Kinematic Signs of Halo Substructure in Spiral Galaxies

Details Kinematic Signs of Halo Substructure in Spiral Galaxies Kinematic Signs of Halo Substructure in Spiral Galaxies

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aspc..421..259h&link_type=abstract

Galaxies in Isolation: Exploring Nature Versus Nurture, proceedings of a conference held 12 to 15 May 2009 in Granada, Spain. Ed

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the results from a kinematic study of planetary nebulae (PNe) in five face-on spiral galaxies: IC 342, M74, M83, M94, and M101. We find that in the inner regions of the galaxies, the vertical velocity dispersion (σz) generally falls off exponentially with the light, as expected for a constant mass-to-light ratio (M/L), constant scale height (hz) disk. However, beyond three optical scale lengths (hR), σz asymptotes out at roughly 20 km s-1. Our analysis finds evidence for significant flaring in the outer regions as well, especially in M94. Our observations are in excellent agreement with predictions derived from models of disk heating by halo substructure.

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