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J/A+A/599/A90       Characterization of HD 108874 system        (Benatti+, 2017)

The GAPS Programme with HARPS-N at TNG. XII: Characterization of the planetary system around HD 108874. Benatti S., Desidera S., Damasso M., Malavolta L., Lanza A.F., Biazzo K., Bonomo A.S., Claudi R.U., Marzari F., Poretti E., Gratton R., Micela G., Pagano I., Piotto G., Sozzetti A., Boccato C., Cosentino R., Covino E., Maggio A., Molinari E., Smareglia R., Affer L., Andreuzzi G., Bignamini A., Borsa F., di Fabrizio L., Esposito M., Martinez Fiorenzano A., Messina S., Giacobbe P., Harutyunyan A., Knapic C., Maldonado J., Masiero S., Nascimbeni V., Pedani M., Rainer M., Scandariato G., Silvotti R. <Astron. Astrophys. 599, A90 (2017)> =2017A&A...599A..90B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Radial velocities Keywords: stars: individual: HD 108874 - techniques: radial velocities - stars: activity - planetary systems Abstract: In order to understand the observed physical and orbital diversity of extrasolar planetary systems, a full investigation of these objects and of their host stars is necessary. Within this field, one of the main purposes of the GAPS observing project with HARPS-N@TNG is to provide a more detailed characterisation of already known systems. In this framework we monitored the star, hosting two giant planets, HD108874, with HARPS-N for three years in order to refine the orbits, to improve the dynamical study and to search for additional low-mass planets in close orbits. We subtracted the radial velocity (RV) signal due to the known outer planets, finding a clear modulation of 40.2d period. We analysed the correlation between RV residuals and the activity indicators and modelled the magnetic activity with a dedicated code. Our analysis suggests that the 40.2d periodicity is a signature of the rotation period of the star. A refined orbital solution is provided, revealing that the system is close to a mean motion resonance of about 9:2, in a stable configuration over 1Gyr. Stable orbits for low-mass planets are limited to regions very close to the star or far from it. Our data exclude super-Earths with Msini≳5M{earth} within 0.4AU and objects with Msini≳2M{earth} with orbital periods of a few days. Finally we put constraints on the habitable zone of the system, assuming the presence of an exomoon orbiting the inner giant planet. Description: This table includes the time series of the radial velocity, the bisector span and the chromospheric activity indices LogR'HK and Halpha of the new HARPS-N spectra collected in the framework of the GAPS Project for the target HD 108874, analysed in the paper. The corresponding uncertainties are provided as well. Objects: -------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------- 12 30 26.88 +22 52 47.4 HD 108874 = HIP 61028 -------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablea1.dat 71 91 Time series of the HARPS-N spectra for HD 108874
See also: J/A+A/554/A28 : Qatar-1 differential light curve (Covino+, 2013) J/A+A/575/A111 : GAPS V: Global analysis of the XO-2 system (Damasso+, 2015) J/A+A/575/L15 : TrES-4b RV and Ic curves (Sozzetti+, 2015) J/A+A/578/A64 : Velocity curve of τ Boo A (Borsa+, 2015) J/A+A/579/A136 : HAT-P-36 and WASP-11/HAT-P-10 light curves (Mancini+, 2015) J/A+A/583/A135 : XO-2N and XO-2S spectra (Biazzo+, 2015) J/A+A/588/A118 : Pr0211 RVs, photometry and activity indexes (Malavolta+, 2016) Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 11 F11.6 d BJD Barycentric Julian Date (UTC) (BJD-2450000) 13- 20 F8.4 km/s RV Radial Velocity 22- 27 F6.4 km/s e_RV Error on the Radial Velocity 29- 35 F7.4 km/s BVS Bisector Velocity Span 37- 42 F6.4 km/s e_BVS Error on the Bisector Velocity Span 44- 50 F7.4 --- logR'HK Activity index of the H&K lines of the CaII 52- 57 F6.4 --- e_logR'HK Error on the logR'HK 59- 64 F6.4 --- Halpha Activity index of the Halpha line 66- 71 F6.4 --- e_Halpha Error on the Halpha
Acknowledgements: Serena Benatti, serena.benatti(at)oapd.inaf.it References: Covino et al., Paper I 2013A&A...554A..28C, Cat. J/A+A/554/A28 Desidera et al., Paper II 2013A&A...554A..29D Esposito et al., Paper III 2014A&A...564L..13E Desidera et al., Paper IV 2014A&A...567L...6D Damasso et al., Paper V 2015A&A...575A.111D, Cat. J/A+A/575/A111 Sozzetti et al., Paper VI 2015A&A...575L..15S, Cat. J/A+A/575/L15 Borsa et al., Paper VII 2015A&A...578A..64B, Cat. J/A+A/578/A64 Mancini et al., Paper VIII 2015A&A...579A.136M, Cat. J/A+A/579/A136 Damasso et al., Paper IX 2015A&A...581L...6D, Cat. J/A+A/581/L6 Biazzo et al., Paper X 2015A&A...583A.135B, Cat. J/A+A/583/A135 Malavolta et al., Paper XI 2016A&A...588A.118M, Cat. J/A+A/588/A118
(End) S. Benatti [INAF - Astron. Obs. of Padova], P. Vannier [CDS] 16-Dec-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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