TESTING DIAGNOSTICS OF NUCLEAR ACTIVITY AND STAR FORMATION IN GALAXIES AT
                    <i>z</i>
                    &gt; 1

Trump, Jonathan R.; Konidaris, Nick; Barro, Guillermo; Koo, David C.; Kocevski, Dale D.; Juneau, Stéphanie; Weiner, Benjamin J.; Faber, S. M.; McLean, Ian S.; Yan, Renbin; Pérez‐González, Pablo G.; Villar, V.

doi:10.1088/2041-8205/763/1/l6

Cited by 52 publications

(70 citation statements)

References 52 publications

(71 reference statements)

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“…Barro et al (2014) find in the GOODS-S field that compact starforming sources at z ∼ 2 are more likely to host X-ray bright AGN compared to more extended counterparts. Trump et al (2013) also show that clumpy and compact galaxies at z ∼ 0.11 harbor a high fraction of AGN in the SDSS survey. Kocevski et al (2017) confirm that ∼ 40% of M > 10 10 M compact SF galaxies observed in four fields of candels with 3 > z > 1.4 host an AGN.…”

Section: Introductionmentioning

confidence: 54%

“…More compact and star-forming galaxies have a higher probability of hosting a more luminous AGN (up to Lx ∼ 10 44 erg/s) in the simulation. The simulation is able to reproduce the qualitative trends found in several observational studies for AGN fractions in different galaxy types (Trump et al 2013;Barro et al 2014;Kocevski et al 2017).…”

Section: Correlation Between Galaxy Structural Properties and Bh Actimentioning

confidence: 64%

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Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG

Habouzit

Genel

Somerville

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study the connection between active galactic nuclei (AGN) and their host galaxies through cosmic time in the large-scale cosmological IllustrisTNG simulations. We first compare BH properties, i.e. the hard X-ray BH luminosity function, AGN galaxy occupation fraction, and distribution of Eddington ratios, to available observational constraints. The simulations produce a population of BHs in good agreement with observations, but we note an excess of faint AGN in hard X-ray (L x ∼ 10 43−44 erg/s), and a lower number of bright AGN (L x > 10 44 erg/s), a conclusion that varies quantitatively but not qualitatively with BH luminosity estimation method. The lower Eddington ratios of the 10 9 M BHs compared to observations suggest that AGN feedback may be too efficient in this regime. We study galaxy star formation activity and structural properties, and design sample-dependent criteria to identify different galaxy types (star-forming/quiescent, extended/compact) that we apply both to the simulations and observations from the candels fields. We analyze how the simulated and observed galaxies populate the specific star formation rate -stellar mass surface density diagram. A large fraction of the z = 0 M 10 11 M quiescent galaxies first experienced a compaction phase (i.e. reduction of galaxy size) while still forming stars, and then a quenching event. We measure the dependence of AGN fraction on galaxies' locations in this diagram. After correcting the simulations with a redshift and AGN luminosity-dependent model for AGN obscuration, we find good qualitative and quantitative agreement with observations. The AGN fraction is the highest among compact star-forming galaxies (16 − 20% at z ∼ 1.5 − 2), and the lowest among compact quiescent galaxies (6 − 10% at z ∼ 1.5 − 2).

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Section: Introductionmentioning

confidence: 54%

Section: Correlation Between Galaxy Structural Properties and Bh Actimentioning

confidence: 64%

Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG

Habouzit

Genel

Somerville

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…A link between clumpy disks and AGN activity atz 0.7 has been reported by Bournaud et al (2012), yet for luminosities well below our cutoff, i.e., < L 10 X 42 erg s −1 , arguing that this mechanism would only account for very modest levels of activity at these redshifts. Atz 2, however, Trump et al (2014) found similar levels of AGN activity in clumpy and smooth disks, ruling out violent disk instabilities as a dominant or more efficient BH fueling mechanism.…”

Section: Most Active Disk Galaxies Are Unbarredmentioning

confidence: 85%

The Role of Bars in Agn Fueling in Disk Galaxies Over the Last Seven Billion Years

Cisternas

Sheth

Salvato

et al. 2015

ApJ

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We present empirical constraints on the influence of stellar bars on the fueling of active galactic nuclei (AGNs) out to z = 0.84 using a sample of X-ray-selected AGNs hosted in luminous non-interacting face-on and moderately inclined disk galaxies from the Chandra COSMOS survey. Using high-resolution Hubble Space Telescope imaging to identify bars, we find that the fraction of barred active galaxies displays a similar behavior as that of inactive spirals, declining with redshift from 71% atz 0.3, to 35% atz 0.8. With active galaxies being typically massive, we compare them against a mass-matched sample of inactive spirals and show that, while at face value the AGN bar fraction is slightly higher at all redshifts, we cannot rule out that the bar fractions of active and inactive galaxies are the same. The presence of a bar has no influence on the AGN strength, with barred and unbarred active galaxies showing equivalent X-ray luminosity distributions. From our results, we conclude that the occurrence and the efficiency of the fueling process is independent of the large scale structure of a galaxy. The role of bars, if any, may be restricted to providing the suitable conditions for black hole fueling to occur, i.e., bring a fresh supply of gas to the central 100 pc. At the high-redshift end, we find that roughly 60% of active disk galaxies are unbarred. We speculate this to be related with the known dynamical state of disks at higher redshifts-more gas-rich and prone to instabilities than local spirals-which could also lead to gas inflows without the need of bars.

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“…The galaxies in SIGMA are located in the UDS, GOODS-S, and GOODS-N fields. Spectra were taken with the MOSFIRE spectrograph (McLean et al 2010(McLean et al , 2012 on the Keck I telescope as a part of the TKRS-2 survey (Wirth et al 2015) and were also published in Trump et al (2013) and Barro et al (2014). The slits were 0 7 wide and the spectral resolution wasR…”

Section: Sigma Samplementioning

confidence: 99%

z ∼ 2: An Epoch of Disk Assembly

Simons

Kassin

Weiner

et al. 2017

ApJ

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123

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We explore the evolution of the internal gas kinematics of star-forming galaxies from the peak of cosmic star formation atz 2 to today. Measurements of galaxy rotation velocity V rot , which quantify ordered motions, and gas velocity dispersion s g , which quantify disordered motions, are adopted from the DEEP2 and SIGMA surveys. This sample covers a continuous baseline in redshift over < < z 0.1 2.5, spanning 10 Gyr. At low redshift, nearly all sufficiently massive star-forming galaxies are rotationally supported (By z=2, 50% and 70% of galaxies are rotationally supported at low ( ) stellar mass, respectively. For, the percentage drops below 35% for all masses. From z=2 to now, galaxies exhibit remarkably smooth kinematic evolution on average. All galaxies tend toward rotational support with time, and higher-mass systems reach it earlier. This is largely due to a mass-independent decline in s g by a factor of 3 since z=2. Over the same time period, V rot increases by a factor of 1.5 in low-mass systems but does not evolve at high mass. These trends in V rot and s g are at a fixed stellar mass and therefore should not be interpreted as evolutionary tracks for galaxy populations. When populations are linked in time via abundance matching, s g declines as before and V rot strongly increases with time for all galaxy populations, enhancing the evolution in s V g rot . These results indicate that = z 2 is a period of disk assembly, during which strong rotational support is only just beginning to emerge.

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TESTING DIAGNOSTICS OF NUCLEAR ACTIVITY AND STAR FORMATION IN GALAXIES AT z > 1

Cited by 52 publications

References 52 publications

Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG

Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG

The Role of Bars in Agn Fueling in Disk Galaxies Over the Last Seven Billion Years

z ∼ 2: An Epoch of Disk Assembly

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