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Date and Time of the Query: 2019-04-19 T17:59:05 PDT
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For refcode 2000AJ....120.2884P:
Retrieve 77 NED objects in this reference.
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Copyright by American Astronomical Society. Reproduced by permission
2000AJ....120.2884P MAXIMUM DISK MASS MODELS FOR SPIRAL GALAXIES POVILAS PALUNAS Laboratory for Astronomy and Solar Physics, NASA/Goddard Space Flight Center, Greenbelt, MD 20771; palunas@gsfc.nasa.gov AND T. B. WILLIAMS Department of Physics and Astronomy, Rutgers University, Box 0849, Piscataway, NJ 08855-0849; williams@physics.rutgers.edu Received 1996 December 2; accepted 2000 September 6 ABSTRACT We present axisymmetric maximum disk mass models for a sample of 74 spiral galaxies taken from the southern sky Fabry-Perot Tully-Fisher survey by Schommer et al. The sample contains galaxies spanning a large range of morphologies and having rotation widths from 180 km s^-1^ to 680 km s^-1^. For each galaxy we have an I-band image and a two-dimensional H{alpha} velocity field. We decompose the disk and bulge by fitting models directly to the I-band image. This method utilizes both the distinct surface brightness profiles and shapes of the projected disk and bulge in the galaxy images. The luminosity profiles and rotation curves are derived using consistent centers, position angles, and inclinations derived from the photometry and velocity maps. The distribution of mass is modeled as a sum of disk and bulge components with distinct, constant mass-to-light ratios. No dark matter halo is included in the fits. The models reproduce the overall structure of the rotation curves in the majority of galaxies, providing good fits to galaxies that exhibit pronounced structural differences in their surface brightness profiles. Of galaxies for which the rotation curve is measured to R_23.5_ or beyond 75% are well fitted by a mass-traces-light model for the entire region within R_23.5_. The models for about 20% of the galaxies do not fit well; the failure of most of these models is traced directly to nonaxisymmetric structures, primarily bars but also strong spiral arms. The median I-band M/L of the disk plus bulge is 2.4 +/- 0.9 h_75_ in solar units, consistent with normal stellar populations. These results require either that the mass of dark matter within the optical disk of spiral galaxies is small or that its distribution is very precisely coupled to the distribution of luminous matter. Key words: galaxies: fundamental parameters-galaxies: halos -galaxies: kinematics and dynamics-galaxies: photometry -galaxies: spiral-galaxies: structure
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