An H i view of galaxy conformity: H i-rich environment around H i-excess galaxies

Wang, Jing; Serra, P.; Józsa, G. I. G.; Koribalski, B. S.; Hulst, J. M. van der; Kamphuis, P.; Li, Cheng; Fu, Jiang; Xiao, Ting; Overzier, Roderik; Wieringa, M.; Wang, Enci

doi:10.1093/mnras/stv1767

Cited by 21 publications

(18 citation statements)

References 61 publications

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“…Here we have been considering possible scenarios that can explain their H i gas content. H i-rich central galaxies could be a result of H i-rich mergers and/or gas accretion from the intrafilament medium (Janowiecki et al 2017;Kleiner et al 2017;Wang et al 2015). However, gas accretion from minor mergers is thought not to be significant, Sancisi et al (2008) and Di Teodoro & Fraternali (2014) estimate (for spiral galaxies from the WHISP sample) a maximum gas accretion rate to be 0.1-0.2 and 0.28 M yr −1 respectively, which is not enough to sustain star formation.…”

Section: Discussionmentioning

confidence: 99%

The neutral hydrogen properties of galaxies in gas-rich groups

Džudžar

Kilborn

Meurer

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the integrated neutral hydrogen (H i) properties for 27 galaxies within nine low mass, gas-rich, late-type dominated groups which we denote "Choirs". We find that majority of the central Choir galaxies have average H i content: they have a normal gas-mass fraction with respect to isolated galaxies of the same stellar mass. In contrast, we find more satellite galaxies with a lower gas-mass fraction than isolated galaxies of the same stellar mass. A likely reason for the lower gas content in these galaxies is tidal stripping. Both the specific star formation rate and the star formation efficiency of the central group galaxies are similar to galaxies in isolation. The Choir satellite galaxies have similar specific star formation rate as galaxies in isolation, therefore satellites that exhibit a higher star formation efficiency simply owe it to their lower gas-mass fractions. We find that the most H i massive galaxies have the largest H i discs and fall neatly onto the H i size-mass relation, while outliers are galaxies that are experiencing interactions. We find that high specific angular momentum could be a reason for galaxies to retain the large fraction of H i gas in their discs. This shows that for the Choir groups with no evidence of interactions, as well as those with traces of minor mergers, the internal galaxy properties dominate over the effects of residing in a group. The probed galaxy properties strengthen evidence that the Choir groups represent the early stages of group assembly.

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Section: Discussionmentioning

confidence: 99%

The neutral hydrogen properties of galaxies in gas-rich groups

Džudžar

Kilborn

Meurer

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…The less massive galaxies have smaller gravitational potentials and no evidence of cold gas accretion from the large-scale structure is observed. Wang et al (2015) show H i-rich galaxies are surrounded by a H i-rich environment where the gas is situated in clumps, hosted by small satellite galaxies or density peaks in the diffuse H i intergalactic medium. These observations also support the CWD model and are best explained by cold mode accretion.…”

Section: Discussionmentioning

confidence: 99%

Evidence for Hi replenishment in massive galaxies through gas accretion from the cosmic web

Kleiner

Pimbblet

Jones

et al. 2016

Mon. Not. R. Astron. Soc.

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We examine the H i-to-stellar mass ratio (H i fraction) for galaxies near filament backbones within the nearby Universe (d < 181 Mpc). This work uses the 6 degree Field Galaxy Survey and the Discrete Persistent Structures Extractor to define the filamentary structure of the local cosmic web. H i spectral stacking of H i Parkes all sky survey observations yields the H i fraction for filament galaxies and a field control sample. The H i fraction is measured for different stellar masses and fifth nearest neighbour projected densities (Σ 5 ) to disentangle what influences cold gas in galaxies. For galaxies with stellar masses log(M ) < 11 M in projected densities 0 ≤ Σ 5 < 3 galaxies Mpc −2 , all H i fractions of galaxies near filaments are statistically indistinguishable from the control sample. Galaxies with stellar masses log(M ) ≥ 11 M have a systematically higher H i fraction near filaments than the control sample. The greatest difference is 0.75 dex, which is 5.5σ difference at mean projected densities of 1.45 galaxies Mpc −2 . We suggest that this is evidence for massive galaxies accreting cold gas from the intrafilament medium that can replenish some H i gas. This supports cold mode accretion where filament galaxies with a large gravitational potential can draw gas from the large-scale structure.

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“…Recent studies have shown that the quenching (i.e., the cessation of star forming activities in galaxies) properties of central galaxies, such as star formation rate (SFR), morphology, neutral hydrogen content, and broad-band colour, are correlated with those of their neighbouring galaxies (Weinmann et al 2006;Yang et al 2006;Ann et al 2008;Kauffmann et al 2010;Prescott et al 2011;Kauffmann et al 2013;Knobel et al 2015;Hartley et al 2015;Wang et al 2015;Kawinwanichakij et al 2016;Berti et al 2017). This socalled "galactic conformity" phenomenon exists over two distinct distance scales between the central galaxy of a primary dark matter halo and its surrounding galaxies, including the true satellite galaxies within the same halo (<0.5 h −1 Mpc; E-mail: zu.4@osu.edu first detected by Weinmann et al 2006) 1 , and galaxies in halos that are a few virial radii away from the primary (∼3 h −1 Mpc) -effects we refer to as "1-halo" and "2-halo" conformities, respectively.…”

Section: Introductionmentioning

confidence: 99%

Mapping stellar content to dark matter haloes – III. Environmental dependence and conformity of galaxy colours

Mandelbaum

2018

Monthly Notices of the Royal Astronomical Society

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Recent studies suggest that the quenching properties of galaxies are correlated over several mega-parsecs. The large-scale "galactic conformity" phenomenon around central galaxies has been regarded as a potential signature of "galaxy assembly bias" or "preheating", both of which interpret conformity as a result of direct environmental effects acting on galaxy formation. Building on the iHOD halo quenching framework developed in Zu & Mandelbaum (2015, we discover that our fiducial halo mass quenching model, without any galaxy assembly bias, can successfully explain the overall environmental dependence and the conformity of galaxy colours in SDSS, as measured by the mark correlation functions of galaxy colours and the red galaxy fractions around isolated primaries, respectively. Our fiducial iHOD halo quenching mock also correctly predicts the differences in the spatial clustering and galaxy-galaxy lensing signals between the more vs. less red galaxy subsamples, split by the red-sequence ridge-line at fixed stellar mass. Meanwhile, models that tie galaxy colours fully or partially to halo assembly bias have difficulties in matching all these observables simultaneously. Therefore, we demonstrate that the observed environmental dependence of galaxy colours can be naturally explained by the combination of 1) halo quenching and 2) the variation of halo mass function with environment -an indirect environmental effect mediated by two separate physical processes.

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An H i view of galaxy conformity: H i-rich environment around H i-excess galaxies

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Cited by 21 publications

References 61 publications

The neutral hydrogen properties of galaxies in gas-rich groups

The neutral hydrogen properties of galaxies in gas-rich groups

Evidence for Hi replenishment in massive galaxies through gas accretion from the cosmic web

Mapping stellar content to dark matter haloes – III. Environmental dependence and conformity of galaxy colours

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