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تسجيل مستخدم جديدHidden Starbursts and Active Galactic Nuclei at 0<z<4 from the Herschel-VVDS-CFHTLS-D1 Field: Inferences on Coevolution and Feedback
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We investigate of the properties of $sim$2000 Herschel/SPIRE-selected galaxies from $0<z<4$ using a combination of extensive spectroscopy, deep imaging from CFHT, VLA, Spitzer, XMM-Newton, and Herschel, and well-calibrated SED fitting. Herschel galaxies are observed to span a range of stellar masses, colors, and absolute magnitudes equivalent to galaxies undetected in SPIRE. Though many Herschel galaxies appear to be in transition, such galaxies are largely consistent with normal star-forming galaxies when rest-frame colors are utilized. The nature of the star-forming main sequence is studied and we warn against adopting this framework unless the main sequence is determined precisely. Herschel galaxies at different total infrared luminosities ($L_{TIR}$) are compared. Bluer colors, larger nebular extinctions, and larger contributions from younger stellar populations are observed for galaxies with larger $L_{TIR}$, suggesting that low-$L_{TIR}$ galaxies are undergoing rejuvenated starbursts while galaxies with higher $L_{TIR}$ are forming a larger percentage of their stellar mass. A variety of methods are used to select powerful active galactic nuclei (AGN). Galaxies hosting AGN are observed to be undergoing starbursts more commonly and vigorously than a matched sample of galaxies without powerful AGN and, additionally, the fraction of galaxies with an AGN increases with increasing star formation rate at all redshifts. At all redshifts ($0<z<4$) the most prodigious star-forming galaxies are found to contain the highest fraction of powerful AGN. For redshift bins that allow a comparison ($z>0.5$), the highest $L_{TIR}$ galaxies in a given redshift bin are unobserved by SPIRE at subsequently lower redshifts, a trend linked to downsizing. In conjunction with other results, this evidence is used to argue for prevalent AGN-driven quenching in starburst galaxies across cosmic time.
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