Hostname: page-component-cd9895bd7-p9bg8 Total loading time: 0 Render date: 2024-12-28T03:20:12.639Z Has data issue: false hasContentIssue false
  • English
  • Français

XMM-Newton survey of the Local Group galaxy M 33 – catalogue results and global properties

Published online by Cambridge University Press:  12 May 2006

Z. Misanovic ,
W. Pietsch ,
F. Haberl ,
M. Ehle ,
D. Hatzidimitriou  and
G. Trinchieri
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
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
G. Trinchieri
Affiliation:
Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy email: ginevra@brera.mi.astro.it
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.

Using 24 overlapping XMM-Newton observations of the Local Group spiral galaxy M 33, we have detected 447 sources in each individual pointing and in deep combined images. A total of 61 sources exhibit significant flux variations by a factor of up to 144, on time scales of hours to months or years. The detected variability, together with the hardness ratio (HR) method and optical identification (when available), is used to classify the sources as X-ray binaries (XRBs), supernova remnants (SNRs) and super-soft sources (SSS) in M 33, as well as background AGN and foreground stars in the field of view. The majority of sources can only be classified as ‘hard’, according to their HRs. We find that the luminosity distribution of the detected SNRs and SNR candidates in M 33 is similar to M 31, and slightly steeper than that of the LMC.

Keywords

X-rays: galaxiesX-rays: binaries(ISM:) supernova remnants
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S230: Populations of High Energy Sources in Galaxies , August 2005 , pp. 160 - 161
Copyright
2006 International Astronomical Union