Ultra-diffuse and Ultra-compact Galaxies in the Frontier Fields Cluster Abell 2744

Janssens, Steven; Abraham, Roberto; Brodie, Jean P.; Forbes, Duncan A.; Romanowsky, Aaron J.; Dokkum, Pieter van

doi:10.3847/2041-8213/aa667d

Cited by 73 publications

(88 citation statements)

References 47 publications

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“…The abundances of UDGs are observed to correlate with the mass of their host cluster (van der Burg et al 2016;Janssens et al 2017): N ∝ M 0. 93±0.16 200 , where N is the number of UDGs in a cluster and M 200 is the cluster mass within a radius, r 200 , within which the average density is 200 times the cosmic critical density.…”

Section: Udgs In Clustersmentioning

confidence: 99%

“…van Dokkum et al (2015a,b) defined UDGs as the galaxies with μ 0,B > 24 mag arcsec −2 and r e > 1.5 kpc; some others used a slightly different quantity, the mean surface brightness within r e , μ e,r ≥ 24 mag arcsec −2 (e.g. van der Burg et al 2016;Yagi et al 2016;Janssens et al 2017). Given that the Sérsic indices, n, of most UDGs are around 1 (Koda et al 2015;Román & Trujillo 2017a;Yagi et al 2016) and colours g − r ∼ 0.6 (van der Burg et al 2016), μ e,r ≥ 24 mag arcsec −2 is approximately equivalent to g band μ 0,g > 23.5 mag arcsec −2 (Graham & Driver 2005).…”

Section: Sample Selectionmentioning

confidence: 99%

“…in Coma (van Dokkum et al 2015a), A168 (Román & Trujillo 2017a), A2744 (Janssens et al 2017), and other eight low-redshift clusters (van der Burg et al 2016, hereafter vdB16). Here, we focus on the comparison of the UDGs in clusters between the model predictions and observations.…”

Section: Udgs In Clustersmentioning

confidence: 99%

“…Coma (Koda et al 2015;van Dokkum et al 2015a,b;Yagi et al 2016), Virgo (Mihos et al 2015), Fornax (Muñoz et al 2015), A168 (Román & Trujillo 2017a), A2744 (Janssens et al 2017), eight other clusters with redshifts z ∼ 0. 044-0.063 (van der Burg, Muzzin & Hoekstra 2016) and PiscesPerseus supercluster (Martinez-Delgado et al 2016), as well as several galaxy groups (Makarov et al 2015;Toloba et al 2016;Román & Trujillo 2017b;Trujillo et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

Guo

Gao

et al. 2017

Monthly Notices of the Royal Astronomical Society

124

138

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A particular population of galaxies have drawn much interest recently, which are as faint as typical dwarf galaxies but have the sizes as large as L * galaxies, the so called ultra-diffuse galaxies (UDGs). The lack of tidal features of UDGs in dense environments suggests that their host halos are perhaps as massive as that of the Milky Way. On the other hand, galaxy formation efficiency should be much higher in the halos of such masses. Here we use the model galaxy catalog generated by populating two large simulations: the Millennium-II cosmological simulation and Phoenix simulations of 9 big clusters with the semi-analytic galaxy formation model. This model reproduces remarkably well the observed properties of UDGs in the nearby clusters, including the abundance, profile, color, and morphology, etc. We search for UDG candidates using the public data and find 2 UDG candidates in our Local Group and 23 in our Local Volume, in excellent agreement with the model predictions. We demonstrate that UDGs are genuine dwarf galaxies, formed in the halos of ∼ 10 10 M . It is the combination of the late formation time and high-spins of the host halos that results in the spatially extended feature of this particular population. The lack of tidal disruption features of UDGs in clusters can also be explained by their late infall-time.

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Section: Udgs In Clustersmentioning

confidence: 99%

Section: Sample Selectionmentioning

confidence: 99%

Section: Udgs In Clustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

Guo

Gao

et al. 2017

Monthly Notices of the Royal Astronomical Society

124

138

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show abstract

“…Some of the studies focused on the nearby and well-studied Fornax (Muñoz et al 2015), Coma (Koda et al 2015;Kadowaki et al 2017) and Virgo (Mihos et al 2015;Davies et al 2016) clusters. Other works studied more distant clusters (van der Burg et al 2016;Román & Trujillo 2017a), including a Frontier-fields cluster at z = 0.3 (Janssens et al 2017). It is clear that UDGs are a common phenomenon in galaxy clusters, and their ubiquity has to be understood in the context of existing galaxy formation models.…”

Section: Introductionmentioning

confidence: 99%

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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VEGAS-SSS. II. Comparing the globular cluster systems in NGC 3115 and NGC 1399 using VEGAS and FDS survey data

Cantiello¹,

D’Abrusco

Spavone

et al. 2018

A&A

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We analyze the globular cluster (GC) systems in two very different galaxies, NGC 3115 and NGC 1399. With the papers of this series, we aim at highlighting common and different properties in the GC systems in galaxies covering a wide range of parameter space. We compare the GCs in NGC 3115 and NGC 1399 as derived from the analysis of one square degree u−, g−, and i−band images taken with the VST telescope as part of the VST early-type galaxy survey (VEGAS) and Fornax deep survey (FDS). We selected GC candidates using as reference the morpho-photometric and color properties of confirmed GCs. The surface density maps of GCs in NGC 3115 reveal a morphology similar to the light profile of field stars; the same is true when blue and red GCs are taken separately. The GC maps for NGC 1399 are richer in structure and confirm the existence of an intra-cluster GC component. We confirm the presence of a spatial offset in the NGC 1399 GC centroid and find that the centroid of the GCs for NGC 3115 coincides well with the galaxy center. Both GC systems show unambiguous color bimodality in (g−i) and (u−i); the color-color relations of the two GC systems are slightly different with NGC 3115 appearing more linear than NGC 1399. The azimuthal average of the radial density profiles in both galaxies reveals a larger spatial extent for the total GCs population with respect to the galaxy surface brightness profile. For both galaxies, the red GCs have radial density profiles compatible with the galaxy light profile, while the radial profiles for blue GCs are shallower. As for the specific frequency of GCs, S N , we find it is a factor of two higher in NGC 1399 than for NGC 3115; this is mainly the result of extra blue GCs. By inspecting the radial behavior of the specific frequency, S N (< r), for the total, blue, and red GCs, we find notable similarities between the trends for red GCs in the two targets. In spite of extremely different host environments, the red GCs in both cases appear closely linked to the light distribution of field stars. Blue GCs extend to larger galactocentric scales than red GCs, marking a significant difference between the two galaxies: the blue/red GCs and field stellar components of NGC 3115 appear well thermalized with each other and the blue GCs in NGC 1399 appear to fade into an unrelaxed intra-cluster GC population.

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Ultra-diffuse and Ultra-compact Galaxies in the Frontier Fields Cluster Abell 2744

Cited by 73 publications

References 47 publications

A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

The abundance of ultra-diffuse galaxies from groups to clusters

VEGAS-SSS. II. Comparing the globular cluster systems in NGC 3115 and NGC 1399 using VEGAS and FDS survey data

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