NoSOCS in SDSS – VI. The environmental dependence of AGN in clusters and  field in the local Universe

Lopes, P. A. A.; Ribeiro, André; Rembold, Sandro Barboza

doi:10.1093/mnras/stx2046

Cited by 41 publications

(48 citation statements)

References 57 publications

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“…This is consistent with what might be expected based on our demonstration of the importance of halo mass for galaxy nuclear activity. Furthermore, both Lopes et al (2017) and Barsanti et al (2017) observe the opposite effect for passive galaxies, with the passive population being more centrally located. As would be expected based on our observations, this effect is stronger in clusters than groups.…”

Section: Galaxy Location Within the Group Structurementioning

confidence: 92%

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Galaxy And Mass Assembly (GAMA): the effect of galaxy group environment on active galactic nuclei

Gordon

Pimbblet

Owers

et al. 2018

Monthly Notices of the Royal Astronomical Society

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In galaxy clusters, efficiently accreting active galactic nuclei (AGN) are preferentially located in the infall regions of the cluster projected phase-space, and are rarely found in the cluster core. This has been attributed to both an increase in triggering opportunities for infalling galaxies, and a reduction of those mechanisms in the hot, virialised, cluster core. Exploiting the depth and completeness (98 per cent at r < 19.8 mag) of the Galaxy And Mass Assembly survey (GAMA), we probe down the group halo mass function to assess whether AGN are found in the same regions in groups as they are in clusters. We select 451 optical AGN from 7498 galaxies with log 10 (M * /M ) > 9.9 in 695 groups with 11.53 ≤ log 10 (M 200 /M ) ≤ 14.56 at z < 0.15. By analysing the projected phase-space positions of these galaxies we demonstrate that when split both radially, and into physically derived infalling and core populations, AGN position within group projected phase-space is dependent on halo mass. For groups with log 10 (M 200 /M ) > 13.5, AGN are preferentially found in the infalling galaxy population with 3.6σ confidence. At lower halo masses we observe no difference in AGN fraction between core and infalling galaxies. These observations support a model where a reduced number of low-speed interactions, ram pressure stripping and intra-group/cluster medium temperature, the dominance of which increase with halo mass, work to inhibit AGN in the cores of groups and clusters with log 10 (M 200 /M ) > 13.5, but do not significantly affect nuclear activity in cores of less massive structures.

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Section: Galaxy Location Within the Group Structurementioning

confidence: 92%

“…The likelihood of a galaxy hosting an AGN increases with stellar mass (Pimbblet & Jensen 2012;Pimbblet et al 2013;Wang et al 2017;Lopes et al 2017). Given that the central galaxies in groups are the most massive, the deficit of AGN in the cores of massive groups and clusters is unlikely to be a stellar mass bias.…”

Section: Stellar Massmentioning

confidence: 99%

Galaxy And Mass Assembly (GAMA): the effect of galaxy group environment on active galactic nuclei

Gordon

Pimbblet

Owers

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…Interestingly, the HDSGs that do not have evidence for star formation at their centers primarily occupy the small velocity, large radius region of the arc-like shape in PPS. The KDE contours reveal that the PASGs and SFGs exhibit a mirrorflipped distribution about the R/R 200 axis: the density of SFGs increases with radius and the velocity spread stays rel- We test the significance of the difference observed in the PPS distributions for the PASG, SFG, and HDSG samples using the multivariate two-sample KDE test developed by Duong et al (2012) for the purpose of comparing cell morphologies, and recently applied to PPS distributions by Lopes et al (2017) andde Carvalho et al (2017). The KDE test is nonparametric and uses the integrated square error as a measure of the discrepancy between two KDEs to test the hypothesis that two distributons are drawn from the same underlying density distribution (see Duong et al 2012, for details).…”

Section: Projected Phase Space Distributionmentioning

confidence: 99%

The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies

Owers

Hudson

Oman

et al. 2019

ApJ

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We use integral field spectroscopy from the SAMI Galaxy Survey to identify galaxies that show evidence for recent quenching of star formation. The galaxies exhibit strong Balmer absorption in the absence of ongoing star formation in more than 10% of their spectra within the SAMI field of view. These Hδ-strong galaxies (HDSGs) are rare, making up only ∼ 2% (25/1220) of galaxies with stellar mass log(M * /M ⊙ )> 10. The HDSGs make up a significant fraction of non-passive cluster galaxies (15%; 17/115) and a smaller fraction (2.0%; 8/387) of the non-passive population in low-density environments. The majority (9/17) of cluster HDSGs show evidence for star formation at their centers, with the HDS regions found in the outer parts of the galaxy. Conversely, the Hδ-strong signal is more evenly spread across the galaxy for the majority (6/8) of HDSGs in low-density environments, and is often associated with emission lines that are not due to star formation. We investigate the location of the HDSGs in the clusters, finding that they are exclusively within 0.6R 200 of the cluster centre, and have a significantly higher velocity dispersion relative to the cluster population. Comparing their distribution in projected-phase-space to those derived from cosmological simulations indicates that the cluster HDSGs are consistent with an infalling population that have entered the central 0.5r 200,3D cluster region within the last ∼ 1 Gyr. In the 8/9 cluster HDSGs with central star formation, the extent of star formation is consistent with that expected of outside-in quenching by ram-pressure stripping. Our results indicate that the cluster HDSGs are currently being quenched by ram-pressure stripping on their first passage through the cluster.

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“…It is well-known that massive quiescent galaxies are more predominant in the centres of galaxy clusters relative to the general fields in the present day. This trend is often characterised by colours (de Vaucouleurs 1961;Visvanathan & Sandage 1977;Butcher & Oemler 1984;Bower et al 1992Bower et al , rhythm@naoj.org 1998Terlevich et al 2001;Tanaka et al 2005;Kodama et al 2007;Mei et al 2009;Bamford et al 2009;Peng et al 2010;Muzzin et al 2012;Wetzel et al 2012;Darvish et al 2016) and morphological types (Dressler 1980;Dressler et al 1997;Couch et al 1998;Goto et al 2003;Kauffmann et al 2004;van der Wel 2008;Cappellari et al 2011;Houghton et al 2013;Fogarty et al 2014;Brough et al 2017;Lopes et al 2017). Over ten billion years ago, the most massive structures in the Universe -galaxy protoclusters -played a prominent role in the star formation and mass assembly of massive galaxies (Chiang et al 2017).…”

Section: Introductionmentioning

confidence: 99%

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

Shimakawa

Koyama

Röttgering

et al. 2018

Monthly Notices of the Royal Astronomical Society

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This paper is the second in a series presenting the results of our deep Hα-line survey towards protoclusters at z > 2, based on narrow-band imaging with the Subaru Telescope. This work investigates massive galaxies in a protocluster region associated with a radio galaxy (PKS 1138−262), the Spiderweb galaxy, at z = 2.2. Our 0.5 mag deeper narrow-band imaging than previous surveys collects a total of 68 Hα emitters (HAE). 17 out of the 68 are newly discovered protocluster members. First, a very high characteristic stellar mass of M * = 10 11.73 M is measured from a Schechter function fit to the mass distribution of HAEs. Together with the Chandra X-ray data, we find that four out of six massive HAEs (M > 10 11 M ) show bright X-ray emission, suggesting that they host active galactic nuclei (AGNs). Their mass estimates, therefore, would be affected by the nuclear emission from AGNs. Notably, the X-ray detected HAEs are likely positioned near the boundary between star-forming and quiescent populations in the rest-frame UV J plane. Moreover, our deep narrow-band data succeed in probing the bright Hα (+[Nii]) line nebula of the Spiderweb galaxy extending over ∼ 100 physical kpc. These results suggest that the massive galaxies in the Spiderweb protocluster are on the way to becoming the bright red sequence objects seen in local galaxy clusters, where AGNs might play an essential role in their quenching processes. Though a more statistical database is needed to build a general picture.

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NoSOCS in SDSS – VI. The environmental dependence of AGN in clusters and field in the local Universe

Cited by 41 publications

References 57 publications

Galaxy And Mass Assembly (GAMA): the effect of galaxy group environment on active galactic nuclei

Galaxy And Mass Assembly (GAMA): the effect of galaxy group environment on active galactic nuclei

The SAMI Galaxy Survey: Quenching of Star Formation in Clusters I. Transition Galaxies

MAHALO Deep Cluster Survey II. Characterizing massive forming galaxies in the Spiderweb protocluster at z = 2.2

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