2010A&A...516A..95H


Query : 2010A&A...516A..95H

2010A&A...516A..95H - Astronomy and Astrophysics, volume 516, A95-95 (2010/6-3)

Observation of the full 12-hour-long transit of the exoplanet HD 80606b. Warm-Spitzer photometry and SOPHIE spectroscopy.

HEBRARD G., DESERT J.-M., DIAZ 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., SEGRANSAN D., SING D.K., UDRY S. and VIDAL-MADJAR A.

Abstract (from CDS):

We present new observations of a transit of the 111.4-day-period exoplanet HD80606b. Due to this long orbital period and to the orientation of the eccentric orbit (e=0.9), HD80606b'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 HD80606 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 HD80606 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 λ=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 HD80606, 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.

Abstract Copyright:

Journal keyword(s): techniques: radial velocities - techniques: photometric - stars: individual: HD80606

VizieR on-line data: <Available at CDS (J/A+A/516/A95): spitzer.dat sophie.dat>

Simbad objects: 27

goto Full paper

goto View the references in ADS

Number of rows : 27
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HD 17156b Pl 02 49 44.4866941172 +71 45 11.632197644           ~ 173 1
2 HD 17156 PM* 02 49 44.4871034544 +71 45 11.629235988   8.78 8.16     F9V 160 2
3 HD 20782b Pl 03 20 03.5777409770 -28 51 14.660409684           ~ 63 1
4 BD+57 793 * 04 21 52.7048156328 +57 49 01.889294952   10.27 9.85     F5V 144 2
5 CoRoT-1 * 06 48 19.1723766840 -03 06 07.710745140     13.6 13.44 12.88 G0V 117 2
6 HAT-P-13 * 08 39 31.8072358440 +47 21 07.273799280   11.15 10.42 10.40   G4 127 2
7 HD 80606 PM* 09 22 37.5768032712 +50 36 13.435326684   9.78 9.00     G8V 310 2
8 HD 80606b Pl 09 22 37.5769478105 +50 36 13.434928660           ~ 301 1
9 HD 80607 PM* 09 22 39.7366541424 +50 36 13.952919312   9.937 9.070     G5 92 2
10 BD+22 2716 * 14 33 06.3571702344 +21 53 40.981395876   10.194 9.745     F5V 92 1
11 CD-27 10695 * 15 59 50.9491505016 -28 03 42.312819096   11.83 11.59 11.31 10.92 F4 106 1
12 HD 147506 * 16 20 36.3576063720 +41 02 53.106772488   9.15 8.69     F8V 155 2
13 HD 149026 PM* 16 30 29.6185771608 +38 20 50.308980864   8.75 8.14     G0IV 215 1
14 TrES-4 Pl 17 53 13.0490781575 +37 12 42.586106196           ~ 196 2
15 BD+35 3293 V* 18 34 31.6252443960 +35 39 41.491899468   11.07 10.63 10.52   F7V 121 1
16 CoRoT-9b Pl 18 43 08.8101080314 +06 12 14.912939950           ~ 63 1
17 Kepler-8 Ro* 18 45 09.1489991376 +42 27 03.891327156           F6V 101 1
18 NAME V672 Lyr b Pl 19 04 09.8516024106 +36 37 57.445911611           ~ 324 1
19 Kepler-1b Pl 19 07 14.0379171930 +49 18 59.090895318           ~ 308 2
20 CoRoT-2 * 19 27 06.4944378024 +01 23 01.359897468   13.422 12.568 12.204 11.49 G7V+K9V 234 2
21 CoRoT-3 EB* 19 28 13.2642131544 +00 07 18.613986132   14.199 13.292 13.099 12.54 F3V 73 1
22 BD+47 2846 Er* 19 28 59.3538826128 +47 58 10.217007804   10.97 10.48     F6V 284 2
23 HD 189733 BY* 20 00 43.7129433648 +22 42 39.073143456 9.241 8.578 7.648 7.126 6.68 K2V 820 1
24 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1305 1
25 HD 209458 V* 22 03 10.7727465312 +18 53 03.549393384   8.21 7.63     F9V 1061 1
26 BD+37 4734B PM* 22 57 46.8442481880 +38 40 30.358351704   10.82 9.87     G0V 156 1
27 WASP-6 * 23 12 37.7368282608 -22 40 26.273805024   12.90 11.91     G8V 84 1

To bookmark this query, right click on this link: simbad:objects in 2010A&A...516A..95H and select 'bookmark this link' or equivalent in the popup menu


2022.12.07-05:20:34

© Université de Strasbourg/CNRS

    • Contact