Volume 618, October 2018
|Number of page(s)||11|
|Section||Catalogs and data|
|Published online||03 October 2018|
A Radial velocity survey of spatially resolved young, low-mass binaries⋆
1 Astrophysics Research Center, Queens University Belfast, Belfast, UK
2 Department of Astronomy, Stockholm University, Stockholm, Sweden
e-mail: firstname.lastname@example.org, email@example.com
3 Max Planck Institute for Astronomy, Heidelberg, Germany
4 NASA Exoplanet Science Institute, Caltech, Pasadena, CA, USA
5 Université Grenoble Alpes, IPAG, Grenoble, France
Accepted: 8 June 2018
The identification and characterisation of low-mass binaries is of importance for a range of astrophysical investigations. Low-mass binaries in young (∼10–100 Myr) moving groups (YMGs) in the solar neighborhood are of particular significance as they provide unique opportunities to calibrate stellar models and evaluate the ages and coevality of the groups themselves. Low-mass M-dwarfs have pre-main sequence life times on the order of ∼100 Myr and therefore are continually evolving along a mass-luminosity track throughout the YMG phase, providing ideal laboratories for precise isochronal dating, if a model-independent dynamical mass can be measured. AstraLux lucky imaging multiplicity surveys have recently identified hundreds of new YMG low-mass binaries, where a subsample of M-dwarf multiples have estimated orbital periods less than 50 yr. We have conducted a radial velocity survey of a sample of 29 such targets to complement the astrometric data. This will allow enhanced orbital determinations and precise dynamical masses to be derived in a shorter timeframe than possible with astrometric monitoring alone, and allow for a more reliable isochronal analysis. Here we present radial velocity measurements derived for our sample over several epochs. We report the detection of the three-component spectroscopic multiple 2MASS J05301858-5358483, for which the C component is a new discovery, and forms a tight pair with the B component. Originally identified as a YMG member, we find that this system is a likely old field interloper, whose high chromospheric activity level is caused by tidal spin-up of the tight BC pair. Two other triple systems with a tight pair exist in the sample, 2MASS J04244260-0647313 (previously known) and 2MASS J20163382-0711456, but for the rest of the targets we find that additional tidally synchronized companions are highly unlikely, providing further evidence that their high chromospheric activity levels are generally signatures of youth.
Key words: binaries: spectroscopic / binaries: visual / stars: pre-main sequence
Table 2 is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (220.127.116.11) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/618/A5
© ESO 2018
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