J/AJ/152/8 Impact of stellar multiplicity on planetary systems I. (Kraus+, 2016)
The impact of stellar multiplicity on planetary systems. I. The ruinous
influence of close binary companions.
Kraus A.L., Ireland M.J., Huber D., Mann A.W., Dupuy T.J.
<Astron. J., 152, 8-8 (2016)>
=2016AJ....152....8K 2016AJ....152....8K (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Effective temperatures ;
Stars, masses ; Stars, distances
Keywords: binaries: close - binaries: general - binaries: visual -
planets and satellites: detection -
planets and satellites: dynamical evolution and stability -
planets and satellites: formation
Abstract:
The dynamical influence of binary companions is expected to profoundly
influence planetary systems. However, the difficulty of identifying
planets in binary systems has left the magnitude of this effect
uncertain; despite numerous theoretical hurdles to their formation and
survival, at least some binary systems clearly host planets. We
present high-resolution imaging of 382 Kepler Objects of Interest
(KOIs) obtained using adaptive-optics imaging and nonredundant
aperture-mask interferometry on the Keck II telescope. Among the full
sample of 506 candidate binary companions to KOIs, we super-resolve
some binary systems to projected separations of <5au, showing that
planets might form in these dynamically active environments. However,
the full distribution of projected separations for our planet-host
sample more broadly reveals a deep paucity of binary companions at
solar-system scales. For a field binary population, we should have
found 58 binary companions with projected separation ρ<50au and
mass ratio q>0.4; we instead only found 23 companions (a 4.6σ
deficit), many of which must be wider pairs that are only close in
projection. When the binary population is parametrized with a
semimajor axis cutoff acut and a suppression factor inside that
cutoff Sbin, we find with correlated uncertainties that inside
acut=47-23+59au, the planet occurrence rate in binary systems is
only Sbin=0.34-0.15+0.14 times that of wider binaries or single
stars. Our results demonstrate that a fifth of all solar-type stars in
the Milky Way are disallowed from hosting planetary systems due to the
influence of a binary companion.
Description:
We list all of the observed KOIs and their stellar parameters in
Table1, divided into the likely planet hosts (359 KOIs that have been
confirmed or remain as candidates) and the false positives (23 stars
that have been rejected).
We observed our targets with the Keck II telescope and either natural
guide star or laser guide star AO in vertical angle mode. Our
observations were taken over the space of 22 half or full nights
between 2012 May and 2014 August. All observations were conducted with
the facility adaptive optics imager NIRC2, which also has a 9-hole
aperture mask installed in a cold filter wheel near the pupil stop.
All observations used the smallest pixel scale (9.952±0.002mas/pix)
and we corrected for geometric distortion using their NIRC2 distortion
solution. We summarize the salient details of our imaging observations
in the same tables as our detection limits (Table2 and Table4).
Our Non-Redundant aperture Masking (NRM) observations were used to
identify 26 candidate companions among the 346 KOIs observed with this
technique, revealing candidates at projected separations as low as
16mas (1/3λ/D). We summarize the detection limits and the
details of the observations in Table2, and list the candidate
companions and their observed properties in Table3. The median target
had contrast limits of ΔK'=4.3mag at ρ=40mas (0.8λ/D)
and ΔK'=3.0mag at ρ=20mas (0.4λ/D). The nominal limit
at ρ=40mas also applies for all larger separations, though for
most targets this limit was superceded by imaging at ρ∼100-150mas.
Our imaging observations have identified 486 candidate companions
among the full sample of 382 KOIs. We summarize the detection limits
and the details of the observations in Table4, and list the 427
candidate companions measured with aperture photometry in Table5. In
Table6, we list the 43 close pairs and 7 close triples for which we
used our multi-PSF fitting algorithm, as well as the observed
properties of the candidate companion(s) with respect to the brightest
star in the system. The median target had contrast limits of
ΔK'=5.5mag at ρ=150mas (3λ/D), typically superceding
the masking limits at ρ≳100mas. At wide separations, the
median limit (corresponding to the fainter majority of stars that were
not observed with the coronagraph) were ΔK'=8.0mag at ρ>1''.
For coronagraphic data, we achieved contrast limits as deep as
ΔK'>12mag at wide separations (≳2'', in the sky- and
readnoise-limited regime).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 164 382 Kepler objects of interest
table2.dat 51 346 Keck/NIRC2 Non-Redundant aperture Masking (NRM)
detection limits
table3.dat 64 26 Keck/NIRC2 Non-Redundant aperture Masking (NRM)
candidate companions
table4.dat 81 465 Keck/NIRC2 imaging detection limits
table5.dat 82 454 Keck/NIRC2 imaging candidate companions
table6.dat 82 59 Keck/NIRC2 PSF-fitting candidate companions
table7.dat 34 463 System properties for candidate binary systems
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See also:
J/A+A/576/A88 : RVs of 8 KOI eclipsing binaries (Lillo-Box+, 2015)
J/ApJS/218/26 : Parameters of planets orbiting coolest dwarfs (Swift+, 2015)
J/A+A/566/A103 : Kepler planet host candidates imaging (Lillo-Box+, 2014)
J/AJ/147/146 : Spectroscopy of Tuc-Hor candidate members (Kraus+, 2014)
J/ApJ/779/188 : Spectra of nearby late K and M Kepler stars (Mann+, 2013)
J/ApJ/753/90 : Parameters of K5 and later type Kepler stars (Mann+, 2012)
J/A+A/546/A10 : Multiplici. in transiting planet-host stars (Lillo-Box+, 2012)
J/ApJ/757/141 : Companion IR detection limits in young assoc. (Kraus+, 2012)
J/ApJ/745/19 : Binary systems in Taurus-Auriga (Kraus+, 2012)
J/AJ/144/42 : Infrared photometry of 90 KOIs (Adams+, 2012)
J/ApJ/731/8 : Multiple star formation in Taurus-Auriga (Kraus+, 2011)
J/AJ/142/160 : Kepler Mission. II. Eclipsing binaries in DR2 (Slawson+, 2011)
J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)
J/AJ/134/2340 : Membership of Praesepe and Coma Berenices (Kraus+, 2007)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Type Candidate type (C=Candidate or confirmed planet
host, FP=False Positive)
4- 7 A4 --- --- [KOI-]
8- 11 I4 --- KOI Kepler Object of Interest number
13- 14 I2 h RAh Hour of Right Ascension (J2000)
16- 17 I2 min RAm Minute of Right Ascension (J2000)
19- 24 F6.3 s RAs Second of Right Ascension (J2000)
26 A1 --- DE- Sign of the Declination (J2000)
27- 28 I2 deg DEd Degree of Declination (J2000)
30- 31 I2 arcmin DEm Arcminute of Declination (J2000)
33- 37 F5.2 arcsec DEs Arcsecond of Declination (J2000)
39- 43 F5.2 mag Kpmag [7.84/17.48] Kepler magnitude (mKp)
45- 49 F5.2 mag Ksmag [6.49/13.56] 2MASS Ks band magnitude (mKs)
51- 54 I4 K Teff [3068/9071] Effective temperature (Teff)
56- 58 I3 K e_Teff [58/317] Uncertainty in Teff
60- 64 F5.3 Msun Mass1 [0.125/1.849] Primary mass (Mprim)
66- 70 F5.3 Msun E_Mass1 [0.021/0.403] Upper uncertainty in Mass1
72- 76 F5.3 Msun e_Mass1 [0.01/0.485] Lower uncertainty in Mass1
78- 83 F6.1 pc UDist [33.9/2761.6] Uncorrected distance (1)
85- 89 F5.1 pc E_UDist [1.1/993.9] Upper uncertainty in UDist
91- 95 F5.1 pc e_UDist [1.1/378.7] Lower uncertainty in UDist
97-102 F6.1 pc CDist [33.9/2764.3] Corrected distance (1)
104-110 A7 --- --- [Kepler-]
111-113 I3 --- Kepler ? Kepler number when available (for the hosts
of confirmed planets)
115-122 A8 --- OName Other name
124-164 A41 --- Ref Reference by which the false positives have
been rejected (2)
--------------------------------------------------------------------------------
Note (1): Distances are listed both with and without the luminosity correction
applied for flux contributions for companions that were unresolved in
2MASS. Targets were selected for observation using uncorrected distances,
mostly the spectrophotometric distances described in Section 2, while
isochronal distances that were corrected for multiplicity are used to
calculate physical projected separations. Binary systems are weighted by a
1/Vmax weighting in our analysis to avoid Malmquist bias.
Note (2): Many of the false positives are labeled as such on the Kepler
Community Follow-On Project (CFOP) website
(https://exofop.ipac.caltech.edu/cfop.php) so we attribute those labels to
specific community members when their identities are known.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 A4 --- --- [KOI-]
5- 8 I4 --- KOI Kepler Object of Interest number
10- 17 F8.2 d MJD Modified Julian Date of the observation
19- 28 A10 "Y:M:D" Date UT date of the observation
30- 31 I2 --- Nf [3/18] Number of frames obtained (Nframes)
33- 36 F4.2 mag L15 [0/4.12] Magnitude limit at 15mas projected
separation
38- 41 F4.2 mag L20 [0.01/4.85] Magnitude limit at 20mas projected
separation
43- 46 F4.2 mag L30 [0.33/5.78] Magnitude limit at 30mas projected
separation
48- 51 F4.2 mag L40-160 [0.55/6] Magnitude limit between 40-160mas
projected separation
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Type Candidate type (C=Candidate, FP=False Positive,
or DD=Duplicate Detection)
4- 7 A4 --- --- [KOI-]
8- 11 I4 --- KOI Kepler Object of Interest number
13- 15 A3 --- m_KOI KOI multiplicity (1)
17- 24 F8.2 d MJD Modified Julian Date of the observation
26- 30 F5.3 mag dKmag [0.001/5.39] Magnitude difference in K' band
(ΔK')
32- 36 F5.3 mag e_dKmag [0.006/0.456] Error in dKmag
38- 44 F7.3 mas Sep [16.089/208.52] Separation ρ
46- 50 F5.3 mas e_Sep [0.08/7.1] Error in Sep
52- 58 F7.3 deg PA [3.229/348.651] Position angle
60- 64 F5.3 deg e_PA [0.087/4.71] Error in PA
--------------------------------------------------------------------------------
Note (1): KOI-2032 B-C was also detected as part of a triple system in imaging
data; we use the imaging results to achieve consistent astrometry and
photometry across all three components, but we list the Non-Redundant
aperture Masking (NRM) detection here for completeness. KOI-1613 was
previously identified as a candidate companion by Law et al.
2014ApJ...791...35L 2014ApJ...791...35L.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Type Candidate type (C=Candidate, FP=False Positive)
4- 7 A4 --- --- [KOI-]
8- 11 I4 --- KOI Kepler Object of Interest number
13- 20 F8.2 d MJD Modified Julian Date of the observation
22- 23 A2 --- Filt Filter used (Kc or Kp)
24 A1 --- --- [+]
25- 27 A3 --- Inst Instrument (coronagraph) used (C06)
29- 30 I2 --- Nf [1/17] Number of frames obtained (Nfram)
32- 37 F6.2 s Tint [10/340] Integration time (tint)
39- 41 F3.1 mag L150 [2.9/6.9]? Magnitude limit at 150mas projected
separation
43- 45 F3.1 mag L200 [3.6/7.6]? Magnitude limit at 200mas projected
separation
47- 49 F3.1 mag L250 [3.8/7.7]? Magnitude limit at 250mas projected
separation
51- 53 F3.1 mag L300 [4/8]? Magnitude limit at 300mas projected
separation
55- 57 F3.1 mag L400 [4.6/8.8] Magnitude limit at 400mas projected
separation
59- 61 F3.1 mag L500 [4.6/9] Magnitude limit at 500mas projected
separation
63- 66 F4.1 mag L700 [3.7/10] Magnitude limit at 700mas projected
separation
68- 71 F4.1 mag L1000 [4.6/10.7] Magnitude limit at 1000mas projected
separation
73- 76 F4.1 mag L1500 [5/12.1] Magnitude limit at 1500mas projected
separation
78- 81 F4.1 mag L2000 [4.9/12.7] Magnitude limit at 2000mas projected
separation
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table[56].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 A2 --- Type Candidate type (C=Candidate, FP=False Positive, or
DD=Duplicate Detection) (1)
4- 7 A4 --- --- [KOI-]
8- 11 I4 --- KOI Kepler Object of Interest number
13- 15 A3 --- m_KOI KOI multiplicity
17- 24 F8.2 d MJD Modified Julian Date of the observation
26- 27 A2 --- Flt [Kp] Filter used (Kp)
28 A1 --- --- [+ ]
29- 31 A3 --- Inst Instrument (coronagraph) used (C06)
33- 34 I2 --- Nf [1/17] Number of frames obtained (Nframes)
36- 42 F7.2 mas Sep [53.57/7949.4] Projected separation ρ
44- 47 F4.2 mas e_Sep [0.08/7.6] Uncertainty in Sep
49- 55 F7.3 deg PA [0.372/359.425] Position angle
57- 61 F5.3 deg e_PA [0.005/1.616] Uncertainty in PA
63- 68 F6.3 mag dmag [-0.058/13.512] Magnitude difference between
companions (Δm)
70- 74 F5.3 mag e_dmag [0.001/0.173] Uncertainty in dmag
76- 82 A7 --- Ref Reference(s) (2)
--------------------------------------------------------------------------------
Note (1): This note about the type is defined as follows depending on the table:
* Table5: When candidate companions were detected in both coronagraphic
and non-coronagraphic imaging, we list the non-coronagraphic entry
first and use it for all analysis; the coronagraphic detections
are listed at the end of the table for completeness, but are not
used further;
* Table6: When candidate companions were detected in both Non-Redundant
aperture Masking (NRM) observations and imaging observations, we
use the NRM detection for all analysis; the imaging measurements
are listed at the end of this table for completeness, but are not
used further. The exceptions are KOI-0005 and KOI-0854, where the
imaging and NRM detections represent separate companions in
compact triple systems.
Note (2): Reference codes are defined as follows:
1 = Howell et al. 2011 (Cat. J/AJ/142/19);
2 = Adams et al. 2012 (Cat. J/AJ/144/42);
3 = Lillo-Box et al. 2012 (Cat. J/A+A/546/A10);
4 = Horch et al. (2012AJ....144..165H 2012AJ....144..165H);
5 = Adams et al. (2013AJ....146....9A 2013AJ....146....9A);
6 = Law et al. (2014ApJ...791...35L 2014ApJ...791...35L);
7 = Dressing et al. (2014AJ....148...78D 2014AJ....148...78D);
8 = Lillo-Box et al. 2014 (Cat. J/A+A/566/A103);
9 = Wang et al. (2014ApJ...791..111W 2014ApJ...791..111W);
10 = Gilliland et al. (2015AJ....149...24G 2015AJ....149...24G);
11 = Everett et al. (2015AJ....149...55E 2015AJ....149...55E);
12 = Borucki et al. (2013Sci...340..587B 2013Sci...340..587B);
13 = Daemgen et al. (2009A&A...498..567D 2009A&A...498..567D);
14 = Narita et al. (2010PASJ...62..779N 2010PASJ...62..779N).
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Byte-by-byte Description of file: table7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 A1 --- Gr Group type (M=Masking, B=PSF fitting binary,
T=PSF fitting triple, or I=Imaging)
3- 6 A4 --- --- [KOI-]
7- 10 I4 --- KOI Kepler Object of Interest number
12 A1 --- l_Mass2 [<] Upper limit flag on Mass2
13- 18 F6.3 Msun Mass2 [0.099/1.597] Secondary mass (Msec)
20 A1 --- l_M2/M1 [<] Upper limit flag on M2/M1
21- 26 F6.3 --- M2/M1 [0.068/1.021] Ratio of secondary to primary
masses (q)
28- 34 F7.1 AU Sep [4.7/12439.1] Separation
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History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 12-Sep-2016