A New Technique for Mapping the Structure of the Stellar Bar and Disk of the Milky Way Galaxy

Details A New Technique for Mapping the Structure of the Stellar Bar and Disk of the Milky Way Galaxy A New Technique for Mapping the Structure of the Stellar Bar and Disk of the Milky Way Galaxy

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21821704b&link_type=abstract

American Astronomical Society, AAS Meeting #218, #217.04; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

Using data from the Spitzer Space Telescope GLIMPSE/Legacy project, 2MASS, and the UKIDSS Galactic plane survey, I present a new diagnostic diagram for identifying large scale stellar structures in the Milky Way Galaxy: the "longitude-magnitude" diagram. This is obtained by plotting the slopes of infared point source histogram as a function of longitude (or latitude) and magnitude. Because most sources brighter than m=12 are giants, common classes of giants, such as red clump giants, asymptotic giant branch bump, and the tip of red giant branch produce detectable changes of slopes in the source histograms. For large-scale overensities or underdensities in the Galaxy, the apparent magnitude of the inflections in these histograms changes with longitude, allowing one to map the distance to the regions of stellar over-density in the Galaxy. I demonstrate that this technique recreates previous results on the Galactic Long Bar and Triaxial Bulge and present new results on the "truncation" and warp of the stellar disk. The observed longitude-magnitude plots are also compared with synthetic longitude-magnitude plots produced with the TRILEGAL and Besancon stellar population synthesis models.

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