J/AJ/157/52 Radial velocity observations in super-Earth systems (Bryan+, 2019)
An excess of Jupiter analogs in super-Earth systems.
Bryan M.L., Knutson H.A., Lee E.J., Fulton B.J., Batygin K., Ngo H.,
Meshkat T.
<Astron. J., 157, 52 (2019)>
=2019AJ....157...52B 2019AJ....157...52B (SIMBAD/NED BibCode)
ADC_Keywords: Exoplanets ; Stars, masses ; Abundances, [Fe/H] ;
Radial velocities
Keywords: methods: statistical - planetary systems -
techniques: radial velocities
Abstract:
We use radial velocity (RV) observations to search for long-period gas
giant companions in systems hosting inner super-Earth (1-4 R⊕,
1-10 M⊕) planets to constrain formation and migration scenarios
for this population. We consistently refit published RV data sets for
65 stars and find nine systems with statistically significant trends
indicating the presence of an outer companion. We combine these RV data
with AO images to constrain the masses and semi-major axes of these
companions. We quantify our sensitivity to the presence of long-period
companions by fitting the sample with a power-law distribution and find
an occurrence rate of 39%±7% for companions 0.5-20 MJup and 1-20 au.
Half of our systems were discovered by the transit method, and half were
discovered by the RV method. While differences in the RV baselines and
number of data points between the two samples lead to different
sensitivities to distant companions, we find that occurrence rates of
gas giant companions in each sample are consistent at the 0.5σ
level. We compare the frequency of Jupiter analogs in these systems to
the equivalent rate from field star surveys and find that Jupiter analogs
are more common around stars hosting super-Earths. We conclude that
the presence of outer gas giants does not suppress the formation of inner
super-Earths, and that these two populations of planets instead appear
to be correlated. We also find that the stellar metallicities of systems
with gas giant companions are higher than those without companions, in
agreement with the well-established metallicity correlation from RV
surveys of field stars.
Description:
We collected published RV data for systems with at least one confirmed
super-Earth, where we define a super-Earth as a planet with either a mass
between 1 and 10 M⊕ or a radius between 1 and 4 R⊕,
depending on the detection technique (Table 1). We exclude systems with
fewer than 10 data points and baselines shorter than 100 days, leaving us
with 65 systems that meet these criteria (Figure 1). Of that sample,
34 systems host at least one super-Earth discovered using the transit
method, and 31 systems host at least one super-Earth discovered using
the RV method. Eighteen of these systems are single-planet systems, while
the remaining 47 are multiplanet systems. Forty-five planets have both
measured masses and radii and thus measured densities. We provide a summary
of the RV data used in this work in Table 1. We also include best-fit
values for the RV acceleration from our orbital solution fitting as
described in the following section in Table 1. We list the complete set
of individual RV measurements used in our analysis in Table 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 97 65 Sample of systems
table2.dat 41 12279 Published RVs used in this study
refs.dat 54 59 List of references
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See also:
J/A+A/469/L43 : Radial velocities of Gl 581 (Udry+, 2007)
J/A+A/493/639 : Velocity curves of HD 40307 (Mayor+, 2009)
J/A+A/493/645 : Gl 176 radial velocities (Forveille+, 2009)
J/A+A/496/527 : Radial velocity curves of HD 47186 and HD 181433
(Bouchy+, 2009)
J/A+A/506/303 : CoRoT-7 radial velocities (Queloz+, 2009)
J/A+A/507/487 : GJ 581 radial velocity curve (Mayor+, 2009)
J/A+A/511/A21 : Radial velocities of GJ876 planetary system (Correia+, 2010)
J/A+A/512/A48 : HARPS RV curves of HD125612, HD215497, HIP5158
(Lo Curto+, 2010)
J/ApJ/708/1366 : Radial velocities for 61 Vir (Vogt+, 2010)
J/A+A/528/A111 : GJ3634 radial velocity and 4.5um flux (Bonfils+, 2011)
J/A+A/534/A58 : HD20794, HD85512, HD192310 HARPS radial velocities
(Pepe+, 2011)
J/ApJ/749/15 : The Kepler-20 planetary system (Gautier+, 2012)
J/A+A/556/A110 : HARPS radial velocities of GJ 163 (Bonfils+, 2013)
J/A+A/556/A126 : GJ667C Doppler and activity measurements
(Anglada-Escude+, 2013)
J/ApJ/789/154 : Kepler-10 RV measurements by HARPS-N (Dumusque+, 2014)
J/ApJ/805/175 : Keck and APF radial velocities of HD7924 (Fulton+, 2015)
J/A+A/585/A134 : HD1461, HD40307, and HD204313 radial velocities (Diaz+, 2016)
J/A+A/585/A135 : HD175607 RV, logRHK and Halpha index (Mortier+, 2016)
J/A+A/586/A93 : WASP41 and WASP47 photometric and RV data
(Neveu-VanMalle+, 2016)
J/A+A/593/A117 : GJ 3998 RVs, S and Halpha indexes (Affer+, 2016)
J/A+A/595/A77 : GJ676A radial velocity curve (Sahlmann+, 2016)
J/ApJ/821/89 : 12yrs of radial velocity obs. of exoplanet systems
(Bryan+, 2016)
J/A+A/597/A108 : GJ 536 HARPS and HARPS-N data (Suarez Mascareno+, 2017)
J/AJ/154/123 : Radial velocity follow-up of the HD 3167 system
(Gandolfi+, 2017)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- ID System identifier
13 A1 --- n_ID [c] Note on ID (1)
15- 18 F4.2 Msun M* [0.12/1.41] Stellar mass
20- 23 F4.2 Msun e_M* [0.02/0.09]? Lower limit uncertainty in M*
25- 28 F4.2 Msun E_M* [0.02/0.09]? Upper limit uncertainty in M*
30- 34 F5.2 [-] [Fe/H] [-0.62/0.36] Metallicity
36- 39 F4.2 [-] e_[Fe/H] [0.01/0.2] Uncertainty in [Fe/H] (2)
41 I1 --- Npl [1/6] Number of planet(s)
43- 49 A7 --- Meth Discovery method (Transit or RV)
51- 54 I4 --- Nobs [13/1126] Number of observations
56- 59 I4 d Base [103/8476] Time baseline
61- 68 F8.3 m/s/yr Trend [-156.59/60.2] Radial velocity trend
70- 75 F6.3 m/s/yr e_Trend [0/32] Lower limit uncertainty in Trend
77- 82 F6.3 m/s/yr E_Trend [0/42] Upper limit uncertainty in Trend
83- 85 A3 --- n_Trend Note on Trend (3)
87- 97 A11 --- Ref Reference(s) (see refs.dat file)
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Note (1): Note as follows:
c = For systems GJ 667, GJ 876, GJ 581, and HD 40307, we fit fewer signals
than the published number, and for systems HD 156668, HD 175607, and
GJ 163, we fit additional signals. See Section 3.1 for details.
Note (2): We note that uncertainties on the metallicity were not published for
systems 61 Vir, GJ 433, GJ 667, Proxima Cen, and GJ 3634. For these systems,
we adopt metallicity uncertainties of 0.1 dex.
Note (3): Note as follows:
b = Systems which have statistically significant long-term trends;
d = Because the RV acceleration in GJ 676 has curvature, we fit this
long-period signal with an orbital solution. Since this partially resolved
orbit and a linear trend are degenerate, we fix the linear trend term in
this fit to zero, as well as the eccentricity of this outer companion.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- ID System identifier
13- 25 F13.5 d BJD Barycentric Julian Date
27- 35 F9.2 m/s RV [-98756.37/87956.58] Radial velocity
37- 41 F5.2 m/s e_RV [0.0/48.0] The 1σ uncertainty in RV
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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 [1/59] Reference code
4- 34 A31 --- Aut First author's name(s)
36- 54 A19 --- Bibcode Bibcode of the reference
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 15-May-2019