The Chandra Deep Field North Survey. IX. Extended X-ray sources

The approximate to1 Ms Chandra Deep Field North observation is used to study the extended X-ray sources in the region surrounding the Hubble Deep Field North (HDF-N), yielding the most sensitive probe of extended X-ray emission at cosmological distances to date. A total of six such sources are detected, the majority of which align with small numbers of optically bright galaxies. Their angular sizes, band ratios, and X-ray luminosities assuming they lie at the same distances as the galaxies coincident with the X-ray emission are generally consistent with the properties found for nearby groups of galaxies. One source is notably different and is likely to be a poor-to-moderate X-ray cluster at high redshift (i.e., z greater than or similar to 0.7). This source has a large angular extent, a double-peaked X-ray morphology, and an overdensity of unusual objects [very red objects, optically faint (I greater than or equal to 24) radio and X-ray sources]. Another of the six sources is coincident with several z approximate to 1.01 galaxies located within the HDF-N itself, including the FRI radio galaxy VLA J123644+621133, and is likely to be a group or poor cluster of galaxies at that redshift. We are also able to place strong constraints on the optically detected cluster of galaxies ClG 1236+6215 at z = 0.85 and the wide-angle tailed radio galaxy VLA J123725+621128 at z similar to 1-2; both sources are expected to have considerable associated diffuse X-ray emission, and yet they have rest-frame 0.5-2.0 keV X-ray luminosities of less than or similar to3 x 10(42) and less than or similar to(3-15) x 10(42) ergs s(-1), respectively. The environments of both sources are either likely to have a significant deficit of hot intracluster gas compared with local clusters of galaxies, or they are X-ray groups. We find the surface density of extended X-ray sources in this observation to be 167(-67)(+97) deg(-2) at a limiting soft-band flux of approximate to3 x 10(-16) ergs cm(-2) s(-1). No evolution in the X-ray luminosity function of clusters is needed to explain this value.