J/ApJS/262/21 3-D selection of 167 sub-stellar companions (Feng+, 2022)
3-D selection of 167 sub-stellar companions to nearby stars.
Feng F., Butler R.P., Vogt S.S., Clement M.S., Tinney C.G., Cui K.,
Aizawa M., Jones H.R.A., Bailey J., Burt J., Carter B.D., Crane J.D.,
Flammini Dotti F., Holden B., Ma B., Ogihara M., Oppenheimer R.,
O'Toole S.J., Shectman S.A., Wittenmyer R.A., Wang S.X., Wright D.J.,
Xuan Y.
<Astrophys. J. Suppl. Ser. 262, 21 (2022)>
=2022ApJS..262...21F 2022ApJS..262...21F (SIMBAD/NED BibCode)
ADC_Keywords: Stars, nearby ; Stars, dwarfs; Stars, subdwarf ; Exoplanets ;
Binaries, orbits ; Optical
Keywords: astrometric exoplanet detection - radial velocity -
exoplanet detection methods - exoplanet astronomy -
brown dwarfs - exoplanet catalogs
Abstract:
We analyze 5108 AFGKM stars with at least five high-precision radial
velocity points, as well as Gaia and Hipparcos astrometric data,
utilizing a novel pipeline developed in previous work. We find 914
radial velocity signals with periods longer than 1000 days. Around
these signals, 167 cold giants and 68 other types of companions are
identified, through combined analyses of radial velocity, astrometry,
and imaging data. Without correcting for detection bias, we estimate
the minimum occurrence rate of the wide-orbit brown dwarfs to be 1.3%,
and find a significant brown-dwarf valley around 40MJup. We also find
a power-law distribution in the host binary fraction beyond 3 au,
similar to that found for single stars, indicating no preference of
multiplicity for brown dwarfs. Our work also reveals nine substellar
systems (GJ 234 B, GJ 494 B, HD 13724 b, HD 182488 b, HD 39060 b and
c, HD 4113 C, HD 42581 d, HD 7449 B, and HD 984 b) that have
previously been directly imaged, and many others that are observable
at existing facilities. Depending on their ages, we estimate that an
additional 10-57 substellar objects within our sample can be
detected with current imaging facilities, extending the imaged cold
(or old) giants by an order of magnitude.
Description:
This table lists the orbital parameters of 230 companions detected in
our work. The systems are sorted by the host names listed in the first
column, while the companions in each system are sorted by their
orbital periods. For companions with orbital periods of less than
1000-days, the inclination is not given and the mass reported in this
table is mcsini. For companions with mass higher than 75 MJup, we use
capital letters to label them. Among the parameters, the directly
inferred parameters are P (orbital period), K (RV semi-amplitude), e
(eccentricity), ω* (argument of periastron), i (inclination), and
Ω (longitude of ascending node). The derived parameters are Tp
(periastron epoch), mc (companion mass), and a (semimajor axis). The
dynamical stabilities of Earth-like planets in the habitable zones
(HZs) of their host stars are determined numerically, as described in
Section 7. The median and 1σ quantiles (i.e., the 16% and 84%
quantiles) are used to measure the uncertainty of each parameter.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 321 230 Orbital parameters for the stellar and planetary
companions detected in this work
refs.dat 90 119 References
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- Companion Companion Name
15 A1 --- ImFlag [d] Direct imaging flag (1)
17- 27 A11 --- Host Host Name
29 A1 --- BinFlag [*] Wide binary flag (2)
31- 41 F11.7 yr Per-yr Orbital period, years
43- 53 F11.7 yr e_Per-yr Uncertainty in Per (3)
55- 65 F11.7 yr E_Per-yr Uncertainty in Per (3)
67- 78 F12.5 d Per-d Orbital period, days
80- 90 F11.5 d e_Per-d Uncertainty in Per (3)
92-102 F11.5 d E_Per-d Uncertainty in Per (3)
104-110 F7.3 deg i ? inclination (4)
112-117 F6.3 deg e_i ? Lower uncertainty on i
119-124 F6.3 deg E_i ? Upper uncertainty on i
127-131 F5.3 --- e Eccentricity
133-138 F6.4 --- e_e Lower uncertainty on e
140-145 F6.4 --- E_e Upper uncertainty on e
147-153 F7.3 deg omega* Argument of periastron
155-161 F7.3 deg e_omega* Lower uncertainty on omega*
163-169 F7.3 deg E_omega* Upper uncertainty on omega*
171-178 F8.3 m/s K Radial velocity semi-amplitude
180-186 F7.3 m/s e_K Lower uncertainty on K
188-194 F7.3 m/s E_K Upper uncertainty on K
196-202 F7.3 deg Omega ? Longitude of ascending node
204-210 F7.3 deg e_Omega ? Lower uncertainty on Omega
212-218 F7.3 deg E_Omega ? Upper uncertainty on Omega
220-226 F7.3 Mjup mc Companion mass (4)
228-233 F6.3 Mjup e_mc Lower uncertainty on mc
235-240 F6.3 Mjup E_mc Upper uncertainty on mc
242-247 F6.3 au a Semi-major axis
249-253 F5.3 au e_a Lower uncertainty on a
255-260 F6.3 au E_a Upper uncertainty on a
262-272 A11 d Tp Periastron epoch, BJD-2400000
274-282 F9.3 d e_Tp ? Lower uncertainty on Tp
284-293 F10.3 d E_Tp Upper uncertainty on Tp
295-302 A8 --- HZ Dynamical stability of Earth-like planets
in the habitable zones
304-314 A11 --- Ref Reference, in refs.dat file
316-321 I6 --- HIP ? Hipparcos identifier
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Note (1): Note as follows:
d = systems imaged and their relative astrometry data are analyzed in
combination with other types of data in the solutions.
Note (2): Note as follows:
* = systems have wide-binary companions that are identified by
El-Badry et al. (2021MNRAS.506.2269E 2021MNRAS.506.2269E) or other studies.
Note (3): The median and the 1-σ quantiles (i.e. 16% and 84% quantiles)
are used to measure the uncertainty of each parameter.
Note (4): For companions with orbital period less than 1000 days, the
inclination is not given and the mass reported in this table is mc*sin(i).
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Byte-by-byte Description of file: refs.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Ref Reference number
5- 23 A19 --- BibCode BibCode
25- 48 A24 --- Aut Author's name
50- 90 A41 --- Com Comments
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Acknowledgements:
Fabo Feng, ffeng(at)sjtu.edu.cn
History:
19-Sep-2022 : Fabo Feng slightly modified the published data table.
This table shows the orbital period parameters "Per-yr" and "Per-d" with
higher precision than that shown in the published data table.
07-Oct-2022 : some values corrected in table3.dat
(End) Patricia Vannier [CDS] 19-Sep-2022