The Next Generation Virgo Cluster Survey. Vi. The Kinematics of Ultra-Compact Dwarfs and Globular Clusters in M87

Zhang, Hongxin; Peng, Eric W.; Côté, Patrick; Liu, Chengze; Ferrarese, Laura; Cuillandre, Jean-Charles; Caldwell, Nelson; Gwyn, Stephen; Jordán, Andrés; Lançon, A.; Li, Biao; Muñoz, Roberto P.; Puzia, Thomas H.; Bekki, Kenji; Blakeslee, John P.; Boselli, A.; Drinkwater, Michael J.; Duc, Pierre–Alain; Durrell, Patrick R.; Emsellem, Éric; Firth, P.; Sánchéz-Janssen, R.

doi:10.1088/0004-637x/802/1/30

Cited by 94 publications

(164 citation statements)

References 139 publications

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“…Filled circles indicate colors of spectroscopically confirmed GCs of M87 in previous studies to guide location of GCs in the color-color diagram. (Hanes et al 2001;Strader et al 2011;Zhang et al 2015). We drew dashed polygon based on M87 GCs, and chose GC candidates in NGC 474 using this polygon we chose GC candidates within 2.5R e,GCS , represented by the largest circle (red) in Figure 1.…”

Section: Global Propertiesmentioning

confidence: 99%

Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474

Lim

Peng

Duc

et al. 2017

ApJ

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Globular clusters (GCs) are some of the most visible tracers of the merging and accretion history of galaxy halos. Metal-poor GCs, in particular, are thought to arrive in massive galaxies largely through dry, minor merging events, but it is rare to see a direct connection between GCs and visible stellar streams. NGC 474 is a post-merger early-type galaxy with dramatic fine structures made of concentric shells and radial streams that have been more clearly revealed by deep imaging. We present a study of GCs in NGC 474 to better establish the relationship between merger-induced fine structure and the GC system. We find that many GCs are superimposed on visible streams and shells, and about 35% of GCs outside 3R e,galaxy are located in regions of fine structure. The spatial correlation between the GCs and fine structure is significant at the 99.9% level, showing that this correlation is not coincidental. The colors of the GCs on the fine structures are mostly blue, and we also find an intermediate-color population that is dominant in the central region, and which will likely passively evolve to have colors consistent with a traditional metal-rich GC population. The association of the blue GCs with fine structures is direct confirmation that many metal-poor GCs are accreted onto massive galaxy halos through merging events, and that progenitors of these mergers are sub-L ⋆ galaxies.

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Section: Global Propertiesmentioning

confidence: 99%

Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474

Lim

Peng

Duc

et al. 2017

ApJ

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“…dwarf galaxies (UCDs), a population of extragalactic sources with characteristics in between those of compact elliptical galaxies and globular clusters (Hilker et al 1999;Drinkwater et al 2000;Zhang et al 2015). These sources, however, have NUV apparent magnitudes below the NUV = 20 mag limit because of their relatively red colours ) and should not be counted in the determination of the NUV luminosity function of Virgo.…”

Section: Possible Biasesmentioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg 2 , an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV − i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = −1.19), here sampled down to ∼NUV = −11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M * = −17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments.

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“…These "ultra-compact dwarfs" (UCDs) have characteristics reminiscent of both the nuclei of low-mass galaxies (Georgiev & Böker 2014), and massive GCs, and they may well have a connection to both populations (see, e.g., Mieske et al 2002Mieske et al , 2012Brodie et al 2011;Norris et al 2014;Zhang et al 2015). UCDs seem to occur mostly in dense environments (both near the centers of clusters and near massive galaxies), suggesting that environmental factors (e.g., tidal stripping) drives their formation (e.g., Bekki et al 2003;Pfeffer & Baumgardt 2013).…”

Section: Introductionmentioning

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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The Next Generation Virgo Cluster Survey. Vi. The Kinematics of Ultra-Compact Dwarfs and Globular Clusters in M87

Cited by 94 publications

References 139 publications

Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474

Globular Clusters as Tracers of Fine Structure in the Dramatic Shell Galaxy NGC 474

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

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

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