Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.mso.anu.edu.au/~kcf/surya/spiralstructure/kregel05 Дата изменения: Mon Mar 26 18:09:53 2007 Дата индексирования: Sun Apr 10 07:19:38 2016 Кодировка: Поисковые слова: spiral galaxy

Mon. Not. R. Astron. Soc. 000, 1­?? (2004)

Printed 26 March 2007

A (MN L TEX style file v2.2)

Structure and kinematics of edge-on galaxy discs ­ V. The dynamics of the stellar discs.
M. Kregel1, P. C. van der Kruit 1
1

and K. C. Freeman2

arXiv:astro-ph/0501503v1 24 Jan 2005

Kapteyn Astronomical Institute, University of Groningen, P.O.Box 800, 9700AV Groningen, the Netherlands Research School for Astronomy & Astrophysics, Mount Stromlo Observatory, The Australian National University, Private Bag, Weston Creek, 2611 Canberra, Australia
2

Accepted. Received.

ABSTRACT

In earlier papers in this series we determined the intrinsic stellar disc kinematics of fifteen intermediate to late type edge-on spiral galaxies using a dynamical modeling technique. The sample covers a substantial range in maximum rotation velocity and depro jected face-on surface brightness, and contains seven spirals with either a boxyor peanut-shaped bulge. Here we discuss the structural, kinematical and dynamical properties. From the photometry we find that intrinsically more flattened discs tend to have a lower face-on central surface brightness and a larger dynamical mass-to-light ratio. This observation suggests that at a constant maximum rotational velocity lower surface brightness discs have smaller vertical stellar velocity dispersions. Although the individual uncertainties are large, we find from the dynamical modeling that at least twelve discs are submaximal. The average disc contributes 53±4 percent to the observed rotation at 2.2 disc scalelengths (hR ), with a 1 scatter of 15 percent. This percentage becomes somewhat lower when effects of finite disc flattening and gravity by the dark halo and the gas are taken into account. Since boxy and peanut-shaped bulges are probably associated with bars, the result suggests that at 2.2hR the submaximal nature of discs is independent of barredness. The possibility remains that very high surface brightness discs are maximal, as these discs are underrepresented in our sample. We confirm that the radial stellar disc velocity dispersion is related to the galaxy maximum rotational velocity. The scatter in this - vmax relation appears to correlate with the disc flattening, face-on central surface brightness and dynamical mass-to-light ratio. Low surface brightness discs tend to be more flattened and have smaller stellar velocity dispersions. The findings are consistent with the observed correlation between disc flattening and dynamical mass-to-light ratio and can generally be reproduced by the simple collapse theory for disc galaxy formation. Finally, the disc mass Tully-Fisher relation is offset from the maximum-disc scaled stellar mass Tully-Fisher relation of the Ursa Ma jor cluster. This offset, -0.3 dex in mass, is naturally explained if the discs of the Ursa Ma jor cluster spirals are submaximal. surface brightness discs. This paper has been accepted for publication by MNRAS and is available in pdf-format at the following URL: http://www.astro.rug.nl/vdkruit/jea3/homepage/paperV.pdf. Key words: galaxies: fundamental parameters ­ galaxies: kinematics and dynamics ­ galaxies: spiral ­ galaxies: structure



E-mail: vdkruit@astro.rug.nl