J/ApJS/270/8 The KGPS. I. Kepler planet-host RVs from HIRES (Weiss+, 2024)
The Kepler Giant Planet Search.
I. A decade of Kepler planet-host radial velocities from W. M. Keck observatory.
Weiss L.M., Isaacson H., Howard A.W., Fulton B.J., Petigura E.A.,
Fabrycky D., Jontof-Hutter D., Steffen J.H., Schlichting H.E.,
Wright J.T., Beard C., Brinkman C.L., Chontos A., Giacalone S., Hill M.L.,
Kosiarek M.R., MacDougall M.G., Mocnik T., Polanski A.S., Turtelboom E.V.,
Tyler D., Van Zandt J.
<Astrophys. J. Suppl. Ser., 270, 8 (2024)>
=2024ApJS..270....8W 2024ApJS..270....8W
ADC_Keywords: Exoplanets; Radial velocities; Stars, masses; Spectra, optical;
Rotational velocities
Keywords: Exoplanets ; Exoplanet catalogs ; Exoplanet systems ;
Radial velocity ; Transits ; Orbital elements ;
Exoplanet detection methods ; Mini Neptunes ; Super Earths ;
Extrasolar rocky planets ; Binary stars
Abstract:
Despite the importance of Jupiter and Saturn to Earth's formation and
habitability, there has not yet been a comprehensive observational
study of how giant exoplanets correlate with the architectural
properties of close-in, sub-Neptune-sized exoplanets. This is largely
because transit surveys are particularly insensitive to planets at
orbital separations ≳1au, and so their census of Jupiter-like planets
is incomplete, inhibiting our study of the relationship between
Jupiter-like planets and the small planets that do transit. To
investigate the relationship between close-in, small and distant,
giant planets, we conducted the Kepler Giant Planet Survey (KGPS).
Using the W. M. Keck Observatory High Resolution Echelle Spectrometer,
we spent over a decade collecting 2844 radial velocities (RVs; 2167 of
which are presented here for the first time) of 63 Sunlike stars that
host 157 transiting planets. We had no prior knowledge of which
systems would contain giant planets beyond 1au, making this survey
unbiased with respect to previously detected Jovians. We announce
RV-detected companions to 20 stars from our sample. These include
13 Jovians (0.3MJ<Msini<13MJ, 1au<a<10au), eight nontransiting
sub-Saturns, and three stellar-mass companions. We also present
updated masses and densities of 84 transiting planets. The KGPS
project leverages one of the longest-running and most data-rich
collections of RVs of the NASA Kepler systems yet, and it will provide
a basis for addressing whether giant planets help or hinder the growth
of sub-Neptune-sized and terrestrial planets. Future KGPS papers will
examine the relationship between small, transiting planets and their
long-period companions.
Description:
We accessed the orbital ephemerides of all planetary systems from the
NASA Exoplanet Archive.
RVs were obtained at the W. M. Keck Observatory using the HIRES
instrument. See Section 3.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 62 2844 Radial velocities from Keck-HIRES of
63 Kepler planet-hosting stars
table3.dat 88 98 Results of KGPS automated planet and trend search
table4.dat 346 63 Stellar properties and RV data summary
table5.dat 428 187 KGPS planet physical properties
table6.dat 159 27 KGPS non-transiting companion orbital properties
for 22 systems
--------------------------------------------------------------------------------
See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
V/117 : Geneva-Copenhagen Survey of Solar neighbourhood (Holmberg+, 2007)
J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)
J/ApJ/725/875 : Chromospheric activity for CPS stars (Isaacson+, 2010)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/ApJ/756/186 : TTVs from Kepler. VI. Statistical tests (Steffen+, 2012)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/ApJ/763/41 : Kepler multiple-candidate systems radii (Ciardi+, 2013)
J/ApJ/767/127 : Asteroseismic solutions for 77 Kepler stars (Huber+, 2013)
J/ApJS/210/19 : Kepler planetary candidates. IV. 22 months (Burke+, 2014)
J/ApJ/789/154 : Kepler-10 RV measurements by HARPS-N (Dumusque+, 2014)
J/ApJ/787/80 : 139 Kepler planets transit time variations (Hadden+, 2014)
J/ApJS/210/20 : Small Kepler planets radial velocities (Marcy+, 2014)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/ApJS/210/25 : Transit timing var. for 15 planetary pairs. II. (Xie, 2014)
J/ApJ/800/135 : HARPS-N radial velocities of KOI-69 (Dressing+, 2015)
J/ApJS/217/31 : Kepler planetary cand. VI. 4yr Q1-Q16 (Mullally+, 2015)
J/ApJS/217/16 : Kepler planetary candidates. V. 3yr Q1-Q12 (Rowe+, 2015)
J/MNRAS/452/2127 : Fundamental param. of Kepler stars (Silva Aguirre+, 2015)
J/AJ/152/160 : HARPS-N radial velocities of KOI-70 (Buchhave+, 2016)
J/ApJS/225/9 : Kepler TTVs. IX. Long-cadence data set (Holczer+, 2016)
J/ApJ/822/86 : False positive prob. for Q1-Q17 DR24 KOIs (Morton+, 2016)
J/ApJ/825/62 : Stars with hot Jupiter planets (Schlaufman+, 2016)
J/ApJ/839/94 : Abundances of solar twins from Keck/HIRES (Bedell+, 2017)
J/AJ/154/109 : California-Kepler Survey (CKS). III. Radii (Fulton+, 2017)
J/AJ/154/5 : Transit timing variations of Kepler planets (Hadden+, 2017)
J/AJ/154/107 : California-Kepler Survey (CKS). I. (Petigura+, 2017)
J/ApJ/836/77 : A library of high-S/N opt. sp. of FGKM stars (Yee+, 2017)
J/ApJ/866/99 : Radii of KIC stars & planets using Gaia DR2 (Berger+, 2018)
J/ApJS/237/38 : Extended abundance analysis of KOIs (Brewer+, 2018)
J/A+A/618/A41 : Photometry of Kepler-9b and c transits (Freudenthal+, 2018)
J/AJ/156/264 : CKS. VII. Planet radius gap (Fulton+, 2018)
J/AJ/155/89 : California-Kepler Survey (CKS). IV. (Petigura+, 2018)
J/ApJS/235/38 : Kepler pl. cand. VIII. DR25 reliability (Thompson+, 2018)
J/AJ/158/181 : RVs and S-index values for HR 5183 (Blunt+, 2019)
J/ApJ/877/60 : YMGs. I. Young bin. & lithium-rich stars (Bowler+, 2019)
J/AJ/157/52 : Radial velocity obs. in super-Earth systems (Bryan+, 2019)
J/other/RAA/19.41 : TTVs & ephemerides of Kepler exoplanets (Gajdos+, 2019)
J/AJ/158/165 : RV obs. & activity indicators for Kepler-538b (Mayo+, 2019)
J/AJ/157/145 : HIRES RVs of 3 compact, multiplanet systems (Mills+, 2019)
J/MNRAS/490/5088 : Stellar companions of exoplanet host stars (Mugrauer, 2019)
J/A+A/624/A15 : Kepler-411 mid-transit times (Sun+, 2019)
J/AJ/159/235 : RV jitters in ∼600 planet host stars (Luhn+, 2020)
J/MNRAS/491/5287 : Exoplanet evaporation in multitransit syst. (Owen+, 2020)
J/AJ/159/242 : Vel. & transit times in the Kepler-88 system (Weiss+, 2020)
J/AJ/161/36 : Exoplanets in HZ with Kepler DR25 (Bryson+, 2021)
J/AJ/161/202 : Transit timing var. of Kepler-90g and h (Liang+, 2021)
J/MNRAS/507/1847 : A HARPS-N mass for the elusive Kepler-37d (Rajpaul+, 2021)
J/AJ/162/55 : 65 Transit-timing variation planets properties (Yee+, 2021)
J/AJ/162/89 : HIRES RV follow up for Kepler-129 (Zhang+, 2021)
J/A+A/677/A33 : 38 Kepler and K2 systems RVs (Bonomo+, 2023)
J/AJ/165/74 : HIRES/HARPS-N RVs of Kepler-102 (Brinkman+, 2023)
http://exoplanetarchive.ipac.caltech.edu/ : NASA Exoplanet Archive homepage
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Syst System name used to link tables in this work (1)
8- 15 A8 --- KOA Object name in the Keck Observatory Archive
17- 28 F12.6 d BJD [4989/10214] Barycentric Julian date,
BJD-2450000
30- 41 F12.6 m.s-1 RV [-1759/2632] Radial velocity
43- 48 F6.3 m.s-1 e_RV [0.9/12] Uncertainty in RV
50- 55 F6.4 --- SHK [0.06/0.8] Mt. Wilson calcium activity index
57- 62 F6.3 [-] logRHK [-6/0] Chromospheric contribution of the
H and K Ca lines
--------------------------------------------------------------------------------
Note (1): Object names are linked in between tables in this work using
this field. This is the 5-digit KOI number (left-filled with zeroes),
which corresponds to most but not all of the identifiers in the
Keck Observatory Archive (See KOA column).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Syst System name used to link tables in this work (1)
8- 11 I4 --- KOI [41/3179] Kepler object of interest identifier
13- 16 I4 --- Kepler [9/1911]? Kepler planetary system number
18- 20 I3 --- Nrv [10/226] Number of radial velocity measurements
22- 25 F4.1 yr dRV [4.8/13.4] Radial velocity baseline
27- 36 A10 "Y/M/D" Date Date (UTC) of last RV observation
38- 42 A5 --- Model Model addition (2)
44- 49 F6.1 d Per [15/6226.4]? Orbital period, proposed companion
51- 56 F6.1 m.s-1 K [1.5/2244.6]? RV semi-amplitude,
proposed companion
58- 63 F6.1 m.s-1 RMS [2.4/1649.3] RMS of RV residuals before MCMC
fitting
65- 71 F7.5 --- FAP [0/1]? False alarm probability
73- 84 F12.6 --- dBIC [-3855/6.7]? Difference, Bayesian Information
Criterion (3)
86- 88 A3 --- Flag Flags for matching sources to KOA (4)
--------------------------------------------------------------------------------
Note (1): Object names are linked in between tables in this work using
this field. This is the 5-digit KOI number (left-filled with zeroes),
which corresponds to most but not all of the identifiers in the
Keck Observatory Archive (See Flag column).
Note (2): Proposed companion number added to the model; "trend" proposes
including a linear RV trend in the model rather than an additional
companion.
Note (3): Difference in the Bayesian Information Criterion with and without
the addition of the companion (or trend). Negative values indicate that
an N+1-planet model is preferred.
Note (4): Flags on sources, including modeling flags and translations to
identifiers in the Keck Observatory Archive as follows:
1 = The KOA name is preceded by a C (e.g., CK00094);
2 = The KGPS automatic pipeline did not include eccentricity for
the massive non-transiting planet, but our final analysis did;
3 = The KGPS automatic pipeline did not detect a companion that
was apparent by eye;
4 = The KGPS automatic pipeline detected what is likely an alias
of the true orbital period;
5 = The KOA name is the Hipparcos name, e.g, Kepler-444 (K03158)
is designated as HIP94931 in the KOA.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Syst System name used to link tables in this
work (1)
8- 18 A11 --- Kepler Kepler planetary system
20- 21 I2 h RAh [18/20] SIMBAD Hour of Right Ascension
(J2000)
23- 24 I2 min RAm Minute of Right Ascension (J2000)
26- 27 I2 s RAs Second of Right Ascension (J2000)
29 A1 --- DE- [+] SIMBAD Sign of the Declination (J2000)
30- 31 I2 deg DEd [37/50] SIMBAD Degree of Declination
(J2000)
33- 34 I2 arcmin DEm Arcminute of Declination (J2000)
36- 39 F4.1 arcsec DEs Arcsecond of Declination (J2000), Simbad
41- 46 F6.3 mag Vmag [8.8/13.8] V-band magnitude, Simbad
48- 56 F9.6 mag Gmag [8.6/13.8] Gaia DR3 G-band magnitude
58- 63 F6.1 K Teff [4457/6214] Surface Effective temperature
(2)
65- 75 F11.9 [cm.s-2] logg [3.2/4.7] Log of surface gravity (2)
77- 88 F12.10 Msun Mstar [0.6/1.5] Star mass (2)
90- 95 F6.3 [-] [Fe/H] [-0.6/0.5] Metallicity (2)
97- 109 E13.6 m.s-1 vsini [1.4e-07/10.1] Projected rotational
velocity, star (2)
111 I1 --- Ntp [1/8] Number of transiting planets
113- 115 I3 --- Nrv [10/226] Number of radial velocity
measurements
117- 127 F11.6 d dRV [1749/4786] Radial velocity baseline
129- 138 A10 "Y/M/D" Date Date (UTC) of last RV observation
140- 151 F12.9 m.s-1 RMS [2/20] RMS, RV residuals to the best-fit
model
153- 163 F11.9 m.s-1 RMSexp [3.5/6.6] Expected RV residuals
165- 175 F11.9 m.s-1 sigjit [1.7/5.2] Expected stellar jitter,
Section 4.2
177- 191 E15.6 m/s dRMS [-0.97/1643] Improvement in RMS
193 I1 --- NsS [0/1] Number, RV-detected sub-Saturns
195 I1 --- Ngp [0/2] Number, RV-detected giant planets
197 I1 --- Nsc [0/1] Number, RV-detected stellar
companions
199 I1 --- Trend [0/1] RV Trend detected (1=Yes, 0=No)
208 I1 --- Nntp [0/2] Number of non-transiting companions
detected
210- 224 E15.6 --- FAP [2.4e-40/1]? False alarm probability
226- 243 F18.10 --- dBIC [-227801.5/6.7] Difference, Bayesian
Information Criterion (3)
245- 255 A11 --- Model Model Name
257- 272 E16.6 m.s-1.d-1 dvdt [-0.03/0.04] Measured RV trend
274- 288 F15.13 m.s-1.d-1 e_dvdt [0/0.03] Uncertainty in dvdt
290- 304 F15.11 --- snr-dvdt [0.05/112.3] Signal-to-noise, dvdt
306- 318 F13.11 Mjup Mpsini05 [0.05/4.8] 3σ upper limit on Mp
sini at 5au based on the trend
320- 332 F13.10 Mjup Mpsini10 [0.2/19.2] 3σ upper limit on Mp
sini at 10au based on the trend
334- 346 F13.10 Mjup Mpsini20 [0.8/76.6] 3σ upper limit on Mp
sini at 20au based on the trend
--------------------------------------------------------------------------------
Note (1): Object names are linked in between tables in this work using
this field. This is the 5-digit KOI number (left-filled with zeroes).
Note (2): From Fulton & Petigura (2018, J/AJ/156/264)
Note (3): Difference in the Bayesian Information Criterion with and without
the addition of the companion (or trend). Negative values indicate that
an N+1-planet model is preferred (see also Table 3)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Syst System name used to link tables in this
work (1)
8- 20 A13 --- Kepler Kepler planetary system if any
22- 30 A9 --- KOI KOI-based planet name if any (2)
32- 47 F16.9 d Per [0.6/119297]? Planet orbital period, days
49- 60 F12.6 d e_Per [0.0005/10285]? Uncertainty in Per
62- 76 F15.9 d b_Per [0.6/19144] Minimum period
78- 91 F14.11 au a [0.01/52.2]? Planet orbital semi-major
axis
93 I1 au e_a [3]? Uncertainty in a
95- 106 F12.9 au b_a [9.8/14.7]? Minimum semi-major axis
108- 120 F13.10 Rgeo Rp [0.2/11.3]? Planetary radius, Earth units
122- 134 F13.11 Rgeo e_Rp [0.02/0.7]? Uncertainty in Rp
136- 146 F11.6 m.s-1 K [0.01/2196]? RV semi-amplitude (3)
148- 155 F8.6 m.s-1 e_K [0.1/5.3]? Uncertainty in K (3)
157- 171 E15.6 --- Mpusini [3.3e-08/0.3]? Planet to star mass ratio
173- 187 E15.6 --- e_Mpusini [1.4e-06/0.003]? Uncertainty in Mpusini
189- 203 E15.6 Mjup Mpsini [2.7e-05/629]? Planet
mass*sin(inclination) ;
Jupiter units (3)
205- 219 F15.12 Mjup e_Mpsini [0.001/21]? Uncertainty in mpsini (3)
221- 233 F13.10 Mjup b_Mpsini [0.6/15.5]? Minimum, mpsini (3)
235- 253 F19.12 Mgeo Mp-earth [0.008/199876]? Planet
mass*sin(inclination)
255- 269 F15.10 Mgeo e_Mp-earth [0.4/6663]? Uncertainty in Mp-earth
271- 283 F13.10 g.cm-3 rhop [0.19/18.5]? Mean planet density (3)
285- 298 F14.11 g.cm-3 e_rhop [0.04/14]? Uncertainty in rhop (3)
300- 313 F14.12 --- e [0/0.7]? Orbital eccentricity (3)
315- 328 F14.12 --- e_e [0/0.4]? Uncertainty in e (3)
330- 334 F5.3 Msun Mstar [0.67/1.7] Star mass
336- 348 F13.11 Msun e_Mstar [0.01/0.2]? Uncertainty in Mstar
350- 358 E9.6 m.s-1.d-1 dvdt [-0.025/0.04] Measured RV trend
360- 367 F8.6 m.s-1.d-1 e_dvdt [0.0001/0.02] Uncertainty in dvdt
369- 383 F15.11 --- snr-dvdt [0.07/114] Signal-to-noise, dvdt
385- 399 E15.6 --- FAP [2.4e-40/1]? False alarm probability
401- 416 F16.8 --- dBIC [-227802/-10]? Difference, Bayesian
Information Criterion (4)
418- 426 A9 --- Disp Disposition ("confirmed": 184 occurrences;
"candidate": 3 occurrences)
428 A1 --- Flag Flag (5)
--------------------------------------------------------------------------------
Note (1): Object names are linked in between tables in this work using
this field. This is the 5-digit KOI number (left-filled with zeroes).
Note (2): Non-transiting companions are given KOI indices beginning
with KNNNN.10 for consistency with Marcy+ (2014, J/ApJS/210/20).
For names, companions with planetary masses are given lowercase
letters, companions with stellar masses are given uppercase letters,
and companions with ambiguous masses are left nameless.
Note (3): Values are fixed for planets with no reported errors on
these values. Planet masses are based on a mass-radius relation
(Weiss & Marcy 2014ApJ...783L...6W 2014ApJ...783L...6W) and eccentricities are
circular.
Note (4): Difference in the Bayesian Information Criterion with and without
the addition of the companion (or trend). Negative values indicate that
an N+1-planet model is preferred (see also Table 3)
Note (5):
A = Planet candidate due to uncertain orbital period or low significance.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Syst System name used to link tables in this work (1)
8- 20 A13 --- Planet Planet name (2)
22- 30 A9 --- KOI KOI-based planet name (2)
32 A1 --- l_Per Limit flag on Per
34- 41 E8.4 d Per [22.26/119000] Planet orbital period
43- 50 E8.6 d e_Per [0.0006/10000]? Uncertainty in Per
52 A1 --- l_a Limit flag on a
54- 58 F5.2 au a [0.15/52.2] Planet orbital semi-major axis
60- 62 F3.1 au e_a [3.0]? Uncertainty in a
64 A1 --- l_K Limit flag on K
66- 71 F6.1 m.s-1 K [3.5/2195.1] RV semi-amplitude
73- 75 F3.1 m.s-1 e_K [0.5/5]? Uncertainty in K
77 A1 --- l_Msini Limit flag on Msini
79- 85 F7.3 Mgeo Msini [0.05/629] Planet mass * sin(inclination)
87- 92 F6.3 Mgeo e_Msini [0.01/21]? Uncertainty in Msini
94- 100 F7.5 --- e [0/0.7]? Orbital eccentricity
102- 108 F7.5 --- e_e [0.0002/0.4]? Uncertainty in e
110- 131 A22 --- FAP False alarm probability
133- 155 F23.15 --- dBIC [-227802/-10]? Difference, Bayesian Information
Criterion (3)
157 A1 --- New Newly discovered companion? (4)
159 A1 --- Flag Flag on modeling (5)
--------------------------------------------------------------------------------
Note (1): Object names are linked in between tables in this work using
this field. This is the 5-digit KOI number (left-filled with zeroes).
Note (2): Non-transiting companions are given KOI indices beginning
with KNNNN.10 for consistency with Marcy+ (2014, J/ApJS/210/20).
For names, companions with planetary masses are given lowercase
letters, companions with stellar masses are given uppercase letters,
and companions with ambiguous masses are left nameless.
Note (3): Difference in the Bayesian Information Criterion with and without
the addition of the companion (or trend). Negative values indicate that
an N+1-planet model is preferred (see also Table 3)
Note (4): Y = newly discovered in the KGPS data;
other companions were previously announced in the literature, and we
update their orbits and masses based on our new RVs.
Note (5): Flags and comments as follows:
A = Trend;
B = TTV detection preceded RV discovery; the eccentricity of
KOI-142c is 0.05 based on TTVs;
C = Automated routine fails to find planet (long-period structure
is evident but no peak is strongly preferred);
D = Period ambiguous because of aliasing (91 or 122 days);
E = Peak power at P∼360 days; 2000 day orbit preferred;
F = Kepler-454d is contemporaneously announced in
Bonomo+ (2023, J/A+A/677/A33), but their RVs were not available
at the time of our analysis
G = The eccentricity of the companion is poorly constrained
because of time sampling, with either a circular or
substantially eccentric model providing comparably good fits;
H = Automated routine places companion at P=6000 days because of
window function; a much longer period is preferred;
I = Known stellar companion (Zhang+ 2023AJ....165...73Z 2023AJ....165...73Z).
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 22-Feb-2024