Colors of Active Galactic Nucleus Host Galaxies at 0.5 < z < 1.1 from the GEMS Survey

By S. Sánchez, K. Jahnke, L. Wisotzki, D. H. Mcintosh, Eric F. Bell, M. Barden, S. Beckwith, A. Borch, J. Caldwell, B. Häußler and 6 more. 2004

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Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Probing the Coevolution of Supermassive Black Holes and Galaxies Using Gravitationally Lensed Quasar Hosts (2006, background): “We deliberately excluded observations of unlensed host galaxies for which the only available data were at optical rather than near-IR wavelengths (e.g., Aretxaga, Terlevich, & Boyle 1998; Lehnert et al. 1999; Hutchings et al. 2002; Hutchings 2003, Sánchez et al. 2004, Jahnke et al 2004).”
A semi-analytic model for the co-evolution of galaxies, black holes and active galactic nuclei (2008, background): “…the spectral energy distribution beneath the glare of the quasar, one always uncovers evidence of young stellar populations indicative of a recent starburst (Brotherton et al. 1999; Canalizo & Stockton 2001; Kauffmann et al. 2003b; Jahnke et al. 2004; Sánchez et al. 2004; Vanden Berk et al. 2006).”
DETAILED DECOMPOSITION OF GALAXY IMAGES. II. BEYOND AXISYMMETRIC MODELS (2009, background): “…et al. 2009; Hopkins et al. 2008b,a), quasar host galaxies (e.g., Hutchings et al. 1984; McLeod & Rieke 1994; McLure et al. 2000; Jahnke et al. 2004; Sánchez et al. 2004; Kim et al. 2008b), gravitational lensing of quasar host galaxies (Rix et al. 2001; Peng et al. 2006b), and the clustering of…”
Galaxies in the Hubble Ultra Deep Field. I. Detection, Multiband Photometry, Photometric Redshifts, and Morphology (2006, methodology): “Particular care was taken to resample the noise histogram and noise pattern seen in the UDF ACS dithered images, as described in Sánchez et al. (2004).”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, background): “This distribution of AGN hosts for this luminosity interval is consistent with observations (Kauffmann et al. 2003a; Sánchez et al. 2004; Best et al. 2005), specifically those of e.g. Dong & De Robertis (2005) who find that Sa/b and S0 systems make up most of the low-moderate luminosity…”
The Relation between Quasar and Merging Galaxy Luminosity Functions and the Merger-driven Star Formation History of the Universe (2006, background): “The distribution demonstrates the lack of correlation between quasar and host galaxy luminosity and agrees well with various observational estimates (e.g., Bahcall et al. 1997; McLure et al. 1999; Jahnke & Wisotzki 2003; Sánchez et al. 2004).”
ON THE COSMIC EVOLUTION OF THE SCALING RELATIONS BETWEEN BLACK HOLES AND THEIR HOST GALAXIES: BROAD-LINE ACTIVE GALACTIC NUCLEI IN THE zCOSMOS SURVEY (2009, methodology): “Other groups have chosen to try and derive information on the host mass of broad line AGN using multi-colour image decomposition techniques (Jahnke, Kuhlbrodt & Wisotzki 2004; Sanchez et al. 2004) or spatially deconvolving optical spectra (Letawe et al. 2007).”
ACTIVE GALACTIC NUCLEUS HOST GALAXY MORPHOLOGIES IN COSMOS (2009, methodology): “AGN host galaxies at both low and high redshift are found to be bluer than quiescent elliptical galaxies (Kauffmann et al. 2003; Jahnke et al. 2004a, 2004b; Sanchez et al. 2004), indicating recent or ongoing star formation.”
CANDELS: CONSTRAINING THE AGN–MERGER CONNECTION WITH HOST MORPHOLOGIES AT z ∼ 2 (2011, background): “…Giavalisco et al. 2004) and the All-wavelength Extended Groth strip International Survey (AEGIS; Davis et al. 2007), respectively, find that host galaxies at z ∼ 1 do not show disturbances or interaction signatures more often than their quiescent counterparts (see also Sánchez et al. 2004).”
What drives the growth of black holes (2011, background): “…to initial expectations, only a comparatively small fraction of the X-ray AGNs out to z ≈ 3 clearly reside in galaxy major mergers (≈ 15–20%; e.g., Sánchez et al. 2004; Pierce et al. 2007; Georgakakis et al. 2009; Cisternas et al. 2011; Kocevski et al. 2011, comparable to that found for…”
Determining the Properties and Evolution of Red Galaxies from the Quasar Luminosity Function (2005, background): “…at high redshift (which should relax to become normal present ellipticals) are excessively blue, both from AGN contributions and recent starburst activity (see, e.g. Bahcall et al. 1997; Canalizo & Stockton 2001; Dunlop et al. 2003; Sánchez et al. 2004; Jahnke et al. 2004, and references therein).”
ONGOING AND CO-EVOLVING STAR FORMATION IN zCOSMOS GALAXIES HOSTING ACTIVE GALACTIC NUCLEI (2008, background): “1.4 having blue rest-frame colors (Sanchez et al. 2004; Böhm et al. 2007; Nandra et al. 2007) with evidence for such a trend remaining in place for quasar hosts at higher redshifts 1.8 < z < 2.8 (Jahnke et al. 2004b).”
Evidence for Merger Remnants in Early-Type Host Galaxies of Low-Redshift QSOs (2008, background): “…AGNs are bulge-dominated, they seem to be significantly bluer than inactive elliptical galaxies, and indeed show evidence for starbursts in the relatively recent past (1–2 Gyr; e.g., Kauffmann et al. 2003; Sánchez et al. 2004; Canalizo et al. 2006; Schweitzer et al. 2006; Jahnke et al. 2007).”
Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, background): “…rest-frame colors of AGN hosts (Aird et al. 2012; Georgakakis et al. 2014; Azadi et al. 2014) or their position on the color–magnitude diagram (e.g. Sánchez et al. 2004; Nandra et al. 2007; Schawinski et al. 2009) indicate that they are scattered at the red sequence of passive galaxies, the…”
On-axis spectroscopy of the host galaxies of 20 optically luminous quasars at z ~ 0.3 (2006, background): “We thus find that ∼50 per cent of our host galaxies display signs of interaction, which is compatible with several previous studies (Smith et al. 1986; Hutchings & Neff 1992; Bahcall et al. 1997; Jahnke et al. 2004; Sanchez et al. 2004).”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. I. Galaxy Mergers and Quasar Activity (2007, background): “…host galaxies reveal the presence of young stellar populations indicative of a recent starburst (Brotherton et al. 1999; Canalizo & Stockton 2001; Kauffmann et al. 2003; Yip et al. 2004; Jahnke et al. 2004a, 2004b; Sánchez et al. 2004; Vanden Berk et al. 2006; Barthel 2006; Zakamska et al. 2006).”
AGN Host Galaxies at z ~ 0.4-1.3: Bulge-dominated and Lacking Merger-AGN Connection (2005, background): “This may be remedied by the wider area Galaxy Evolution from Morphology and SEDs project HST imaging within the extended CDF-S, where Sanchez et al. (2004) have already noted a higher incidence of merger/ interaction among 15 optically selected, , type 1z ∼ 0.5–1.1 AGNs with luminosities spanning…”
MAJOR GALAXY MERGERS ONLY TRIGGER THE MOST LUMINOUS ACTIVE GALACTIC NUCLEI (2012, methodology): “Morphologies of AGN host galaxies have been estimated before using automatic classifications (e.g., Grogin et al. 2005), and 2-dimensional surface brightness fitting (Sánchez et al. 2004).”
THE BULK OF THE BLACK HOLE GROWTH SINCE z ∼ 1 OCCURS IN A SECULAR UNIVERSE: NO MAJOR MERGER–AGN CONNECTION (2010, methodology): “For each object, we build specific PSFs by averaging the nearest ∼30 stars in the same manner to other similar studies with large HST coverage (Jahnke et al. 2004; Sánchez et al. 2004).”