J/A+A/603/A3 VLT/NaCo Large program. IV. Statistical analysis (Vigan+, 2017)
The VLT/NaCo large program to probe the occurrence of exoplanets and brown
dwarfs at wide orbits.
IV. Gravitational instability rarely forms wide, giant planets.
Vigan A., Bonavita M., Biller B., Forgan D., Rice K., Chauvin G.,
Desidera S., Meunier J.-C., Delorme P., Schlieder J. E., Bonnefoy M.,
Carson J., Covino E., Hagelberg J., Henning T., Janson M., Lagrange A.-M.,
Quanz S. P., Zurlo A., Beuzit J.-L., Boccaletti A., Buenzli E., Feldt M.,
Girard J. H. V., Gratton R., Kasper M., Le Coroller H., Mesa D., Messina S.,
Meyer M., Montagnier G., Mordasini C., Mouillet D., Moutou C., Reggiani M.,
Segransan D., Thalmann C.
<Astron. Astrophys. 603, A3 (2017)>
=2017A&A...603A...3V 2017A&A...603A...3V (SIMBAD/NED BibCode)
ADC_Keywords: Fundamental catalog ; Stars, nearby ; Stars, ages ;
Stars, distances
Keywords: techniques: high angular resolution - methods: statistical -
infrared: planetary systems - planetary systems -
planets and satellites: formation
Abstract:
Understanding the formation and evolution of giant planets (>1MJup)
at wide orbital separation (>5AU) is one of the goals of direct
imaging. Over the past 15 years, many surveys have placed strong
constraints on the occurrence rate of wide-orbit giants, mostly based
on non-detections, but very few have tried to make a direct link with
planet formation theories. In the present work, we combine the results
of our previously published VLT/NaCo large program with the results of
12 past imaging surveys to constitute a statistical sample of 199 FGK
stars within 100 pc, including three stars with sub-stellar
companions. Using Monte Carlo simulations and assuming linear flat
distributions for the mass and semi-major axis of planets, we estimate
the sub-stellar companion frequency to be within 0.75-5.70% at the 68%
confidence level (CL) within 20-300AU and 0.5-75MJup, which is
compatible with previously published results. We also compare our
results with the predictions of state-of-the-art population synthesis
models based on the gravitational instability (GI) formation scenario
with and without scattering. We estimate that in both the scattered
and non-scattered populations, we would be able to detect more than
30% of companions in the 1-75MJup range (95% CL). With the three
sub-stellar detections in our sample, we estimate the fraction of
stars that host a planetary system formed by GI to be within 1.0-8.6%
(95% CL). We also conclude that even though GI is not common, it
predicts a mass distribution of wide-orbit massive companions that is
much closer to what is observed than what the core accretion scenario
predicts. Finally, we associate the present paper with the release of
the Direct Imaging Virtual Archive (DIVA), a public database that aims
at gathering the results of past, present, and future direct imaging
surveys.
Description:
Ages, spectral types and distances of 199 nearby stars.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 124 199 Full NaCo-LP sample (table A.1)
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See also:
J/A+A/573/A126 : VLT/NaCo Large program I. Sample (Desidera+, 2015)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Target Star name
19- 20 I2 h RAh Right ascension (J2000.0)
22- 23 I2 min RAm Right ascension (J2000.0)
25- 29 F5.2 s RAs Right ascension (J2000.0)
31 A1 --- DE- Declination sign (J2000.0)
32- 33 I2 deg DEd Declination (J2000.0)
35- 36 I2 arcmin DEm Declination (J2000.0)
38- 42 F5.2 arcsec DEs Declination (J2000.0)
44- 50 A7 --- SpType MK spectral type
52- 75 A24 --- Surveys Previous direct imaging surveys (1)
77- 88 A12 --- MG Name of the moving group or association (2)
90- 94 I5 Myr Age Optimal age
96-100 I5 Myr b_Age Minimum age
102-106 I5 Myr B_Age Maximum age
108-112 F5.1 pc Dist Distance of the star
114-120 F7.2 --- [Fe/H] ? Metalicity
122-124 F3.1 Msun Mass Stellar mass
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Note (1): Previous direct imaging surveys abbreviation as follows:
M05 = Masciadri et al., 2005ApJ...625.1004M 2005ApJ...625.1004M
L05 = Lowrance et al., 2005AJ....130.1845L 2005AJ....130.1845L
S06 = Song et al., unpublished (HST, cycle 13, GO10176)
K07 = Kasper et al., 2007A&A...472..321K 2007A&A...472..321K
B07 = Biller et al., 2007ApJS..173..143B 2007ApJS..173..143B
L07 = Lafreniere et al., 2007ApJ...670.1367L 2007ApJ...670.1367L, Cat. J/ApJ/670/1367
C10 = Chauvin et al., 2010A&A...509A..52C 2010A&A...509A..52C, Cat. J/A+A/509/A52
H10 = Heinze et al., 2010ApJ...714.1551H 2010ApJ...714.1551H
V12 = Vigan et al., 2012A&A...544A...9V 2012A&A...544A...9V, Cat. J/A+A/544/A9
R13 = Rameau et al., 2013A&A...553A..60R 2013A&A...553A..60R
B13 = Biller et al., 2013ApJ...777..160B 2013ApJ...777..160B, Cat. J/ApJ/777/160
B14 = Brandt et al., 2014ApJ...786....1B 2014ApJ...786....1B
C15 = Chauvin et al., 2015A&A...573A.127C 2015A&A...573A.127C
Note (2): Young moving group or association membership as follows:
AB Dor = AB Doradus
Arg = Argus
Beta Pic = Beta Pictoris
Car = Carina
Cas = Castor
Col = Columba
Her/Lyr = Hercules/Lyrae
LA = Local association
LCC = Lower Centaurus Crux
Tuc/Hor = Tucana/Horlogium
UCL = Upper Centaurus Lupus
UMa = Ursa Major
US = Upper Scorpius
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Acknowledgements:
Arthur Vigan, arthur.vigan(at)lam.fr
References:
Desidera et al., Paper I 2015A&A...573A.126D 2015A&A...573A.126D, Cat. J/A+A/573/A126
Chauvin et al., Paper II 2015A&A...573A.127C 2015A&A...573A.127C
Reggiani et al., Paper III 2016A&A...586A.147R 2016A&A...586A.147R
(End) Arthur Vigan [CNRS/LAM, France], Patricia Vannier [CDS] 20-Mar-2017