5 results
ATLAS probe: Breakthrough science of galaxy evolution, cosmology, Milky Way, and the Solar System
- Yun Wang, Massimo Robberto, Mark Dickinson, Lynne A. Hillenbrand, Wesley Fraser, Peter Behroozi, Jarle Brinchmann, Chia-Hsun Chuang, Andrea Cimatti, Robert Content, Emanuele Daddi, Henry C. Ferguson, Christopher Hirata, Michael J. Hudson, J. Davy Kirkpatrick, Alvaro Orsi, Russell Ryan, Alice Shapley, Mario Ballardini, Robert Barkhouser, James Bartlett, Robert Benjamin, Ranga Chary, Charlie Conroy, Megan Donahue, Olivier Doré, Peter Eisenhardt, Karl Glazebrook, George Helou, Sangeeta Malhotra, Lauro Moscardini, Jeffrey A. Newman, Zoran Ninkov, Michael Ressler, James Rhoads, Jason Rhodes, Daniel Scolnic, Stephen Smee, Francesco Valentino, Risa H. Wechsler
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- Journal:
- Publications of the Astronomical Society of Australia / Volume 36 / 2019
- Published online by Cambridge University Press:
- 08 April 2019, e015
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Astrophysics Telescope for Large Area Spectroscopy Probe is a concept for a National Aeronautics and Space Administration probe-class space mission that will achieve ground-breaking science in the fields of galaxy evolution, cosmology, Milky Way, and the Solar System. It is the follow-up space mission to Wide Field Infrared Survey Telescope (WFIRST), boosting its scientific return by obtaining deep 1–4 μm slit spectroscopy for ∼70% of all galaxies imaged by the ∼2 000 deg2 WFIRST High Latitude Survey at z > 0.5. Astrophysics Telescope for Large Area Spectroscopy will measure accurate and precise redshifts for ∼200 M galaxies out to z < 7, and deliver spectra that enable a wide range of diagnostic studies of the physical properties of galaxies over most of cosmic history. Astrophysics Telescope for Large Area Spectroscopy Probe and WFIRST together will produce a 3D map of the Universe over 2 000 deg2, the definitive data sets for studying galaxy evolution, probing dark matter, dark energy and modifications of General Relativity, and quantifying the 3D structure and stellar content of the Milky Way. Astrophysics Telescope for Large Area Spectroscopy Probe science spans four broad categories: (1) Revolutionising galaxy evolution studies by tracing the relation between galaxies and dark matter from galaxy groups to cosmic voids and filaments, from the epoch of reionisation through the peak era of galaxy assembly; (2) Opening a new window into the dark Universe by weighing the dark matter filaments using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of General Relativity using galaxy clustering; (3) Probing the Milky Way’s dust-enshrouded regions, reaching the far side of our Galaxy; and (4) Exploring the formation history of the outer Solar System by characterising Kuiper Belt Objects. Astrophysics Telescope for Large Area Spectroscopy Probe is a 1.5 m telescope with a field of view of 0.4 deg2, and uses digital micro-mirror devices as slit selectors. It has a spectroscopic resolution of R = 1 000, and a wavelength range of 1–4 μm. The lack of slit spectroscopy from space over a wide field of view is the obvious gap in current and planned future space missions; Astrophysics Telescope for Large Area Spectroscopy fills this big gap with an unprecedented spectroscopic capability based on digital micro-mirror devices (with an estimated spectroscopic multiplex factor greater than 5 000). Astrophysics Telescope for Large Area Spectroscopy is designed to fit within the National Aeronautics and Space Administration probe-class space mission cost envelope; it has a single instrument, a telescope aperture that allows for a lighter launch vehicle, and mature technology (we have identified a path for digital micro-mirror devices to reach Technology Readiness Level 6 within 2 yr). Astrophysics Telescope for Large Area Spectroscopy Probe will lead to transformative science over the entire range of astrophysics: from galaxy evolution to the dark Universe, from Solar System objects to the dusty regions of the Milky Way.
Contributors
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- By J. Todd Arnedt, Sharon Aronovich, Alon Y. Avidan, Alp Sinan Baran, Johnathan Barkham, Lizabeth Binns, Tiffany J. Braley, Devin Brown, Paul R. Carney, Philip Cheng, Ronald D. Chervin, Naricha Chirakalwasan, Wattanachai Chotinaiwattarakul, Deirdre A. Conroy, Charles R. Davies, Dawn Dore-Stites, Alan S. Eiser, Todd Favorite, Barbara T. Felt, James D. Geyer, Jennifer R. Goldschmied, Cathy A. Goldstein, John J. Harrington, Fauziya Hassan, Judith L. Heidebrink, Joseph I. Helman, Shelley Hershner, Timothy F. Hoban, Edward D. Huntley, Rahul K. Kakkar, Douglas Kirsch, Raman K. Malhotra, Beth A. Malow, Lauren O’Connell, Shalini Paruthi, Meredith D. Peters, Scott M. Pickett, Satya Krishna Ramachandran, Fouad Reda, Daniel I. Rifkin, Emerson Robinson, Helena M. Schotland, Q. Afifa Shamim-Uzzaman, Anita Valanju Shelgikar, Renée A. Shellhaas, Jeffrey J. Stanley, Leslie M. Swanson, Mihai C. Teodorescu, Mihai C. Teodorescu, Sheila C. Tsai, Katherine Wilson, Michael E. Yurcheshen, Sarah Nath Zallek
- Edited by Ronald D. Chervin
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- Book:
- Common Pitfalls in Sleep Medicine
- Published online:
- 05 April 2014
- Print publication:
- 10 April 2014, pp x-xiv
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Near-infrared Integral-Field Spectrograph (NIFS): An Instrument Proposed for Gemini
- Peter J. McGregor, Peter Conroy, Gabe Bloxham, Jan van Harmelen
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- Journal:
- Publications of the Astronomical Society of Australia / Volume 16 / Issue 3 / 1999
- Published online by Cambridge University Press:
- 05 March 2013, pp. 273-287
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In late 1998 the International Gemini Project Office identified a need for a low cost, near-infrared spectrograph to be commissioned on the Gemini South telescope on the shortest possible timescale. In response, the Research School of Astronomy and Astrophysics of the Australian National University proposed to design, construct, and commission a near-infrared, integral-field spectrograph on Gemini. The science drivers and novel design of the Near-infrared Integral-Field Spectrograph (NIFS) are described in this paper. NIFS will achieve significant economies in cost and schedule in several ways:
• By addressing targeted science with high efficiency. NIFS will primarily target velocity measurements in galaxies to study the demographics of black holes in galactic nuclei and the evolution of structural properties in high redshift galaxies. However, NIFS will also be applied to a wide range of general astronomical topics, but these will not dictate the instrument design.
• By adopting a largely fixed-format design. A 3·2″ × 3·2″ ‘stair-case’ integral field unit (IFU) will feed a near-infrared spectrograph with four fixed-angle gratings mounted on a single grating wheel. A single, fixed-format camera will form the spectral image on a 2048 × 2048 Rockwell HgCdTe HAWAII-2 array. Two-pixel spectral resolving powers of ∼5400 will be achieved with complete wavelength coverage in each of the J, H, and K photometric bands through 32 optimally sampled 0·1″ wide slitlets. The velocity resolution of ∼55 km s−1 will be sufficient to achieve the targeted science objectives, and will allow software rejection of OH airglow lines.
• By packaging the NIFS instrument within a duplicate of the Near-Infrared Imager (NIRI) cryostat. The NIRI cryostat, On-Instrument Wavefront Sensor (OIWFS), detector focusing mechanism, control system, and EPICS software will all be duplicated with only minimal change. Construction of the duplicate NIRI cryostat, OIWFS, and control system will be done by the University of Hawaii.
A New Acquisition and Autoguiding Camera for the ANU 2·3 m Telescope
- Peter J. McGregor, Peter Conroy, Jan van Harmelen, Michael S. Bessell
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- Journal:
- Publications of the Astronomical Society of Australia / Volume 17 / Issue 1 / 2000
- Published online by Cambridge University Press:
- 05 March 2013, pp. 102-108
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A new, direct CCD acquisition and autoguiding camera is in use on the ANU 2·3 m telescope Nasmyth foci. The camera is a model AP7 manufactured by Apogee Instruments Inc. and is controlled by the MaxIm CCD camera control and image processing software developed by Diffraction Ltd. The factors influencing our choice of this new camera are discussed, and its performance, operation, and commercial control software are described. The new camera allows stellar objects as faint as B = 21·5 to be acquired on the Double Beam Spectrograph slit in 1·4″ seeing. The camera has far superior performance to the Fairchild intensified CCD cameras that it replaces. The improved acquisition and guiding permitted by this camera has already allowed several new scientific programs to begin on the telescope, including the use of aperture plates with the Double Beam Spectrograph.
Contributors
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- By Joëlle Adrien, M. Y. Agargun, Negar Ahmadi, Imran M. Ahmed, J. Todd Arnedt, Joseph Barbera, Simon Beaulieu-Bonneau, Marie E. Beitinger, Francesco Benedetti, Glenn Berall, Kirk J. Brower, Gregory M. Brown, Kumaraswamy Budur, Daniel P. Cardinali, Deirdre A. Conroy, Sara Dallaspezia, José Manuel de la Fuente, Paolo De Luca, Diana De Ronchi, Antonio Drago, Matthew R. Ebben, Irshaad Ebrahim, Pingfu Feng, Peter B. Fenwick, Lina Fine, Jonathan Adrian Ewing Fleming, Paul A. Fredrickson, Stephany Fulda, Lucile Garma, Roger Godbout, Reut Gruber, J. Allan Hobson, Andrea Iaboni, Anna Ivanenko, Mayumi Kimura, Milton Kramer, Christoph J. Lauer, Remy Luthringer, Luis Fernando Martínez, Sara Matteson-Rusby, Robert W. McCarley, Charles J. Meliska, Harvey Moldofsky, Charles M. Morin, Sricharan Moturi, Marie-Christine Ouellet, James F. Pagel, S. R. Pandi-Perumal, Barbara L. Parry, Timo Partonen, Wilfred R. Pigeon, Thomas Pollmächer, Nathalie Pross, Elliott Richelson, Naomi L. Rogers, Stefan Rupprecht-Mrozek, Philip Saleh, Andreas Schuld, Alessandro Serretti, Colin M. Shapiro, Christopher Michael Sinton, Marcel G. Smits, D. Warren Spence, Jürgen Staedt, Corinne Staner, Luc Staner, Axel Steiger, Deborah Suchecki, Michael J. Thorpy, Inna Voloh, Bradley G. Whitwell, Robert A. Zucker
- Edited by S. R. Pandi-Perumal, Milton Kramer, University of Illinois, Chicago
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- Book:
- Sleep and Mental Illness
- Published online:
- 05 July 2011
- Print publication:
- 01 April 2010, pp ix-xiii
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