How elevated is the dynamical-to-stellar mass ratio of the ultracompact dwarf S999?

Forbes, Duncan A.; Norris, Mark A.; Strader, Jay; Fagioli, Martina; Romanowsky, Aaron J.

doi:10.1093/mnras/stv389

Cited by 31 publications

(31 citation statements)

References 87 publications

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“…The presence of SMBHs with such masses is indeed suggested or observationally confirmed at least for a few UCDs (e.g. Seth et al 2014;Janz et al 2015;Ahn et al 2017).…”

Section: The Implications Of Observed M/l V -Ratiosmentioning

confidence: 72%

The formation of ultra compact dwarf galaxies and massive globular clusters

Jeřabková

Kroupa

Dabringhausen

et al. 2017

A&A

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The stellar initial mass function (IMF) has been described as being invariant, bottom-heavy, or top-heavy in extremely dense starburst conditions. To provide usable observable diagnostics, we calculate redshift dependent spectral energy distributions of stellar populations in extreme star-burst clusters, which are likely to have been the precursors of present day massive globular clusters (GCs) and of ultra compact dwarf galaxies (UCDs). The retention fraction of stellar remnants is taken into account to assess the mass to light ratios of the ageing star-burst. Their redshift dependent photometric properties are calculated as predictions for James Webb Space Telescope (JWST) observations. While the present day GCs and UCDs are largely degenerate concerning bottom-heavy or top-heavy IMFs, a metallicity-and density-dependent top-heavy IMF implies the most massive UCDs, at ages <100 Myr, to appear as objects with quasar-like luminosities with a 0.1-10% variability on a monthly timescale due to core collapse supernovae.

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“…The presence of SMBHs with such masses is indeed suggested or observationally confirmed at least for a few UCDs (e.g. Seth et al 2014;Janz et al 2015;Ahn et al 2017).…”

Section: The Implications Of Observed M/l V -Ratiosmentioning

confidence: 72%

The formation of ultra compact dwarf galaxies and massive globular clusters

Jeřabková

Kroupa

Dabringhausen

et al. 2017

A&A

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“…Mieske et al 2013;Forbes et al 2014;Janz et al 2015;Janz et al 2016a). Figure 13 shows such mass ratios vs the stellar mass (this time from the luminosity-weighted M/L) for all the compact systems in the AIMSS sample (N+14; filled dots) and our galaxies (pentagons).…”

Section: Results From the Individual Discriminant Toolsmentioning

confidence: 99%

On the formation mechanisms of compact elliptical galaxies

Ferré-Mateu

Forbes

Romanowsky

et al. 2017

Monthly Notices of the Royal Astronomical Society

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In order to investigate the formation mechanisms of the rare compact elliptical galaxies (cE) we have compiled a sample of 25 cEs with good SDSS spectra, covering a range of stellar masses, sizes and environments. They have been visually classified according to the interaction with their host, representing different evolutionary stages. We have included clearly disrupted galaxies, galaxies that despite not showing signs of interaction are located close to a massive neighbour (thus are good candidates for a stripping process), and cEs with no host nearby. For the latter, tidal stripping is less likely to have happened and instead they could simply represent the very low-mass, faint end of the ellipticals. We study a set of properties (structural parameters, stellar populations, star formation histories and mass ratios) that can be used to discriminate between an intrinsic or stripped origin. We find that one diagnostic tool alone is inconclusive for the majority of objects. However, if we combine all the tools a clear picture emerges. The most plausible origin, as well as the evolutionary stage and progenitor type, can be then determined. Our results favor the stripping mechanism for those galaxies in groups and clusters that have a plausible host nearby, but favors an intrinsic origin for those rare cEs without a plausible host and that are located in looser environments.

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“…At least some UCDs contain a central supermassive black hole (see Seth et al 2014;Janz et al 2015 for detections, andFrank et al 2011;Norris et al 2015 for non-detections). UCDs appear not to have high dark matter fractions (Frank et al 2011;Mieske et al 2013;Forbes et al 2014;Janz et al 2015).…”

Section: Introductionmentioning

confidence: 90%

M32 Analogs? A Population of Massive Ultra-compact Dwarf and Compact Elliptical Galaxies in Intermediate-redshift Clusters

Zhang¹,

Bell²

2017

ApJL

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We report the discovery of relatively massive, M32-like ultra compact dwarf (UCD) and compact elliptical (CE) galaxy candidates in 0.2 < z < 0.6 massive galaxy clusters imaged by the Cluster Lensing And Supernova survey with Hubble (CLASH) survey. Examining the nearly unresolved objects in the survey, we identify a sample of compact objects concentrated around the cluster central galaxies with colors similar to cluster red sequence galaxies. Their colors and magnitudes suggest stellar masses around 10 9 M . More than half of these galaxies have half-light radii smaller than 200 pc, falling into the category of massive UCDs and CEs, with properties similar to M32. The properties are consistent with a tidal stripping origin, but we cannot rule out the possibility that they are earlyformed compact objects trapped in massive dark matter halos. The 17 CLASH clusters studied in this work on average contain 2.7 of these objects in their central 0.3 Mpc and 0.6 in their central 50 kpc. Our study demonstrates the possibility of statistically characterizing UCDs/CEs with a large set of uniform imaging survey data.

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How elevated is the dynamical-to-stellar mass ratio of the ultracompact dwarf S999?

Cited by 31 publications

References 87 publications

The formation of ultra compact dwarf galaxies and massive globular clusters

The formation of ultra compact dwarf galaxies and massive globular clusters

On the formation mechanisms of compact elliptical galaxies

M32 Analogs? A Population of Massive Ultra-compact Dwarf and Compact Elliptical Galaxies in Intermediate-redshift Clusters

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