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:
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RA (2000) DE Designation(s)
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08 42 11.49 +19 16 37.7 Pr 0211 = NAME Pr 0211
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File Summary:
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FileName Lrecl Records Explanations
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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
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See also:
J/A+A/533/A141 : Stellar parameters for 582 HARPS FGK stars (Sousa+, 2011)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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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)
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Byte-by-byte Description of file: table3a.dat
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Bytes Format Units Label Explanations
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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)
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Byte-by-byte Description of file: table3b.dat
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Bytes Format Units Label Explanations
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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)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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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
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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