The ram pressure stripped radio tails of galaxies in the Coma cluster

Chen, H; Sun, Ming; Yagi, Masafumi; Bravo-Alfaro, H.; Brinks, E.; Kenney, Jeffrey D. P.; Combes, F.; Sivanandam, Suresh; Jáchym, Pavel; Fossati, M.; Gavazzi, G.; Boselli, A.; Nulsen, P. E. J.; Sarazin, Craig L.; Ge, Chong; Yoshida, Michitoshi; Röediger, E.

doi:10.1093/mnras/staa1868

Cited by 50 publications

(55 citation statements)

References 114 publications

(159 reference statements)

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“…Additionally, as a consequence of the passive evolution of their stellar populations, UDGs surface brightness have decreased with time (Román & Trujillo 2017;Román et al 2019;Tremmel et al 2020). This scenario is consistent with observations of cluster UDGs as gas-poor (Karunakaran et al 2020;Chen et al 2020) quiescent (Singh et al 2019), old, metal-poor, and alpha-enhanced (Kadowaki et al 2017;Gu et al 2018;Pandya et al 2018;Ruiz-Lara et al 2018;Ferré-Mateu et al 2018). This model stemmed from the idea that UDGs are massive objects with 𝐿 * -like haloes (van Dokkum et al 2015a).…”

Section: Introductionsupporting

confidence: 88%

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Saifollahi,

Zaritsky,

Trujillo

et al. 2022

Preprint

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We present an analysis of Hubble Space Telescope observations of globular clusters (GCs) in six ultra-diffuse galaxies (UDGs) in the Coma cluster, a sample that represents UDGs with large effective radii (𝑅 e ), and use the results to evaluate competing formation models. We eliminate two significant sources of systematic uncertainty in the determination of the number of GCs, 𝑁 GC by using sufficiently deep observations that (i) reach the turnover of the GC luminosity function and (ii) provide a sufficient number of GCs with which to measure the GC number radial distribution. We find that 𝑁 GC for these galaxies is on average ∼ 20, which implies an average total mass, 𝑀 total , ∼ 10 11 𝑀 when applying the relation between 𝑁 GC and 𝑀 total . This value of 𝑁 GC lies at the upper end of the range observed for dwarf galaxies of the same stellar mass and is roughly a factor of two larger than the mean. The GC luminosity function, radial profile and average colour are more consistent with those observed for dwarf galaxies than with those observed for the more massive (𝐿 * ) galaxies, while both the radial and azimuthal GC distributions closely follow those of the stars in the host galaxy. Finally, we discuss why our observations, specifically the GC number and GC distribution around these six UDGs, pose challenges for several of the currently favoured UDG formation models.

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Section: Introductionsupporting

confidence: 88%

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Saifollahi,

Zaritsky,

Trujillo

et al. 2022

Preprint

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“…For example, radio continuum observations are sensitive to synchrotron emission from cosmic rays accelerated by supernovae. For galaxies experiencing strong ram pressure, these cosmic rays can be stripped out of the galaxy and detected as ram pressure stripped tails in the radio continuum (e.g., Gavazzi et al 1987;Murphy et al 2009;Chen et al 2020), giving reliable identifications of jellyfish galaxies. Roberts et al (2021a) used the LOFAR Two-metre Sky Survey (LoTSS) to search for jellyfish galaxies at 120-168 MHz radio wavelengths.…”

Section: Discussionmentioning

confidence: 99%

The relevance of ram pressure stripping for the evolution of blue cluster galaxies as seen at optical wavelengths

Vulcani,

Poggianti,

Smith

et al. 2022

Preprint

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Ram pressure stripping is one of the most efficient mechanisms able to affect the gas reservoir in cluster galaxies and in the last decades many studies have characterized the properties of stripped galaxies. A definite census of the importance of this process in local clusters is though still missing.Here we characterize the fraction of galaxies showing signs of stripping at optical wavelengths, using the data of 66 clusters from the WINGS and OMEGAWINGS surveys. We focus on the infalling galaxy population and hence only consider blue, bright (B< 18.2) late-type spectroscopically confirmed cluster members within 2 virial radii. In addition to "traditional" stripping candidates (SC) -i.e. galaxies showing unilateral debris and tails -we also consider unwinding galaxies (UG) as potentially stripped galaxies. Recent work has indeed unveiled a connection between unwinding features and ram pressure stripping and even though only integral field studies can inform on how often these features are indeed due to ram pressure, it is important to include them in the global census. We performed a visual inspection of B-band images and here we release a catalog of 143 UG. SC and UG each represent ∼ 15 − 20% of the inspected sample. If we make the assumption that they both are undergoing ram pressure stripping, we can conclude that at any given time in the low-z universe about 35% of the infalling cluster population show signs of stripping in their morphology at optical wavelengths. These fractions depend on color, mass, morphology, and little on clustercentric distance. Making some rough assumptions on the duration of the tail visibility and on the time cluster galaxies can maintain blue colors, we infer that almost all bright blue late-type cluster galaxies undergo a stripping phase during their life, boosting the importance of ram pressure stripping in cluster galaxy evolution.

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“…Observations and simulations find galaxies in clusters to be experiencing various combinations of these processes (e.g. Gunn 1977;Moore et al 1996Moore et al , 1998Gnedin 2003a,b;Kenney et al 2004;Chung et al 2007;Vollmer et al 2009;Scott et al 2010;Abramson et al 2011;Bialas et al 2015;Chen et al 2020;Ramatsoku et al 2020). Of these processes, the proposed dominant driver for evolving galaxies' neutral atomic hydrogen (H ) morphology and quenching star formation is ram pressure stripping (e.g.…”

Section: Introductionmentioning

confidence: 99%

WALLABY pilot survey: first look at the Hydra I cluster and ram pressure stripping of ESO 501−G075

Reynolds

Westmeier

Elagali

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present results from neutral atomic hydrogen (H i) observations of Hydra I, the first cluster observed by the Widefield ASKAP L-band Legacy All-sky Blind Survey (WALLABY) on the Australian Square Kilometre Array Pathfinder. For the first time we show that WALLABY can reach its final survey sensitivity. Leveraging the sensitivity, spatial resolution and wide field of view of WALLABY, we identify a galaxy, ESO 501−G075, that lies near the virial radius of Hydra I and displays an H i tail. ESO 501−G075 shows a similar level of morphological asymmetry as another cluster member, which lies near the cluster centre and shows signs of experiencing ram pressure. We investigate possible environmental processes that could be responsible for producing the observed disturbance in the H i morphology of ESO 501−G075. We rule out tidal interactions, as ESO 501−G075 has no nearby neighbours within ∼0.34 Mpc. We use a simple model to determine that ram pressure can remove gas from the disc at radii r ≳ 25 kpc. We conclude that, as ESO 501−G075 has a typical H i mass compared to similar galaxies in the field and its morphology is compatible with a ram pressure scenario, ESO 501−G075 is likely recently infalling into the cluster and in the early stages of experiencing ram pressure.

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The ram pressure stripped radio tails of galaxies in the Coma cluster

Cited by 50 publications

References 114 publications

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

Implications for Galaxy Formation Models from Observations of Globular Clusters around Ultra-Diffuse Galaxies

The relevance of ram pressure stripping for the evolution of blue cluster galaxies as seen at optical wavelengths

WALLABY pilot survey: first look at the Hydra I cluster and ram pressure stripping of ESO 501−G075

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