The Non-axisymmetric Distribution of Stars and Dust in the Milky Way

Details The Non-axisymmetric Distribution of Stars and Dust in the Milky Way The Non-axisymmetric Distribution of Stars and Dust in the Milky Way

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.6206d&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #62.06; Bulletin of the American Astronomical Society, Vol. 31, p.1464

Astronomy and Astrophysics

Astronomy

Scientific paper

Using far-infrared (FIR) and near-infrared (NIR) data from the COBE/DIRBE instrument for Galactic latitudes |b| < 30 degrees, we model the stellar and dust distribution in the Galactic plane. Making the assumption that the Galaxy is transparent in the 240 μ FIR waveband, the dust emission can be modeled using the following components: a warped exponential disk with scale length 0.30 Rsun and scale height 0.017 Rsun, an spiral arm component, and a feature coinciding with the local (Orion) arm that produces prominent emission features at l = 80 and -100 degrees. The dust distribution is used to calculate absorbtion at the NIR J and K wavebands, while stellar emission in these wavebands is modeled with two components: a warped exponential disk with a scale length of 0.27 Rsun and scale height of 0.029 Rsun, and from a spiral arm component. The warp is evident in both the dust and stellar component, and starts within the Solar Circle. In the FIR (dust) emission, the spiral arms are well described by their mapping with the HII regions, which shows four arms, whereas in the NIR the (stellar) emission can be well described by a two-armed logarithmic spiral with a pitch angle of 13.7 degrees.

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