Connections between Internal Galaxy Kinematics, HI Line Widths, and the Cosmic Distance Scale

Details Connections between Internal Galaxy Kinematics, HI Line Widths, and the Cosmic Distance Scale Connections between Internal Galaxy Kinematics, HI Line Widths, and the Cosmic Distance Scale

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...20710505s&link_type=abstract

American Astronomical Society Meeting 207, #105.05; Bulletin of the American Astronomical Society, Vol. 37, p.1336

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Scientific paper

21 cm line profiles for spiral galaxies are essential for understanding the internal kinematics and gas distribution in spiral galaxies. In addition, the velocity width is used in the magnitude-velocity width (Tully-Fisher) relation. In order to better understand the dispersion in the Tully-Fisher relation, and to gain a better understanding of how 21 cm line profiles are affected by internal velocity dispersion, rotation curve shapes, turbulence, warps, high-velocity clouds, telescope pointing errors, inclination, and other effects, we have created a model that simulates neutral hydrogen in galaxies. Synthetic emission line profiles generated from the model are compared to a sample of galaxies observed with both the Robert C. Byrd Green Bank Telescope (GBT) and the Giant Metrewave Radio Telescope (GMRT). The results of our simulations can be used to better understand deviations from the Magnitude-velocity width (Tully-Fisher) relation. In addition, our results should allow for an increased understanding of gas distribution and kinematics merely from studying single-dish line profile shapes. The results from the simulation should lead to a better empirical correction for inclination effects.

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