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J/A+A/613/A41       5 exoplanet light and RV curves             (Mancini+, 2018)

The GAPS Programme with HARPS-N at TNG. XVI. Measurement of the Rossiter-McLaughlin effect of the transiting planetary systems HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60. Mancini L., Esposito M., Covino E., Southworth J., Biazzo K., Bruni I., Ciceri S., Evans D., Lanza A. F., Poretti E., Sarkis P., Smith A.M.S., Brogi M., Affer L., Benatti S., Bignamini A., Boccato C., Bonomo A.S., Borsa F., Carleo I., Claudi R., Cosentino R., Damasso M., Desidera S., Giacobbe P., Gonzalez-Alvarez E., Gratton R., Harutyunyan A., Leto G., Maggio A., Malavolta L., Maldonado J., Martinez-Fiorenzano A., Masiero S., Micela G., Molinari E., Nascimbeni V., Pagano I., Pedani M., Piotto G., Rainer M., Scandariato G., Smareglia R., Sozzetti A., Andreuzzi G., Henning T. <Astron. Astrophys. 613, A41 (2018)> =2018A&A...613A..41M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Exoplanets ; Radial velocities ; Photometry Keywords: planetary systems - stars: late-type - stars: fundamental parameters - techniques: radial velocities - techniques: photometric - Abstract: The measurement of the orbital obliquity of hot Jupiters, with different physical characteristics, can provide clues to the mechanisms of migration and orbital evolution of this particular class of giant exoplanets. We aim to derive the degree of alignment between planetary orbit and stellar spin angular momentum vectors and look for possible links with other orbital and fundamental physical parameters of the star-planet system. Here we focus on the characterisation of five transiting planetary systems (HAT-P-3, HAT-P-12, HAT-P-22, WASP-39 and WASP-60) and the determination of their sky-projected planet orbital obliquity through the measurement of the Rossiter-McLaughlin effect. We used HARPS-N high-precision radial velocity measurements, gathered during transit events, to measure the Rossiter-McLaughlin effect in the target systems and determine the sky-projected angle between the planetary orbital plane and the stellar equator. The characterisation of stellar atmospheric parameters was performed exploiting the HARPS-N spectra, using line equivalent width ratios, and spectral synthesis methods. Photometric parameters of the five transiting exoplanets were re-analysed through 17 new light curves, obtained with an array of medium-class telescopes, and other light curves from the literature. Survey-time-series photometric data were analysed for determining the rotation periods of the five stars and their spin inclination. From the analysis of the Rossiter-McLaughlin effect we derived a sky-projected obliquity of λ=21.2±8.7°, {lambda=-54+41-13°, {lambda=-2.1±3.0°, lambda=0±11° and lambda=-129±17° for HAT-P-3 b, HAT-P-12 b, HAT-P-22 b, WASP-39 b and WASP-60 b, respectively. The latter value indicates that WASP-60 b is moving on a retrograde orbit. These values represent the first measurements of λ for the five exoplanetary systems under study. The stellar activity of HAT-P-22 indicates a rotation period of 28.7±0.4-days, which allowed us to estimate the true misalignment angle of HAT-P-22 b, ψ=24±18°. The revision of the physical parameters of the five exoplanetary systems returned values fully compatible with those existing in the literature, with the exception of the WASP-60 system, for which, based on higher quality spectroscopic and photometric data, we found a more massive and younger star, and a larger and hotter planet. Description: Radial velocity measurements of HAT-P-3, HAT-P-12, HAT-P-22, WASP-39, and WASP-60 obtained with HARPS-N at the 3.5m TNG telescope. Light curves of transit events of the extrasolar planet HAT-P-3b, HAT-P-12b and WASP-60b. Two of the datasets were obtained using the Cassini 1.52m Telescope (Gunn r and Gunn i) at the Astronomical Observatory of Bologna in Loiano (Italy). Ten of the datasets were obtained using the Zeiss 1.23m telescope (Cousins R and Cousins I) at the German-Spanish Astronomical Centre at Calar Alto (Spain). Four of the datasets were obtained using the 2.2m telescope (Stromgren u, Gunn g, Gunn r, Johnson I) at the German-Spanish Astronomical Centre at Calar Alto (Spain). One of the datasets was obtained using the 2.5m Isaac Newton Telescope (INT) in La Palma (Spain). Objects: -------------------------------------------------------------- RA (2000) DE Designation(s) -------------------------------------------------------------- 13 44 22.59 +48 01 43.2 HAT-P-3 = 2MASS J13442258+4801432 13 57 33.47 +43 29 36.8 HAT-P-12 = 2MASS J13573347+4329367 10 22 43.51 +50 07 42.0 HAT-P-22 = HD 233731 14 29 18.42 -03 26 40.1 WASP-039 = 2MASS J14291840-0326403 23 46 39.98 +31 09 21.4 WASP-060 = 2MASS J23463997+3109213 -------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 101 5 Final photometric parameters for the five exoplanetary systems analysed in this work listphot.dat 49 17 List of photometric files phot/* 35 17 Individual light curve files rv/* 31 5 Individual velocity curve files
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) J/A+A/599/A90 : Characterization of HD 108874 system (Benatti+, 2017) J/A+A/602/A107 : 231 transiting planets eccentricity and mass (Bonomo+, 2017) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 A8 --- System System name 10 A1 --- n_System [abcde] Note on System (1) 12- 21 F10.8 d Porb Orbital period 23- 31 F9.8 d e_Porb rms uncertainty on Porb 33- 43 F11.5 d BJD Time of mid-transit (BJD-2400000) 45- 50 F6.5 d e_BJD rms uncertainty on BJD 52- 56 F5.2 deg Incl Orbital inclination 58- 61 F4.2 deg e_Incl rms uncertainty on Incl 63- 69 F7.5 --- r*+rP Sum of fractional stellar and planetary radii 71- 77 F7.5 --- e_r*+rP rms uncertainty on r*+rP 79- 85 F7.5 --- rP/r* Ratio of fractional planetary to stellar radii 87- 93 F7.5 --- e_rP/r* rms uncertainty on rP/r* 95- 98 A4 --- phot Indicates photometric data in subdirectory phot 100-101 A2 --- rv Indicates radial velocity data in subdirectory rv
Note (1): Notes as follows: a = The photometric parameters of HAT-P-3 were estimated from the light curves presented in this work (Fig. 1), incorporating results from Southworth (2012. Cat. J/MNRAS/426/1291) (see text). Photometric files for CA 1.23m I and Cassini i. b = The photometric parameters of HAT-P-12 were estimated from the light curves presented in this work, see Fig. 2. Photometric files for CA 2.2m ugri, CA 1.23m IR, INT r and Cassini r c = The photometric parameters of HAT-P-22 were estimated from the light curves taken from different works (Bakos et al., 2011, Cat. J/ApJ/742/116; Basturk et al., 2015, ASP Conference Series, 496, 370; Hinse et al., 2015, . Astron. Space Sci, 32, 21; Turner et al., 2016MNRAS.459..789T), see Fig. 3. d = The photometric parameters of WASP-39 were estimated from the light curves taken from different works (Faedi et al., 2011, Cat. J/A+A/531/A40; Ricci et al., 2015, Cat. J/PASP/127/143; Maciejewski et al., 2016AcA....66...55M), see Fig. 4. e = The photometric parameters of WASP-60 were estimated from the light curve presented in this work and the one from Turner et al. (2017MNRAS.472.3871T), see Fig. 5. Photometric file for CA 1.23m I.
Byte-by-byte Description of file: listphot.dat
Bytes Format Units Label Explanations
1- 8 A8 --- System System name 10- 19 A10 "date" Obs.date Observation date 21- 28 A8 --- Inst Instrument 30 A1 --- Band [ugriIR] Band 32- 49 A18 --- FileName Name of the file with photometry in subdirectory phot
Byte-by-byte Description of file: phot/*
Bytes Format Units Label Explanations
1- 12 F12.6 d BJD(TDB) Barycentric JD for the midpoint of observation 16- 24 F9.6 mag mag Differential magnitude of the target 28- 35 F8.6 mag e_mag Measurement error of the magnitude
Byte-by-byte Description of file: rv/*
Bytes Format Units Label Explanations
1- 12 F12.6 d BJD(TDB) Barycentric JD for the midpoint of observation 14- 21 F8.1 m/s RV Radial Velocity (RV) of the target 23- 26 F4.1 m/s e_RV Measurement error of RV 28- 31 F4.1 m/s S/N Signal-to-noise ration
Acknowledgements: Luigi Mancini, lmancini(at)roma2.infn.it, University of Rome Tor Vergata 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 Benatti et al., Paper XII 2017A&A...599A..90B, Cat. J/A+A/599/A90 Esposito et al., Paper XIII 2017A&A...601A..53E Bonomo et al. Paper XIV 2017A&A...602A.107B, Cat. J/A+A/602/A107 Gonzalez-Alvarez et al., Paper XV 2017A&A...606A..51G
(End) L. Mancini [Rome Tor Vergata Univ. Italy], P. Vannier [CDS] 16-Feb-2018
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