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Decoding 3D Disk Structure and Dynamics Using Doppler Tomography

Published online by Cambridge University Press:  09 February 2015

Arthur D. Eigenbrot  and
Matthew A. Bershady
Arthur D. Eigenbrot
Affiliation:
Department of Astronomy, University of Wisconsin - Madison, 475 N. Charter St. Madison, WI, 53703, USA email: eigenbrot@astro.wisc.edu
Matthew A. Bershady
Affiliation:
Department of Astronomy, University of Wisconsin - Madison, 475 N. Charter St. Madison, WI, 53703, USA email: eigenbrot@astro.wisc.edu
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Abstract

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We demonstrate a method to measure both rotation curves and 3D ISM structure in edge-on galaxies. Two-dimensional spectral coverage of edge-on galaxies reveals substantial deviations in emission line shapes from a purely gaussian profile that vary with radius and height. Non-gaussianity is quantified using statistical moments to third order. We infer the 3D density distribution by comparing the measured line profiles to synthetic line-of-sight velocity distributions from a suite of three-dimensional galaxy models with different 3D distributions of dust and gas and different rotation curve shapes and amplitudes. We apply this method using multi-position longslit data of nearby edge-on galaxy ESO 435-G25 and find our derived rotation curve matches measured HI rotation from envelope fitting but requires a flared dust disk to accurately describe the radial and vertical trends in the measured statistical moments. Our results are consistent with dynamical expectations for constant pressure support in a disk with exponentially declining surface-density.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Issue S309: Galaxies in 3D across the Universe , July 2014 , pp. 311
Copyright
Copyright © International Astronomical Union 2015 

References

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