Reference : An XMM-Newton view of the M 17 nebula
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
An XMM-Newton view of the M 17 nebula
Mernier, François mailto [Université de Liège - ULiège > > GAPHE : Astrophysique observationnelle (sol et espace) >]
Rauw, Grégor mailto [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Sciences spatiales >]
New Astronomy
[en] We present the analysis of an XMM-Newton observation of the M 17 nebula. The X-ray point source population consists of massive O-type stars and a population of probable low-mass pre-main sequence stars. CEN 1a,b and OI 352, the X-ray brightest O-type stars in M 17, display hard spectra (kT of 3.8 and 2.6 keV) consistent with a colliding wind origin in binary/multiple systems. We show that the strong interstellar reddening towards the O-type stars of M 17 yields huge uncertainties on their L[SUB]X[/SUB]/L[SUB]bol[/SUB] values. The low-mass pre-main sequence stars exhibit hard spectra resulting from a combination of high plasma temperatures and very large interstellar absorption. We find evidence for considerable long term (months to years) variability of these sources. M 17 is one of the few star formation complexes in our Galaxy producing diffuse X-ray emission. We analyze the spectrum of this emission and compare it with previous studies. Finally, we discuss the Optical Monitor UV data obtained simultaneously with the X-ray images. We find very little correspondence between the UV and X-ray sources, indicating that the majority of the UV sources are foreground stars, whilst the bulk of the X-ray sources are deeply embedded in the M 17 complex.

File(s) associated to this reference

Fulltext file(s):

Open access
1210.2936v1.pdfAuthor preprint461.47 kBView/Open

Bookmark and Share SFX Query

All documents in ORBi are protected by a user license.