Transforming gas-rich low-mass disky galaxies into ultra-diffuse galaxies by ram pressure

Grishin, Kirill; Chilingarian, Igor; Afanasiev, Anton V.; Fabricant, Daniel G.; Katkov, Ivan; Moran, Sean M.; Yagi, Masafumi

doi:10.1038/s41550-021-01470-5

Cited by 24 publications

(19 citation statements)

References 85 publications

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“…Our result that a majority of galaxies with tails are moving toward the cluster center, i.e., the radio trails point away from the cluster center, is fully consistent with the findings of Smith et al (2010), Roberts & Parker (2020) and Roberts et al (2021). We note that the tail orientations of the small post-starburst galaxy sample in Grishin et al (2021) are less clear and that their selection criteria may favor objects with more tangential orbits. Roberts & Parker (2020) noted that the motion of the majority of stripping galaxies was pointing away from the cluster center, i.e., these galaxies are moving toward the cluster center.…”

Section: Orientation Of Trailing Featuressupporting

confidence: 88%

“…Two sources, GMP 4629 and GMP 3071, from these seven sources, were marginally detected at 1.4 GHz (Chen et al 2020), and assuming a spectral index α = −0.7 for these two sources, the non-detections are consistent in our 250-500 MHz and 550-850 MHz band images within the uncertainties. Grishin et al (2021) observed nine low-mass post-starburst galaxies in the Coma cluster using the multiobject Binospec 3 and 4, is labeled in the lower-left and lower-right corners of each image. The optical host positions are marked by a "+" sign.…”

Section: Radio Morphologies Of Rps Galaxiesmentioning

confidence: 99%

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High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

Lal

Lyskova

Zhang

et al. 2022

ApJ

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We present high-resolution, high-sensitivity upgraded Giant Metrewave Radio Telescope observations of the Coma cluster (A1656) at 250–500 MHz and 550–850 MHz. At 250–500 MHz, 135 sources have extensions >0.′45 (with peak-to-local-noise ratio >4). Of these, 24 sources are associated with Coma-member galaxies. In addition, we supplement this sample of 24 galaxies with 20 ram pressure stripped (RPS) galaxies from (Chen et al. 2020, eight are included in the original extended radio source sample) and an additional five are detected and extended. We present radio morphologies, radio spectra, spectral index maps, and equipartition properties for these two samples. In general, we find the equipartition properties lie within a narrow range (e.g., P min = 1–3 × 10− 13 dynes cm−2). Only NGC 4874, one of the two brightest central Coma cluster galaxies, has a central energy density and pressure about five times higher and a radio source age about 50% lower than that of the other Coma galaxies. We find a diffuse tail of radio emission trailing the dominant galaxy of the merging NGC 4839 group that coincides with the slingshot tail seen in X-rays. The southwestern radio relic, B1253+275, has a large extent ≈32′ × 10′ (≃1.08 × 0.34 Mpc2). For NGC 4789, whose long radio tails merge into the relic and may be a source of its relativistic seed electrons, we find a transverse radio spectral gradient, a steepening from southwest to northeast across the width of the radio source. Finally, radio morphologies of the extended and RPS samples suggest that these galaxies are on their first infall into Coma on (predominantly) radial orbits.

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Section: Orientation Of Trailing Featuressupporting

confidence: 88%

Section: Radio Morphologies Of Rps Galaxiesmentioning

confidence: 99%

High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

Lal

Lyskova

Zhang

et al. 2022

ApJ

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“…This could be either the properties of the orbits on which the galaxy is located, the properties of the hosting cluster (its mass, relaxation state, conditions of the ICM) or galaxy mass. In a very massive galaxy, the anchoring force could be sufficiently high to contrast the strength of the ram pressure and prevent the formation of galaxy tails (but see Poggianti et al 2019a), while low mass galaxies more easily develop tails (e.g., Grishin et al 2021). All these considerations are similar to those faced by Gullieuszik et al (2020) to explain the development of tails in SC.…”

Section: Discussionmentioning

confidence: 73%

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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“…In recent years, with advancements in technology, it has become possible to obtain deeper observations, allowing astronomers to study this very significant population with a new perspective (e.g., owing to instruments such as CFHT Megacam, Subaru Suprime-Cam, the Dragonfly Telescope Array, and VLT-MUSE). Ultra-diffuse galaxies (UDGs), a subclass of LSBs, have attracted a lot of attention in the past few years (van Dokkum et al 2015;Koda et al 2015;Leisman et al 2017;Grishin et al 2021). While UDGs are usually broadly defined as galaxies with a lower surface brightness and a larger extent than other galaxies or dwarfs, various working definitions have been used (depending especially on available data).…”

Section: Introductionmentioning

confidence: 99%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Junais

Boissier

Boselli

et al. 2022

A&A

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Context. Low-surface-brightness galaxies (LSBs) contribute to a significant fraction of all the galaxies in the Universe. Ultra-diffuse galaxies (UDGs) form a subclass of LSBs that has attracted a lot of attention in recent years (although its definition may vary between studies). Although UDGs are found in large numbers in galaxy clusters, groups, and in the field, their formation and evolution are still very much debated. Aims. Using a comprehensive set of multiwavelength data from the NGVS (optical), VESTIGE (Hα narrowband), and GUViCS (UV) surveys, we studied a sample of 64 diffuse galaxies and UDGs in the Virgo cluster to investigate their formation history. Methods. We analyzed the photometric colors and surface-brightness profiles of these galaxies and then compared them to models of galaxy evolution, including ram-pressure stripping (RPS) events to infer any possible strong interactions with the hot cluster gas in the past. Results. While our sample consists mainly of red LSBs, which is typical in cluster environments, we found evidence of a color variation with the cluster-centric distance. Blue, H i-bearing, star-forming diffuse galaxies are found at larger distances from the cluster center than the rest of the sample. The comparison of our models with multifrequency observations suggests that most of the galaxies of the sample might have undergone a strong RPS event in their lifetime, on average 1.6 Gyr ago (with a large dispersion, and RPS still ongoing for some of them). This process resulted in the transformation of initially gas-rich diffuse blue galaxies into gas-poor and red ones that form the dominant population now, the more extreme UDGs having undergone the process in a more distant past on average. Conclusions. The RPS in dense environments could be one of the major mechanisms for the formation of the large number of quiescent UDGs we observe in galaxy clusters.

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Transforming gas-rich low-mass disky galaxies into ultra-diffuse galaxies by ram pressure

Cited by 24 publications

References 85 publications

High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

High-resolution, High-sensitivity, Low-frequency uGMRT View of Coma Cluster of Galaxies

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

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

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