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Astron. Astrophys. 324, 1145-1148 (1997)

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A very reduced upper limit on the interstellar abundance of beryllium *

Guillaume Hébrard 1, Martin Lemoine 2, Roger Ferlet 1 and Alfred Vidal-Madjar 1

1 Institut d'Astrophysique de Paris, CNRS, 98 bis boulevard Arago, F-75014 Paris, France
2 Department of Astronomy & Astrophysics, Enrico Fermi Institute, The University of Chicago, Chicago IL 60637-1433, USA

Received 22 January 1997 / Accepted 24 February 1997

Abstract

We present the results of observations of the [FORMULA] Å interstellar absorption line of 9 Be [FORMULA] in the direction of [FORMULA]  Per. The data were obtained at the Canada-France-Hawaii 3.6m Telescope using the Coudé f/4 Gecko spectrograph at a resolving power [FORMULA] [FORMULA], and a signal-to-noise ratio [FORMULA]. The 9 Be [FORMULA] line is not detected, and we obtain an upper limit on the equivalent width [FORMULA] µÅ. This upper limit is 7 times below the lowest upper limit ever reported hitherto. The derived interstellar abundance is (9 Be/H) [FORMULA], not corrected for the depletion of 9 Be onto interstellar grains; it corresponds to an upper limit [FORMULA] dex on the depletion factor of 9 Be. As such, it argues in favour of models of formation of dust grains in stellar atmospheres.

Key words: ISM: abundances – stars: individual: i Per

* Based on observations collected at the Canada-France-Hawaii Telescope, Hawaii, USA.

Send offprint requests to: G. Hébrard (hebrard@iap.fr)

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© European Southern Observatory (ESO) 1997

Online publication: May 5, 1998

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