Modeling the Bar Component in Dusty Spiral Galaxies

Details Modeling the Bar Component in Dusty Spiral Galaxies Modeling the Bar Component in Dusty Spiral Galaxies

Jul 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aspc..424..261a&link_type=abstract

Proceedings of the 9th International Conference of the Hellenic Astronomical Society, proceedings of a conference held 20-24 Sep

Astronomy and Astrophysics

Astronomy

Scientific paper

We make use of a 3D radiative transfer model of spiral galaxies in order to investigate the effects of a stellar bar component in the morphology of a spiral galaxy. The model galaxy is described by three axisymmetric components (i.e., a stellar disk, a dusty disk and a stellar bulge) and one non-axisymmetric (a stellar bar). The basic characteristics of the stellar bar that are observed in spiral galaxies (e.g. the X-shape central feature and the boxy/peanut shape of the bulge) are well described with our model. Our model is applied on four spiral galaxies (namely, NGC 4013, IC 2531, UGC2048, and the Milky Way) and the geometrical characteristics of the stellar bar (semi-major axis, height and position angle) are determined very accurately. Finally, we also conduct diagnostic studies of how the morphology of the galaxy changes with various geometrical parameters like the inclination angle and the position angle of the galaxy.

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