Globular clusters, satellite galaxies and stellar haloes from early dark matter peaks

By B. Moore, J. Diemand, P. Madau, Marcel Zemp, J. W. U. O. Zurich, U. California, Santa Cruz, E. Zurich. 2005

190 citations recorded by the source corpus.

The Milky Way contains several distinct old stellar components that provide a fossil record of its formation. We can understand their spatial distribution and kinematics in a hierarchical formation scenario by associating the proto-galactic fragments envisaged by Searle and Zinn (1978) with the rare peaks able to cool gas in the cold dark matter density field collapsing at redshift z > 10. We use hierarchical structure formation simulations to explore the kinematics and spatial distribution of these early star-forming structures in galaxy haloes today. Most of the proto-galaxies rapidly merge, their stellar contents and dark matter becoming smoothly distributed and forming the inner Galactic halo. The metal-poor globular clusters and old halo stars become tracers of this early evolutionary phase, centrally biased and naturally reproducing the observed steep fall off with radius. The most outlying peaks fall in late and survive to the present day as satellite galaxies. The observed radial velocity dispersion profile and the local radial velocity anisotropy of Milky Way halo stars are successfully reproduced in this model. If this epoch of structure formation coincides with a suppression of further cooling into lower sigma peaks then we can reproduce the rarity, kinematics and spatial distribution of satellite galaxies as suggested by Bullock et al. (2000). Reionisation at z = 12±2 provides a natural solution to the missing satellites problem. Measuring the distribution of globular clusters and halo light on scales from galaxies to clusters could be used to constrain global versus local reionisation models. If reionisation occurs contemporary, our model predicts a constant frequency of blue globulars relative to the host halo mass, except for dwarf galaxies where the average relative frequencies become smaller.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5c96e32f4fdaf1bfab4fef2833b548317e05f510

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure (2007, methodology): “Similar models (Bullock et al. 2000; Moore et al. 2006) select only systems above the atomic cooling mass at the reionisation epoch (z ≃ 10).”
Small scale problems of the $\Lambda$CDM model: a short review (2016, background): “This can prevent small mass DM haloes gas accretion, “quenching” star formation after z ' 10 [380,381,394].”
METALLICITY EVOLUTION OF DAMPED Lyα SYSTEMS OUT TO z ∼ 5 (2012, background): “The second is an accretion scenario where a number of smaller galaxies merge to form the Galactic halo (e.g. Searle & Zinn 1978; Bullock & Johnston 2005; Moore et al. 2006).”
Dark Matter Substructure and Gamma-Ray Annihilation in the Milky Way Halo (2006, methodology): “The same two systems are also the only ones that form early enough to become luminous in the Moore et al. (2006) scenario.”
The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies (2012, background): “…numerical predictions are in part due to the diverse recipes with which simulations were built (B+05; B+08; Diemand et al. 2005; Kravtsov & Gnedin 2005; Moore et al. 2006), but they might also reflect a real diversity of formation mechanisms that built up the GC systems in the first place.”
MODELING THE METALLICITY DISTRIBUTION OF GLOBULAR CLUSTERS (2010, background): “Moore et al. (2006) showed that the early-forming halos are more spatially concentrated and in order to match the Galactic distribution, globular clusters would need to form at z ∼ 12.”
The Accretion Origin of the Milky Way’s Stellar Halo (2007, background): “9 of Bullock & Johnston 2005, see also Diemand, Madau, & Moore 2005, Moore et al. 2006),ii) total stellar halo masses from∼ 109M⊙ (integrated over all radii), andiii) richly substructured halos with increasingly evident substructure at larger distances (e.g., Figs.”
The stellar halo of the Galaxy (2008, background): “…profile can be ruled out, while both a dark halo following a truncated flat model (Wilkinson & Evans 1999) of mass 5+2.5 −1.7 × 10 11 M⊙ and an NFW profile of mass 9.4 +1.4 −0.9 × 10 11 M⊙ and concentration c = 18 are consistent with the data (see also Moore et al. 2006; Abadi et al. 2006).”
H i IN LOCAL GROUP DWARF GALAXIES AND STRIPPING BY THE GALACTIC HALO (2009, background): “Given the amount of time for the Local Group galaxies to evolve since reionization (e.g., Moore et al. 2006), it seems unlikely that reionization could lead to the present day HI-distance effect.”
Galaxies as simple dynamical systems: observational data disfavor dark matter and stochastic star formation (2014, unknown): “[52,91–94]).”
Bayesian strong gravitational-lens modelling on adaptive grids: objective detection of mass substructure in Galaxies (2008, background): “From an astrophysical point of view, the number of visible satellites can be reduced by suppressing the gas collapse/cooling (e.g., Bullock et al. 2000; Kravtsov et al. 2004; Moore et al. 2006) via supernova feedback, photoionization or reionization.”
The Luminosity Function of the Milky Way Satellites (2007, background): “For example, the satellites that are observed could be embedded only in the rarer, more massive dark sub-halos (Stoehr et al. 2002), or, the satellites may form only in the rare peaks of halos that were above a given mass at reionization (Diemand et al. 2005; Moore et al. 2006).”
WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, background): “…constraints, but they do illustrate conceptually the kind of inferences that one might make about the accretion history with more detailed models, e.g., based on the ellipticity, kinematics, and radial density profile of the GC system (Diemand et al. 2005; Moore et al. 2006; Griffen et al. 2010).”