Issue |
A&A
Volume 488, Number 3, September IV 2008
|
|
---|---|---|
Page(s) | 969 - 973 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:200810232 | |
Published online | 17 July 2008 |
Diffuse interstellar bands in RAVE survey spectra*
1
INAF Osservatorio Astronomico di Padova, Asiago, Italy e-mail: ulisse.munari@oapd.inaf.it
2
Observatoire de Strasbourg, Strasbourg, France
3
Rudolf Pierls Center for Theoretical Physics, University of Oxford, UK
4
Institute of Astronomy, School of Physics, University of Sydney, Australia
5
Astrophysikalisches Institut Potsdam, Potsdam, Germany
6
Macquarie University, Sidney, Australia
7
RSAA Mount Stromlo Observatory, Camberra, Australia
8
University of Central Lancashire, Preston, UK
9
Institute of Astronomy, University of Cambridge, UK
10
Astronomisches Rechen-Institut, Center for Astronomy of the University of Heidelberg, Heidelberg, Germany
11
University of Groningen, Groningen, The Netherlands
12
University of Victoria, Victoria, Canada
13
e2v Centre for Electronic Imaging, School of Engineering and Design, Brunel University, Uxbridge, UK
14
Anglo Australian Observatory, Sydney, Australia
15
Johns Hopkins University, Baltimore, Maryland, USA
16
Faculty of Mathematics and Physics, University of Ljubljana, Ljubljana, Slovenia
Received:
21
May
2008
Accepted:
9
July
2008
We have used spectra of hot stars from the RAVE Survey in
order to investigate the visibility and properties of five
diffuse interstellar bands previously reported in the
literature. The RAVE spectroscopic survey for Galactic
structure and kinematics records CCD spectra covering the
8400–8800 Å wavelength region at 7500 resolving power. The
spectra are obtained with the UK Schmidt at the AAO, equipped with the 6dF
multi-fiber positioner. The DIB at 8620.4 Å is by far the
strongest and cleanest of all DIBs occurring within the RAVE
wavelength range, with no interference by underlying
absorption stellar lines in hot stars. It correlates so
tightly with reddening that it turns out to be a reliable
tool to measure it, following the relation (Å), valid throughout the general
interstellar medium of our Galaxy. The presence of a DIB at
8648 Å is confirmed. Its intensity appears unrelated to
reddening, in agreement with scanty and preliminary reports
available in the literature, and its measurability is
strongly compromised by severe blending with underlying
stellar He I doublet at 8649 Å. The two weak DIBs at 8531
and 8572 Å do not appear real and should actually be
blends of underlying stellar lines. The very weak DIB at
8439 Å cannot be resolved within the profile of the much
stronger underlying hydrogen Paschen 18 stellar line.
Key words: ISM: general / ISM: lines and bands / surveys
© ESO, 2008
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