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Distances, depth structure, and kinematics of the Magellanic Clouds from disentangling spectra of eclipsing binaries and Cepheids

Published online by Cambridge University Press:  26 February 2013

P. Hadrava ,
S. Štefl ,
R. Klement  and
C. Martayan
P. Hadrava
Affiliation:
Astronomical Institute, Academy of Sciences, Boční II 1401, CZ 141 31 Praha 4, Czech Republic email: had@sunstel.asu.cas.cz
S. Štefl
Affiliation:
European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile email: sstefl@eso.org, cmartaya@eso.org
R. Klement
Affiliation:
Department of Theoretical Physics and Astrophysics, Masaryk University, CZ 611 37 Brno, Czech Republic email: robertklement@gmail.com
C. Martayan
Affiliation:
European Organisation for Astronomical Research in the Southern Hemisphere, Casilla 19001, Santiago 19, Chile email: sstefl@eso.org, cmartaya@eso.org
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Abstract

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Spectroscopy and photometry of eclipsing binaries and Cepheids (using the Baade–Wesselink method) yield primary distance markers applicable to the Local Group of galaxies. The technique of disentangling spectra has proved helpful in resolving stellar physical parameters. Our method also allows us to disentangle interstellar absorption lines and, thus, to complement the radial-velocity structure of the interstellar medium with an (otherwise unattainable) upper limit to its distance. The mapping of the spatial and kinematic structure of the stellar and interstellar components of the Magellanic Clouds and Stream enables constraining their tidal evolution and, thus, of the mass of the Galaxy.

Keywords

binaries: eclipsingCepheidsISM: kinematics and dynamicsMagellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 231 - 234
Copyright
Copyright © International Astronomical Union 2013

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