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  • 2010-2014  (3)
  • 1
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    Properties of the Flight Model Gas Electron Multiplier for the GEMS Mission (2014)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: We present the gain properties of the gas electron multiplier (GEM) foil in pure dimethyl ether (DME) at 190 Torr. The GEM is one of the micro pattern gas detectors and it is adopted as a key part of the X-ray polarimeter for the GEMS mission. The X-ray polarimeter is a time projection chamber operating in pure DME gas at 190 Torr. We describe experimental results of (1) the maximum gain the GEM can achieve without any discharges, (2) the linearity of the energy scale for the GEM operation, and (3) the two-dimensional gain variation of the active area. First, our experiment with 6.4 keV X-ray irradiation of the whole GEM area demonstrates that the maximum effective gain is 2 x 10(exp 4) with the applied voltage of 580 V. Second, the measured energy scale is linear among three energies of 4.5, 6.4, and 8.0 keV. Third, the two-dimensional gain mapping test derives the standard deviation of the gain variability of 7% across the active area.
    Keywords: Instrumentation and Photography
    Type: GSFC-E-DAA-TN28531 , SPIE Astronomical Telescopes + Instrumentation 2014; Jun 22, 2014 - Jun 27, 2014; Montreal, Quebec; Canada|Proceedings of SPIE; 9144; 91444N|Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray; Jun 22, 2014 - Jun 27, 2014; Montreal, Quebec; Canada
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  • 2
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    Broad-Band Spectroscopy of Hercules X-1 with Suzaku (2014)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Hercules X-1 was observed with Suzaku in the main-on state from 2005 to 2010. The 0.4- 100 keV wide-band spectra obtained in four observations showed a broad hump around 4-9 keV in addition to narrow Fe lines at 6.4 and 6.7 keV. The hump was seen in all the four observations regardless of the selection of the continuum models. Thus it is considered a stable and intrinsic spectral feature in Her X-1. The broad hump lacked a sharp structure like an absorption edge. Thus it was represented by two different spectral models: an ionized partial covering or an additional broad line at 6.5 keV. The former required a persistently existing ionized absorber, whose origin was unclear. In the latter case, the Gaussian fitting of the 6.5-keV line needs a large width of sigma = 1.0-1.5 keV and a large equivalent width of 400-900 eV. If the broad line originates from Fe fluorescence of accreting matter, its large width may be explained by the Doppler broadening in the accretion flow. However, the large equivalent width may be inconsistent with a simple accretion geometry.
    Keywords: Astrophysics
    Type: GSFC-E-DAA-TN21608 , Publications of the Astronomical Society of Japan; 66; 2; 44(1-15)
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  • 3
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    Broad-band Spectroscopy of Hercules X-1 with Suzaku (2014)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Hercules X-1 was observed with Suzaku in the main-on state from 2005 to 2010. The 0.4100keV wide-band spectra obtained in four observations showed a broad hump around 49keV in addition to narrow Fe lines at 6.4 and 6.7keV. The hump was seen in all the four observations regardless of the selection of the continuum models. Thus it is considered a stable and intrinsic spectral feature in Her X-1. The broad hump lacked a sharp structure like an absorption edge. Thus it was represented by two different spectral models: an ionized partial covering or an additional broad line at 6.5keV. The former required a persistently existing ionized absorber, whose origin was unclear. In the latter case, the Gaussian fitting of the 6.5-keV line needs a large width of = 1.01.5keV and a large equivalent width of 400900 eV. If the broad line originates from Fe fluorescence of accreting matter, its large width may be explained by the Doppler broadening in the accretion flow. However, the large equivalent width may be inconsistent with a simple accretion geometry.
    Keywords: Instrumentation and Photography; Astrophysics
    Type: GSFC-E-DAA-TN64673 , Publications of the Astronomical Society of Japan (ISSN 0004-6264) (e-ISSN 2053-051X); 66; 2; 44
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