J/ApJ/876/23 Multiple populations of extrasolar gas giants (Goda+, 2019)
Multiple populations of extrasolar gas giants.
Goda S., Matsuo T.
<Astrophys. J., 876, 23 (2019)>
=2019ApJ...876...23G 2019ApJ...876...23G
ADC_Keywords: Exoplanets; Stars, masses; Abundances, [Fe/H]
Keywords: planets and satellites: formation ; techniques: radial velocities ;
planets and satellites: gaseous planets
Abstract:
There are two planetary formation scenarios: core accretion and
gravitational disk instability. Based on the fact that gaseous objects
are preferentially observed around metal-rich host stars, most
extrasolar gaseous objects discovered to date are thought to have been
formed by core accretion. Here, we present 569 samples of gaseous
planets and brown dwarfs found in 485 planetary systems that span
three mass regimes with boundary values at 4 and 25 Jupiter-mass
masses through performing cluster analyses of these samples regarding
the host-star metallicity, after minimizing the impact of the
selection effect of radial-velocity measurement on the cluster
analysis. The larger mass is thought to be the upper mass limit of the
objects that were formed during the planetary formation processes. In
contrast, the lower mass limit appears to reflect the difference
between planetary formation processes around early-type and G-type
stars; disk instability plays a greater role in the planetary
formation process around early-type stars than that around G-type
stars. Populations with masses between 4 and 25 Jupiter masses that
orbit early-type stars comprise planets formed not only via the
core-accretion process but also via gravitational disk instability
because the population preferentially orbits metal-poor stars or is
independent of the host-star metallicity. Therefore, it is essential
to have a hybrid scenario for the planetary formation of the diverse
systems.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 112 569 Planet parameters
table2.dat 73 485 Parameters of stars hosting 569 original samples
and parameters of radial-velocity observations
used in this paper
--------------------------------------------------------------------------------
See also:
J/A+AS/141/371 : Low-mass stars evolutionary tracks (Girardi+, 2000)
J/A+A/398/363 : Statistical properties of exoplanets II (Santos+, 2003)
J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)
J/ApJ/646/505 : Catalog of nearby exoplanets (Butler+, 2006)
J/ApJ/654/625 : Radial velocities of 9 long-period objects (Wittenmyer+, 2007)
J/A+A/487/373 : Spectroscopic parameters of 451 HARPS-GTO stars (Sousa+, 2008)
J/A+A/505/1311 : Radial velocity curves of 11 UMa & HD 32518 (Dollinger+, 2009)
J/A+A/507/1659 : Radial velocity measurements of 30 Ari B (Guenther+, 2009)
J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)
J/A+A/556/A150 : SWEETCat I. Stellar parameters for host stars (Santos+, 2013)
J/A+A/603/A30 : Evidence for two distinct giant planet pop. (Santos+, 2017)
J/A+A/620/A58 : SWEET-Cat updated (Sousa+, 2018)
J/ApJS/235/38 : Kepler planet cand. VIII. DR25 reliability (Thompson+, 2018)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 18 A18 --- ID Planet identifier
20- 24 F5.2 AU MajAxis [0.02/22] Semi-major axis (1)
26- 29 F4.2 AU e_MajAxis [0/3.4] Uncertainty in MajAxis
31- 31 A1 --- l_Msini [l] l=lower limit of companion mass was
applied as that listed in Ref
33- 38 F6.2 Mjup Msini [0.3/103.1] Planet mass times sine
of inclination
40- 44 F5.2 Mjup e_Msini [0/28.7] Uncertainty in Msini
46- 55 F10.5 m/s K [3.1/6114]? Stellar velocity semi-amplitude
57- 63 F7.2 m/s e_K [0/1361]? Uncertainty in K
65- 72 F8.2 d P [1.3/39785] Orbital period
74- 80 F7.2 d e_P [0/6205] Uncertainty in P
82- 86 F5.3 --- e [0/0.97] Eccentricity
88- 92 F5.3 --- e_e [0/0.3] Uncertainty in e
94-112 A19 --- BibCode Bibcode of reference
--------------------------------------------------------------------------------
Note (1): Calculated based on Equations 1 and 2:
Equation (1): a∼9.996x10-1P2/3M*1/3 (au)
where P is the orbital period in years.
Equation (2): Mpsini∼4.919x10-3P1/3(1-e2)1/2KM*2/3 (MJ)
where P is in days, e is the orbital eccentricity, and K is the velocity
semi-amplitude of the star in m/s.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 16 A16 --- ID Star identifier
18 A1 --- f_[Fe/H] Flag on [Fe/H] (1)
20- 24 F5.2 [Sun] [Fe/H] [-0.8/0.5] Metallicity
26- 29 F4.2 [Sun] e_[Fe/H] [0.01/0.2] Uncertainty in [Fe/H]
31 A1 --- f_Mass Flag on Mass (1)
33- 36 F4.2 Msun Mass [0.3/4.2] Stellar mass
38- 41 F4.2 Msun e_Mass [0.02/1.5] Uncertainty in Mass
43- 48 F6.2 m/s sigma [0.9/720]? Companion detection accuracy (2)
50- 53 F4.1 yr tau [0.2/33]? Companion detection duration (2)
55- 73 A19 --- BibCode Bibcode reference
--------------------------------------------------------------------------------
Note (1): Flag as follows:
a = The host-star metallicity was calibrated based on linear regression
derived from the host-star metallicity correlations between the
SWEET-Cat and Geneva-Copenhagen catalogs.
Note (2): A blank indicates that the accuracy and duration of the radial
velocity measurement for the sample were not used for constructing
the detection probabilities for a companion as derived from the
radial-velocity measurements.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 02-Oct-2020