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Issue A&A
Volume 471, Number 3, September I 2007
Page(s) 865 - 872
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20077381



A&A 471, 865-872 (2007)
DOI: 10.1051/0004-6361:20077381

Abundances of planetary nebula M 1-42

S. R. Pottasch1, J. Bernard-Salas2, and T. L. Roellig3

1  Kapteyn Astronomical Institute, PO Box 800, 9700 AV Groningen, The Netherlands
    e-mail: pottasch@astro.rug.nl
2  Center for Radiophysics and Space Research, Cornell University, Ithaca, NY 14853, USA
3  NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035-1000, USA

(Received 1 March 2007 / Accepted 19 June 2007)

Abstract
The spectra of the planetary nebula M 1-42 is reanalysed using spectral measurements made in the mid-infrared with the Spitzer Space Telescope. The aim is to determine the chemical composition of this object. We also make use of ISO, IUE and ground based spectra. Abundances determined from the mid- and far-infrared lines, which are insensitive to electron temperature, are used as the basis for the determination of the composition, which are found to substantially differ from earlier results. High values of neon, argon and sulfur are found. They are higher than in other PN, with the exception of NGC 6153, a nebula of very similar abundances. The high values of helium and nitrogen found indicate that the second dredge-up and hot bottom burning has occurred in the course of evolution and that the central star was originally more massive than 4 $M_{\odot}$. The present temperature and luminosity of the central star is determined and at first sight may be inconsistent with such a high mass.


Key words: ISM: abundances -- planetary nebulae: individual: M 1-42 -- infrared: ISM



© ESO 2007


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