2018
DOI: 10.1093/mnras/sty1616
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Origins of ultradiffuse galaxies in the Coma cluster – I. Constraints from velocity phase space

Abstract: We use Keck/DEIMOS spectroscopy to confirm the cluster membership of 16 ultra-diffuse galaxies (UDGs) in the Coma cluster, bringing the total number of spectroscopically confirmed UDGs to 24. We also identify a new cluster background UDG. In this pilot study of Coma UDGs in velocity phase-space, we find evidence that most present-day Coma UDGs have a recent infall epoch while a few may be ancient infalls. These recent infall UDGs have higher absolute relative line-of-sight velocities, bluer optical colors, and… Show more

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Cited by 62 publications
(68 citation statements)
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“…Local dwarfs are relevant as UDGs may have formed their GCs in low density environments before falling into clusters, e.g. Alabi et al (2018). If UDGs are simply puffed-up dwarfs, then it is relevant to compare them to a sample of Coma early-type dwarf galaxies.…”
Section: Dwarf Galaxy Comparison Samplesmentioning
confidence: 99%
“…Local dwarfs are relevant as UDGs may have formed their GCs in low density environments before falling into clusters, e.g. Alabi et al (2018). If UDGs are simply puffed-up dwarfs, then it is relevant to compare them to a sample of Coma early-type dwarf galaxies.…”
Section: Dwarf Galaxy Comparison Samplesmentioning
confidence: 99%
“…Three other low surface brightness galaxies in the vicinity of Dragonfly 44 (Dragonfly 42, DFX1, and DFX2) have redshifts, all from the DEIMOS multi-slit spectroscopy described in van Dokkum et al (2016van Dokkum et al ( , 2017a, and Alabi et al (2018). Of this sample of four faint galaxies, three (Dragonfly 42, Dragonfly 44, and DFX2) are within ≈ 100 km s −1 of each other (see van Dokkum et al 2017a;Alabi et al 2018). The velocity dispersion of the Coma cluster is ∼ 1000 km s −1 (Colless & Dunn 1996), and the probability that three out of four randomly selected galaxies have a velocity range ∆v < 100 km s −1 is 3 × 10 −3 .…”
Section: Robustness Of the Radial Dispersion Profilementioning
confidence: 99%
“…UDGs in clusters are typically on the red sequence (Koda et al 2015;van der Burg et al 2016;RS et al 2019) and show little evidence for tidal interaction even close to the cluster centres (Mowla et al 2017), suggesting relatively high mass-to-light ratios. There is tentative evidence that UDGs tend to be bluer towards the outskirts of galaxy groups (Román & Trujillo 2017b;Alabi et al 2018;Zaritsky et al 2019) (and more generally in lower-density environments cf. Greco et al 2018a,b), suggesting that interactions with the environment during in-fall can diminish star formation in the UDGs.…”
Section: Introductionmentioning
confidence: 99%