Astrophys. J., 719, 1393-1407 (2010/August-3)
The AGN, star-forming, and morphological properties of luminous IR-bright/optically-faint galaxies.
DONLEY J.L., RIEKE G.H., ALEXANDER D.M., EGAMI E. and PEREZ-GONZALEZ P.G.
Abstract (from CDS):
We present the active galactic nucleus (AGN), star-forming, and morphological properties of a sample of 13 MIR-luminous (f24≳ 700 µJy) IR-bright/optically-faint galaxies (IRBGs, f24/fR≳ 1000). While these z ∼ 2 sources were drawn from deep Chandra fields with >200 ks X-ray coverage, only seven are formally detected in the X-ray and four lack X-ray emission at even the 2σ level. Spitzer InfraRed Spectrograph (IRS) spectra, however, confirm that all of the sources are AGN-dominated in the mid-IR, although half have detectable polycyclic aromatic hydrocarbon (PAH) emission responsible for ∼25% of their mid-infrared flux density. When combined with other samples, this indicates that at least 30%-40% of luminous IRBGs have star formation rates in the ultraluminous infrared galaxy (ULIRG) range (∼100-2000 M☉/yr). X-ray hardness ratios and MIR to X-ray luminosity ratios indicate that all members of the sample contain heavily X-ray obscured AGNs, 80% of which are candidates to be Compton thick. Furthermore, the mean X-ray luminosity of the sample, log L_2-10 keV_(erg/s) ∼44.6, indicates that these IRBGs are Type 2 QSOs, at least from the X-ray perspective. While those sources most heavily obscured in the X-ray are also those most likely to display strong silicate absorption in the mid-IR, silicate absorption does not always accompany X-ray obscuration. Finally, ∼70% of the IRBGs are merger candidates, a rate consistent with that of sub-mm galaxies (SMGs), although SMGs appear to be physically larger than IRBGs. These characteristics are consistent with the proposal that these objects represent a later, AGN-dominated, and more relaxed evolutionary stage following soon after the star-formation-dominated one represented by the SMGs.
galaxies: active - infrared: galaxies - X-rays: galaxies
Tables 1-4: [DRA2010] IRBGNN (Nos 1-13).
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