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KELT-6b: A P~7.9 d Hot Saturn Transiting a Metal-Poor Star with a Long-Period Companion | | Karen A. Collins
; Jason D. Eastman
; Thomas G. Beatty
; Robert J. Siverd
; B. Scott Gaudi
; Joshua Pepper
; John F. Kielkopf
; John Asher Johnson
; Andrew W. Howard
; Debra A. Fischer
; Mark Manner
; Allyson Bieryla
; David W. Latham
; Benjamin J. Fulton
; Joao Gregorio
; Lars A. Buchhave
; Eric L. N. Jensen
; Keivan G. Stassun
; Kaloyan Penev
; Justin R. Crepp
; Sasha Hinkley
; Rachel A. Street
; Phillip Cargile
; Claude E. Mack
; Thomas E. Oberst
; Ryan L. Avril
; Samuel N. Mellon
; Kim K. McLeod
; Matthew T. Penny
; Robert P. Stefanik
; Perry Berlind
; Michael L. Calkins
; Qingqing Mao
; Alexander J. W. Richert
; Darren L. DePoy
; Gilbert A. Esquerdo
; Andrew Gould
; Jennifer L. Marshall
; Ryan J. Oelkers
; Richard W. Pogge
; Mark Trueblood
; Patricia Trueblood
; | | Date: |
10 Aug 2013 | | Abstract: | We report the discovery of KELT-6b, a mildly-inflated Saturn-mass planet
transiting a metal-poor host. The initial transit signal was identified in
KELT-North survey data, and the planetary nature of the occulter was confirmed
using a combination of follow-up photometry, high-resolution imaging,
high-resolution spectroscopy, and precise radial velocity measurements. The
fiducial model from a global analysis including constraints from isochrones
indicates that the V=10.38 host star (TYC 2532-556-1) is a mildly evolved,
late-F star with T_eff=6102 pm 43 K, log(g_*)=4.07_{-0.07}^{+0.04} and
[Fe/H]=-0.28 pm 0.04, with an inferred mass M_*=1.09 pm 0.04 M_sun and radius
R_*=1.58_{-0.09}^{+0.16} R_sun. The planetary companion has mass M_p=0.43 pm
0.05 M_Jup, radius R_p=1.19_{-0.08}^{+0.13} R_Jup, surface gravity
log(g_p)=2.86_{-0.08}^{+0.06}, and density rho_p=0.31_{-0.08}^{+0.07} g
cm^{-3}. The planet is on an orbit with semimajor axis a=0.079 pm 0.001 AU and
eccentricity e=0.22_{-0.10}^{+0.12}, which is roughly consistent with circular,
and has ephemeris of T_C(BJD_TDB)=2456347.79679 pm 0.00036 and P=7.845631 pm
0.000046 d. Equally plausible fits that employ empirical constraints on the
host star parameters rather than isochrones yield a larger planet mass and
radius by ~4-7%. KELT-6b has surface gravity and incident flux similar to HD
209458b, but orbits a host that is more metal poor than HD 209458b by ~0.3 dex.
Thus, the KELT-6 system is a metal-poor analog of HD 209458, and offers the
unique opportunity to perform a comparative measurement of two similar planets
in similar environments around stars of very different metallicities. The
precise radial velocity data also reveal an acceleration indicative of a
longer-period third body in the system, although the companion is not detected
in Keck adaptive optics images. | | Source: | arXiv, 1308.2296 | | Services: | Forum | Review | PDF | Favorites | |
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