A class of compact dwarf galaxies from disruptive processes in galaxy clusters

Drinkwater, Michael J.; Gregg, Michael D.; Hilker, M.; Bekki, Kenji; Couch, Warrick J.; Ferguson, Henry C.; Jones, Bryn; Phillipps, S.

doi:10.1038/nature01666

Cited by 257 publications

(372 citation statements)

References 26 publications

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“…Ultracompact dwarf galaxies (Drinkwater et al 2003), the formation of S0 galaxies (Quilis et al 2000 and references therein), and tidal debris in nearby clusters (Trentham & Mobasher 1998;Gregg & West 1998;Calcáneo-Roldán et al 2000) may all be closely related to the ICL phenomenon. Since searches for individual intracluster stars in nearby galaxy clusters can be influenced by metallicity effects (Durrell et al 2002;Feldmeier et al 2004), knowing the dominant progenitor population is critical to avoid underestimating the true fraction of intracluster light.…”

Section: Introductionmentioning

confidence: 99%

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Feldmeier¹,

Mihos²,

Morrison³

et al. 2004

ApJ

132

150

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We report the search for intracluster light in four Abell type II-III (non-cD) galaxy clusters: A801, A1234, A1553, and A1914. We find that on average these clusters contain $10% of their detected stellar luminosity in a diffuse component. We show that for two of the clusters the intracluster light closely follows the galaxy distribution, but in the other two cases, there are noticeable differences between the spatial distribution of the galaxies and the intracluster light. We report the results of a search for intracluster tidal debris in each cluster and note that A1914 in particular has a number of strong tidal features likely due to its status as a recent cluster merger. One of the A1914 features appears to be spatially coincident with an extension seen in weak lensing maps, implying that the feature traces a large amount of mass. We compare these results with numerical simulations of hierarchically formed galaxy clusters and find good general agreement between the observed and simulated images, although we also find that our observations sample only the brightest features of the intracluster light. Together, these results suggest that intracluster light can be a valuable tool in determining the evolutionary state of galaxy clusters.

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Section: Introductionmentioning

confidence: 99%

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Feldmeier¹,

Mihos²,

Morrison³

et al. 2004

ApJ

132

150

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“…Bell et al 2003;Oppenheimer et al 2010), and as such can be an important tracer of environmental effects (e.g. Drinkwater et al 2003). Moreover, the contribution by dwarf galaxies to hierarchical assembly and accretion onto giant galaxies is a vital part of our understanding of galaxy formation (e.g.…”

Section: Introductionmentioning

confidence: 99%

Kinematics of dwarf galaxies in gas-rich groups, and the survival and detectability of tidal dwarf galaxies

Sweet

Drinkwater

Meurer

et al. 2015

Mon. Not. R. Astron. Soc.

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We present DEIMOS multi-object spectroscopy (MOS) of 22 star-forming dwarf galaxies located in four gas-rich groups, including six newly-discovered dwarfs. Two of the galaxies are strong tidal dwarf galaxy (TDG) candidates based on our luminosity-metallicity relation definition. We model the rotation curves of these galaxies. Our sample shows low mass-to-light ratios (M/L=0.73±0.39M /L ) as expected for young, star-forming dwarfs. One of the galaxies in our sample has an apparently strongly-falling rotation curve, reaching zero rotational velocity outside the turnover radius of r turn = 1.2r e . This may be 1) a polar ring galaxy, with a tilted bar within a face-on disk; 2) a kinematic warp. These scenarios are indistinguishable with our current data due to limitations of slit alignment inherent to MOS-mode observations. We consider whether TDGs can be detected based on their tidal radius, beyond which tidal stripping removes kinematic tracers such as Hα emission. When the tidal radius is less than about twice the turnover radius, the expected falling rotation curve cannot be reliably measured. This is problematic for as much as half of our sample, and indeed more generally, galaxies in groups like these. Further to this, the Hα light that remains must be sufficiently bright to be detected; this is only the case for three (14%) galaxies in our sample. We conclude that the falling rotation curves expected of tidal dwarf galaxies are intrinsically difficult to detect.

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“…If we assume a mass to light ratio of three, we expect an absolute visual magnitude of -11 for the final object. For comparison, a typical UCDs found in Fornax has a central velocity dispersion of 22 km/s, an absolute magnitude of -12 and a half mass radius of 25 pc (Haşegan et al 2005;Drinkwater et al 2003). In order to form this system by merging globular clusters one would need to consider many more globulars to reach the observed luminosity.…”

Section: The Globular Cluster Simulationsmentioning

confidence: 99%

The Formation of Ultra-Compact Dwarf Galaxies and Nucleated Dwarf Galaxies

Goerdt

2011

Astrophysics and Space Science Proceedings

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Ultra compact dwarf galaxies (UCDs) have similar properties as massive globular clusters or the nuclei of nucleated galaxies. Recent observations suggesting a high dark matter content and a steep spatial distribution within groups and clusters provide new clues as to their origins. We perform high-resolution N -body / smoothed particle hydrodynamics simulations designed to elucidate two possible formation mechanisms for these systems: the merging of globular clusters in the centre of a dark matter halo, or the massively stripped remnant of a nucleated galaxy. Both models produce density profiles as well as the half light radii that can fit the observational constraints. However, we show that the first scenario results to UCDs that are underluminous and contain no dark matter. This is because the sinking process ejects most of the dark matter particles from the halo centre. Stripped nuclei give a more promising explanation, especially if the nuclei form via the sinking of gas, funneled down inner galactic bars, since this process enhances the central dark matter content. Even when the entire disk is tidally stripped away, the nucleus stays intact and can remain dark matter dominated even after severe stripping. Total galaxy disruption beyond the nuclei only occurs on certain orbits and depends on the amount of dissipation during nuclei formation. By comparing the total disruption of CDM subhaloes in a cluster potential we demonstrate that this model also leads to the observed spatial distribution of UCDs which can be tested in more detail with larger data sets.

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A class of compact dwarf galaxies from disruptive processes in galaxy clusters

Cited by 257 publications

References 26 publications

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Deep CCD Surface Photometry of Galaxy Clusters. II. Searching for Intracluster Starlight in Non‐cD clusters

Kinematics of dwarf galaxies in gas-rich groups, and the survival and detectability of tidal dwarf galaxies

The Formation of Ultra-Compact Dwarf Galaxies and Nucleated Dwarf Galaxies

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