Showing papers by "S. D. Hunsberger published in 2004"
Goddard Space Flight Center1, Brera Astronomical Observatory2, University of Milan3, University College London4, Pennsylvania State University5, University of Leicester6, Sonoma State University7, University of California, Berkeley8, Universities Space Research Association9, National Research Council10, University of Southampton11, Los Alamos National Laboratory12, National Radio Astronomy Observatory13, Space Telescope Science Institute14, Max Planck Society15, California Institute of Technology16, University of Texas at Austin17, French Alternative Energies and Atomic Energy Commission18, University of Toronto19, University of Maryland, College Park20, Princeton University21, Lawrence Livermore National Laboratory22, University of Cambridge23, University of California, Santa Barbara24, Rice University25, University of Tokyo26, Saitama University27, University of Florence28
TL;DR: The Swift mission as discussed by the authors is a multi-wavelength observatory for gamma-ray burst (GRB) astronomy, which is a first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions.
Abstract: The Swift mission, scheduled for launch in 2004, is a multiwavelength observatory for gamma-ray burst (GRB) astronomy. It is a first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions. It will be far more powerful than any previous GRB mission, observing more than 100 bursts yr � 1 and performing detailed X-ray and UV/optical afterglow observations spanning timescales from 1 minute to several days after the burst. The objectives are to (1) determine the origin of GRBs, (2) classify GRBs and search for new types, (3) study the interaction of the ultrarelativistic outflows of GRBs with their surrounding medium, and (4) use GRBs to study the early universe out to z >10. The mission is being developed by a NASA-led international collaboration. It will carry three instruments: a newgeneration wide-field gamma-ray (15‐150 keV) detector that will detect bursts, calculate 1 0 ‐4 0 positions, and trigger autonomous spacecraft slews; a narrow-field X-ray telescope that will give 5 00 positions and perform spectroscopy in the 0.2‐10 keV band; and a narrow-field UV/optical telescope that will operate in the 170‐ 600 nm band and provide 0B3 positions and optical finding charts. Redshift determinations will be made for most bursts. In addition to the primary GRB science, the mission will perform a hard X-ray survey to a sensitivity of � 1m crab (� 2;10 � 11 ergs cm � 2 s � 1 in the 15‐150 keV band), more than an order of magnitude better than HEAO 1 A-4. A flexible data and operations system will allow rapid follow-up observations of all types of
3,753 citations
03 Feb 2004
TL;DR: The UV/optical telescope (UVOT) is one of the three instruments flying aboard the Swift Gamma-ray Observatory (SGOA) as mentioned in this paper, which is designed to capture the early (~1 minute) UV and optical photons from the afterglow of gamma-ray bursts as well as long term observations of these afterglows.
Abstract: The UV/optical telescope (UVOT) is one of three instruments flying aboard the Swift Gamma-ray Observatory. It is designed to capture the early (~1 minute) UV and optical photons from the afterglow of gamma-ray bursts as well as long term observations of these afterglows. This is accomplished through the use of UV and optical broadband filters and grisms. The UVOT has a modified Ritchey-Chretien design with micro-channel plate intensified charged-coupled device detectors that provide sub-arcsecond imaging. Unlike most UV/optical telescopes the UVOT can operate in a photon-counting mode as well as an imaging mode. We discuss some of the science to be pursued by the UVOT and the overall design of the instrument.
52 citations
03 Feb 2004
TL;DR: Roming et al. as mentioned in this paper evaluated the performance of the Swift/UVOT and its photon counting detectors in a series of calibration measurements made under vacuum conditions in a test facility at the Goddard Space Flight Center.
Abstract: The Swift /UVOT is a 30-cm aperture imaging telescope that is sensitive to photons in the wavelength range 170nm-600nm and is designed to provide near-ultraviolet and optical measurements of -ray bursts and other targets that the Swift observatory observes. The performance of the telescope and its photon counting detectors has been assessed in a series of calibration measurements made under vacuum conditions in a test facility at the Goddard Space Flight Center. We describe some of the results of this campaign, including measurements of the instrument throughput, image quality and distortion, and linearity of response. We also describe the spectroscopic capability of the instrument, which is enabled by the use of two grisms operating in the UV and optical bands respectively. The results from the ground calibration activities will form the basis for establishing the full calibration matrix of the instrument once on orbit. 1 INTRODUCTION The UltraViolet and Optical Telescope (UVOT) on the Swift observatory is designed to register the light of -ray bursts over almost six orders of magnitude in brightness, in the range B~10-24. The instrument, which is described in more detail in the accompanying paper by Roming et al., is a development of the Optical/UV monitor telescope
12 citations
01 Oct 2004
TL;DR: The Ultra-Violet/Optical Telescope (UVOT) as mentioned in this paper is a Ritchey-Chretien telescope with MCP intensified CCD detectors which operate in either a photon-timing or an imaging mode while providing sub-arcsecond resolution.
Abstract: The Ultra‐Violet/Optical Telescope (UVOT), one of three telescopes to fly on the Swift Gamma‐ray Burst Observatory, is capable of detecting the early UV/optical photons and performing long‐term UV/optical observations of GRB afterglows. The UVOT is a Ritchey‐Chretien telescope with MCP intensified CCD detectors which operate in either a photon‐timing or an imaging mode while providing sub‐arcsecond resolution. A filter wheel accommodates broadband UV and visual filters for photometric studies including determination of photometric redshifts. UV and visual grisms for low‐resolution spectroscopy are also housed in the filter wheel. We present a brief overview of the UVOT, calibration results, and science to be carried out.
5 citations