H i in Virgo’s “Red and Dead” Dwarf Ellipticals—A Tidal Tail and Central Star Formation

Hallenbeck, Gregory; Koopmann, Rebecca A.; Giovanelli, Riccardo; Haynes, Martha P.; Huang, Shan; Papastergis, Emmanouil

doi:10.3847/1538-3881/aa7c1d

Cited by 11 publications

(14 citation statements)

References 80 publications

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“…Conselice et al 2013; see Sanchez Almeida 2014 for a review). Observations that may indicate cold gas accretion include streams of HI gas surrounding M31 (Thilker et al 2004), HI in red early-type dwarf galaxies on the outskirts of the Virgo cluster (Hallenbeck et al 2012, but see Hallenbeck et al 2017 for follow-up observations that suggest the HI might not be recently accreted), and an HI envelope surrounding a small extended grouping of galaxies within a void (Beygu et al 2013). At the same time, cold gas is expected to be removed or cut off from galaxies through a variety of physical mechanisms that depend on largescale environment.…”

Section: Introductionmentioning

confidence: 99%

The Effect of Filaments and Tendrils on the H i Content of Galaxies

Odekon

Hallenbeck

Haynes

et al. 2018

ApJ

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We use the ALFALFA HI survey to examine whether the cold gas reservoirs of galaxies are inhibited or enhanced in large-scale filaments. Our sample includes 9947 late-type galaxies with HI detections, and 4236 late-type galaxies with well-determined HI detection limits that we incorporate using survival analysis statistics. We find that, even at fixed local density and stellar mass, and with group galaxies removed, the HI deficiency of galaxies in the stellar mass range 8.5

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Section: Introductionmentioning

confidence: 99%

The Effect of Filaments and Tendrils on the H i Content of Galaxies

Odekon

Hallenbeck

Haynes

et al. 2018

ApJ

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“…In low density environments, the HI gas in dEs could result from interactions with a companion or a gas accretion from the intergalactic medium (Grossi et al 2009). At most a dozen of HI-bearing dEs have been reported in the outskirts the Virgo cluster (Conselice et al 2003;di Serego Alighieri et al 2007;Hallenbeck et al 2012Hallenbeck et al , 2017, and a couple were observed in low density environments (Grossi et al 2009). With an HI line detection for 42 dEs, our sample is significantly larger than the ones previously reported.…”

Section: Dwarf Ellipticalsmentioning

confidence: 69%

“…Most of the optical studies of HI-bearing dwarf galaxies report blue colors caused by recent star formation activity (Grossi et al 2009;Cannon et al 2011;Huang et al 2012;Honey et al 2018). However, some studies have detected HI in red dEs located in the Virgo cluster (Conselice et al 2003;Hallenbeck et al 2017). In Figure 4, we show the color-magnitude relation for the Galactic extinction 5 corrected g−i and g−r colors of the MATLAS dwarfs present in the regions of the sky observed by either ALFALFA and ATLAS 3D HI survey.…”

Section: Dwarfs Colorsmentioning

confidence: 97%

“…Several assumptions have been put forward to explain the observation of HI-bearing dEs. In the cluster environment, the HIbearing dEs could be the evolution of an infalling star-forming galaxy into the cluster or could have recently accreted HI gas from an infalling HI cloud (Conselice et al 2003;Hallenbeck et al 2012Hallenbeck et al , 2017. In low density environments, the HI gas in dEs could result from interactions with a companion or a gas accretion from the intergalactic medium (Grossi et al 2009).…”

Section: Dwarf Ellipticalsmentioning

confidence: 99%

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HI observations of the MATLAS dwarf and ultra-diffuse galaxies

Poulain,

Marleau,

Habas

et al. 2021

Preprint

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The presence of HI gas in galaxies is inextricably linked to their morphology and evolution. This paper aims to understand the HI content of the already identified 2210 dwarfs located in the low-to-moderate density environments of the MATLAS deep imaging survey. We combine the HI observations from the ATLAS 3D survey, with the extragalactic HI sources from the ALFALFA survey, to extract the HI line width, velocity and mass of the MATLAS dwarfs. From the 1773 dwarfs in our sample with available HI observations, 8% ( 145) have an HI line detection. The majority of the dwarfs show irregular morphology, while 29% (42) are ellipticals, the largest sample of HI-bearing dwarf ellipticals (dEs) to date. Of the HI dwarf sample, 2% (3) are ultra-diffuse galaxies (UDGs), 12% have a transition-type morphology, 5% are tidal dwarf candidates, and 10% appear to be disrupted objects. In our optically selected sample, 9.5% of the dEs, 7% of the UDGs and 10% of the classical dwarfs are HI-bearing. The HI-bearing dwarfs have on average bluer colors than the dwarfs without detected HI. We find relations between the stellar and HI masses, gas fraction, color and absolute magnitude consistent with previous studies of dwarfs probing similar masses and environments. For 79% of the dwarfs identified as satellites of massive early-type galaxies, we find that the HI mass increases with the projected distance to the host. Using the HI line width, we estimate dynamical masses and find that 5% (7) of the dwarfs are dark matter deficient.

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“…The second caveat is that, even though it is an indicator of a disturbance, the magnitude of the velocity offset between the Hi and optical is much larger than might be expected. Local galaxies have been shown (Oosterloo & van Gorkom 2005;Chung et al 2007;Koopmann et al 2008;Leisman et al 2016;Hallenbeck et al 2017;Minchin et al 2019;Taylor et al 2020) to usually have only a small fraction of their Hi present in their tails, and retain the bulk of their gas in close proximity to their optical discs. Here, the velocity offsets (200-400 km s −1 ) are high enough that the gas may have been entirely displaced from the parent galaxy.…”

Section: Ram-pressure Strippingmentioning

confidence: 99%

Mapping the working of environmental effects in A963

Deshev

Haines

Hwang

et al. 2020

A&A

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Aims. We qualitatively assess and map the relative contribution of pre-processing and cluster related processes to the build-up of A963, a massive cluster at z = 0.2 showing an unusually high fraction of star forming galaxies in its interior. Methods. We use Voronoi binning of positions of cluster members on the plane of the sky in order to map the 2D variations of galaxy properties in the centre and infall region of A963. We map four galaxy parameters (fraction of star forming galaxies, specific star formation rate, H I deficiency and age of the stellar population) based on full SED fitting, 21 cm imaging and optical spectroscopy. Results. We find an extended region dominated by passive galaxies along a north–south axis crossing the cluster centre, possibly associated with known filaments of the large-scale structure. There are signs that the passive galaxies in this region were quenched long before their arrival in the vicinity of the cluster. Contrary to that, to the east and west of the cluster centre lie regions of recent accretion dominated by gas rich, actively star forming galaxies not associated with any substructure or filament. The few passive galaxies in this region appear to be recently quenched, and some gas rich galaxies show signs of ongoing ram-pressure stripping. We report the first tentative observations at 21 cm of ongoing ram-pressure stripping at z = 0.2, as well as observed inflow of low-entropy gas into the cluster along filaments of the large-scale structure. Conclusions. The observed galaxy content of A963 is a result of strongly anisotropic accretion of galaxies with different properties. Gas rich, star forming galaxies are being accreted from the east and west of the cluster and these galaxies are being quenched at r < R200, likely by ram-pressure stripping. The bulk of the accretion onto the cluster, containing multiple groups, happens along the north–south axis and brings mostly passive galaxies, likely quenched before entering A963.

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H i in Virgo’s “Red and Dead” Dwarf Ellipticals—A Tidal Tail and Central Star Formation

Cited by 11 publications

References 80 publications

The Effect of Filaments and Tendrils on the H i Content of Galaxies

The Effect of Filaments and Tendrils on the H i Content of Galaxies

HI observations of the MATLAS dwarf and ultra-diffuse galaxies

Mapping the working of environmental effects in A963

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