ti lines only faintly reveal magnetic features, and weak Fe lines of comparable strength to Mn show nothing. Title: Data Calibration and Analysis for He I 1083 nm Imaging Spectroscopy Authors: Jones, Harrison P. Bibcode: 2003SoPh..218....1J Altcode: Imaging spectroscopy in the He i 1083 nm lines is a powerful tool for probing the top of the chromosphere and bottom of the transition region, but simple techniques for spectral calibration and analysis often fail for this line. A method for spectral flat-fielding using a uniform solar exposure with spectral lines in place is presented and illustrated with 1083 nm data obtained at the National Solar Observatory (NSO) Kitt Peak Vacuum Telescope with the NASA/NSO Spectromagnetograph. An efficient method for analysis of the data producing images in continuum intensity, line-of-sight velocity, equivalent width, central line depth, Doppler width, and line asymmetry is also presented and illustrated. Title: First Results from SOLIS Authors: Harvey, J.; Giampapa, M.; Henney, C.; Jones, H.; Keller, C. Bibcode: 2003AGUFMSH42B0545H Altcode: SOLIS (Synoptic Optical Long-term Investigations of the Sun) is a project to replace antiquated synoptic observing equipment at the National Solar Observatory. SOLIS includes a suite of three instruments on an equatorial mount originally installed at a site in Tucson and will be moved to Kitt Peak before the end of 2003. The major SOLIS instrument is a vector spectromagnetograph that maps magnetic fields across the full solar disk using a slit spectrograph and one arc sec pixels. Daily observations include several line-of-sight component magnetograms in the photosphere and chromosphere and, for the first time, full-disk vector magnetograms. At a medium scan speed ( ∼10 minutes for the full disk) noise is less than 1 Mx/cm2. This low noise, combined with negligible instrumental polarization and well resolved spectral line profiles, yields moderate resolution magnetograms of unprecedented quality. Sample observations show magnetic flux nearly everywhere in the photosphere from the disk center to the solar limb. The flux is organized in large scale patterns that heretofore had been visible only in strong flux elements or after substantial spatial smearing. Good results have been obtained from the other SOLIS instruments: a full-disk filter imager at several narrow wavelengths and a grating spectrograph that provides high-accuracy line spectra of integrated sunlight. SOLIS data are freely available via the Internet and users may submit observing time requests for special observations. The National Solar Observatory is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. Additional support for the development of SOLIS from NASA and ONR is gratefully acknowledged. Title: DASL--Data and Activities for Solar Learning Authors: Hill, F.; Gearen, M. V.; Henney, C. J.; Jones, H. P.; Stagg, T. Bibcode: 2003AGUFMED41D1189H Altcode: Data and Activities for Solar Learning (DASL) provides a classroom learning environment based on a twenty-five year record of solar magnetograms from the National Solar Observatory (NSO) at Kitt Peak, AZ. The data, together with image processing software for Macs or PCs, can be used to learn basic facts about the Sun and astronomy at the middle school level. At the high school level, students can study properties of the Sun's magnetic cycle with classroom excercises emphasizing data and error analysis and can participate in a new scientific study, Research in Active Solar Longitudes (RASL), in collaboration with classrooms throughout the country and scientists at NSO and NASA. We will demonstrate a compact disc with the data and software, and a web site for uploading the RASL results. Title: Comparison of Total Solar Irradiance with NASA/National Solar Observatory Spectromagnetograph Data in Solar Cycles 22 and 23 Authors: Jones, Harrison P.; Branston, Detrick D.; Jones, Patricia B.; Popescu, Miruna D. Bibcode: 2003ApJ...589..658J Altcode: NASA/National Solar Observatory Spectromagnetograph (SPM) data are compared with spacecraft measurements of total solar irradiance (TSI) variations for 8 yr beginning with the declining phase of solar cycle 22 and extending into the maximum of cycle 23. Previously reported conclusions based on a similar comparison for a shorter time period appear to be robust: three factors (sunspots, strong unipolar regions, and strong mixed-polarity regions) describe most of the variation in the SPM record, but only the first two are associated with TSI. Additionally, the residuals of a linear multiple regression of TSI against SPM observations over the entire 8 yr period show an unexplained, increasing, linear time variation with a rate of about 0.05 W m-2 yr-1. Separate regressions for the periods before and after 1996 January 1 show no unexplained trends but differ substantially in regression parameters. This behavior may reflect a solar source of TSI variations beyond sunspots or uncompensated nonsolar effects in one or both of the TSI and SPM data sets. Title: Calibration and Data Analysis for the SOLIS-VSM Authors: Henney, C. J.; Harvey, J. W.; Keller, C. U.; Jones, H. P.; SOLIS Team Bibcode: 2003SPD....34.0303H Altcode: 2003BAAS...35..808H The Vector Spectromagnetograph (VSM) instrument of the Synoptic Optical Long-term Investigations of the Sun (SOLIS) project will provide a unique 25-year record of synoptic solar observations with daily full-disk photospheric vector and high sensitivity longitudinal magnetograms. In addition, the VSM will produce daily full-disk chromospheric longitudinal magnetograms along with various He I 1083 nm parameter images. The VSM is being prepared for installation at a temporary site in Tucson for a comparison period with observations from the Kitt Peak Vacuum Telescope (KPVT). After the cross-calibration period, the VSM will replace the KPVT spectromagnetograph at Kitt Peak. We outline the various VSM data products, with emphasis on the calibration and data reduction efforts.

The data transmission and storage resources are such that the reduction of VSM data will be performed at the observing site on Kitt Peak. Reduced data products will be transmitted via a DS3 link from Kitt Peak to the National Solar Observatory's digital archive in Tucson. During a typical observing day, three full-disk photospheric vector magnetograms will be available over the Internet in two stages: first, as a ``quick-look'' product within 10 minutes of data acquisition, and then as a full Milne-Eddington (ME) inversion product within 12 hours of each observation. The quick-look parameters will include estimates of the magnetic field strength, azimuth and inclination based on Auer, Heasley, House (1977, Solar Physics 55, p. 47). The high-precision vector products will be determined with the High Altitude Observatory ME inversion technique implemented by Skumanich and Lites (1987, ApJ, 322, p.473). The flexible design of the VSM data handling system can incorporate future improvements under consideration (e.g., principal component analysis).

This research was supported in part by the Office of Naval Research Grant N00014-91-J-1040. Title: A New Way to Identify Coronal Holes. Authors: Malanushenko, O.; Jones, H. P. Bibcode: 2003SPD....34.0419M Altcode: 2003BAAS...35R.813M The location of a coronal hole (CH) in the upper chromosphere is usually based on equivalent width (EqW) images in the He 1083 nm line. A CH is seen on these images as bright areas, which represents low values of EqW. But sometimes it is difficult to differentiate a CH from the bright centers of chromospheric network, or filament channels, without complementary data and the skill of an experienced of observer.

To remove the above ambiguity we apply a new spectral analysis technique for the He I 1083 nm line to imaging spectroscopy of several CHs obtained with the NASA/NSO spectromagnetograph (Malanushenko and Jones, 2002, BAAS 33, 700). Reduction includes making dark and flat-field corrections; normalization to a non-linear continuum on the basis of a comparison to a spectral standard; a differential method for the de-blending of spectra; and multi-profile fitting to define the He line components.

We fit a Gaussian profile to the main component of the He line and deduce the parameters of central intensity (I) and half width at half maximum (HW). On the HW-images, CHs are distinguished from the surrounding regions as bright areas; similarly, they are also seen as bright on the I-images. Chromospheric network is seen on W-images as opposite in contrast to the I-images, and this distinction is the basis for our CH identification method. We normalize the I- and HW-images by subtracting their respective quiet-sun means and dividing by the corresponding standard deviations. The sum of the normalized I- and HW-images shows increasing contrast of the CH and a depression of contrast in the network and can be used as an independent CH diagnostic. Title: A New Fitting Procedure for the Blended He I 1083 nm Multiplet Authors: Jones, H. P.; Malanushenko, O. V. Bibcode: 2003SPD....34.1712J Altcode: 2003BAAS...35..839J The He I 1083 nm multiplet is a powerful tool for observing the outer solar atmosphere but is difficult to analyze because the lines are weak, highly variable, and spectrally blended, both internally and with other neighboring solar and telluric lines. After separation from nearby spectral features (see accompanying poster by Malanushenko and Jones), two components of the He I multiplet are resolved. Fitting these lines with two unconstrained Gaussian profiles always gives a ratio of major to minor component of less than half the value which would be expected for optically thin lines. One possibility for explaining the discrepancy between the weakness of the lines and the ratio of the spectral components is to assume that the line formation regions are concentrated in laterally unresolved, optically thick structures with small filling factor. However, we present here a least-squares fitting technique using cubic splines with fixed breakpoints with the constraint that the blend is the sum of three identically shaped profiles shifted in wavelength according to the atomic structure of the blend and weighted by the corresponding statistical weights, in agreement with optically thin line formation. The basis functions for the fitting procedure have no built-in spectral symmetry or shape. The resulting underlying profiles tend to be asymmetric with excess absorption to the blue, consistent with formation by "hot" and "cool" spatial elements within the observed volume, with the hotter regions having differential motion toward the observer. The results agree well with NASA/NSO Spectromagnetograph observations in quiet sun and coronal holes. Partial funding of this research was provided through the NASA Sun-Earth Connection SR&T program. Title: Recent Discoveries from the Anglo-Australian Planet Search Authors: McCarthy, C.; Tinney, C.; Jones, H.; Butler, P.; Carter, B.; Marcy, G.; Penny, A.; Blundell, J.; Bond, J. Bibcode: 2003ASPC..294...35M Altcode: We present the latest precision radial velocity results from the Anglo Australian Planet Search. These include new planet mass companions to HD216437, HD196050, HD30177, HD73526, and HD2039, as well as evidence for a second companion to HD160691 residing in a long period orbit. The results come from a sample of approx. 200 nearby inactive FGKM dwarfs with V<7.5 and a subsample of 20 more distant metal rich stars. At least 25 ± 11% of metal rich stars appear to have planets within 2.5 AU, somewhat more than the 8% of stars which appear to have planets within 3.5 AU. Title: Helicity and the SOLIS Vector-Spectromagnetograph Authors: Keller, Christoph U.; Harvey, John W.; Henney, Carl J.; Jones, Harrison P. Bibcode: 2003IAUJD...3E..18K Altcode: SOLIS (Synoptic Optical Long-term Investigations of the Sun) is a suite of three innovative instruments that greatly improve ground-based synoptic solar observations. The main instrument the Vector Spectro-Magnetograph (VSM) is a compact high-throughput vector-polarimeter that measures the magnetic field strength and direction over the full solar disk within 15 minutes. Helicity can be directly calculated from the full-disk vector field data provided by the Stokes inversion of the observed polarized line profiles. We present an anlysis of the difficulties and problems that one faces when interpreting the the helicity derived from VSM data. Title: Stokes V Profiles in a Post-flare Ca II 854.2nm Downflow Authors: Penn, M. J.; Jones, H. P. Bibcode: 2003ASPC..286..355P Altcode: 2003ctmf.conf..355P No abstract at ADS Title: Long-Term Solar Irradiance Variations From Solar Cycle 21 to 23 Authors: Pap, J. M.; Arge, C.; Jones, H.; Floyd, L. Bibcode: 2002AGUFMSH21B..03P Altcode: In this paper we show the recent results on total solar and UV irradiance variations and their relation to solar magnetic activity over solar cycles 21 to 23. Comparison of the multi-decade long irradiance and magnetic field measurements indicates that the shape and magnitude of irradiance variations are different from that of magnetic indices. Specifically, while magnetic indices show that solar cycle 23 is weaker than the two previous cycles, the long-term variation of total solar irradiance over solar cycles 21 to 23 is rather symmetrical, showing that its maximum and minimum levels were about the same within their measuring uncertainties. In this paper we address the questions: (1) is there a strict linear relationship between solar variability and irradiance variations; (2) what is the role of polar magnetic fields in irradiance changes; (3) is there a significant non-magnetic component in the observed irradiance variations? The results presented in this paper underscore the need to further develop new analysis techniques to determine whether there is a secular variation in solar irradiance over years to decades - a necessary step to study and predict the climate impact of solar variability. Title: Comparison of Three Solar Magnetographs Authors: Thornton, C. E.; Jones, H. P. Bibcode: 2002AAS...201.8307T Altcode: 2002BAAS...34.1243T The Sun's magnetic field controls the structure and activity of the outer solar atmosphere. Although the surface magnetic flux is now frequently observed over the entire visible hemisphere by several instruments, accurate quantitative measurment is still difficult as reflected by comparisons of different instruments which can show relative differences of 50% or more. We extend a previous study (Jones and Ceja, 2001, ASP Conference Series 236, 87)comparing data via histogram equating from three widely used sources: the SOHO Michelson Doppler Imager (MDI), the refurbished Global Oscillations Network Group (GONG+) and the NASA/NSO Spectromagnetograph (SPM). Data from GONG+ and SPM are quite comparable but underestimate flux values in comparison with MDI by 20-40%. Our analysis shows that MDI and SPM magnetograms agree better in later time periods when solar activity is higher, suggesting that strong-field regions are better measured than weak-field ones. This is probably due to the broader extents and higher filling factors for strong-field areas which cause them to be less sensitive to blurring and cancellation by atmospheric seeing in ground-based instruments. That seeing affects instrumental comparisons is reinforced by our examination of contrasts in cotemporal and cospatial intensity images accompanying SPM magnetograms; overall agreement between MDI and SPM data is generally better for higher rms contrasts in the SPM intensities. Title: Data analysis for the SOLIS Vector Spectromagnetograph Authors: Jones, Harrison P.; Harvey, John W.; Henney, Carl J.; Hill, Frank; Keller, Christoph U. Bibcode: 2002ESASP.505...15J Altcode: 2002solm.conf...15J; 2002IAUCo.188...15J The National Solar Observatory's SOLIS Vector Spectromagnetograph, which will produce three or more full-disk maps of the Sun's photospheric vector magnetic field every day for at least one solar magnetic cycle, is in the final stages of assembly. Initial observations, including cross-calibration with the current NASA/NSO spectromagnetograph (SPM), will soon be carried out at a test site in Tucson. This paper discusses data analysis techniques for reducing the raw data, calculation of line-of-sight magnetograms, and both quick-look and high-precision inference of vector fields from Stokes spectral profiles. Existing SPM algorithms, suitably modified to accommodate the cameras, scanning pattern, and polarization calibration optics for the VSM, will be used to "clean" the raw data and to process line-of-sight magnetograms. A recent version of the High Altitude Observatory Milne-Eddington (HAO-ME) inversion code will be used for high-precision vector fields. Title: New Analysis of He I 1083 nm Imaging Spectroscopy Authors: Malanushenko, O. V.; Jones, H. P. Bibcode: 2002AAS...200.3812M Altcode: 2002BAAS...34..700M We apply our new analysis method (Jones, H.P., Malanushenko, E.V, American Geophysical Union, Spring Meeting 2001, abstract #SH31A-01), which uses a spectral standard to determine the continuum and least-squares fitting of all relevant spectral features to removed effects of nearby solar and telluric lines, to imaging spectroscopy in the He I 1083 nm line of coronal holes and quiet sun obtained with the NASA/NSO spectromagnetograph. We find that in coronal holes the central line depth is slightly lower compared to cell centers in nearby quiet network, that the full-width-half maxima (FWHM)of coronal hole profiles is significantly (approximately 35%) higher than in quiet cell centers, and that the coronal hole line-of-sight velocities show a blue shift of 3-4 km/s. Preferential asymmetry with excess blue absorption is clearly evident in the processed profiles. We note that the blue shift of line center is not seen using earlier analysis techniques and explore the reasons for this difference. We suggest that FWHM may be a better coronal hole diagnostic than the lower contrast equivalent width which is currently used. Partial support of this research was provided by NASA Supporting Research and Technology grants under the Sun-Earth Connection program. Title: Stokes Inversion Techniques for the SOLIS-VSM Authors: Henney, C. J.; Keller, C. U.; Jones, H. P.; SOLIS Team Bibcode: 2002AAS...200.5514H Altcode: 2002BAAS...34Q.734H The Vector Spectromagnetograph (VSM) instrument of the Synoptic Optical Long-term Investigations of the Sun (SOLIS) project will begin operation in 2002 and provide a 25 year record of synoptic solar observations. The 50-cm aperture VSM will provide daily full-disk photospheric vector and high sensitivity longitudinal magnetograms. In addition, the VSM will produce daily full-disk chormospheric longitudinal magnetograms, along with 1083 nm equivalent width images. Current data transmission and storage resources are such that the reduction of VSM data will be performed at the observing site on Kitt Peak. Reduced data products will be transmitted via a DS3 link from Kitt Peak to the National Solar Observatory's digital archive in Tucson. During a typical observing day, three full-disk photospheric vector magnetograms will be available over the web in two stages: first, as a ``quick-look'' product within 10 minutes of data acquisition, and then as a full Milne-Eddington (ME) inversion product within 24 hours of each observation. The quick-look parameters will include estimates of the magnetic field strength, azimuth and inclination based on Auer, Heasley, House (1977, Solar Physics 55, p. 47). The high-precision vector products will be determined with the High Altitude Observatory ME inversion technique implemented by Skumanich and Lites (1987, ApJ, 322, p.473). The flexible design of the VSM data handling system can incorporate future improvements under consideration (e.g., principal component analysis). However, since the original Stokes profiles observed will not be archived, a retrospective reduction of VSM data will not be possible. Quick-look and full ME inversion results are compared using simulated VSM Stokes profile data based on Kitt Peak Vacuum Telescope magnetograms. This research was supported in part by the Office of Naval Research Grant N00014-91-J-1040. Title: Solar Irradiance Variations over Solar Cycles 21 to 23 Authors: Pap, J. M.; Kuhn, J.; Jones, H.; Turmon, M.; Arge, N.; Schmutz, W.; Floyd, L. Bibcode: 2002AAS...200.2803P Altcode: 2002BAAS...34..679P In this paper we describe the science requirements and a new measurement strategy to better understand solar variability and its potential effect on climate. We study the relation between the variations in solar total and UV irradiances and solar magnetic fields as observed within the last three decades. The results of our analysis raise important questions: (1) is there a significant non-magnetic component in the observed irradiance variations?; (2) may polar magnetic fields play a role in irradiance changes?; (3) is there a strict linear relationship between solar variability and irradiance variations as the current irradiance models used in climate studies assume? The results presented in this paper underscore the need to further develop new measurement and analysis techniques to study and predict the climate impact of solar variability. Title: The Diagnostic Potential of the CaII 8542 spectral line for Stokes I, V Spectropolarimetry Authors: Balasubramaniam, K. S.; Uitenbroek, H.; Havey, J. W.; Jones, H. Bibcode: 2002AAS...200.3807B Altcode: 2002BAAS...34R.699B The number of available spectral lines to probe magnetic fields in the solar chromosphere from the ground is practically limited to resonance lines of hydrogen, calcium, sodium and magnesium and the multiplets of helium. The range of heights over which each these spectral lines form extends over several hundred kilometers and temperatures over several hundreds of degrees, in a significantly non-local thermodynamic equilibrium atmosphere. In this paper we explore the diagnostic potential of the CaII 8542 A spectral line and the inference of active region magnetic and velocity fields. We will provide a NLTE analysis of the radiative transfer of this spectral line in the presence of magnetic fields and compare theoretical and measured spectral line profiles (observed using the NSO/KP Vacuum Telescope), to infer magnetic field strengths using the center-of-gravity separation of the Stokes (I+V), (I-V) components, and using the weak field approximation. Title: A comparison of feature classification methods for modeling solar irradiancevariation Authors: Jones, H.; Harvey, K.; Pap, J.; Preminger, D.; Turmon, M.; Walton, S. Bibcode: 2002cosp...34E.641J Altcode: 2002cosp.meetE.641J A physical understanding of both total (bolometric) and spectral solar irradiance variations depends upon establishing a connection between the temporal variability of spatially resolved solar structures and spacecraft observations of irradiance. One difficulty in comparing models derived from different data sets is that the many ways for identifying solar features such as faculae, sunspots, quiet sun, and various flavors of "network" are not necessarily consistent. To learn more about classification differences and how they affect irradiance models, we compare feature "masks" on selected days together with the temporal variation of feature areas derived from four current methods: multidimensional histogram analysis of NASA/NSO Kitt Peak spectromagnetograph data (Jones et al., 2000, ApJ 529, 1070); statistical pattern recognition applied to SOHO/MDI photograms and magnetograms (Turmon et al., 2002, ApJ 568, 396); threshhold masks allowing for influence of spatial surroundings applied to NSO magnetograms (Harvey and White, 1999, ApJ 515, 541); and the "three-trigger" algorithm applied to CSUN CFDT images (Preminger et al., 2001, Sol. Phys. 202, 53.). Developing a more uniform classification system of features contributing to irradiance variations will help to improve irradiance models used for climate studies. A practical benefit of understanding the relationships between various methods is the possibility of constructing a more continuous and extensive time series from several incomplete sources. Title: Long-term solar irradiance variations: results and perspectives Authors: Pap, J.; Fleck, B.; Frohlich, C.; Jones, H.; Kuhn, J.; Schmutz, W. Bibcode: 2002cosp...34E.553P Altcode: 2002cosp.meetE.553P In this paper we show the recent result on irradiance variations and their relation to solar magnetic activity over solar cycles 21 to 23. Comparison of the multi-decade long irradiance and magnetic field measurements indicates that the shape and magnitude of irradiance variations are different from that of magnetic indices. Specifically, while magnetic indices show that solar cycle 23 is weaker than the two previous cycles, the long-term variation of total solar irradiance over solar cycles 21 to 23 is rather symmetrical, showing that its maximum and minimum levels were about the same within their measuring uncertainties. These results raise questions like: (1) is there a strict linear relationship between solar variability and irradiance variations as the current irradiance models used in climate studies assume?; (2) what is the role of polar magnetic fields in irradiance changes?; (3) is there a significant non-magnetic component in the observed irradiance variations? The results presented in this paper underscore the need to further develop new measurement and analysis techniques to study and predict the climate impact of solar variability. Title: Solar irradiance variations over solar cycles 21 to 23 Authors: Pap, J.; Arge, N.; Floyd, L.; Helizon, R.; Jones, H. Bibcode: 2002cosp...34E1521P Altcode: 2002cosp.meetE1521P The Sun's radiative output has been monitored at various UV wavelengths and integrated over the entire solar spectrum - hence total irradiance - for almost three consecutive solar cycles. These multi-decade long measurements of total solar and spectral irradiance established conclusively that the Sun's radiative output varies on time scales from minutes to the 11-year solar cycle. To study long-term irradiance variations and their possible effects on climate, solar irradiance has been modeled empirically using the Photometric Sunspot Index and proxy indicators for facular brightening. These empirical models assume that solar irradiance varies in phase with the 11-year solar cycle, being higher during high solar activity cycles and lower during weaker cycles. However, direct photometric measurements of sunspots and faculae have shown that both the number and size of active regions were smaller during cycle 23 than during cycle 22. In addition, both the sunspot number and the full disk magnetic flux show that cycle 23 was weaker than the previous two solar cycles, while solar irradiance reached about the same maximum level during cycle 23 as during the last cycles. In this paper we compare the long-term variations of the composite total and UV irradiances with solar magnetic indices, such as the Photometric Sunspot Index, the equivalenth width of the He-line at 1083 nm, full disk magnetic flux, polar magnetic fields and facular proxies. The controversy between measured irradiance variations and their magnetic surrogates over solar cycles 21 to 23 is discussed in the paper. Title: Ground-Based Correlates of Solar Irradiance Variation Authors: Jones, H. P. Bibcode: 2001AAS...199.3603J Altcode: 2001BAAS...33.1360J Ground-based instruments cannot directly measure solar irradiance variablity at the 0.1% level at which it occurs because of the earth's atmosphere. However, many forms of ground-based solar observations correlate well with solar irradiance variations, and this fact has been used to construct facular-sunspot models which can explain about 90% of the variance of total solar irradiance as observed by spacecraft radiometers. It is not yet clear whether remaining discrepancies are observational or require additional sources in the model. This paper is a selective review of the current status of the use of ground-based data to understand spaceraft observations of solar irradiance and to apply this understanding to periods before space-based measurements were available. New results from the extension of the histogram analysis of NASA/NSO spectromagnetograph observations (Jones et al., 2000, ApJ 529, 1070) to the period from Nov. 1992 to Sep. 2000 are reported which confirm that strong mixed polarity magnetic regions (quiet network) are not significantly correlated with total solar irradiance and which show an unexplained linear trend in the residuals of a multiple regression. Title: Helioseismic Holography and a Study of the Process of Magnetic Flux Disappearance in Canceling Bipoles Authors: Lindsey, Charles; Harvey, Karen L.; Braun, D.; Jones, H. P.; Penn, M.; Hassler, D. Bibcode: 2001STIN...0156300L Altcode: Project 1: We have developed and applied a technique of helioseismic holography along the lines of originally set out in our proposal. The result of the application of this diagnostic technique to solar activity and the quiet Sun has produced a number of important discoveries: (1) acoustic moats surrounding sunspots; (2) acoustic glories surround large active regions; (3) acoustic condensations beneath active regions; and (4) temporally-resolve acoustic images of a solar flare. These results have been published in a series of papers in the Astrophysical Journal. We think that helioseismic holography is now established as the most powerful and discriminating diagnostic in local helioseismology. Project 2: We conducted a collaborative observational program to define the physical character and magnetic geometry of canceling magnetic bipoles aimed at determining if the cancellation process is the result of submergence of magnetic fields. This assessment is based on ground-based observations combining photospheric and chromospheric magnetograms from NSO/KP, BBSO, and SOHO-MDI, and EUV and X-ray images from SOHO EIT/CDS, Yohkoh/SXT, and TRACE. Our study involves the analysis of data taken during three observing campaigns to define the height structure of canceling bipoles inferred from magnetic field and intensity images, and how this varies with time. We find that some canceling bipoles can be explained by the submerge of their magnetic flux. A paper on the results of this analysis will be presented at an upcoming scientific meeting and be written up for publication. Title: 2p2 Team News Authors: Jones, H.; Pompei, E. Bibcode: 2001Msngr.104....7J Altcode: Team member Patrick Fran Title: Achieving 1% photometric accuracy with the ESO Wide Field Imager Authors: Manfroid, J.; Selman, F.; Jones, H. Bibcode: 2001Msngr.104...16M Altcode: The highly successful Wide Field Imager on the ESO/MPG 2.2-m telescope offers the possibility of undertaking photometry over a half-degree field. The authors discuss findings concerning the photometric performance of the camera. They describe strategies for dealing with the flat-field calibration error, which is often underestimated by observers. Title: Two-Component Fitting of Coronal-Hole and Quiet-Sun He I 1083 nm Spectra Authors: Jones, H. P.; Malanushenko, E. V. Bibcode: 2001AGUSM..SH31A01J Altcode: We present reduction techniques and first results for detailed fitting of solar spectra obtained with the NASA/National Solar Observatory Spectromagnetograph (NASA/NSO SPM) over a 2 nm bandpass centered on the He I 1083 nm line. The observation for this analysis was a spectra-spectroheliogram obtained at the NSO/Kitt Peak Vacuum Telescope (KPVT) on 00 Apr 17 at 21:46 UT spanning an area of 512 x 900 arc-seconds; the field of view included a coronal hole near disk center as well as surrounding quiet sun. Since the He I line is very weak and blended with nearby solar and telluric lines, accurate determination of the continuum intensity as a function of wavelength is crucial. We have modified the technique of Malanushenko et al. (1992; AA 259, 567) to tie regions of continuua and the wings of spectral lines which show little variation over the image to standard reference spectra such as the NSO Fourier Transform Spectrometer atlas (Wallace et al. 1993; NSO Tech Report #93-001). We performed detailed least-squares fits of spectra from selected areas, accounting for all the known telluric and solar absorbers in the spectral bandpass. The best physically consistent fits to the Helium lines were obtained with Gaussian profiles from two components (one ``cool'', characteristic of the upper chromosphere; one ``hot'', representing the cool transition region at 2-3 x 104 K). In the coronal hole, the transition-region component, shifted by 6-7 km/s to the blue, is mildly dominant, consistent with mass outflow as suggested by Dupree et al., (1996; Ap. J.~467, 121). In quiet-sun spectra there is less evidence of outward flow, and the chromospheric component is more important. All our fitted spectra show a very weak unidentified absorption feature at 1082.880 nm in the red wing of the nearby Si I line. Title: 2p2 Team News Authors: Jones, H. Bibcode: 2001Msngr.103....9J Altcode: In December we welcomed Emanuel Galliano to our team. Emanuel is a French student at ESO Chile who is already familiar with La Silla, through his previous work with the DENIS group. He will be working primarily on operations at the 2.2-m. In February, however, we bade farewell to Emanuela Pompei after nearly two years with the team. Although Emanuela is leaving La Silla, she will remain with ESO in Chile, commencing work as a Staff Astronomer on Paranal in March. We wish her all the best in her move north. Title: Discovery of a bow-shock nebula around the pulsar B0740-28 Authors: Jones, H.; Stappers, B.; Gaensler, B. Bibcode: 2001Msngr.103...27J Altcode: Bow-shock nebulae around highvelocity pulsars provide our primary insight into the interaction between a pulsar and its surrounding environment. Specifically, optical observations of such nebulae allow us to derive full three-dimensional pulsar velocities which are extremely important for the birth rates and evolution of pulsars. They can also provide important information on the density, temperature and composition of the surrounding ambient medium. Unfortunately, only a few bow-shock nebulae have been discovered, despite there being nearly a thousand pulsars known from radio surveys. We have therefore commenced a search for pulsar bow-shocks, using the results to characterise the properties of the associated pulsars, pulsar winds and ambient environments. Title: Tunable filters and large telescopes Authors: Jones, H.; Renzini, A.; Rosati, P.; Seifert, W. Bibcode: 2001Msngr.103...10J Altcode: Traditionally, astronomy has relied upon filters with a fixed bandpass to select the wavelengths of the light allowed to reach the detector, thus allowing the astronomer to derive some colour information about the objects under study. In the optical, these filters are most often classical broadband UBVRI, or narrow passbands centred at the wavelengths of the common emission-line features, either at rest-frame or redshifted wavelengths. Examples of the latter are becoming numerous, especially on the 8-10-mclass telescopes that make it possible to detect very faint, distant emissionline objects, even through narrow passbands. In this vein, Kurk et al. (2000) used FORS1 at the VLT with a 65-Åwide filter at 3814 Å to image a z = 2.2 radio galaxy, searching for nearby Lyalpha detections at the same redshift. They detected around 50 such objects, collectively suggestive of strong clustering around the dominant radio galaxy. Moreover, they also found extended Ly-alpha emission (~ 100 kpc in extent) centred on the galaxy, adding further evidence to the possible scenario of protocluster formation. Title: Preliminary Comparison of Magnetograms from KPVT/SPM, SOHO/MDI and GONG+ Authors: Jones, H. P.; Ceja, J. A. Bibcode: 2001ASPC..236...87J Altcode: 2001aspt.conf...87J No abstract at ADS Title: Real Research In The Classroom - Solar Active Longitudes Authors: Stagg, T.; Gearen, M.; Jacoby, S. H.; Jones, H. P.; Henney, C. J.; Hill, F. Bibcode: 2000AAS...197.8709S Altcode: 2000BAAS...32.1556S We present a high-school level educational/research module for a project that improves computer and analytical skills and contributes new scientific results to the field of solar astronomy and physics. The module has been developed within the RET (Research Experience for Teachers) program as a new application of a cooperative project between the RBSE (Research-Based Science Education) initiative of the NSF and the NASA Education/Public Outreach program. The research goal is to improve our knowledge of the characteristics of solar active longitudes, where sunspots tend to cluster. In particular, the rotation rate of these regions is poorly known. It is suspected that the active longitude rotation rate (ALRR) is different from the rotation rate of the solar surface. If this is true, the ALRR can be compared with the internal rotation rate deduced by helioseismology providing an estimate of the active region depth. A good determination of the ALRR requires the measurement of the position of thousands of individual active regions, a step best done by interactive examination of images, selection of regions, and determination of heliographic position. These tasks are well-suited for high school students, who are thus provided with a motivation to improve their computer and scientific thinking skills. ScionImage (PC)/NIH Image (Macs) macros for this purpose have been developed which access a CD-ROM of 25 years of NSO/Kitt Peak magnetogram data and laboratory exercises developed previously for classroom use. In the future, a web site will be created for collecting the data from classrooms across the US, and for status reports on the results. Title: 2p2 Team News Authors: Jones, H. Bibcode: 2000Msngr.102...12J Altcode: In September we welcomed new team member Lisa Germany from Australia. Lisa is a new ESO Fellow and has interests in supernovae and their use in cosmological distance determinations. S e p t e m b e r, however, was also a month for departures when we said goodbye to long-time team member James Brewer. James was a pivotal member of the 2p2 Team since his arrival at ESO in 1996. He has returned to Canada to take up a position at the University of British Columbia, in Vancouver, Canada. We wish him all the best under northern skies. Title: Water vapour in cool dwarf stars Authors: Jones, H.; Viti, S. Bibcode: 2000ESASP.456..195J Altcode: 2000ibp..conf..195J M dwarf spectra beyond 1.35 μm are dominated by water vapour yet terrestrial water vapour makes it notoriously difficult to make accurate measurement of the water vapour bands from ground-based observations. We have used the short wavelength spectrometer on the Infrared Space Observatory (ISO) at four wavelength settings to cover the 2.5 - 3.0 μm region for a range of M dwarfs. The observations show a good match with previous ground-based observations and a reasonable match with the best available synthetic spectra. In particular the synthetic spectra and particularly the ab initio calculations for water vapour on which they hinge now accurately predict the positions of water vapour transitions. However, further work extending the calculation of water vapour to higher energy levels is probably necessary before a detailed match in intensity will be possible. Title: 2p2 Team News Authors: Jones, H. Bibcode: 2000Msngr.100...29J Altcode: The 2p2 Team continued towards the implementation at the 2.2-m of the same BOB (Broker for Observation Blocks) observing interface as seen at other ESO telescopes. This requires an interface to be written between the existing BOB software and the non-VLT compatible control software for the Wide-Field Imager (WFI) and 2.2-m. Cristian Urrutia, Tatiana Paz and Eduardo Robledo are heading its development. With this software in place, observers can use the VLT Phase 2 Proposal Preparation System (P2PP) for definition of their exposures, whether they are for Visitor or Service Mode. Title: Helium 1083 nm Imaging Spectroscopy: November 1999 Authors: Jones, H. P. Bibcode: 2000SPD....31.0231J Altcode: 2000BAAS...32..816J An observing program using the NASA/NSO Spectromagnetograph (SPM) at the NSO/Kitt Peak Vacuum Telescope and SOHO/SUMER to look for Doppler shifts and line asymmetries in coronal holes was completed in early November, 1999 in collaboration with D. Hassler. This paper presents first results from the SPM only; analysis of and comparison with the SUMER observations is in progress and will be reported at a later date. SPM spectra-spectroheliograms were obtained on 99 Nov. 3-10 (no data for Nov. 7) for two coronal holes, surrounding active regions, and the decay phase of a small flare. Images and sample spectra are displayed. The first target of opportunity for this program was a small coronal hole approaching disk center whose identification was based on EIT images but which was not identified as a hole in the NSO synoptic 1083 nm images (K. Harvey, private communication, 1999). The area did not show 1083 nm line asymmetries as are often seen in polar holes near the limb (Dupree et al, 1996). However, a larger and more prominent coronal hole was observed in the latter portion of the observing run over a wide range of heliocentric angle, including near disk center, which showed strong 1083 nm asymmetry consistent with the observations of Dupree et al (1996), Jones et al (1997), and Jones and Bender (2000). Preliminary analysis of the SUMER observations in Si II, C IV, and Ne VIII show blue shifts in the high temperature line (Hassler, private communication, 2000), and future work will involve the removal of systematics from both data sets and their careful registration and comparison with each other and with magnetograms. This work was supported by NASA tasks 682-344-12-19-01 and 682-370-16-22-0. NSO/Kitt Peak data used here are produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL. Title: Analysis of NASA/NSO Spectromagnetograph Observations for Comparison with Solar Irradiance Variations Authors: Jones, Harrison P.; Branston, Detrick D.; Jones, Patricia B.; Wills-Davey, Meredith J. Bibcode: 2000ApJ...529.1070J Altcode: The NASA/NSO Spectromagnetograph (SPM) at the National Solar Observatory/Kitt Peak Vacuum Telescope (NSO/KPVT) has produced daily full-disk solar images of line-of-sight (LOS) magnetic flux, LOS velocity, continuum intensity, equivalent width, and central line depth in either Fe I 550.7 nm or Fe I 868.8 nm since 1992 April. Internally, these five images are strictly cospatial and cotemporal. This paper describes reduction techniques for removing spurious effects (principally from clouds and optical vignetting) from the images and presents summary statistics from the first 2 years of operation. Pairs of bivariate histograms as well as five-dimensional histograms are formed from the ``cleaned'' images. Factor analysis of various summary statistics from the histograms shows that mixed-polarity magnetic elements of weak to moderate strength; unipolar magnetic features, including active regions and strong enhanced network; and sunspots are the most important sources of variance in the SPM data. Multiple regressions of spacecraft measurements of bolometric solar irradiance on the dominant factors, however, yield strong correlations with only unipolar regions and sunspots; the weak and mixed-polarity features that account for most of the SPM variance are only weakly correlated with the spacecraft measurements. Title: The Tunable Filter Approach to Measuring Cosmic Star Formation History Authors: Jones, H. Bibcode: 2000ASPC..221..207J Altcode: 2000sgdg.conf..207J No abstract at ADS Title: The Solar Magnetic Cycle: An Educational Display: Year 2 Authors: Jacoby, Suzanne H.; Jones, H. P.; Gearen, M. V. Bibcode: 2000ASPC..220..371J Altcode: 2000appa.conf..371J No abstract at ADS Title: Does Magnetic Flux Submerge at Flux Cancelation Sites? Authors: Harvey, Karen L.; Jones, Harrison P.; Schrijver, Carolus J.; Penn, Matthew J. Bibcode: 1999SoPh..190...35H Altcode: Simultaneous measurements of the magnetic fields in the photosphere and chromosphere were used to investigate if magnetic flux is submerging at sites between adjacent opposite polarity magnetic network elements in which the flux is observed to decrease or `cancel'. These data were compared with chromospheric and coronal intensity images to establish the timing of the emission structures associated with these magnetic structures as a function of height. We found that most of the cancelation sites show either that the bipole is observed longer in the photosphere than in the chromosphere and corona (44%) or that the timing difference of the disappearance of the bipole between these levels of the atmosphere is unresolved. The magnetic axis lengths of the structures associated with the cancelation sites are on average slightly smaller in the chromosphere than the photosphere. These observations suggest that magnetic flux is retracting below the surface for most, if not all, of the cancelation sites studied. Title: Low Transition-Region Outflow: Solar He I 1083 nm Asymmetry in a Disk-Center Coronal Hole Authors: Jones, H. P.; Bender, C. F. Bibcode: 1999AAS...19510703J Altcode: 1999BAAS...31.1531J We analyze imaging spectroscopy in the He I 1083 nm line of a solar coronal hole observed near disk center on 26 Feb 1999 with the NASA/NSO Spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope. For this study we examine the equivalent width of the He I absorption feature along with its wing asymmetry as determined by the difference in the wavelength position of the line bisector at 30% of central line depth from line center. Dupree, Penn, and Jones (1996, ApJ 467, L121) previously used a similar measure to show that excess blue absorption, indicative of line-of-sight motion towards the observer, is found preferentially in some polar coronal holes where the line is weakest. They suggested on the basis of the variation of this asymmetry with heliocentric angle over the limited domain spanned by their observations that these motions are vertical and are candidates for source regions of high-speed solar wind. Our data confirm that this phenomenon can be observed in coronal holes at disk center with about the magnitude (7-9 km/s) suggested from extrapolating the results of Dupree et al. Motions parallel to the solar surface cannot explain our observations, and these areas may indeed point to low-lying origins of the solar wind. We compare our results to observations on other days of quiet Sun outside of coronal holes near disk center as well as to other polar coronal holes. CFB participated in this research as an NSO Student Research Assistant supported by NASA task 344-12-19-01 (NRA 96-OSS-09). NSO/Kitt Peak data used here are produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEL. Title: Large-Scale Chromospheric Magnetic Fields Authors: Harvey, J.; Bippert-Plymate, T.; Branston, D.; Plymate, C.; Recely, F.; Jones, H. Bibcode: 1999AAS...194.9406H Altcode: 1999BAAS...31R.991H Since mid-1996, NSO and its partners have made regular full-disk, line-of-sight component magnetograms using the 854.2 nm line of Ca II. These observations are primarily sensitive to the magnetic field about 800 km above the photosphere. Several new features of the solar magnetic field have emerged in these observations. At a sensitivity of about 3 Gauss and using one arc sec pixels, we observe diffuse, large-scale magnetic fields in the chromosphere that have no significant counterparts in the photosphere. The most obvious of these fields are found surrounding the borders of active regions and seem to correspond to the "circumfacule" phenomenon first described in 1910 by Deslandres. In other words, these fields seem to be the nearly horizontal field component associated with long chromospheric fibrils found around some active regions. The next most obvious example of large-scale chromospheric fields is a surprise. These fields are found closely associated with filament channels but, unlike the ubiquitous polarity reversal always seen in the photospheric magnetic field under filament channels, the chromospheric field has only one apparent polarity across the filament channel. However, the apparent sign of the chromospheric field reverses near the central meridian as the feature traverses the solar disk. This behavior indicates that the field is predominantly horizontal with a strong east-west component. These fields are typically seen on the poleward side of mature active regions and may last several solar rotations. They should be an important diagnostic of magnetic field patterns surrounding solar filaments. It is not clear why some filament channels show these fields while others do not. A final type of large-scale chromospheric magnetic field is at our present limit of detection and is simply a predominance of one magnetic polarity or the other over large areas of the solar disk. Such patterns can be seen in the photosphere after a large amount of spatial averaging, but require no such averaging in the chromosphere. The NSO is one of the National Optical Astronomy Observatories which are sponsored by the National Science Foundation. The NSO data used here are produced cooperatively by NSF/NOAO, NASA/GSFC, and NOAA/SEC. Title: Flat-Fielding Solar Spectroscopic Images Authors: Jones, H. P. Bibcode: 1999AAS...194.7612J Altcode: 1999BAAS...31Q.958J A key problem for the analysis of the spectral-spatial datacubes produced by the many operational and planned solar spectroscopic imagers (e.g., SUMER and CDS on SOHO; the SOLIS Vector Spectromagnetograph (VSM)) is how to obtain a suitable "flat-field" image for fixed-pattern correction of each slice (long-slit spectrum) of the data. We describe here some algorithms developed for flat-fielding NASA/NSO Spectromagnetograph (SPM) and NSO Near-Infrared Magnograph (NIM 1) data both for analysis of He I 1083 nm data and as prototype procedures for the future VSM. The 1083 nm line is a severe test since the line is very weak, and similarly stringent requirements need to be met for precision spectral polarimetry from the VSM. The procedures remove spectrum lines from ``raw'' flat-fields derived by integrating spectra as the solar image is scanned to give an equivalent exposure to each spatial element along the spectrograph slit with the exact instrument configuration that is used in the observations. We find this preferable to other techniques such as moving the grating to nearby continuum or image defocussing, both of which change fringe patterns and/or the way optical impurities such as dust are imaged. An iterative fitting procedure is described which works well on the SPM data but is less satisfactory for NIM 1 because, in the latter case, the detector readout introduces a columnar pattern parallel to the spectrum lines which is removed by the SPM algorithm. The orientation of read-out and spectrum will be the same as NIM-1 for the VSM. We describe initial attempts to use a new least-squares spline technique (Thijsse, Hollanders, and Hendrikse, 1998, Computers in Physics 12, 393) to address this difficulty. Title: An Educational Display of the Solar Magnetic Cycle: Year 2 Authors: Jones, H. P.; Gearen, M. V.; Jacoby, S. H. Bibcode: 1999AAS...194.7012J Altcode: 1999BAAS...31..939J We are developing an educational module to improve student and public understanding of the Sun's magnetic cycle. The instructional package features a CDROM compatible with most personal computers available in the home or classroom with a day-by-day record of an entire magnetic cycle as recorded in magnetograms from the National Solar Observatory Kitt Peak Vacuum Telescope (NSO/KPVT) near Tucson, AZ. These data have in fact been crucial to developing our present understanding of the solar cycle and its terrestrial effects. In the second year of the project, we have loaded the data to compact disks both as individual "gif" files for inspection and analysis and as QuickTime movies, have prepared the first version of the accompanying textual material, and are developing macros to aid extraction of information from the data for various laboratory exercises. We will display samples of these images and movies, and will furnish copies of the compact disks and accompanying textual material for testing and comment. Title: Optical observations of GRB990907. Authors: Palazzi, E.; Pian, E.; Masetti, N.; Frontera, F.; Vreeswijk, P. M.; Rol, E.; Pedersen, H.; Hjorth, J.; van Paradijs, J.; Kouveliotou, C.; Leisy, P.; Pizzella, A.; Pompei, E.; Mennickent, R.; Tinney, C. G.; Freeman, F.; Lee, S.; Bland-Hawthorn, J.; McMahon, R.; Maddox, S.; Singleton, C.; Jones, H. Bibcode: 1999GCN...413....1P Altcode: No abstract at ADS Title: Optical observations of GRB990217. Authors: Palazzi, E.; Masetti, N.; Pian, E.; Frontera, F.; Vreeswijk, P. M.; Rol, E.; Galama, T. J.; Dubus, G.; van Paradijs, J.; Kouveliotou, C.; Hainaut, O.; Tinney, C.; Axelrod, T.; Schmidt, B.; Jones, H. Bibcode: 1999GCN...262....1P Altcode: No abstract at ADS Title: GRB980326 optical observations Authors: Groot, P. J.; Vreeswijk, P. M.; Galama, T. J.; Pian, E.; Frontera, F.; Palazzi, E.; Feroci, M.; Kouveliotou, C.; Robinson, C.; van Paradijs, J.; Tinney, C.; Phillips; Driver; Smith; Jones; Windridge; Keane, M.; Hall, P.; Smith, M.; Gonzalez, J. F.; Lidman, C.; CTIO GRB Collaboration Bibcode: 1998GCN....32....1G Altcode: Comparison of optical R-band observations of the error box of GRB980326 (IAUC 6851) taken at the AAT at Mar 27.42 UT (480s), the CTIO 4m-telescope at Mar 28.04 UT (600s) and the ESO 3.5m NTT at Mar 28.01 UT (ESO1, 600s) and Mar 28.17 UT (ESO2, 600s) shows a clearly variable object located at RA 08:36:34.28, Decl -18:51:23.9 (J2000). Differential photometry with respect to three local stars shows a decrease between the AAT and ESO1 of 1.2(1) mag, AAT and CTIO of 1.6(1) mag and AAT and ESO2 of 1.7(1) mag. The three local standards have coordinate end-figures: 1) 36:35.41, 51:41.6; 2) 36:31.00, 51:17.3; 3) 36:34.03, 50:53.2. Their R-band magnitudes are: 1) 18.4(1); 2) 21.7(1); 3) 20.3(1), as determined with respect to Landolt SA 98, no. 626, 624, 634, 590. At the time of the AAT observation (Mar. 27.42 UT) the R-band magnitude of the variable was R=21.7, equal to that of comparison star 2. A finding chart of the variable can be found at: http://www.astro.uva.nl/paulgr/grb/grb980326.html. This message is citeable. Title: Histograms of Synoptic Spectromagnetograph Observations Authors: Jones, Harrison P. Bibcode: 1998ASPC..140..145J Altcode: 1998ssp..conf..145J No abstract at ADS Title: The Helium Spectrum in the Quiet Sun: The January 16/17 and May 7-13 1997 Coordinated SOHO/Ground-Based Observational Campaigns Authors: Andretta, Vincenzo; Jordan, Stuart D.; Muglach, Karin; Garcia, Adriana; Jones, Harrison P.; Penn, Matthew J.; Soltau, Dirk Bibcode: 1998ASPC..155..336A Altcode: 1998sasp.conf..336A No abstract at ADS Title: Investigating the Formation of the Helium Spectrum in the Solar Atmosphere Authors: Andretta, Vincenzo; Jordan, Stuart D.; Muglach, Karin; Garcia, Adriana; Jones, Harrison P.; Soltau, Dirk Bibcode: 1998ASPC..154..559A Altcode: 1998csss...10..559A We present the first results of coordinated observations with SOHO (Solar Heliospheric Observatory) and ground-based observatories aimed at investigating the mechanisms responsible for the formation of helium lines in the quiescent solar atmosphere. The observations described here were taken on 7-13 May 1997; the SOHO instruments involved were CDS, SUMER and EIT, while ground-based support was provided by the German Vacuum Tower Telescope on Tenerife (He 1 lambda10830 and Ca 2 lambda8498 spectra-spectroheliograms), Coimbra Solar Observatory (Hα spectroheliograms), and NASA/NSO Vacuum Tower Telescope on Kitt Peak (Ca 2 lambda8542 spectra-spectroheliograms and polarimetry). Title: The USAF Improved Solar Observing Optical Network (ISOON) and its Impact on Solar Synoptic Data Bases Authors: Neidig, D.; Wiborg, P.; Confer, M.; Haas, B.; Dunn, R.; Balasubramaniam, K. S.; Gullixson, C.; Craig, D.; Kaufman, M.; Hull, W.; McGraw, R.; Henry, T.; Rentschler, R.; Keller, C.; Jones, H.; Coulter, R.; Gregory, S.; Schimming, R.; Smaga, B. Bibcode: 1998ASPC..140..519N Altcode: 1998ssp..conf..519N No abstract at ADS Title: Comparison of NSO/KPVT 1083 NM and SOHO/CDS/SUMER Observations of a Coronal Hole. Authors: Jones, H. P.; Andretta, V.; Jordan, S. D.; Penn, M. J. Bibcode: 1997AAS...191.7304J Altcode: 1997BAAS...29.1321J As part of SOHO Joint Observing Program 16 to study the solar formation of Helium, coordinated observations of a coronal hole were obtained on 17 Jan 97. In this paper, we compare the NSO/KPVT full-disk 1083 nm spectroheliogram and a time sequence of spectra-spectroheliograms of the coronal hole near the south solar pole with approximately cospatial and cotemporal SOHO spatial-spectral data taken in He I (58.4 nm, CDS and SUMER) and He II 30.4 nm (CDS) together with several transition-region and coronal lines of CIII, OIII, OIV, MgIX, MgX, SiIX, and SiXII. We have previously reported on correlations of line intensities. Here we concentrate as well on Doppler shifts and, in particular, line asymmetry in the He I 1083 nm line which shows augmented absorption in the blue wing of the line within the coronal hole in the same sense as reported by Dupree, Penn, and Jones (1996, ApJ 467, L121). Title: On the Role of the Solar Corona and Transition Region in the Excitation of the Spectrum of Neutral Helium Authors: Andretta, Vincenzo; Jones, Harrison P. Bibcode: 1997ApJ...489..375A Altcode: We investigate the formation of the spectrum of neutral helium in the solar atmosphere by solving the corresponding non-LTE problem in an extended grid of model atmospheres. From the results we infer several general properties and scaling laws that can be used to discriminate the different proposed formation mechanisms. Some of the scaling laws have also been tested in a comparison with previous calculations made with different assumptions.

In our models, the excitation of the spectrum by direct photoionization by EUV radiation shortward of 504 Å followed by recombinations (PR mechanism), seems to be capable of influencing significantly the resonance continuum and the subordinate lines, even in the presence of other (collisional) excitation mechanisms. While this influence is almost unavoidable in most atmospheric features, it is hardly justifiable as the only possible contribution. Moreover, the resonance lines seem inclined to respond much more effectively to the conditions of the lower transition region, even in the presence of a significant coronal EUV illumination. With the help of the detailed non-LTE calculations and of the derived scaling laws, we explore the interplay of the possible formation mechanisms and their effect on the individual spectral features. Title: A model of the far-infrared emission from the Galaxy Authors: Davies, J. I.; Trewhella, M.; Jones, H.; Lisk, C.; Madden, A.; Moss, J. Bibcode: 1997MNRAS.288..679D Altcode: The warm dust (<25K) that lies in the plane of the Galaxy (scaleheight of about 0.13 kpc) was detected by IRAS and is preferentially associated with star formation regions. In this paper we describe a model of the diffuse far-infared emission from cool dust within the Galaxy. We identify a more diffuse, cool (18-22K) dust component (scaleheight of about 0.5 kpc) that has been detected by the DIRBE (at 140 and 240 μm) on the COBE satellite. This dust may be supported above the Galactic plane by radiation pressure. We show that the excess emission cannot be accounted for by the far-infrared background (upper limits of 1.0 and 0.5 MJ sr^-1 at 140 and 240mum respectively) or by the zodiacal light. The total luminosity of this cool component is ~7x10^9Lsolar, and it has a mass of ~3x10^7Msolar. We calculate extinction values for the cool component of A_v~27 mag towards the Galactic Centre, and A_v~0.3 mag at the poles. Title: Quiet Sun He I 1083 NM Chromospheric Events Authors: Penn, M. J.; Jones, H. P. Bibcode: 1997SPD....28.1303P Altcode: 1997BAAS...29..917P Several types of flows are observed in the quiet solar chromosphere using the He I 1083 nm absorption line with data from the NSO/KPVT. Downflow events, termed ``He Rain'' are described by about 4 km/sec Doppler red-shift of the line, an increased line width, and enhanced line absorption. The ``He Rain'' events begin with a small, compact morphology then evolve during 500 seconds to become extended and diffuse. The birth-rate of these ``He Rain'' events suggests an association with either coronal loop interactions or macrospicules. Loop-flow events observed with the He I 1083 nm line show blue-shifts followed by a red-shift, an increased line width and enhanced line absorption. The events follow curving trajectories with sizes about 30 arcsec. These events occur much less frequently than spicules, but may be associated with a type of spicule or some flow along the local magnetic field. Recent observations of these quiet Sun events and discussion of the associated coronal events will be presented. Title: Reduction and Analysis of He I 1083 NM Spectra-Spectroheliograms Authors: Jones, H. P.; Winters, W. F.; Penn, M. J.; Schwitters, J. D. Bibcode: 1997SPD....28.0225J Altcode: 1997BAAS...29..897J Over two decades of synoptic 1083 nm data from the National Solar Observatory/Kitt Peak Vacuum Telescope (NSO/KPVT) attest to the fact that satisfactory equivalent width images may be obtained from simple sums over ``line''and ``continuum'' bandpasses. However, much more care is needed to extract Doppler velocity, line depth, and asymmetry since the 1083 nm line typically has line depths of only a few percent and is blended with both telluric water vapor and the red wing of a nearby Si I line at 1082.8 nm. We present a new algorithm for analysis of He I 1083 nm data obtained with the NASA/NSO Spectromagnetograph (SPM) at the KPVT. A linear fit to intensity averages over bands near 1082.4 nm and 1083.6 nm specifies the continuum intensity across the wavelength domain of interest. The spectral algorithm currently used for 868.8 nm SPM magnetograms computes line-center wavelengths and depths for the strong adjacent telluric and Si lines. Quick fits of the damping wings of these features together with a scaled profile of the weak water vapor feature which is coincident in wavelength with the 1083 nm line (Breckenridge and Hall, 1973: Solar Phys. 28, 15) are removed from the spectral region containing the 1083 nm line. The spectral algorithm then computes the central wavelength and line depth of the 1083 nm line. An extension of this algorithm locates the bisector at the 0.35 central line-depth position on the profile to compute a line asymmetry parameter (Dupree, Penn, and Jones, 1976: ApJ 467, L121). We show sample results of the algorithm applied both off-line to spectra-spectroheliograms and on-line to spatial-spectral data as they are acquired. Title: Investigating the Formation of the Helium Spectrum with Coordinated SOHO/Kitt Peak/Sacramento Peak Observations Authors: Andretta, V.; Jordan, Stuart D.; Jones, Harrison P.; Penn, Matthew J. Bibcode: 1997ESASP.404..163A Altcode: 1997cswn.conf..163A No abstract at ADS Title: The distribution of galactic inclinations - a clue to opacity? Authors: Jones, H.; Davies, J. I.; Trewhella, M. Bibcode: 1996MNRAS.283..316J Altcode: No abstract at ADS Title: Online analysis and compression of spectra-spectroheliograms Authors: Jones, Harrison P. Bibcode: 1996SPIE.2804..110J Altcode: The on-line algorithm used by the NASA/National Solar Observatory Spectromagnetograph for analysis of long-slit spectrum-line profiles is presented with a view towards future application to processing large volumes of data from spacecraft and other remote instruments. At every spatial position, the procedure finds continuum intensity, equivalent width, and wavelength position and intensity of the central extremum of absorption or emission. The wavelength position of line center is found from the zero- crossing of the convolution of the line profile with a fixed anti-symmetric kernel. As currently used with the spectromagnetograph, images based on the line parameters computed at every spatial position are saved, but the original data are discarded. This paper explores the possibility of preserving the data in compressed form by saving, in addition to the derived line parameters, the differences between the data and model profiles synthesized from the on-line analysis. Title: Limb Observations of HE I 1083 NM Authors: Penn, M. J.; Jones, H. P. Bibcode: 1996SoPh..168...19P Altcode: Imaging spectroscopic data of the He I 1083 nm limb emission were taken on several dates in October and November 1995 with the NASA/NSO spectromagnetograph at the NSO/Kitt Peak vacuum telescope and on 9 December, 1993 with the Michigan infrared camera at the NSO/Sacramento Peak vacuum tower telescope. Emission line profiles were observed in quiet-Sun and coronal hole locations on the northern and southern solar poles and on the east solar limb. The height of the He I 1083 nm shell above the continuum limb at 1083 nm was measured to be 2.11 ± 0.12 Mm with the Kitt Peak data, and 1.74 ± 0.05 Mm with the Sacramento Peak data. The Kitt Peak data show (1) within the measurement error there is no significant difference in the height or thickness of the emission shell in coronal holes compared with the quiet Sun, (2) the 1083 nm emission intensity drops by 50% in coronal holes, (3) the line width decreases by about 2 km s-1 in coronal holes (suggesting less inclined spicules), (4) the line width of the He I 1083 nm line jumps significantly as the line of sight crosses the solar limb (consistent with a higher temperature upper shell), (5) a quiescent prominence shows a smaller spectral line width (consistent with a cooler temperature or less velocity broadening), and (6) the entire emission shell and the prominence show a He I spectral component ratio of about 8 (suggesting optically thin emission). Title: He i 10830 Angstrom Wing Asymmetry in Polar Coronal Holes: Evidence for Radial Outflows Authors: Dupree, A. K.; Penn, M. J.; Jones, H. P. Bibcode: 1996ApJ...467L.121D Altcode: Imaging spectroscopy of the Sun, carried out across the the solar poles, yielded several thousand profiles of the He I 10830 A chromospheric absorption line with effective spatial pixels of 1.1 x 2 arcsec2. Profiles of He I 10830 A show the relative blue-wing absorption is stronger in the coronal holes than in the quiet Sun, creating an asymmetric profile indicative of mass outflow. Within the coronal holes, blueshifted line wings are found where He I absorption is weak, corresponding to the center of supergranular cells. However, in the quiet Sun, there is no line wing shift in supergranular centers. Spatially compact regions of strong red-wing absorption also occur across the disk. Within the polar coronal holes, the amplitude of the wing shift shows a linear dependence with cos theta (where the angle theta is measured with respect to an outward normal to the Sun's surface), suggesting that a radial outflow occurs with a characteristic speed of ~8 km s-1. These observations represent the first detection of systematic outflows near the chromosphere transition region interface that appear to mark the origin of the high-speed wind acceleration from the solar surface. Title: GONG Observations of Solar Surface Flows Authors: Hathaway, D. H.; Gilman, P. A.; Harvey, J. W.; Hill, F.; Howard, R. F.; Jones, H. P.; Kasher, J. C.; Leibacher, J. W.; Pintar, J. A.; Simon, G. W. Bibcode: 1996Sci...272.1306H Altcode: Doppler velocity observations obtained by the Global Oscillation Network Group (GONG) instruments directly measure the nearly steady flows in the solar photosphere. The sun's differential rotation is accurately determined from single observations. The rotation profile with respect to latitude agrees well with previous measures, but it also shows a slight north-south asymmetry. Rotation profiles averaged over 27-day rotations of the sun reveal the torsional oscillation signal-weak, jetlike features, with amplitudes of 5 meters per second, that are associated with the sunspot latitude activity belts. A meridional circulation with a poleward flow of about 20 meters per second is also evident. Several characteristics of the surface flows suggest the presence of large convection cells. Title: Limb Observations of He I 1083nm Authors: Penn, M.; Jones, H. Bibcode: 1996AAS...188.7906P Altcode: 1996BAAS...28..956P Imaging spectroscopic data of the He I 1083 nm limb emission were taken on several dates in Oct and Nov 1995 with the NASA/NSO Spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope and on 09 Dec 1993 with the Michigan Infrared Camera at the NSO/Sac Peak Vacuum Tower Telescope. Emission line profiles were observed in quiet Sun and coronal hole locations on the northern and southern solar poles and on the east solar limb. The height of the He I 1083 nm shell above the continuum limb at 1083 nm was measured to be 2.11+/-0.12 Mm with the Kitt Peak data, and 1.74+/-0.05 Mm with the Sac Peak data. The Kitt Peak data show (1) within the measurement error there is no significant difference in the height or thickness of the emission shell in coronal holes compared with the quiet Sun, (2) the 1083 nm emission intensity drops by 50% in coronal holes, (3) the line width decreases by about 2 km s(-1) in coronal holes (suggesting less inclined spicules), (4) the line width of the He I 1083 nm line jumps significantly as the line-of-sight crosses the solar limb (consistent with a higher temperature upper shell), (5) a quiescent prominence shows a smaller spectral line width (consistent with a cooler temperature or less velocity broadening), and (6) the entire emission shell and the prominence show a He I spectral component ratio of about 8 (suggesting optically thin emission). Title: GONG Observations of Solar Surface Flows Authors: Hathaway, D. H.; Gilman, P. A.; Jones, H. P.; Kasher, J.; Simon, G. W.; GONG Nearly Steady Flows Team; GONG Magnetic Fields Team Bibcode: 1996AAS...188.5304H Altcode: 1996BAAS...28..903H Doppler velocity observations obtained by the GONG instruments directly measure the nearly steady flows in the solar photosphere. The Sun's differential rotation profile is accurately determined from single observations. This profile is well represented by a fourth order polynomial which includes a rapidly rotating equator and a slight north-south asymmetry. Rotation profiles averaged over 27 day rotations of the Sun are sufficient to reveal the torsional oscillation signal - weak, 5 m/s, jet-like features associated with the sunspot latitude activity belts. A meridional circulation with poleward flow of about 20 m/s is also found from single observations and its spatial structure is well determined. Several of the observed characteristics of the surface flows suggest the presence of large convection cells. The convection spectrum is measured and found to have peak power for cells with wavelengths of about 50,000 km but the spectrum extends to much larger wavelengths. Day-to-day variations in the observed structure of the differential rotation and meridional circulation profiles indicate the presence of large-scale, nonaxisymmetric velocity signals which may be of solar origin. Studies correlating the convective flow patterns on consecutive days also indicate the presence of large cellular patterns that rotate at the Sun's rotation rate. Title: Solar-Cycle Variation of Polarity Inversion Authors: Jones, H. P. Bibcode: 1996AAS...188.3505J Altcode: 1996BAAS...28..871J Multi-scale polarity inversion maps are constructed from National Solar Observatory/Kitt Peak magnetograms for periods coinciding with those used by Harvey (1993, PhD Thesis, Utrecht University). The motivation for this analysis stems from earlier work on a small sample which suggested that neutral-line "length" varies as a power of the scale used to determine the polarity inversion loci and that only the amplitude, not the exponent, varies between maximum and minimum phases of the solar cycle. Harvey observed similar behavior in the areal distribution of new bipolar regions, and a plausible hypothesis is that neutral line length vs. scale is a mapping of this areal distribution, i.e., an efficient way to count bipoles. Broadly speaking, the behavior of neutral line length vs. scale is confirmed from this more extensive sample; the curves from many days at either minimum or maximum are tightly clustered and are nearly parallel on log-log plots. Empirically, if one represents the areal distribution of new bipolar regions as a function of time and area as n(t,A) \sim f(t)g(A), then neutral-line length, l, varies with scale, s, as \ell(s) \sim const*[g(s2)/f(t)]r where r =~ 0.2. To explore whether this relation has more than emperical significance, future work is planned to compute neutral line maps from synthesized magnetograms based on the superposition of known, prespecified distributions of dipoles. Title: The Solar Acoustic Spectrum and Eigenmode Parameters Authors: Hill, F.; Stark, P. B.; Stebbins, R. T.; Anderson, E. R.; Antia, H. M.; Brown, T. M.; Duvall, T. L., Jr.; Haber, D. A.; Harvey, J. W.; Hathaway, D. H.; Howe, R.; Hubbard, R. P.; Jones, H. P.; Kennedy, J. R.; Korzennik, S. G.; Kosovichev, A. G.; Leibacher, J. W.; Libbrecht, K. G.; Pintar, J. A.; Rhodes, E. J., Jr.; Schou, J.; Thompson, M. J.; Tomczyk, S.; Toner, C. G.; Toussaint, R.; Williams, W. E. Bibcode: 1996Sci...272.1292H Altcode: The Global Oscillation Network Group (GONG) project estimates the frequencies, amplitudes, and linewidths of more than 250,000 acoustic resonances of the sun from data sets lasting 36 days. The frequency resolution of a single data set is 0.321 microhertz. For frequencies averaged over the azimuthal order m, the median formal error is 0.044 microhertz, and the associated median fractional error is 1.6 x 10-5. For a 3-year data set, the fractional error is expected to be 3 x 10-6. The GONG m-averaged frequency measurements differ from other helioseismic data sets by 0.03 to 0.08 microhertz. The differences arise from a combination of systematic errors, random errors, and possible changes in solar structure. Title: Infrared and optical studies of cool low-mass dwarfs Authors: Jones, H. Bibcode: 1996Obs...116...62J Altcode: No abstract at ADS Title: Comparison and Relation of HeI 1083 NM Two-Ribbon Flares and Large-Scale Coronal Arcades Observed by YOHKOH Authors: Harvey, Karen L.; McAllister, Alan; Hudson, Hugh; Alexander, David; Lemen, James R.; Jones, Harrison P. Bibcode: 1996ASPC...95..100H Altcode: 1996sdit.conf..100H No abstract at ADS Title: The distribution of cold dust within the Galaxy Authors: Davies, J. I.; Trewhella, M.; Jones, H. Bibcode: 1996ASSL..209..525D Altcode: 1996nepn.conf..525D No abstract at ADS Title: Observations of a Quiescent Prominence Straddling the Solar Limb during the Total Eclipse of 11 July 1991 Authors: Gaizauskas, V.; Deluca, E.; Golub, L.; Jones, H. P.; November, L. Bibcode: 1996mpsa.conf..491G Altcode: 1996IAUCo.153..491G No abstract at ADS Title: Helium in the Spectrum of the Sun and of Solar-Type Stars Authors: Andretta, V.; Giampapa, M. S.; Jones, H. P. Bibcode: 1995IrAJ...22..177A Altcode: We present results from detailed non-LTE radiative transfer calculations of the He I spectrum in the Sun. Using an extended grid of model chromospheres, we explore the relative importance of, respectively, the coronal XUV illumination and the thermal structure of the lower transition region. With reference to the He I lambda 587.6 and lambda 1083.0 triplet lines, we point out some implications for the study of activity in solar-type stars. Title: Tracking Magnetogram Proper Motions by Multiscale Regularization Authors: Jones, H. P. Bibcode: 1995ESASP.376b.227J Altcode: 1995help.confP.227J; 1995soho....2..227J No abstract at ADS Title: The dependence of disc galaxy properties on viewing angle: simulating the observations Authors: Davies, J. I.; Jones, H.; Trewhella, M. Bibcode: 1995MNRAS.273..699D Altcode: Recent inclination-dependent tests have indicated that galaxies may have high optical opacities at large distances from their centres. These results are difficult to reconcile with other measures of opacity that indicate very much lower values. In this paper we specifically consider work by Burstein, Haynes & Faber, to see if their result with regard to high opacities at large galactic distances is the correct interpretation of the data used. We start by constructing simulated samples of both optically thick and optically thin galaxies and show that they are in excellent correspondence with the observational data used by Burstein et al. The Burstein et al. method does appear to have overcome many of the selection effects inherent in other surface brightness inclination tests. The problem is that they now appear to have introduced yet another selection effect by requiring that all of the galaxies in their sample need a distance estimate. The redshift cut-off of their data renders their distance-based test totally inconclusive with regard to the opacity of galactic discs. Title: A Multiple Scale View of Magnetic Polarity Inversion Authors: Jones, Harrison P. Bibcode: 1995SPD....26.1010J Altcode: 1995BAAS...27..979J No abstract at ADS Title: Working Group 7 - Surface Flows and Feature Tracking Authors: Hathaway, D.; Hurlburt, N.; Jones, H.; Simon, G. Bibcode: 1995ESASP.376a.205H Altcode: 1995heli.conf..205H No abstract at ADS Title: The distribution of galactic inclinations. Authors: Jones, H.; Davies, J.; Trewhella, M. Bibcode: 1995ASIC..469..115J Altcode: 1995osd..conf..115J No abstract at ADS Title: The NSO/NASA He I 1083.0 nm Video Filtergraph/Magnetograph Authors: Jones, H. P.; Harvey, J. W. Bibcode: 1995itsa.conf...97J Altcode: No abstract at ADS Title: Why a distance selection effect invalidates the Burstein, Haynes and Faber opacity test. Authors: Davies, J.; Jones, H.; Trewhella, M. Bibcode: 1995ASIC..469...85D Altcode: 1995osd..conf...85D No abstract at ADS Title: Opacity from luminosity functions. Authors: Trewhella, M.; Davies, J.; Disney, M.; Jones, H. Bibcode: 1995ASIC..469..293T Altcode: 1995osd..conf..293T No abstract at ADS Title: Preliminary Comparison of NASA/NSO Spectromagnetograph Observations with Solar Irradiance Authors: Jones, H. P.; Wills, M. J. Bibcode: 1994AAS...185.4409J Altcode: 1994BAAS...26.1378J The NASA/NSO Spectromagnetograph (SPM) at the National Solar Observatory/Kitt Peak Vacuum Telescope has obtained diachronic, full-disk images of the Sun in photospheric magnetic flux, line-of-sight velocity, continuum intensity, equivalent width, and central line depth from 21 Apr 92 to 19 Nov 92 in Fe I 550.7 nm and from 21 Nov 92 to date in Fe I 868.8 nm. The five daily images are formed from on-line analysis of spatially and spectrally resolved line profiles obtained by scanning the solar image across a long-slit spectrograph and are thus strictly simultaneous and cospatial. We discuss a set of curve-fitting procedures for measuring and removing center-to-limb variations, systematic instrumental effects, and terrestrial atmospheric variations with which we have reduced six months of data from 12 Aug 92 to 3 Feb 93. One major purpose of this analysis is to explore how the spatial structures in the SPM diachronic data relate to variations in total solar irradiance. To reduce the data volume (each day's observation is 32 Mbytes) while retaining flexibility to explore a wide variety of possible criteria for classification of features, we have prepared pairs of 2-D histograms comparing each of the four other variables to magnetic flux as well as coarse but strategically binned 5-D histograms. We compare summary statistics based on preliminary feature classification with solar irradiance data obtained over the same period. Title: Bright Rims Adjacent to a Quiescent Hα Filament Authors: Gaizauskas, V.; de Luca, E.; Golub, L.; Jones, H. P. Bibcode: 1994AAS...18512304G Altcode: 1994BAAS...26.1522G Recent models of filament-formation invoke reconnection between small-scale magnetic elements adjacent to the polarity inversion line separating large areas of unipolar magnetic fields. In an attempt to confirm this process, we examine joint observations of a quiescent filament straddling the SW limb of the Sun during the total solar eclipse of 1991 July 11. We test a hypothesis that a signature of the reconnection process might be carried by the prominent bright rims beside or enclosed between curved feet, or 'barbs', which connect the body of the Hα filament to structures near the base of the atmosphere. We spatially register digitized Hα (ORSO) images of the filament with coronal (NIXT) images and with photospheric magnetograms (NSO/KP) to a precision of +/- 2". Our findings relate to five rims, elongated bright patches in Hα with a maximum length of 20". We find a better spatial association of the rims with bipolar magnetic elements (4/5) than with small patches of weakly enhanced soft X-rays (2/4). We point out that projection effects at these extreme limb positions could alter these associations. We conclude from these limited 'snapshot' observations that we are not yet able to decide whether or not bright rims on quiescent prominences are locations of magnetic reconnection on a small scale. Because reconnection is highly dynamic, compelling evidence for or against this process will have to await prolonged observations at multiple wavelengths in X-rays of a single filament at high spatial and temporal resolution, such as those envisaged for the Transition Region and Coronal Explorer (TRACE). Title: Joint observations of the chromosphere, transition region, and corona from SOHO and NSO/Kitt Peak Authors: Jones, H. P.; Harvey, John W.; Andretta, Vincenzo Bibcode: 1994ESASP.373..345J Altcode: 1994soho....3..345J No abstract at ADS Title: The Global Oscillation Network Group Site Survey - Part Two Authors: Hill, Frank; Fischer, George; Forgach, Suzanne; Grier, Jennifer; Leibacher, John W.; Jones, Harrison P.; Jones, Patricia B.; Kupke, Renate; Stebbins, Robin T.; Clay, Donald W.; Ingram, Robert E. L.; Libbrecht, Kenneth G.; Zirin, Harold; Ulrichi, Roger K.; Websteri, Lawrence; Hieda, Lester S.; Labonte, Barry J.; Lu, Wayne M. T.; Sousa, Edwin M.; Garcia, Charles J.; Yasukawa, Eric A.; Kennewell, John A.; Cole, David G.; Zhen, Huang; Su-Min, Xiao; Bhatnagar, Arvind; Ambastha, Aashok; Al-Khashlan, Abdulrahman Sa'ad; Abdul-Samad, Muhammad-Saleh; Benkhaldoun, Zouhair; Kadiri, Samir; Sánchez, Francisco; Pallé, Pere L.; Duhalde, Oscar; Solis, Hernan; Saá, Oscar; González, Ricardo Bibcode: 1994SoPh..152..351H Altcode: The Global Oscillation Network Group (GONG) Project will place a network of instruments around the world to observe solar oscillations as continuously as possible for three years. The Project has now chosen the six network sites based on analysis of survey data from fifteen sites around the world. The chosen sites are: Big Bear Solar Observatory, California; Mauna Loa Solar Observatory, Hawaii; Learmonth Solar Observatory, Australia; Udaipur Solar Observatory, India; Observatorio del Teide, Tenerife; and Cerro Tololo Interamerican Observatory, Chile. Title: Flow Patterns in Active Regions Authors: Jones, Harrison P. Bibcode: 1994ASPC...68..286J Altcode: 1994sare.conf..286J No abstract at ADS Title: Interpreting Recent Observations of He 110830 Angstrom Authors: Jones, H. P. Bibcode: 1994IAUS..154...49J Altcode: 1994IAUS..154..498J No abstract at ADS Title: Zodiacal Light and Ancient Symbolism Authors: Jones, H. Bibcode: 1993JBAA..103..283J Altcode: No abstract at ADS Title: Contrast of faculae near the disk center and solar variability Authors: Lawrence, J. K.; Topka, K. P.; Jones, H. P. Bibcode: 1993JGR....9818911L Altcode: We analyze simultaneous, or near-simultaneous, coregistered, digital, photometric images of solar photospheric intensity and line-of-sight magnetic field. Images were made with the Lockheed tunable filter instrument at the Swedish Solar Observatory, La Palma, with the video spectra-spectroheliograph system at the San Fernando Observatory and with the new NASA spectromagnetograph at the National Solar Observatory at Kitt Peak. We study the disk center contrasts of small magnetic elements. While active region faculae are dark at disk center quiet Sun network features are bright. The populations of magnetic field elements that make up these two kinds of are quite different. Different contrast center-limb functions must be used when estimating their irradiance or luminosity contributions. The disk center contrasts of active region faculae are color dependent and indicate a depth effect related to the H- opacity of the facular atmosphere. This result is important for calibration of monochromatic observations of faculae to bolometric irradiance fluctuations. We emphasize the value of cooperative observations among installations whose differing strengths are complementary. Title: Correlation of He II lyman alpha with He I 10830 Å, and with chromospheric and EUV coronal emission Authors: Thompson, W. T.; Neupert, W. M.; Jordan, S. D.; Jones, H.; Thomas, R. J.; Schmieder, B. Bibcode: 1993SoPh..147...29T Altcode: This paper describes the results of comparing SERTS-3 images obtained in the transition region line of HeII 304 å with chromospheric HeI 10830 å absorption, with strong coronal lines of MgIX 368 å, FeXV 284 å and 417 å, and FeXVI 335 å and 31 å, with Hα, with CaII 8542 å, and with magnetograms in FeI 8688Hα. All of the images are illustrated, and the image reconstruction techniques used are described and evaluated. The high correlation of the HeII 304 å and HeI 10830 å images, originally found by Harvey and Sheeley (1977), is confirmed and is put on a quantitative basis. We find that the supergranulation network has greater contrast, and that filaments appear darker, in 10830 å than in 304 å. In active regions, the 304 å line follows more closely the behavior of Hα and CaII 8542 å than the 10830 å line. Title: Simultaneous Observations of Solar Plage with the Solar Extreme Ultraviolet Rocket Telescope and Spectrograph (SERTS), the VLA, and the Kitt Peak Magnetograph Authors: Brosius, Jeffrey W.; Davila, Joseph M.; Thompson, William T.; Thomas, Roger J.; Holman, Gordon D.; Gopalswamy, N.; White, Stephen M.; Kundu, Mukul R.; Jones, Harrison P. Bibcode: 1993ApJ...411..410B Altcode: We obtained simultaneous images of solar plage on 1991, May 7 with SERTS, the VLA,4 and the NASA/National Solar Observatory spectromagnetograph at the NSO/Kitt Peak Vacuum Telescope. Using intensity ratios of Fe XVI to Fe XV emission lines, we find that the coronal plasma temperature is (2.3-2.9) x 10 exp 6 K throughout the region. The column emission measure ranges from 2.5 x 10 exp 27 to l.3 x 10 exp 28 cm exp -5. The calculated structure and intensity of the 20 cm wavelength thermal bremsstrahlung emission from the hot plasma observed by SERTS is quite similar to the observed structure and intensity of the 20 cm microwave emission observed by the VLA. Using the Meyer (1991, 1992) revised coronal iron abundance, we find no evidence either for cool absorbing plasma or for contributions from thermal gyroemission. Using the observed microwave polarization and the SERTS plasma parameters, we calculate a map of the coronal longitudinal magnetic field. The resulting values, about 30-60 G, are comparable to extrapolated values of the potential field at heights of 5000 and 10,000 km. Title: Planets and Symbolism Authors: Jones, H. Bibcode: 1993JBAA..103..109J Altcode: No abstract at ADS Title: A Magnetograph Comparison Workshop Authors: Jones, H.; Bogart, R.; Canfield, R.; Chapman, G.; Henney, C.; Kopp, G.; Lites, B.; Mickey, D.; Montgomery, R.; Pillet, V.; Rabin, D.; Ulrich, R.; Walton, S. Bibcode: 1993BAAS...25.1216J Altcode: No abstract at ADS Title: Solar Coronal Plasma and Magnetic Field Diagnostics Using SERTS and Coordinated VLA Observations Authors: Brosius, J. W.; Davila, J. M.; Thompson, W. T.; Thomas, R. J.; Holman, G. D.; Gopalswamy, N.; White, S. M.; Kundu, M. R.; Jones, H. P. Bibcode: 1993BAAS...25.1224B Altcode: No abstract at ADS Title: Intercomparison of Seven Magnetographs Authors: Walton, S. R.; Bogart, R. S.; Chapman, G. A.; Henney, C.; Jones, H.; Kopp, G.; Lites, B.; Mickey, D.; Montgomery, R.; Pillet, V.; Rabin, D. Bibcode: 1993BAAS...25.1205W Altcode: No abstract at ADS Title: Analysis of EUV, Microwave and Magnetic Field Observations of Solar Plage Authors: Brosius, J. W.; Davila, J. M.; Jones, H. P.; Thompson, W. T.; Thomas, R. J.; Holman, G. D.; White, S. W.; Gopalswamy, N.; Kundu, M. R. Bibcode: 1993ASPC...46..291B Altcode: 1993mvfs.conf..291B; 1993IAUCo.141..291B No abstract at ADS Title: Spectrometer-Based Magnetographs (Invited) Authors: Jones, H. Bibcode: 1993ASPC...46..156J Altcode: 1993mvfs.conf..156J; 1993IAUCo.141..156J No abstract at ADS Title: Comparison of Magnetograms by Histogram Equating Authors: Jones, H. P. Bibcode: 1992AAS...181.8105J Altcode: 1992BAAS...24.1252J No abstract at ADS Title: The NASA/NSO Spectromagnetograph Authors: Jones, Harrison P.; Duvall, Thomas L., Jr.; Harvey, John W.; Mahaffey, Charles T.; Schwitters, Jan D.; Simmons, Jorge E. Bibcode: 1992SoPh..139..211J Altcode: The NASA/NSO Spectromagnetograph is a new focal plane instrument for the National Solar Observatory/Kitt Peak Vacuum Telescope which features real-time digital analysis of long-slit spectra formed on a two-dimensional CCD detector. The instrument is placed at an exit port of a Littrow spectrograph and uses an existing modulator of circular polarization. The new instrument replaces the 512-channel Diode Array Magnetograph first used in 1973. Commercial video processing boards are used to digitize the spectral images at video rates and to separate, accumulate, and buffer the spectra in the two polarization states. An attached processor removes fixed-pattern bias and gain from the spectra in cadence with spatial scanning of the image across the entrance slit. The data control computer performs position and width analysis of the line profiles as they are acquired and records line-of-sight magnetic field, Doppler shift, and other computed parameters. The observer controls the instrument through windowed processes on a data control console using a keyboard and mouse. Early observations made with the spectromagnetograph are presented and plans for future development are discussed. Title: Analysis of EUV, Microwave, and Magnetic Field Observations of a Solar Active Region Authors: Brosius, J. W.; Davila, J. M.; Jones, H. P.; Thompson, W. T.; White, S. M.; Gopalswamy, N.; Kundu, M. R. Bibcode: 1992AAS...180.4002B Altcode: 1992BAAS...24R.792B No abstract at ADS Title: Calibrating the NASA/NSO Spectromagnetograph Authors: Jones, H. P. Bibcode: 1992AAS...180.5107J Altcode: 1992BAAS...24..814J No abstract at ADS Title: New Solar Cycle Data from the NASA/NSO Spectromagnetograph Authors: Jones, Harrison P. Bibcode: 1992ASPC...27..315J Altcode: 1992socy.work..315J No abstract at ADS Title: Simultaneous EUV, Microwave, and Magnetic Field Observations of Solar Active Regions Authors: Brosius, J. W.; Davila, J. M.; Thompson, W. T.; Gopalswamy, N.; White, S. M.; Jones, H. P.; Metcalf, T. R. Bibcode: 1991BAAS...23.1388B Altcode: No abstract at ADS Title: Comparison of SERTS Spectroheliograms with Ground-Based Observations Authors: Thompson, W. T.; Neupert, W. M.; Brosius, J. W.; Jones, H. P.; Schmieder, B. Bibcode: 1991BAAS...23R1061T Altcode: No abstract at ADS Title: The Bartol/NASA/NSO High-Degree Helioseismometer Authors: Harvey, J.; Hill, F.; Duvall, T., Jr.; Jones, H.; Jefferies, S.; Pomerantz, M. Bibcode: 1991BAAS...23.1032H Altcode: No abstract at ADS Title: Spatial Correlation of Spectrum Line Properties with Magnetic Flux Authors: Jones, H. P. Bibcode: 1991BAAS...23.1068J Altcode: No abstract at ADS Title: First Magnetograms from the NASA/NSO Spectromagnetograph Authors: Jones, H. P.; Duvall, T. L., Jr.; Mahaffey, C. T. Bibcode: 1990BAAS...22..809J Altcode: No abstract at ADS Title: High-Resolution Magnetograph for the Southwest Solar Facility Authors: Jones, Harrison Bibcode: 1990rete.conf...36J Altcode: No abstract at ADS Title: Formation of fourier phase shifts in the solar Ni i 6768 Å line Authors: Jones, Harrison P. Bibcode: 1989SoPh..120..211J Altcode: A formalism is developed to understand better how Doppler shifts of spectrum lines as inferred from phase shifts in the Fourier transforms of line profiles are related to the underlying velocity structures which they are intended to measure. With a standard model atmosphere and a simplified, quasi-LTE treatment of line formation, the formalism is applied to the NiI 6768 Å line which has been selected for use with a network of imaging interferometers under development by the Global Oscillations Network Group (GONG) for research in helioseismology. Fourier phase shifts are found to be a remarkably linear measure of velocity even in the presence of gradients and unresolved lateral variations in the assumed velocity field. An assumed outward increase in amplitude of a model oscillatory velocity is noticeably reflected in the center-to-limb behavior of the simulated velocity measure, and a sample model of solar granulation is found to have a strong influence on the formation of the Fourier phase. Title: Digitizing Video Spectra at the NASA/NSO Spectromagnetograph Authors: Jones, H. P.; Brodzik, D.; Duvall, T. L., Jr. Bibcode: 1989BAAS...21..852J Altcode: No abstract at ADS Title: Magnetograph Observations During the International Solar Month Authors: Jones, H. P. Bibcode: 1989BAAS...21..862J Altcode: No abstract at ADS Title: Preflare activity. Authors: Priest, E. R.; Gaizauskas, V.; Hagyard, M. J.; Schmahl, E. J.; Webb, D. F.; Cargill, P.; Forbes, T. G.; Hood, A. W.; Steinolfson, R. S.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.; Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmieder, B.; Smith, J. B., Jr.; Toomre, J.; Woodgate, B.; Waggett, P.; Bentley, R.; Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.; Martens, P. Bibcode: 1989epos.conf....1P Altcode: Contents: 1. Introduction. 2. Magnetohydrodynamic instability. 3. Preflare magnetic and velocity fields. 4. Coronal manifestations of preflare activity. Title: Magnetograph group summary Authors: Jones, Harrison P. Bibcode: 1989dots.work...17J Altcode: The Magnetograph Group focussed on the techniques and many practical problems of interleaving ground-based measurements of magnetic fields from diverse sites and instruments to address the original scientific objectives. The predominant view of the discussion group was that present instrumentation and analysis resources do not warrant immediate, specific plans for further worldwide campaigns of cooperative magnetograph observing. The several reasons for this view, together with many caveats, qualifications, and suggestions for future work are presented. Title: The GONG data reduction and analysis system. Authors: Pintar, J. A.; Andersen, B.; Anderson, E. R.; Armet, D. B.; Brown, T. M.; Hathaway, D. H.; Hill, F.; Jones, H. P.; GONG Data Team Bibcode: 1988ESASP.286..217P Altcode: Each of the six GONG observing stations will produce three, 16-bit, 256×256 images of the Sun every 60 seconds of sunlight. These data will be transferred from the observing sites to the GONG Data Management and Analysis Center (DMAC), in Tucson, on high-density tapes at a combined rate of over 1 gigabyte per day. The contemporaneous processing of these data will produce several standard data products and will require a sustained throughput in excess of 7 megaflops. Peak rates may exceed 50 megaflops. Archives will accumulate at the rate of approximately 1 terabyte per year, reaching nearly 3 terabytes in three years of observing. Researchers will access the data products with a machine-independent GONG Reduction and Analysis Software Package (GRASP). Based on the Image Reduction and Analysis Facility (IRAF), this package will include database facilities and helioseismic analysis tools. Users may access the data as visitors in Tucson, or may access DMAC remotely through networks, or may process subsets of the data at their local institutions using GRASP or other systems of their choice. Elements of the system will reach the prototype stage by the end of 1988. Full operation is expected in 1992 when data acquisition begins. Title: The GONG site survey. Authors: Hill, F.; Ambastha, A.; Ball, W.; Duhalde, O.; Farris, D.; Fischer, G.; Hieda, L.; Zhen, Huang; Ingram, B.; Jackson, P.; Jones, H.; Jones, W.; Kennewell, J.; Kunkel, W.; Kupke, R.; Labonte, B.; Leibacher, J.; Libbrecht, K.; Lu, W.; Morrison, L.; Odell, C.; Pallé, P.; Saá, O.; Sousa, E.; Stebbins, T.; Xiao, Suming; GONG Site Survey Team Bibcode: 1988ESASP.286..209H Altcode: The Global Oscillation Network Group (GONG) project is planning to place six observing stations around the world to observe the solar oscillations as continuously as possible. This paper describes the procedures that are being used to select the six sites. The latest results of measurements of cloud cover obtained by networks of 6 (out of 10) radiometers show a duty cycle of over 93%, with the first diurnal sidelobe in the window power spectrum suppressed by a factor of 400. The results are in good agreement with the predictions of a computer model of the expected cloud cover at individual sites. Title: Experimental constraints on heating and cooling rates of refractory inclusions in the early solar system Authors: Boynton, W. V.; Drake; Hildebrand; Jones; Lewis; Treiman; Wark Bibcode: 1987eprs.nasaQ....B Altcode: The refractory inclusions in carbonaceous chondrites were the subject of considerable interest since their discovery. These inclusions contain minerals that are predicted to be some of the earliest condensates from the solar nebula, and contain a plethora of isotopic anomalies of unknown origin. Of particular interest are those coarse-grained inclusions that contain refractory metal particles (Fe, Ni, Pt, Ru, Os Ir). Experimental studies of these inclusions in terrestrial laboratories are, however, complicated because the dense particles tend to settle out of a molten or partially molten silicate material. Heating experiments in the Space Station technology and microgravity in order to observe the effects of metal nuggets (which may act as heterogeneous nucleation sites) on nucleation rates in silicate systems and to measure simultaneously the relative volatilization rate of siderophile and lithophile species. Neither experiment is possible in the terrestrial environment. Title: Experimental constraints on the origin of chondrules Authors: Boynton, W. V.; Drake; Hildebrand; Jones; Lewis; Treiman; Wark Bibcode: 1987eprs.nasaR....B Altcode: Chrondule formation was an important (perhaps ubiguitous) process in the early solar system, yet their origins remain elusive. Some points, however, are clear. The precursor material of chondules (dust) was rapidly heated at rates of perhaps thousands of degrees per second and was cooled more slowly. It was proposed to investigate chondrule formation in the Space Station environment via a dust-box (a chamber in which dust can be suspended, heated, and cooled. A microgravity environment is conducive to this kind of experiment because of the significant retardation of settling rates compared with a terrestrial laboratory environment. These long-duration experiments might require the development of technologies to counteract even the small, but finite and permanent gravitation field of the Space Station. Simple, but interesting experiments on dust suspensions immediately present themselves. Title: "Underluminous" Lyman-alpha Emission Associated with Active-Region Magnetic Canopy Authors: Jones, H. P.; Skumanich, A.; Lemaire, P. Bibcode: 1987BAAS...19..930J Altcode: No abstract at ADS Title: The NSO/NASA CCD Spectromagnetograph Authors: Jones, H. P. Bibcode: 1987BAAS...19..929J Altcode: No abstract at ADS Title: Preflare magnetic and velocity fields Authors: Hagyard, M. J.; Gaizauskas, V.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.; Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmeider, B. Bibcode: 1986epos.conf.1.16H Altcode: 1986epos.confA..16H A characterization is given of the preflare magnetic field, using theoretical models of force free fields together with observed field structure to determine the general morphology. Direct observational evidence for sheared magnetic fields is presented. The role of this magnetic shear in the flare process is considered within the context of a MHD model that describes the buildup of magnetic energy, and the concept of a critical value of shear is explored. The related subject of electric currents in the preflare state is discussed next, with emphasis on new insights provided by direct calculations of the vertical electric current density from vector magnetograph data and on the role of these currents in producing preflare brightenings. Results from investigations concerning velocity fields in flaring active regions, describing observations and analyses of preflare ejecta, sheared velocities, and vortical motions near flaring sites are given. This is followed by a critical review of prevalent concepts concerning the association of flux emergence with flares Title: Magnetic Shear. III. Hale Region 17255 Authors: Athay, R. G.; Jones, H. P.; Zirin, H. Bibcode: 1986ApJ...303..877A Altcode: Hale active region 17255, which in many respects was the most vigorous active region observed during the first operational period of SMM, appears to lie between two large areas of flow (observed in C IV) converging toward the major axis of the region. In the 6-day period from November 6-12, 1980, the major axis of the region rotates by about 25 deg. Several segments of the magnetic neutral line show C IV flow velocities of opposite sign on either side of the neutral line. Those segments whose orientation is favorable for measuring velocity components parallel to the neutral line show evidence that such flow is present, which is interpreted as evidence for magnetic shear. This, together with other evidence, suggests that magnetic shear is widespread in this region, as in the two previous regions studied. It is concluded that magnetic shear is often associated with flaring activity but is not a sufficient condition for flaring to occur. Title: Magnetic Shear. IV. Hale Regions 16740, 16815, and 16850 Authors: Athay, R. G.; Klimchuk, J. A.; Jones, H. P.; Zirin, H. Bibcode: 1986ApJ...303..884A Altcode: Dopplergrams made in C IV 1548 A are studied for evidence of velocity shear near H-alpha dark filaments and for large-scale flow convergent on active regions. The three regions studied support earlier conclusions that shear is a common property of active regions and that active regions may be the foci of converging plasma flow. Flow patterns near filaments show divergence or convergence as well as shear. Also the sense of the shear can be either cyclonic or anticyclonic. No preference is noted for convergence or divergence or for a particular sense of shear, and there appears to be no correlation between the sense of the shear and the sign of the velocity gradient normal to the filament. The close association of H-alpha dark filaments with shear lines leads to the suggestion that the filaments may arise from a cooling instability induced by the Bernoulli effect. Title: Preflare activity. Authors: Priest, E. R.; Gaizauskas, V.; Hagyard, M. J.; Schmahl, E. J.; Webb, D. F.; Cargill, P.; Forbes, T. G.; Hood, A. W.; Steinolfson, R. S.; Chapman, G. A.; Deloach, A. C.; Gary, G. A.; Jones, H. P.; Karpen, J. T.; Martres, M. -J.; Porter, J. G.; Schmieder, B.; Smith, J. B., Jr.; Toomre, J.; Woodgate, B.; Waggett, P.; Bentley, R.; Hurford, G.; Schadee, A.; Schrijver, J.; Harrison, R.; Martens, P. Bibcode: 1986NASCP2439....1P Altcode: Contents: 1. Introduction: the preflare state - a review of previous results. 2. Magnetohydrodynamic instability: magnetic reconnection, nonlinear tearing, nonlinear reconnection experiments, emerging flux and moving satellite sunspots, main phase reconnection in two-ribbon flares, magnetic instability responsible for filament eruption in two-ribbon flares. 3. Preflare magnetic and velocity fields: general morphology of the preflare magnetic field, magnetic field shear, electric currents in the preflare active region, characterization of the preflare velocity field, emerging flux. 4. Coronal manifestations of preflare activity: defining the preflare regime, specific illustrative events, comparison of preflare X-rays and ultraviolet, preflare microwave intensity and polarization changes, non-thermal precursors, precursors of coronal mass ejections, short-lived and long-lived HXIS sources as possible precursors. Title: The Interpretation of Spectrum Lines Formed in Small Solar Structures Authors: Jones, H. P. Bibcode: 1986ssmf.conf..127J Altcode: The author reviews some important aspects of radiative transfer bearing on the interpretation of high-resolution solar data. Recent developments in techniques for solving transfer problems were discussed along with some known effects of lateral radiative exchange such as thermal smoothing and channeling. Also discussed were the effects of non-uniform fields which must occur along the lines of sight which traverse small solar flux concentrations. Title: Erratum - a Study of Flare Buildup from Simultaneous Observations in Microwave Hα and Ultraviolet Wavelengths Authors: Kundu, M. R.; Gaizauskas, V.; Woodgate, B. E.; Schmahl, E. J.; Shine, R.; Jones, H. P. Bibcode: 1985ApJS...58..195K Altcode: No abstract at ADS Title: Magnetic shear. II - Hale region 17244 Authors: Athay, R. G.; Jones, H. P.; Zirin, H. Bibcode: 1985ApJ...291..344A Altcode: A B-gamma(delta) sunspot group with growing delta-spots of trailing polarity shows evidence in H-alpha filament structure of a transition from a state of weak magnetic shear to a state of strong shear. The shear develops in the chromosphere and transition region to the corona overlying the photospheric magnetic neutral line separating the delta-spots from the leading polarity at a time when the delta-spots are undergoing rapid growth. Several major flares occur along the sheared portion of the neutral line following the shear development. Other segments of the neutral line far removed from the delta-spots show similar evidence of shear in the H-alpha filament structure and in C IV velocity patterns as well. These 'quiescent' regions of shear are relatively steady or decaying with time and show very little related activity. Title: Potential Fields and Magnetic Canopies Authors: Jones, H. P. Bibcode: 1985BAAS...17..633J Altcode: No abstract at ADS Title: A study of flare buildup from simultaneous observations in microwave, H-alpha, and UV wavelengths Authors: Kundu, M. R.; Gaizauskas, V.; Woodgate, B. E.; Schmahl, E. J.; Shine, R.; Jones, H. P. Bibcode: 1985ApJS...57..621K Altcode: The results of high-resolution observations of the solar preflare activity of June 25, 1980 are analyzed. The observations were carried out simultaneously in the UV microwave, and H-alpha wavelengths using the VLA, the Ottawa River photoheliograph, and the Solar Max spectrometer and polarimeter instruments. Increases were observed in the intensitiy and polarization of compact sources at a wavelength of 6-cm during the preflare hour. The increases were associated with rising and twisting motions in the magnetic loops near the sight of the subsequent flare. Consistent with this process, analysis of the transverse and Doppler motions observed in the H-alpha filament before disruption showed that the filament was activated internally by the motions of evolving magnetic flux patterns. Ultraviolet data for C IV brightenings and upflows at the first appearance of the H-alpha filament indicated the presence of rising magnetic loops and material rising within the loops. The complete VLA, microwave and H-alpha data sets are given. Title: Full Disk Continuum Photometry with the NSO/Tusson Vacuum Telescope Authors: Luttermoser, D. G.; Jones, H. P. Bibcode: 1985BAAS...17..639L Altcode: No abstract at ADS Title: Magnetic shear. I - Hale region 16918 Authors: Athay, R. G.; Jones, H. P.; Zirin, H. Bibcode: 1985ApJ...288..363A Altcode: Material motion observed in spectral lines of C IV, C II, and Ca II formed in the chromosphere-corona transition region and upper chromosphere exhibits patterns that are closely identified with magnetic field structure at photospheric levels. Assuming that the fluid flow follows magnetic lines of force, the authors use chromospheric and transition region Dopplergrams to infer the broad features of the magnetic field geometry in these upper layers. For Hale region 16918 they find an area in the transition region and upper chromosphere, centered roughly over the photospheric magnetic neutral line, in which the lines of force show a strong tendency to parallel the photospheric neutral line. The authors interpret this as evidence for magnetic shear, which is pronounced in the upper layers of the atmosphere. Title: Working group on chromospheric fields - canopies. Authors: Jones, H. P. Bibcode: 1985cdm..proc...10J Altcode: Although there are many points of uncertainty and controversy, the working group on chromospheric fields focussed its discussion on the concept of canopies; i.e., no one disagreed that a central issue relating to magnetic fields and chromospheric models is to learn how the photospheric field spreads with height. However, it quickly became apparent that in the time available, there was little prospect of building new unified models of magnetic field phenomena in the chromosphere beyond the scope of the formal presentations. Thus, the discussion was devoted to formulating questions which seemed both possible to address in future work and important for advancing understanding of the chromosphere. It began by discussing unresolved physical issues (almost everything) and then proceeded to consider means, both observational and synthetic, to address them. Title: Recent studies of magnetic canopies Authors: Jones, H. P. Bibcode: 1985AuJPh..38..919J Altcode: Two current studies are described which stem from Giovanelli's seminal studies of the spreading of chromospheric fields near active regions and active-region network. First, improved observational techniques are described for obtaining magnetograms in the Ca II 8542 A, Fe I 8688 A, and C I 9111 A lines which at least in principle allow for more accurate treatment of instrumental noise and allow better inference of field orientation. Second, a generalized response function is developed for calculating theoretical magnetograph signals from arbitrary line-of-sight variations of magnetic field, and initial applications to two-dimensional, potential-field models of network fields are described. Preliminary indications are that potential-field models can better explain the presence of low-lying, diffuse horizontal fields than can thin flux-tube models, but fail to predict a differential response between the different lines. Title: Magnetic canopies and models of the solar chromosphere. Authors: Jones, H. P. Bibcode: 1985cdm..proc..175J Altcode: Magnetic canopies are the topologies formed by magnetic field lines as they spread from compact, nearly vertical concentrations of flux in the low photosphere into the large-scale organization of the corona and heliosphere. Analytical techniques for inferring the base-heights of canopies from magnetographic data are reviewed together with observational evidence that much of the sun is covered by canopies which lie two or more pressure scale heights below the level which is traditionally inferred from thin flux tube models. Implications of these results for modeling the structure and energetics of the chromosphere are discussed, and it is argued that future models should be based upon both spectroscopic and polarimetric data. Recent improvements in magnetostatic model atmospheres are reviewed, and new observational data, including C IV Doppler-grams from the Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission, are considered. Directions for future research in MHD modeling of canopies, in simulating spectrographic and polarimetric data from such models, and in observational programs are discussed. Title: Magnetic changes observed in a solar flare Authors: Moore, R. L.; Hurford, G. J.; Jones, H. P.; Kane, S. R. Bibcode: 1984ApJ...276..379M Altcode: The authors present observations of a large impulsive flare (1B/M4, 1980 April 10). Observations of the microwave/hard X-ray burst show the time development of the impulsive energy release. Chromospheric (Hα) and photospheric (Fe I λ5324) filtergrams and photospheric (Fe I λ8688) magnetograms, intensitygrams, and velocitygrams show magnetic structure, flare emission, mass motion, and magnetic changes. These observations show that strong flare-wrought magnetic changes in the chromosphere and corona produce observable, sudden, permanent changes in the photospheric magnetic field. The observations also show that one of the changes was initiated by transient brightening in Fe I λ5324 and λ8688 in step with the impulsive energy release and filament eruption. Title: Relationships of a growing magnetic flux region to flares Authors: Martin, S. F.; Bentley, R. D.; Schadee, A.; Antalova, A.; Kucera, A.; Dezső, L.; Gesztelyi, L.; Harvey, K. L.; Jones, H.; Livi, S. H. B.; Wang, J. Bibcode: 1984AdSpR...4g..61M Altcode: 1984AdSpR...4...61M Some sites for solar flares are known to develop where new magnetic flux emerges and becomes abutted against opposite polarity pre-existing magnetic flux (review by Galzauskas/1/). We have identified and analyzed the evolution of such flare sites at the boundaries of a major new and growing magnetic flux region within a complex of active regions, Hale No. 16918. This analysis was done as a part of a continuing study of the circumstances associated with flares in Hale Region 16918, which was designated as an FBS target during the interval 18 - 23 June 1980. We studied the initiation and development of both major and minor flares in Hα images in relation to the identified potential flare sites at the boundaries of the growing flux region and to the general development of the new flux. This study lead to our recognition of a spectrum of possible relationships of growing flux regions to flares as follows: (1) intimate interaction with adjacent old flux - flare sites centered at new/old flux boundary, (2) forced or ``intimidated'' interaction in which new flux pushes old field having lower flux density towards a neighboring old polarity inversion line where a flare then takes place, (3) ``influential'' interaction - magnetic lines of force over an old polarity inversion line, typically containing a filament, reconnect to the new emerging flux; a flare occurs with erupting filament when the magnetic field overlying the filament becomes too weak to prevent its eruption, (4) inconsequential interaction - new flux region is too small or has wrong orientation for creating flare conditions, (5) incidental - flare occurs without any significant relationship to new flux regions. Title: Variations of Total Solar Irradiance During Rapid Sunspot Growth Authors: Hudson, H. S.; Jones, H.; McIntosh, P. Bibcode: 1983BAAS...15Q.950H Altcode: No abstract at ADS Title: Solar oscillations with 13-day period Authors: Duvall, T. L., Jr.; Jones, H. P.; Harvey, J. W. Bibcode: 1983Natur.304..517D Altcode: Reference is made to the solar observations made by Claverie et al. (1982) over a three-month period in the summer of 1981 which show oscillatory velocity with a period of 13.1 days and amplitude of 6.6 m/s. These investigators reject the possibility that they see the Doppler shift from a radial oscillation, because the amplitude is implausibly large. They also do not believe that their signal was induced by solar magnetic fields, since typical mean solar fields are too small. Photo-electric drift-scan measurements of the solar diameter and full-disk magnetograms taken at Kitt Peak National Observatory are examined here for evidence of variations corresponding to the velocity oscillations of the 13.1-day period. An upper limit on radius variations is reported which is a factor of six below the amplitude needed to explain the velocity observations as a radial oscillation. Attention is also given to the possible role of the rotation of large-scale surface magnetic features. Title: Magnetic canopies in unipolar regions. Authors: Jones, H. P.; Giovanelli, R. G. Bibcode: 1983SoPh...87...37J Altcode: Base-height statistics are presented for magnetic canopies in six unipolar magnetic regions which were observed near the limb with the Kitt Peak Vacuum Telescope and Diode Array Magnetograph during the period 25 April-3 July, 1980. As in earlier studies, extensive areas are found to be covered by low-lying canopies. Title: Photospheric, Chromospheric and Transition-Region Flows in AR 2517 Authors: Athay, R. G.; Jones, H. P.; Zirin, H. Bibcode: 1983BAAS...15Q.719A Altcode: No abstract at ADS Title: Permafrost melting and dissolution of the landscape of Mars. Authors: Jones, H. P. Bibcode: 1982ESASP.185...89J Altcode: 1982plma.rept...89J It is supposed that during or after the updoming of the Noctis Labyrinthus-/Valles Marineris dome, postulated permafrost either completely or partly melted. The result was probably a slow sliding of the overlying volcanic rocks to the east, southeast and south, according to the inclination of the areas surface. Title: Magnetic Changes Observed in a Flare: True and Flase Transients and True Permanent Changes Authors: Moore, R. L.; Hurford, G. J.; Jones, H. P.; Kane, S. R. Bibcode: 1982BAAS...14..899M Altcode: No abstract at ADS Title: Scaling-Law Equilibria for Calcium in Canopy-Type Models of the Solar Chromosphere Authors: Jones, H. P. Bibcode: 1982SoPh...79..279J Altcode: Scaling laws for resonance line formation are used to obtain approximate excitation and ionization equilibria for a three-level model of singly ionized calcium. The method has been developed for and is applied to the study of magnetograph response in the 8542 Å infrared triplet line to magnetostatic canopies which schematically model diffuse, nearly horizontal fields in the low solar chromosphere. For this application, the method is shown to be efficient and semi-quantitative, and the results indicate the type and range of effects on calcium-line radiation which result from reduced gas pressure inside the magnetic regions. Title: The Three-Dimensional Structure of Atmospheric Magnetic Fields in Two Active Regions Authors: Giovanelli, R. G.; Jones, H. P. Bibcode: 1982SoPh...79..267G Altcode: The magnetic field above two unrelated active regions on 11 and 12 September, 1974 has been studied using magnetograms obtained in C I 9111, Fe I 8688, Ca II 8542, and Hα. In C I 9111, originating low in the photosphere, the fields are strong and sharply defined. In Ca II 8542 and Hα they are very diffuse, with significant diffuseness also in Fe I 8688, due to the spreading of the field with height to form almost horizontal magnetic canopies over regions free of field at lower levels. Title: Magnetograph Response to Canopy-Type Fields Authors: Jones, H. P.; Giovanelli, R. G. Bibcode: 1982SoPh...79..247J Altcode: The response of longitudinal-field magnetographs to magnetic fields which are semi-infinite or confined to a horizontal layer is discussed with respect to the interpretation of solar diffuse fields, observed towards the limb, in terms of magnetic canopy models. Numerical results are presented for several reference solar models and typical `calibration' curves are shown for the C I 9111 Å, Fe I 8688 Å, and Ca II 8542 Å lines in magnetostatic atmospheres derived from a mean model. A procedure is developed for determining the base heights of magnetic canopies from observations with an uncertainty not exceeding the order of a pressure scale height. Until definitive information regarding atmospheric structure inside flux tubes can be developed from theory or observation, reliable field strengths cannot be derived from the data. Title: Observations of sudden changes of magnetic structure in a flare. Authors: Moore, R. L.; Hurford, G. J.; Jones, H. P.; Kane, S. R. Bibcode: 1982BAAS...14Q.572M Altcode: No abstract at ADS Title: Solar radius measurements Authors: Duvall, T. L., Jr.; Jones, H. P. Bibcode: 1981NASCP2191..129D Altcode: 1981vsc..conf..129D Preliminary results of measurements made during 1979-1980 are discussed. Variability in the radius measurements of 0.4 pi is found, of unknown origin. Title: Ultramafic blocks from the ocean floor southwest of Australia Authors: Nicholls, I. A.; Ferguson, John; Jones, H.; Marks, G. P.; Mutter, J. C. Bibcode: 1981E&PSL..56..362N Altcode: Samples dredged from the ocean floor near the junction of the Naturaliste Fracture Zone and the Diamantina Zone, 300 km southwest of Cape Leeuwin, Western Australia, contain 3- to 10-cm blocks of Cr-spinel lherzolites and Al-spinel-olivine clinopyroxenites. Both assemblages show textural evidence for deformation and recrystallization, with extensive development of kaersutite in one clinopyroxenite. The blocks are enclosed by clay and Fe-Mn oxide-rich fragmental material, which also contains a diverse detrital mineral suite and microfossils. Diopsides in the lherzolites are Na- and Cr-rich, with marked similarities to those of lherzolite nodules in alkaline basaltic suites. The Al- and Ti-rich diopsides of the clinopyroxenites are more magnesium than those of common pyroxene-rich nodules. The lherzolites are interpreted as upper mantle residues, while the clinopyroxenites probably represent partly recrystallized cumulates from high-temperature basaltic magmas traversing the lherzolite mantle. Both are thought to have been derived from an ultramafic body emplaced into the shallow crust near the Cretaceous/early Tertiary continent-ocean boundary off Australia. Title: Solar Radius Measurements Authors: Duvall, T.; Jones, H. Bibcode: 1981siwn.conf..366D Altcode: No abstract at ADS Title: Magnetic Canopies in Unipolar Regions Authors: Jones, H. P.; Giovanelli, R. G. Bibcode: 1981BAAS...13R.881J Altcode: No abstract at ADS Title: Effects of Field Stratification on Magnetographic Measurements in the Infrared Triplet Lines of CaII Authors: Jones, H. P.; Giovanelli, R. G. Bibcode: 1980BAAS...12..807J Altcode: No abstract at ADS Title: Support of SMM with the Kitt Peak Vacuum Telescope; A Survey of Active Regions Authors: Jones, H. P.; Duvall, T. L., Jr.; Recely, F. J. Bibcode: 1980BAAS...12..906J Altcode: No abstract at ADS Title: A New Method for Measureing the Solar Radius Authors: Duvall, T. L., Jr.; Jones, H. P. Bibcode: 1980BAAS...12..474D Altcode: No abstract at ADS Title: The Physical Effects of Radiative Transfer in Multidimensional Media Including Models of the Solar Atmosphere Authors: Jones, H. P.; Skumanich, A. Bibcode: 1980ApJS...42..221J Altcode: We review the astrophysical literature concerning radiative transfer in multidimensional media where one requires the solution of the transfer equation under scattering conditions for a medium in which some combination of boundary configuration, external illumination, and internal thermodynamic structure causes the radiation field to vary with more than one spatial dimension. In constant opacity atmospheres, the radiation field is shown to scale systematically with to a characteristic geometric scale for a wide variety of configurations and types of scattering. Some effects of radiative exchange between different regions of multidimensional media are reviewed, and the constraining influence of an exponential vertical variation of opacity is discussed. Particular emphasis is given to recent applications of multidimensional transfer to the interpretation of the fine spatial structure on the Sun. Title: Multidimensional Radiative Transfer in Exponential Atmospheres Authors: Jones, H. P. Bibcode: 1979BAAS...11..405J Altcode: No abstract at ADS Title: Splines under Tension in Integral Transfer Problems Authors: Jones, H. P. Bibcode: 1977JQSRT..17..776J Altcode: No abstract at ADS Title: A possible edge effect in enhanced network. Authors: Jones, H. P.; Brown, D. R. Bibcode: 1977SoPh...52..337J Altcode: K-line observations of enhanced network taken with the NASA/SPO Multichannel Spectrometer on 28 September 1975 in support of OSO-8 are discussed. The data show a correlation between core brightness and asymmetry for spatial scans which cross enhanced network boundaries. The implications of this result concerning mass flow in and near supergranule boundaries are discussed. Title: Space telescope solar array. Feasibility study. Volume 2: Technical report Authors: Jones, H. Bibcode: 1976STIN...7719966J Altcode: The results of a feasibility study of the space telescope solar array are described and consideration of design is included. The selected concept with the rationale for its choice is described. A BISTEM actuated ROSA is chosen on the basis of its general compliance particularly with the dynamics, comparative simplicity, and mainly proven technology. Other candidate concepts are described and evaluated. A design description is given which includes configuration, mechanical, electrical, dynamic, and thermal aspects. Title: Observations of Enhanced Network from the NASA/SPO Multichannel Spectrometer in Support of OSO-8 Authors: Jones, H. P.; Brown, D. R. Bibcode: 1976BAAS....8..332J Altcode: No abstract at ADS Title: Automation of the Solar Multichannel Spectrometer. Authors: Hobbs, R. W.; Harris, G. D.; Jones, H. P.; Epstein, G. L.; Brown, D. R.; Wassmund, P. Bibcode: 1975BAAS....7..432H Altcode: No abstract at ADS Title: A two-layer plus background model for the solar K-line. Authors: Jones, H. P. Bibcode: 1974BAAS....6..485J Altcode: No abstract at ADS Title: Splat cooling and metastable phases Authors: Jones, H. Bibcode: 1973RPPh...36.1425J Altcode: No abstract at ADS Title: The Formation of Resonance Lines in Multidimensional Media. II. Radiation Operators and Their Numerical Representation Authors: Jones, Harrison P.; Skumanich, A. Bibcode: 1973ApJ...185..167J Altcode: A general integral-operator representation of radiative transfer in an atmosphere whose properties vary in more than one spatial dimension is developed together with well-posed procedures for its discrete numerical representation. This methodology is applied to the "non-LTE" excitation equilibrium of a two-level impurity species, i.e., to the formation of a resonance absorption line. The radiation operator that appears in the excitation equation is converted into a finite but large matrix by means of a suitably selected finite set of basis functions. This matrix-excitation equation is inverted directly to yield the excitation state and, hence, the impurity absorption characteristics of the plasma. Illustrative applications to the formation of a resonance line in a constant-density plasma with several types of two-dimensional temperature structures are presented. Subject headings: line formation - radiative transfer Title: The Formation of Resonance Lines in Multidimensional Media. III. Interpolation Functions, Accuracy, and Stability Authors: Jones, Harrison P. Bibcode: 1973ApJ...185..183J Altcode: The accuracy and stability for several specific representations of the integral-operator technique presented in Paper II (Jones and Skumanich 1973) are discussed. Solutions are tested against independently calculated results for an effectively thin "embedded slab." It is found that the cardinal interpolation functions for approximating the source function along characteristics must be "local," must give accurate representation of a variety of functions and their second derivatives on coarse, irregular grids, and must be compatible with interpolation functions used to map functions of spatial position to functions of path length. Cubic splines appear to meet these requirements and give good overall results. Subject headings: line formation - radiative transfer Title: Asymmetries in the Solar K-Line. Authors: Jones, H. P. Bibcode: 1973BAAS....5..445J Altcode: No abstract at ADS Title: Observations of the Solar Flare of 7 August 1972 Authors: Epstein, Gabriel L.; Hobbs, Robert W.; Maran, Stephen P.; Jones, Harrison P. Bibcode: 1973BAAS....5R.272E Altcode: No abstract at ADS Title: Line Formation in Multidimensional Atmospheres with Rapid Depth Variation of Absorption Coefficient Authors: Jones, H. P. Bibcode: 1973BAAS....5R.274J Altcode: No abstract at ADS Title: Interpolation Functions, Accuracy, and Stability in Multidimensional Transfer Problems. Authors: Jones, H. P. Bibcode: 1972BAAS....4..211J Altcode: No abstract at ADS Title: The Formation of Resonance Lines in Multidimensional Media. I. Scaling Properties in Two Dimensions Authors: Jones, Harrison P. Bibcode: 1971ApJ...164..341J Altcode: A method developed by Rybicki is applied to the non-LTE line-transfer problem for some simple two-dimensional temperature variations which crudely represent some aspects of the lateral fine structure of the solar atmosphere. Approximate scaling formulae are found which describe the spatial variation of the source function and its dependence on the geometric properties of the atmosphere. It is shown that the resulting spatial behavior of the emergent radiation can vary with frequency within a single profile as well as from line to line even when the underlying horizontal temperature structure is independent of depth. Title: The Scaling of Resonance-Line Radiation in Two-Dimensional Imbedded Slabs Authors: Jones, Harrison P. Bibcode: 1970BAAS....2R.324J Altcode: No abstract at ADS Title: Line Formation in Multi-Dimensional Media. Authors: Jones, Harrison Price Bibcode: 1970PhDT.........5J Altcode: No abstract at ADS Title: Line Formation in Multi-Dimensional Media Authors: Jones, H. P.; Skumanich, A. Bibcode: 1970sfss.coll..138J Altcode: 1970IAUCo...2..138J No abstract at ADS Title: Line Formation in Multidimensional Media Authors: Jones, H. P.; Skumanich, A. Bibcode: 1969BAAS....1S.281J Altcode: No abstract at ADS Title: Line Formation in Multi-Dimensional Media Authors: Jones, H. P.; Skumanich, A. Bibcode: 1968rla..conf...79J Altcode: No abstract at ADS Title: Statistical Equilibrium for a Multilevel Model of Calcium in the Solar Chromosphere. Authors: Jones, H. P.; Domenico, B. A.; Skumanich, A. Bibcode: 1968AJS....73S..66J Altcode: The statistical equilibrium of Ca is studied for collisional and radiative interactions a~propriate to various states of the solar chromosphere (cf. Athay and Skumanich, 1967). A model ion with levels representing the ground states of Ca I, II, and III is used, including the 4p2P and 3d2D excited states (ignoring fine structure) of Ca II. Dielectronic recombination from Ca II to Ca I is included in such a way as to display its maximum effect. For the mean chromosphere the ratio of continuum to line absorption coefficient, r0, for the "H-K" line (2P-2S transition) of Ca II is found to be independent of the radiation fields in the "H-K" and infrared "triplet" (2P-2D) lines. For other chromospheric conditions (e.g., spicules and plages) the above is not true and care must be exercised because line transfer calculations must include a self-consistent treatment of the effect of line radiation fields on line opacities. Dielectronic recombination does not affect r0 by more than a factor of 2 to 3. For an optically thick chromosphere in the "H-K" line ETH~K(Tmin) 3 X 104J such as used by Athay and Skumanich (1967), Linsky (1967), and Dumont (1967), studies of the interlocking terms in the "H-K" source function show the two-level atom to be a useful first approximation. In such a thick atmosphere the infrared "triplet" saturates to a condition of radiative detailed balance well before the temperature minimum. This requires the K1 intensities to yield a temperature minimum of the order of 42000K regardless of the rate coefficients assumed in the model atom. To reconcile the K1 intensities with a Tn~jn of 46000K as suggested by the Bilderberg model (1967) requires an unsaturated infrared "triplet" and hence a reduction in the "H-K" line optical depth by a factor of several hundred. Title: Electrons in Nearly Periodic Fields Authors: Jones, H. Bibcode: 1966RSPSA.294..405J Altcode: A detailed investigation is made of the change in the energy spectrum of a single electron in a pure metal brought about by the addition of small quantities of other elements in solid solution. To obtain numerical results the foreign atoms are represented by exponentially screened positive charges. The combined effects of line displacement and line broadening are determined and the change in the density of states at the Fermi limit is calculated. It is shown that the distortion of the energy band depends critically on the nature of the electronic states in the pure metal. Comparisons are made with the observed electronic specific heats of silver-based and copper-based solid solutions. Title: The properties of liquid helium Authors: Jones, H. Bibcode: 1939RPPh....6..280J Altcode: No abstract at ADS