Catalog of Ultra-Diffuse Galaxies in the Coma Clusters From Subaru Imaging Data*

Yagi, Masafumi; Koda, Jin; Komiyama, Yutaka; Yamanoi, Hitomi

doi:10.3847/0067-0049/225/1/11

Cited by 194 publications

(421 citation statements)

References 95 publications

(181 reference statements)

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“…This UDG has an intermediate mass neighbor at a projected distance of 0.6 Mpc (IC 1668 with M * ≈ 4 × 10 9 M ) and two massive neighbors within 1.0 Mpc (UGC 862 and CGCG 502-039, with M * ≈ 3 × 10 10 M ). At the same time, it should be kept in mind that DGSAT I is still found in a relatively low density environment, especially when compared to the vast majority of UDGs discovered to date (e.g., Yagi et al 2016). In fact, even the star-forming UDG progenitors discovered by Román & Trujillo (2017) in nearby compact groups lie at a projected distance of just 0.2−0.3 Mpc from massive neighbors.…”

Section: Discussionmentioning

confidence: 99%

The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

Papastergis

Adams

Romanowsky

2017

A&A

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We report on the results of radio observations in the 21 cm emission line of atomic hydrogen (HI) of four relatively isolated ultradiffuse galaxies (UDGs): DGSAT I, R-127-1, M-161-1, and SECCO-dI-2. Our Effelsberg observations resulted in non-detections for the first three UDGs, and a clear detection for the last. DGSAT I, R-127-1, and M-161-1 are quiescent galaxies with gas fractions that are much lower than those of typical field galaxies of the same stellar mass. On the other hand, SECCO-dI-2 is a star forming gas-rich dwarf, similar to two other field UDGs that have literature HI data: SECCO-dI-1 and UGC 2162. This group of three gas-rich UDGs have stellar and gaseous properties that are compatible with a recently proposed theoretical mechanism for the formation of UDGs, based on feedback-driven outflows. In contrast, the physical characteristics of R-127-1 and M-161-1 are puzzling, given their isolated nature. We interpret this dichotomy in the gaseous properties of field UDGs as a sign of the existence of multiple mechanisms for their formation, with the formation of the quiescent gas-poor UDGs remaining a mystery.

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Section: Discussionmentioning

confidence: 99%

The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

Papastergis

Adams

Romanowsky

2017

A&A

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“…Since the purpose of the XDF observations was to determine the level of background contamination from field UDGs, the physical sizes of XDF objects were calculated assuming they are at the same redshift as A2744. The right-hand panel of Figure 1 shows the sizes, absolute r magnitudes, and stellar masses of A2744 UDG candidates, along with those in Coma from Yagi et al (2016) for comparison. We calculated stellar masses from the F814W magnitudes using the same SSP as above.…”

Section: Ultra-diffuse Galaxy Selectionmentioning

confidence: 99%

“…UDGs from Yagi et al (2016) in light gray. Since the purpose of the XDF observations was to determine the level of background contamination from field UDGs, the physical sizes of XDF objects were calculated assuming they are at the same redshift as A2744.…”

Section: Ultra-diffuse Galaxy Selectionmentioning

confidence: 99%

“…Adding A2744 (M 200 =5×10 15 M e ) allows us to extend this relation by 0.7 dex, as shown in Figure 4, which overplots our A2744 number on top of the relation of vdB16. We include UDGs in Coma and Fornax by applying our selection to the Yagi et al (2016) and Muñoz et al (2015) catalogs, respectively, the numbers in A168 and UGC842 (Román & Trujillo 2017), and three Hickson Compact Groups (Román & Trujillo 2016). For Fornax, the catalog covers the inner 350 kpc, so we apply a geometrical incompleteness correction 9 out to R 200 =700 kpc (Drinkwater et al 2001).…”

Section: Ultra-diffuse and Ultra-compact Galaxies In Abell 2744mentioning

confidence: 99%

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

Janssens

Abraham

Brodie

et al. 2017

ApJL

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We report the discovery of a large population of ultra-diffuse galaxies (UDGs) in the massive galaxy cluster Abell 2744 (z = 0.308) as observed by the Hubble Frontier Fields program. Since this cluster is ∼5 times more massive than Coma, our observations allow us to extend 0.7 dex beyond the high-mass end of the relationship between UDG abundance and cluster mass reported by van der Burg et al. Using the same selection criteria as van der Burg et al., A2744 hosts an estimated 1961±577 UDGs, 10 times the number in Coma. As noted by Lee & Jang, A2744 contains numerous unresolved compact objects, which those authors identified predominantly as globular clusters. However, these objects have luminosities that are more consistent with ultra-compact dwarf (UCD) galaxies. The abundances of both UCDs and UDGs scale with cluster mass as a power law with a similar exponent, although UDGs and UCDs have very different radial distributions within the cluster. The radial surface density distribution of UCDs rises sharply toward the cluster center, while the surface density distribution of the UDG population is essentially flat. Together, these observations hint at a picture where some UCDs in A2744 may have once been associated with infalling UDGs. As UDGs fall in and dissolve, they leave behind a residue of unbound UCDs.

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“…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%

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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Catalog of Ultra-Diffuse Galaxies in the Coma Clusters From Subaru Imaging Data*

Cited by 194 publications

References 95 publications

The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

The HI content of isolated ultra-diffuse galaxies: A sign of multiple formation mechanisms?

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

A Universe of ultradiffuse galaxies: theoretical predictions from ΛCDM simulations

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