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|Title:||The GAPS Programme with HARPS-N at TNG. VIII. Observations of the Rossiter-McLaughlin effect and characterisation of the transiting planetary systems HAT-P-36 and WASP-11/HAT-P-10||Authors:||Mancini, L.
BONOMO, ALDO STEFANO
LANZA, Antonino Francesco
Martinez Fiorenzano, A. F.
MOLINARI, Emilio Carlo
Zanmar Sanchez, R.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||579||First Page:||A136||Abstract:||Context. Orbital obliquity is thought to be a fundamental parameter in tracing the physical mechanisms that cause the migration of giant planets from the snow line down to roughly 10<SUP>-2</SUP> au from their host stars. We are carrying out a large programme to estimate the spin-orbit alignment of a sample of transiting planetary systems to study what the possible configurations of orbital obliquity are and whether they correlate with other stellar or planetary properties. <BR /> Aims: We determine the true and the projected obliquity of HAT-P-36 and WASP-11/HAT-P-10 systems, respectively, which are both composed of a relatively cool star (with effective temperature T<SUB>eff</SUB>< 6100 K) and a hot-Jupiter planet. <BR /> Methods: Thanks to the high-resolution spectrograph HARPS-N, we observed the Rossiter-McLaughlin effect for both systems by acquiring precise (3-8 m s<SUP>-1</SUP>) radial-velocity measurements during planetary transit events. We also present photometric observations comprising six light curves that cover five transit events, which were obtained using three medium-class telescopes. One transit of WASP-11/HAT-P-10 was followed simultaneously from two observatories. The three transit light curves of HAT-P-36 b show anomalies that are attributable to starspot complexes on the surface of the parent star, in agreement with the analysis of its spectra that indicates moderate activity ( log R'<SUB>HK</SUB> = -4.65 dex). By analysing the complete HATNet data set of HAT-P-36, we estimated the stellar rotation period by detecting a periodic photometric modulation in the light curve caused by star spots, obtaining P<SUB>rot</SUB> = 15.3 ± 0.4 days, which implies that the inclination of the stellar rotational axis with respect to the line of sight is i<SUB>⋆</SUB> = 65° ± 34°. <BR /> Results: We used the new spectroscopic and photometric data to revise the main physical parameters and measure the sky-projected misalignment angle of the two systems. We found λ = -14° ± 18° for HAT-P-36 and λ = 7° ± 5° for WASP-11/HAT-P-10, indicating in both cases a good spin-orbit alignment. In the case of HAT-P-36, we were also able to estimate an upper limit of its real obliquity, which turned out to be ψ< 63 degrees. <P />Based on observations made with (i) the Italian 3.58 m Telescopio Nazionale Galileo at the Observatory of Roque de los Muchachos; (ii) the Cassini 1.52 m telescope at the Astronomical Observatory of Bologna; (iii) the Zeiss 1.23 m telescope at the Observatory of Calar Alto, and the IAC 80 cm telescope at the Teide Observatory.Table 1 and Appendix A are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201526030/olm">http://www.aanda.org</A>Data of the light curves are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://18.104.22.168) or via <A href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/579/A136">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/579/A136</A>||Acknowledgments:||The HARPS-N instrument has been built by the HARPS-N Consortium, a collaboration between the Geneva Observatory (PI Institute), the Harvard-Smithonian Center for Astrophysics, the University of St. Andrews, the University of Edinburgh, the Queen’s University of Belfast, and INAF. Operations at the Calar Alto telescopes are jointly performed by the Max-Planck Institut für Astronomie (MPIA) and the Instituto de Astrofísica de Andalucía (CSIC). The reduced light curves presented in this work will be made available at the CDS ( http://cdsweb.u-strasbg.fr/ ). The GAPS project in Italy acknowledges support from INAF through the “Progetti Premiali” funding scheme of the Italian Ministry of Education, University, and Research. We acknowledge the use of the following internet-based resources: the ESO Digitized Sky Survey; the TEPCat catalogue; the SIMBAD data base operated at the CDS, Strasbourg, France; and the arXiv scientific paper preprint service operated by Cornell University.||URI:||http://hdl.handle.net/20.500.12386/23112||URL:||https://www.aanda.org/articles/aa/abs/2015/07/aa26030-15/aa26030-15.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201526030||Bibcode ADS:||2015A&A...579A.136M||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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