The X-ray stellar population of the LMC

[en] In the study of stars, the high energy domain occupies a place of choice, since it is the only one able to directly probe the most violent phenomena: indeed, young pre-main sequence objects, hot massive stars, or X-ray binaries are best revealed in X-rays. However, previously available X-ray observatories often provided only crude information on individual objects in the Magellanic Clouds. The advent of the highly efficient X-ray facilities XMM-Newton and Chandra has now dramatically increased the sensitivity and the spatial resolution available to X-ray astronomers, thus enabling a fairly easy determination of the properties of individual sources in the LMC.

Research Center/Unit :

STAR - Space sciences, Technologies and Astrophysics Research - ULiège

Disciplines :

Space science, astronomy & astrophysics

Author, co-author :

Nazé, Yaël ; Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Sciences spatiales

Language :

English

Title :

The X-ray stellar population of the LMC

Publication date :

01 March 2009

Event name :

The Magellanic System: Stars, Gas, and Galaxies, IAU S256

Event date :

2008

By request :

Yes

Audience :

International

Journal title :

Proceedings of the International Astronomical Union

ISSN :

1743-9213

eISSN :

1743-9221

Publisher :

Cambridge University Press, Cambridge, United Kingdom

Additional URL :

http://adsabs.harvard.edu/abs/2009IAUS..256...20N
http://de.arxiv.org/abs/0808.3924

Available on ORBi :

since 02 July 2009

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