A CENSUS OF MID-INFRARED-SELECTED ACTIVE GALACTIC NUCLEI IN MASSIVE GALAXY CLUSTERS AT 0 ≲<i>z</i>≲ 1.3

Tomczak, Adam; Tran, Kim‐Vy H.; Saintonge, A.

doi:10.1088/0004-637x/738/1/65

Cited by 8 publications

(8 citation statements)

References 101 publications

(205 reference statements)

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“…10), we do not see any significant dependence of f AGN on redshift. However, note that the redshift range in this study is much narrower than other studies that show a substantial increase of AGN fraction of cluster galaxies (e.g., 0.0 < ∼ z < ∼ 1.3 in Martini et al 2009;and Tomczak et al 2011). …”

Section: Notescontrasting

confidence: 53%

Activity in galactic nuclei of cluster and field galaxies in the local universe

Hwang

Park

Elbaz

et al. 2012

A&A

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Aims. We study the environmental effects on the activity in galactic nuclei by comparing galaxies in clusters and in the field. Methods. Using a spectroscopic sample of galaxies in Abell clusters from the Sloan Digital Sky Survey Data Release 7, we investigate the dependence of nuclear activity on the physical parameters of clusters as well as the nearest neighbor galaxy. We also compare galaxy properties between active galactic nuclei (AGNs) hosts and non-AGN galaxies. Results. We find that the AGN fraction of early-type galaxies starts to decrease around one virial radius of clusters (r 200,cl ) as decreasing clustercentric radius, while that of late types starts to decrease close to the cluster center (R ∼ 0.1−0.5r 200,cl ). The AGN fractions of early-type cluster galaxies, on average, are found to be lower than those of early-type field galaxies by a factor ∼3. However, the mean AGN fractions of late-type cluster galaxies are similar to those of late-type field galaxies. The AGN fraction of early-type brightest cluster galaxies lies between those of other early-type, cluster and field galaxies with similar luminosities. In the field, the AGN fraction is strongly dependent on the morphology of and the distance to the nearest neighbor galaxy. We find an anti-correlation between the AGN fraction and the velocity dispersion of clusters for all subsamples divided by morphology and luminosity of host galaxies. The AGN power indicated by L [OIII] /M BH is found to depend strongly on the mass of host galaxies rather than the clustercentric radius. The difference in physical parameters such as luminosity, (u − r) colors, star formation rates, and (g − i) color gradients between AGN hosts and non-AGN galaxies is seen for both early and late types at all clustercentric radii, while the difference in structure parameters between the two is significant only for late types. Conclusions. These results support the idea that the activity in galactic nuclei is triggered through galaxy-galaxy interactions and mergers when gas supply for AGN is available.

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Section: Notescontrasting

confidence: 53%

Activity in galactic nuclei of cluster and field galaxies in the local universe

Hwang

Park

Elbaz

et al. 2012

A&A

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“…Eastman et al 2007;Martini, Sivakoff & Mulchaey 2009;Tomczak, Tran & Saintonge 2011). Although we expect that the majority of our Hα-selected sources are starforming galaxies, a fraction of Hα emitters might be powered by AGNs, and so we here check the possible contribution of AGNs into our sample.…”

Section: Agn Contaminationmentioning

confidence: 99%

Massive starburst galaxies in a z = 2.16 proto-cluster unveiled by panoramic Hα mapping

Koyama

Kodama

Tadaki

et al. 2012

Monthly Notices of the Royal Astronomical Society

168

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We present a panoramic narrow-band study of Hα emitters in the field of the z = 2.16 protocluster around PKS 1138−262 using MOIRCS on the Subaru Telescope. We find 83 Hα emitters down to a star formation rate of SFR (Hα) ∼ 10 M yr −1 across a ∼7 × 7 arcmin 2 region centred on the radio galaxy, and identify ∼10-Mpc scale filaments of emitters running across this region. By examining the properties of Hα emitters within the large-scale structure, we find that galaxies in the higher density environments at z = 2.16 tend to have redder colours and higher stellar masses compared to galaxies in more underdense regions. We also find a population of Hα emitters with red colours [(J − K s ) 1], which are much more frequent in the denser environments and which have apparently very high stellar masses with M * 10 11 M , implying that these cluster galaxies have already formed a large part of their stellar mass before z ∼ 2. Spitzer Space Telescope 24-µm data suggest that many of these red Hα emitters are bright, dusty starbursts (rather than quiescent sources). We also find that the proto-cluster galaxies follow the same correlation between SFR and M * (the 'main sequence') of z ∼ 2 field star-forming galaxies, but with an excess of massive galaxies. These very massive star-forming galaxies are not seen in our similar, previous study of z ∼ 1 clusters, suggesting that their star formation activity has been shut off at 1 z 2. We infer that the massive red (but active) galaxies in this rich proto-cluster are likely to be the products of environmental effects, and they represent the accelerated galaxy formation and evolution in a biased high-density region in the early Universe.

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“…Throughout we make the simplification that the IR luminosity is entirely produced by star-formation, with no AGN contamination. This assumption is likely an oversimplification (Tomczak et al 2011) and does not affect the primary conclusions of the paper which depend only on the IR luminosity, not the source of activity. We discuss AGN throughout the paper, when they are relevant to the conclusions.…”

Section: Introductionmentioning

confidence: 97%

THE EVOLUTION OF DUSTY STAR FORMATION IN GALAXY CLUSTERS TOz= 1:SPITZERINFRARED OBSERVATIONS OF THE FIRST RED-SEQUENCE CLUSTER SURVEY

Webb

O'Donnell

Yee

et al. 2013

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We present the results of an infrared (IR) study of high-redshift galaxy clusters with the MIPS camera on board the Spitzer Space Telescope. We have assembled a sample of 42 clusters from the Red-Sequence Cluster Survey-1 over the redshift range 0.3 < z < 1.0 and spanning an approximate range in mass of 10 14−15 M ⊙ . We statistically measure the number of IR-luminous galaxies in clusters above a fixed inferred IR luminosity of 2×10 11 M ⊙ , assuming a star forming galaxy template, per unit cluster mass and find it increases to higher redshift. Fitting a simple power-law we measure evolution of (1 + z) 5.1±1.9 over the range 0.3 < z < 1.0. These results are tied to the adoption of a single star forming galaxy template; the presence of AGN, and an evolution in their relative contribution to the mid-IR galaxy emission, will alter the overall number counts per cluster and their rate of evolution. Under the star formation assumption we infer the approximate total SFR per unit cluster mass (ΣSFR/M cluster ). The evolution is similar, with ΣSFR/M cluster ∼ (1 + z) 5.4±1.9 . We show that this can be accounted for by the evolution of the IR-bright field population over the same redshift range; that is, the evolution can be attributed entirely to the change in the in-falling field galaxy population. We show that the ΣSFR/M cluster (binned over all redshift) decreases with increasing cluster mass with a slope (ΣSFR/M cluster ∼ M −1.5±0.4 cluster ) consistent with the dependence of the stellarto-total mass per unit cluster mass seen locally. The inferred star formation seen here could produce ∼5-10% of the total stellar mass in massive clusters at z = 0, but we cannot constrain the descendant population, nor how rapidly the star-formation must shut-down once the galaxies have entered the cluster environment. Finally, we show a clear decrease in the number of IR-bright galaxies per unit optical galaxy in the cluster cores, confirming star formation continues to avoid the highest density regions of the universe at z ∼ 0.75 (the average redshift of the high-redshift clusters). While several previous studies appear to show enhanced star formation in high-redshift clusters relative to the field we note that these papers have not accounted for the overall increase in galaxy or dark matter density at the location of clusters. Once this is done, clusters at z ∼ 0.75 have the same or less star formation per unit mass or galaxy as the field.

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A CENSUS OF MID-INFRARED-SELECTED ACTIVE GALACTIC NUCLEI IN MASSIVE GALAXY CLUSTERS AT 0 ≲z≲ 1.3

Cited by 8 publications

References 101 publications

Activity in galactic nuclei of cluster and field galaxies in the local universe

Activity in galactic nuclei of cluster and field galaxies in the local universe

Massive starburst galaxies in a z = 2.16 proto-cluster unveiled by panoramic Hα mapping

THE EVOLUTION OF DUSTY STAR FORMATION IN GALAXY CLUSTERS TOz= 1:SPITZERINFRARED OBSERVATIONS OF THE FIRST RED-SEQUENCE CLUSTER SURVEY

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