2001AJ....122.2156A

We provide constraints on the nature of the optically faint (I≥24) X-ray source population from a 1 Ms Chandra exposure of a 8'.4x8'.4 region within the Hawaii flanking-field area containing the Hubble Deep Field North region. We detect 47 (2400⁺⁴⁰⁰_–350 deg^–2) optically faint sources down to 0.5-2.0 keV and 2.0-8.0 keV fluxes of ~3x10^–17 ergs.cm^–2.s^–1 and ~2x10^–16 ergs.cm^–2.s^–1, respectively; these sources contribute ~14% and ~21% of the 0.5-2.0 keV and 2.0-8.0 keV X-ray background radiation, respectively. The fraction of optically faint X-ray sources is approximately constant (at ~35%) for 0.5-8.0 keV fluxes from 3x10^–14 ergs.cm^–2.s^–1 down to the X-ray flux limit. A considerable fraction (30⁺¹⁴_–10%) of the optically faint X-ray sources are Very Red Objects (I-K≥4). Analysis of the optical and X-ray properties suggests a large number of optically faint X-ray sources are likely to host obscured active galactic nucleus (AGN) activity at z=1-3. From these results we calculate that a significant fraction (~5%-45%) of the optically faint X-ray source population could be obscured QSOs (rest-frame unabsorbed 0.5-8.0 keV luminosity >3x10⁴⁴ ergs.s^–1) at z≤3. Given the number of X-ray sources without I-band counterparts, there are unlikely to be more than ~15 sources at z>6. We provide evidence that the true number of z>6 sources is considerably lower.

We investigate the multiwavelength properties of optically faint X-ray sources. Nine optically faint X-ray sources have µJy radio counterparts; ~53⁺²⁴_–17% of the optically faint µJy radio sources in this region. The most likely origin of the X-ray emission in these X-ray detected, optically faint µJy radio sources is obscured AGN activity. However, two of these sources have been previously detected at submillimeter wavelengths, and the X-ray emission from these sources could be due to luminous star formation activity. Assuming the spectral energy distribution of NGC 6240, we estimate the 175 µm flux of a typical optically faint X-ray source to be less than 10 mJy; however, those sources with detectable submillimeter counterparts (i.e., f_850 µm_>3 mJy) could be substantially brighter. Hence, most optically faint X-ray sources are unlikely to contribute significantly to the far-IR (140-240 µm) background radiation. However, as expected for sources with AGN activity, the two optically faint X-ray sources within the most sensitive area of the ISOCAM HDF-N region have faint (≲50 µJy) 15 µm counterparts.

We also provide constraints on the average X-ray properties of classes of optically faint sources not individually detected at X-ray energies. Stacking analyses of optically faint µJy radio sources not individually detected with X-ray emission yields a possible detection (at 98.3% confidence) in the 0.5-2.0 keV band; this X-ray emission could be produced by star formation activity at z=1-3. None of the optically faint AGN-candidate sources in the HDF-N itself are detected at X-ray energies either individually or with stacking analyses, showing that these sources have low X-ray luminosities if they are indeed AGNs.