Abstract
We present a refined orbital solution for the components A, B, and C of the nearby late-M type multiple system LHS 1070. By combining astrometric datapoints from NACO/VLT, CIAO/SUBARU, and PUEO/CFHT, as well as a radial velocity measurement from the newly commissioned near infrared high-resolution spectrograph CRIRES/VLT, we achieve a very precise orbital solution for the B and C components and a first realistic constraint on the much longer orbit of the A-BC system. Both orbits appear to be co-planar. Masses for the B and C components calculated from the new orbital solution (M B+C = 0.157 ± 0.009 M ⊙ ) are in excellent agreement with theoretical models, but do not match empirical mass-luminosity tracks. The preliminary orbit of the A-BC system reveals no mass excess for the A component, giving no indication for a previously proposed fourth (D) component in LHS 1070.
Highlights
LHS 1070 (GJ 2005, LP 881-64) is a low-mass triple system at a distance of 7.72±0.15 pc from the Sun (Costa et al 2005)
By combining astrometric datapoints from NACO/VLT, CIAO/SUBARU, and PUEO/Canada-France-Hawaii Telescope (CFHT), as well as a radial velocity measurement from the newly commissioned near infrared high-resolution spectrograph CRIRES/VLT, we achieve a very precise orbital solution for the B and C components and a first realistic constraint on the much longer orbit of the A-BC system
In addition to the astrometric datapoints published in Leinert et al (2001), we used archived images from the adaptive optics (AO) cameras PUEO/CFHT and NACO/VLT covering a timespan of nearly 6 years, see Table 1 for details
Summary
LHS 1070 (GJ 2005, LP 881-64) is a low-mass triple system at a distance of 7.72±0.15 pc from the Sun (Costa et al 2005) It consists of two components with masses close to the substellar limit (LHS 1070 B and C) with spectral types of M 8.5 to M 9, orbited by a slightly more massive M 5.5 type component, LHS 1070 A. During the science verification phase of CRIRES at the VLT (Käufl et al 2006), we obtained spatially resolved measurements of the rotational velocity and magnetic activity for all three components of LHS 1070 (see Reiners et al 2007, for details).
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