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SPIE Astronomical Telescopes and Instrumentation 1-6 July 2012 Recommended papers Optical, Infrared, and Millimeter Wave 8442-1 Review of small angle coronagraphic techniques in the wake of second-generation adaptive optics systems: choice of coronagraph, optimized wavefront control, observing strategy, and post-processing methods Sunday 1 July, 9.00-9.30 Dimitri P. Mawet, European Southern Observatory; Pierre Baudoz, LESIA - Observatoire de Paris; Jean-Luc Beuzit, Institut de Planétologie et d'Astrophysique de Grenoble; Anthony Boccaletti, LESIA - Observatoire de Paris; Julien H. V. Girard, European Southern Observatory; Bertrand P. Mennesson, Jet Propulsion Lab.; Julien Milli, David Mouillet, Institut de Planétologie et d'Astrophysique de Grenoble; Laurent A. Pueyo, Johns Hopkins Univ.; Eugene Serabyn, J. Kent Wallace, John E. Krist, John T. Trauger, Jet Propulsion Lab. We will tentatively review the four pillars of high contrast imaging and their intricate interactions at very small angles (between 1 and 5 resolution elements from the star). We will then explore the solutions that were proposed and chosen to tackle each challenge. While emphasizing remaining open questions, we will show with concrete examples (from either simulated, lab or on-sky results) how the trade-off between the four pillars influence instrument design and performance, and how informative the commissioning of nextgen instrument will be in that respect. Finally, we will show how the lessons of the whole current ground-based experience can be applied to future space-based and giant ground-based facilities. 8442-21 The next-generation infrared space telescope SPICA Monday 2 July, 10.30-11-00 Takao Nakagawa, Hideo Matsuhara, Yasuhiro Kawakatsu, Japan Aerospace Exploration Agency We present an overview of the SPICA (Space Infrared Telescope for Cosmology and Astrophysics) mission, which is an astronomical mission optimized for mid- and far-infrared astronomy with a cryogenically cooled 3.2 m telescope. Its high spatial resolution and unprecedented sensitivity in the mid- and far-infrared will enable us to address a number of key problems in present-day astronomy, ranging from the star-formation history of the universe to the formation of planets. SPICA is proposed as a Japanese-led mission together with extensive international collaboration with ESA, European consortium, Korea and Taiwan. US participations are also being discussed extensively. The target launch year of SPICA is around 2020. 8442-39 Transiting Exoplanet Survey Satellite (TESS) Tuesday 3 July, 11.40-12.00 George R. Ricker, Jr., Massachusetts Institute of Technology; Mark C. Clampin, NASA Goddard Space Flight Ctr.; David Latham, Harvard-Smithsonian Ctr. for Astrophysics; Sara Seager, Roland K. Vanderspek, Jesus S. Villaseñor, Joshua Winn, Massachusetts Institute of Technology The Transiting Exoplanet Survey Satellite (TESS) will discover thousands of exoplanets in orbit around the brightest stars in the sky. In a two-year survey, TESS will monitor more than 500,000 stars for temporary drops in brightness caused by planetary transits. This first-ever spaceborne all-sky transit

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survey will identify planets ranging from Earth-sized to gas giants, around a wide range of stellar types and orbital distances. No ground-based survey can achieve this feat. A large fraction of TESS target stars will be 30-100 times brighter than those observed by Kepler satellite, and therefore TESS planets will be far easier to characterize with follow-up observations. TESS will make it possible to study the masses, sizes, densities, orbits, and atmospheres of a large cohort of small planets, including a sample of rocky worlds in the habitable zones of their host stars. TESS will provide prime targets for observation with the James Webb Space Telescope (JWST), as well as other large ground-based and space-based telescopes of the future. TESS data will be released with minimal delay (no proprietary period), inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the very nearest and brightest main-sequence stars hosting transiting exoplanets, thus providing future observers with the most favorable targets for detailed investigations. 8442-59 Gaia´s FPA: sampling the sky in silicon Wednesday 4 July, 14.20-14.40 Ralf Kohley, European Space Astronomy Ctr.; Philippe Garé, European Space Research and Technology Ctr.; Cyril Vétel, Denis Marchais, François Chassat, EADS Astrium ESA´s astrometry satellite Gaia is scheduled for launch in 2013 and will chart more than a billion stars of the entire sky to unprecedented accuracy. A key element to its mission success is the focal plane assembly (FPA), comprising an almost Giga-pixel mosaic of 106 large area CCDs. The focal plane is now assembled and will undergo its final tests during 2012. The paper summarizes the expected in-flight performances of Gaia´s FPA and the implemented tools and procedures to monitor its operation in space to guarantee the high accuracy needed in calibrating the science data on-ground. 8442-66 Characterizing persistence in the IR detector within the wide field camera 3 instrument on Hubble Space Telescope Thursday 5 July, 10.50-11.10 Knox S. Long, Sylvia M. Baggett, John W. MacKenty, Adam G. Riess, Space Telescope Science Institute The IR detector that is part of WFC3 on HST exhibits after images, known as persistence, following exposure to bright objects that saturate or nearly saturate portions of the HgCdTe detector. The persistence in the WFC3/IR detector is somewhat unusual in that the amount of persistence is not simply proportional to the exposure level. Here we characterize the persistence in WFC3/IR detector and the effectiveness of a model we are using to estimate the amount of persistence in all WFC3/IR images. These estimates are available through the Multi-Mission Archive at STScI to help HST users remove persistence from WFC3/IR images. 8442-81 Overview and status of the James Webb Space Telescope Observatory Friday 6 July, 9.30-9.50 Mark C. Clampin, Charles W. Bowers, NASA Goddard Space Flight Ctr. The James Webb Space Telescope (JWST) is a large aperture (6.5 meter), cryogenic space telescope with a suite of near and mid-infrared instruments spanning the wavelength range of 0.6 μm to 28 μm. JWST's primary science goals are to detect and characterize the first galaxies, study the assembly of galaxies, star formation, and the formation of evolution of planetary systems. Development of observatory is making rapid progress as major hardware sub-systems near-completion. We will discuss key performance parameters of the observatory, including thermal performance, image quality, sensitivity, and the ability to achieve background-limited observations. The observatory deployment after launch will also be discussed in the context of recent sub-system testing of deployment mechanisms. Ultraviolet to Gamma Ray

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8443-1 Little mirror, big science Sunday 1 July, 9.00-9.20 James C. Green, Univ. of Colorado at Boulder It will be decades before a flagship class mission in the ultraviolet will be implemented to succeed the Hubble Space Telescope. However, advances in technology can enable smaller aperture systems to achieve and surpass HST sensitivity by reducing attacking the noise portion of the signal/noise calculation. Through the use of ultra-low noise photon counting detectors, low scatter optics, narrow band filters and optical design, instruments in the ultraviolet can be developed that can attack critical science questions that cannot be addressed by current instrumentation, even in a Explorer class mission. I will review the science cases and the technologies needed to implement this vision. 8443-19 Cryogenic micro calorimeters as future imaging detectors for x-ray missions Monday 2 July, 10.30-11.00 Christian Enss, Ruprecht-Karls-Univ. Heidelberg The development of cryogenic detectors for high resolution x-ray spectroscopy has made rapid progress in the last decade. Todays, state of the art devices have a spectral resolving power of over 3000 at 6 keV. Among the most promising calorimeter technologies are superconducting transition edge sensors (TES), metallic magnetic calorimeters (MMC) and the recently proposed magnetic penetration depth thermometers (MPT). Despite the enormous progress, it still remains a major challenge to build large arrays of such detectors with high quality imaging capability. By far the most mature technology in this respect is based on TES detectors, for which arrays with several thousand pixels have already been demonstrated. We will review the current state of the development and discuss prospective for broad-band imaging x-ray spectroscopy using cryogenic micro calorimeters. 8443-34 The Chandra X-Ray Observatory: progress report and highlights Tuesday 3 July, 10.30-11.00 Martin C. Weisskopf, NASA Marshall Space Flight Ctr. The Chandra X-ray Observatory, the third of NASA's four Great Observatories and its flagship mission for X-ray astronomy, was launched by NASA's Space Shuttle Columbia on July 23, 1999. The first X-ray sources were observed on August 12, 1999. The brightest of these sources named Leon X-1 in honor of Chandra's Telescope Scientist who played the leading role in establishing the key to Chandra's great advance in angular resolution - sub-arcsecond Full Width at Half Maximum (FWHM). Over the course of a the past years, the Chandra X-ray Observatory's ability to provide sub-arc second X-ray images and high resolution spectra has established it as one of the most versatile and powerful tools for astrophysical research in the 21st century. Chandra explores the high-energy regions of the universe, observing X-ray sources with fluxes spanning more than 10 orders of magnitude. The longevity of Chandra provides a long observing baseline enabling temporal studies over time-scales of years. We will discuss the current operational status of the Observatory and present recent scientific highlights covering a variety of objects from stars with nearby planets that impact the stellar activity to the deepest Chandra surveys which measured space density of Active Galactic Nuclei (AGN) over a large range of obscuration and redshift. 8443-71 The ASTRO-H Mission Thursday 5 July, 14.30-14.50 Tadayuki Takahashi, Kazuhisa Mitsuda, Japan Aerospace Exploration Agency; Richard L. Kelley, NASA Goddard Space Flight Ctr.

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ASTRO-H, the Japanese X-ray Astronomy Satellite following Suzaku, is an international X-ray mission, planed for launch in 2014. ASTRO-H covers very wide energy range from 0.3 keV to 600 keV. The

simultaneous broad band pass, coupled with high spectral resolution of ＜7 eV by the micro-calorimeter will enable a wide variety of important science themes to be pursued. The ASTRO-H mission objectives are to study the evolution of yet-unknown obscured super massive Black Holes in Active Galactic Nuclei; trace the growth history of the largest structures in the Universe; provide insights into the behavior of material in extreme gravitational fields; trace particle acceleration structures in clusters of galaxies and SNRs; and investigate the detailed physics of jets. We will summarize the mission and report the recent progress of the project Ground-based and Airborne Telescopes IV 8444-1 The 1.6 m off-axis new solar telescope (NST) in Big Bear Sunday 1 July, 8.30-9.00 Philip R. Goode, Wenda Cao, Big Bear Solar Observatory The NST has been used to observe the Sun for more than three years with ever increasing capabilities. The NST is the first facility-class solar telescope built in the US in a generation, and it has an off-axis design as is planned for the 4 m Advanced Technology Solar Telescope. Lessons learned will be discussed. 8444-5 The Advanced Technology Solar Telescope: design and early construction Sunday 1 July, 10.30-11.00 Joseph P. McMullin, Thomas R. Rimmele, Stephen L. Keil, Mark Warner, Robert P. Hubbard, Eric R. Hansen, Samuel C. Barden, Steve L. Hegwer, William R. McBride, Bret Goodrich, Scott Bulau, Steve Shimko, Jennifer Ditsler, National Solar Observatory The Advanced Technology Solar Telescope is the first large U.S. solar telescope accessible to the worldwide solar physics community to be constructed in more than 30 years. The 4-meter diameter facility will operate over a broad wavelength range (0.3 to 28 $\micro$m), employing adaptive optics systems to achieve diffraction limited imaging and resolve features approximately 20 km on the Sun. This paper will review the ATST goals and specifications, describe each of the major subsystems under construction, and review the contracts and and lessons learned during the contracting and early construction phases. 8444-9 The Large Synoptic Survey Telescope final design status Sunday 1 July, 13.30-14.00 Victor L. Krabbendam, National Optical Astronomy Observatory; Donald W. Sweeney, LSST Corp. The Large Synoptic Survey Telescope (LSST) Project is a public-private partnership that has recently completed its Preliminary Design Review, an important step toward potential construction funding. The science objectives remain consistent with the New Worlds New Horizons endorsement of the LSST. The engineering approach requires a 3-mirror wide field optical system with an 8.4 meter primary mirror and a 64 cm 3.2 gigapixel focal plane camera. The data management system will reduce, transport, alert, and archive the 15 terabytes of data produced nightly. The Project is preparing for a 2014 construction authorization. 8444-35 Early science results from SOFIA Tuesday 3 July, 10.30-11.00 Erick T. Young, SOFIA / USRA; Terry L. Herter, Cornell Univ.; Rolf Guesten, Max-Planck-Institut für Radioastronomie; Edward W. Dunham, Lowell Observatory; Eric E. Becklin, SOFIA / USRA; Pamela M.

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Marcum, SOFIA / NASA; Alfred Krabbe, Deutsches SOFIA Institut; B. G. Andersson, William T. Reach, SOFIA / USR; Hans Zinnecker, Deutsches SOFIA Institut The Stratospheric Observatory for Infrared Astronomy successfully conducted its first year of science observations in 2011, performing 30 science flights. Named "Early Science", this period of time was intended to demonstrate the observing potential of SOFIA while still undergoing development as a facility. Observations were conducted with the FORCAST mid-infrared camera, the GREAT heterodyne spectrometer, and the HIPO occultation photometer. In this paper we present some of the science highlights from the early science period. 8444-41 The Cherenkov Telescope Array (CTA): status of the project and development of the telescopes Tuesday 3 July, 14.10-14.40 Giovanni Pareschi, INAF - Osservatorio Astronomico di Brera The Very High Energy band (above a few tens of GeV up to 100 TeV) is the natural domain where the study of the astrophysical sources is tangled with the realm of the particle physics. Several outstanding results were obtained so far by the HESS, MAGIC, and VERITAS Cherenkov arrays, both on Galactic and extra-Galactic sources. The forthcoming Cherenkov Telescope Array (CTA), with its innovative approach based on the use of three different sizes of telescopes (with dishes of 24, 12 and 7 m respectively), will obtain a sensitivity of 1 mCrab, i.e. one-order-of-magnitude improvement with respect to the current Cherenkov telescope performance. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. In this talk I will review the technological aspects being developed for the CTA telescopes, in particular on structures and mirrors. We will also report on the status of the project. 8444-45 The Large Binocular Telescope Tuesday 3 July, 16.20-16.40 John M. Hill, Richard F. Green, David S. Ashby, Joar G. Brynnel, Large Binocular Telescope Observatory; Norman J. Cushing, Norm Cushing Productions; John K. Little, James H. Slagle, R. Mark Wagner, Large Binocular Telescope Observatory The Large Binocular Telescope Observatory is a collaboration between institutions in Arizona, Germany, Italy, Indiana, Minnesota, Ohio and Virginia. The telescope uses two 8.4-m diameter primary mirrors mounted side-by-side to produce a collecting area equivalent to an 11.8-meter aperture. The light from the two primary mirrors can be combined to produce phased-array imaging of an extended field. This coherent imaging along with adaptive optics gives the telescope the diffraction-limited resolution of a 22.65-meter telescope. The first on-sky phasing of the two telescopes in the mid-infrared occurred in October 2010 with the LBTI instrument. Science observations are scheduled for 60% of the nights including a significant fraction of adaptive optics imaging with the first adaptive secondary mirror and the FLAO system with natural guide stars. The second of the two F/15 adaptive secondary mirrors has been installed on the telescope. 8444-48 Commissioning results from the Large Binocular Telescope Tuesday 3 July, 17.20-17.40 Joar G. Brynnel, Norman J. Cushing, Richard F. Green, John M. Hill, Douglas L. Miller, Andrew Rakich, David J. Thompson, The Univ. of Arizona Commissioning of a telescope facility such as the Large Binocular Telescope presents us with unprecedented challenges. The logistical and managerial balance act of scheduling commissioning of telescope, adaptive optics and twelve focal stations with subsequent commissioning of the instruments that populate the focal stations, while still providing for adequate science opportunity with already

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operational instruments is an equation that is problematic to solve in a way that meets the interests of all stakeholders. This paper presents strategies and priorities used at the LBTO, and status of telescope commissioning programs. We provide a summary of telescope commissioning results, including a discussion about specific efforts to improve performance of the LBT. 8444-83 LOFAR, the low frequency array Friday 6 July, 9.30-10.00 Rene Vermeulen, ASTRON LOFAR, the Low Frequency Array, is a next-generation radio telescope designed by ASTRON, with antenna stations concentrated in the north of the Netherlands and currently spread into Germany, France, Sweden and the United Kingdom; plans for more LOFAR stations exist in several other countries. Utilizing a novel, phased-array design, LOFAR is optimized for the largely unexplored low frequency range between 30 and 240 MHz. Digital beam-forming techniques make the LOFAR system agile and allow for rapid re-pointing of the telescopes as well as the potential for multiple simultaneous observations. Processing (e.g. cross-correlation) takes place in the LOFAR BlueGene/P supercomputer, and associated post-processing facilities. With its dense core (inner few km) array and long (more than 1000 km) interferometric baselines, LOFAR reaches unparalleled sensitivity and resolution in the low frequency radio regime. The International LOFAR Telescope (ILT) is now issuing its first call for observing projects that will be peer reviewed and selected for observing starting later this year. Allocations will be based in part on reserved fractions assigned by national consortia in return for contributions from their country to the ILT, and in part will be on the basis of Open Skies. In this invited talk, the gradually expanding complement of operationally verified observing modes and capabilities will be reviewed, and some of the exciting first astronomical results will be presented. 8444-90 ALMA commissioning and science verification Friday 6 July, 14.20-14.40 Richard E. Hills, Alison B. Peck, Joint ALMA Observatory ALMA is a large and complicated telescope and the process of bringing it into operation is a substantial task. This paper will describe the steps required to get from the stage where the sub-systems - antennas, receivers, correlators, etc. - have been assembled and tested, to the point where the complete system is functioning as a telescope and the astronomical data it produces have been shown to be valid. Topics covered will include the approach taken, the progress so far and the plans for the remaining stages of the program. Optical and Infrared Interferometry III 8445-6 Exo-zodiacal light around nearby main sequence stars: What did we learn with the Keck interferometer nuller? Sunday 1 July, 15.50-16.20 Bertrand P. Mennesson, Jet Propulsion Lab.; Rafael Millan-Gabet, California Institute of Technology; Eugene Serabyn, Jet Propulsion Lab.; Philip M. Hinz, The Univ. of Arizona; Marc Kuchner, NASA Goddard Space Flight Ctr.; Olivier Absil, Institut d'Astrophysique et de Géophysique de Liège; Denis Defrère, Max-Planck-Institut für Radioastronomie The determination of nearby main sequence stars zodiacal emission level has long been identified as crucial information for planetary dynamical formation, planet-disk interaction models, and for the proper design of direct exoplanet imaging space missions. We summarize here the results gathered by all 4 exo-zodi observing campaigns conducted with the Keck Interferometer Nuller between 2008 and 2011. A total of 49 stars were observed -mostly A to K dwarfs-, with a typical sensitivity (1-sigma) of 150

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solar zodis at 8.5 microns. Based on these measurements, we look for statistically significant trends and possible correlations between the observed mid-infrared excess levels and basic stellar properties. 8445-27 GRAVITY: observing the universe in motion Tuesday 3 July, 14.00-14.30 Frank Eisenhauer, Max-Planck-Institut für extraterrestrische Physik; Guy S. Perrin, LESIA - Observatoire de Paris à Meudon (France); Wolfgang Brandner, Max-Planck-Institut für Astronomie; Christian Straubmeier, Univ. zu Köln; Karine Rousselet-Perraut, Institut de Planétologie et d'Astrophysique de Grenoble (France); António Amorim, Univ. de Lisboa (Portugal); Markus Schöller, European Southern Observatory; Reinhard Genzel, Max-Planck-Institut für extraterrestrische Physik; Pierre Kervella, Observatoire de Paris à Meudon (France); Myriam Benisty, Max-Planck-Institut für Astronomie; Sebastian Fischer, Univ. zu Köln; Laurent Jocou, Institut de Planétologie et d'Astrophysique de Grenoble (France); Paulo J. V. Garcia, Univ. do Porto (Portugal); Gerd H. Jakob, European Southern Observatory; Stefan Gillessen, Max-Planck-Institut für extraterrestrische Physik; Yann Clénet, LESIA - Observatoire de Paris (France); Armin Boehm, Max-Planck-Institut für Astronomie; Constanza Araujo-Hauck, Univ. zu Köln; Jean-Philippe Berger, Institut de Planétologie et d'Astrophysique de Grenoble (France); Jorge Lima, Univ. de Lisboa (Portugal); Roberto N. Abuter, European Southern Observatory; Oliver Pfuhl, Thibaut Paumard, Max-Planck-Institut für extraterrestrische Physik; Casey P. Deen, Max-Planck-Institut für Astronomie; Michael Wiest, Univ. zu Köln; et al. GRAVITY is the second generation Very Large Telescope Interferometer instrument for precision narrow-angle astrometry and interferometric imaging. With its fiber-fed integrated optics, wavefront sensors, fringe tracker, beam stabilization and a novel metrology concept, GRAVITY will push the sensitivity and accuracy of astrometry and interferometric imaging far beyond what is offered today. Providing precision astrometry of order 10 microarcseconds, and imaging with 4-milliarcsecond resolution, GRAVITY will revolutionize high angular resolution imaging and dynamical measurements of celestial objects. This presentation summarizes the science opportunities and the technical concept of GRAVITY and gives an update on the current state of the instrument development. Ground-based and Airborne Instrumentation for Astronomy IV 8446-15 Performance of the Apache Point Observatory Galactic Evolution Experiment (APOGEE) high-resolution near-infrared multi-object fiber spectrograph Sunday 1 July, 16.40-17.00 John C. Wilson, Fred R. Hearty, Michael F. Skrutskie, Steve R. Majewski, Univ. of Virginia; Ricardo Schiavon, Gemini Observatory; Daniel J. Eisenstein, Harvard-Smithsonian Ctr. for Astrophysics; James E. Gunn, Princeton Univ.; Bruce Gillespie, Apache Point Observatory; David H. Weinberg, The Ohio State Univ.; Basil Blank, Charles P. Henderson, PulseRay; Stephen A. Smee, Robert H. Barkhouser, Albert Harding, Steve Hope, Johns Hopkins Univ.; Greg J. Fitzgerald, Todd M. Stolberg, New England Optical Systems; James Arns, Kaiser Optical Systems, Inc.; Matthew J. Nelson, Sophia D. Brunner, Adam Burton, Eric Walker, Charles R. Lam, Univ. of Virginia; Paul A. Maseman, The Univ. of Arizona; Jim Barr, Univ. of Virginia; R. French Leger, Larry N. Carey, Nick MacDonald, Univ. of Washington; Garrett Ebelke, Apache Point Observatory; Stephane Beland, Univ. of Colorado at Boulder; Todd Horne, The Univ. of Arizona; Erick T. Young, NASA Ames Research Ctr.; George H. Rieke, Marcia J. Rieke, The Univ. of Arizona; Thomas P. O'Brien, The Ohio State Univ.; Jeffrey D. Crane, Carnegie Observatories; Michael A. Carr, Princeton Univ.; et al. The Apache Point Observatory Galactic Evolution Experiment (APOGEE) uses a dedicated 300-fiber, narrow-band near-infrared (1.5-1.7 micron), high resolution (R~22,500) spectrograph to survey approximately 100,000 giant stars across the Milky Way. This survey, in operation since late-summer

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2011 as part of the Sloan Digital Sky Survey III (SDSS III), will revolutionize our understanding of kinematical and chemical enrichment histories of all Galactic stellar populations. We present the performance of the instrument from its first year in operation. The instrument design includes numerous innovations to enable spectroscopy of 300 sources simultaneously. 8446-18 Status of the KMOS multi-object near-infrared integral field spectrograph Monday 2 July, 10.30-10.50 Ray M. Sharples, Durham Univ.; Ralf Bender, Univ.-Sternwarte München and Max-Planck-Institut für extraterrestrische Physik; Alex Agudo Berbel, Max-Planck-Institut für extraterrestrische Physik; Richard J. Bennett, Naidu Bezawada, Michele Cirasuolo, UK Astronomy Technology Ctr.; Paul Clark, Durham Univ.; Richard I. Davies, Max-Planck-Institut für extraterrestrische Physik; Roger L. Davies, Univ. of Oxford; Cornelis M. Dubbeldam, Durham Univ.; Alasdair E. Fairley, UK Astronomy Technology Ctr.; Gert Finger, European Southern Observatory; Reinhard Genzel, Max-Planck-Institut für extraterrestrische Physik; Reinhold Haefner, Hans-Joachim Hess, Univ.-Sternwarte München; Ian J. Lewis, Univ. of Oxford; David M. Montgomery, John Murray, UK Astronomy Technology Ctr.; Bernard Muschielok, Univ.-Sternwarte München; Natascha M. Förster-Schreiber, Max-Planck-Institut für extraterrestrische Physik; Jean-Francois Pirard, Suzanne K. Ramsay, European Southern Observatory; Philip Rees II, UK Astronomy Technology Ctr.; Josef Richter, Univ.-Sternwarte München; David J. Robertson, Durham Univ.; Ian Robson, UK Astronomy Technology Ctr.; Stephen Rolt, Durham Univ.; et al. KMOS is a multi-object near-infrared integral field spectrograph being built by a consortium of UK and German institutes. We report on the final integration and test phases of KMOS, and its performance verification, prior to commissioning on the ESO VLT later this year. 8446-63 The habitable-zone planet finder: a stabilized fiber-fed NIR spectrograph for the Hobby-Eberly Telescope Thursday 5 July, 11.10-11.30 Suvrath Mahadevan, Lawrence W. Ramsey, The Pennsylvania State Univ.; Fred R. Hearty, Univ. of Virginia; Chad F. Bender, Ryan Terrien, The Pennsylvania State Univ.; Stephen L. Redman, National Institute of Standards and Technology; Samuel Halverson, The Pennsylvania State Univ.; Steven N. Osterman, Univ. of Colorado at Boulder; Scott A. Diddams, National Institute of Standards and Technology; James Kasting, Jason T. Wright, The Pennsylvania State Univ.; Michael Endl, The Univ. of Texas at Austin We present the conceptual design for the recently funded Habitable-zone Planet Finder (HPF), a stabilized fiber-fed NIR spectrograph for the 10m Hobby Eberly Telescope. The HPF will cover the NIR Y & J bands to enable precise radial velocities to be obtained on mid M dwarfs, and enable the detection of low mass planets around these stars. The conceptual design is comprised of a cryostat cooled to 200K, a dual fiber-feed with a science and calibration fiber, a gold coated echelle grating, and a H2RG NIR detector with a 1.7um cutoff, with the ability to upgrade to an H4RG in the future. A Uranium-Neon hollow-cathode lamp is the baseline wavelength calibration source, and we are actively testing laser frequency combs to enable even higher radial velocity precision. We will present the overall instrument system design and integration with the HET, and discuss major system challenges and proposed mitigation paths. 8446-65 The Gemini Planet Imager: integration and status Thursday 5 July, 11.50-12.10 Bruce A. Macintosh, Lawrence Livermore National Lab.; Stephen J. Goodsell, Gemini Observatory; David W. Palmer, Lawrence Livermore National Lab.; James R. Graham, Dunlap Institute for Astronomy & Astrophysics; René Doyon, Univ. de Montreal; Jennifer Dunn, National Research Council Canada; Donald

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T. Gavel, Univ. of California, Santa Cruz; James E. Larkin, Univ. of California, Los Angeles; Ben R. Oppenheimer, American Museum of Natural History; Leslie Saddlemyer, National Research Council Canada; J. Kent Wallace, Jet Propulsion Lab. The Gemini Planet Imager is a next-generation instrument for the direct detection and characterization of young warm exoplanets, designed to be an order of magnitude more sensitive than existing facilities. It combines a 1700-actuator adaptive optics system, an apodized-pupil Lyot coronagraph, a precision interferometric infrared wavefront sensor, and a integral field spectrograph. All hardware and software subsystems are now complete and undergoing integration and test at UC Santa Cruz. We will present test results on each subsystem and the results of end-to-end testing. Adaptive Optics Systems III 8447-1 Status of the ARGOS ground layer adaptive optics system Sunday 1 July, 9.00-9.20 Wolfgang Gässler, Max-Planck-Institut für Astronomie; Sebastian Rabien, Max-Planck-Institut für extraterrestrische Physik; Simone Esposito, INAF - Osservatorio Astrofisico di Arcetri; Michael Lloyd-Hart, The Univ. of Arizona; Lothar Barl, Max-Planck-Institut für extraterrestrische Physik; Udo Beckmann, Max-Planck-Institut für Radioastronomie; Thomas Bluemchen, Max-Planck-Institut für Astronomie; Marco Bonaglia, INAF - Osservatorio Astrofisico di Arcetri; José Luis Borelli, Max-Planck-Institut für Astronomie; Guido Brusa, Joar G. Brynnel, Large Binocular Telescope Observatory; Peter Buschkamp, Max-Planck-Institut für extraterrestrische Physik; Lorenzo Busoni, Luca Carbonaro, INAF - Osservatorio Astrofisico di Arcetri; Claus Connot, Max-Planck-Institut für Radioastronomie; Richard I. Davies, Matthias Deysenroth, Max-Planck-Institut für extraterrestrische Physik; Olivier Durney, The Univ. of Arizona; Richard F. Green, Large Binocular Telescope Observatory; Hans Gemperlein, Max-Planck-Institut für extraterrestrische Physik; Victor Gasho, The Univ. of Arizona; Marcus Haug, Max-Planck-Institut für extraterrestrische Physik; Pete Hubbard, The Univ. of Arizona; Sebastian Ihle, Max-Planck-Institut Halbleiterlabor; et al. ARGOS, a seeing reducer correcting the turbulence in the lower atmosphere over an field of 2' radius, is built by an German-Italian-American consortium for the LBT. We expect the system to improve the spatial resolution over the seeing of about a factor of two and more and to increase the throughput for spectroscopy accordingly. ARGOS will feed the two near-infrared imaging spectrographs - LUCI I and LUCI II. The installation and commissioning of the instrument will start 2012. We will give an overview of ARGOS and its goals and report about the status and new challenges we encountered during the building phase. Finally we will give an outlook of the upcoming work, how we will operate it and the further possibilities enabled by its design. 8447-10 Adaptive optics observations of the galactic center Sunday 1 July, 14.00-14.30 Sylvana Yelda, Andrea M. Ghez, Mark Morris, Leo Meyer, Univ. of California, Los Angeles; Jessica R. Lu, Univ. of Hawai'i; Tuan Do, Univ. of California, Irvine Optics observations have dramatically improved the quality and versatility of high angular resolution measurements of the center of our Galaxy. In this paper, we quantify the quality of our Adaptive Optics observations and present results that provide the best evidence to date that supermassive, black holes exist at the center of normal galaxies, that star formation does proceed in the vicinity of central black holes despite the strong tidal fields, and that the giant star population does not have the predicted cusp distribution. 8447-69 How ELTs will acquire the first spectra of rocky habitable planets Thursday 5 July, 15.50-16.10

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Olivier Guyon, Frantz Martinache, Subaru Telescope, National Astronomical Observatory of Japan; Eric J. Cady, Kunjithapatham Balasubramanian, Jet Propulsion Lab.; Ruslan Belikov, NASA Ames Research Ctr.; Christophe S. Clergeon, Subaru Telescope, National Astronomical Observatory of Japan; Mala Mateen, College of Optical Sciences, The Univ. of Arizona While direct imaging of Earth-like exoplanets around Sun-like stars will stay out of reach of ELTs, we show that coronagraphy at the ELT's diffraction limit will allow imaging of habitable planets around nearby M-type main sequence stars thanks to their more moderate contrast. We show that coronagraphy and wavefront control technologies required to achieve this goal already exist, and conclude that large ground-based telescopes will acquire the first high quality spectra of habitable planets orbiting M-type stars, while future space mission(s) will later target F-G-K type stars. 8447-76 Modeling anisoplanatism in the Keck II laser guide star AO system Friday 6 July, 9.10-9.30 Michael P. Fitzgerald, Univ. of California, Los Angeles; Matthew Britton, the Optical Sciences Company (tOSC); Andrea M. Ghez, Leo Meyer, Breann N. Sitarski, Eric E. Becklin, Univ. of California, Los Angeles; Randall D. Campbell, W. M. Keck Observatory; Carina Cheng, Univ. of California, Los Angeles; Tuan Do, Univ. of California, Irvine; Jessica R. Lu, Univ. of Hawai'i; Keith Y. Matthews, California Institute of Technology; Mark Morris, Univ. of California, Los Angeles; Christopher R. Neyman, W. M. Keck Observatory; Glenn A. Tyler, the Optical Sciences Company (tOSC); Peter Wizinowich, W. M. Keck Observatory; Sylvana Yelda, Univ. of California, Los Angeles A primary source of photometric and astrometric error in single-conjugate adaptive optics is anisoplanatism. For example, anisoplanatism limits the accuracy of stellar orbital measurements in the Galactic Center. We describe our project to model the off-axis optical transfer function in the LGS AO system and NIRC2 camera at the Keck II telescope, accounting for field-dependent atmospheric and instrumental aberrations. Here we present the results of a validation campaign using observations of naturally guided visual binary stars under varying turbulence conditions. We also discuss our plans to extend the work to laser guide star operation. 8447-121LINC-NIRVANA pathfinder: testing the next generation of wave front sensors at LBT Tuesday 3 July, 10.50-11.10 Albert R. Conrad, Max-Planck-Institut für Astronomie; Carmelo Arcidiacono, INAF - Osservatorio Astronomico di Bologna; Harald Baumeister, Max-Planck-Institut für Astronomie; Maria Bergomi, INAF - Osservatorio Astronomico di Padova; Thomas Bertram, Jürgen Berwein, Max-Planck-Institut für Astronomie; Christopher Biddick, Large Binocular Telescope Observatory; Peter Bizenberger, Matthieu Brangier, Florian Briegel, Max-Planck-Institut für Astronomie; Alessandro Brunelli, INAF - Osservatorio Astronomico di Padova; Joar G. Brynnel, Large Binocular Telescope Observatory; Lorenzo Busoni, INAF - Osservatorio Astrofisico di Arcetri; Norman J. Cushing, Large Binocular Telescope Observatory; Fulvio De Bonis, Max-Planck-Institut für Astronomie; Michele De La Pena, Large Binocular Telescope Observatory; Simone Esposito, INAF - Osservatorio Astrofisico di Arcetri; Jacopo Farinato, INAF - Osservatorio Astronomico di Bologna; Luca Fini, INAF - Osservatorio Astrofisico di Arcetri; Wolfgang Gässler, Max-Planck-Institut für Astronomie; Richard F. Green, Large Binocular Telescope Observatory; Thomas M. Herbst, Ralph Hofferbert, Frank Kittmann, Martin Kürster, Daniel Meschke, Lars Mohr, Jörg-Uwe Pott, Max-Planck-Institut für Astronomie; et al. LINC-NIRVANA (Herbst et al., SPIE, 2010) will employ four wave front sensors to realize multi-conjugate correction on both arms of a Fizeau interferometer for LBT. Of these, one of the two ground-layer wave front sensors, together with its infrared test camera, comprise a stand-alone test platform that follows in the footsteps of the multi-conjugate adaptive optics demonstrator (MAD) (Marchetti, et al., 2003). Unlike MAD, however, this system, called the LINC-NIRVANA Pathfinder, will achieve ground-layer AO

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correction via an adaptive secondary; the 672-actuator thin shell at the LBT. Since reporting our progress at AO4ELT2 (Conrad, et al., AO4ELT2, 2011), we have initiated design and development in three key areas. a software interface for external control of the adaptive secondary, a software extension to the instrument interface to the telescope control system, and calibration. We will report on our progress and future plans in these three areas, and on the project overall. Observatory Operations

8448-40 Science commissioning of JWST: applying Hubble's lessons to the Webb Friday 6 July, 11.00-11.20 Carl P. Biagetti, Victoria Balzano, Space Telescope Science Institute The Space Telescope Science Institute (STScI) has the primary role for planning and carrying out the science program for the James Webb Space Telescope (JWST). It also has a lead role, in support of the Prime Contractor, in planning and carrying out the science instrument commissioning program designed to enable, post-launch, the start of Observatory science. In this paper, we address planning principles and operational lessons stemming from our Hubble experience and show how those principles and lessons are being applied to the science commissioning plans for the JWST Observatory. In doing so, we contrast JWST's expected early-life operations with Hubble's post-servicing performance, and address any adjustments needed in our HST principles and lessons in order to effectively apply them to the specific challenges of JWST science commissioning.

8448-41 Mixing completion, commissioning, and operations at the LBT Friday 6 July, 11.20 – 11.40 Richard F. Green, John M. Hill, Joar G. Brynnel, James H. Slagle, David S. Ashby, Norman J. Cushing, John K. Little, Large Binocular Telescope Observatory; R. Mark Wagner, Ohio State Univ. By July 2012, the Large Binocular Telescope Observatory will be supporting scientific observing 60% of the time with binocular prime focus imaging, single-sided optical and near-IR imaging and spectroscopy, and adaptive optics imaging. Interspersed in the last year were installation and commissioning of the second adaptive optics system and re-commissioning of the LUCI near-IR instrument with a replacement detector. Initial commissioning of mid-IR interferometry is also underway. The goal is to apply the lessons learned to the continuing period of observation plus commissioning as new spectroscopic and interferometric capabilities are added through 2014.

Modeling, Systems Engineering, and Project Management for Astronomy V 8449-27 Managing large astronomy projects: Herschel-HIFI and ALMA Tuesday 3 July, 11.50-12.10 Mattheus W. M. de Graauw, Richard J. Kurz, ALMA; Kees Wafelbakker, SRON Nationaal Instituut voor Ruimteonderzoek As astronomical projects are aiming for higher angular and spectral resolution and larger collecting area, the project teams have become more complex to deal with the wider variety of technologies, and are geographically more distributed to meet the larger budgetary requirements. Two recent examples are the Heterodyne Instrument for the Far-Infrared (HIFI) on-board ESA's Herschel Space Observatory and the Atacama Large Millimeter/submillimeter Array (ALMA) a ground based observatory under construction in the Andes in the North of Chile. Both projects are indeed large international projects in terms of scope, carried out by large consortia of institutes with a wide geographic distribution. We will describe and analyse the governance and management approaches for these two projects, the

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similarities and differences in their programmatic and technical management and the tools used during the various phases of the program. Modern Technologies in Space- and Ground-based Telescopes and Instrumentation II 8450-52 A near infrared frequency comb for Y-band astronomical spectroscopy Wednesday 4 July, 11.10-11.30 Steven N. Osterman, Univ. of Colorado at Boulder; Gabriel G. Ycas, Scott A. Diddams, Franklyn Quinlan, National Institute of Standards and Technology; Chad F. Bender, Suvrath Mahadevan, Lawrence W. Ramsey, The Pennsylvania State Univ. Radial velocity surveys supported by high precision wavelength references (notably ThAr lamps and I2 cells) have successfully identified hundreds of exoplanets; however, as the search for exoplanets moves to cooler, lower mass stars, the optimum wave band for observation moves into the NIR and new wavelength standards are required. To address this we are developing a laser frequency comb for the Y and potentially J bands (0.98-1.3μm). This comb is optimized for use with a 50,000 resolution NIR spectrograph such as the Penn State Habitable Zone Planet Finder. We present design and performance details of the current Y band comb. Software and Cyberinfrastructure for Astronomy II 8451-12 The Dark Energy Survey data processing and calibration system Sunday 1 July, 14.50-15.10 Joseph J. Mohr, Ludwig-Maximilians-Univ. München; Robert Armstrong, Univ. of Pennsylvania; Emmanuel Bertin, Institut d'Astrophysique de Paris; Arthur Carlson, Ludwig-Maximilians-Univ. München; Greg Daues, Univ. of Illinois at Urbana-Champaign; Shantanu Desai, Ludwig-Maximilians-Univ. München; Michelle Gower, Robert Gruendl, William Hanlon, Univ. of Illinois at Urbana-Champaign; Rick Kessler, The Univ. of Chicago; Nikolay Kuropatkin, Huan Lin, John Marriner, Fermi National Accelerator Lab.; Donald Petravic, Univ. of Illinois at Urbana-Champaign; Ignacio Sevilla, Ctr. de Investigaciones Energéticas, Medioambientales y Tecnológicas (Spain); Molly Swanson, Smithsonian Astrophysical Observatory; Todd Tomashek, Univ. of Illinois at Urbana-Champaign; Douglas Tucker, Fermi National Accelerator Lab.; Yuxuan Yang, Univ. of Illinois at Urbana-Champaign; Brian Yanny, Fermi National Accelerator Lab. The Dark Energy Survey (DES) is a 5000 deg^2 grizY survey reaching photometric depths of 24th magnitude (10 sigma). The DES data management system (DESDM) is a high performance computing enabled system that will be used for processing, calibrating and serving the ~4PB of DES data. It includes special purpose image detrending and photometric calibration codes as well as new extensions of the AstrOmatic toolkit for PSF modeling and homogenization, and for model fitting across multiple input images. We have extensively tested DESDM using simulated and real datasets. In Fall 2012 the DESDM system will go into science operation. 8451-20 Virtual clouds on an astronomical observatory: virtualization at ESO, its status and its future Monday 2 July, 10.30-11.00 Andrea Balestra, European Southern Observatory Virtualization and Cloud Computing are hyped buzzwords in today's computing world, but, regardless of this, they are also consolidated technologies that offer many opportunities to improve the efficiency of a cyberinfrastructure. At ESO they are used from several years in various domains, from IT infrastructure to development and simulation as well as in data handling. Different models, tools and vendors have been extensively investigated. In this contribution we describe virtualization and cloud computing usage

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at ESO as well as what are the plans for the future. Moreover, based on our experience, we envisage what a "cloudy" astronomical observatory may look like. Millimeter, Submillimeter, Far-Infrared Detectors and Instrumentation 8452-25 Development of 1000 arrays MKID camera for the CMB observation Wednesday 4 July, 16.40-17.00 Kenichi Karatsu, National Astronomical Observatory of Japan; Masato Naruse, The Univ. of Tokyo and National Astronomical Observatory of Japan; Tom Nitta, Univ. of Tsukuba and National Astronomical Observatory of Japan; Masakazu Sekine, The Univ. of Tokyo and National Astronomical Observatory of Japan; Yutaro Sekimoto, Takashi Noguchi, Yoshinori Uzawa, Hiroshi Matsuo, Hitoshi Kiuchi, National Astronomical Observatory of Japan We have been developing antenna-coupled MKID at NAOJ in cooperation with KEK and RIKEN, aiming for a precise CMB measurement. We have successfully fabricated 102-pixel MKID camera with epitaxially-formed Al on Si wafer, and beam measurement with Si lens array is underway. In parallel, we are developing 1000 pixels camera with mosaic of 256-pixel MKID cameras. We are also constructing a new test-bench for the module with optimizing antenna design, Si lens size for each pixel and optics system inside the cryostat. We would like to present the status of the development of the camera with its performance assessments. 8452-48 The POLARBEAR experiment Friday 6 July, 9.30-9.50 Zigmund D. Kermish, Univ. of California, Berkeley; Peter A. Ade, Cardiff Univ.; Kam S. Arnold, Univ. of California, Berkeley; Aubra Anthony, Univ. of Colorado at Boulder; Darcy Barron, Univ. of California, San Diego; Julian Borrill, Lawrence Berkeley National Lab. (United States) and Univ. of California, Berkeley; Yuji Chinone, High Energy Accelerator Research Organization; Matthew A. Dobbs, McGill Univ.; Josquin Errard, Giulio Fabbian, AstroParticule et Cosmologie; Daniel Flanigan, Univ. of California, Berkeley; George Fuller, Univ. of California, San Diego; William F. Grainger, Cardiff Univ.; Nils W. Halverson, Univ. of Colorado at Boulder; Masaya Hasegawa, Masashi Hazumi, High Energy Accelerator Research Organization; William L. Holzapfel, Jacob Howard, Univ. of California, Berkeley; Peter O. Hyland, Austin College; Andrew Jaffe, Imperial College London; Brian G. Keating, Univ. of California, San Diego; Adrian T. Lee, Univ. of California, Berkeley (United States) and Lawrence Berkeley National Lab.; Theodore S. Kisner, Lawrence Berkeley National Lab.; Maude Le Leune, AstroParticule et Cosmologie; Eric V. Linder, Lawrence Berkeley National Lab.; et al. We present the design and characterization of the POLARBEAR experiment. POLARBEAR will measure the B- mode polarization of the cosmic microwave background (CMB) on angular scales ranging from the experiment's 4' beam size to several degrees. POLARBEAR was assembled for an engineering run in the Inyo Mountains of California in 2010 and was deployed in late 2011 to the Atacama Desert in Chile. An overview of the instrument is presented along with characterization results from both the California engineering run and observations in Chile. High Energy, Optical, and Infrared Detectors for Astronomy V 8453-1 Photon counting EMCCDs: new opportunities for high time resolution astrophysics Sunday 1 July, 8.40-9.10 Craig D. MacKay, Univ. of Cambridge Electron Multiplying CCDs (EMCCDs) are used much less often than they might be because of the challenges they offer camera designers more comfortable with slow-scan detector systems. However

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they offer an entirely new range of opportunities in astrophysical instrumentation. This paper will show some of the most exciting new results obtained with these remarkable devices and talk about their potential in other areas of astrophysical application. We will then describe how they may be operated to give the very best performance at the lowest possible light levels. We will show that clock induced charge may be reduced to negligible levels and that, with care, devices may be clocked at significantly higher speeds than usually achieved. As an example of the advantages offered by these detectors we will show how a multi-detector EMCCD curvature wavefront sensor will revolutionise the sensitivity of adaptive optics instruments.

Poster of interest

8447-161 Early science results from the first light AO (FLAO) system for LBT Monday 2 July, poster Carmelo Arcidiacono, INAF - Osservatorio Astronomico di Bologna; Filippo Mannucci, Simone Esposito, Armando Riccardi, INAF - Osservatorio Astrofisico di Arcetri; Richard F. Green, Joar G. Brynnel, Large Binocular Telescope Observatory; Donald W. McCarthy, Jr., Laird M. Close, Andrew Skemer, The Univ. of Arizona; Guido Agapito, Runa Briguglio, Lorenzo Busoni, Luca Fini, Enrico Pinna, Alfio Timothy Puglisi, Fernando Quiros-Pacheco, Marco Xompero, INAF - Osservatorio Astrofisico di Arcetri; Juan Carlos Guerra Ramon, Guido Brusa, Konstantina Boutsia, Douglas L. Miller, Large Binocular Telescope Observatory; Craig A. Kulesa, Jared R. Males, The Univ. of Arizona The First Light Adaptive Optics (FLAO) system for LBT has been commissioned in October 2011. In Science Verification and Science Demonstration time the capabilities of the AO to provide optimal Science-grade imaging using the PISCES Near Infrared Camera have been proven. In this paper we collect sample results of the observations made, in order to exemplify the different abilities, such as astrometry and photometry, ranging from Solar System to QSO.