J/other/RAA/23.E5022 Masses and RV of exoplanets (Xiao+, 2023)
The masses of a sample of radial-velocity exoplanets with astrometric
measurements.
Xiao G.-Y., Liu Y.-J., Teng H.-Y., Wang W., Brandt T.D., Zhao G., Zhao F.,
Zhai M., Gao Q.
<Res. Astron. Astrophys. 23, 055022 (2023)>
=2023RAA....23e5022X 2023RAA....23e5022X (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, masses ;
Binaries, orbits ; Radial velocities ; Optical
Keywords: techniques: radial velocities - astrometry - stars: formation -
catalogs
Abstract:
Being one of the most fundamental physical parameter of astronomical
objects, mass plays a vital role in the study of exoplanets, including
their temperature structure, chemical composition, formation, and
evolution. However, nearly a quarter of the known confirmed exoplanets
lack measurements of their masses. This is particularly severe for
those discovered via the radial velocity (RV) technique, which alone
could only yield the minimum mass of planets. In this study, we use
published RV data combined with astrometric data from a
cross-calibrated Hipparcos-Gaia Catalog of Accelerations to jointly
constrain the masses of 115 RV-detected substellar companions, by
conducting full orbital fits using the public tool orvara. Among them,
9 exoplanets with Mpsini<13.5MJup are reclassified to the brown
dwarf (BD) regime, and 16 BD candidates (13.5≤Mpsini<80MJup)
turn out to be low-mass M dwarfs. We point out the presence of a
transition in the BD regime as seen in the distributions of host star
metallicity and orbital eccentricity with respect to planet masses. We
confirm the previous findings that companions with masses below
42.5MJup might primarily form in the protoplanetary disk through
core accretion or disk gravitational instability, while those with
masses above 42.5MJup formed through the gravitational instability
of a molecular cloud like stars. Selection effects and detection
biases, which may affect our analysis to some extent, are discussed.
Description:
We use the orbit fitting package orvara to measure the masses and
inclinations of 115 RV-detected companions, including 55 planets, 24
BDs and 36 low-mass M dwarfs. Among them, nine planets are verified as
BDs, and 16 BD candidates should be classified as M dwarfs. Our
results show that the majority of planets with Mpsini<13.5MJup
are still planets, while half of the BD candidates have masses above
the hydrogen-burning limit implying that the BD desert is more
deficient than previous observations suggested.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 117 113 Stellar parameters
tablea2.dat 50 235 Published RV data for our sample
tablea3.dat 299 122 Posteriors of RV companions,
ordered by the value of Mp
refs.dat 64 58 References
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Star name
11 A1 --- m_Name [A] Multiplicity index on Name
13- 18 I6 --- HIP HIP ID
20- 28 A9 --- SpType Spectral Type
30- 35 F6.3 mag Vmag V magnitude
37- 41 F5.3 mag B-V B-V colour index
44- 49 F6.2 mas plx Parallax
51- 54 F4.2 mas e_plx Parallax error
56- 59 I4 K Teff Effective temperature
61- 63 I3 K e_Teff ?=- Effective temperature error
65- 69 F5.3 [cm/s2] logg Surface gravity
71- 75 F5.3 [cm/s2] e_logg ?=- Surface gravity error
77- 82 F6.3 [-] [Fe/H] Metallicity
84- 88 F5.3 [-] e_[Fe/H] ?=- Metallicity error
90- 94 F5.3 Msun Mstar Stellar mass
96-100 F5.3 Msun e_Mstar Stellar mass error
101 A1 --- n_Mstar [*] Note on Mstar (1)
103-110 F8.2 --- chi2HGCA ?=- Reduced chi2
112-117 A6 --- Ref Reference, in refs.dat file
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Note (1): * for stellar masses are determined by isochrones in this work.
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Byte-by-byte Description of file: tablea2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Star name
12- 20 A9 --- Inst Instrument (1)
23- 25 I3 --- Nobs Number of observations
27- 30 F4.1 m/s sigma0 Velocity dispersion
32- 35 I4 d Timespan ? Time span
37- 50 A14 --- Ref Reference, in refs.dat file
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Note (1): The symbol "+" signifies that the instrument has been upgraded.
The symbol a signifies that the systematic velocity offset between
pre-upgrade and post-upgrade has been ignored in our analysis.
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Byte-by-byte Description of file: tablea3.dat
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Bytes Format Units Label Explanations
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1- 12 A12 --- Planet Planet name
14- 20 F7.3 Mjup Mp Planet mass
22- 27 F6.3 Mjup e_Mp Planet mass
29- 33 F5.2 Mjup E_Mp Planet mass
35- 40 F6.3 deg im90deg ?=- Inclination for prograde orbit, i<90°
42- 47 F6.3 deg e_im90deg ? im90deg error (lower value)
49- 54 F6.3 deg E_im90deg ? im90deg error (upper value)
56- 62 F7.3 deg ip90deg ?=- Inclination for retrograde orbit, i>90°
64- 69 F6.3 deg e_ip90deg ? ip90deg error (lower value)
71- 76 F6.3 deg E_ip90deg ? ip90deg error (upper value)
78- 85 F8.3 au a Semi-major axis
87- 93 F7.3 au e_a Semi-major axis error (lower value)
95-101 F7.3 au E_a Semi-major axis error (upper value)
103-109 F7.5 --- e Ellipticity
111-117 F7.5 --- e_e Ellipticit error (lower value)y
119-125 F7.5 --- E_e Ellipticity error (upper value)
127-137 F11.5 yr P Period
139-149 F11.5 yr e_P Period error (lower value)
151-161 F11.5 yr E_P Period error (upper value)
163-168 F6.2 deg Omega Longitude of ascending node
170-175 F6.2 deg e_Omega Longitude of ascending node error (lower value)
177-182 F6.2 deg E_Omega Longitude of ascending node error (upper value)
184-190 F7.3 deg omega Argument of Periastron
192-198 F7.3 deg e_omega Argument of Periastron error (lower value)
200-206 F7.3 deg E_omega Argument of Periastron error (upper value)
208-215 F8.2 mas arel Semimajor axis of the secondary relative to
the primary star
217-223 F7.2 mas e_arel arel error (lower value)
225-232 F8.2 mas E_arel arel error (upper value)
234-243 F10.1 d Tp Periastron epoch (JD-2450000)
245-254 F10.2 d e_Tp Periastron epoch error (lower value)
256-265 F10.2 d E_Tp Periastron epoch error (upper value)
267-273 F7.3 Mjup Mpsini Planet mass*sini value
275-281 F7.3 Mjup e_Mpsini Planet mass*sini value error (lower value)
283-288 F6.3 Mjup E_Mpsini Planet mass*sini value error (upper value)
290-299 A10 --- Name Star name
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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- 2 I2 -- Ref Reference number
4- 22 A19 --- BibCode BibCode
24- 44 A21 --- Aut Author's name
46- 64 A19 --- Com Comments
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Aug-2023