Red Misfits in the Sloan Digital Sky Survey: properties of star-forming red galaxies

Evans, Fraser A.; Parker, Laura C.; Roberts, Ian

doi:10.1093/mnras/sty581

Cited by 22 publications

(42 citation statements)

References 215 publications

(318 reference statements)

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“…The KS test shows that the distributions of clustercentric distances of red star forming galaxies, and galaxies in rich and poor groups are statistically similar, with p-value p > 0.12. This agrees with earlier findings that red star forming galaxies in superclusters can be found in groups of various richness, they may also be central galaxies of groups (Wolf et al 2005;Einasto et al 2008Einasto et al , 2014Evans et al 2018, and references therein).…”

Section: Phase Space Diagram and Clustercentric Distancessupporting

confidence: 93%

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Einasto

Gramann

Park

et al. 2018

A&A

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Context. Superclusters with collapsing cores represent dynamically evolving environments for galaxies, galaxy groups, and clusters. Aims. We study the dynamical state and properties of galaxies and groups in the supercluster SCl A2142 that has a collapsing core, to understand its possible formation and evolution. Methods. We find the substructure of galaxy groups using normal mixture modelling. We have used the projected phase space (PPS) diagram, spherical collapse model, clustercentric distances, and magnitude gap between the brightest galaxies in groups to study the dynamical state of groups and to analyse group and galaxy properties. We compared the alignments of groups and their brightest galaxies with the supercluster axis. Results. The supercluster core has a radius of about 8 h −1 Mpc and total mass M tot ≈ 2.3 × 10 15 h −1 M ⊙ and is collapsing. Galaxies in groups on the supercluster axis have older stellar populations than off-axis groups, with median stellar ages 4 − 6 and < 4 Gyr, correspondingly. The cluster A2142 and the group Gr8 both host galaxies with the oldest stellar populations among groups in SCl A2142 having the median stellar age t > 8 Gyr. Recently quenched galaxies and active galactic nuclei (AGNs) are mostly located at virial radii or in merging regions of groups, and at clustercentric distances D c ≈ 6 h −1 Mpc. The most elongated groups lie along the supercluster axis and are aligned with it. Magnitude gaps between the brightest galaxies of groups are less than one magnitude, suggesting that groups in SCl A2142 are dynamically young. Conclusions. The collapsing core of the supercluster, infall of galaxies and groups, and possible merging groups, which affect galaxy properties and may trigger the activity of AGNs, show how the whole supercluster is evolving.

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Section: Phase Space Diagram and Clustercentric Distancessupporting

confidence: 93%

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Einasto

Gramann

Park

et al. 2018

A&A

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“…To explore the connection on this trend for these two different population of galaxies, we have checked that low-mass red isolated galaxies with a SFN at high Q LSS are also star-forming galaxies. This population of red and star-forming galaxies in the Local Universe is known as Red Misfits (Evans et al 2018), a transition population to the red sequence, where the quenching is dominated by internal processes rather than environmentallydriven processes. Then it would be somehow expected to find this population in isolated galaxies.…”

Section: Dependence On the Lss Environmentmentioning

confidence: 99%

The dependence of mass and environment on the secular processes of AGNs in terms of morphology, colour, and specific star-formation rate

Argudo-Fernández

Lacerna

Puertas

2018

A&A

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Context. Galaxy mass and environment play a major role in the evolution of galaxies. In the transition from star-forming to quenched galaxies, Active galactic nuclei (AGN) have also a principal action. However, the connections between these three actors are still uncertain. Aims. In this work we investigate the effects of stellar mass and the large-scale environment (LSS), on the fraction of optical nuclear activity in a population of isolated galaxies, where AGN would not be triggered by recent galaxy interactions or mergers. Methods. As a continuation of a previous work, we focus on isolated galaxies to study the effect of stellar mass and the LSS in terms of morphology (early-and late-type), colour (red and blue), and specific star formation rate (quenched and star-forming). To explore where AGN activity is affected by the LSS we fix the stellar mass into low-and high-mass galaxies. We use the tidal strength parameter to quantify their effects. Results. We found that AGN is strongly affected by stellar mass in "active" galaxies (namely late-type, blue, and star-forming), however it has no influence for "quiescent" galaxies (namely early-type, red, and quenched), at least for masses down to 10 10 [M ]. In relation to the LSS, we found an increment on the fraction of SFN with denser LSS in low-mass star forming and red isolated galaxies. Regarding AGN, we find a clear increment of the fraction of AGN with denser environment in quenched and red isolated galaxies, independently of the stellar mass. Conclusions. AGN activity would be "mass triggered" in "active" isolated galaxies. This means that AGN is independent of the intrinsic property of the galaxies, but on its stellar mass. On the other hand, AGN would be "environment triggered" in "quiescent" isolated galaxies, where the fraction of AGN in terms of sSFR and colour increases from void regions to denser LSS, independently of its stellar mass.

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“…Environmental quenching is often used to explain the morphology-density relation, whereby red bulge-dominated galaxies are more likely to be found in dense environments, and blue disc-dominated galaxies are more commonly found in underdense environments (Oemler 1974;Dressler 1980;Lewis et al 2002;Goto et al 2003;Gómez et al 2003;Balogh et al 2004;Yang et al 2007;Bamford et al 2009). Although there are some exceptions to these trends -such as blue ellipticals (Schawinski et al 2014) and red spirals (Masters et al 2010;Evans et al 2018) -the general bi-modality of galaxy colour and morphology holds true.…”

Section: Introductionmentioning

confidence: 99%

Smaller stellar disc scale lengths in rich environments

Demers

Parker

Roberts

2019

Monthly Notices of the Royal Astronomical Society

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We investigate the dependence of stellar disc scale lengths on environment for a sample of Sloan Digital Sky Survey Data Release 7 galaxies with published photometric bulge-disc decompositions. We compare disc scale lengths at fixed bulge mass for galaxies in an isolated field environment to galaxies in X-ray rich and X-ray poor groups. At low bulge mass, stellar disc scale lengths in X-ray rich groups are smaller compared to discs in both X-ray poor groups and in isolated field environments. This decrease in disc scale length is largely independent of halo mass, though shows some dependence on group-centric distance. We also find that stellar disc scale lengths are smaller in X-ray rich environments for a subset of starforming galaxies and for galaxies of different morphological types. We note that disc scale lengths of low mass galaxies are known to have large systematic uncertainties, however we focus on differences between samples with the same measurement biases. Our results show that stellar disc scale lengths depend on X-ray brightness, a tracer of IGM density, suggesting a role for hydrodynamic processes such as ram-pressure stripping and/or starvation.

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Red Misfits in the Sloan Digital Sky Survey: properties of star-forming red galaxies

Cited by 22 publications

References 215 publications

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

Supercluster A2142 and collapse in action: infalling and merging groups and galaxy transformations

The dependence of mass and environment on the secular processes of AGNs in terms of morphology, colour, and specific star-formation rate

Smaller stellar disc scale lengths in rich environments

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