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Using HARPS-N to characterise the long-period planets in the PH-2 and Kepler-103 systems | | Sophie C. Dubber
; Annelies Mortier
; Ken Rice
; Chantanelle Nava
; Luca Malavolta
; Helen Giles
; Adrien Coffinet
; David Charbonneau
; Andrew Vanderburg
; Aldo S. Bonomo
; Walter Boschin
; Lars A. Buchhave
; Andrew Collier Cameron
; Rosario Cosentino
; Xavier Dumusque
; Adriano Ghedina
; Avet Harutyunyan
; Raphaelle D. Haywood
; David Latham
; Mercedes Lopez-Morales
; Giusi Micela
; Emilio Molinari
; Francesco A. Pepe
; David Phillips
; Giampaolo Piotto
; Ennio Poretti
; Dimitar Sasselov
; Alessandro Sozzetti
; Stephane Udry
; | | Date: |
8 Oct 2019 | | Abstract: | We present confirmation of the planetary nature of PH-2b, as well as the
first mass estimates for the two planets in the Kepler-103 system. PH-2b and
Kepler-103c are both long-period and transiting, a sparsely-populated category
of exoplanet. We use {it Kepler} light-curve data to estimate a radius, and
then use HARPS-N radial velocities to determine the semi-amplitude of the
stellar reflex motion and, hence, the planet mass. For PH-2b we recover a
3.5-$sigma$ mass estimate of $M_p = 109^{+30}_{-32}$ M$_oplus$ and a radius
of $R_p = 9.49pm0.16$ R$_oplus$. This means that PH-2b has a Saturn-like bulk
density and is the only planet of this type with an orbital period $P > 200$
days that orbits a single star. We find that Kepler-103b has a mass of
$M_{ ext{p,b}} = 11.7^{+4.31}_{-4.72}$ M$_{oplus}$ and Kepler-103c has a mass
of $M_{ ext{p,c}} = 58.5^{+11.2}_{-11.4}$ M$_{oplus}$. These are 2.5$sigma$
and 5$sigma$ results, respectively. With radii of $R_{ ext{p,b}} =
3.49^{+0.06}_{-0.05}$ R$_oplus$, and $R_{ ext{p,c}} = 5.45^{+0.18}_{-0.17}$
R$_oplus$, these results suggest that Kepler-103b has a Neptune-like density,
while Kepler-103c is one of the highest density planets with a period $P > 100$
days. By providing high-precision estimates for the masses of the long-period,
intermediate-mass planets PH-2b and Kepler-103c, we increase the sample of
long-period planets with known masses and radii, which will improve our
understanding of the mass-radius relation across the full range of exoplanet
masses and radii. | | Source: | arXiv, 1910.3518 | | Services: | Forum | Review | PDF | Favorites | |
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