3.7 Comparison with other X-ray satellites
A basic comparison of XMM-Newton's properties with those of Chandra, ROSAT,
ASCA, RXTE, Swift, Suzaku and NuSTAR is given in Table 28.
It is immediately clear
that Chandra and XMM-Newton have complementary characteristics and that both
have constituted a new generation of X-ray missions, with enormously improved
capabilities compared to their predecessors ASCA, ROSAT and RXTE.
Notes to Table 28:
Comparison of XMM-Newton with other X-ray satellites
||A at 1 keV
||at 1 keV [eV]
||0.15 - 12
||0.1 - 10
|| 555 (ACIS-S)
||0.1 - 2.4
||0.5 - 10
||96 - 120
||108 - 138
||0.2 - 600
a) Mirror effective area.
b) Note that Figs. 11 and
12 do not just show the mirror effective areas
but have the EPIC detector responses included as well.
c) Orbital visibility outside the particle-radiation dominated zone.
d) The Chandra High Resolution Camera (HRC) spatial response is well matched
to the mirror resolution and the intrinsic on-axis PSF of the HRC is well
modelled by a Gaussian with a FWHM of 0.4 arcsec. The spatial resolution
for on-axis imaging with the ACIS instrument is limited by the physical
size of the CCD pixels (0.492 arcsec) and not the mirrors.
e) Low orbit with Earth occultation.
f) At 1.5 keV.
g) n.av.: not available, n.a.: not applicable.
Some special strengths of XMM-Newton are e.g.:
- Extreme sensitivity to extended emission.
- High-resolution spectroscopy (RGS) with simultaneous
medium-resolution spectroscopy and imaging (EPIC) and optical/UV
- High sensitivity (EPIC) at high energies.
- Excellent low energy response down to 0.15 keV.
- High time resolution (EPIC).
European Space Agency - XMM-Newton Science Operations Centre