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Astron. Astrophys. 327, 1194-1205


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On the distance to the Chamaeleon I and II associations

D.C.B. Whittet1,2, T. Prusti3, G.A.P. Franco4, P.A. Gerakines1,5, D. Kilkenny6, K.A. Larson1, and P.R. Wesselius2

1Department of Physics, Applied Physics & Astronomy, Rensselaer Polytechnic Institute, Troy, NY 12180-3590, USA
2SRON, P.O. Box 800, 9700 AV Groningen, The Netherlands
3ISO Science Operations Centre, Astrophysics Division, ESA, Villafranca del Castillo, P.O. Box 50727, E-28080 Madrid, Spain
4Departamento de Física - ICEx - UFMG, Caixa Postal 702, 30.161-970 - Belo Horizonte - MG, Brasil
5Leiden Observatory, P.O. Box 9513, 2300 RA Leiden, The Netherlands
6SAAO, P.O. Box 9, Observatory, Cape 7935, South Africa

Received 23 December 1996 / Accepted 25 June 1997

Abstract

Constraints on the distances to the dark clouds Chamaeleon I and II are investigated in detail. A compilation of photometric data, spectral types and absolute magnitudes for field stars towards each cloud is presented, and results are used to examine the distribution of reddening with distance along each line of sight. The distances to stars associated with reflection nebulae in each cloud are examined in detail. On the basis of these results, we deduce the most probable distance of Cha I to be $160\pm15$, and that of 2 to be $178\pm18$. An examination of the mean fluxes of T Tauri stars in each cloud provides independent evidence to suggest that 2 is significantly more distant than Cha I. Both clouds appear to be embedded in a macroscopic sheet-like structure extending over much of the Chamaeleon-Musca-Crux region. The Chamaeleon III and DC300.2-16.9 clouds are probably part of the same structure, with probable distances $\sim$140-160.

Key words: stars: distances - ISM: clouds; dust, extinction; Chamaeleon clouds; reflection nebulae

Send offprint requests to: D.C.B. Whittet


© European Southern Observatory (ESO) 1997

Online publication: October 20, 1997
Last change: April 6, 1998
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