Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:1004.0790)
· On-line Data
· References in the article
· Citations to the Article (67) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (27)
· Associated Articles
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Observation of the full 12-hour-long transit of the exoplanet HD 80606b. Warm-Spitzer photometry and SOPHIE spectroscopy
Authors:
Hébrard, G.; Désert, J.-M.; Díaz, R. F.; Boisse, I.; Bouchy, F.; Lecavelier Des Etangs, A.; Moutou, C.; Ehrenreich, D.; Arnold, L.; Bonfils, X.; Delfosse, X.; Desort, M.; Eggenberger, A.; Forveille, T.; Gregorio, J.; Lagrange, A.-M.; Lovis, C.; Pepe, F.; Perrier, C.; Pont, F.; Queloz, D.; Santerne, A.; Santos, N. C.; Ségransan, D.; Sing, D. K.; Udry, S.; Vidal-Madjar, A.
Affiliation:
AA(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France ), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France), AC(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France), AD(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France), AE(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France; Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l'Observatoire, France), AF(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France), AG(Laboratoire d'Astrophysique de Marseille, Univ. de Provence, CNRS (UMR6110), 38 rue F. Joliot Curie, 13388 Marseille, France), AH(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AI(Observatoire de Haute-Provence, CNRS/OAMP, 04870 Saint-Michel-l'Observatoire, France), AJ(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France; Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland), AK(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AL(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AM(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AN(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AO(CROW-Observatory Portalegre, Portugal, and Atalaia.org group, Portugal), AP(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AQ(Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland), AR(Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland), AS(Laboratoire d'Astrophysique de Grenoble, Université Joseph-Fourier, CNRS (UMR5571), BP 53, 38041 Grenoble Cedex 9, France), AT(School of Physics, University of Exeter, Exeter, EX4 4QL, UK), AU(Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland), AV(Laboratoire d'Astrophysique de Marseille, Univ. de Provence, CNRS (UMR6110), 38 rue F. Joliot Curie, 13388 Marseille, France), AW(Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal), AX(Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland), AY(School of Physics, University of Exeter, Exeter, EX4 4QL, UK), AZ(Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland), BA(Institut d'Astrophysique de Paris, UMR7095 CNRS, Université Pierre & Marie Curie, 98bis boulevard Arago, 75014 Paris, France)
Publication:
Astronomy and Astrophysics, Volume 516, id.A95, 14 pp. (A&A Homepage)
Publication Date:
06/2010
Origin:
EDP Sciences
Astronomy Keywords:
techniques: radial velocities, techniques: photometric, stars: individual: HD 80606
DOI:
10.1051/0004-6361/201014327
Bibliographic Code:
2010A&A...516A..95H

Abstract

We present new observations of a transit of the 111.4-day-period exoplanet HD 80606b. Due to this long orbital period and to the orientation of the eccentric orbit (e = 0.9), HD 80606b's transits last for about 12 hours. This makes the observation of a full transit practically impossible from a given ground-based observatory. With the Spitzer Space Telescope and its IRAC camera on the post-cryogenic mission, we performed a 19-h photometric observation of HD 80606 that covers the full 2010 January 13-14 transit as well as off-transit references immediately before and after the event. We complement these photometric data by new spectroscopic observations that we simultaneously performed with SOPHIE at the Haute-Provence Observatory. This provides radial velocity measurements of the first half of the transit that was previously uncovered with spectroscopy. This new dataset allows the parameters of this singular planetary system to be significantly refined. We obtained a planet-to-star radius ratio Rp/R* = 0.1001 ± 0.0006 that is more accurate but slightly lower than the one measured from previous ground observations in the optical. We found no astrophysical interpretations able to explain this difference between optical and infrared radii; we rather favor underestimated systematic uncertainties, maybe in the ground-based composite light curve. We detected a feature in the Spitzer light curve that could be due to a stellar spot. We also found a transit timing about 20 minutes earlier than the ephemeris prediction; this could be caused by actual transit-timing variations due to an additional body in the system, or again by underestimated systematic uncertainties. The actual angle between the spin-axis of HD 80606 and the normal to the planetary orbital plane is found to be near 40° thanks to the fit of the Rossiter-McLaughlin anomaly, with a sky-projected value lambda = 42° ± 8°. This allows scenarios with aligned spin-orbit to be definitively rejected. Over the twenty planetary systems with measured spin-orbit angles, a few are misaligned; this is probably the signature of two different evolution scenarios for misaligned and aligned systems, depending whether or not they experienced gravitational interaction with a third body. As in the case of HD 80606, most of the planetary systems including a massive planet are tilted; this could be the signature of a separate evolution scenario for massive planets compared with Jupiter-mass planets.

Based on observations collected with the SOPHIE spectrograph on the 1.93-m telescope at the Observatoire de Haute-Provence (CNRS), France, and with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Radial velocity and photometry tables are available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/516/A95

Associated Articles

Source Paper     Catalog Description    

Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints