The Flattened Dark Matter Halo of NGC 4244

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dc.creatorOlling, Rob P.
dc.date1996-10-30
dc.date.accessioned2026-07-07T02:22:12Z
dc.date.available2026-07-07T02:22:12Z
dc.descriptionIn a previous paper (Olling 1995, astro-ph/9505002) a method was developed to determine the shapes of dark matter halos of spiral galaxies from an accurate determination of the rotation curve, the flaring of the gas layer and the velocity dispersion in the HI. Here I report the results for the almost edge-on Scd galaxy NGC 4244 (Olling 1996a,astro-ph/9605110; 1996b, astro-ph/9605111). The observed flaring of the HI beyond the optical disk puts significant constraints on the shape of the dark matter halo, which are almost independent of the stellar mass-to-light ratio. NGC 4244's dark matter halo is found to be highly flattened with a shortest-to-longest axis ratio of 0.2 (-0.1,+0.3). If the dark matter is disk-like, the data presented in this paper imply that the vertical velocity dispersion of the dark matter must be 10% - 30% larger than the measured tangential dispersion in the HI.
dc.description8 pages LaTeX, including 3 figures. Uses paspconf.sty and epsf.sty. To appear in "Dark and Visible Matter in Galaxies and Cosmological Implications," eds. M. Persic and P. Salucci, A.S.P. Conference Series. 1997
dc.identifierhttps://arxiv.org/abs/astro-ph/9610249
dc.identifierhttp://arxiv.org/abs/astro-ph/9610249
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/10787
dc.subjectAstrophysics
dc.titleThe Flattened Dark Matter Halo of NGC 4244
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