Radial-velocity of CARMENES M dwarfs Virtual Observatory Resource

Authors
  1. Tal-Or L.
  2. Zechmeister M.
  3. Reiners A.
  4. Jeffers S.V.
  5. Schoefer P.,Quirrenbach A.
  6. Amado P.J.
  7. Ribas I.
  8. Caballero J.A.
  9. Aceituno J.,Bauer F.F.
  10. Bejar V.J.S.
  11. Czesla S.
  12. Dreizler S.
  13. Fuhrmeister B.,Hatzes A.P.
  14. Johnson E.N.
  15. Kurster M.
  16. Lafarga M.
  17. Montes D.,Morales J.C.
  18. Reffert S.
  19. Sadegi S.
  20. Seifert W.
  21. Shulyak D.
  22. Published by
    CDS
Abstract

Previous simulations predicted the activity-induced radial-velocity (RV) variations of M dwarfs to range from ~1cm/s to ~1km/s, depending on various stellar and activity parameters. We investigate the observed relations between RVs, stellar activity, and stellar parameters of M dwarfs by analyzing CARMENES high-resolution visual-channel spectra (0.5-1um), which were taken within the CARMENES RV planet survey during its first 20 months of operation. During this time, 287 of the CARMENES- sample stars were observed at least five times. From each spectrum we derived a relative RV and a measure of chromospheric Halpha emission. In addition, we estimated the chromatic index (CRX) of each spectrum, which is a measure of the RV wavelength dependence. Despite having a median number of only 11 measurements per star, we show that the RV variations of the stars with RV scatter of >10m/s and a projected rotation velocity vsini>2km/s are caused mainly by activity. We name these stars 'active RV-loud stars' and find their occurrence to increase with spectral type: from ~3% for early-type M dwarfs (M0.0-2.5V) through ~30% for mid-type M dwarfs (M3.0-5.5V) to >50% for late-type M dwarfs (M6.0-9.0V). Their RV-scatter amplitude is found to be correlated mainly with vsini. For about half of the stars, we also find a linear RV-CRX anticorrelation, which indicates that their activity-induced RV scatter is lower at longer wavelengths. For most of them we can exclude a linear correlation between RV and Halpha emission. Our results are in agreement with simulated activity-induced RV variations in M dwarfs. The RV variations of most active RV-loud M dwarfs are likely to be caused by dark spots on their surfaces, which move in and out of view as the stars rotate.

Keywords
  1. late-type-stars
  2. m-stars
  3. radial-velocity
  4. narrow-band-photometry
  5. atomic-spectroscopy
Bibliographic source Bibcode
2018A&A...614A.122T
See also HTML
https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/614/A122
IVOA Identifier IVOID
ivo://CDS.VizieR/J/A+A/614/A122
Document Object Identifer DOI
doi:10.26093/cds/vizier.36140122

Access

Web browser access HTML
http://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/614/A122
https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/614/A122
http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/614/A122
IVOA Table Access TAP
http://tapvizier.cds.unistra.fr/TAPVizieR/tap
Run SQL-like queries with TAP-enabled clients (e.g., TOPCAT).
IVOA Cone Search SCS
For use with a cone search client (e.g., TOPCAT).
http://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/614/A122/stars?
https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/614/A122/stars?
http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/614/A122/stars?

History

2018-06-25T08:23:33Z
Resource record created
2018-06-25T08:23:33Z
Created
2018-09-25T12:03:27Z
Updated

Contact

Name
CDS support team
Postal Address
CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France
E-Mail
cds-question@unistra.fr