File Download
  Links for fulltext
     (May Require Subscription)
Supplementary

Article: Precise Radial Velocities of Giant Stars VIII. Testing for the Presence of Planets with CRIRES Infrared Radial Velocities.

TitlePrecise Radial Velocities of Giant Stars VIII. Testing for the Presence of Planets with CRIRES Infrared Radial Velocities.
Authors
Issue Date2015
PublisherEDP Sciences. The Journal's web site is located at http://www.aanda.org
Citation
Astronomy & Astrophysics, 2015, v. 582, p. article no. A54:1-14 How to Cite?
AbstractContext. We have been monitoring 373 very bright (V ≤ 6 mag) G and K giants with high precision optical Doppler spectroscopy for more than a decade at Lick observatory. Our goal was to discover planetary companions around those stars and to better understand planet formation and evolution around intermediate-mass stars. However, in principle long-term g-mode non-radial stellar pulsations or rotating stellar features such as spots could effectively mimic a planetary signal in the radial velocity data. Aims. Our goal is to compare optical and infrared radial velocities for those stars with periodic radial velocity patterns and test for consistency of their fitted radial velocity semi-amplitudes. Thereby, we distinguish processes intrinsic to the star from orbiting companions as reason for the radial velocity periodicity observed in the optical. Methods. Stellar spectra with high spectral resolution have been taken in the H-band with the CRIRES near-infrared spectrograph at ESO’s VLT for twenty stars of our Lick survey. Radial velocities are derived using many deep and stable telluric CO2 lines for precise wavelength calibration. Results. We find that the optical and the near-infrared radial velocities of the giant stars in our sample are consistent. We present detailed results for eight stars in our sample previously reported to have planets or brown dwarf companions. All eight stars passed the infrared test. Conclusions. We conclude that the planet hypothesis provides the best explanation for the periodic radial velocity patterns observed for these giant stars.
Persistent Identifierhttp://hdl.handle.net/10722/215279
ISSN
2014 Impact Factor: 4.378
2015 SCImago Journal Rankings: 2.446

 

DC FieldValueLanguage
dc.contributor.authorTrifonov, TH-
dc.contributor.authorReffert, S-
dc.contributor.authorZechmeister, M-
dc.contributor.authorReiners, A-
dc.contributor.authorQuirrenbach, A-
dc.date.accessioned2015-08-21T13:20:43Z-
dc.date.available2015-08-21T13:20:43Z-
dc.date.issued2015-
dc.identifier.citationAstronomy & Astrophysics, 2015, v. 582, p. article no. A54:1-14-
dc.identifier.issn0004-6361-
dc.identifier.urihttp://hdl.handle.net/10722/215279-
dc.description.abstractContext. We have been monitoring 373 very bright (V ≤ 6 mag) G and K giants with high precision optical Doppler spectroscopy for more than a decade at Lick observatory. Our goal was to discover planetary companions around those stars and to better understand planet formation and evolution around intermediate-mass stars. However, in principle long-term g-mode non-radial stellar pulsations or rotating stellar features such as spots could effectively mimic a planetary signal in the radial velocity data. Aims. Our goal is to compare optical and infrared radial velocities for those stars with periodic radial velocity patterns and test for consistency of their fitted radial velocity semi-amplitudes. Thereby, we distinguish processes intrinsic to the star from orbiting companions as reason for the radial velocity periodicity observed in the optical. Methods. Stellar spectra with high spectral resolution have been taken in the H-band with the CRIRES near-infrared spectrograph at ESO’s VLT for twenty stars of our Lick survey. Radial velocities are derived using many deep and stable telluric CO2 lines for precise wavelength calibration. Results. We find that the optical and the near-infrared radial velocities of the giant stars in our sample are consistent. We present detailed results for eight stars in our sample previously reported to have planets or brown dwarf companions. All eight stars passed the infrared test. Conclusions. We conclude that the planet hypothesis provides the best explanation for the periodic radial velocity patterns observed for these giant stars.-
dc.languageeng-
dc.publisherEDP Sciences. The Journal's web site is located at http://www.aanda.org-
dc.relation.ispartofAstronomy & Astrophysics-
dc.rightsThe original publication is available at [journal web site] or Credit: Author, A&A, vol., page, year, reproduced with permission, © ESO-
dc.rightsCreative Commons: Attribution 3.0 Hong Kong License-
dc.titlePrecise Radial Velocities of Giant Stars VIII. Testing for the Presence of Planets with CRIRES Infrared Radial Velocities.-
dc.typeArticle-
dc.identifier.emailTrifonov, TH: trifonov@hku.hk-
dc.description.naturepublished_or_final_version-
dc.identifier.doi10.1051/0004-6361/201526196-
dc.identifier.hkuros248276-
dc.identifier.volume582-
dc.identifier.spagearticle no. A54:1-
dc.identifier.epage14-
dc.publisher.placeFrance-

Export via OAI-PMH Interface in XML Formats


OR


Export to Other Non-XML Formats