J/A+A/689/A302 Multiplicity of stars with planets (Gonzalez-Payo+, 2024)
Multiplicity of stars with planets in the solar neighbourhood.
Gonzalez-Payo J., Caballero J.A., Gorgas J., Cortes-Contreras M.,
Gelvez-Ortiz M.-C., Cifuentes C.
<Astron. Astrophys. 689, A302 (2024)>
=2024A&A...689A.302G 2024A&A...689A.302G (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, double and multiple ; Exoplanets ;
Optical ; Stars, distances ; Proper motions
Keywords: astronomical data bases: miscellaneous - virtual observatory tools -
astrometry - binaries: general - binaries: visual - planetary systems
Abstract:
We intended to quantify the impact of stellar multiplicity on the
presence and properties of exoplanets.
We investigated all exoplanet host stars at less than 100 pc using the
latest astrometric data from Gaia DR3 and advanced statistical
methodologies. We complemented our search for common proper motion and
parallax companions with data from the Washington Double Star
catalogue and the literature. After excluding a number of systems
based on radial velocity data, and membership in clusters and open
associations, or with resolved ultracool companions, we kept 215
exoplanet host stars in 212 multiple-star systems.
We found 17 new companions in the systems of 15 known exoplanet host
stars, measured precise angular and projected physical separations and
position angles for 236 pairs of stars, compiled key parameters for
276 planets in multiple systems, and established a comparison sample
comprising 687 single stars with exoplanets. With all of this, we
statistically analysed a series of hypothesis regarding planets in
multiple stellar systems. Although they are only statistically
significant at a 2σ level, our analysis pointed to several
interesting results on the comparison in the mean number of planets in
multiple versus single stellar systems and the tendency of high mass
planets to be located in closer orbits in multiple systems. We confirm
that planets in multiple systems tend to have orbits with larger
eccentricities than those in single systems. In particular, we found a
significant (>4σ) preference for planets to exhibit high
orbital eccentricities at small ratios between star-star projected
physical separations and star-planet semi-major axes.
Description:
We compiled all stars with reported planets from the Extrasolar
Planets Encyclopaedia (http://exoplanet.eu) and the NASA Exoplanet
Archive (https://exoplanetarchive.ipac.caltech.edu). at less than
100pc. Employing primarily Gaia DR3 data supplemented by searches in
the Washington Double Star catalogue and available literature, we
identified 215 exoplanet host stars in 212 multiple-star systems with
common parallax and proper motion.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tableb1.dat 58 998 Exoplanet host stars at d<100pc
tableb2.dat 106 145 Multiple systems with one or more ultracool
dwarfs and without proper planets
tableb3.dat 82 35 Astrometry of systems with new common proper
motions and parallax companions
tableb4.dat 200 435 Basic data of the identified multiple stellar
systems with planets
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Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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1- 28 A28 --- Star Name of the star
30- 31 I2 h RAh Right ascension (J2000)
33- 34 I2 min RAm Right ascension (J2000)
36- 40 F5.2 s RAs Right ascension (J2000)
42 A1 --- DE- Declination sign (J2000)
43- 44 I2 deg DEd Declination (J2000)
46- 47 I2 arcmin DEm Declination (J2000)
49- 52 F4.1 arcsec DEs Declination (J2000)
54- 58 F5.1 pc Dist Distance
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Id [1/65] System identification number
4- 31 A28 --- Star Name of the star
33- 34 I2 h RAh Right ascension (J2000)
36- 37 I2 min RAm Right ascension (J2000)
39- 43 F5.2 s RAs Right ascension (J2000)
45 A1 --- DE- Declination sign (J2000)
46- 47 I2 deg DEd Declination (J2000)
49- 50 I2 arcmin DEm Declination (J2000)
52- 55 F4.1 arcsec DEs Declination (J2000)
57- 60 F4.1 mag Gmag ? G-band mean magnitude from Gaia DR3 (1)
62- 66 A5 --- SpType Spectral type
68-106 A39 --- Refs BibCode(s) of the reference of UCD Discovery
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Note (1): maximum error in G provided by Gaia DR3 is less than 0.005 mag.
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Id [1/15] System identification number
4- 6 A3 --- Host [Yes/No ] Indicates whether the star hosts
planets or not
8- 35 A28 --- Star Name of the star
37- 41 F5.2 mas plx Parallax
43- 46 F4.2 mas e_plx Standard error of Parallax
48- 54 F7.2 mas/yr pmRA Proper motion in right ascension direction,
pmRA*cosDE
56- 59 F4.2 mas/yr e_pmRA Standard error of proper motion in
right ascension direction
61- 67 F7.2 mas/yr pmDE Proper motion in declination direction
69- 72 F4.2 mas/yr e_pmDE Standard error of proper motion in
declination direction
74- 77 F4.2 --- muratio ? Proper motions of star and companion
ratio (1)
79- 82 F4.2 deg DPA ? Difference of position angles of star
and companion (1)
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Note (1): as defined in 2018MNRAS.479.1332M 2018MNRAS.479.1332M, where
(muratio)2=
[(pmRAcosDE1-pmRAcosDE2)2 + [pmDE1-pmDE2)2]/[(pmRAcosDE1)2+pmDE12,
DPA= |PA1-PA2|.
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Byte-by-byte Description of file: tableb4.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Id [1/212] System identification number
5- 14 A10 --- WDS Washington Double Star Id
16- 54 A39 --- Disc WDS Discoverer code (1)
56- 58 A3 --- Host [Yes/No ] It indicates whether the star
hosts planets or not
60- 91 A32 --- Star Name of the star
93- 94 I2 h RAh Right ascension (J2000)
96- 97 I2 min RAm Right ascension (J2000)
99-103 F5.2 s RAs Right ascension (J2000)
105 A1 --- DE- Declination sign (J2000)
106-107 I2 deg DEd Declination (J2000)
109-110 I2 arcmin DEm Declination (J2000)
112-116 F5.2 arcsec DEs Declination (J2000)
118 A1 --- l_Dist [~] Limit flag on Dist
119-124 F6.2 pc Dist ? Distance
127-130 F4.2 pc e_Dist ? Standard error of distance
132 A1 --- l_rho [~] Limit flag on rho
133-142 F10.4 arcsec rho ? Projected physical separation between the
current star and the first star of the system
(not tabulated if rho < 1 arcsec)
144-149 F6.2 deg theta ? Position angle of the current star relative
to the first star of the system
(not tabulated if rho < 1 arcsec)
151-160 F10.3 au Sep ? Separation
162-200 A39 --- Ref Literature reference(s)
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Note (1): formed by the current and the first star of the system, or
19-digit bibliographic code of the reference of the binarity existence.
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Acknowledgements:
Javier Gonzalez-Payo, fcojgonz(at)ucm.es
(End) Patricia Vannier [CDS] 31-Jul-2024