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The 3-dimensional structure of NGC 891 and M51

Published online by Cambridge University Press:  17 August 2012

Andrew Schechtman-Rook ,
Matthew A. Bershady ,
Kenneth Wood  and
Thomas P. Robitaille
Andrew Schechtman-Rook
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, 425 N. Charter St., Madison, WI 53706 email: [email protected], [email protected]
Matthew A. Bershady
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, 425 N. Charter St., Madison, WI 53706 email: [email protected], [email protected]
Kenneth Wood
Affiliation:
Department of Astronomy, University of Wisconsin-Madison, 425 N. Charter St., Madison, WI 53706 email: [email protected], [email protected] School of Physics & Astronomy, University of St Andrews, North Haugh, StAndrews, Fife, Scotland, KY16 9SS email: [email protected]
Thomas P. Robitaille
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138 email: [email protected]
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Abstract

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We investigate the three-dimensional structure of the nearby edge-on spiral galaxy NGC 891 using 3D Monte Carlo radiative transfer models, with realistic spiral structure and fractally clumped dust. Using the spiral and clumpiness parameters found from recently completed scattered light models we produce lower resolution SED models which reproduce the spatially-integrated UV-to-FIR SED of NGC 891. Our models contain a color gradient across the major axis of the galaxy - similar to what is seen in images of the NGC 891. With minor adjustment our SED models are able to match the SED of M51, a similar galaxy at a near face-on inclination.

Keywords

radiative transfergalaxies: ISMgalaxies: spiralgalaxies: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S284: The Spectral Energy Distribution of Galaxies , September 2011 , pp. 104 - 106
Copyright
Copyright © International Astronomical Union 2012

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