Wijnands, Rin't Zand, JJMRupen, MMaccarone, THoman, JCornelisse, RFender, RGrindlay, Jvan der Klis, MKuulkers, EMarkwardt, CBMiller-Jones, JCAWang, QD2024-04-262024-04-262006-01-01https://doi.org/10.1051/0004-6361:20054129https://hdl.handle.net/20.500.14394/2699<p>This is the pre-published version harvested from ArXiv. The published version is located at <a href="http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361:20054129&Itemid=129">http://www.aanda.org/index.php?option=com_article&access=doi&doi=10.1051/0004-6361:20054129&Itemid=129</a></p>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).accretionaccretion disks -- binaries: close -- X-rays: binariesAstrophysics and Astronomyarticle