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Proceedings Paper

Wide Field X-ray Telescope: a moderate class mission
Author(s): Stephen S. Murray; R. Giacconi; A. Ptak; P. Rosati; M. Weisskopf; S. Borgani; C. Jones; G. Pareschi; P. Tozzi; R. Gilli; S. Campana; M. Paolillo; G. Tagliaferri; M. Bautz; A. Vikhlinin; R. Hickox; W. Forman
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Paper Abstract

Sensitive surveys of the X-ray universe have been limited to small areas of the sky due to the intrinsically small field of view of Wolter-I X-ray optics, whose angular resolution degrades with the square of the off axis angle. High angular resolution is needed to achieve a low background per source, minimize source confusion, and distinguish point from extended objects. WFXT consists of three co-aligned wide field X-ray telescopes with a 1° field of view and a≲ 10" (goal of 5") angular resolution (HEW) over the full field. Total effective area at 1 keV will be > 5000 cm2. WFXT will perform three surveys that will cover most of the extragalactic sky to 100-1000 times the sensitivity of the ROSAT All Sky Survey, ≳ 2000 deg2 to deep Chandra or XMM-Newton sensitivity, and ≳ 100 deg2 to the deepest Chandra sensitivity. WFXT will generate a legacy X-ray data set of ≳ 5 x 105 clusters and groups of galaxies to z ~ 2, also characterizing the physics of the intracluster gas for a significant fraction of them, thus providing an unprecedented data set for cosmological applications; it will detect > 107 AGN to z > 6, again obtaining spectra for a substantial fraction; it will detect > 105 normal/starburst galaxies; and it will detect and characterize star formation regions across the Galaxy. WFXT is the only X-ray survey mission that will match, in area and sensitivity, the next generation of wide-area optical, IR and radio surveys. http://wfxt.pha.jhu.edu

Paper Details

Date Published: 29 July 2010
PDF: 7 pages
Proc. SPIE 7732, Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray, 77321W (29 July 2010); doi: 10.1117/12.856921
Show Author Affiliations
Stephen S. Murray, Harvard-Smithsonian Ctr. for Astrophysics (United States)
The Johns Hopkins Univ. (United States)
R. Giacconi, The Johns Hopkins Univ. (United States)
A. Ptak, The Johns Hopkins Univ. (United States)
P. Rosati, European Southern Observatory (Germany)
M. Weisskopf, NASA Marshall Space Flight Ctr. (United States)
S. Borgani, Univ. of Trieste (Italy)
C. Jones, Harvard-Smithsonian Ctr. for Astrophysics (United States)
G. Pareschi, Osservatorio Astronomico di Brera (Italy)
P. Tozzi, Osservatorio Astronomico di Trieste (Italy)
R. Gilli, Osservatorio Astronomico di Trieste (Italy)
S. Campana, Osservatorio Astronomico di Brera (Italy)
M. Paolillo, Univ. of Naples (Italy)
G. Tagliaferri, Osservatorio Astronomico di Brera (Italy)
M. Bautz, Massachusetts Institute of Technology (United States)
A. Vikhlinin, Harvard-Smithsonian Ctr. for Astrophysics (United States)
R. Hickox, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Durham Univ. (United Kingdom)
W. Forman, Harvard-Smithsonian Ctr. for Astrophysics (United States)


Published in SPIE Proceedings Vol. 7732:
Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray
Monique Arnaud; Stephen S. Murray; Tadayuki Takahashi, Editor(s)

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