The quasar relation through cosmic time – II. Evidence for evolution from z = 3 to the present age

By R. Decarli, R. Falomo, A. Treves, M. Labita, J. Kotilainen, R. Scarpa. 2009

142 citations recorded by the source corpus.

We study the dependence of the MBH–Mhost relation on the redshift up to z = 3 for a sample of 96 quasars, the host galaxy luminosities of which are known. Black hole masses were estimated assuming virial equilibrium in the broad-line regions, while the host galaxy masses were inferred from their luminosities. With these data, we are able to pin down the redshift dependence of the MBH–Mhost relation along 85 per cent of the Universe age. We show that, in the sampled redshift range, the MBH–Lhost relation remains nearly unchanged. Once we take into account the ageing of the stellar population, we find that the MBH/Mhost ratio (� )

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/7c25844db33128305eda283003c003900aa4c44d

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Citations in the corpus

The LABOCA survey of the Extended Chandra Deep Field-South: clustering of submillimetre galaxies (2011, background): “…to the local black hole–galaxy mass relations (e.g. Alexander et al. 2008; Carrera et al. 2011), while the black holes in z ∼ 2 QSOs tend to lie above the local relation, with masses similar to those in local massive ellipticals (e.g. Bennert et al. 2010; Decarli et al. 2010; Merloni et al. 2010).”
The clustering of intermediate-redshift quasars as measured by the Baryon Oscillation Spectroscopic Survey (2012, background): “4– while Decarli et al. (2010) measure a best-fit power-law of(1+z)0.28 –a factor of 1.4 between z = 0 and2.”
The transition between BL Lac objects and flat spectrum radio quasars (2010, background): “…Merritt 2000; Gültekin et al. 2009), and iii) the correlation between the luminosity of the continuum at selected fr - quencies and the size of the Broad Line Region (BLR, Vestergaard 2002; Decarli et al. 2010 and references therein), made the estimate of the black hole mass much more affordable.”
Physical Properties of 15 Quasars at z ≳ 6.5 (2017, methodology): “We consider regions of the rest-frame spectra which are free from strong emission lines: [1285−1295; 1315−1325; 1340−1375; 1425−1470; 1680−1710; 1975−2050; 2150−2250; and 2950−2990] Å (Decarli et al. 2010).”
BLACK HOLE MASS ESTIMATES AND EMISSION-LINE PROPERTIES OF A SAMPLE OF REDSHIFT z > 6.5 QUASARS (2013, methodology): “Decarli et al. (2010), for example, analyzed a sample of 96 quasars at z < 3 and obtained a mean value of α = −1.3 with a 1σ dispersion of 1.6.”
THE NON-CAUSAL ORIGIN OF THE BLACK-HOLE–GALAXY SCALING RELATIONS (2010, background): “…scaling relations (Treu et al. 2004; Peng et al. 2006a,b; Treu et al. 2007; Schramm et al. 2008; Jahnke et al. 2009; Merloni et al. 2010; Bennert et al. 2010; Decarli et al. 2010) is investigated in order to constrain the physical drivers behind co-evolution and the growth mechanisms of BHs. 1.1.”
An expanded Mbh–σ diagram, and a new calibration of active galactic nuclei masses (2010, background): “…no significant ramifications: e.g. the evolution in the relationship between black holes and spheroids in AGN samples (e.g. Peng et al. 2006a,b; Bennert et al. 2010; Decarli et al. 2010a,b); or the slope of the active BH mass function (e.g. Kelly, Vestergaard & Fan 2009; Vestergaard & Osmer 2009).”
What drives the growth of black holes (2011, methodology): “The presence of an AGN also presents the additional challenge of separating the light from the host galaxy to that from the accreting BH, and difficulties in separating the mass or potential of the stellar bulge from the rest of the galaxy (e.g., Decarli et al., 2010a; Merloni et al., 2010).”
RELATIONS BETWEEN CENTRAL BLACK HOLE MASS AND TOTAL GALAXY STELLAR MASS IN THE LOCAL UNIVERSE (2015, background): “…SED fitting (e.g., Jahnke et al. 2009; Cisternas et al. 2011; Targett et al. 2012; Merloni 2010; Bongiorno et al. 2014; Sun et al. 2015), sometimes trying to select quasars with bulge-dominated host galaxies (Decarli et al. 2010) to lessen the discrepancy between bulge mass and total stellar mass.”
EVIDENCE FOR NON-EVOLVING Fe ii/Mg ii RATIOS IN RAPIDLY ACCRETING z ∼ 6 QSOs (2011, methodology): “We obtain a mean value α = −1.5 ± 1.2 which is in agreement within the uncertainties with both the local slope estimate by Shen et al. (2008) and with the global one by Decarli et al. (2010).”
An ALMA [C ii] Survey of 27 Quasars at z > 5.94 (2018, methodology): “Observations of the host galaxy starlight in conditions of natural seeing (e.g., Decarli et al. 2010; Targett et al. 2012; Matsuoka et al. 2014), using adaptive optics (e.g., Falomo et al. 2005; Inskip et al. 2011), or capitalizing on the exquisite angular resolution of the Hubble Space Telescope…”
Self-regulated growth of supermassive black holes by a dual jet-heating active galactic nucleus feedback mechanism: methods, tests and implications for cosmological simulations (2011, background): “Despite these difficulties, an increasing amount of data is suggesting that the MBH–Ms relationship shows some positive evolution with redshift (McLure et al. 2006; Peng et al. 2006; Shields et al. 2006; Salviander et al. 2007; Bennert et al. 2010; Decarli et al. 2010; Merloni et al. 2010).”