J/A+A/666/A187 Gl514 RVs and activity diagnostics (Damasso+, 2022)
A quarter century of spectroscopic monitoring of the nearby M dwarf Gl514.
A super-Earth on an eccentric orbit moving in and out of the habitable zone.
Damasso M., Perger M., Almenara J.M., Nardiello D., Perez-Torres M.,
Sozzetti A., Hara N.C., Quirrenbach A., Bonfils X., Zapatero Osorio M.R.,
Astudillo-Defru N., Gonzalez Hernandez J.I., Suarez Mascareno A.,
Amado P.J., Forveille T., Lillo-Box J., Alibert Y., Caballero J.A.,
Cifuentes C., Delfosse X., Figueira P., Galadi-Enriquez D., Hatzes A.P.,
Henning T., Kaminski A., Mayor M., Murgas F., Montes D., Pinamonti M.,
Reiners A., Ribas I., Bejar V.J.S., Schweitzer A., Zechmeister M.
<Astron. Astrophys. 666, A187 (2022)>
=2022A&A...666A.187D 2022A&A...666A.187D (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Radial velocities ;
Photometry ; Optical
Keywords: techniques: radial velocities - techniques: photometric -
planetary systems - stars: activity - stars: individual: Gl 514
Abstract:
Statistical analyses based on Kepler data show that most of the
early-type M dwarfs host multi-planet systems consisting of Earth to
sub-Neptune sized planets with orbital periods up to ∼250 days,
and that at least one such planet is likely located within the
habitable zone. M dwarfs are therefore primary targets to search for
potentially habitable planets in the solar neighbourhood.
We investigated the presence of planetary companions around the nearby
(7.6pc) and bright (V=9mag) early-type M dwarf Gl 514, analysing 540
radial velocities collected over nearly 25 years with the HIRES,
HARPS, and CARMENES spectrographs. The data are affected by
time-correlated signals at the level of 2-3m/s due to stellar
activity, that we filtered out testing three different models based on
Gaussian process regression. As a sanity cross-check, we repeated the
analyses using HARPS radial velocities extracted with three different
algorithms. We used HIRES radial velocities and Hipparcos-Gaia
astrometry to put constraints on the presence of long-period
companions, and we analysed TESS photometric data.
We found strong evidence that Gl∼514 hosts a super-Earth on a likely
eccentric orbit, residing in the conservative habitable zone for
nearly 34% of its orbital period. The planet Gl 514 b has minimum mass
mbsinib=5.2±0.9M☉, orbital period Pb=140.43±0.41 days,
and eccentricity eb=0.45+0.15-0.14. No evidence for transits is
found in the TESS light curve. There is no evidence for a longer
period companion in the radial velocities and, based on astrometry, we
can rule out a ∼0.2M{Jup} planet at a distance of ∼3-10au, and
massive giant planets/brown dwarfs out to several tens of au. We
discuss the possible presence of a second low-mass companion at a
shorter distance from the host than Gl 514 b.
Gl 514 b represents an interesting science case to study the
habitability of planets on eccentric orbits. We advocate for
additional spectroscopic follow-up to get more accurate and precise
planetary parameters. Further follow-up is also needed to investigate
sub m/s and shorter period signals.
Description:
Radial velocities (RVs) of Gl 514 from HARPS and CARMENES-VIS spectra.
RVs have been extracted from HARPS spectra using three different
pipelines based on the template matching technique: TERRA, NAIRA
(included here), and SERVAL (see Trifonov et al., 2020A&A...636A..74T 2020A&A...636A..74T,
Cat. J/A+A/636/A74). Tables include spectroscopic diagnostics to
characterize stellar activity.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 22 162 HARPS RVs extracted with TERRA
tablea2.dat 25 162 HARPS RVs extracted with NAIRA
tablea3.dat 71 162 Activity diagnostics from HARPS spectra
tablea4.dat 22 274 CARMENES-VIS RVs
tablea5.dat 68 272 Activity diagnostics from CARMENES spectra
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See also:
J/A+A/636/A74 : HARPS radial velocity database (Trifonov+, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 11 F11.6 d Time Epochs of the observations (BJD-2450000)
13- 17 F5.2 m/s RV Relative radial velocity
19- 22 F4.2 m/s e_RV Radial velocity uncertainty
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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- 11 F11.6 d Time Epochs of the observations (BJD-2450000)
13- 20 F8.2 m/s RV Radial velocity
22- 25 F4.2 m/s e_RV Radial velocity uncertainty
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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- 11 F11.6 d Time Epochs of the observations (BJD-2450000)
13- 18 F6.4 km/s FWHM CCF FWHM
20- 25 F6.4 km/s e_FWHM CCF FWHM uncertainties
27- 33 F7.5 --- H-alpha H-alpha activity index
35- 41 F7.5 --- e_H-alpha H-alpha activity index errors
43- 48 F6.4 --- CaIIHK CaIIHK activity index
50- 55 F6.4 --- e_CaIIHK CaIIHK activity index errors
57- 63 F7.5 --- NaI NaI activity index
65- 71 F7.5 --- e_NaI NaI activity index errors
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 11 F11.6 d Time Epochs of the observations (BJD-2450000)
13- 17 F5.2 m/s RV Relative radial velocity
19- 22 F4.2 m/s e_RV Radial velocity uncertainty
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Byte-by-byte Description of file: tablea5.dat
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Bytes Format Units Label Explanations
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1- 11 F11.6 d Time Epochs of the observations (BJD-2450000)
13- 19 F7.5 -- Ca-IRT Calcium infrared triplet index
21- 27 F7.5 -- e_Ca-IRT Calcium infrared triplet index error
29- 35 F7.5 -- NaD Sodium doublet index
37- 43 F7.5 -- e_NaD Sodium doublet index error
45- 50 F6.2 -- dLW Differential line width
52- 55 F4.2 -- e_dLW Differential line width error
57- 62 F6.2 -- CRX Chromatic index
64- 68 F5.2 -- e_CRX Chromatic index error
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Acknowledgements:
Mario Damasso, mario.damasso(at)inaf.it
(End) Mario Damasso [INAF-OATo, Italy], Patricia Vannier [CDS] 19-Apr-2022