Search for radial velocity variations in eight M-dwarfs with NIRSPEC/Keck II
| Autor: | M. M. Montgomery, Carlos del Burgo, Maria Rosa Zapatero Osorio, Eduardo L. Martín, Orlagh L. Creevey, Rohit Deshpande, Florian Rodler |
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| Rok vydání: | 2011 |
| Předmět: |
Physics
Instrumentation Brown dwarf FOS: Physical sciences Astronomy and Astrophysics Context (language use) Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Stellar classification Spectral line Radial velocity Stars Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Planet Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Astrophysics::Galaxy Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) |
| DOI: | 10.48550/arxiv.1112.1382 |
| Popis: | Context. Radial velocity (RV) measurements from near-infrared spectra have become a potentially powerful tool to search for planets around cool stars and sub-stellar objects. As part of a large survey to characterize M-dwarfs using NIRSPEC at Keck II, we obtained spectra of eight late M-dwarfs (spectral types M5.0-M8.0) during two or more observing epochs per target. These spectra were taken with intermediate spectral resolving powers (R \sim 20,000) in the J-band. Aims. We search for relative radial velocity variability in these late M-dwarfs and test the NIRSPEC capability of detecting short period brown dwarf and massive planetary companions around low-mass stars in the J-band (\approx 1.25 micron). Additionally, we reanalyzed the data of the M8-type star vB10 (one of our targets) presented in Zapatero Osorio et al. (2009), which were obtained with the same instrumentation as our data. Methods. [...] Results. For the entire M-dwarf sample, we do not find any evidence of relative RV variations induced by a short period brown dwarf or massive planetary companion. The typical RV precision of the measurements is between 180 and 300 m/s, which is sufficient to detect hot Neptunes around M-dwarfs. Also, we find that the spurious RV shift in Zapatero et al. (2009) of the star VB10 was caused by asymmetries in the instrumental profile between different observing epochs, which were not taken into account in their analysis. Comment: A&A, 7 pages, 5 figures |
| Databáze: | OpenAIRE |
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