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- 5.1. Data points indicate the C column density of the
contaminant derived from observations. The solid lines indicate
the best fit empirical model to the temporal evolution of the
contamination for each sensor, as available, e.g. for
xissimarfgen, through the CALDB files released
in 2013 September (ae_xiN_contami_20130813.fits). The
dashed lines indicate the previous version of the calibration
- 5.2. Same as Fig. 5.1 but for the O column density.
- 5.3. Same as Fig. 5.1 but for the N column density.
- 5.4. 2011 April 26 observation of PKS2155304 fitted using (a) old and (b) new models of the contaminant.
- 5.5. 2012 June 11 observation of the Cygnus Loop fitted using (a) old and (b) new models of the contaminant.
- . Example for typical residuals around 2keV due to
instrumental effects (blue: BI - XIS1, red, combined FI -
XIS0+3), with respect to a smooth continuum fit (top) and modeled
with two Gaussian lines (bottom), see text for line energies
(Suchy et al., 2011, ApJ, 733,
15). The 2012
improvements (see text) are not taken into account. While these
improvements reduce the residuals their typical shape is still
apparent in some observations.
- . Spectra and best fit models for an observation of
GX3012 including data from the three individual XIS
instruments and the two HXD instruments. At lower energies, one
clearly sees the constant level in the modeled flux discussed in
the text (Suchy et al., 2012, ApJ, 745,
- 5.8. Example of an overall PIN spectrum with noise contamination.
- 5.9. Example of 64 individual PIN spectra with noise contamination.
- 5.10. HXD-PIN (black) and HXD-GSO (red) spectra and fit residuals
for the Crab as observed on 2005 Sep. 15 using the nominal HXD
pointing position. The adopted model is
=3.810cm, photon indices of 2.09
and 2.27, a break energy of 103keV, and a nomalization of
10.9photos keV cm s (at 1keV). To
illustrate the effect of the correction arf file, fit residuals
without applying the file are displayed as well (blue). The 20%
difference of the 70-400keV flux between the data and the model
without the arf and the bump-like residual around 50-70keV due to
calibration uncertainties around the Gd-K edge are reduced by
introducing the correction arf file, resulting in better agreement
with the HXD-PIN spectrum.
- 5.11. Relative flux normalization between different
- 6.1. Example for an extraction region for a point source.
- 6.2. Example for extraction regions for an extended source.
- 6.3. Incident versus observed count rates of a point source for
the FI sensor. The thick colored lines show the range that can be
observed without strong pile-up for a given window option (defined
by the figure legend) and burst option (defined by the time values
indicated in the figure). Note that the window frame
times are 8, 2, and 1s for the full, 1/4, and 1/8
window options, respectively, with exposures per frame of
for a given burst option.
- 7.1. Schematic picture of the HXD instrument, which consists of
two types of detectors: the PIN diodes located in the front of the GSO
scintillator, and the scintillator itself.
- 7.2. Numbering of the well- and
- 7.3. Example for a GSO spectrum as observed for Cygnus X-1 on
April 8, 2009. The black, red, green, and blue data show the raw
data, NXB, raw data NXB, and 1% NXB spectrum,
respectively. Since the systematic uncertainty of the NXB would be
at most 3% at present, the source is clearly detected up to
- 7.4. Example for a GSO light curve as observed for Cygnus X-1 on
April 8, 2009. The black, red, and green data show the raw data,
NXB, and raw data NXB light curve, respectively. 20counts/s
is a typical count rate of Cyg X-1.
- 7.5. Typical one-day WAM light curve.