The globular cluster systems of Abell 1185

West, Michael J.; Jordán, Andrés; Blakeslee, John P.; Côté, Patrick; Gregg, Michael D.; Takamiya, M.; Marzke, Ronald O.

doi:10.1051/0004-6361/201015939

Cited by 33 publications

(30 citation statements)

References 84 publications

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“…Those authors estimated that about 30% to 40% of globular clusters in Coma are intra-cluster globular clusters. West et al (2011) confirmed the presence of ∼ 1300 globular clusters in the Abell 1185 galaxy cluster that apparently are not bound to any galaxy. Recently, Harris and Mulholland (2017) estimate ∼ 50000 − 80000 intra-cluster globular clusters in the Perseus cluster, with a radial distribution extending several kiloparsecs away from the cluster center.…”

Section: Introductionsupporting

confidence: 53%

Intra-cluster Globular Clusters in a Simulated Galaxy Cluster

Ramos

Abadi

Muriel

et al. 2018

ApJ

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Using a cosmological dark matter simulation of a galaxy-cluster halo, we follow the temporal evolution of its globular cluster population. To mimic the red and blue globular cluster populations, we select at high redshift (z ∼ 1) two sets of particles from individual galactic halos constrained by the fact that, at redshift z = 0, they have density profiles similar to observed ones. At redshift z = 0, approximately 60% of our selected globular clusters were removed from their original halos building up the intra-cluster globular cluster population, while the remaining 40% are still gravitationally bound to their original galactic halos. Since the blue population is more extended than the red one, the intra-cluster globular cluster population is dominated by blue globular clusters, with a relative fraction that grows from 60% at redshift z = 0 up to 83% for redshift z ∼ 2. In agreement with observational results for the Virgo galaxy cluster, the blue intra-cluster globular cluster population is more spatially extended than the red one, pointing to a tidally disrupted origin.

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Section: Introductionsupporting

confidence: 53%

Intra-cluster Globular Clusters in a Simulated Galaxy Cluster

Ramos

Abadi

Muriel

et al. 2018

ApJ

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“…(e.g., West et al 2011). Although GCs have been found distributed between galaxies in rich clusters (e.g., Peng et al 2011;West et al 2011), their density drops with clustercentric radius, and we would not expect a significant number of IC GCs at the location of this SN Ia, 616 kpc from the BCG.…”

Section: Abell 399mentioning

confidence: 86%

CONFIRMATION OF HOSTLESS TYPE Ia SUPERNOVAE USINGHUBBLE SPACE TELESCOPEIMAGING

Graham

Sand

Zaritsky

2015

ApJ

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We present deep Hubble Space Telescope imaging at the locations of four, potentially hostless, long-faded Type Ia supernovae (SNe Ia) in low-redshift, rich galaxy clusters that were identified in the Multi-Epoch Nearby Cluster Survey. Assuming a steep faint-end slope for the galaxy cluster luminosity function (a = -1.5 d ), our data includeall but 0.2%of the stellar mass in cluster galaxies (0.005% with a = -1. ) may be either a globular cluster (GC) or a faint dwarf galaxy. We estimate the local surface densities of GCs and dwarfs to show that a GC is more likely, due to the proximity of an elliptical galaxy, but neither can be ruled out. This faint host implies that the SN Ia rate in dwarfs or GCs may be enhanced, but remains within previous observational constraints. We demonstrate that our results do not preclude the use of SNe Ia as bright tracers of IC light at higher redshifts, but that it will be necessary to first refine the constraints on their rate in dwarfs and GCs with deep imaging for a larger sample of low-redshift, apparently hostless SNe Ia.

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“…The first posits that globular clusters are formed in galaxies, but that strong galaxy-galaxy interactions might subsequently lead to some fraction becoming unbound. This is thought to be the origin of the significant IGC populations observed in galaxy clusters, where close encounters between galaxies frequently lead to tidal disruption or stripping (e.g., West et al 2011; ⋆ E-mail: dougal.mackey@anu.edu.au Samsing 2015). It is well known that galaxy interactions, mergers and accretions have occurred in the Local Group.…”

Section: Introductionmentioning

confidence: 99%

No sign (yet) of intergalactic globular clusters in the Local Group

Mackey

Beasley

Leaman

2016

Monthly Notices of the Royal Astronomical Society: Letters

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We present Gemini/GMOS imaging of twelve candidate intergalactic globular clusters (IGCs) in the Local Group, identified in a recent survey of the SDSS footprint by di Tullio Zinn & Zinn (2015). Our image quality is sufficiently high, at ∼ 0.4 ′′ − 0.7 ′′ , that we are able to unambiguously classify all twelve targets as distant galaxies. To reinforce this conclusion we use GMOS images of globular clusters in the M31 halo, taken under very similar conditions, to show that any genuine clusters in the putative IGC sample would be straightforward to distinguish. Based on the stated sensitivity of the di Tullio Zinn & Zinn (2015) search algorithm, we conclude that there cannot be a significant number of IGCs with M V −6 lying unseen in the SDSS area if their properties mirror those of globular clusters in the outskirts of M31 -even a population of 4 would have only a ≈ 1% chance of non-detection.

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The globular cluster systems of Abell 1185

Cited by 33 publications

References 84 publications

Intra-cluster Globular Clusters in a Simulated Galaxy Cluster

Intra-cluster Globular Clusters in a Simulated Galaxy Cluster

CONFIRMATION OF HOSTLESS TYPE Ia SUPERNOVAE USINGHUBBLE SPACE TELESCOPEIMAGING

No sign (yet) of intergalactic globular clusters in the Local Group

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