Families of dynamically hot stellar systems over 10 orders of magnitude in mass

By I. Misgeld, Michael Hilker. 2011

156 citations recorded by the source corpus.

Dynamically hot stellar systems, whether star clusters or early-type galaxies, follow well-defined scaling relations over many orders of magnitudes in mass. These fundamental plane relations have been subject of several studies, which have been mostly confined to certain types of galaxies and/or star clusters so far. Here, we present a complete picture of hot stellar systems ranging from faint galaxies and star clusters of only a few hundred solar masses up to giant ellipticals (gEs) with 10 12 M � , in particular including – for the first time – large samples of compact ellipticals (cEs), ultra-compact dwarf galaxies (UCDs), dwarf ellipticals (dEs) of nearby galaxy clusters and Local Group ultra-faint dwarf spheroidals (dSphs). For all those stellar systems we show the effective radius–luminosity, effective radius–stellar mass, and effective mass surface density–stellar mass plane. Two clear families of hot stellar systems can be differentiated: the ’galaxian’ family, ranging from gEs over Es and dEs to dSphs, and the ’star cluster’ family, comprising globular clusters (GCs), UCDs and nuclear star clusters (NCs). Interestingly, massive ellipticals have a similar size–mass relation as cEs, UCDs and NCs, with a clear common boundary towards minimum sizes, which can be approximated by Reff > 2:24 �10 6 �M 4=5

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/009d26fabccb73ec2c9560316de626bd5c19aae0

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Citations in the corpus

The stellar and sub-stellar IMF of simple and composite populations (2011, result): “They are, like galaxies, collisionless stellar-dynamical systems such that two-body relaxation driven evaporation of low-mass stars is insignificant, contrary to the case for GCs (Anders et al. 2009; Misgeld & Hilker 2011; Forbes & Kroupa 2011).”
CONFIRMATION OF FAINT DWARF GALAXIES IN THE M81 GROUP (2013, background): “…1995; Mateo 1998; McConnachie & Irwin 2006; Simon & Geha 2007; Belokurov et al. 2007; Willman et al. 2005; Walsh et al. 2007; Zucker et al. 2006; Martin et al. 2006; Ibata et al. 2007; Irwin et al. 2008; McConnachie 2012) along with Centaurus and Hydra cluster members (Misgeld & Hilker 2011).”
The AIMSS Project I: bridging the star cluster, galaxy divide (2014, methodology): “The principle literature sources for CSSs are the compilations of Misgeld & Hilker (2011) and Brodie et al. (2011) plus the recent update from Forbes et al. (2013), and to these compilations we add additional data for specific systems.”
CO-EVOLUTION OF GALACTIC NUCLEI AND GLOBULAR CLUSTER SYSTEMS (2013, background): “…at the effective radius) of the most massive NSCs (MNSC = 107 − 109 M⊙) in both nearby latetype galaxies (Hartmann et al. 2011) and in early-type galaxies with M∗ < 4×1010M⊙ in the Virgo and Fornax clusters (Turner et al. 2012), as well as ultracompact dwarf galaxies (Misgeld & Hilker 2011).”
Greatly Enhanced Merger Rates of Compact-object Binaries in Non-spherical Nuclear Star Clusters (2017, background): “These nuclear clusters (NCs) have masses in the range ≈ 105 − 108 M⊙ and half mass radii of only a few parsecs, making them the most massive and densest stellar clusters observed in the local Universe (Forbes et al. 2008; Misgeld & Hilker 2011).”
The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, background): “Similar differences in the slope of the luminosity–size relation of dwarfs and ellipticals were presented by a number of authors (e.g. Kormendy 1985; Graham & Guzmán 2003; Kormendy et al. 2009; Misgeld & Hilker 2011).”
Eccentric Black Hole Gravitational-wave Capture Sources in Galactic Nuclei: Distribution of Binary Parameters (2017, methodology): “…1max SMBH 2 where MSMBH is the mass of the SMBH, σ* is the velocity dispersion of the underlying stellar populations in the nucleus near the SMBH, and we use the MSMBH−σ* relationship (Tremaine et al. 2002; Walcher et al. 2005; Misgeld & Hilker 2011; Norris et al. 2014): *s´ - ⎜ ⎟ ⎛ ⎝ ⎞ ⎠ ( )M M1.”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “It is populated by objects generally called dwarf ellipticals (dE) and ultra compact dwarfs (UCD) (e.g. Misgeld & Hilker 2011; Norris et al. 2014).”
Dwarf galaxies in CDM and SIDM with baryons: observational probes of the nature of dark matter (2014, background): “…data of Local Group dwarfs (MW+M31 dSphs+dIrrs) (taken from Côté, Carignan & Freeman 2000; McGaugh 2005; Peñarrubia, McConnachie & Navarro 2008; Woo, Courteau & Dekel 2008; Stark, McGaugh & Swaters 2009; Misgeld & Hilker 2011; Oh et al. 2011; Ferrero et al. 2012; Tollerud et al. 2012).”
THE SIZE–VIRIAL RADIUS RELATION OF GALAXIES (2012, methodology): “First, I use a compilation of stellar masses and effective radii for spheroidal, early-type galaxies from Misgeld & Hilker (2011).”
Surface brightness profile of the Milky Way’s nuclear star cluster (2014, background): “(2) Since NSCs are, on average, the densest observable stellar systems (Walcher et al. 2005; Misgeld & Hilker 2011) and may frequently contain MBHs, they play a key role in the study of stellar dynamics, for example in tests of fundamental ideas such as the formation of stellar cusps around MBHs.”
Masses and scaling relations for nuclear star clusters, and their co-existence with central black holes (2016, unknown): “…and possible evolutionary connections between them (e.g. Gregg et al. 2009; Price et al. 2009; Georgiev et al. 2009b,a, 2012; Taylor et al. 2010; Misgeld & Hilker 2011; Chiboucas et al. 2011; Brüns et al. 2011; Norris & Kannappan 2011; Foster et al. 2011; Pfeffer & Baumgardt 2013; Puzia et al.…”
THE RELATIONSHIPS AMONG COMPACT STELLAR SYSTEMS: A FRESH VIEW OF ULTRACOMPACT DWARFS (2011, background): “Such a database was published by Misgeld & Hilker (2011), and serves as one of our major sources of data.”
A MegaCam Survey of Outer Halo Satellites. III. Photometric and Structural Parameters (2018, background): “…structural properties of stellar systems in the Milky Way, M31 and nearby galaxy groups and clusters (e.g., Kormendy 1990; Côté et al. 2002; Willman et al. 2005a; Belokurov et al. 2007a; Dabringhausen et al. 2008; Tollerud et al. 2011; Huxor et al. 2011; Misgeld & Hilker 2011; Norris et al. 2014).”
How do minor mergers promote inside-out growth of ellipticals, transforming the size, density profile and dark matter fraction? (2012, methodology): “Therefore we assume two scenarios: a fixed size of ∼ 1kpc for the satellites, similar to local galaxies (see e.g. Misgeld & Hilker 2011), indicated by the filled red and green circles.”
Nuclear star clusters (2009, result): “Similar plots have previously been published by various authors (e.g., Hopkins and Quataert 2010b; Misgeld and Hilker 2011; Norris et al. 2014).”