File Download

There are no files associated with this item.

  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Diffuse interstellar band at 8620 å in rave: A new method for detecting the diffuse interstellar band in spectra of cool stars

TitleDiffuse interstellar band at 8620 å in rave: A new method for detecting the diffuse interstellar band in spectra of cool stars
Authors
Keywordslocal interstellar matter
surveys
astrochemistry
dust, extinction
ISM: lines and bands
Issue Date2013
Citation
Astrophysical Journal, 2013, v. 778, n. 2 How to Cite?
AbstractDiffuse interstellar bands (DIBs) are usually observed in spectra of hot stars, where interstellar lines are rarely blended with stellar ones. The need for hot stars is a strong limitation in the number of sightlines we can observe and their distribution in the Galaxy, as hot stars are rare and concentrated in the Galactic plane. We are introducing a new method, where interstellar lines can be observed in spectra of cool stars in large spectroscopic surveys. The method is completely automated and does not require prior knowledge of the stellar parameters. The main step is a construction of the stellar spectrum, which is done by finding other observed spectra that lack interstellar features and are otherwise very similar to the spectrum in question. Such spectra are then combined into a single stellar spectrum template, matching the stellar component of the observed spectrum. We demonstrate the performance of this new method on a sample of 482,430 Radial Velocity Experiment survey spectra. However, many spectra have to be combined (48 on average) in order to achieve a signal-to-noise ratio high enough to measure the profile of the DIB at 8620 Å, hence limiting the spatial information about the interstellar medium. We compare its equivalent width with extinction maps and with Bayesian reddening, calculated for individual stars, and provide a linear relation between the equivalent width and reddening. Separately from the introduced method, we calculate equivalent widths of the DIB in spectra of hot stars with known extinction and compare all three linear relations. © 2013. The American Astronomical Society. All rights reserved..
Persistent Identifierhttp://hdl.handle.net/10722/209013
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266

 

DC FieldValueLanguage
dc.contributor.authorKos, Janez-
dc.contributor.authorZwitter, Tomaž-
dc.contributor.authorGrebel, Eva K.-
dc.contributor.authorBienaymé, Olivier-
dc.contributor.authorBinney, James J.-
dc.contributor.authorBland-Hawthorn, Joss Bland-
dc.contributor.authorFreeman, Kenneth C.-
dc.contributor.authorGibson, Brad K.-
dc.contributor.authorGilmore, Gerard F.-
dc.contributor.authorKordopatis, Georges-
dc.contributor.authorNavarro, Julio F.-
dc.contributor.authorParker, Quentin A.-
dc.contributor.authorReid, Warren A.-
dc.contributor.authorSeabroke, George M.-
dc.contributor.authorSiebert, Arnaud-
dc.contributor.authorSiviero, Alessandro-
dc.contributor.authorSteinmetz, Matthias-
dc.contributor.authorWatson, Fred G.-
dc.contributor.authorWyse, Rosemary F G-
dc.date.accessioned2015-03-23T02:31:09Z-
dc.date.available2015-03-23T02:31:09Z-
dc.date.issued2013-
dc.identifier.citationAstrophysical Journal, 2013, v. 778, n. 2-
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10722/209013-
dc.description.abstractDiffuse interstellar bands (DIBs) are usually observed in spectra of hot stars, where interstellar lines are rarely blended with stellar ones. The need for hot stars is a strong limitation in the number of sightlines we can observe and their distribution in the Galaxy, as hot stars are rare and concentrated in the Galactic plane. We are introducing a new method, where interstellar lines can be observed in spectra of cool stars in large spectroscopic surveys. The method is completely automated and does not require prior knowledge of the stellar parameters. The main step is a construction of the stellar spectrum, which is done by finding other observed spectra that lack interstellar features and are otherwise very similar to the spectrum in question. Such spectra are then combined into a single stellar spectrum template, matching the stellar component of the observed spectrum. We demonstrate the performance of this new method on a sample of 482,430 Radial Velocity Experiment survey spectra. However, many spectra have to be combined (48 on average) in order to achieve a signal-to-noise ratio high enough to measure the profile of the DIB at 8620 Å, hence limiting the spatial information about the interstellar medium. We compare its equivalent width with extinction maps and with Bayesian reddening, calculated for individual stars, and provide a linear relation between the equivalent width and reddening. Separately from the introduced method, we calculate equivalent widths of the DIB in spectra of hot stars with known extinction and compare all three linear relations. © 2013. The American Astronomical Society. All rights reserved..-
dc.languageeng-
dc.relation.ispartofAstrophysical Journal-
dc.subjectlocal interstellar matter-
dc.subjectsurveys-
dc.subjectastrochemistry-
dc.subjectdust, extinction-
dc.subjectISM: lines and bands-
dc.titleDiffuse interstellar band at 8620 å in rave: A new method for detecting the diffuse interstellar band in spectra of cool stars-
dc.typeArticle-
dc.description.naturelink_to_subscribed_fulltext-
dc.identifier.doi10.1088/0004-637X/778/2/86-
dc.identifier.scopuseid_2-s2.0-84887889550-
dc.identifier.volume778-
dc.identifier.issue2-
dc.identifier.eissn1538-4357-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats