Dark Matter Halos of Disk Galaxies: Constraints from the Tully‐Fisher Relation

2007 ◽  
Vol 671 (2) ◽  
pp. 1115-1134 ◽  
Author(s):  
Oleg Y. Gnedin ◽  
David H. Weinberg ◽  
James Pizagno ◽  
Francisco Prada ◽  
Hans‐Walter Rix
Keyword(s):  
Dark Matter ◽  
Disk Galaxies ◽  
Dark Matter Halos ◽  
Fisher Relation

Constraints on the Clumpiness of Dark Matter Halos Through Heating of Disk Galaxies

2003 ◽  
Vol 10 ◽  
pp. 95-95
Author(s):  
E. Ardi ◽  
T. Tsuchiya ◽  
A. Burkert
Keyword(s):  
Dark Matter ◽  
Disk Galaxies ◽  
Dark Matter Halos

scholarly journals DARK MATTER HALOS AND EVOLUTION OF BARS IN DISK GALAXIES: VARYING GAS FRACTION AND GAS SPATIAL RESOLUTION

2010 ◽  
Vol 719 (2) ◽  
pp. 1470-1480 ◽  
Author(s):  
Jorge Villa-Vargas ◽  
Isaac Shlosman ◽  
Clayton Heller
Keyword(s):  
Dark Matter ◽  
Spatial Resolution ◽  
Disk Galaxies ◽  
Dark Matter Halos

scholarly journals How the first stars shaped the faintest gas-dominated dwarf galaxies

2015 ◽  
Vol 11 (S317) ◽  
pp. 360-361
Author(s):  
Robbert Verbeke ◽  
Bert Vandenbroucke ◽  
Sven De Rijcke
Keyword(s):  
Dark Matter ◽  
Dwarf Galaxies ◽  
Ultra Violet ◽  
Mass Range ◽  
Dark Matter Halos ◽  
First Stars ◽  
Star Forming ◽  
Neutral Gas ◽  
Entire Mass Range ◽  
Fisher Relation

AbstractCosmological simulations predict that dark matter halos with circular velocities lower than 30 km/s should have lost most of their neutral gas by heating of the ultra-violet background. This is in stark contrast with gas-rich galaxies such as e.g. Leo T, Leo P and Pisces A, which all have circular velocities of ~15 km/s (Ryan-Weber et al. 2008, Bernstein-Cooper et al. 2014, Tollerud et al. 2015). We show that when we include feedback from the first stars into our models, simulated dwarfs have very different properties at redshift 0 than when this form of feedback is not included. Including this Population-III feedback leads to galaxies that lie on the baryonic Tully-Fisher relation over the entire mass range of star forming dwarf galaxies, as well as reproducing a broad range of other observational properties.

scholarly journals The Angular Momentum Dichotomy

2014 ◽  
Vol 10 (S309) ◽  
pp. 349-349
Author(s):  
Adelheid Teklu ◽  
Rhea-Silvia Remus ◽  
Klaus Dolag ◽  
Andreas Burkert
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Lognormal Distribution ◽  
Spiral Galaxies ◽  
Disk Galaxies ◽  
Dark Matter Halos ◽  
Central Galaxy ◽  
Relative Angular Momentum ◽  
Spin Parameter ◽  
Spheroidal Galaxies

AbstractIn the context of the formation of spiral galaxies the evolution and distribution of the angular momentum of dark matter halos have been discussed for more than 20 years, especially the idea that the specific angular momentum of the halo can be estimated from the specific angular momentum of its disk (e.g. Fall & Efstathiou (1980), Fall (1983) and Mo et al. (1998)). We use a new set of hydrodynamic cosmological simulations called Magneticum Pathfinder which allow us to split the galaxies into spheroidal and disk galaxies via the circularity parameter ϵ, as commonly used (e.g. Scannapieco et al. (2008)). Here, we focus on the dimensionless spin parameter λ = J |E|1/2 / (G M5/2) (Peebles 1969, 1971), which is a measure of the rotation of the total halo and can be fitted by a lognormal distribution, e.g. Mo et al. (1998). The spin parameter allows one to compare the relative angular momentum of halos across different masses and different times. Fig. 1 reveals a dichotomy in the distribution of λ at all redshifts when the galaxies are split into spheroids (dashed) and disk galaxies (dash-dotted). The disk galaxies preferentially live in halos with slightly larger spin parameter compared to spheroidal galaxies. Thus, we see that the λ of the whole halo reflects the morphology of its central galaxy. For more details and a larger study of the angular momentum properties of disk and spheroidal galaxies, see Teklu et al. (in prep.).

scholarly journals Constraints of the Clumpiness of Dark Matter Halos through Heating of the Disk Galaxies

2003 ◽  
Vol 596 (1) ◽  
pp. 204-215 ◽  
Author(s):  
Eliani Ardi ◽  
Toshio Tsuchiya ◽  
Andreas Burkert
Keyword(s):  
Dark Matter ◽  
Disk Galaxies ◽  
Dark Matter Halos

scholarly journals Lenticular vs spiral galaxies: dark matter content and the Tully-Fisher relation

2009 ◽  
Vol 5 (H15) ◽  
pp. 82-82
Author(s):  
M. Bureau ◽  
M. J. Williams ◽  
M. Cappellari
Keyword(s):  
Dark Matter ◽  
Galaxy Evolution ◽  
Spiral Galaxies ◽  
Matter Content ◽  
Disk Galaxies ◽  
Observational Constraints ◽  
Modelling Techniques ◽  
Fisher Relation ◽  
Local Edge ◽  
Zero Points

We provide observational constraints on disk galaxy evolution for a sample of 28 local edge-on early-type (S0–Sb) disk galaxies. We do this in two ways: (i) we use simple dynamical modelling techniques to constrain their stellar and dark matter content (Williams et al. 2009) and (ii) we compare the zero points of the Tully-Fisher relations (TFRs; Tully & Fisher 1977) of the spirals and S0s.

scholarly journals The Structure of Cold Dark Matter Halos

1996 ◽  
Vol 171 ◽  
pp. 255-258 ◽  
Author(s):  
Julio F. Navarro
Keyword(s):  
Dark Matter ◽  
Cold Dark Matter ◽  
Large Range ◽  
Disk Galaxies ◽  
Dark Matter Halos ◽  
Density Profiles ◽  
Halo Structure ◽  
Disk Rotation ◽  
Disk Mass ◽  
The Masses

High resolution N-body simulations show that the density profiles of dark matter halos formed in the standard CDM cosmogony can be fit accurately by scaling a simple “universal” profile. Regardless of their mass, halos are nearly isothermal over a large range in radius, but significantly shallower than r–2 near the center and steeper than r–2 in the outer regions. The characteristic overdensity of a halo correlates strongly with halo mass in a manner consistent with the mass dependence of the epoch of halo formation. Matching the shape of the rotation curves of disk galaxies with this halo structure requires (i) disk mass-to-light ratios to increase systematically with luminosity, (ii) halo circular velocities to be systematically lower than the disk rotation speed, and (iii) that the masses of halos surrounding bright galaxies depend only weakly on galaxy luminosity. This offers an attractive explanation for the puzzling lack of correlation between luminosity and dynamics in observed samples of binary galaxies and of satellite companions of bright spiral galaxies, suggesting that the structure of dark matter halos surrounding bright spirals is similar to that of cold dark matter halos.

scholarly journals DARK MATTER HALOS OF BARRED DISK GALAXIES

2015 ◽  
Vol 807 (1) ◽  
pp. 111 ◽  
Author(s):  
Bernardo Cervantes Sodi ◽  
Cheng Li ◽  
Changbom Park
Keyword(s):  
Dark Matter ◽  
Disk Galaxies ◽  
Dark Matter Halos

scholarly journals The dark matter density problem in massive disk galaxies

2004 ◽  
Vol 220 ◽  
pp. 265-270 ◽  
Author(s):  
Benjamin J. Weiner
Keyword(s):  
Dark Matter ◽  
Angular Momentum ◽  
Momentum Transfer ◽  
Matter Density ◽  
Disk Galaxies ◽  
Dark Matter Halos ◽  
Barred Galaxies ◽  
Dark Matter Density ◽  
Disk Mass ◽  
Density Problem

We discuss measurements of disk mass from non-circular streaming motions of gas in the barred galaxies NGC 3095 and NGC 4123. in these galaxies with strong shocks and non-circular motions, the inner regions must be disk-dominated to reproduce the shocks. This requires dark matter halos of low central density and low concentration, compared to LCDM halo predictions. in addition, the baryonic collapse to a disk should have compressed the halo and increased the dark matter density, which sharpens the disagreement. One possible resolution is a substantial amount of angular momentum transfer from disk to halo, but this is not particularly attractive nor elegant.

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