The Swift X-Ray Telescope

David N. Burrows; J. E. Hill; J. A. Nousek; A. Wells; G. Chincarini; A. F. Abbey; A. Beardmore; J. Bosworth; H. W. Bräuninger; W. Burkert; S. Campana; M. Capalbi; W. Chang; O. Citterio; M. J. Freyberg; P. Giommi; G. D. Hartner; R. Killough; B. Kittle; R. Klar; C. Mangels; M. McMeekin; B. J. Miles; A. Moretti; K. Mori; D. C. Morris; K. Mukerjee; J. P. Osborne; A. D.T. Short; G. Tagliaferri; F. Tamburelli; D. J. Watson; R. Willingale; M. Zugger

doi:10.1117/12.504868

The Swift X-Ray Telescope

David N. Burrows, J. E. Hill, J. A. Nousek, A. Wells, G. Chincarini, A. F. Abbey, A. Beardmore, J. Bosworth, H. W. Bräuninger, W. Burkert, S. Campana, M. Capalbi, W. Chang, O. Citterio, M. J. Freyberg, P. Giommi, G. D. Hartner, R. Killough, B. Kittle, R. KlarC. Mangels, M. McMeekin, B. J. Miles, A. Moretti, K. Mori, D. C. Morris, K. Mukerjee, J. P. Osborne, A. D.T. Short, G. Tagliaferri, F. Tamburelli, D. J. Watson, R. Willingale, M. Zugger

Astronomy & Astrophysics

Research output: Contribution to journal › Conference article › peer-review

89 Scopus citations

Abstract

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 × 23.6 arcminutes, and angular resolution of 18 arcseconds (HEW). The detection sensitivity is 2×10 ^-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.

Original language	English (US)
Pages (from-to)	201-216
Number of pages	16
Journal	Proceedings of SPIE - The International Society for Optical Engineering
Volume	5165
DOIs	https://doi.org/10.1117/12.504868
State	Published - 2004
Event	X-Ray and Gamma-Ray Instrumentation for Astronomy XIII - San Diego, CA, United States Duration: Aug 3 2003 → Aug 5 2003

All Science Journal Classification (ASJC) codes

Electronic, Optical and Magnetic Materials
Condensed Matter Physics
Computer Science Applications
Applied Mathematics
Electrical and Electronic Engineering

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10.1117/12.504868

Cite this

Burrows, D. N., Hill, J. E., Nousek, J. A., Wells, A., Chincarini, G., Abbey, A. F., Beardmore, A., Bosworth, J., Bräuninger, H. W., Burkert, W., Campana, S., Capalbi, M., Chang, W., Citterio, O., Freyberg, M. J., Giommi, P., Hartner, G. D., Killough, R., Kittle, B., ... Zugger, M. (2004). The Swift X-Ray Telescope. Proceedings of SPIE - The International Society for Optical Engineering, 5165, 201-216. https://doi.org/10.1117/12.504868

@article{435f54ab6d654353ad3c39b98b94d14c,

title = "The Swift X-Ray Telescope",

abstract = "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 × 23.6 arcminutes, and angular resolution of 18 arcseconds (HEW). The detection sensitivity is 2×10 -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.",

author = "Burrows, {David N.} and Hill, {J. E.} and Nousek, {J. A.} and A. Wells and G. Chincarini and Abbey, {A. F.} and A. Beardmore and J. Bosworth and Br{\"a}uninger, {H. W.} and W. Burkert and S. Campana and M. Capalbi and W. Chang and O. Citterio and Freyberg, {M. J.} and P. Giommi and Hartner, {G. D.} and R. Killough and B. Kittle and R. Klar and C. Mangels and M. McMeekin and Miles, {B. J.} and A. Moretti and K. Mori and Morris, {D. C.} and K. Mukerjee and Osborne, {J. P.} and Short, {A. D.T.} and G. Tagliaferri and F. Tamburelli and Watson, {D. J.} and R. Willingale and M. Zugger",

year = "2004",

doi = "10.1117/12.504868",

language = "English (US)",

volume = "5165",

pages = "201--216",

journal = "Proceedings of SPIE - The International Society for Optical Engineering",

issn = "0277-786X",

publisher = "SPIE",

note = "X-Ray and Gamma-Ray Instrumentation for Astronomy XIII ; Conference date: 03-08-2003 Through 05-08-2003",

}

Burrows, DN, Hill, JE, Nousek, JA, Wells, A, Chincarini, G, Abbey, AF, Beardmore, A, Bosworth, J, Bräuninger, HW, Burkert, W, Campana, S, Capalbi, M, Chang, W, Citterio, O, Freyberg, MJ, Giommi, P, Hartner, GD, Killough, R, Kittle, B, Klar, R, Mangels, C, McMeekin, M, Miles, BJ, Moretti, A, Mori, K, Morris, DC, Mukerjee, K, Osborne, JP, Short, ADT, Tagliaferri, G, Tamburelli, F, Watson, DJ, Willingale, R & Zugger, M 2004, 'The Swift X-Ray Telescope', Proceedings of SPIE - The International Society for Optical Engineering, vol. 5165, pp. 201-216. https://doi.org/10.1117/12.504868

TY - JOUR

T1 - The Swift X-Ray Telescope

AU - Burrows, David N.

AU - Hill, J. E.

AU - Nousek, J. A.

AU - Wells, A.

AU - Chincarini, G.

AU - Abbey, A. F.

AU - Beardmore, A.

AU - Bosworth, J.

AU - Bräuninger, H. W.

AU - Burkert, W.

AU - Campana, S.

AU - Capalbi, M.

AU - Chang, W.

AU - Citterio, O.

AU - Freyberg, M. J.

AU - Giommi, P.

AU - Hartner, G. D.

AU - Killough, R.

AU - Kittle, B.

AU - Klar, R.

AU - Mangels, C.

AU - McMeekin, M.

AU - Miles, B. J.

AU - Moretti, A.

AU - Mori, K.

AU - Morris, D. C.

AU - Mukerjee, K.

AU - Osborne, J. P.

AU - Short, A. D.T.

AU - Tagliaferri, G.

AU - Tamburelli, F.

AU - Watson, D. J.

AU - Willingale, R.

AU - Zugger, M.

PY - 2004

Y1 - 2004

N2 - 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 × 23.6 arcminutes, and angular resolution of 18 arcseconds (HEW). The detection sensitivity is 2×10 -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.

AB - 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 × 23.6 arcminutes, and angular resolution of 18 arcseconds (HEW). The detection sensitivity is 2×10 -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.

UR - http://www.scopus.com/inward/record.url?scp=1942484068&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=1942484068&partnerID=8YFLogxK

U2 - 10.1117/12.504868

DO - 10.1117/12.504868

M3 - Conference article

AN - SCOPUS:1942484068

SN - 0277-786X

VL - 5165

SP - 201

EP - 216

JO - Proceedings of SPIE - The International Society for Optical Engineering

JF - Proceedings of SPIE - The International Society for Optical Engineering

T2 - X-Ray and Gamma-Ray Instrumentation for Astronomy XIII

Y2 - 3 August 2003 through 5 August 2003

ER -

The Swift X-Ray Telescope

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