J/A+A/651/A93 A candidate super-Earth orbiting GJ 9689 (Maldonado+, 2021)
HADES RV programme with HARPS-N at TNG.
XIV. A candidate super-Earth orbiting the M-dwarf GJ 9689 with a period close
to half the stellar rotation period.
Maldonado J., Petralia A., Damasso M., Pinamonti M., Scandariato G.,
Gonzalez-Alvarez E., Affer L., Micela G., Lanza A.F., Leto G., Poretti E.,
Sozzetti A., Perger M., Giacobbe P., Zanmar Sanchez R., Maggio A.,
Gonzalez Hernandez J.I., Rebolo R., Ribas I., Suarez-Mascareno A.,
Toledo-Padron B., Bignamini A., Molinari E., Covino E., Claudi R.,
Desidera S., Herrero E., Morales J.C., Pagano I., Piotto G.
<Astron. Astrophys. 651, A93 (2021)>
=2021A&A...651A..93M 2021A&A...651A..93M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Stars, late-type ; Spectroscopy ;
Exoplanets
Keywords: techniques: spectroscopic - techniques: radial velocities -
stars: late-type - planetary systems - stars: individual: GJ9689
Abstract:
It is now well-established that small, rocky planets are common around
low-mass stars. However, the detection of such planets is challenged
by the short-term activity of the host stars.
The HArps-N red Dwarf Exoplanet Survey (HADES) program is a long-term
project at the Telescopio Nazionale Galileo aimed at the monitoring of
nearby, early-type, M dwarfs, using the HARPS-N spectrograph to search
for small, rocky planets.
A total of 174 HARPS-N spectroscopic observations of the M0.5V-type
star GJ 9689 taken over the past seven years have been analysed. We
combined these data with photometric measurements to disentangle
signals related to the stellar activity of the star from possible
Keplerian signals in the radial velocity data. We run an MCMC
analysis, applying Gaussian Process regression techniques to model the
signals present in the data.
We identify two periodic signals in the radial velocity time series,
with periods of 18.27d, and 39.31d. The analysis of the activity
indexes, photometric data, and wavelength dependency of the signals
reveals that the 39.31d signal corresponds to the stellar rotation
period. On the other hand, the 18.27d signal shows no relation to any
activity proxy or the first harmonic of the rotation period. We,
therefore, identify it as a genuine Keplerian signal. The best-fit
model describing the newly found planet, GJ 9689 b, corresponds to an
orbital period Pb=18.27±0.01d, and a minimum mass
MPsini=9.65±1.41M☉.
Description:
File tableA.1.dat provides the observational data collected with the
HARPS-N spectrograph for GJ 9689 and used in the present study.
Objects:
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RA (2000) DE Designation(s)
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20 13 51.81 +13 23 19.7 GJ 9689 = HIP 99699
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 66 174 Observational data for GJ 9689
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See also:
J/A+A/593/A117 : GJ 3998 RVs, S and Halpha indexes (Affer+, 2016)
J/A+A/598/A26 : HADES RV Programme with HARPS-N at TNG. II. (Perger+, 2017)
J/A+A/605/A92 : GJ 625 HARPS-N data (Suarez Mascareno+, 2017)
J/A+A/608/A63 : HADES VI. GJ 3942b activity with HARPS-N (Perger+, 2017)
J/A+A/622/A193 : Gl686 RV curves and BVR photometry (Affer+, 2019)
J/A+A/644/A68 : Abundance signature of M dwarf stars (Maldonado+, 2020)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 12 F12.6 d BJD Observation date (BJD-2400000)
14- 19 F6.2 m/s RV ?=- Radial Velocity
21- 24 F4.2 m/s e_RV ?=- Uncertainty on radial velocity
26- 31 F6.4 --- S-index Activity S-index
33- 38 F6.4 --- e_S-index Uncertainty on S-index
40- 45 F6.4 --- Halpha Activity Halpha index
47- 52 F6.4 --- e_Halpha Uncertainty on Halpha index
54- 59 F6.4 --- NaI Activity NaI index
61- 66 F6.4 --- e_NaI Uncertainty on NaI index
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Acknowledgements:
Jesus Maldonado, jesus.maldonado(at)inaf.it
References:
Affer et al., Paper I 2016A&A...593A.117A 2016A&A...593A.117A, Cat. J/A+A/593/A117
Perger et al., Paper II 2017A&A...598A..26P 2017A&A...598A..26P, Cat. J/A+A/598/A26
Maldonado et al. Paper III 2017A&A...598A..27M 2017A&A...598A..27M
Scandariato et al., Paper IV 2017A&A...598A..28S 2017A&A...598A..28S
Suarez Mascareno et al., Paper V 2017A&A...605A..92S 2017A&A...605A..92S, Cat. J/A+A/605/A92
Perger et al., Paper VI 2017A&A...608A..63P 2017A&A...608A..63P, Cat. J/A+A/608/A63
Mascareno et al., Paper VII 2018A&A...612A..89M 2018A&A...612A..89M
Pinamonti et al., Paper VIII 2018A&A...617A.104P 2018A&A...617A.104P
Affer et al., Paper IX 2019A&A...622A.193A 2019A&A...622A.193A, Cat. J/A+A/622/A193
Gonzalez-Alvarez et al., Paper X 2019A&A...624A..27G 2019A&A...624A..27G
Pinamonti et al., Paper XI 2019A&A...625A.126P 2019A&A...625A.126P
Maldonado et al., Paper XII 2020A&A...644A..68M 2020A&A...644A..68M, Cat. J/A+A/644/A68
(End) Jesus Maldonado [INAF-OAPa, Italy], Patricia Vannier [CDS] 17-May-2021