Journal
ASTRONOMY & ASTROPHYSICS
Volume 488, Issue 3, Pages 969-U61Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361:200810232
Keywords
ISM : general; ISM : lines and bands; surveys
Categories
Funding
- Astrophysikalisches Institut Potsdam
- Anglo-Australian Observatory
- Australian National University
- University of Basel
- University of Cambridge
- University of Edinburgh
- University of Heidelberg
- Johns Hopkins University
- University of Ljubljana
- Macquarie University
- University of Oxford
- INAF Astronomical Observatory of Padova
- Steward Observatory
- Swinburne University
- University of Utrecht
- University of Victoria
- STFC [PP/E001068/1] Funding Source: UKRI
- Science and Technology Facilities Council [PP/E001068/1, PP/E00105X/1] Funding Source: researchfish
Ask authors/readers for more resources
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 angstrom 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 angstrom 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 E(B-V) = 2.72(+/- 0.03) x EW (angstrom), valid throughout the general interstellar medium of our Galaxy. The presence of a DIB at 8648 angstrom 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 angstrom. The two weak DIBs at 8531 and 8572 angstrom do not appear real and should actually be blends of underlying stellar lines. The very weak DIB at 8439 angstrom cannot be resolved within the profile of the much stronger underlying hydrogen Paschen 18 stellar line.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available