The shape of dark matter haloes – V. Analysis of observations of edge-on galaxies

In previous papers in this series, we measured the stellar and H i content in a sample of edge-on galaxies. In the present paper, we perform a simultaneous rotation curve and vertical force field gradient decomposition for five of these edge-on galaxies. The rotation curve decomposition provides a m...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2017-01, Vol.464 (1), p.65-65
Main Authors: Peters, S P C, van der Kruit, P C, Allen, R J, Freeman, K C
Format: Article
Language:English
Subjects:
Astronomy
Dark matter
Decomposition
Dispersion
Error analysis
Galactic halos
Galactic rotation
Galaxies
Halos
Stars & galaxies
Velocity
Vertical forces
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Summary:In previous papers in this series, we measured the stellar and H i content in a sample of edge-on galaxies. In the present paper, we perform a simultaneous rotation curve and vertical force field gradient decomposition for five of these edge-on galaxies. The rotation curve decomposition provides a measure of the radial dark matter potential, while the vertical force field gradient provides a measure of the vertical dark matter potential. We fit dark matter halo models to these potentials. Using our H i self-absorption results, we find that a typical dark matter halo has a less dense core (0.094 plus or minus 0.230 M... pc super( -3)) than that for an optically thin H i model (0.150 plus or minus 0.124 M... pc super( -3)). The H i self-absorption dark matter halo has a longer scale-length R sub( c) of 1.42 plus or minus 3.48 kpc, versus 1.10 plus or minus 1.81 kpc for the optically thin H i model. The median halo shape is spherical at q = 1.0 plus or minus 0.6 for self-absorbing H i, while it is prolate at q = 1.5 plus or minus 0.6 for the optically thin case. Our best results were obtained for ESO 274-G001 and UGC 7321, for which we were able to measure the velocity dispersion in Paper III. These two galaxies have very different halo shapes, with one oblate and one strongly prolate. Overall, we find that the many assumptions required make this type of analysis susceptible to errors. (ProQuest: ... denotes formulae/symbols omitted.)
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stw2101