The origin of H I-deficiency in galaxies on the outskirts of the Virgo cluster

Mamon, G. A.; Sanchís, T.; Salvador-Solé, E.; Solanes, J. M.

doi:10.1051/0004-6361:20034155

Cited by 138 publications

(158 citation statements)

References 28 publications

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“…Cetus and Tucana) are likely systems that previously interacted with either the Milky Way or M31 (i.e. "backsplash" or "super-virial" galaxies, Mamon et al 2004, Wetzel et al 2014. This broadly agrees with our observations of low-mass isolated systems as well as the results of Geha et al (2012).…”

Section: Comparison To Previous Studiessupporting

confidence: 88%

The mass dependence of satellite quenching in Milky Way-like haloes

Phillips

Wheeler

Cooper

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using the Sloan Digital Sky Survey, we examine the quenching of satellite galaxies around isolated Milky Way-like hosts in the local Universe. We find that the efficiency of satellite quenching around isolated galaxies is low and roughly constant over two orders of magnitude in satellite stellar mass (M = 10 8.5 − 10 10.5 M ), with only ∼ 20% of systems quenched as a result of environmental processes. While largely independent of satellite stellar mass, satellite quenching does exhibit clear dependence on the properties of the host. We show that satellites of passive hosts are substantially more likely to be quenched than those of star-forming hosts, and we present evidence that more massive halos quench their satellites more efficiently. These results extend trends seen previously in more massive host halos and for higher satellite masses. Taken together, it appears that galaxies with stellar masses larger than about 10 8 M are uniformly resistant to environmental quenching, with the relative harshness of the host environment likely serving as the primary driver of satellite quenching. At lower stellar masses (< 10 8 M ), however, observations of the Local Group suggest that the vast majority of satellite galaxies are quenched, potentially pointing towards a characteristic satellite mass scale below which quenching efficiency increases dramatically.

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Section: Comparison To Previous Studiessupporting

confidence: 88%

The mass dependence of satellite quenching in Milky Way-like haloes

Phillips

Wheeler

Cooper

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…Bahé et al 2013). To address this, we also show pre-processing results for our 'strict' infall sample (2 < R < 3 R 200 ) which should be less susceptible to backsplash contamination, as many previous studies have shown that the majority of backsplashing galaxies are found within two virial radii (Mamon et al 2004;Mahajan et al 2011;Oman et al 2013;Haines et al 2015). If contamination from backsplash galaxies is low, this field excess should approximate the fraction of galaxies which have been pre-processed prior to infalling onto their present-day group.…”

Section: Galaxy Properties At Large Radiimentioning

confidence: 88%

Evidence of pre-processing and a dependence on dynamical state for low-mass satellite galaxies

Roberts¹,

Parker²

2017

Monthly Notices of the Royal Astronomical Society

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We study the dependence of satellite star formation rate and morphology on group dynamics for a sample of SDSS groups. We classify the group dynamical state and study satellite properties for populations of galaxies at small and large group-centric radii. For galaxies at large radii we find no differences in the star-forming or disc fraction for those in Gaussian groups compared to those in non-Gaussian groups. By comparing the star-forming and disc fractions of infalling galaxies to field galaxies we find evidence for the pre-processing of both star formation rate and morphology. The strength of pre-processing increases with halo mass and is highest for low-mass galaxies infalling onto high-mass haloes. We show that the star formation rate of galaxies at small radii correlates with group dynamical state, with galaxies in nonGaussian groups showing enhanced star-forming fractions compared to galaxies in Gaussian groups. Similar correlations are not seen for the disc fractions of galaxies at small radii. This seems to suggest that either the mechanisms driving star formation quenching at small halo-centric radii are more efficient in dynamically relaxed groups, or that non-Gaussian groups have assembled more recently and therefore satellites of the groups will have been exposed to these transforming mechanisms for less time.

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“…Our analysis shows that most of the galaxies located at the position of the bump at a given redshift, are also positioned in the region of the bumps in later outputs. This finding leads us to rule out the possibility of rebound galaxies (Mamon et al 2004;Gill et al 2005;Mamon 2006) being the cause of the bump since these galaxies are expected to dramatically change their positions with respect to the group centre between redshifts 0.69 and 0.00. The apparent movement of the bump could therefore be the result of either infalling substructure or simply the growth of the virial radii of the systems concerned, i.e.…”

Section: The Apparent Movementmentioning

confidence: 98%

Fossil groups in the Millennium simulation

Díaz-Giménez

Zandivarez

Proctor³

et al. 2011

A&A

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Context. Fossil systems are defined to be X-ray bright galaxy groups (or clusters) with a two-magnitude difference between their two brightest galaxies within half the projected virial radius, and represent an interesting extreme of the population of galaxy agglomerations. However, the physical conditions and processes leading to their formation are still poorly constrained. Aims. We compare the outskirts of fossil systems with that of normal groups to understand whether environmental conditions play a significant role in their formation. We study the groups of galaxies in both, numerical simulations and observations. Methods. We use a variety of statistical tools including the spatial cross-correlation function and the local density parameter Δ 5 to probe differences in the density and structure of the environments of "normal" and "fossil" systems in the Millennium simulation. Results. We find that the number density of galaxies surrounding fossil systems evolves from greater than that observed around normal systems at z = 0.69, to lower than the normal systems by z = 0. Both fossil and normal systems exhibit an increment in their otherwise radially declining local density measure (Δ 5 ) at distances of order 2.5 r vir from the system centre. We show that this increment is more noticeable for fossil systems than normal systems and demonstrate that this difference is linked to the earlier formation epoch of fossil groups. Despite the importance of the assembly time, we show that the environment is different for fossil and non-fossil systems with similar masses and formation times along their evolution. We also confirm that the physical characteristics identified in the Millennium simulation can also be detected in SDSS observations. Conclusions. Our results confirm the commonly held belief that fossil systems assembled earlier than normal systems but also show that the surroundings of fossil groups could be responsible for the formation of their large magnitude gap.

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The origin of H I-deficiency in galaxies on the outskirts of the Virgo cluster

Cited by 138 publications

References 28 publications

The mass dependence of satellite quenching in Milky Way-like haloes

The mass dependence of satellite quenching in Milky Way-like haloes

Evidence of pre-processing and a dependence on dynamical state for low-mass satellite galaxies

Fossil groups in the Millennium simulation

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