Volume 531, July 2011
|Number of page(s)||19|
|Section||Interstellar and circumstellar matter|
|Published online||06 June 2011|
Institute of Astronomy, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
2 Astrobiology Group, Leiden Institute of Chemistry, Leiden University, The Netherlands
3 ESA Research and Scientific Support Department, PO Box 299, 2200 - AG Noordwijk, The Netherlands
4 Institut d’ Astrophysique Spatiale, France
5 NASA Ames Research Centre, CA, USA
6 School of Chemistry, The University of Nottingham, University Park, Nottingham, NG7 2RD, UK
Received: 20 December 2010
Accepted: 22 March 2011
Context. The identification of the carriers of diffuse interstellar bands (DIBs) remains one of the long-standing mysteries in astronomy. The detection of a polarisation signal in a DIB profile can be used to distinguish between a dust or gas-phase carrier. The polarisation profile can give additional information on the grain or molecular properties of the absorber.
Aims. To measure the polarisation efficiency of the carriers of the diffuse interstellar bands.
Methods. In order to detect and measure the linear and circular polarisation of the DIBs we observed reddened lines of sight showing continuum polarisation. For this study we selected two stars HD 197770 and HD 194279. We used high-resolution (R ~ 64 000) spectropolarimetry in the wavelength range from 3700 to 10 480 Å with the ESPaDOnS échelle spectrograph mounted at the CFHT.
Results. High S/N and high resolution Stokes V (circular), Q and U (linear) spectra were obtained. We constrained upper limits by a factor of 10 for previously observed DIBs. Furthermore, we analysed ~30 additional DIBs for which no spectropolarimetry data has been obtained before. This included the 9577 Å DIB and the 8621 Å DIB. The former is attributed to the fullerene, which could become aligned in a magnetic field. The latter shows a tight correlation with the amount of dust in the line-of-sight and therefore most likely may show a polarisation signal related the aligned grains.
Conclusions. The lack of polarisation in 45 DIB profiles suggests that none of the absorption lines is induced by a grain-type carrier. The strict upper limits, less than ~0.01%, derived for the observed lines-of-sight imply that if DIBs are due to gas-phase molecules these carriers have polarisation efficiencies which are at least 6 times, and up to 300 times, smaller than those predicted for grain-related carriers.
Key words: astrochemistry / polarization / dust, extinction / ISM: lines and bands / ISM: molecules
Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientique of France, and the University of Hawaii.
Appendices are available in electronic form at http://www.aanda.org
Intensity and polarisation spectra are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (184.108.40.206) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/531/A25
© ESO, 2011
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