J/AJ/168/129 Planet-host binary systems. IV. Radius distrib. (Sullivan+, 2024)
Revising properties of planet-host binary systems.
IV. The radius distribution of small planets in binary star systems is dependent
on stellar separation.
Sullivan K., Kraus A.L., Berger T.A., Dupuy T.J., Evans E., Gaidos E.,
Huber D., Ireland M.J., Mann A.W., Petigura E.A., Thao Pa C., Wood M.L.,
Zhang J.
<Astron. J., 168, 129 (2024)>
=2024AJ....168..129S 2024AJ....168..129S
ADC_Keywords: Stars, double and multiple; Exoplanets; Effective temperatures;
Stars, diameters; Spectra, optical; Infrared
Keywords: Binary stars ; Super Earths ; Exoplanets ; Mini Neptunes ;
Exoplanet formation ; Planet hosting stars ; Stellar astronomy
Abstract:
Small planets (Rp≤4R⊕) are divided into rocky super-Earths
and gaseous sub-Neptunes separated by a radius gap, but the mechanisms
that produce these distinct planet populations remain unclear. Binary
stars are the only main-sequence systems with an observable record of
the protoplanetary disk lifetime and mass reservoir, and the
demographics of planets in binaries may provide insights into planet
formation and evolution. To investigate the radius distribution of
planets in binary star systems, we observed 207 binary systems hosting
283 confirmed and candidate transiting planets detected by the Kepler
mission, then recharacterized the planets while accounting for the
observational biases introduced by the secondary star. We found that
the population of planets in close binaries (ρ≤100au) is
significantly different from the planet population in wider binaries
(ρ>300au) or single stars. In contrast to planets around single
stars, planets in close binaries appear to have a unimodal radius
distribution with a peak near the expected super-Earth peak of Rp
∼1.3R⊕ and a suppressed population of sub-Neptunes. We
conclude that we are observing the direct impact of a reduced disk
lifetime, smaller mass reservoir, and possible altered distribution of
solids reducing the sub-Neptune formation efficiency. Our results
demonstrate the power of binary stars as a laboratory for exploring
planet formation and as a controlled experiment of the impact of
varied initial conditions on mature planet populations.
Description:
We assembled our list of binary stars from a variety of sources. We
primarily used the catalog of binary stars from
Furlan+ (2017, J/AJ/153/71), which in turn was a compilation of
several sources of high-resolution imaging of KOIs. We supplemented
this catalog with Robo-AO imaging presented in
Ziegler+ (2018, J/AJ/155/161) and new adaptive optics (AO) imaging
using the Near Infra Red Camera 2 (NIRC2) at the Keck Observatory.
See Section 2.1.
We present new AO imaging of KOIs using the NIRC2 AO camera on the
Keck II telescope, obtained as part of an ongoing survey of the
multiplicity of Kepler planet-hosting stars. The typical observing
strategy was described by Kraus+ (2016, J/AJ/152/8). To briefly recap,
a modest number of 20s exposures (typically 4-8, with more in marginal
conditions) were obtained using a mix of natural guide star and laser
guide star AO on nights spanning 2015-2022, using the narrow camera
and the broadband filter centered at 2.2um. See Section 2.2.
We took spectroscopic observations of the full sample of KOIs with the
LRS on the 10m Hobby-Eberly Telescope (HET) between 2021 April 2 and
2023 September 26 at the McDonald Observatory. See Section 2.3.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 42 65 Excluded systems
table2.dat 134 286 System parameters for each source
table3.dat 64 82 New Keck/NIRC2 observations
table4.dat 121 286 Stellar parameter fit results for all KOIs in
our sample
table5.dat 160 404 Planet parameter fit results for all planets in
the binary KOI sample
--------------------------------------------------------------------------------
See also:
J/ApJ/696/L84 : Primordial circumstellar disks in binary syst. (Cieza+, 2009)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)
J/AJ/144/42 : Infrared photometry of 90 KOIs (Adams+, 2012)
J/ApJ/751/115 : Millimeter emission from Taurus binary systems (Harris+, 2012)
J/ApJ/745/19 : Binary systems in Taurus-Auriga (Kraus+, 2012)
J/A+A/546/A10 : Mult. in transiting planet-host stars (Lillo-Box+, 2012)
J/ApJS/204/24 : Kepler planetary candidates. III. (Batalha+, 2013)
J/A+A/556/A15 : Effective temperature scale of M dwarfs (Rajpurohit+, 2013)
J/ApJ/795/64 : Exoplanet physical parameters (Foreman-Mackey+, 2014)
J/A+A/566/A103 : Kepler planet host candidates imaging (Lillo-Box+, 2014)
J/ApJ/809/8 : Terrestrial planet occurrence rates for KOIs (Burke+, 2015)
J/ApJ/813/130 : Kepler multiple transiting planet systems (Wang+, 2015)
J/AJ/152/18 : Robo-AO Kepler planetary cand. survey. II. (Baranec+, 2016)
J/AJ/152/8 : Impact of stellar mult. on planetary syst. I. (Kraus+, 2016)
J/AJ/154/109 : California-Kepler Survey (CKS). III. Radii (Fulton+, 2017)
J/AJ/153/71 : Kepler follow-up observation program. I. (Furlan+, 2017)
J/ApJS/229/30 : Revised properties of Q1-17 Kepler targets (Mathur+, 2017)
J/ApJ/866/99 : Radii of KIC stars & planets using Gaia DR2 (Berger+, 2018)
J/ApJS/235/38 : Kepler planet. cand. VIII. DR25 reliability (Thompson+, 2018)
J/AJ/155/161 : Stars nearby Robo-AO Kepler planetary cand. (Ziegler+, 2018)
J/AJ/160/108 : Gaia-Kepler stellar properties catalog. II. (Berger+, 2020)
J/ApJS/247/28 : K2 star param. from Gaia & LAMOST (Hardegree-Ullman+, 2020)
J/AJ/161/265 : Compared rot. periods for 1189 CKS host stars (David+, 2021)
J/AJ/161/134 : Stellar & planetary comp. within 25pc (Hirsch+, 2021)
J/AJ/162/75 : Speckle obs. TESS exoplanet host stars. II. (Lester+, 2021)
J/AJ/161/171 : THYME. V. Discovering a new stellar assoc. (Tofflemire+, 2021)
J/AJ/163/179 : The California-Kepler Survey. X. (Petigura+, 2022)
J/ApJ/928/134 : NIR phot. & optical veiling in T Tauri stars (Sullivan+, 2022)
J/AJ/165/177 : Planet-Host Binary Systems. III. (Sullivan+, 2023)
J/AJ/165/85 : THYME. IX. MELANGE-4 association members (Wood+, 2023)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [KOI-]
5- 8 I04 --- KOI [5/6610] Kepler object of interest
10- 24 A15 --- Reason Reason for exclusion
26- 42 A17 --- Source Source of exclusion information
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I04 --- KOI [42/8253] Kepler object of interest identifier
6- 9 F4.2 arcsec Sep [0.02/3.72] Angular separation
11- 20 A10 "Y/M/D" Date Observation date
22- 26 F5.2 mag rmag [9.33/17.11] r'-band magnitude
28- 31 I4 --- SNR [37/2095] Signal-to-Noise Ratio
33- 36 F4.2 mag dmi [0.01/4.3]? Observed contrast, i-band
magnitude
38- 41 F4.2 mag e_dmi [0.01/3.5]? Uncertainty in dmi
43- 46 F4.2 mag dmLP600 [0.03/5]? Observed contrast, LP600 magnitude
48- 51 F4.2 mag e_dmLP600 [0.02/0.6]? Uncertainty in dmLP600
53- 56 F4.2 mag dmGaia [0/5.3]? Observed contrast, Gaia G-band
magnitude
58- 61 F4.2 mag e_dmGaia [0/0.1]? Uncertainty in dmGaia
63- 66 F4.2 mag dm562nm [0/4.3]? Observed contrast, 562nm magnitude
68- 71 F4.2 mag e_dm562nm [0.15]? Uncertainty in dm562nm
73- 76 F4.2 mag dm692nm [0.12/6]? Observed contrast, 692nm magnitude
78- 81 F4.2 mag e_dm692nm [0.15/0.3]? Uncertainty in dm692nm
83- 86 F4.2 mag dm880nm [0.05/4.8]? Observed contrast, 880nm
magnitude
88- 91 F4.2 mag e_dm880nm [0.1/1]? Uncertainty in dm880nm
93- 96 F4.2 mag dmJ [0/5.1]? Observed contrast, J-band magnitude
98-101 F4.2 mag e_dmJ [0.01/0.4]? Uncertainty in dmJ
103-107 F5.2 mag dmK [0/3.6]? Observed contrast, K-band magnitude
109-112 F4.2 mag e_dmK [0/0.5]? Uncertainty in dmK
114-134 A21 --- Ref References (1)
--------------------------------------------------------------------------------
Note (1): References as follows:
F17 = Furlan+ 2017, J/AJ/153/71
A12 = Adams+ 2012, J/AJ/144/42
H11 = Howell+ 2011, J/AJ/142/19
B16 = Baranec+ 2016, J/AJ/152/18
LB12 = Lillo-Box+ 2012, J/A+A/546/A10
LB14 = Lillo-Box+ 2014, J/A+A/566/A103
K16 = Kraus+ 2016, J/AJ/152/8
-- = Any unmarked K magnitudes are from this work.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [KOI-]
5- 8 I04 --- KOI [163/8077] Kepler object of interest identifier
10- 17 F8.2 d MJD Modified Julian Date of Observation
(JD-2400000.5)
19- 20 A2 --- Filt Filter
22- 23 I2 --- Nf [1/16] Number of frames
25- 31 F7.2 arcsec rho [41.5/1868] Separation
33- 37 F5.2 arcsec e_rho [1.5/11] Uncertainty in rho
39- 45 F7.3 deg PA [3.8/344] Position angle, east of north
47- 51 F5.3 deg e_PA [0.04/6] Uncertainty in PA
53- 58 F6.3 mag dmag [-0.21/3.21] Delta magnitude in Filt
60- 64 F5.3 mag e_dmag [0/0.4] Uncertainty in Δmag
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I04 --- KOI [42/8253] Kepler object of interest
identifier
6- 9 I4 K Teff1 [3493/6888] Stellar effective
temperature, component 1
11- 13 I3 K E_Teff1 [3/305] Upper uncertainty in Teff1
15- 18 I4 K e_Teff1 [2/1904] Lower uncertainty in Teff1
20- 23 I4 K Teff2 [3016/6881] Stellar effective
temperature, component 2
25- 28 I4 K E_Teff2 [5/1799] Upper uncertainty in Teff2
30- 32 I3 K e_Teff2 [7/380] Lower uncertainty in Teff2
34- 37 I4 K Teffkep [2703/6995] Stellar effective
temperature, Kepler (1)
39- 41 I3 K e_Teffkep [58/297]? Uncertainty in Teffkep
43- 47 F5.3 Rsun Rstar1 [0.19/1.5] Radius, solar units,
component 1
49- 53 F5.3 Rsun E_Rstar1 [0.003/0.3] Upper uncertainty in Rstar1
55- 59 F5.3 Rsun e_Rstar1 [0.003/0.25] Lower uncertainty in Rstar1
61- 65 F5.3 --- Rstar2/Rstar1 [0.3/1.1] Ratio, radii, component 2 to 1
67- 71 F5.3 --- E_Rstar2/Rstar1 [0.002/1] Upper uncertainty in
Rstar2/Rstar1
73- 77 F5.3 --- e_Rstar2/Rstar1 [0.002/0.4] Lower uncertainty in
Rstar2/Rstar1
79- 83 F5.3 Rsun Rstarkep [0.1/3.4] Radius, solar units, Kepler (1)
85- 89 F5.3 Rsun e_Rstarkep [0.01/1.1]? Uncertainty in Rstarkep
91- 94 F4.2 --- fcorr-p [0.2/2.1]? Planetary radius correction
factor, if primary host
96- 99 F4.2 --- E_fcorr-p [0.02/1.2]? Upper uncertainty in fcorr-p
101- 104 F4.2 --- e_fcorr-p [0.02/0.4]? Lower uncertainty in fcorr-p
106- 109 F4.2 --- fcorr-s [0.5/4.4]? Planetary radius correction
factor, if secondary host
111- 114 F4.2 --- E_fcorr-s [0.03/1.5]? Upper uncertainty in fcorr-s
116- 119 F4.2 --- e_fcorr-s [0.03/1.1]? Lower uncertainty in fcorr-s
121 I1 --- Source [1/2] Source (1)
--------------------------------------------------------------------------------
Note (1): Kepler Teff and Rstar from Berger+ 2018, J/ApJ/866/99 (Source=1) or
Mathur+ 2017, J/ApJS/229/30 (Source=2) values for the composite stellar
system properties.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.2 --- KOIpl [42.01/8253.01] Kepler object of interest planet
identifier
9- 14 F6.2 Rgeo Rppri [0.29/520]? Planet radius, primary
as host
16- 20 F5.2 Rgeo E_Rppri [0.03/48]? Upper uncertainty in Rppri
22- 26 F5.2 Rgeo e_Rppri [0.03/48.1]? Lower uncertainty in Rppri
28- 34 F7.2 Rgeo Rpsec [0.37/1447]? Planet radius,
secondary as host
36- 41 F6.2 Rgeo E_Rpsec [0.05/130.1]? Upper uncertainty in Rpsec
43- 48 F6.2 Rgeo e_Rpsec [0.04/129]? Lower uncertainty in Rpsec
50- 55 F6.2 Rgeo Rpkep [0.36/577] Planet radius, Kepler (1)
57- 61 F5.2 Rgeo e_Rpkep [0/31] Uncertainty in Rpkep
63- 66 I4 K Teqpri [138/2908]? Planet equilibrium temperature,
secondary
68- 70 I3 K E_Teqpri [4/344]? Upper uncertainty in Teqpri
72- 74 I3 K e_Teqpri [4/401]? Lower uncertainty in Teqpri
76- 79 I4 K Teqsec [78/2615]? Planet equilibrium temperature,
secondary
81- 83 I3 K E_Teqsec [2/309]? Upper uncertainty in Teqsec
85- 87 I3 K e_Teqsec [2/321]? Lower uncertainty in Teqsec
89- 92 I4 K Teqkep [106/3653] Planet equilibrium temperature,
Kepler (1)
94- 101 F8.2 --- Spri [0.05/15155] Isolation, Earth units, primary as
host
103- 108 F6.2 --- E_Spri [0/945] Upper uncertainty in Spri
110- 115 F6.2 --- e_Spri [0/938] Lower uncertainty in Spri
117- 123 F7.2 --- Ssec [0.02/9992] Isolation, Earth units, secondary
as host
125- 130 F6.2 --- E_Ssec [0/730] Upper uncertainty in Ssec
132- 137 F6.2 --- e_Ssec [0/707] Lower uncertainty in Ssec
139- 146 F8.2 --- Skep [0.03/41864]?=-99 Isolation, Earth units,
Kepler (1)
148- 155 F8.2 --- e_Skep [0/29069]?=-99 Uncertainty in Skep
157- 160 I04 --- KOI Host star KOI number; column added by CDS
--------------------------------------------------------------------------------
Note (1): Kepler values from Thompson+ 2018, J/ApJS/235/38
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Sullivan et al. Paper I. 2022ApJ...935..141S 2022ApJ...935..141S
Sullivan & Kraus Paper II. 2022AJ....164..138S 2022AJ....164..138S
Sullivan et al. Paper III. 2023AJ....165..177S 2023AJ....165..177S Cat. J/AJ/165/177
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 12-Mar-2025