Physics
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6677m&link_type=abstract
HST Proposal ID #6677
Physics
Hst Proposal Id #6677 Galaxies &Amp, Clusters
Scientific paper
To determine the origin of the X-ray background {XRB} we have made the deepest optically identified {ROSAT} X-ray survey yet. At `bright' flux levels {ie 1 x 10**-14 ergs/cm/s} QSOs dominate the survey but below 5 x 10**-15 ergs/cm/s our sample is dominated by a population of narrow emission line galaxies {NELGs}, at typical redshifts of 0.2-0.5. The NELG source counts rise rapidly at faint X-ray fluxes making them a major contributor to the XRB. The X-ray spectra of the NELGs are hard, as is required for any major contributor to the XRB. Deep sub-arcsecond CFHT images indicate that the brightest {m_R < 18.5} systems are mainly interacting galaxies, probably spirals. Here we request WFC R-band images to determine the morphologies of the remaining systems which we cannot study from the ground to determine whether the remaining non-QSO XRB might be explained by emission from interacting or disturbed spirals. Disturbed systems are thought to be responsible for the faint blue galaxy population, IRAS starburst galaxies and the sub-mJy radio sources so our observations may have implications for the unification of all these populations, including X-ray NELGs.
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