J/A+A/588/A118    Pr0211 RVs, photometry and activity indexes (Malavolta+, 2016)

The GAPS programme with HARPS-N at TNG. XI. Pr 0211 in M 44: the first multi-planet system in an open cluster. Malavolta L., Nascimbeni V., Piotto G., Quinn S.N., Borsato L., Granata V., Bonomo A.S., Marzari F., Bedin L.R., Rainer M., Desidera S., Lanza A.F., Poretti E., Sozzetti A., White R.J., Latham D.W., Cunial A., Libralato M., Nardiello D., Boccato C., Claudi R.U., Cosentino R., Covino E., Gratton R., Maggio A., Micela G., Molinari E., Pagano I., Smareglia R., Affer L., Andreuzzi G., Aparicio A., Benatti S., Bignamini A., Borsa F., Damasso M., Di Fabrizio L., Harutyunyan A., Esposito M., Fiorenzano A.F.M., Gandolfi D., Giacobbe P., Gonzalez Hernandez J.I., Maldonado J., Masiero S., Molinaro M., Pedani M., Scandariato G. <Astron. Astrophys. 588, A118 (2016)> =2016A&A...588A.118M 2016A&A...588A.118M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Stars, double and multiple ; Planets ; Radial velocities ; Photometry Keywords: techniques: radial velocities - techniques: photometric planetary systems Abstract: Open cluster (OC) stars share the same age and metallicity, and, in general, their age and mass can be estimated with higher precision than for field stars. For this reason, OCs are considered an important laboratory to study the relation between the physical properties of the planets and those of their host stars, and the evolution of planetary systems. However, only a handful of planets have been discovered around OC main-sequence stars so far, all of them in single-planet systems. For this reason we started an observational campaign within the GAPS collaboration to search for and characterize planets in OCs. We monitored the Praesepe member Pr 0211 to improve our knowledge of the eccentricity of the hot Jupiter (HJ) that is already known to orbit this star and search for additional intermediate-mass planets. An eccentric orbit for the HJ would support a planet-planet scattering process rather than a disk-driven migration after its formation. From 2012 to 2015, we collected 70 radial velocity (RV) measurements with HARPS-N and 36 with TRES of Pr 0211. Simultaneous photometric observations were carried out with the robotic STELLA telescope to characterize the stellar activity. We discovered a long-term trend in the RV residuals that we show as being due to the presence of a second, massive, outer planet. Orbital parameters for the two planets are derived by simultaneously fitting RVs and photometric light curves, with the activity signal modelled as a series of sinusoids at the rotational period of the star and its harmonics. We confirm that Pr 0211b has a nearly circular orbit (e=0.02±0.01), with an improvement of a factor two with respect to the previous determination of its eccentricity, and estimate that Pr 0211c has a mass Msini=7.9±0.2M{jup}, a period P>3500-days and a very eccentric orbit (e>0.60). This kind of peculiar system may be typical of open clusters if the planet-planet scattering phase, which lead to the formation of HJs, is caused by stellar encounters rather than by unstable primordial orbits. Pr 0211 is the first multi-planet system discovered around an OC star. Description: Table 1 contains the spectral linelist used in the determination of the photospheric parameters of the star, with the oscillator strength log(gf) updated to reflect the new solar abundances in Asplund et al., 2009. Table 3 contains the radial velocities from HARPS-N and TRES. Table 4 contains the CCF asymmetry indicators from HARPS-N spectra. Table 5 contains the activity indicators measured from HARPS-N spectra. Objects: --------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------- 08 42 11.49 +19 16 37.7 Pr 0211 = NAME Pr 0211 --------------------------------------------------- File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table1.dat 35 298 Line list for EW measurement table3a.dat 29 70 HARPS-N radial velocities of Pr 0211 table3b.dat 29 54 TRES radial velocities of Pr 0211 table4.dat 80 70 CCF Asymmetry indexes from HARPS-N spectra table5.dat 71 70 Activity indexes from HARPS-N spectra -------------------------------------------------------------------------------- See also: J/A+A/533/A141 : Stellar parameters for 582 HARPS FGK stars (Sousa+, 2011) Byte-by-byte Description of file: table1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 A4 [-] Element Chemical element 6- 9 F4.1 [-] Ion Ionization status in MOOG notation 11- 17 F7.2 0.1nm lambda Central wavelength (Å) 19- 22 F4.2 eV EP Lower excitation potential 24- 29 F6.3 [-] loggf Oscillator strength 31- 35 F5.1 0.1pm EW Equivalent width of the line (mÅ) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3a.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 14 F14.6 d BJD Barycentric Julian date 16- 22 F7.1 m/s RV Radial velocity (relative to the absolute calibration provided by the ThAr lamp) 24- 27 F4.1 m/s e_RV Error on RV 29 A1 [-] Instr [a] Intrument (a = HARPS-N) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3b.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 14 F14.6 d BJD Barycentric Julian date 16- 22 F7.1 m/s RV-RV0 Radial velocity (determined using one of the observations as template) 24- 27 F4.1 m/s e_RV-RV0 Error on RV-RV0 29 A1 [-] Instr [b] Intrument (b = TRES) -------------------------------------------------------------------------------- Byte-by-byte Description of file: table4.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 14 F14.6 d BJD Barycentric Julian date 16- 21 F6.1 m/s RVres RV residuals after subtracting Pr 0211b 23- 26 F4.1 m/s e_RVres Error on RV residuals 28- 32 F5.1 m/s BIS ?=- Bisector span 34- 38 F5.1 m/s b_BIS ?=- Lower value of BIS interval 40- 45 F6.1 m/s B_BIS ?=- Upper value of BIS interval 47- 51 F5.1 m/s DeltaV ?=- DeltaV 53- 57 F5.1 m/s Vspan ?=- Velocity span 59- 63 F5.3 km/s FWHM ?=- FWHM of the CCF 65- 69 F5.3 km/s e_FWHM ?=- Error on FWHM 71- 75 F5.2 10-3 Vasy ?=- V asymmetry 77- 80 F4.2 10-3 e_Vasy ?=- Error on V Asymmetry -------------------------------------------------------------------------------- Byte-by-byte Description of file: table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 14 F14.6 d BJD Barycentric Julian date 16- 22 F7.4 [-] logRHK ?=- Mount Wilson logR_HK index 24- 29 F6.4 [-] e_logRHK ?=- Error on logR_HK 31- 36 F6.4 [-] Halpha ?=- Halpha activity index 38- 43 F6.4 [-] e_Halpha ?=- Error on Halpha activity index 45- 50 F6.4 [-] HeI ?=- HeI activity index 52- 57 F6.4 [-] e_HeI ?=- Error on HeI activity index 59- 64 F6.4 [-] NaID ?=- NaID activity index 66- 71 F6.4 [-] e_NaID ?=- Error on NaID activity index -------------------------------------------------------------------------------- Acknowledgements: Luca Malavolta, luca.malavolta(at)unipd.it References: Santos et al., 2011A&A...533A.141S 2011A&A...533A.141S, Cat. J/A+A/533/A141 Figueira et al., 2013A&A...557A..93F 2013A&A...557A..93F
(End) Luca Malavolta [UniPD, Italy], Patricia Vannier [CDS] 25-Feb-2016
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