Galaxy And Mass Assembly (GAMA): A “No Smoking” Zone for Giant Elliptical Galaxies?

Khosroshahi, Habib G.; Raouf, Mojtaba; Miraghaei, H.; Brough, Sarah; Croton, Darren J.; Driver, Simon P.; Graham, Alister W.; Baldry, I. K.; Brown, M. J. I.; Prescott, M.; Wang, Lingyu

doi:10.3847/1538-4357/aa7048

Cited by 25 publications

(27 citation statements)

References 73 publications

(104 reference statements)

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“…Raouf et al (2016) analysed the properties of the black holes developed in the center of the BCGs for fossil and non-fossil systems. They found that the mass of the black holes hosted in BCGs is larger in dynamically evolved groups with a lower rate of mass accretion, a result confirmed also in Khosroshahi et al (2017). Kanagusuku et al (2016) found that fossil and non-fossil systems selected from the Millennium Simulation shown different galaxy populations.…”

Section: Theoretical Frameworkmentioning

confidence: 63%

Properties of Fossil Groups of Galaxies

Aguerri

Zarattini

2021

Universe

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We review the formation and evolution of fossil groups and clusters from both the theoretical and the observational points of view. In the optical band, these systems are dominated by the light of the central galaxy. They were interpreted as old systems that had enough time to merge all the M* galaxies within the central one. During the last two decades, many observational studies were performed to prove the old and relaxed state of fossil systems. The majority of these studies that spans a wide range of topics including halos global scaling relations, dynamical substructures, stellar populations, and galaxy luminosity functions seem to challenge this scenario. The general picture that can be obtained by reviewing all the observational works is that the fossil state could be transitional. Indeed, the formation of the large magnitude gap observed in fossil systems could be related to internal processes rather than an old formation.

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Section: Theoretical Frameworkmentioning

confidence: 63%

Properties of Fossil Groups of Galaxies

Aguerri

Zarattini

2021

Universe

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“…In particular, many unrelaxed clusters host MMGs with large offsets from other cluster centre definitions (e.g. Katayama et al 2003;Sanderson et al 2009;Carollo et al 2013;Khosroshahi et al 2017), therefore the offset between MMG position and luminosityweighted centre can be a useful measure of cluster relaxation.…”

Section: Mmg Offsetmentioning

confidence: 99%

Connecting optical and X-ray tracers of galaxy cluster relaxation

Roberts

Parker

Hlavacek-Larrondo

2018

Monthly Notices of the Royal Astronomical Society

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Substantial effort has been devoted in determining the ideal proxy for quantifying the morphology of the hot intracluster medium in clusters of galaxies. These proxies, based on X-ray emission, typically require expensive, high-quality X-ray observations making them difficult to apply to large surveys of groups and clusters. Here, we compare optical relaxation proxies with X-ray asymmetries and centroid shifts for a sample of SDSS clusters with high-quality, archival X-ray data from Chandra and XMM-Newton. The three optical relaxation measures considered are: the shape of the member-galaxy projected velocity distribution -measured by the Anderson-Darling (AD) statistic, the stellar mass gap between the most-massive and second-most-massive cluster galaxy, and the offset between the most-massive galaxy (MMG) position and the luminosityweighted cluster centre. The AD statistic and stellar mass gap correlate significantly with X-ray relaxation proxies, with the AD statistic being the stronger correlator. Conversely, we find no evidence for a correlation between X-ray asymmetry or centroid shift and the MMG offset. High-mass clusters (M halo > 10 14.5 M ) in this sample have X-ray asymmetries, centroid shifts, and Anderson-Darling statistics which are systematically larger than for low-mass systems. Finally, considering the dichotomy of Gaussian and non-Gaussian clusters (measured by the AD test), we show that the probability of being a non-Gaussian cluster correlates significantly with X-ray asymmetry but only shows a marginal correlation with centroid shift. These results confirm the shape of the radial velocity distribution as a useful proxy for cluster relaxation, which can then be applied to large redshift surveys lacking extensive X-ray coverage.

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“…In addition to the biases caused by the host galaxy types, the definition of environment may also influence the results. Different environmental properties have been used to measure the level of galaxy interaction such as: local density or overdensity defined based on the nth nearest neighbour (Man et al 2019) or on the projected two-point cross-correlation function (Wang & Li 2018); number of galaxies within a specific radius (Malavasi et al 2015); the level of tidal interaction (Sabater et al 2013); galaxies in field, void galaxies and isolated galaxies versus galaxies in pairs, groups, clusters, filaments and walls Manzer & De Robertis 2014;Argudo-Fernandez et al 2016Magliocchetti et al 2018;Amiri et al 2019); galaxy group richness or halo mass (Li et al 2019); the distance to the center of galaxy group or galaxies in the core versus outskirt (Pimbblet et al 2013;Lopes et al 2017;Gordon et al 2018); group luminosity gap (Miraghaei et al 2014(Miraghaei et al , 2015Khosroshahi et al 2017) and status as a merging or non-merging system (Hong et al 2015).…”

Section: Agnmentioning

confidence: 99%

The Effect of Environment on AGN Activity: The Properties of Radio and Optical AGN in Void, Isolated, and Group Galaxies

Miraghaei

2020

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The evolution of galaxies depends on their environments. In this work, active galactic nucleus (AGN) activity in different environments has been studied. The fractions of radio and optical AGN in four different environments have been compared using samples of void, isolated, group member, and the brightest group galaxies (BGGs). Galaxies in voids show significantly lower stellar ages, concentrations, colours and surface mass densities, and they experience more oneon-one interactions compared to the isolated galaxies and galaxies in groups. In order to study pure environmental effects, the biases caused by the stellar mass and galaxy type quantified by 4000Å break strength have been removed. While the results confirm no dependence of the optical AGN activity on environment in blue galaxies and with lower significance in green galaxies, a higher fraction of optical AGN has been observed for the massive red galaxies in voids compared to the galaxies in dense environments. This may be related to the higher amount of one-on-one interaction observed in the void galaxies, or it may reflect more fundamental differences in the host galaxies or environments of the voids. The radio-mode AGN activity increases in dense environment for red galaxies. No changes in the radio-loud AGN fraction have been observed for the blue and green galaxies. This shows that the effect of environment on AGN activity is not significant in the presence of cold gas in galaxies. We also discuss whether the efficiency of gas accretion depends on the properties of the host galaxy.

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Galaxy And Mass Assembly (GAMA): A “No Smoking” Zone for Giant Elliptical Galaxies?

Cited by 25 publications

References 73 publications

Properties of Fossil Groups of Galaxies

Properties of Fossil Groups of Galaxies

Connecting optical and X-ray tracers of galaxy cluster relaxation

The Effect of Environment on AGN Activity: The Properties of Radio and Optical AGN in Void, Isolated, and Group Galaxies

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