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Title:
Massive Galaxies in COSMOS: Evolution of Black Hole Versus Bulge Mass but not Versus Total Stellar Mass Over the Last 9 Gyr?
Authors:
Jahnke, Knud; Bongiorno, Angela; Brusa, Marcella; Capak, Peter; Cappelluti, Nico; Cisternas, Mauricio; Civano, Francesca; Colbert, James; Comastri, Andrea; Elvis, Martin; Hasinger, Günther; Ilbert, Olivier; Impey, Chris; Inskip, Katherine; Koekemoer, Anton M.; Lilly, Simon; Maier, Christian; Merloni, Andrea; Riechers, Dominik; Salvato, Mara; Schinnerer, Eva; Scoville, Nick Z.; Silverman, John; Taniguchi, Yoshi; Trump, Jonathan R.; Yan, Lin
Affiliation:
AA(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AB(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85741 Garching b. München, Germany ; University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, MD 21250, USA ), AC(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85741 Garching b. München, Germany ), AD(California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA ), AE(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85741 Garching b. München, Germany ), AF(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AG(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA ), AH(California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA ), AI(INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy ), AJ(Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA ), AK(Max-Planck-Institut für Plasmaphysik, Boltzmanstrasse 2, D-85741 Garching, Germany ), AL(Institute for Astronomy, 2680 Woodlawn Drive, University of Hawaii, Honolulu, HI 96822, USA ), AM(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ), AN(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AO(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ), AP(Department of Physics, ETH Zürich, CH-8093 Zürich, Switzerland ), AQ(Department of Physics, ETH Zürich, CH-8093 Zürich, Switzerland ), AR(Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85741 Garching b. München, Germany ; Excellence Cluster Universe, TUM, Boltzmannstr. 2, D-85748 Garching, Germany ), AS(California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA ; Hubble Fellow.), AT(California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA ; Max-Planck-Institut für Plasmaphysik, Boltzmanstrasse 2, D-85741 Garching, Germany ), AU(Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany ), AV(California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA ), AW(Department of Physics, ETH Zürich, CH-8093 Zürich, Switzerland ), AX(Research Center for Space and Cosmic Evolution, Ehime University, Bunkyo-cho, Matsuyama 790-8577, Japan ), AY(Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA ), AZ(California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA )
Publication:
The Astrophysical Journal Letters, Volume 706, Issue 2, pp. L215-L220 (2009). (ApJL Homepage)
Publication Date:
12/2009
Origin:
IOP
ApJ Keywords:
galaxies: active, galaxies: evolution, galaxies: fundamental parameters, galaxies: nuclei
DOI:
10.1088/0004-637X/706/2/L215
Bibliographic Code:
2009ApJ...706L.215J

Abstract

We constrain the ratio of black hole (BH) mass to total stellar mass of type-1 active galactic nuclei (AGNs) in the COSMOS survey at 1 < z < 2. For 10 AGNs at mean redshift z ~ 1.4 with both Hubble Space Telescope (HST)/ACS and HST/NICMOS imaging data, we are able to compute the total stellar mass M *,total, based on rest-frame UV-to-optical host galaxy colors which constrain mass-to-light ratios. All objects have virial M BH estimates available from the COSMOS Magellan/IMACS and zCOSMOS surveys. We find within errors zero difference between the M BH-M *,total relation at z ~ 1.4 and the M BH-M *,bulge relation in the local universe. Our interpretation is (1) if our objects were purely bulge-dominated, the M BH-M *,bulge relation has not evolved since z ~ 1.4. However, (2) since we have evidence for substantial disk components, the bulges of massive galaxies (M *,total = 11.1 ± 0.3 or log M BH ~ 8.3 ± 0.2) must have grown over the last 9 Gyr predominantly by redistribution of the disk into the bulge mass. Since all necessary stellar mass exists in galaxies at z = 1.4, no star formation or addition of external stellar material is required, but only a redistribution, e.g., induced by minor and major merging or through disk instabilities. Merging, in addition to redistributing mass in the galaxy, will add both BH and stellar/bulge mass, but does not change the overall final M BH/M *,bulge ratio. Since the overall cosmic stellar and BH mass buildup trace each other tightly over time, our scenario of bulge formation in massive galaxies is independent of any strong BH feedback and means that the mechanism coupling BH and bulge mass until the present is very indirect.

Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, the XMM-Newton telescope, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA, the European Southern Observatory under Large Program 175.A-0839, the Magellan Telescope which is operated by the Carnegie Observatories, and the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.


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