Globular Clusters, Ultracompact Dwarfs, and Dwarf Galaxies in Abell 2744 at a Redshift of 0.308

Lee, Myung Gyoon; Jang, In Sung

doi:10.3847/0004-637x/831/1/108

Cited by 22 publications

(33 citation statements)

References 89 publications

(200 reference statements)

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“…If analogies with Virgo or Coma are useful, roughly half of these should belong to the member galaxies, with the remainder in the IGM; thus, N IGC ∼ 50, 000, which agrees to within a factor of two with our estimate working directly from the observations. GC populations this large are not unprecedented: Coma, which has a total mass very similar to Perseus, contains at least N GC = 70, 000 GCs (Peng et al 2011), and estimates well above N GC = 100, 000 have been proposed for the more distant clusters A1689 and A2744 (Alamo-Martínez et al 2013;Lee & Jang 2016).…”

Section: Discussion: the Igc Populationmentioning

confidence: 99%

“…In the richer Coma cluster, Peng et al (2011) find a substantial IGC population filling the cluster core regions. Three other and more distant galaxy clusters for which IGCs have been sampled with unusually deep HST imaging include A1185 (West et al 2011), A1689 (Alamo-Martínez et al 2013, and A2744 (Lee & Jang 2016), though for various reasons of either field coverage or depth these also remain more uncertain than for Virgo or Coma (see also Harris et al 2017, for additional discussion of A1689 and A2744).…”

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confidence: 99%

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Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Harris

Mulholland

2017

ApJ

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Hubble Space Telescope photometry from the ACS/WFC and WFPC2 cameras is used to detect and measure globular clusters (GCs) in the central region of the rich Perseus cluster of galaxies. A detectable population of Intragalactic GCs is found extending out to at least 500 kpc from the cluster center. These objects display luminosity and color (metallicity) distributions that are entirely normal for GC populations. Extrapolating from the limited spatial coverage of the HST fields, we estimate very roughly that the entire Perseus cluster should contain ∼ 50000 or more IGCs, but a targetted wide-field survey will be needed for a more definitive answer. Separate brief results are presented for the rich GC systems in NGC 1272 and NGC 1275, the two largest Perseus ellipticals. For NGC 1272 we find a specific frequency S N ≃ 8, while for the central giant NGC 1275, S N ≃ 12. In both these giant galaxies, the GC colors are well matched by bimodal distributions, with the majority in the blue (metal-poor) component. This preliminary study suggests that Perseus is a prime target for a more comprehensive deep imaging survey of Intragalactic GCs.

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Section: Discussion: the Igc Populationmentioning

confidence: 99%

mentioning

confidence: 99%

Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Harris

Mulholland

2017

ApJ

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“…Lee & Jang (2016;hereafter LJ16) reported an extrapolated total of 385,000 GCs, with a quoted error of only 6%. These authors assumed the Milky Way GCLF with σ = 1.2 mag and that the observed F814W bandpass matched identically the rest-frame r-band.…”

Section: +71200mentioning

confidence: 99%

Specific Frequencies and Luminosity Profiles of Cluster Galaxies and Intracluster Light in Abell 1689

Álamo-Martínez

Blakeslee

2017

ApJ

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We present magnitudes and profile fits for 180 galaxies in the central field of the massive lensing cluster Abell 1689 using very deep imaging with the Hubble Space Telescope Advanced Camera for Surveys in the F814W bandpass. Previous work revealed an exceptionally large number of globular clusters (GCs) in A1689 and mapped their number density distribution. We decompose this number density map into GCs associated with individual cluster galaxies and ICGCs (intracluster globular clusters) associated with the intracluster light (ICL). In all, we measure GC specific frequencies S N for 33 cluster members and the ICL. The relation between S N and galaxy magnitude is consistent with the trend observed in Virgo, although some intermediate luminosity galaxies scatter to S N > 10. We estimate the ICL makes up 11% of the starlight in this field, whereas the ICGCs account for ∼ 35% of the GCs, both consistent with predictions from simulations. Galaxies with higher S N values tend to be rounder, and there is a marginally significant trend of decreasing S N with increasing specific angular momenta λ R . We also reevaluate the GC population in the A2744 Frontier Field, for which fewer than one-tenth as many GCs have been detected because of its larger distance. Finally, our core-Sérsic fit to the light profile of the A1689 BCG implies a break radius of 3.8 kpc, among the largest known; we discuss implications of the sizable core and extensive GC population for the supermassive black hole in light of scaling relations.

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“…6 M e (a widely accepted upper mass cutoff for a GC), and it seems much more likely to us that the vast majority of the objects identified by Lee & Jang (2016) are UCDs.…”

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

confidence: 99%

“…Recently, Lee & Jang (2016) studied compact (FWHM400 pc) objects within the A2744 cluster field (using the parallel field for background subtraction). These sources are concentrated around the BCGs, confirming their membership of A2744.…”

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

confidence: 99%

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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Globular Clusters, Ultracompact Dwarfs, and Dwarf Galaxies in Abell 2744 at a Redshift of 0.308

Cited by 22 publications

References 89 publications

Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Detection of the Stellar Intracluster Medium in Perseus (Abell 426)

Specific Frequencies and Luminosity Profiles of Cluster Galaxies and Intracluster Light in Abell 1689

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

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