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Proceedings Paper

ATLAS probe for the study of galaxy evolution with 300,000,000 galaxy spectra
Author(s): Robert Content; Yun Wang; Massimo Roberto; Mark Dickinson; Henry Ferguson; Lynne Hillenbrand; Wesley Fraser; Peter Behroozi; Jarle Brinchmann; Andrea Cimatti; Emanuele Daddi; Christopher Hirata; Michael Hudson; J. Davy Kirkpatrick; Robert Barkhouser; James Bartlett; Robert Benjamin; Ranga Chary; Charlie Conroy; Megan Donahue; Olivier Doré; Peter Eisenhardt; Karl Glazebrook; George Helou; Sangeeta Malhotra; Lauro Moscardini; Zoran Ninkov; Alvaro Orsi; Michael Ressler; James Rhoads; Jason Rhodes; Alice Shapley; Stephen Smee
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Paper Abstract

ATLAS (Astrophysics Telescope for Large Area Spectroscopy) Probe is a mission concept for a NASA probe-class space mission with primary science goal the definitive study of galaxy evolution through the capture of 300,000,000 galaxy spectra up to z=7. It is made of a 1.5-m Ritchey-Chretien telescope with a field of view of solid angle 0.4 deg2. The wavelength range is at least 1 μm to 4 μm with a goal of 0.9 μm to 5 μm. Average resolution is 600 but with a possible trade-off to get 1000 at the longer wavelengths. The ATLAS Probe instrument is made of 4 identical spectrographs each using a Digital Micro-mirror Device (DMD) as a multi-object mask. It builds on the work done for the ESA SPACE and Phase-A EUCLID projects. Three-mirror fore-optics re-image each sub-field on its DMD which has 2048 x 1080 mirrors 13.6 μm wide with 2 possible tilts, one sending light to the spectrograph, the other to a light dump. The ATLAS Probe spectrographs use prisms as dispersive elements because of their higher and more uniform transmission, their larger bandwidth, and the ability to control the resolution slope with the choice of glasses. Each spectrograph has 2 cameras. While the collimator is made of 4 mirrors, each camera is made of only one mirror which reduces the total number of optics. All mirrors are aspheric but with a relatively small P-V with respect to their best fit sphere making them easily manufacturable. For imaging, a simple mirror to replace the prism is not an option because the aberrations are globally corrected by the collimator and camera together which gives large aberrations when the mirror is inserted. An achromatic grism is used instead. There are many variations of the design that permit very different packaging of the optics. ATLAS Probe will enable ground-breaking science in all areas of astrophysics. It will (1) revolutionize galaxy evolution studies by tracing the relation between galaxies and dark matter from the local group to cosmic voids and filaments, from the epoch of reionization through the peak era of galaxy assembly; (2) open a new window into the dark universe by mapping the dark matter filaments to unveil the nature of the dark Universe using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of gravity using cosmic large-scale structure; (3) probe the Milky Way's dust-shrouded regions, reaching the far side of our Galaxy; and (4) characterize asteroids and other objects in the outer solar systems.

Paper Details

Date Published: 22 August 2018
PDF: 15 pages
Proc. SPIE 10698, Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave, 106980I (22 August 2018); doi: 10.1117/12.2313082
Show Author Affiliations
Robert Content, Australian Astronomical Optics (Australia)
Yun Wang, Caltech (United States)
IPAC (United States)
Massimo Roberto, Space Telescope Science Institute (United States)
Johns Hopkins Univ. (United States)
Mark Dickinson, National Optical Astronomy Observatory (United States)
Henry Ferguson, Space Telescope Science Institute (United States)
Lynne Hillenbrand, Caltech (United States)
IPAC (United States)
Wesley Fraser, Queen's Univ. Belfast (United Kingdom)
Peter Behroozi, The Univ. of Arizona (United States)
Jarle Brinchmann, Leiden Observatory (Netherlands)
Andrea Cimatti, Univ. degli Studi di Bologna (Italy)
11INAF - Osservatorio Astrofisico di Arcetri (Italy)
Emanuele Daddi, CEA-IRFU (France)
Univ. Paris Diderot - Paris 7 (France)
Christopher Hirata, The Ohio State Univ. (United States)
Michael Hudson, Univ. of Waterloo (Canada)
J. Davy Kirkpatrick, Caltech (United States)
IPAC (United States)
Robert Barkhouser, Johns Hopkins Univ. (United States)
James Bartlett, Jet Propulsion Lab. (United States)
Robert Benjamin, Univ. of Wisconsin-Whitewater (United States)
Ranga Chary, Caltech (United States)
IPAC (United States)
Charlie Conroy, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Megan Donahue, Michigan State Univ. (United States)
Olivier Doré, Jet Propulsion Lab. (United States)
Peter Eisenhardt, Jet Propulsion Lab. (United States)
Karl Glazebrook, Swinburne Univ. of Technology (Australia)
George Helou, Caltech (United States)
IPAC (United States)
Sangeeta Malhotra, NASA Goddard Space Flight Ctr. (United States)
Lauro Moscardini, Univ. degli Studi di Bologna (Italy)
INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna (Italy)
INFN - Sezione di Bologna (Italy)
Zoran Ninkov, National Optical Astronomy Observatory (United States)
Alvaro Orsi, Ctr. de Estudios de Física del Cosmos de Aragón (Spain)
Michael Ressler, Jet Propulsion Lab. (United States)
James Rhoads, NASA Goddard Space Flight Ctr. (United States)
Jason Rhodes, Jet Propulsion Lab. (United States)
Alice Shapley, Univ. of California, Los Angeles (United States)
Stephen Smee, Johns Hopkins Univ. (United States)

Published in SPIE Proceedings Vol. 10698:
Space Telescopes and Instrumentation 2018: Optical, Infrared, and Millimeter Wave
Makenzie Lystrup; Howard A. MacEwen; Giovanni G. Fazio; Natalie Batalha; Nicholas Siegler; Edward C. Tong, Editor(s)

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