HEAD Division Meeting 1999, April 1999
Session 17. Missions and Instruments
Poster, Tuesday, April 13, 1999, 8:30am-6:02pm, Gold Room

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[17.20] The Swift X-ray Telescope

D.N. Burrows, J.A. Nousek, J.E. Hill (Penn State U.), A. Wells, M. Turner, R. Willingale, A. Holland (Leicester U.), O. Citterio, G. Chincarini, S. Campana, G. Tagliaferri (OAB), Swift XRT Team

The Swift Gamma Ray Burst Explorer will observe hundreds of gamma ray bursts per year and study their X-ray and optical afterglows, using a multiwavelength complement of three instruments: a wide-field Burst Alert Telescope (BAT), an X-Ray Telescope (XRT), and a UV/Optical Telescope (UVOT).

The XRT is designed to study X-ray counterparts of the gamma ray bursts and their afterglows, beginning within ~50 s from the time of the burst, and extending for days or weeks following the burst. The XRT utilizes a superb mirror set built for JET-X (Citterio et al. 1996) and a state-of-the-art XMM/EPIC CCD detector to provide a sensitive broad-band (0.2-10 keV) X-ray imager with effective area of 110 cm2 at 1.5 keV, and field of view of 23.6 \times 23.6 arcminutes, and angular resolution of 15 arcsec HPD. The sensitivity is 2 \times 10-14 erg cm-2 s-1 in 104 seconds. The telescope electronics will be designed to provide automated source detection and position reporting, with position good to 2.5 arcseconds transmitted to the ground within two minutes of the burst detection. 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 within about a minute after the burst and will follow each burst until it fades from view, typically monitoring 2-3 ``old'' bursts at a time while waiting for a new burst to be detected.


If the author provided an email address or URL for general inquiries, it is as follows:
http://www.astro.psu.edu/xray/swift/

burrows@astro.psu.edu


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