The Westerbork Coma Survey

Molnár, D. Cs.; Serra, P.; Hulst, Thijs van der; Jarrett, T. H.; Boselli, A.; Cortese, Luca; Healy, J.; Blok, W. J. G. de; Cappellari, Michele; Hess, Kelley M.; Józsa, G. I. G.; McDermid, Richard M.; Oosterloo, Thomas; Verheijen, Marc

doi:10.1051/0004-6361/202142614

Cited by 18 publications

(16 citation statements)

References 130 publications

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“…Most U types are distributed in the first and second quadrants, with only a few in the fourth quadrant. The absence of galaxies in the fourth quadrant is similar to the RPS galaxies explored by Molnar et al (2022). We also find that more strongly warped U types prefer the first quadrant.…”

Section: Stellar Mass Star Formation Rate and Gas Mass Fractionsupporting

confidence: 77%

“…Similarly, Mun et al (2021) showed that the HI deficiency of RPS galaxies in the Virgo cluster strongly depends on the evolutionary phase of infall. Molnar et al (2022) investigated RPS galaxies in the Coma cluster and showed using a simple model that the distribution of Δf HI and ΔsSFR can trace the evolutionary phase of RPS. The residual of f HI , Δf HI , is defined by the difference in f HI between the warp sample and the mean f HI of its corresponding control sample.…”

Section: Stellar Mass Star Formation Rate and Gas Mass Fractionmentioning

confidence: 99%

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Warped Disk Galaxies. I. Linking U-type Warps in Groups/Clusters to Jellyfish Galaxies

Yoon

Moon

et al. 2022

ApJ

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Warped disk galaxies are classified into two morphologies: S and U types. Conventional theories routinely attribute both types to galactic tidal interaction and/or gas accretion, but reproducing U types in simulations is extremely challenging. Here we investigate whether both types are governed by the same mechanisms using the most extensive sample of ∼8000 nearby (0.02 < z < 0.06) massive (M */M ⊙ > 109) edge-on disks from the Sloan Digital Sky Survey. We find that U types show on average bluer optical colors and a higher specific star formation rate (sSFR) than S types, with more strongly warped U types having a higher sSFR. We also find that while the S-type warp properties correlate with the tidal force by the nearest neighbor regardless of the environment, there is no such correlation for U types in groups/clusters, suggesting a nontidal environmental could be at play for U types, such as ram pressure stripping (RPS). Indeed, U types are more common in groups/clusters than in fields and they have stellar mass, gas fraction, sSFR enhancement, and phase-space distribution closely analogous to RPS-induced jellyfish galaxies in clusters. We furthermore show that the stellar disks of most RPS galaxies in the IllustrisTNG simulation are warped in a U shape and bent in the opposite direction of stripped gas tails, satisfying theoretical expectations for stellar warps embedded in jellyfishes. We therefore suggest that despite the majority of U types that live in fields being still less explained, RPS can be an alternative origin for those in groups/clusters.

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Section: Stellar Mass Star Formation Rate and Gas Mass Fractionsupporting

confidence: 77%

Section: Stellar Mass Star Formation Rate and Gas Mass Fractionmentioning

confidence: 99%

Warped Disk Galaxies. I. Linking U-type Warps in Groups/Clusters to Jellyfish Galaxies

Yoon

Moon

et al. 2022

ApJ

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“…6). As a matter of fact, the central regions of A85 could be an extreme case even compared with Coma, where a number of gas deficient spirals are still detected within 1 Mpc, with similar Hi mass limit detection than the present work (Bravo-Alfaro et al 2000;Healy et al 2021;Molnár et al 2022). In A85 the only Hi projected close to the center is the high-speed infalling jellyfish JO201, which shows signs of strong ram pressure stripping (Ramatsoku et al 2020;Luber et al 2022).…”

Section: Global Properties Of the Studied Clusterssupporting

confidence: 66%

“…Several studies have been devoted to the nearest clusters such as Virgo, Hydra, A 1367 and Coma (e.g. Giovanelli & Haynes 1985;Cayatte et al 1990;Bravo-Alfaro et al 2000;Solanes et al 2001;Chung et al 2009;Scott et al 2010Scott et al , 2018Boselli et al 2021;Wang et al 2021;Molnár et al 2022). The large coverage and high sensitive Hi-surveys carried out with single dish telescopes, such as HIPASS and ALFALFA (Giovanelli et al 2005;Haynes et al 2018), provided statistical information on the Hi content of large samples of spirals in different environments.…”

Section: Introductionmentioning

confidence: 99%

Environmental cluster effects and galaxy evolution: The H i properties of the Abell clusters A85/A496/A2670

López-Gutiérrez

Bravo-Alfaro

Gorkom

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We study the impact of local environment on the transformation of spiral galaxies in three nearby (z < 0.08) Abell clusters: A85/A496/A2670. These systems were observed in H i with the Very Large Array, covering a volume extending beyond the virial radius and detecting 10, 58, 38 galaxies, respectively. High fractions (0.40–0.86) of bright spirals [log(M*/M⊙) = 9 − 10] are not detected in H i. We provide further evidence of environmental effects consisting in significant fractions (0.10–0.33) of abnormal objects and a number of red (passive) spirals, suggesting an ongoing process of quenching. Ram-pressure profiles, and the sample of the brightest spirals used as test particles for environmental effects, indicate that ram-pressure plays an important role in stripping and transforming late-types. Phase-space diagrams and our search for substructures helped to trace the dynamical stage of the three systems. This was used to compare the global cluster effects vs. pre-processing, finding that the former is the dominating mechanism in the studied clusters. By contrasting the global distribution of H i normal vs. H i disturbed spirals in the combined three clusters, we confirm the expected correlation of disturbed objects located, on average, at shorter projected radii. However, individual clusters do not necessarily follow this trend and we show that A496 and A2670 present an atypical behavior. In general we provide conclusive evidence about the dependence of the transformation of infalling spirals on the ensemble of cluster properties like mass, ICM density, dynamical stage and surrounding large-scale structure.

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“…To better understand the formation and evolution of galaxies in various global and local environments, a next step is to analyse the morphological properties of galaxies in more detail than in the present study. For this purpose, one could use data on galaxies in our local cosmic neighbourhood, such as those provided by Quilley & de Lapparent (2022), and future multi-wavelength surveys with detailed information on galaxies, such as the J-PAS survey, or the HI Westerbork Coma Survey (Molnár et al 2022), which showed that cluster galaxies are HI deficient in comparison with galaxies found around the cluster. Were galaxies born similar, turning into ellipticals or spirals during evolution in hugely different environments, or are the seeds of primeval galaxies already different?…”

Section: Discussionmentioning

confidence: 99%

Death at watersheds: Galaxy quenching in low-density environments

Einasto

Kipper

Tenjes

et al. 2022

A&A

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Context. The evolution of galaxies is influenced by their local and global environment in the cosmic web. Galaxies with very old stellar populations (VO galaxies with D n (4000) index ≥ 1.75) mostly lie in the centres of galaxy clusters, where they evolve under the influence of processes characteristic of high-density cluster environments. However, VO galaxies have also been found in poor groups in global low-density environments between superclusters, which we call watershed regions. Aims. Our aim is to analyse the properties of galaxies in various cosmic environments with a focus on VO galaxies in the watershed regions to understand their evolution, and the origin of the large-scale morphology-density relation. Methods. We employ the Sloan Digital Sky Survey DR10 MAIN spectroscopic galaxy sample in the redshift range 0.009 ≤ z ≤ 0.200 to calculate the luminosity-density field of galaxies, to determine groups and filaments in the galaxy distribution, and to obtain data on galaxy properties. The luminosity-density field with smoothing length 8 h −1 Mpc, D8, characterises the global environment of galaxies. We analyse the group and galaxy contents of regions with various D8 thresholds. We divide groups into low-and highluminosity groups based on the highest luminosity of groups in the watershed region, L gr ≤ 15 × 10 12 h −2 L ⊙ . We compare the stellar masses, the concentration index, and the stellar velocity dispersions of quenched and star-forming galaxies among single galaxies, satellite galaxies, and the brightest group galaxies (BGGs) in various environments. Results. We show that the global density is most strongly related to the richness of galaxy groups. Its influence on the overall star formation quenching in galaxies is less strong. Correlations between the morphological properties of galaxies and the global density field are the weakest. The watershed regions with D8 < 1 are populated mostly by single galaxies, constituting 70 % of all galaxies there, and by low-luminosity groups. Still, approximately one-third of all galaxies in the watershed regions are VO galaxies. They have lower stellar masses, smaller stellar velocity dispersions, and stellar populations that are up to 2 Gyr younger than those of VO galaxies in other global environments. In higher density global environments (D8 > 1), the morphological properties of galaxies are very similar. Differences in galaxy properties are the largest between satellites and BGGs in groups. Conclusions. Our results suggest that galaxy evolution is determined by the birthplace of galaxies in the cosmic web, and mainly by internal processes which lead to the present-day properties of galaxies. This may explain the similarity of (VO) galaxies in extremely different environments.

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The Westerbork Coma Survey

Cited by 18 publications

References 130 publications

Warped Disk Galaxies. I. Linking U-type Warps in Groups/Clusters to Jellyfish Galaxies

Warped Disk Galaxies. I. Linking U-type Warps in Groups/Clusters to Jellyfish Galaxies

Environmental cluster effects and galaxy evolution: The H i properties of the Abell clusters A85/A496/A2670

Death at watersheds: Galaxy quenching in low-density environments

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