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Proceedings Paper

Arcus: the x-ray grating spectrometer explorer
Author(s): R. K. Smith; M. H. Abraham; R. Allured; M. Bautz; J. Bookbinder; J. N. Bregman; L. Brenneman; N. S. Brickhouse; D. N. Burrows; V. Burwitz; R. Carvalho; P. N. Cheimets; E. Costantini; S. Dawson; C. DeRoo; A. Falcone; A. R. Foster; C. E. Grant; R. K. Heilmann; E. Hertz; B. Hine; D. Huenemoerder; J. S. Kaastra; K. K. Madsen; R. L. McEntaffer; E. D. Miller; J. Miller; E. Morse; R. Mushotzky; K. Nandra; M. Nowak; F. Paerels; R. Petre; L. Plice; K. Poppenhaeger; A. Ptak; P. Reid; J. Sanders; M. L. Schattenburg; N. Schulz; A. Smale; P. Temi; L. Valencic; S. Walker; R. Willingale; J. Wilms; S. J. Wolk
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Paper Abstract

Arcus will be proposed to the NASA Explorer program as a free-flying satellite mission that will enable high-resolution soft X-ray spectroscopy (8-50) with unprecedented sensitivity – effective areas of >500 sq cm and spectral resolution >2500. The Arcus key science goals are (1) to determine how baryons cycle in and out of galaxies by measuring the effects of structure formation imprinted upon the hot gas that is predicted to lie in extended halos around galaxies, groups, and clusters, (2) to determine how black holes influence their surroundings by tracing the propagation of out-flowing mass, energy and momentum from the vicinity of the black hole out to large scales and (3) to understand how accretion forms and evolves stars and circumstellar disks by observing hot infalling and outflowing gas in these systems. Arcus relies upon grazing-incidence silicon pore X-ray optics with the same 12m focal length (achieved using an extendable optical bench) that will be used for the ESA Athena mission. The focused X-rays from these optics will then be diffracted by high-efficiency off-plane reflection gratings that have already been demonstrated on sub-orbital rocket flights, imaging the results with flight-proven CCD detectors and electronics. The power and telemetry requirements on the spacecraft are modest. The majority of mission operations will not be complex, as most observations will be long (~100 ksec), uninterrupted, and pre-planned, although there will be limited capabilities to observe targets of opportunity, such as tidal disruption events or supernovae with a 3-5 day turnaround. After the end of prime science, we plan to allow guest observations to maximize the science return of Arcus to the community.

Paper Details

Date Published: 30 September 2016
PDF: 7 pages
Proc. SPIE 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, 99054M (30 September 2016); doi: 10.1117/12.2231778
Show Author Affiliations
R. K. Smith, Smithsonian Astrophysical Observatory (United States)
M. H. Abraham, The Aerospace Corp. (United States)
R. Allured, Smithsonian Astrophysical Observatory (United States)
M. Bautz, Massachusetts Institute of Technology (United States)
J. Bookbinder, NASA Ames Research Ctr. (United States)
J. N. Bregman, Univ. of Michigan (United States)
L. Brenneman, The Aerospace Corp. (United States)
N. S. Brickhouse, Smithsonian Astrophysical Observatory (United States)
D. N. Burrows, The Pennsylvania State Univ. (United States)
V. Burwitz, Max-Planck-Institut für extraterrestrische Physik (Germany)
R. Carvalho, NASA Ames Research Ctr. (United States)
P. N. Cheimets, Smithsonian Astrophysical Observatory (United States)
E. Costantini, SRON Netherlands Institute for Space Research (Netherlands)
S. Dawson, NASA Ames Research Ctr. (United States)
C. DeRoo, Smithsonian Astrophysical Observatory (United States)
A. Falcone, The Pennsylvania State Univ. (United States)
A. R. Foster, Smithsonian Astrophysical Observatory (United States)
C. E. Grant, Massachusetts Institute of Technology (United States)
R. K. Heilmann, Massachusetts Institute of Technology (United States)
E. Hertz, Smithsonian Astrophysical Observatory (United States)
B. Hine, NASA Ames Research Ctr. (United States)
D. Huenemoerder, Massachusetts Institute of Technology (United States)
J. S. Kaastra, SRON Netherlands Institute for Space Research (Netherlands)
K. K. Madsen, California Institute of Technology (United States)
R. L. McEntaffer, The Pennsylvania State Univ. (United States)
E. D. Miller, Massachusetts Institute of Technology (United States)
J. Miller, Univ. of Michigan (United States)
E. Morse, Orbital ATK (United States)
R. Mushotzky, Univ. of Maryland, College Park (United States)
K. Nandra, Max-Planck-Institut für extraterrestrische Physik (Germany)
M. Nowak, Massachusetts Institute of Technology (United States)
F. Paerels, Columbia Univ. (United States)
R. Petre, NASA Goddard Space Flight Ctr. (United States)
L. Plice, NASA Ames Research Ctr. (United States)
K. Poppenhaeger, Queen's Univ. Belfast (United Kingdom)
A. Ptak, NASA Goddard Space Flight Ctr. (United States)
P. Reid, Smithsonian Astrophysical Observatory (United States)
J. Sanders, Max-Planck-Institut für extraterrestrische Physik (Germany)
M. L. Schattenburg, Massachusetts Institute of Technology (United States)
N. Schulz, Massachusetts Institute of Technology (United States)
A. Smale, NASA Goddard Space Flight Ctr. (United States)
P. Temi, NASA Ames Research Ctr. (United States)
L. Valencic, Johns Hopkins Univ. (United States)
S. Walker, NASA Ames Research Ctr. (United States)
R. Willingale, Univ. of Leicester (United Kingdom)
J. Wilms, Friedrich-Alexander-Univ. Erlangen-Nürnberg (Germany)
S. J. Wolk, Harvard-Smithsonian Ctr. for Astrophysics (United States)


Published in SPIE Proceedings Vol. 9905:
Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray
Jan-Willem A. den Herder; Tadayuki Takahashi; Marshall Bautz, Editor(s)

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