Measuring the Dark Matter Scale of Local Group Dwarf Spheroidals

1999 ◽  
Vol 117 (3) ◽  
pp. 1275-1284 ◽  
Author(s):  
J. Kleyna ◽  
M. Geller ◽  
S. Kenyon ◽  
M. Kurtz
Keyword(s):  
Dark Matter ◽  
Local Group ◽  
Dwarf Spheroidals

The Cold Dark Matter Halos of Local Group Dwarf Spheroidals

2008 ◽  
Vol 672 (2) ◽  
pp. 904-913 ◽  
Author(s):  
Jorge Penarrubia ◽  
Alan W. McConnachie ◽  
Julio F. Navarro
Keyword(s):  
Dark Matter ◽  
Cold Dark Matter ◽  
Local Group ◽  
Dark Matter Halos ◽  
Dwarf Spheroidals

Erratum: “The Cold Dark Matter Halos of Local Group Dwarf Spheroidals” (ApJ, 672, 904 [2008])

2008 ◽  
Vol 687 (2) ◽  
pp. 1460-1460 ◽  
Author(s):  
Jorge Peñarrubia ◽  
Alan W. McConnachie ◽  
Julio F. Navarro
Keyword(s):  
Dark Matter ◽  
Cold Dark Matter ◽  
Local Group ◽  
Dark Matter Halos ◽  
Dwarf Spheroidals

scholarly journals The Effect of Tidal Stripping on Composite Stellar Populations in Dwarf Spheroidal Galaxies

2010 ◽  
Vol 2010 ◽  
pp. 1-14 ◽  
Author(s):  
Laura V. Sales ◽  
Amina Helmi ◽  
Giuseppina Battaglia
Keyword(s):  
Dark Matter ◽  
Mass Loss ◽  
Milky Way ◽  
Velocity Dispersion ◽  
Local Group ◽  
Stellar Populations ◽  
Dwarf Spheroidal Galaxies ◽  
Stellar Component ◽  
Dwarf Spheroidals ◽  
Matter Component

We use N-body simulations to study the effects of tides on the kinematical structure of satellite galaxies orbiting a Milky Way-like potential. Here we focus on the evolution of a spherical, dark matter dominated satellite, which is modelled with two stellar components set ab initio to be spatially and kinematically segregated, in a way that resembles the configuration of the metal poor and metal rich stellar populations in several dwarf spheroidals of the Local Group. We find that an important attenuation of the initial differences in the distribution of the two stellar components occurs for orbits with small pericentric radii. This is mainly due to (i) the loss of the gravitational support provided by the dark matter component after tidal stripping takes place and (ii) tides preferentially affect the more extended stellar component, leading to a net decrease in its velocity dispersion as a response for the mass loss, which thus shrinks the kinematical gap. We apply these ideas to the Sculptor and Carina dwarf spheroidals. Differences in their orbits might help to explain why in the former a clear kinematical separation between metal poor and metal rich stars is apparent, while in Carina this segregation is significantly more subtle.

scholarly journals MEASURING DARK MATTER PROFILES NON-PARAMETRICALLY IN DWARF SPHEROIDALS: AN APPLICATION TO DRACO

2013 ◽  
Vol 763 (2) ◽  
pp. 91 ◽  
Author(s):  
John R. Jardel ◽  
Karl Gebhardt ◽  
Maximilian H. Fabricius ◽  
Niv Drory ◽  
Michael J. Williams
Keyword(s):  
Dark Matter ◽  
Dwarf Spheroidals

scholarly journals The importance of tides for the Local Group dwarf spheroidals

2006 ◽  
Vol 367 (1) ◽  
pp. 387-399 ◽  
Author(s):  
J. I. Read ◽  
M. I. Wilkinson ◽  
N. W. Evans ◽  
G. Gilmore ◽  
J. T. Kleyna
Keyword(s):  
Local Group ◽  
Dwarf Spheroidals

scholarly journals THE SIGNATURE OF GALACTIC TIDES IN LOCAL GROUP DWARF SPHEROIDALS

2009 ◽  
Vol 698 (1) ◽  
pp. 222-232 ◽  
Author(s):  
Jorge Peñarrubia ◽  
Julio F. Navarro ◽  
Alan W. McConnachie ◽  
Nicolas F. Martin
Keyword(s):  
Local Group ◽  
Dwarf Spheroidals

scholarly journals Local group star formation in warm and self-interacting dark matter cosmologies

2020 ◽  
Vol 498 (1) ◽  
pp. 702-717 ◽  
Author(s):  
Mark R Lovell ◽  
Wojciech Hellwing ◽  
Aaron Ludlow ◽  
Jesús Zavala ◽  
Andrew Robertson ◽  
...  
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Galaxy Formation ◽  
Cold Dark Matter ◽  
Local Group ◽  
Initial Density ◽  
Dark Matter Mass ◽  
Stellar Ages ◽  
Hydrodynamical Simulations ◽  
Star Formation Histories

ABSTRACT The nature of the dark matter can affect the collapse time of dark matter haloes, and can therefore be imprinted in observables such as the stellar population ages and star formation histories of dwarf galaxies. In this paper, we use high-resolution hydrodynamical simulations of Local Group-analogue (LG) volumes in cold dark matter (CDM), sterile neutrino warm dark matter (WDM) and self-interacting dark matter (SIDM) models with the eagle galaxy formation code to study how galaxy formation times change with dark matter model. We are able to identify the same haloes in different simulations, since they share the same initial density field phases. We find that the stellar mass of galaxies depends systematically on resolution, and can differ by as much as a factor of 2 in haloes of a given dark matter mass. The evolution of the stellar populations in SIDM is largely identical to that of CDM, but in WDM early star formation is instead suppressed. The time at which LG haloes can begin to form stars through atomic cooling is delayed by ∼200 Myr in WDM models compared to CDM. It will be necessary to measure stellar ages of old populations to a precision of better than 100 Myr, and to address degeneracies with the redshift of reionization – and potentially other baryonic processes – in order to use these observables to distinguish between dark matter models.

scholarly journals Morphological Characteristics of Compact High-Velocity Clouds Revealed by High-Resolution WSRT Imaging

2000 ◽  
Vol 174 ◽  
pp. 136-147
Author(s):  
W. B. Burton ◽  
R. Braun
Keyword(s):  
Dark Matter ◽  
High Resolution ◽  
High Velocity ◽  
Physical State ◽  
Local Group ◽  
Morphological Characteristics ◽  
Kinetic Temperature ◽  
High Resolution Imaging ◽  
Resolution Imaging ◽  
High Velocity Clouds

AbstractA class of compact, isolated high–velocity clouds which plausibly represents a homogeneous subsample of the HVC phenomenon in a single physical state was objectively identified by Braun and Burton (1999). Six examples of the CHVCs, unresolved in single–dish data, have been imaged with the Westerbork Synthesis Radio Telescope. The high–resolution imaging reveals the morphology of these objects, including a core/halo distribution of fluxes, signatures of rotation indicating dark matter, and narrow linewidths constraining the kinetic temperature of several opaque cores. In these regards, as well as in their kinematic and spatial deployment on the sky, the CHVC objects are evidently a dynamically cold ensemble of dark–matter–dominated H ɪ clouds accreting onto the Local Group in a continuing process of galactic evolution.

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