J/AJ/156/254 California-Kepler Survey.VI. Kepler multis & singles (Weiss+, 2018)
The California-Kepler Survey.
VI. Kepler multis and singles have similar planet and stellar properties
indicating a common origin.
Weiss L.M., Isaacson H.T., Marcy G.W., Howard A.W., Petigura E.A.,
Fulton B.J., Winn J.N., Hirsch L., Sinukoff E., Rowe J.F.
<Astron. J., 156, 254 (2018)>
=2018AJ....156..254W 2018AJ....156..254W (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets ; Effective temperatures ; Abundances, [Fe/H] ;
Rotational velocities ; Stars, masses ; Stars, diameters
Keywords: catalogs - planetary systems - planets and satellites: formation -
planets and satellites: fundamental parameters -
stars: fundamental parameters
Abstract:
The California-Kepler Survey (CKS) catalog contains precise stellar and
planetary properties for the Kepler planet candidates, including systems
with multiple detected transiting planets ("multis") and systems with
just one detected transiting planet ("singles", although additional planets
could exist). We compared the stellar and planetary properties of the
multis and singles in a homogeneous subset of the full CKS-Gaia catalog.
We found that sub-Neptune-sized singles and multis do not differ in their
stellar properties or planet radii. In particular: (1) The distributions of
stellar properties M*, [Fe/H], and vsini for the Kepler sub-Neptune-sized
singles and multis are statistically indistinguishable. (2) The radius
distributions of the sub-Neptune-sized singles and multis with P>3 days
are indistinguishable, and both have a valley at ∼1.8 R⊕. However,
there are significantly more detected short-period (P<3 days),
sub-Neptune-sized singles than multis. The similarity of the host-star
properties, planet radii, and radius valley for singles and multis suggests
a common origin. The similar radius valley, which is likely sculpted by
photo-evaporation from the host star within the first 100 Myr, suggests
that planets in both singles and multis spend much of the first 100 Myr
near their present, close-in locations. One explanation that is consistent
with the similar fundamental properties of singles and multis is that
many of the singles are members of multi-planet systems that underwent
planet-planet scattering.
Description:
In this paper (CKS VI), we use the refined stellar and planetary
properties presented in CKS VII (Fulton & Petigura. 2018AJ....156..264F 2018AJ....156..264F)
to compare a large, homogeneous, high-purity sample of Kepler singles and
multis. Where applicable, we also examine how the stellar and planetary
properties of the multis differ for system with two, three, and four or
more transiting planets.
The initial CKS data set consists of 1944 signals that were at one time
flagged as transiting planet candidates, orbiting 1222 stars that have Gaia
properties reported in DR2 (Cat. I/345). From these, we discarded the
signals that are now known to be false positives (as determined on either
the NASA Exoplanet Archive or in CKS I, Petigura et al. 2017, J/AJ/154/107),
removing 156 non-planetary signals around 104 stars. We then discarded
stars that are diluted by at least 5% by a second star in the Kepler
aperture, removing 88 planet candidates around 58 stars. We discarded
planets for which Mullally et al. (2015, J/ApJS/217/31) measured b>0.9, for
which the high impact parameters adversely affected our ability to
determine accurate planet radii, removing 137 planet candidates from
around 70 stars. We removed planet candidates for which the measured
signal-to-noise ratio (S/N) is less than 10 since these planets have poorly
determined radii and impact parameters, removing 48 planet candidates. We
also removed planet candidates with Rp>22.4 R⊕, which are likely
eclipsing binaries rather than planets. Of the four planet candidates with
Rp>22.4 R⊕, all four were singles, and three orbited giant stars
with log(g)<3.9. Systems that were originally multis but had been purified
to the extent that only one planet remained were excluded. After these
cuts, our sample included 892 high-purity planet candidates in multi-planet
systems around 349 stars.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 80 892 High purity CKS-Gaia multis
table3.dat 80 802 Bright multis and singles
--------------------------------------------------------------------------------
See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/ApJS/197/8 : Kepler's candidate multiple transiting planets
(Lissauer+, 2011)
J/ApJ/784/45 : Kepler's multiple planet candidates. III. (Rowe+, 2014)
J/ApJ/790/146 : Planets in Kepler's multi-transiting systems (Fabrycky+, 2014)
J/ApJ/813/130 : Kepler multiple transiting planet systems (Wang+, 2015)
J/ApJS/217/31 : Kepler planetary candidates. VI. 4yr Q1-Q16 (Mullally+, 2015)
J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars (Petigura+, 2017)
J/AJ/154/108 : California-Kepler Survey (CKS). II. Properties (Johnson+, 2017)
J/AJ/154/109 : California-Kepler Survey (CKS). III. Planet radii
(Fulton+, 2017)
J/AJ/155/48 : California-Kepler Survey (CKS). V. Masses and radii
(Weiss+, 2018)
J/AJ/155/89 : California-Kepler Survey (CKS). IV. Planets (Petigura+, 2018)
Byte-by-byte Description of file: table2.dat table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 A9 --- KOI Kepler Object of Interest identifier (K0NNNN.NN)
11- 15 F5.2 mag Kpmag [8.22/15.96] Kepler apparent magnitude
17- 22 F6.2 ppm CDPP [12.37/384.89] Combined differential photometric
precision (1)
24- 30 F7.2 K Teff [4589.65/6556.92] Effective temperature
32- 35 F4.2 [cm/s2] log(g) [3.56/4.63] Log surface gravity
37- 41 F5.2 [Sun] [Fe/H] [-0.47/0.42] Metallicity
43- 47 F5.1 km/s vsin(i) [0/456.7] Projected rotational velocity
49- 52 F4.2 Msun M* [0.7/1.58] Stellar mass
54- 57 F4.2 Rsun R* [0.67/3.17] Stellar radius
59- 65 F7.2 d Per [0.54/1071.23] Planetary period
67- 71 F5.2 Rgeo Rp [0.35/20.12] Planetary radius
73- 78 F6.2 --- S/N [10.25/104.29]? Model signal-to-noise ratio
(only in Table 3) (2)
80 I1 --- Ntp [1/7] Number of transiting planets surviving
our cuts
--------------------------------------------------------------------------------
Note (1): In the Kepler light curve over 6 hours.
Note (2): For a 1.5 Earth radii planet at 30 days.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Petigura et al., Paper I 2017AJ....154..107P 2017AJ....154..107P, Cat. J/AJ/154/107
Johnson et al., Paper II 2017AJ....154..108J 2017AJ....154..108J, Cat. J/AJ/154/108
Fulton et al., Paper III 2017AJ....154..109F 2017AJ....154..109F, Cat. J/AJ/154/109
Petigura et al., Paper IV 2018AJ....155...89P 2018AJ....155...89P, Cat. J/AJ/155/89
Weiss et al., Paper V 2018AJ....155...48W 2018AJ....155...48W, Cat. J/AJ/155/48
Fulton & Petigura., Paper VII 2018AJ....156..264F 2018AJ....156..264F
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 15-Apr-2019