J/A+A/671/A10 Planets around stars with wide brown dwarfs (Subjak+, 2023)
Search for planets around stars with wide brown dwarfs.
Subjak J., Lodieu N., Kabath P., Boffin H.M.J., Nowak G., Grundahl F.,
Bejar V.J.S., Zapatero Osorio M.R., Antoci V.
<Astron. Astrophys. 671, A10 (2023)>
=2023A&A...671A..10S 2023A&A...671A..10S (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Stars, ages ;
Spectroscopy ; Radial velocities ; Optical
Keywords: techniques: spectroscopic - techniques: radial velocities -
techniques: photometric - planets and satellites: detection -
planetary systems - brown dwarfs
Abstract:
The project aims to understand better the role of wide brown dwarf
companions on planetary systems.
We obtained high-resolution spectra of six bright stars with co-moving
wide substellar companions with the SONG, CARMENES, and STELLA
high-resolution spectrographs. We used these spectra to derive radial
velocities together with a complete set of stellar physical
parameters. We then investigated radial velocities signals and
discussed the fraction of planets in such systems. We also re-analyzed
the ages of our targets, which were used to derive the physical
parameters of wide brown dwarf companions. Finally, a compilation of
systems with known planets from the literature is considered along
with our sample to search for possible peculiarities in their
parameter distributions.
Based on the derived ages of six observed systems, we re-computed the
masses of the wide companions, confirming their substellar nature. We
confirmed planets in the HD3651 and HIP70849 systems and found a new
planetary candidate in the HD46588 system. In our survey, which is
sensitive mostly to Neptune-mass planets at short periods of a few
days and Saturn-mass planets at longer periods of hundreds of days, we
derived a frequency of planets orbiting stars with wide brown dwarf
companions below 70% with the uncertainties included. Comparing the
parameter distributions of our sample with single stars, we observe
the enhancement of planets with short periods below six days in
systems with a wide stellar companion. Finally, planets in systems
with wide BD companions follow their own eccentricity distribution
with a maximum at ∼0.65 and have periods larger than 40 days, masses
larger than 0.1MJ, and eccentricities larger than 0.4.
Description:
We tabulated the radial velocities for HD3651, GJ504, HD46588,
HD203030, HNPeg, HD118865 observed with the SONG, CARMENES and STELLA
spectrographs. The data are reduced as described in the paper.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 208 6 System parameters for stars in our sample
rvs.dat 62 1694 SONG, CARMENES, STELLA radial velocities
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Star name
10- 11 I2 h RAh Gaia EDR3 Right ascension (J2000)
13- 14 I2 min RAm Gaia EDR3 Right ascension (J2000)
16- 20 F5.2 s RAs Gaia EDR3 Right ascension (J2000)
22 A1 --- DE- Gaia EDR3 Declination sign (J2000)
23- 24 I2 deg DEd Gaia EDR3 Declination (J2000)
26- 27 I2 arcmin DEm Gaia EDR3 Declination (J2000)
29- 33 F5.2 arcsec DEs Gaia EDR3 Declination (J2000)
35- 39 F5.3 mag Tmag TESS T magnitude
41- 45 F5.3 mag e_Tmag TESS T magnitude error
47- 51 F5.3 mag Gmag Gaia EDR3 G magnitude
53- 57 F5.3 mag e_Gmag Gaia G magnitude error
59- 63 F5.3 mag BTmag Tycho BT magnitude
65- 69 F5.3 mag e_BTmag Tycho BT magnitude error
71- 75 F5.3 mag VTmag Tycho VT magnitude
77- 81 F5.3 mag e_VTmag Tycho VT magnitude error
83- 87 F5.3 mag Jmag 2MASS J magnitude
89- 93 F5.3 mag e_Jmag 2MASS J magnitude error
95- 99 F5.3 mag Hmag 2MASS H magnitude
101-105 F5.3 mag e_Hmag 2MASS H magnitude mag
107-111 F5.3 mag Ksmag 2MASS Ks magnitude
113-117 F5.3 mag e_Ksmag 2MASS Ks magnitude error
119-123 F5.3 mag W1mag WISE1 magnitude
125-129 F5.3 mag e_W1mag WISE1 magnitude error
131-135 F5.3 mag W2mag WISE2 magnitude
137-141 F5.3 mag e_W2mag WISE2 magnitude error
143-147 F5.3 mag W3mag WISE3 magnitude
149-153 F5.3 mag e_W3mag WISE3 magnitude error
155-159 F5.3 mag W4mag WISE4 magnitude
161-165 F5.3 mag e_W4mag WISE4 magnitude error
167-174 F8.3 mas/yr pmRA Gaia EDR3 Proper motion along RA, pmRAcosDE
176-180 F5.3 mas/yr e_pmRA Proper motion along RA, pmRAcosDE, error
182-189 F8.3 mas/yr pmDE Gaia EDR3 Proper motion along DE
191-195 F5.3 mas/yr e_pmDE Proper motion along DE
197-202 F6.3 mag Plx Gaia EDR3 Parallax
204-208 F5.3 mag e_Plx Parallax error
--------------------------------------------------------------------------------
Byte-by-byte Description of file: rvs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Name Star name
10- 17 A8 --- Spec Spectrograph
19- 29 F11.3 d BJD Barycentric Julian date
31- 47 F17.10 m/s RV Radial velocity or relative radial velocity (1)
49- 62 F14.10 m/s e_RV rms uncertainty on Radial velocity
--------------------------------------------------------------------------------
Note (1): Radial velocities for SONG and STELLA, relative radial velocities for
CARM_VIS and CARM_NIR.
--------------------------------------------------------------------------------
History:
From Jan Subjak, jan.subjak(at)asu.cas.cz
Acknowledgements:
JS and PK would like to acknowledge support from MSMT grant LTT-20015.
JS and PK acknowledge a travel budget from ERASMUS+ grant
2020-1-CZ01-KA203-078200. JS would like to acknowledge support from
the Grant Agency of Charles University: GAUK No. 314421. NL was
financially supported by the Ministerio de Economia y Competitividad
and the Fondo Europeo de Desarrollo Regional (FEDER) under
AYA2015-69350-C3-2-P. We thank warmly Matthias Zechmeister for running
the SERVAL pipeline and sending us the CARMENES radial velocities.
This research has made use of the Simbad and Vizier databases,
operated at the centre de Donnees Astronomiques de Strasbourg (CDS),
and of NASA's Astrophysics Data System Bibliographic Services (ADS).
This work has made use of data from the European Space Agency (ESA)
mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia
Data Processing and Analysis Consortium (DPAC,
https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the
DPAC has been provided by national institutions, in particular the
institutions participating in the Gaia Multilateral Agreement. We
acknowledge the use of public TESS data from pipelines at the TESS
Science Office and at the TESS Science Processing Operations Center.
Resources supporting this work were provided by the NASA High-End
Computing (HEC) Program through the NASA Advanced Supercomputing (NAS)
Division at Ames Research Center for the production of the SPOC data
products. This paper includes data collected with the TESS mission,
obtained from the MAST data archive at the Space Telescope Science
Institute (STScI). Funding for the TESS mission is provided by the
NASA Explorer Program. STScI is operated by the Association of
Universities for Research in Astronomy, Inc., under NASA contract NAS
5-26555. This publication makes use of VOSA, developed under the
Spanish Virtual Observatory project supported by the Spanish MINECO
through grant AyA2017-84089. VOSA has been partially updated by using
funding from the European Union's Horizon 2020 Research and
Innovation Programme, under Grant Agreement No 776403 (EXOPLANETS-A).
The SONG data were obtained over several semesters through programme
numbers P02-10, P03-08, P04-02, and P05-02 (PI Lodieu). The Danish
SONG telescope in Tenerife, the Hertzsprung SONG telescope, is owned
and operated by Aarhus University and the University of Copenhagen in
collaboration with the Astrophysics Institute of the Canary Islands
(IAC). It is financed by the Villum Kann Rasmussen Foundation,
Carlsberg Foundation, the Danish Council for Independent Research |
Natural Sciences (FNU), European Research Council, Danish National
Research Foundation, Aarhus University, University of Copenhagen and
Instituto de Astrofisica de Canarias. Based on observations collected
at the Centro Astronomico Hispano-Aleman (CAHA) at Calar Alto,
operated jointly by Junta de Andalucia and Consejo Superior de
Investigaciones Cientificas (IAA-CSIC). The CARMENES dataset was
obtained as part of programme number F19-3.5-011 (PI Lodieu). CARMENES
is an instrument for the Centro Astronomico Hispano-Aleman de Calar
Alto (CAHA, Almeria, Spain). CARMENES is funded by the German
Max-Planck-Gesellschaft (MPG), the Spanish Consejo Superior de
Investigaciones Cientificas (CSIC), the European Union through
FEDER/ERF FICTS-2011-02 funds, and the members of the CARMENES
Consortium (Max-Planck-Institut fur Astronomie, Instituto de
Astrofisica de Andalucia, Landessternwarte Konigstuhl, Institut de
Ciencies de l'Espai, Insitut fur Astrophysik Gottingen,
Universidad Complutense de Madrid, Thuringer Landessternwarte
Tautenburg, Instituto de Astrofisica de Canarias, Hamburger
Sternwarte, Centro de Astrobiologia and Centro Astronomico
Hispano-Aleman), with additional contributions by the Spanish
Ministry of Economy, the German Science Foundation through the Major
Research Instrumentation Programme and DFG Research Unit FOR2544 "Blue
Planets around Red Stars", the Klaus Tschira Stiftung, the states of
Baden-Wurttemberg and Niedersachsen, and by the Junta de Andalucia.
Based on observations made with the Italian Telescopio Nazionale
Galileo (TNG) operated on the island of La Palma by the Fundacion
Galileo Galilei of the INAF (Istituto Nazionale di Astrofisica) at the
Spanish Observatorio del Roque de los Muchachos of the Instituto de
Astrofisica de Canarias. Part of the HARPS-N data used in this work
have been downloaded from the TNG archive. Based on observations
collected at the European Organisation for Astronomical Research in
the Southern Hemisphere under ESO programmes 072.C-0488, 183.C-0972,
085.C-0019, 087.C-0831, 183.C-0972, 089.C-0732, 090.C-0421,
091.C-0034, 093.C-0409, 095.C-0551, 096.C-0460, 196.C-1006,
098.C-0366, 099.C-0458, 0100.C-0097, 0101.C-0379, 0102.C-0558,
0103.C-0432.
(End) Patricia Vannier [CDS] 16-Dec-2022