The dynamical origin of early-type dwarfs in galaxy clusters: a theoretical investigation

Vijayaraghavan, Rukmani; Gallagher, John S.; Ricker, P. M.

doi:10.1093/mnras/stu2761

Cited by 22 publications

(26 citation statements)

References 84 publications

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“…Based on both measures, Skewness and Kurtosis, we conclude that faint galaxies in NG groups are mainly infalling for the first time in the cluster. Obviously, this result should be seen in average for the family of NGs but it is noticeable that 6 out 9 NG systems have Kurtosis < -0.5, strongly supporting the view that faint galaxies in these systems are in the very early stage of infalling, before the first pericentric passage (see Figure 8a of Vijayaraghavan et al 2015).…”

Section: Discussionsupporting

confidence: 56%

Investigating the Relation between Galaxy Properties and the Gaussianity of the Velocity Distribution of Groups and Clusters

Carvalho

Ribeiro²,

Stalder

et al. 2017

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We investigate the dependence of stellar population properties of galaxies on group dynamical stage for a subsample of Yang catalog. We classify groups according to their galaxy velocity distribution into Gaussian (G) and Non-Gaussian (NG). Using two totally independent approaches we have shown that our measurement of Gaussianity is robust and reliable. Our sample covers Yang's groups in the redshift range 0.03 ≤ z ≤ 0.1 having mass ≥ 10 14 M . The new method, Hellinger Distance (HD), to determine whether a group has a velocity distribution Gaussian or Non-Gaussian is very effective in distinguishing between the two families. NG groups present halo masses higher than the G ones, confirming previous findings. Examining the Skewness and Kurtosis of the velocity distribution of G and NG groups, we find that faint galaxies in NG groups are mainly infalling for the first time into the groups. We show that considering only faint galaxies in the outskirts, those in NG groups are older and more metal rich than the ones in G groups. Also, examining the Projected Phase Space of cluster galaxies we see that bright and faint galactic systems in G groups are in dynamical equilibrium which does not seem to be the case in NG groups. These findings suggest that NG systems have a higher infall rate, assembling more galaxies which experienced preprocessing before entering the group.

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Section: Discussionsupporting

confidence: 56%

Investigating the Relation between Galaxy Properties and the Gaussianity of the Velocity Distribution of Groups and Clusters

Carvalho

Ribeiro²,

Stalder

et al. 2017

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“…N-body simulations of infalling galaxy groups support their particular phase-space distribution as the result of a galaxy group accretion onto Virgo. According to simulations, this accretion event has taken place 2 to 3 Gyr ago, along the observer's line-of-sight (Vijayaraghavan et al 2015). Such a picture receives further support by studies of Pasquali et al (2019) and Smith et al (2019), who showed that cluster galaxies occupy different zones in the phase-space diagram with respect to their average infall time to cluster.…”

Section: Rementioning

confidence: 78%

On the accretion of a new group of galaxies on to Virgo: I. Internal kinematics of nine in-falling dEs

Bidaran

Pasquali

Lisker

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Galaxy environment has been shown to play an important role in transforming late-type, star-forming galaxies to quiescent spheroids. This transformation is expected to be more severe for low-mass galaxies (M < 1010M⊙) in dense galaxy groups and clusters, mostly due to the influence of their past host halos (also known as pre-processing) and their present-day environments. For the first time, in this study, we investigate a sample of nine early-type dwarf galaxies (dEs) that were accreted as a likely bound group onto the Virgo galaxy cluster about 2-3 Gyr ago. Considering this special condition, these nine dEs may provide a test bed for distinguishing between the influence of the Virgo galaxy cluster and the effects of the previous host halo on their current properties. Specifically, we use VLT/MUSE integral-field unit spectra to derive their kinematics and specific angular momentum (λR) profiles. We observe a spread in the λR profiles of our sample dEs, finding that the λR profiles of half of them are as high as those of low-mass field galaxies. The remaining dEs exhibit λR profiles as low as those of Virgo dEs that were likely accreted longer ago. Moreover, we detect nebular emission in one dE with a gas velocity offset suggesting ongoing gas stripping in Virgo. We suggest that the low-λR dEs in our sample were processed by their previous host halo, prior to their infall to Virgo, and that the high-λR dEs may be experiencing ram pressure stripping in Virgo.

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“…for signatures of a group infall (see, e.g. Vijayaraghavan et al 2015). On top of the above -and with large enough samples -one should always try to look at any global trends in more than one dimension, plotting them as maps, rather than 1D profiles, thus taking advantage of all the available bits of information on the galaxies.…”

Section: Determining the Dependence Of Galaxy Properties On The Envirmentioning

confidence: 99%

The hELENa project – I. Stellar populations of early-type galaxies linked with local environment and galaxy mass

Sybilska

Lisker

Küntschner

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the first in a series of papers in The role of Environment in shaping Low-mass Early-type Nearby galaxies (hELENa) project. In this paper we combine our sample of 20 low-mass early types (dEs) with 258 massive early types (ETGs) from the ATLAS 3D survey -all observed with the SAURON integral field unit (IFU) -to investigate early-type galaxies' stellar population scaling relations and the dependence of the population properties on local environment, extended to the low-σ regime of dEs. The ages in our sample show more scatter at lower σ values, indicative of less massive galaxies being affected by the environment to a higher degree. The shape of the age-σ relations for cluster vs. non-cluster galaxies suggests that cluster environment speeds up the placing of galaxies on the red sequence. While the scaling relations are tighter for cluster than for the field/group objects, we find no evidence for a difference in average population characteristics of the two samples. We investigate the properties of our sample in the Virgo cluster as a function of number density (rather than simple clustrocentric distance) and find that dE ages negatively correlate with the local density, likely because galaxies in regions of lower density are later arrivals to the cluster or have experienced less pre-processing in groups, and consequently used up their gas reservoir more recently. Overall, dE properties correlate more strongly with density than those of massive ETGs, which was expected as less massive galaxies are more susceptible to external influences.

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The dynamical origin of early-type dwarfs in galaxy clusters: a theoretical investigation

Cited by 22 publications

References 84 publications

Investigating the Relation between Galaxy Properties and the Gaussianity of the Velocity Distribution of Groups and Clusters

Investigating the Relation between Galaxy Properties and the Gaussianity of the Velocity Distribution of Groups and Clusters

On the accretion of a new group of galaxies on to Virgo: I. Internal kinematics of nine in-falling dEs

The hELENa project – I. Stellar populations of early-type galaxies linked with local environment and galaxy mass

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