J/AJ/162/89 HIRES radial velocity follow up for Kepler-129 (Zhang+, 2021)
Long-period jovian tilts the orbits of two sub-Neptunes relative to stellar
spin axis in Kepler-129.
Zhang J., Weiss L.M., Huber D., Blunt S., Chontos A., Fulton B.J.,
Grunblatt S., Howard A.W., Isaacson H., Kosiarek M.R., Petigura E.A.,
Rosenthal L.J., Rubenzahl R.A.
<Astron. J., 162, 89-89 (2021)>
=2021AJ....162...89Z 2021AJ....162...89Z (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets; Stars, G-type; Radial velocities; Spectra, infrared
Keywords: Radial velocity; Asteroseismology; Exoplanet dynamics
Abstract:
We present the discovery of Kepler-129d (Pd=7.2-0.3+0.4yr,
msinid=8.3-0.7+1.1MJup, ed=0.15-0.05+0.07) based on
six years of radial-velocity observations from Keck/HIRES. Kepler-129
also hosts two transiting sub-Neptunes: Kepler-129b (Pb= 15.79days,
rb=2.40±0.04R⊕) and Kepler-129c (Pc=82.20days,
rc=2.52±0.07R⊕) for which we measure masses of
mb<20M⊕ and mc=43-12+13M⊕. Kepler-129 is a
hierarchical system consisting of two tightly packed inner planets and
a massive external companion. In such a system, two inner planets
precess around the orbital normal of the outer companion, causing
their inclinations to oscillate with time. Based on an asteroseismic
analysis of Kepler data, we find tentative evidence that Kepler-129b
and c are misaligned with stellar spin axis by ≳38°, which could
be torqued by Kepler-129 d if it is inclined by ≳19° relative to
inner planets. Using N-body simulations, we provide additional
constraints on the mutual inclination between Kepler-129d and inner
planets by estimating the fraction of time during which two inner
planets both transit. The probability that two planets both transit
decreases as their misalignment with Kepler-129d increases. We also
find a more massive Kepler-129c enables the two inner planets to
become strongly coupled and more resistant to perturbations from
Kepler-129d. The unusually high mass of Kepler-129c provides a
valuable benchmark for both planetary dynamics and interior structure,
since the best-fit mass is consistent with this 2.5R⊕ planet
having a rocky surface.
Description:
We collected the radial velocity data for Kepler-129 from 2014 to 2021
using the High Resolution Echelle Spectrometer (HIRES, R∼60000) at the
W.M. Keck Observatory.
Objects:
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RA (2000) DE Designation(s)
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19 01 14.70 +47 50 54.9 Kepler-129 = Kepler-129
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 152 26 Kepler-129 Radial Velocities
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See also:
J/ApJ/723/L223 : Radial velocities of HAT-P-11 (Winn+, 2010)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/ApJS/210/25 : Transit timing variation for 15 planetary pairs. II (Xie, 2014)
J/MNRAS/452/2127 : Fundamental param. of Kepler stars (Silva Aguirre+, 2015)
J/ApJ/835/172 : Kepler asteroseismic LEGACY sample I Oscillations (Lund+, 2017)
J/AJ/155/255 : Radial velocity & activity measurements of HAT-P-11 (Yee+, 2018)
J/AJ/156/264 : California-Kepler Survey. VII. Planet radius gap (Fulton+, 2018)
J/AJ/161/70 : Rvel for WASP-107 with HIRES & CORALIE (Piaulet+, 2021)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Tobs Observation time; UTC/ISO8601
25- 33 A9 --- Obs.ID Observation id; CPS internal ID
35- 41 A7 --- Tel Telescope/Instrument; HIRES J-band
43- 56 F14.6 d BJD [2456912/2459315] Barycentric Julian Date at TDB
58- 75 F18.13 m/s RVel [-110/86] Mean relative radial velocity
77- 92 F16.14 m/s e_RVel [2/3] Uncertainty in RVel (1)
94-100 F7.1 e cts [5311/11032] Counts raw 1D spectrum near 5500Å
102-117 F16.14 --- chi2 [1.03/1.08] Median reduced chi-squared for the
observation over all chunks
119-128 F10.3 m/s BVel [-10509/10275] Barycentric velocity at
flux-weighted midpoint
130-135 F6.4 --- SHK [0.11/0.15]? CaHK S value
137-141 F5.3 --- e_SHK [0.001]? CaHK S value uncertainty
143-148 F6.2 km/s TRV [-22.1/-21.5]? Telluric calibrated absolute
Radial Velocity
150-152 F3.1 km/s e_TRV [0.1]? Uncertainty in TRV
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Note (1): The RVel uncertainties do not include RVel jitter.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 24-Nov-2021