HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS

Jogee, Shardha; Miller, Seumas; Penner, K.; Skelton, Rosalind E.; Conselice, Christopher J.; Somerville, Rachel S.; Bell, Eric F.; Zheng, Xian Zhong; Rix, Hans─Walter; Robaina, Aday R.; Barazza, Fabio D.; Barden, M.; Borch, Andrea; Beckwith, S.; Caldwell, J. A. R.; Peng, Chien Y.; Heymans, Catherine; McIntosh, Daniel H.; Häußler, Boris; Jahnke, K.; Meisenheimer, K.; Sanchez, Sebastian Francisco Sanchez; Wisotzki, L.; Wolf, Christian; Papovich, C.

doi:10.1088/0004-637x/697/2/1971

Cited by 242 publications

(354 citation statements)

References 120 publications

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“…There has been considerable observational work over the last decades to confirm these theoretical predictions, which bear out many of the general, qualitative predictions of the simulations over a range of redshifts (e.g. Kennicutt et al 1987;Barton, Geller & Kenyon 2000;Kewley, Geller & Barton 2006;Woods, Geller & Barton 2006;Smith et al 2007;Jogee et al 2009;Rupke, Kewley & Chien 2010;Koss et al 2010Koss et al , 2012Silverman et al 2011;Wong et al 2011;Ramos-Almeida et al 2011, 2012Xu et al 2012;Cotini et al 2013;Lanz et al 2013). However, a full and detailed picture of the merger transformation requires large samples of galaxies that span a range in mass, mass ratio, structural properties, environments and projected separation, since all of these properties are likely to impact the specific outcome of a merger.…”

Section: Introductionmentioning

confidence: 81%

Galaxy pairs in the Sloan Digital Sky Survey – VIII. The observational properties of post-merger galaxies

Ellison

Mendel

Patton

et al. 2013

Monthly Notices of the Royal Astronomical Society

252

324

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In order to investigate the effects of galaxy mergers throughout the interaction sequence, we present a study of 10,800 galaxies in close pairs and a smaller sample of 97 post-mergers identified in the Sloan Digital Sky Survey. We find that the average central star formation rate (SFR) enhancement (×3.5) and the fraction of starbursts (20 per cent) peak in the postmerger sample. The post-mergers also show a stronger deficit in gas phase metallicity than the closest pairs, being more metal-poor than their control by −0.09 dex. Combined with the observed trends in SFR and the timescales predicted in merger simulations, we estimate that the post-mergers in our sample have undergone coalescence within the last few hundred Myr. In contrast with the incidence of star-forming galaxies, the frequency of active galactic nuclei (AGN) peaks in the post-mergers, outnumbering AGN in the control sample by a factor of 3.75. Moreover, amongst the galaxies that host an AGN, the black hole accretion rates in the closest pairs and post-mergers are higher by a factor of ∼ 3 than AGN in the control sample. These results are consistent with a picture in which star formation is initiated early on in the encounter, with AGN activity peaking post-coalescence.

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Section: Introductionmentioning

confidence: 81%

Galaxy pairs in the Sloan Digital Sky Survey – VIII. The observational properties of post-merger galaxies

Ellison

Mendel

Patton

et al. 2013

Monthly Notices of the Royal Astronomical Society

252

324

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“…This leads to the galaxy-galaxy merger rates. Extensive discussion and tests of this methodology are presented in Hopkins et al (2010b); we simply note here that taking the merger rate directly from observations gives a similar result, but with large uncertainties (comparisons with observations and semianalytic models are in Stewart et al 2009a;Jogee et al 2009;Lotz et al 2011).…”

Section: Merger-induced Fuelingmentioning

confidence: 97%

Do we expect most AGN to live in discs?

Hopkins¹,

Kocevski²,

Bundy³

2014

Monthly Notices of the Royal Astronomical Society

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Recent observations have indicated that a large fraction of the low to intermediate luminosity AGN population lives in disk-dominated hosts, while the more luminous quasars live in bulge-dominated hosts (that may or may not be major merger remnants), in conflict with some previous model predictions. We therefore build and compare a semi-empirical model for AGN fueling which accounts for both merger and non-merger "triggering." In particular, we show that the "stochastic accretion" model -in which fueling in disk galaxies is essentially a random process arising whenever dense gas clouds reach the nucleusprovides a good match to the present observations at low/intermediate luminosities. However it falls short of the high-luminosity population. We combine this with models for major merger-induced AGN fueling, which lead to rarer but more luminous events, and predict the resulting abundance of disk-dominated and bulge-dominated AGN host galaxies as a function of luminosity and redshift. We compile and compare observational constraints from z ∼ 0 − 2. The models and observations generically show a transition from disk to bulge dominance in hosts near the Seyfert-quasar transition, at all redshifts. "Stochastic" fueling dominates AGN by number (dominant at low luminosity), and dominates BH growth below the "knee" in the present-day BH mass function ( 10 7 M ). However it accounts for just ∼ 10% of BH mass growth at masses 10 8 M . In total, fueling in disky hosts accounts for ∼ 30% of the total AGN luminosity density/BH mass density. The combined model also accurately predicts the AGN luminosity function and clustering/bias as a function of luminosity and redshift; however, we argue that these are not sensitive probes of BH fueling mechanisms.

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“…-Case 2: Each galaxy suffers one major merger in the redshift interval, computed by assuming that each galaxy merges with a galaxy of identical mass (same mass curve). Jogee et al (2009) estimates that 68% of galaxies with stellar masses higher than 2.5 × 10 10 M have undergone a merger of mass ratio higher than 1/10 over lookback times of 3 to 7 Gyr. After including stellar masses as low as 10 9 M , they find that 84% of galaxies have undergone one merger.…”

Section: Build-up Of the "Quiescent" Stellar Mass Functionmentioning

confidence: 99%

“…Case 2 is highly biased in favor of major mergers given the results from several studies. For instance, Jogee et al (2009) find that 16% of galaxies have undergone a major merger over lookback times 3-7 Gyr. Based on galaxy pairs, de Ravel et al (2009) find that 22% of galaxies have undergone a major merger since z ∼ 0.9.…”

Section: Build-up Of the "Quiescent" Stellar Mass Functionmentioning

confidence: 99%

Stellar mass and velocity functions of galaxies

Boissier

Buat

Ilbert

2010

A&A

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Context. In recent years, stellar mass functions of both star-forming and quiescent galaxies have been observed at different redshifts in various fields. In addition, star formation rate (SFR) distributions (e.g. in the form of far infrared luminosity functions) were also obtained. Taken together, they offer complementary pieces of information concerning the evolution of galaxies. Aims. We attempt in this paper to check the consistency of the observed stellar mass functions, SFR functions, and the cosmic SFR density with simple backward evolutionary models. Methods. Starting from observed stellar mass functions for star-forming galaxies, we use backwards models to predict the evolution of a number of quantities, such as the SFR function, the cosmic SFR density and the velocity function. Because the velocity is a parameter attached to a galaxy during its history (contrary to the stellar mass), this approach allows us to quantify the number density evolution of galaxies of a given velocity, e.g. of the Milky Way siblings. Results. Observations suggest that the stellar mass function of star-forming galaxies is constant between redshift 0 and 1. To reproduce this result, we must quench star formation in a number of star-forming galaxies. The stellar mass function of these "quenched" galaxies is consistent with available data concerning the increase in the population of quiescent galaxies in the same redshift interval. The stellar mass function of quiescent galaxies is then mainly determined by the distribution of active galaxies that must stop star formation, with a modest mass redistribution during mergers. The cosmic SFR density and the evolution of the SFR functions are recovered relatively well, although they provide some clues to a minor evolution of the stellar mass function of star forming galaxies at the lowest redshifts. We thus consider that we have obtained in a simple way a relatively consistent picture of the evolution of galaxies at intermediate redshifts. If this picture is correct, 50% of the Milky-Way sisters (galaxies with the same velocity as our Galaxy, i.e. 220 km s −1 ) have quenched their star formation since redshift 1 (and an even higher fraction for higher velocities). We discuss the processes that might be responsible for this transformation.

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HISTORY OF GALAXY INTERACTIONS AND THEIR IMPACT ON STAR FORMATION OVER THE LAST 7 Gyr FROM GEMS

Cited by 242 publications

References 120 publications

Galaxy pairs in the Sloan Digital Sky Survey – VIII. The observational properties of post-merger galaxies

Galaxy pairs in the Sloan Digital Sky Survey – VIII. The observational properties of post-merger galaxies

Do we expect most AGN to live in discs?

Stellar mass and velocity functions of galaxies

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