Hostname: page-component-8448b6f56d-t5pn6 Total loading time: 0 Render date: 2024-04-24T03:35:44.872Z Has data issue: false hasContentIssue false
  • English
  • Français

XMM-Newton survey of the Local Group galaxy M33 – bright individual sources

Published online by Cambridge University Press:  12 May 2006

Z. Misanovic ,
W. Pietsch ,
F. Haberl ,
G. Trinchieri ,
M. Ehle  and
D. Hatzidimitriou
Z. Misanovic
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany email: zdenka@mpe.mpg.de, wnp@mpe.mpg.de, fwh@mpe.mpg.de
W. Pietsch
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany email: zdenka@mpe.mpg.de, wnp@mpe.mpg.de, fwh@mpe.mpg.de
F. Haberl
Affiliation:
Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85741 Garching, Germany email: zdenka@mpe.mpg.de, wnp@mpe.mpg.de, fwh@mpe.mpg.de
G. Trinchieri
Affiliation:
Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy email: ginevra@brera.mi.astro.it
M. Ehle
Affiliation:
XMM-Newton Science Operations Centre, ESAC, ESA, P.O. Box 50727, 28080 Madrid, Spain email: Matthias.Ehle@sciops.esa.int
D. Hatzidimitriou
Affiliation:
Department of Physics, University of Crete, P/O. Box 2208, 71003 Heraklion, Crete, Greece email: dh@physics.uoc.gr
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

As shown in our first poster, in a recent survey of M33 with XMM-Newton we detected the X-ray source population of this nearby spiral galaxy down to the (0.2-4.5) keV luminosity of $10^{35}$ erg s$^{-1}$, a factor of 10 deeper than in previous observations. The majority of the detected sources was classified using, in many cases, only their X-ray properties. In particular, 8 new X-ray binary (XRB) candidates were selected, based on their long-term X-ray light curves. We also classified supernova remnants (SNRs), super-soft sources (SSS), AGN, foreground stars and a population of ‘hard’ sources using the hardness ratio (HR) method. A detailed spectral and timing analysis of the brightest sources is in progress. We present a few examples of spectra for particular source classes. We find that bright ‘hard’ sources can be divided into two broad families: one best modelled by a powerlaw with photon index in the range of 1.0–2.0, and the other displaying disk blackbody spectra with kT of 0.8 to 1.5 keV.

Keywords

X-rays: galaxiesX-rays: binaries
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S230: Populations of High Energy Sources in Galaxies , August 2005 , pp. 162 - 163
Copyright
2006 International Astronomical Union