J/ApJ/785/126 HIRES radial velocity measurements (Knutson+, 2014)
Friends of hot Jupiters.
I. A radial velocity search for massive, long-period companions to close-in gas
giant planets.
Knutson H.A., Fulton B.J., Montet B.T., Kao M., Ngo H., Howard A.W.,
Crepp J.R., Hinkley S., Bakos G.A., Batygin K., Johnson J.A., Morton T.D.,
Muirhead P.S.
<Astrophys. J., 785, 126 (2014)>
=2014ApJ...785..126K 2014ApJ...785..126K (SIMBAD/NED BibCode)
ADC_Keywords: Planets ; Radial velocities ; Stars, double and multiple
Stars, masses ; Abundances, [Fe/H]
Keywords: binaries: eclipsing - instrumentation: adaptive optics -
planetary systems - techniques: radial velocities
Abstract:
In this paper we search for distant massive companions to known
transiting gas giant planets that may have influenced the dynamical
evolution of these systems. We present new radial velocity
observations for a sample of 51 planets obtained using the Keck HIRES
instrument, and find statistically significant accelerations in
fifteen systems. Six of these systems have no previously reported
accelerations in the published literature: HAT-P-10, HAT-P-22,
HAT-P-29, HAT-P-32, WASP-10, and XO-2. We combine our radial velocity
fits with Keck NIRC2 adaptive optics (AO) imaging data to place
constraints on the allowed masses and orbital periods of the
companions responsible for the detected accelerations. The estimated
masses of the companions range between 1-500 MJup, with orbital
semi-major axes typically between 1-75 AU. A significant majority of
the companions detected by our survey are constrained to have minimum
masses comparable to or larger than those of the transiting planets in
these systems, making them candidates for influencing the orbital
evolution of the inner gas giant. We estimate a total occurrence rate
of 51%±10% for companions with masses between 1-13 MJup and
orbital semi-major axes between 1-20 AU in our sample. We find no
statistically significant difference between the frequency of
companions to transiting planets with misaligned or eccentric orbits
and those with well-aligned, circular orbits. We combine our expanded
sample of radial velocity measurements with constraints from transit
and secondary eclipse observations to provide improved measurements of
the physical and orbital characteristics of all of the planets
included in our survey.
Description:
We observed our target stars using the High Resolution Echelle
Spectrometer (HIRES) (Vogt et al. 1994SPIE.2198..362V 1994SPIE.2198..362V) on the 10 m
Keck I telescope over a period of two years beginning in 2011; many of
our targets also had existing HIRES observations taken prior to 2011
by other programs. We used the standard HIRES setup and reduction
pipeline employed by the California Planet Search (CPS) consortium
(Wright et al. 2004, J/ApJS/152/261; Howard et al. 2009ApJ...696...75H 2009ApJ...696...75H;
Johnson et al. 2010PASP..122..149J 2010PASP..122..149J). Observations were typically
obtained with a slit width of 0.86" with integration times
optimized to obtain typical signal to noise ratios of 70 per pixel. An
iodine cell mounted in front of the spectrometer entrance slit
provided a wavelength scale and instrumental profile for the
observations (Marcy & Butler, 1992PASP..104..270M 1992PASP..104..270M; Valenti et al.
1995PASP..107..966V 1995PASP..107..966V). We obtained a total of approximately 270 new
radial velocity measurements for our target sample, with a minimum of
four observations per target separated by at least six months.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 91 51 Stellar Parameters
table3.dat 41 1054 HIRES Radial Velocity Measurements
refs.dat 63 44 References
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See also:
III/185 : Search for Jupiter-Mass Companions (Walker+, 1995)
III/211 : Keck/HIRES Sky Line Atlas (Osterbrock+ 1997)
J/ApJS/152/261 : Chromospheric Ca II emission in nearby stars (Wright+, 2004)
J/MNRAS/426/739 : Velocities for seven transiting hot Jupiters (Hellier+, 2012)
J/A+A/563/A22 : Radial velocities of 3 new hot Jupiters (Moutou+, 2014)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Star name
11- 15 F5.3 Msun Mass Mass
17- 21 F5.3 Msun e_Mass Error in Mass
23- 27 F5.2 [-] [Fe/H] Metallicity
29- 32 F4.2 [-] e_[Fe/H] Error in [Fe/H]
34- 43 A10 --- Sample Sample identification (1)
45- 91 A47 --- Ref Reference(s) (listed in refs.dat file)
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Note (1): The misaligned sample consists of planets with either eccentric or
misaligned orbits, while the control sample contains planets that
appear to have circular and/or well-aligned orbits.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 F15.7 d BJD Barycentric Julian Date; TDB
17- 25 F9.3 m/s RV Radial velocity
27- 32 F6.3 m/s e_RV Error in RV
34- 41 A8 --- Name Star name
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Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 25 A25 --- Ref Reference
29- 47 A19 --- Bibcode Reference bibcode
49- 63 A15 --- Com Comment on reference
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History:
From electronic version of the journal
References:
Ngo et al. Paper II 2015ApJ...800..138N 2015ApJ...800..138N
Piskorz et al. Paper III 2015ApJ...814..148P 2015ApJ...814..148P
Ngo et al. Paper IV 2016ApJ...827....8N 2016ApJ...827....8N
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 13-Jun-2017