Volume 449, Number 3, April III 2006
|Page(s)||1117 - 1127|
|Section||Stellar structure and evolution|
|Published online||24 March 2006|
The XMM-Newton/Chandra monitoring campaign of the Galactic center region
Description of the program and preliminary results
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ, The Netherlands e-mail: [rudy;michiel;jmiller]@science.uva.nl
2 SRON National Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands e-mail: email@example.com
3 National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro, NM 87801, USA
4 NASA, Goddard Space Flight Center, Greenbelt, MD 20711, USA e-mail: [mrupen;craigm]@milkyway.gsfc.nasa.gov
5 School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK e-mail: [tjm;cornelis]@astro.soton.ac.uk;firstname.lastname@example.org
6 Center for Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA e-mail: email@example.com
7 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA e-mail: firstname.lastname@example.org
8 ISOC, ESA/ESAC, Urb. Villafranca del Castillo, PO Box 50727, 28080 Madrid, Spain e-mail: Erik.Kuulkers@esa.int
9 Department of Astronomy, University of Maryland, College Park, MD 20742, USA
10 Astronomy Department, University of Massachusetts, Amherst, MA 01003, USA e-mail: email@example.com
Accepted: 10 December 2005
We present the first results of our X-ray monitoring campaign on a 1.7 square degree region centered on Sgr A* using the satellites XMM-Newton and Chandra. The purpose of this campaign is to monitor the behavior (below 10 keV) of X-ray sources (both persistent and transient) which are too faint to be detected by monitoring instruments aboard other satellites currently in orbit (e.g., Rossi X-ray Timing Explorer; INTEGRAL). Our first monitoring observations (using the HRC-I aboard Chandra) were obtained on June 5, 2005. Most of the sources detected could be identified with foreground sources, such as X-ray active stars. In addition we detected two persistent X-ray binaries (1E 1743.1–2843; 1A 1742–294), two faint X-ray transients (GRS 1741.9–2853; XMM J174457–2850.3), as well as a possible new transient source at a luminosity of a few times 1034 erg s-1. We report on the X-ray results on these systems and on the non-detection of the transients in follow-up radio data using the Very Large Array. We discuss how our monitoring campaign can help to improve our understanding of the different types of X-ray transients (i.e., the very faint ones).
Key words: accretion, accretion disks / binaries: close / X-rays: binaries
© ESO, 2006
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.