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Determining the true mass of radial-velocity exoplanets with Gaia: 9 planet candidates in the brown-dwarf/stellar regime and 27 confirmed planets | | Flavien Kiefer
; Guillaume Hébrard
; Alain Lecavelier
; Eder Martioli
; Shweta Dalal
; Alfred Vidal-Madjar
; | | Date: |
29 Sep 2020 | | Abstract: | Mass is one of the most important parameters for determining the true nature
of an astronomical object. Yet, many published exoplanets lack a measurement of
their true mass, in particular those detected thanks to radial velocity (RV)
variations of their host star. For those, only the minimum mass, or $msin i$,
is known, owing to the insensitivity of RVs to the inclination of the detected
orbit compared to the plane-of-the-sky. The mass that is given in database is
generally that of an assumed edge-on system ($sim$90$^circ$), but many other
inclinations are possible, even extreme values closer to 0$^circ$ (face-on).
In such case, the mass of the published object could be strongly underestimated
by up to two orders of magnitude. In the present study, we use GASTON, a tool
recently developed in Kiefer et al. (2019) & Kiefer (2019) to take advantage of
the voluminous Gaia astrometric database, in order to constrain the inclination
and true mass of several hundreds of published exoplanet candidates. We find 9
exoplanet candidates in the stellar or brown dwarf (BD) domain, among which 6
were never characterized. We show that 30 Ari B b, HD 141937 b, HD 148427 b, HD
6718 b, HIP 65891 b, and HD 16760 b have masses larger than 13.5 M$_ ext{J}$
at 3-$sigma$. We also confirm the planetary nature of 27 exoplanets among
which HD 10180 c, d and g. Studying the orbital periods, eccentricities and
host-star metallicities in the BD domain, we found distributions with respect
to true masses consistent with other publications. The distribution of orbital
periods shows of a void of BD detections below $sim$100 days, while
eccentricity and metallicity distributions agree with a transition between BDs
similar to planets and BDs similar to stars about 40-50 M$_ ext{J}$. | | Source: | arXiv, 2009.14164 | | Services: | Forum | Review | PDF | Favorites | |
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