XMM-Newton
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Next: 3.2.3 Response matrices used in the SAS data analysis
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3.2.2.2 Off-axis effective area
Not only the shape of the X-ray PSF, but also the effective area of the
mirrors is a function of off-axis angle within the mirrors'
FOV.
With increasing off-axis angle, less of the photons entering the telescopes
actually reach the focal plane. This effect is called ``vignetting''. The
vignetting of the XMM-Newton telescopes, which is reflected by the decline
of the X-ray telescope's effective area as a function of off-axis angle, is
displayed for a few energies for the X-ray telescope 2 in
Fig. 13.
Figure 13:
Vignetting function as a function of off-axis angle
(0
-15
, based on simulations), at a few selected energies, of
the X-ray telescope 2 in front of the pn camera
 |
The off-axis vignetting in the two telescopes with an RGA has
a dependence on angle with respect to the RGAs' dispersion direction.
A source at an off-axis position perpendicular to the dispersion direction
will be vignetted by a different amount to one at a position parallel
to the dispersion direction. This azimuthal dependency of the vignetting
is shown in Fig. 14.
Figure 14:
Vignetting function as a function of azimuth angle of the
X-ray telescope 3 in front of the MOS1 camera. The curves are given for an
off-axis angle of 10 arcmin. Due to the presence of reflection grating
assemblies in the exit beams of the X-ray telescopes 3 and 4, the vignetting
functions measured in the MOS cameras are modulated azimuthally.
 |
Next: 3.2.3 Response matrices used in the SAS data analysis
Up: 3.2.2 X-ray effective area
Previous: 3.2.2.1 On-axis effective area
European Space Agency - XMM-Newton Science Operations Centre