Ram pressure stripping of HI-rich galaxies infalling into massive clusters

Wang, Jing; Xu, Weiwei; Lee, Bumhyun; Du, Min; Overzier, Roderik; Shao, Li

doi:10.48550/arxiv.2009.08159

Cited by 5 publications

(7 citation statements)

References 124 publications

(260 reference statements)

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“…Comparing the VIR galaxies with the RIF galaxies without the W-cloud galaxies, we find that starformation activity and cold-gas reservoirs are significantly smaller in the former than the latter. The atomic gas in the VIR and RPS galaxies has been known to be deficient compared to the RIF galaxies in previous studies (Jaffé et al 2015;Wang et al 2020), but this is the first time one has found a similar tendency in molecular gas in the Virgo galaxies on the PSD. The tendency is also confirmed by the positive correlations between (|∆v gal |/σ Virgo )×(R proj /R 200 ) with SFR, sSFR, and gas fractions as seen in the z ∼ 2.5 cluster (Wang et al 2018).…”

Section: Ram-pressure or Tidal Strippingmentioning

confidence: 56%

“…The tendency is also confirmed by the positive correlations between (|∆v gal |/σ Virgo )×(R proj /R 200 ) with SFR, sSFR, and gas fractions as seen in the z ∼ 2.5 cluster (Wang et al 2018). These results suggest the importance of not only the long-period quenching processes but also the rampressure stripping for star-formation quenching since the galaxies that were affected by the ram pressure also exist in the VIR region (Jaffé et al 2015;Wang et al 2020).…”

Section: Ram-pressure or Tidal Strippingmentioning

confidence: 61%

“…It is also shown that the poststarburst galaxies are preferentially found at small clustocentric radii with high clustocentric velocities, suggesting that the ram-pressure stripping is the most plausible candidate for the physical mechanism to quench their star formation (Muzzin et al 2014;Paccagnella et al 2017). At the same time, ram pressure is claimed to enhance star formation activity in galaxies (Fujita & Nagashima 1999;Bekki & Couch 2003;Kronberger et al 2008;Bekki 2014;Ruggiero & Lima Neto 2017) and there are supportive observations (e.g., Vulcani et al 2018a;Roberts & Parker 2020;Wang et al 2020). Additionally, ram pressure is found to induces a gas funneling to the central supermassive black hole of galaxies (Poggianti et al 2017).…”

Section: Ram-pressure or Tidal Strippingmentioning

confidence: 85%

“…The cold gas properties of galaxies on the PSD have been also investigated. H i gas observations toward cluster galaxies showed that galaxies that are expected to be affected by ram pressure on the PSD tend to have lower levels of atomic gas than field galaxies (Jaffé et al 2015;Wang et al 2020). investigated a relationship between H i morphology, as a measure of the ram-pressure stripping, and the location on the PSD of Virgo galaxies and showed that the galaxies with severely stripped H i disks are found deep inside the cluster.…”

Section: Introductionmentioning

confidence: 99%

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A phase-space view of cold-gas properties of Virgo-cluster galaxies: multiple quenching processes at work?

Morokuma-Matsui¹,

Kodama²,

Morokuma³

et al. 2021

Preprint

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We investigate the cold-gas properties of massive Virgo galaxies (> 10 9 M ) at < 3R 200 (R 200 is the radius where the mean interior density is 200 times the critical density) on the projected phasespace diagram (PSD) with the largest archival dataset to date to understand the environmental effect on galaxy evolution in the Virgo cluster. We find: lower H i and H 2 mass fractions and higher starformation efficiencies (SFEs) from H i and H 2 in the Virgo galaxies than the field galaxies for matched stellar masses; the Virgo galaxies generally follow the field relationships between the offset from the main sequence of the star-forming galaxies [∆(MS)] with gas fractions and SFEs but slightly offset to lower gas fractions or higher SFEs than field galaxies at ∆(MS) < 0; lower gas fractions in galaxies with smaller clustocentric distance and velocity; lower gas fractions in the galaxies in the W cloud, a substructure of the Virgo cluster. Our results suggest the cold-gas properties of some Virgo galaxies are affected by their environment at least at 3R 200 maybe via strangulation and/or pre-processes and H i and H 2 in some galaxies are removed by ram pressure at < 1.5R 200 . Our data cannot rule the possibility of the other processes such as strangulation and galaxy harassment accounting for the gas reduction in some galaxies at < 1.5R 200 . Future dedicated observations of a mass-limited complete sample are required for definitive conclusions.

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Section: Ram-pressure or Tidal Strippingmentioning

confidence: 56%

Section: Ram-pressure or Tidal Strippingmentioning

confidence: 61%

Section: Ram-pressure or Tidal Strippingmentioning

confidence: 85%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A phase-space view of cold-gas properties of Virgo-cluster galaxies: multiple quenching processes at work?

Morokuma-Matsui¹,

Kodama²,

Morokuma³

et al. 2021

Preprint

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“…Well known examples of these phenomena are the morphology-density relation (Oemler 1974;Dressler 1980) and higher fraction of quenched galaxies within massive clusters (Kauffmann et al 2004;Peng et al 2010;Davies et al 2019). Environmental processes such as rampressure stripping (Gunn & Gott 1972) and tidal stripping (Binney & Tremaine 1987) can strip the gas out of galaxies, affecting their gas reservoirs (Wang et al 2020a), star formation (Donnari et al 2020a,b), stellar properties (Webb et al 2020), morphology (Joshi et al 2020), and so on.…”

Section: Introductionmentioning

confidence: 99%

Galaxy formation with L-GALAXIES: Modelling the environmental dependency of galaxy evolution and comparing with observations

Ayromlou,

Kauffmann,

Yates

et al. 2020

Preprint

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We present a variation of the recently updated Munich semi-analytical galaxy formation model, L-G , with a new gas stripping method. Extending earlier work, we directly measure the local environmental properties of galaxies to formulate a more accurate treatment of rampressure stripping for all galaxies. We fully re-calibrate the modified L-G model using a Markov Chain Monte Carlo (MCMC) method with the stellar mass function and quenched fraction of galaxies at 0 ≤ 𝑧 ≤ 2 as constraints. Due to this re-calibration, global galaxy population relations, including the stellar mass function, quenched fractions versus galaxy mass and HI mass function are all largely unchanged and remain consistent with observations. By comparing to data on galaxy properties in different environments from the SDSS and HSC surveys, we demonstrate that our modified model improves the agreement with the quenched fractions and star formation rates of galaxies as a function of environment, stellar mass, and redshift. Overall, in the vicinity of haloes with total mass 10 12 to 10 15 M at 𝑧 = 0, our new model produces higher quenched fractions and stronger environmental dependencies, better recovering observed trends with halocentric distance up to several virial radii. By analysing the actual amount of gas stripped from galaxies in our model, we show that those in the vicinity of massive haloes lose a large fraction of their hot halo gas before they become satellites. We demonstrate that this affects galaxy quenching both within and beyond the halo boundary. This is likely to influence the correlations between galaxies up to tens of megaparsecs.

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Ram pressure candidates in UNIONS

Roberts

Parker

Gwyn

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a search for disturbed, candidate ram pressure stripping galaxies across more than 50 spectroscopically selected SDSS groups and clusters. 48 ram pressure candidates are visually identified in these systems using high-quality UNIONS imaging from the Canada-France-Hawaii Telescope, covering ${\sim }6200\, \mathrm{deg^2}$ and ${\sim }2800\, \mathrm{deg^2}$ in the u- and r-bands, respectively. Ram pressure candidates are found in groups and clusters spanning a wide range in halo mass and include ∼30 ram pressure candidates in the group regime (Mh < 1014). The observed frequency of ram pressure candidates shows substantial scatter with group/cluster mass, but on average is larger in clusters ($M_h \ge 10^{14}\, \mathrm{M_\odot }$) than groups ($M_h \lt 10^{14}\, \mathrm{M_\odot }$) by a factor of ∼2. We find that ram pressure candidates are most commonly low-mass galaxies and have enhanced star formation rates relative to star-forming field galaxies. The enhancement in star formation is largely independent of galaxy mass and strongest for galaxies in clusters. As a result of the large survey footprint and excellent image quality from UNIONS, we are able to identify disturbed galaxies, potentially affected by ram pressure stripping, across a wide range of host environment.

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Ram pressure stripping of HI-rich galaxies infalling into massive clusters

Cited by 5 publications

References 124 publications

A phase-space view of cold-gas properties of Virgo-cluster galaxies: multiple quenching processes at work?

A phase-space view of cold-gas properties of Virgo-cluster galaxies: multiple quenching processes at work?

Galaxy formation with L-GALAXIES: Modelling the environmental dependency of galaxy evolution and comparing with observations

Ram pressure candidates in UNIONS

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