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 cm 2. 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 deg 2 to deep Chandra or XMM-Newton sensitivity, and ≳100 deg 2 to the deepest Chandra sensitivity. WFXT will generate a legacy X-ray data set of ≳5 × 10 5 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 > 10 7 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.

Wide Field X-ray Telescope: a moderate class mission / S. S., Murray; R., Giacconi; A., Ptak; P., Rosati; M., Weisskopf; S., Borgani; C., Jones; G., Pareschi; P., Tozzi; R., Gilli; S., Campana; Paolillo, Maurizio; G., Tagliaferri; M., Bautz; A., Vikhlinin; R., Hickox; W., Forman. - STAMPA. - 7732:(2010), pp. 77321W-77321W-7. (Intervento presentato al convegno Space Telescopes and Instrumentation 2010 tenutosi a USA nel 2010-#jul#) [10.1117/12.856921].

Wide Field X-ray Telescope: a moderate class mission

PAOLILLO, MAURIZIO;
2010

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 cm 2. 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 deg 2 to deep Chandra or XMM-Newton sensitivity, and ≳100 deg 2 to the deepest Chandra sensitivity. WFXT will generate a legacy X-ray data set of ≳5 × 10 5 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 > 10 7 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.
2010
9780819482228
Wide Field X-ray Telescope: a moderate class mission / S. S., Murray; R., Giacconi; A., Ptak; P., Rosati; M., Weisskopf; S., Borgani; C., Jones; G., Pareschi; P., Tozzi; R., Gilli; S., Campana; Paolillo, Maurizio; G., Tagliaferri; M., Bautz; A., Vikhlinin; R., Hickox; W., Forman. - STAMPA. - 7732:(2010), pp. 77321W-77321W-7. (Intervento presentato al convegno Space Telescopes and Instrumentation 2010 tenutosi a USA nel 2010-#jul#) [10.1117/12.856921].
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11588/374074
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