2007A&A...461..155R


Query : 2007A&A...461..155R

2007A&A...461..155R - Astronomy and Astrophysics, volume 461, 155-169 (2007/1-1)

Is the dark matter halo of the Milky Way flattened?

RUZICKA A., PALOUS J. and THEIS C.

Abstract (from CDS):

We performed an extended analysis of the parameter space for the interaction of the Magellanic System with the Milky Way (MW). The varied parameters cover the phase space parameters, the masses, the structure, and the orientation of both Magellanic Clouds, as well as the flattening of the dark matter halo of the MW. The analysis was done by a specially adopted optimization code searching for the best match between numerical models and the detailed HI map of the Magellanic System by Bruens et al. (2005A&A...432...45B). The applied search algorithm is a genetic algorithm combined with a code based on the fast, but approximative restricted N-body method. By this, we were able to analyze more than 106 models, which makes this study one of the most extended ones for the Magellanic System. Here we focus on the flattening q of the axially symmetric MW dark matter halo potential, that is studied within the range 0.74≤q≤1.20. We show that creation of a trailing tail (Magellanic Stream) and a leading stream (Leading Arm) is quite a common feature of the Magellanic System-MW interaction, and such structures were modeled across the entire range of halo flattening values. However, important differences exist between the models, concerning density distribution and kinematics of HI, and also the dynamical evolution of the Magellanic System. Detailed analysis of the overall agreement between modeled and observed distribution of neutral hydrogen shows that the models assuming an oblate (q<1.0) dark matter halo of the Galaxy allow for better satisfaction of HI observations than models with other halo configurations.

Abstract Copyright:

Journal keyword(s): methods: N-body simulations - Galaxy: halo - galaxies: interactions - galaxies: Magellanic Clouds

Simbad objects: 16

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Number of rows : 16
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 NGC 55 GiG 00 14 53.602 -39 11 47.86 8.54 8.58 7.87 7.84   ~ 779 2
2 NAME Magellanic Stream HVC 00 32 -30.0           ~ 973 1
3 NAME SGP reg 00 51 26.275 -27 07 41.70           ~ 568 0
4 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 11178 1
5 NGC 300 GiG 00 54 53.4465638304 -37 41 03.168402396 8.83 8.69 8.13 7.46   ~ 1505 2
6 NAME Scl Group GrG 01 00 06 -33 44.2           ~ 509 0
7 NAME Sagittarius Stream St* 02 22 +00.0           ~ 877 0
8 NAME Magellanic Clouds GrG 03 00 -71.0           ~ 7084 0
9 NAME Magellanic Bridge HI 03 11 -77.5           ~ 449 1
10 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 17478 0
11 NAME Magellanic Leading Arm reg 11 26 -82.0           ~ 93 0
12 ACO 1656 ClG 12 59 44.40 +27 54 44.9           ~ 4816 2
13 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 14463 0
14 NAME SDG G 18 55 19.0 -30 32 43   4.5 3.6     ~ 2195 2
15 NGC 7793 GiG 23 57 49.7540045856 -32 35 27.701550744 10.26 9.74 9.28 9.06 9.7 ~ 1108 2
16 NAME Local Group GrG ~ ~           ~ 8415 0

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