The Swift X-ray telescope

被引：77

作者：

Burrows, DN ^{[1
]}

Hill, JE ^{[1
]}

Nousek, JA ^{[1
]}

Wells, A ^{[1
]}

Chincarini, G ^{[1
]}

Abbey, AF ^{[1
]}

Beardmore, A ^{[1
]}

Bosworth, J ^{[1
]}

Bräuninger, HW ^{[1
]}

Burkert, W ^{[1
]}

Campana, S ^{[1
]}

Capalbi, M ^{[1
]}

Chang, W ^{[1
]}

Citterio, O ^{[1
]}

Freyberg, MJ ^{[1
]}

Giommi, P ^{[1
]}

Hartner, GD ^{[1
]}

Killough, R ^{[1
]}

Kittle, B ^{[1
]}

Klar, R ^{[1
]}

Mangels, C ^{[1
]}

McMeekin, M ^{[1
]}

Miles, BJ ^{[1
]}

Moretti, A ^{[1
]}

Mori, K ^{[1
]}

Morris, DC ^{[1
]}

Mukerjee, K ^{[1
]}

Osborne, JP ^{[1
]}

Short, ADT ^{[1
]}

Tagliaferri, G ^{[1
]}

Tamburelli, F ^{[1
]}

Watson, DJ ^{[1
]}

Willingale, R ^{[1
]}

Zugger, M ^{[1
]}

机构：

[1] Penn State Univ, Davey Lab 525, University Pk, PA 16802 USA

来源：

X-RAY AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY XIII | 2004年 / 5165卷

关键词：

gamma-ray burst; X-ray Telescope; Swift; X-ray instrumentation; X-ray CCD detector; X-ray mirrors;

D O I：

10.1117/12.504868

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

The Swift Gamma-Ray Explorer is designed to make prompt multiwavelength observations of Gamma-Ray Bursts (GRBs) and GRB Afterglows. The X-ray Telescope (XRT) provides key capabilities that permit Swift to determine GRB positions with a few arcseconds accuracy within 100 seconds of the burst onset. The XRT utilizes a superb mirror set(1) built for JET-X(2) and a state-of-the-art XMM/EPIC MOS CCD detector(3,4) to provide a sensitive broad-band (0.2-10 keV) X-ray imager with effective area of 135 cm(2) at 1.5 keV, field of view of 23.6 x 23.6 arcminutes, and angular resolution of 18 arcseconds (HEW). The detection sensitivity is 2x10(-14) erg/cm(2)/s in 10(4) seconds. The instrument is designed to provide automated source detection and position reporting within 5 seconds of target acquisition. It can also measure redshifts of GRBs for bursts with Fe line emission or other spectral features. The XRT will operate in an auto-exposure mode, adjusting the CCD readout mode automatically to optimize the science return for each frame as the source fades. The XRT will measure spectra and lightcurves of the GRB afterglow beginning about a minute after the burst and will follow each burst for days as it fades from view.

引用

页码：201 / 216

页数：16

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