Astrophys. J., 746, 37 (2012/February-2)
Astrometry and radial velocities of the planet host M dwarf GJ 317: new trigonometric distance, metallicity, and upper limit to the mass of GJ 317b.
ANGLADA-ESCUDE G., BOSS A.P., WEINBERGER A.J., THOMPSON I.B., BUTLER R.P., VOGT S.S. and RIVERA E.J.
Abstract (from CDS):
We have obtained precision astrometry of the planet host M dwarf GJ 317 in the framework of the Carnegie Astrometric Planet Search project. The new astrometric measurements give a distance determination of 15.3 pc, 65% further than previous estimates. The resulting absolute magnitudes suggest that it is metal-rich and more massive than previously assumed. This result strengthens the correlation between high metallicity and the presence of gas giants around low-mass stars. At 15.3 pc, the minimal astrometric amplitude for planet candidate GJ 317b is 0.3 mas (edge-on orbit), just below our astrometric sensitivity. However, given the relatively large number of observations and good astrometric precision, a Bayesian Monte Carlo Markov Chain analysis indicates that the mass of planet b has to be smaller than twice the minimum mass with a 99% confidence level, with a most likely value of 2.5 MJup. Additional radial velocity (RV) measurements obtained with Keck by the Lick-Carnegie Planet search program confirm the presence of an additional very long period planet candidate, with a period of 20 years or more. Even though such an object will imprint a large astrometric wobble on the star, its curvature is yet not evident in the astrometry. Given high metallicity, and the trend indicating that multiple systems are rich in low-mass companions, this system is likely to host additional low-mass planets in its habitable zone that can be readily detected with state-of-the-art optical and near-infrared RV measurements.
astrometry - planetary systems - stars: individual: GJ 317 - techniques: radial velocities
In Figure 2: 2M J0539-00, J0559-14, J0641-43 and J1058-15 are not identified (not enough information).
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