On the co-evolution of supermassive black holes and their host galaxies since z= 3

Bluck, Asa F. L.; Conselice, Christopher J.; Almaini, O.; Laird, E. S.; Nandra, K.; Grützbauch, Ruth

doi:10.1111/j.1365-2966.2010.17521.x

Cited by 44 publications

(43 citation statements)

References 70 publications

(158 reference statements)

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“…This amounts to ∼13 ± 3 per cent (21/163) of the log M * ≥ 10.5 galaxies and ∼11 ± 4 per cent (10/90) among the most massive log M * ≥ 11 galaxies. In this population of massive red, non‐dusty galaxies, half (5) are curiously detected at 24 μm and two of those are classified as ULIRGs, possibly due to dust heating by another source such as an AGN (Bluck et al 2011).…”

Section: Resultsmentioning

confidence: 99%

Star formation in a stellar mass-selected sample of galaxies to z= 3 from the GOODS-NICMOS Survey

Bauer

Conselice

Pérez‐González

et al. 2011

Monthly Notices of the Royal Astronomical Society

139

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We present a study of the star‐forming properties of a stellar mass‐selected sample of galaxies in the GOODS (Great Observatories Origins Deep Survey) NICMOS Survey (GNS), based on deep Hubble Space Telescope (HST) imaging of the GOODS North and South fields. Using a stellar mass‐selected sample, combined with HST/ACS and Spitzer data to measure both ultraviolet (UV) and infrared‐derived star formation rates (SFRs), we investigate the star forming properties of a complete sample of ∼1300 galaxies down to log M*= 9.5 at redshifts 1.5 < z < 3. Eight per cent of the sample is made up of massive galaxies with M*≥ 1011 M⊙. We derive optical colours, dust extinctions and UV and infrared SFR to determine how the SFR changes as a function of both stellar mass and time. Our results show that SFR increases at higher stellar mass such that massive galaxies nearly double their stellar mass from star formation alone over the redshift range studied, but the average value of SFR for a given stellar mass remains constant over this ∼2 Gyr period. Furthermore, we find no strong evolution in the SFR for our sample as a function of mass over our redshift range of interest; in particular we do not find a decline in the SFR among massive galaxies, as is seen at z < 1. The most massive galaxies in our sample (log M*≥ 11) have high average SFRs with values SFRUV, corr= 103 ± 75 M⊙ yr−1, and yet exhibit red rest‐frame (U−B) colours at all redshifts. We conclude that the majority of these red high‐redshift massive galaxies are red due to dust extinction. We find that A2800 increases with stellar mass, and show that between 45 and 85 per cent of massive galaxies harbour dusty star formation. These results show that even just a few Gyr after the first galaxies appear, there are strong relations between the global physical properties of galaxies, driven by stellar mass or another underlying feature of galaxies strongly related to the stellar mass.

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Section: Resultsmentioning

confidence: 99%

Star formation in a stellar mass-selected sample of galaxies to z= 3 from the GOODS-NICMOS Survey

Bauer

Conselice

Pérez‐González

et al. 2011

Monthly Notices of the Royal Astronomical Society

139

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“…Further description of the GNS, the pointings and the target selection is given in Conselice et al (2011). Other analysis of the GNS data set can be found in Buitrago et al (2008), Bluck et al (2009, 2011), Bauer et al (2010) and Grützbauch et al (2011).…”

Section: Data Reduction and The Gnsmentioning

confidence: 99%

A deep probe of the galaxy stellar mass functions at z∼ 1-3 with the GOODS NICMOS Survey

Mortlock

Conselice

Bluck

et al. 2011

Monthly Notices of the Royal Astronomical Society

Self Cite

106

149

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We use a sample of 8298 galaxies observed as part of the Hubble Space Telescope (HST) H160‐band GOODS NICMOS Survey (GNS) to construct the galaxy stellar mass function both as a function of redshift and as stellar mass up to z= 3.5. Our mass functions are constructed within the redshift range z= 1–3.5 and consist of galaxies with stellar masses of M*= 1012 M⊙ down to nearly dwarf galaxy masses of M*= 108.5 M⊙ in the lowest redshift bin. We discover that a significant fraction of all massive M* > 1011 M⊙ galaxies are in place up to the highest redshifts we probe, with a decreasing fraction of lower mass galaxies present at all redshifts. This is an example of ‘galaxy mass downsizing’, and is the result of massive galaxies forming before lower mass ones, and not just simply ending their star formation earlier as in traditional downsizing scenarios, whose effect is seen at z < 1.5. By fitting Schechter functions to our mass functions we find that the faint‐end slope ranges from α=−1.36 to −1.73, which is significantly steeper than what is found in previous investigations of the mass function at high redshift. We demonstrate that this steeper mass function better matches the stellar mass added due to star formation, thereby alleviating some of the mismatch between these two measures of the evolution of galaxy mass. We furthermore examine the stellar mass function divided into blue/red systems, as well as for star‐forming and non‐star‐forming galaxies. We find a similar mass downsizing present for both blue/red and star‐forming/non‐star forming galaxies, and further find that red galaxies dominate at the high‐mass end of the mass function, but that the low‐mass galaxies are mostly all blue, and therefore blue galaxies are creating the steep mass functions observed at z > 2. We furthermore show that, although there is a downsizing such that high‐mass galaxies are nearer their z= 0 values at high redshift, this turns over at masses M*∼ 1010 M⊙, such that the lowest mass galaxies are more common than galaxies at slight higher masses, creating a ‘dip’ in the observed galaxy mass function. We argue that the galaxy assembly process may be driven by different mechanisms at low and high masses, and that the efficiency of the galaxy formation process is lowest at masses M*∼ 1010 M⊙ at 1 < z < 3. Finally, we calculate the integrated stellar mass density for the total, blue and red populations. We find the integrated stellar mass density of the total and blue galaxy population is consistent with being constant over z= 1–2, while the red population shows an increase in integrated stellar mass density over the same redshift range.

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“…In the local universe, the masses of SMBHs and the masses and velocity dispersions of their hosts' central bulges or spheroids have been shown to be correlated (Ferrarese & Merritt 2000;Tremaine et al 2002;Marconi & Hunt 2003;Häring & Rix 2004;Xu, Wu & Zhao 2007;Graham 2016). As redshift increases up to z ∼ 2, so do both star formation rates and AGN fractions (Boyle & Terlevich 1998;Silverman et al 2008;Bluck et al 2011). Across a wide redshift range, AGNs have been observed to be associ-ated with star-forming galaxies (e.g., Kauffmann et al 2003;Heckman et al 2004;Veilleux et al 2009;Laird et al 2010;Georgantopoulos, Rovilos & Comastri 2011;Juneau et al 2013;Lemaux et al 2014).…”

Section: Introductionmentioning

confidence: 99%

X-ray-emitting active galactic nuclei fromz= 0.6 to 1.3 in the intermediate- and high-density environments of the ORELSE survey

Rumbaugh

Lemaux

Tomczak

et al. 2016

Mon. Not. R. Astron. Soc.

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We studied AGN activity in twelve LSSs in the ORELSE survey, at 0.65 < z < 1.28, using a combination of Chandra observations, optical and NIR imaging and spectroscopy. We located a total of 61 AGNs across our sample that were successfully matched to optical counterparts in the LSSs. Seeking to study AGN triggering mechanisms, we examined the spatial distribution of the AGNs and their average spectral properties. We found that AGN populations across our sample had less time since the last starburst than the overall galaxy populations. We did not find any relation between AGN activity and location within the LSSs, suggesting triggering mechanisms which depend on global environment are at most sub-dominant. To focus on differences between our AGNs, we grouped them into four sub-samples based on the spectral properties of their parents LSSs. We found one of the sub-samples, SG0023 & SC1604, stood out from the others: AGNs in this sample were disproportionately luminous, their average time since the last starburst event was the smallest, despite the fact that this was not true of the overall galaxy population in those LSSs, and both the AGNs and the overall galaxy population had the largest fraction of close kinematic pairs, which indicates a higher rate of galaxy mergers and interactions. These results suggest that major mergers are driving AGN activity in SG0023 & SC1604, while other processes are likely triggering less luminous AGNs in the rest of our sample. Additionally, minor mergers are unlikely to play a significant role, since the same conditions that lead to more major mergers should should also lead to more minor mergers, which is not observed in SG0023 & SC1604.

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On the co-evolution of supermassive black holes and their host galaxies since z= 3

Cited by 44 publications

References 70 publications

Star formation in a stellar mass-selected sample of galaxies to z= 3 from the GOODS-NICMOS Survey

Star formation in a stellar mass-selected sample of galaxies to z= 3 from the GOODS-NICMOS Survey

A deep probe of the galaxy stellar mass functions at z∼ 1-3 with the GOODS NICMOS Survey

X-ray-emitting active galactic nuclei fromz= 0.6 to 1.3 in the intermediate- and high-density environments of the ORELSE survey

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