List of Figures

• The Spectrum-X-Gamma Satellite
• The SODART X-ray Telescope System
• Guide Star and Sun Constraints on SXG Viewing Direction
• OXS Viewing Constraints
• SODART Telescope Viewing Opportunities for Jan. & Feb. 2000 Figures 5 - 10 show visible areas of the sky (RA vs. Dec.) at one-month intervals. Here, ``Jet-X'' refers to the pointing direction of the Jet-X and (co-aligned) SODART telescopes.
• SODART Telescope Viewing Opportunities for March & April 2000
• SODART Telescope Viewing Opportunities for May & June 2000
• SODART Telescope Viewing Opportunities for July & Aug. 2000
• SODART Telescope Viewing Opportunities for Sept. & Oct. 2000
• SODART Telescope Viewing Opportunities for Nov. & Dec. 2000
• OXS Viewing Opportunities for Jan. & Feb. 2000 Figures 11 - 16 show visible areas of the sky (RA vs. Dec.) at one-month intervals.
• OXS Viewing Opportunities for March & April 2000
• OXS Viewing Opportunities for May & June 2000
• OXS Viewing Opportunities for July & Aug. 2000
• OXS Viewing Opportunities for Sept. & Oct. 2000
• OXS Viewing Opportunities for Nov. & Dec. 2000
• SODART on-axis effective area for a single module
• SODART vignetting function measured at three different energies
• On-axis image of a point source at 6.627 keV in FM1
• Point Response Function of the SODART MM at three different energies
• Encircled Energy Function of the SODART MM at three different energies.
• HEPC/LEPC Effective Area
• HEPC/LEPC Spatial Response
• HEPC count rates yielding 1 ASCA SIS c s^-1, for a power law spectrum. This and subsequent figures (25 - 50) are contour plots of count rate conversions derived from PIMMS.
• HEPC count rates yielding 1 ASCA GIS c s^-1, for a power law spectrum.
• HEPC count rates yielding 1 ROSAT PSPC c s^-1, for a power law spectrum.
• HEPC count rates yielding 1 ASCA SIS c s^-1, for a thermal bremsstrahlung spectrum.
• HEPC count rates yielding 1 ASCA GIS c s^-1, for a thermal bremsstrahlung spectrum.
• HEPC count rates yielding 1 ROSAT PSPC c s^-1, for a thermal bremsstrahlung spectrum.
• HEPC count rates yielding 1 ASCA SIS c s^-1, for a blackbody spectrum.
• HEPC count rates yielding 1 ASCA GIS c s^-1, for a blackbody spectrum.
• HEPC count rates yielding 1 ROSAT PSPC c s^-1, for a blackbody spectrum.
• LEPC low-band count rates yielding 1 ASCA SIS c s^-1, for a power law spectrum. This and subsequent figures (34 - 41) are contour plots of count rate conversions derived from PIMMS.
• LEPC low-band count rates yielding 1 ASCA GIS c s^-1, for a power law spectrum.
• LEPC low-band count rates yielding 1 ROSAT PSPC c s^-1, for a power law spectrum.
• LEPC low-band count rates yielding 1 ASCA SIS c s^-1, for a thermal bremsstrahlung spectrum.
• LEPC low-band count rates yielding 1 ASCA GIS c s^-1, for a thermal bremsstrahlung spectrum.
• LEPC low-band count rates yielding 1 ROSAT PSPC c s^-1, for a thermal bremsstrahlung spectrum.
• LEPC low-band count rates yielding 1 ASCA SIS c s^-1, for a blackbody spectrum.
• LEPC low-band count rates yielding 1 ASCA GIS c s^-1, for a blackbody spectrum.
• LEPC low-band count rates yielding 1 ROSAT PSPC c s^-1, for a blackbody spectrum.
• LEPC high-band count rates yielding 1 ASCA SIS c s^-1, for a power law spectrum.
• LEPC high-band count rates yielding 1 ASCA GIS c s^-1, for a power law spectrum.
• LEPC high-band count rates yielding 1 ROSAT PSPC c s^-1, for a power law spectrum.
• LEPC high-band count rates yielding 1 ASCA SIS c s^-1, for a thermal bremsstrahlung spectrum.
• LEPC high-band count rates yielding 1 ASCA GIS c s^-1, for a thermal bremsstrahlung spectrum.
• LEPC high-band count rates yielding 1 ROSAT PSPC c s^-1, for a thermal bremsstrahlung spectrum.
• LEPC high-band count rates yielding 1 ASCA SIS c s^-1, for a blackbody spectrum.
• LEPC high-band count rates yielding 1 ASCA GIS c s^-1, for a blackbody spectrum.
• LEPC high-band count rates yielding 1 ROSAT PSPC c s^-1, for a blackbody spectrum.
• LEPC pulse height spectrum simulated with XSPEC. A 5 ksec LEPC observation of a Raymond-Smith plasma with cosmic abundances, emission integral of 10⁶⁰ cm^-3, temperature of 10^7.5 K, column density of 10²¹ cm^-2, and distance of 10 kpc is simulated.
• HEPC pulse height spectrum simulated with XSPEC. A 5 ksec HEPC observation of a Raymond-Smith plasma with cosmic abundances, emission integral of 10⁶⁰ cm^-3, temperature of 10^7.5 K, column density of 10²¹ cm^-2, and distance of 10 kpc is simulated.
• Minimum Count Rate Detectable by LEPC. The minimum count rate for a 5$\sigma$ count rate significance is plotted as a function of exposure time, for 3 different background rates (in c s^-1) in a $2^{\prime }$ diameter aperture on-axis, using the formula given in section 4.4.4.
• Minimum Count Rate Detectable by HEPC. The minimum count rate for a 5$\sigma$ count rate significance is plotted as a function of exposure time, for 3 different background rates (in c s^-1) in a $2^{\prime }$ diameter aperture on-axis, using the formula given in section 4.4.4.
• OXS Effective Area
• An extended source emitting a He-like line series can be mapped in each spectral feature by combining data from a series of observations, each with a slightly different orientation of the crystal panel and telescope pointing direction. In any one orientation, specific regions of the source, as shown here, will satisfy the Bragg conditions for the Forbidden, Intercombination, and Resonance line energies and thus be imaged into corresponding regions on the detector. Different crystal/telescope orientations will sample different regions of the source.
• Array of 19 SIXA Detector Elements. Individual detector elements are labelled with SIXA pixel numbers.
• SIXA Effective Area
• SIXA count rates yielding 1 ASCA SIS c s^-1, for a power law spectrum. This and subsequent figures (60 - 67) are contour plots of count rate conversions derived from PIMMS. For conversion factors less than 1, one contour per decade is displayed. For factors greater than 1, contour intervals differ by $\sim$30%, on average.
• SIXA count rates yielding 1 ASCA GIS c s^-1, for a power law spectrum.
• SIXA count rates yielding 1 ROSAT PSPC c s^-1, for a power law spectrum.
• SIXA count rates yielding 1 ASCA SIS c s^-1, for a thermal bremsstrahlung spectrum.
• SIXA count rates yielding 1 ASCA GIS c s^-1, for a thermal bremsstrahlung spectrum.
• SIXA count rates yielding 1 ROSAT PSPC c s^-1, for a thermal bremsstrahlung spectrum.
• SIXA count rates yielding 1 ASCA SIS c s^-1, for a blackbody spectrum.
• SIXA count rates yielding 1 ASCA GIS c s^-1, for a blackbody spectrum.
• SIXA count rates yielding 1 ROSAT PSPC c s^-1, for a blackbody spectrum.
• SIXA pulse height spectrum simulated with XSPEC. A 5 ksec SIXA observation of a Raymond-Smith plasma with cosmic abundances, emission integral of 10⁶⁰ cm^-3, temperature of 10^7.5 K, column density of 10²¹ cm^-2, and distance of 10 kpc is simulated.
• Minimum Count Rate Detectable by SIXA The minimum count rate for a 5$\sigma$ count rate significance is plotted as a function of exposure time, for 3 different background rates (in c s^-1) in the central SIXA pixel, using the formula given in section 6.4.4.
• Minimum Equivalent Width at 6 keV detectable by SIXA The minimum detectable equivalent width at 6 keV is plotted as a function of source continuum, for 5 different exposure times in ksec, using the formula given in section 6.4.5. A 5$\sigma$significance is required and background rates of $3\times 10^{-3}$ counts cm^-2 s^-1 keV^-1 (instrumental) and $6.6\times 10^{-7}$ counts cm^-2 s^-1 keV^-1 pixel^-1(cosmic) are assumed.