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R.E. Griffiths, T. Miyaji (Carnegie Mellon University), D. Lumb (ESTEC)
A comparison is made of the results of the 1Ms CXO and the 160ks XMM-Newton deep surveys of the HDF-N. The confusion of sources in the XMM-Newton image is assessed as a function of energy. Source spectra are compared and the optical ids. of many of the XMM sources are aided by the CXO positions. The XMM spectra are summed for each broad optical classification. The harder response of XMM is highlighted with respect to the nature of sources contributing to the bulk of the X-ray background, i.e. AGN with heavy absorption.
Comments are made on the nature of the sources contributing to the log(N) - log(S) at fluxes between 10-16 and 10-17 ergs cm-2 s-1 (0.5 - 2keV), where the number counts are constrained by fluctuation analysis (Miyaji & Griffiths 2001 ApJ 564, L5. We may be observing the X-ray evolution of normal galaxies, as predicted from expected evolution in the numbers of binaries (Ghosh & White (2001 ApJ 559, L97, 2001) and applied to galaxy X-ray fluxes by Ptak et al. (2001 ApJ 559, L91). We also comment on the cosmic variance observed across different deep X-ray surveys.
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Bulletin of the American Astronomical Society, 34
© 2002. The American Astronomical Soceity.