NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-18 T02:43:12 PDT
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For refcode 2018MNRAS.477.3869H:
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Copyright by Royal Astronomical Society. 2018MNRAS.477.3869H The correlation between the sizes of globular cluster systems and their host dark matter haloes Hudson, Michael J.; Robison, Bailey Abstract. The sizes of entire systems of globular clusters (GCs) depend not only on the formation and destruction histories of the GCs themselves but also on the assembly, merger, and accretion history of the dark matter (DM) haloes that they inhabit. Recent work has shown a linear relation between total mass of GCs in the GC system and the mass of its host DM halo, calibrated from weak lensing. Here, we extend this to GC system sizes, by studying the radial density profiles of GCs around galaxies in nearby galaxy groups. We find that radial density profiles of the GC systems are well fit with a de Vaucouleurs profile. Combining our results with those from the literature, we find tight relationship (~0.2 dex scatter) between the effective radius of the GC system and the virial radius (or mass) of its host DM halo, for haloes with masses greater than ~10^12^ M_sun_. The steep non-linear dependence of this relationship (R_{{e, GCS}_} is proportional to R_{200}_^{2.5 - 3} is proportional to M_{200}_^{0.8 - 1}) is currently not well understood, but is an important clue regarding the assembly history of DM haloes and of the GC systems that they host. Key words: globular clusters: general, galaxies: groups: individual, galaxies: haloes
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