A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

Yu, Rong; Guo, Qi; Gao, Liang; Liao, Shihong; Xie, Lizhi; Puzia, Thomas H.; Sun, Shuangpeng; Pan, Jun

doi:10.1093/mnras/stx1440

Cited by 124 publications

(169 citation statements)

References 66 publications

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“…This would mean that they also exist in lower-density environments, albeit with possibly more disk-like morphologies. Rong et al (2017) reached a similar conclusion based on semianalytic galaxy formation models. Di Cintio et al (2017) used the NIHAO simulation to study the formation of UDG-type galaxies, and they also suggested that internal processes, particularly outflow-driven feedback, may be responsible for their formation.…”

Section: Introductionsupporting

confidence: 66%

The abundance of ultra-diffuse galaxies from groups to clusters

Burg

Hoekstra

Muzzin

et al. 2017

A&A

116

106

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In recent years, many studies have reported substantial populations of large galaxies with low surface brightness in local galaxy clusters. Various theories that aim to explain the presence of such ultra-diffuse galaxies (UDGs) have since been proposed. A key question that will help to distinguish between models is whether UDGs have counterparts in host haloes with lower masses, and if so, what their abundance as a function of halo mass is. We here extend our previous study of UDGs in galaxy clusters to galaxy groups. We measure the abundance of UDGs in 325 spectroscopically selected groups from the Galaxy And Mass Assembly (GAMA) survey. We make use of the overlapping imaging from the ESO Kilo-Degree Survey (KiDS), from which we can identify galaxies with mean surface brightnesses within their effective radii down to ∼25.5 mag arcsec −2 in the r band. We are able to measure a significant overdensity of UDGs (with sizes r eff ≥ 1.5 kpc) in galaxy groups down to M 200 = 10 12 M , a regime where approximately only one in ten groups contains a UDG that we can detect. We combine measurements of the abundance of UDGs in haloes that cover three orders of magnitude in halo mass, finding that their numbers scale quite steeply with halo mass: N UDG (R < R 200 ) ∝ M . This shows that compared to bright galaxies, UDGs are relatively more abundant in massive clusters than in groups. We discuss the implications, but it is still unclear whether this difference is related to a higher destruction rate of UDGs in groups or if massive haloes have a positive effect on UDG formation.

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Section: Introductionsupporting

confidence: 66%

The abundance of ultra-diffuse galaxies from groups to clusters

Burg

Hoekstra

Muzzin

et al. 2017

A&A

116

106

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“…Right: Normalised comparison with observations of HI-bearing field UDGs in the literature (Leisman et al 2017). and predictions from the semi-analytical models (SAM) of Rong et al (2017) and Jones et al (2018). Poisson error-bars are shown.…”

Section: Comparison With Hi-bearing Udgsmentioning

confidence: 99%

“…One particularity relevant piece of work is that of Leisman et al (2017) and Jones et al (2018), who have shown that not only do HI-bearing UDGs exist in the field (as theoretically predicted by Di Cintio et al 2017), but also that their number density is too high to be explained by an extrapolation of the empirical relation between the number of UDGs and M halo measured by van der Burg et al (2017). Further, their sample appear systematically bluer than anticipated for UDGs in the field when compared with semi-analytic models (Rong et al 2017;Jones et al 2018). However, this analysis was limited to HI-rich field UDGs and it is unknown how this population relates to the overall field UDG population.…”

Section: Introductionmentioning

confidence: 97%

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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“…Yozin & Bekki 2015;Zaritsky 2017;Sifón et al 2018;Amorisco et al 2018) and theoretical ones (e.g. Amorisco & Loeb 2016;Di Cintio et al 2017;Rong et al 2017;Chan et al 2018;Liao et al 2019;Jiang et al 2019) found that UDGs span a wide range of physical properties, and perhaps a correspondingly large range of origin stories.…”

Section: Introductionmentioning

confidence: 99%

One Hundred SMUDGes in S-PLUS: Ultra-diffuse Galaxies Flourish in the Field

Barbosa

Zaritsky

Donnerstein

et al. 2020

ApJS

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We present the first systematic study of the stellar populations of ultra-diffuse galaxies (UDGs) in the field, integrating the large area search and characterization of UDGs by the SMUDGes survey with the twelve-band optical photometry of the S-PLUS survey. Based on Bayesian modeling of the optical colors of UDGs, we determine the ages, metallicities and stellar masses of 100 UDGs distributed in an area of ∼ 330 deg 2 in the Stripe 82 region. We find that the stellar masses and metallicities of field UDGs are similar to those observed in clusters and follow the trends previously defined in studies of dwarf and giant galaxies. However, field UDGs have younger luminosityweighted ages than do UDGs in clusters. We interpret this result to mean that field UDGs have more extended star formation histories, including some that continue to form stars at low levels to the present time. Finally, we examine stellar population 2 Barbosa et al.scaling relations that show that UDGs are, as a population, similar to other low-surface brightness galaxies.

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A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

Cited by 124 publications

References 66 publications

The abundance of ultra-diffuse galaxies from groups to clusters

The abundance of ultra-diffuse galaxies from groups to clusters

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

One Hundred SMUDGes in S-PLUS: Ultra-diffuse Galaxies Flourish in the Field

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