On the origin of the faint-end of the red sequence in high-density environments

Boselli, A.; Gavazzi, G.

doi:10.1007/s00159-014-0074-y

Cited by 153 publications

(134 citation statements)

References 351 publications

(460 reference statements)

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“…As summarised in Boselli & Gavazzi (2014), these are now available only in optical bands (Sandage et al 1985, photographic B-band;Trentham & Hodgkin 2002, B-band;Rines & Geller 2008, r-band;Lieder et al (2012), V-and I-bands).…”

Section: Figmentioning

confidence: 99%

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg 2 , an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV − i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = −1.19), here sampled down to ∼NUV = −11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M * = −17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments.

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Section: Figmentioning

confidence: 99%

“…Dwarf systems are of particular interest in the study of the effects of the environment on galaxy evolution since they are fragile objects easily perturbed because of their shallow potential well (e.g. Boselli & Gavazzi 2014). …”

Section: Introductionmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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“…Certainly, there are some well known examples of tidal stripping, such as the Sagittarius dwarf spheroidal galaxy (Ibata et al 1994) which has an enormous stellar stream spanning the entire sky that reveals its interaction history with the Milky Way (Ibata et al 2001;Majewski et al 2003 and references therein). There are also numerous examples of galaxies undergoing ram-pressure stripping due to interactions in cluster-like environments (e.g., NGC4522 in the Virgo cluster, Vollmer et al 2000; Peg DIG in the Local Group, McConnachie et al 2007b; see also Boselli & Gavazzi 2014). But the proximity of a large galaxy can introduce more subtle effects in the properties of the smaller satellite.…”

Section: Introductionmentioning

confidence: 99%

Solo dwarfs I: survey introduction and first results for the Sagittarius dwarf irregular galaxy

Higgs¹,

McConnachie²,

Irwin³

et al. 2016

Mon. Not. R. Astron. Soc.

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We introduce the Solitary Local Dwarfs Survey (Solo), a wide field photometric study targeting every isolated dwarf galaxy within 3 Mpc of the Milky Way. Solo is based on (u)gi multi-band imaging from CFHT/MegaCam for northern targets, and Magellan/Megacam for southern targets. All galaxies fainter than M V −18 situated beyond the nominal virial radius of the Milky Way and M31 ( 300 kpc) are included in this volume-limited sample, for a total of 42 targets. In addition to reviewing the survey goals and strategy, we present results for the Sagittarius Dwarf Irregular Galaxy (Sag DIG), one of the most isolated, low mass galaxies, located at the edge of the Local Group. We analyze its resolved stellar populations and their spatial distributions. We provide updated estimates of its central surface brightness and integrated luminosity, and trace its surface brightness profile to a level fainter than 30 mag./sq.arcsec. Sag DIG is well described by a highly elliptical (disk-like) system following a single component Sersic model. However, a low-level distortion is present at the outer edges of the galaxy that, were Sag DIG not so isolated, would likely be attributed to some kind of previous tidal interaction. Further, we find evidence of an extremely low level, extended distribution of stars beyond ∼ 5 arcmins (> 1.5 kpc) that suggests Sag DIG may be embedded in a very low density stellar halo. We compare the stellar and HI structures of Sag DIG, and discuss results for this galaxy in relation to other isolated, dwarf irregular galaxies in the Local Group.

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“…This loss of gas stops the active star formation of the galaxies and produces a decrease in their stellar surface brightness (see e.g. Boselli & Gavazzi 2014;Rodríguez Del Pino et al 2014). In particular, the end of the star formation in the outer galaxy regions would produce a fading of these regions, producing shorter length scales of the discs of the galaxies.…”

Section: Other Possible Formation Scenarios Of Ds0 Galaxiesmentioning

confidence: 99%

“…Arnaboldi et al 2002;Aguerri et al 2005b;Gerhard et al 2005;Castro-Rodriguéz et al 2009). It is still a matter of debate which of these physical mechanisms drives the evolution of dwarf galaxies in high-density environments (see Boselli & Gavazzi 2014, for a recent review).…”

Section: Introductionmentioning

confidence: 99%

Early-type dwarf galaxies with multicomponent stellar structure: Are they remnants of disc galaxies strongly transformed by their environment?

Aguerri

2016

A&A

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Context. The surface brightness distribution of ∼30-40% of the early-type dwarf galaxies with −18 ≤ M B ≤ −15 in the Virgo and the Coma clusters is fitted by models that include two structural components (Sérsic + exponential) as for bright disc galaxies. Aims. The goal of the present study is to determine whether early-type dwarf galaxies with a two-component stellar structure in the Virgo and the Coma clusters are low-luminosity copies of bright disc galaxies or are the remnants of bright galaxies strongly transformed by cluster environmental effects. Methods. I analysed the location of bright disc galaxies and early-type dwarfs in the r b,e /h-n plane. The location in this plane of the two-component dwarf galaxies was compared with the remnants of tidally disrupted disc galaxies reported by numerical simulations. Results. Bright unbarred disc galaxies show a strong correlation in the r b,e /h-n plane. Galaxies with larger Sérsic shape parameters show a higher r b,e /h ratio. In contrast, two-component early-type dwarf galaxies do not follow the same correlation. A fraction (∼55%) of them are located outside the locus defined in this plane by having 95% of bright disc galaxies. This distribution indicates that they are not a low-mass replica of bright disc galaxies. The different location in the r b,e /h-n plane of two-component early-type dwarfs and bright galaxies can be qualitatively explain whether the former are remnants of disc galaxies strongly transformed by tidal processes. Conclusions. The progenitors of ∼20−25% of early-type dwarf galaxies with −18 ≤ M B ≤ −15 in the Virgo and Coma clusters could be bright disc galaxies transformed by effects of the environment. These tidally transformed galaxies can be selected according to their location in the r b,e /h-n plane.

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On the origin of the faint-end of the red sequence in high-density environments

Cited by 153 publications

References 351 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Solo dwarfs I: survey introduction and first results for the Sagittarius dwarf irregular galaxy

Early-type dwarf galaxies with multicomponent stellar structure: Are they remnants of disc galaxies strongly transformed by their environment?

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