Reviewing the frequency and central depletion of ultra-diffuse galaxies in galaxy clusters from the KIWICS survey

Piña, Pavel E. Mancera; Peletier, Reynier F.; Aguerri, J. A. L.; Venhola, Aku; Trager, S. C.; Choque-Challapa, Nelvy

doi:10.1093/mnras/sty2574

Cited by 46 publications

(33 citation statements)

References 43 publications

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“…This behaviour has been described in several nearby clusters (e.g. van der Burg et al 2016;Mancera Piña et al 2018) and is thought to be caused by the tidal disruption of UDGs near the centres of galaxy clusters. However, using simulations, Sales et al (2019) find that the surface density of UDGs rises continually towards the centre of a Virgo-like cluster.…”

Section: Resultsmentioning

confidence: 65%

The Distribution of Ultra-diffuse and Ultra-compact Galaxies in the Frontier Fields

Janssens

Abraham

Brodie

et al. 2019

ApJ

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Large low surface brightness galaxies have recently been found to be abundant in nearby galaxy clusters. In this paper, we investigate these ultra-diffuse galaxies (UDGs) in the six Hubble Frontier Fields galaxy clusters: Abell 2744, MACSJ0416.1−2403, MACSJ0717.5+3745, MACSJ1149.5+2223, Abell S1063 and Abell 370. These are the most massive (1-3 × 10 15 M ) and distant (0.308 < z < 0.545) systems in which this class of galaxy has yet been discovered. We estimate that the clusters host of the order of ∼200-1400 UDGs inside the virial radius (R 200 ), consistent with the UDG abundance halo-mass relation found in the local universe, and suggests that UDGs may be formed in clusters. Within each cluster, however, we find that UDGs are not evenly distributed. Instead their projected spatial distributions are lopsided, and they are deficient in the regions of highest mass density as traced by gravitational lensing. While the deficiency of UDGs in central regions is not surprising, the lopsidedness is puzzling. The UDGs, and their lopsided spatial distributions, may be associated with known substructures late in their infall into the clusters, meaning that we find evidence both for formation of UDGs in clusters and for UDGs falling into clusters. We also investigate the ultracompact dwarfs (UCDs) residing in the clusters, and find the spatial distributions of UDGs and UCDs appear anti-correlated. Around 15% of UDGs exhibit either compact nuclei or nearby point sources. Taken together, these observations provide additional evidence for a picture in which at least some UDGs are destroyed in dense cluster environments and leave behind a residue of UCDs.

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Section: Resultsmentioning

confidence: 65%

The Distribution of Ultra-diffuse and Ultra-compact Galaxies in the Frontier Fields

Janssens

Abraham

Brodie

et al. 2019

ApJ

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“…One outstanding question regarding UDGs is whether they are able to form more efficiently in dense environments like groups and clusters, or whether density plays a detrimental role in UDG formation/survival efficiency. van der Burg et al (2017) find that UDGs are relatively more common in higher-mass environments, but this is in tension with other studies (Román & Trujillo 2017b;Mancera Piña et al 2018) that came to the opposite conclusion.…”

Section: Introductionmentioning

confidence: 58%

“…This is a factor of six higher than the total number density of HI-bearing UDGs measured by Jones et al (2018), who measured a value of 1.5±0.6×10 −3 cMpc −3 . Using a different value than 10 15 M for the halo mass would not strongly modify the initial number density estimate since the slope of the relation between M halo and the number of UDGs hosted by the halo is approximately one (at least down to M halo ∼10 12 M , Román & Trujillo 2017b;van der Burg et al 2017;Mancera Piña et al 2018). However, by selecting a halo mass of 10 15 M , we are essentially comparing the field abundance with that in a 10 15 M cluster in our later analysis.…”

Section: Estimated Number Density Of Udgsmentioning

confidence: 99%

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Observational properties of ultra-diffuse galaxies in low-density environments: field UDGs are predominantly blue and star forming

Prole

Burg

Hilker

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Abstract While we have learnt much about ultradiffuse galaxies (UDGs) in groups and clusters, relatively little is known about them in less dense environments. More isolated UDGs are important for our understanding of UDG formation scenarios because they form via secular mechanisms, allowing us to determine the relative importance of environmentally driven formation in groups and clusters. We have used the public Kilo-Degree Survey together with the Hyper Suprime-Cam Subaru Strategic Program to constrain the abundance and properties of UDGs in the field, targeting sources with low surface brightness (24.0 ≤ $\bar{\mu }_{\mathrm{ e},r}$ ≤ 26.5) and large apparent sizes (3.0 arcsec ≤ $\bar{r}_{\mathrm{ e},r}$ ≤ 8.0 arcsec). Accounting for several sources of interlopers in our selection based on canonical scaling relations, and using an empirical UDG model based on measurements from the literature, we show that a scenario in which cluster-like red-sequence UDGs occupy a significant number of field galaxies is unlikely, with most field UDGs being significantly bluer and showing signs of localized star formation. An immediate conclusion is that UDGs are much more efficiently quenched in high-density environments. We estimate an upper limit on the total field abundance of UDGs of 8 ± 3 × 10−3 cMpc−3 within our selection range. We also compare the total field abundance of UDGs to a measurement of the abundance of H i-rich UDGs from the literature, suggesting that they occupy at least one-fifth of the overall UDG population. The mass formation efficiency of UDGs implied by this upper limit is similar to what is measured in groups and clusters.

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“…H i-rich UDGs represent ∼ 6% of all galaxies with M HI ∼ 10 8.8 M , with a cosmic abundance similar to cluster UDGs(Jones et al 2018;Mancera Piña et al 2018). …”

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confidence: 99%

Off the Baryonic Tully–Fisher Relation: A Population of Baryon-dominated Ultra-diffuse Galaxies

Piña

Fraternali

Adams

et al. 2019

ApJL

101

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We study the gas kinematics traced by the 21-cm emission of a sample of six H i-rich low surface brightness galaxies classified as ultra-diffuse galaxies (UDGs). Using the 3D kinematic modelling code 3D Barolo we derive robust circular velocities, revealing a startling feature: H i-rich UDGs are clear outliers from the baryonic Tully-Fisher relation, with circular velocities much lower than galaxies with similar baryonic mass. Notably, the baryon fraction of our UDG sample is consistent with the cosmological value: these UDGs are compatible with having no "missing baryons" within their virial radii. Moreover, the gravitational potential provided by the baryons is sufficient to account for the amplitude of the rotation curve out to the outermost measured point, contrary to other galaxies with similar circular velocities. We speculate that any formation scenario for these objects will require very inefficient feedback and a broad diversity in their inner dark matter content.

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Reviewing the frequency and central depletion of ultra-diffuse galaxies in galaxy clusters from the KIWICS survey

Cited by 46 publications

References 43 publications

The Distribution of Ultra-diffuse and Ultra-compact Galaxies in the Frontier Fields

The Distribution of Ultra-diffuse and Ultra-compact Galaxies in the Frontier Fields

Observational properties of ultra-diffuse galaxies in low-density environments: field UDGs are predominantly blue and star forming

Off the Baryonic Tully–Fisher Relation: A Population of Baryon-dominated Ultra-diffuse Galaxies

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