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First results from the XMM-Newton / Chandra 13 hour deep survey

First results from the XMM-Newton / Chandra 13 hour deep survey. Mat Page 1 , Keith Mason 1 , Ian M c Hardy 2 , Katherine Gunn 2 , Tim Sasseen 3 , Nicola Loaring 1 , Andy Newsam 4 , Tom Vestrand 5 , Kaz Sekiguchi 6. 1 Mullard Space Science Laboratory, University College London, UK

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First results from the XMM-Newton / Chandra 13 hour deep survey

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  1. First results from the XMM-Newton / Chandra 13 hour deep survey Mat Page1, Keith Mason1, Ian McHardy2, Katherine Gunn2, Tim Sasseen3, Nicola Loaring1, Andy Newsam4, Tom Vestrand5, Kaz Sekiguchi6 1 Mullard Space Science Laboratory, University College London, UK 2 Dept of Physics and Astronomy, Southampton University, UK 3 University of California, Santa Barbara, USA 4 Liverpool John Moores University, UK 5 Los Alamos National Laboratory, USA 6 Subaru Telescope, NAOJ, Hawaii The 13 hour XMM-Newton / Chandra deep survey is the first of two extremely deep XMM-Newton fields belonging to the XMM-OM consortium. A 120 ks Chandra mosaic provides sensitive point source detection with sub-arcsecond positions while the 200 ks XMM-Newton observation provides high quality X-ray spectroscopy. In addition the XMM-Newton imaging has excellent sensitivity to sources at high energy (> 5 keV) and diffuse sources. XMM-Newton imaging Spectroscopy of individual X-ray sources Optical counterparts of the Chandra sources The large collecting area of XMM-Newton allows reliable X-ray spectroscopy of faint sources. Two examples are shown below. R58 Our X-ray survey is supported by deep optical imaging from telescopes including the William Herschel Telescope and Isaac Newton Telescope in La Palma, the 4m at Kitt Peak, and the Subaru Telescope in Hawaii - the Subaru imaging reaches R~27. The combination of sub-arcsecond positions from Chandra and extremely deep optical imaging mean that almost all the X-ray sources can be identified with a unique optical counterpart. XMM-Newton EPIC images of the 13 hour deep field in soft, medium and hard energy bands. Overplotted are the sources detected by the Standard Analysis System sliding box + multi-maximum likelihood source detection tasks. Source detection has been perfomed in each band independently. As well as detecting over 200 sources in the soft and medium bands, we detect 93 sources at energies above 5 keV. R58 0.5-2 keV True colour ultraviolet image of the field from the optical monitor, taken simultaneously to the EPIC X-ray data. The image shows a multitude of UV-bright AGN and star-forming galaxies and provides valuable data for the multi-wavelength characterisation of the X-ray sources. X-ray spectrum of the faint cluster R58 at z=0.308 (marked with a white arrow on the 0.5 – 2 keV XMM image). The best fit temperature of the cluster is 2.3 keV. 2-5 keV Postage stamp (10 arcsecond square) images for all 218 Chandra sources, taken from the Subaru R band Suprime-cam image. The sources are ordered in decreasing X-ray flux from the top-left. XMM PN spectrum of R36, a narrow emission line galaxy at z=0.235. The spectrum is consistent with a G=2 power law, implying it contains an active nucleus. 5-12 keV

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