| Issue |
A&A
Volume 392, Number 1, September II 2002
|
|
|---|---|---|
| Page(s) | 103 - 114 | |
| Section | Cosmology (including clusters of galaxies) | |
| DOI | https://doi.org/10.1051/0004-6361:20020921 | |
| Published online | 22 August 2002 | |
ROSAT PSPC view of the hot interstellar medium of the Magellanic Clouds*
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, Postfach 1312, 85741 Garching, Germany
Corresponding author: M. Sasaki, manami@mpe.mpg.de
Received:
15
March
2002
Accepted:
17
June
2002
Diffuse X-ray emission from the Magellanic Clouds (MCs) is
studied by using all the archival data of pointed ROSAT Position
Sensitive Proportional Counter (PSPC) observations.
For this purpose, contributions from the point and
point-like sources in the ROSAT High Resolution Imager (HRI) and
PSPC source catalogues
are eliminated and periods of high solar activity are excluded.
The spectral analysis yielded characteristic temperatures of
106–107 K for the hot thin plasma of the ISM which
extends over the whole Large Magellanic Cloud (LMC) and the Small
Magellanic Cloud (SMC). The total unabsorbed luminosity in the
0.1–2.4 keV band within the observed area amounts to
erg s-1 in the LMC and
erg s-1 in the SMC, each
with an uncertainty of ~-40%, +100%.
The X-ray luminosity of the LMC is comparable to that of
other nearby galaxies with pronounced star formation.
In the LMC, hot regions were found especially around the
supergiant shell (SGS) LMC 4 and in the field covering SGS LMC 2 and LMC 3.
Highest temperatures for the SMC were derived in the southwestern part of the
galaxy.
The diffuse X-ray emission is most likely a superposition of the emission from
the hot gas in the interior of shells and supershells as well as
from the halo of these galaxies.
Key words: shock waves / ISM: supernova remnants / galaxies: magellanic clouds / X-rays: ISM
© ESO, 2002
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