An ingress and a complete transit of HD 80606 b

Hidas, M. G.; Tsapras, Y.; Mislis, D.; Ramaprakash, A. N.; Barros, S. C. C.; Street, R. A.; Schmitt, J. H. M. M.; Steele, I. A.; Pollacco, D.; Ayiomamitis, Anthony; Antoniadis, John; Nitsos, Athanasios; Seiradakis, J. H.; Urakawa, Seitaro

doi:10.1111/j.1365-2966.2010.16744.x

Cited by 10 publications

(7 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The HD 80606's system parameters that we report in Table 1 have a better accuracy than previous studies Pont et al 2009;Gillon 2009;Winn et al 2009a;Hidas et al 2010). With respect to the ground observation of nearly all the transit phases used by Winn et al (2009a), the uncertainties presented here are better by factors two to five.…”

Section: Comparison With Previous Measurementsmentioning

confidence: 51%

“…The fortunate transiting nature of HD 80606b was established in 2009 February from the detection of a transit reported from ground observations, independently by Moutou et al (2009) from photometric and spectroscopic data, and by Garcia-Melendo & McCullough (2009) and Fossey et al (2009) from photometric measurements. Additional observations of transits were later reported by Winn et al (2009a) and Hidas et al (2010). The 2009 February observations followed the planetary eclipse discovery reported a few months before by Laughlin et al (2009) from Spitzer photometric observations at 8 μm during a 30-h interval around the periastron.…”

Section: Introductionmentioning

confidence: 77%

See 1 more Smart Citation

Observation of the full 12-hour-long transit of the exoplanet HD 80606b

Hébrard¹,

Désert

Díaz³

et al. 2010

A&A

110

View full text Add to dashboard Cite

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 postcryogenic 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 R p /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 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 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.

show abstract

Section: Comparison With Previous Measurementsmentioning

confidence: 51%

Section: Introductionmentioning

confidence: 77%

Observation of the full 12-hour-long transit of the exoplanet HD 80606b

Hébrard¹,

Désert

Díaz³

et al. 2010

A&A

110

View full text Add to dashboard Cite

show abstract

“…The transit planet searches, conveniently operating in the sin i ≈ 1 domain (i being orbital inclination), discover exoplanets with relatively short orbital periods (orbital separations) due to the natural limit of the observable transit length set by the lengths of a night (a condition now being relaxed with the multi-site or space observations, cf. HD 80606 b - Hidas et al 2010;Hébrard et al 2010;Kepler 11g -Lissauer et al 2011). Searches for planets based on the radial velocity (RV) technique are the most versatile.…”

Section: Introductionmentioning

confidence: 99%

The Penn State-Toruń Centre for Astronomy Planet Search stars

Zieliński

Niedzielski

Wolszczan

et al. 2012

A&A

View full text Add to dashboard Cite

Aims. We present basic atmospheric parameters (T eff , log g, v t , and [Fe/H]) as well as luminosities, masses, radii, and absolute radial velocities for 348 stars, presumably giants, from the ∼1000 star sample observed within the Penn State-Toruń Centre for Astronomy Planet Search with the High Resolution Spectrograph of the 9.2 m Hobby-Eberly Telescope. The stellar parameters (luminosities, masses, radii) are key to properly interpreting newly discovered low-mass companions, while a systematic study of the complete sample will create a basis for future statistical considerations concerning the appearance of low-mass companions around evolved low-and intermediate-mass stars. Methods. The atmospheric parameters were derived using a strictly spectroscopic method based on the LTE analysis of equivalent widths of Fe I and Fe II lines. With existing photometric data and the Hipparcos parallaxes, we estimated stellar masses and ages via evolutionary tracks fitting. The stellar radii were calculated from either estimated masses and the spectroscopic log g or from the spectroscopic T eff and estimated luminosities. The absolute radial velocities were obtained by cross-correlating spectra with a numerical template. Results. We completed the spectroscopic analysis for 332 stars, 327 of which were found to be giants. A simplified analysis was applied to the remaining 16 stars, which had incomplete data. The results show that our sample is composed of stars with effective temperatures ranging from 4055 K to 6239 K, with log g between 1.39 and 4.78 (5 dwarfs were identified). The estimated luminosities are between log L/L = −1.0 and 3 and lead to masses ranging from 0.6 to 3.4 M . Only 63 stars with masses larger than 2 M were found. The radii of our stars range from 0.6 to 52 R with the vast majority between 9−11 R . The stars in our sample are generally less metal-abundant than the Sun with median [Fe/H] = −0.15. The estimated uncertainties in the atmospheric parameters were found to be comparable to those reached in other studies. However, due to lack of precise parallaxes, the stellar luminosities and, in turn, the masses are far less precise, within 0.2 M in best cases and 0.3 M on average.

show abstract

“…Even when considering moons of a high density of 6 g cm −3 and an extreme Q p of 10 13 , WASP-19b, CoRoT-7b, WASP-18b and WASP-12b are excluded to have large moons. In the case of HD 80606b (Naef et al 2001;Hidas et al 2010;Hebrard et al 2010) both retro-and prograde moons are excluded due to the large eccentricity of the planets orbit. For this planet, only for a moon with a density larger than 31 g cm −3 would be the Roche-radius smaller than the prograde Hill-radius.…”

Section: Discussionmentioning

confidence: 99%

Limits on the orbits and masses of moons around currently-known transiting exoplanets

Weidner

Horne²

2010

A&A

View full text Add to dashboard Cite

Aims. Current and upcoming space missions may be able to detect moons of transiting extra-solar planets. In this context it is important to understand if exomoons are expected to exist and what their possible properties are. Methods. Using estimates for the stability of exomoon orbits from numerical studies, a list of 87 known transiting exoplanets is tested for the potential to host large exomoons. Results. For 92% of the sample, moons larger than Luna can be excluded on prograde orbits, unless the parent exoplanet's internal structure is very different from the gas-giants of the solar system. Only WASP-24b, OGLE2-TR-L9, CoRoT-3b and CoRoT-9b could have moons above 0.4 m ⊕ , which is within the likely detection capabilities of current observational facilities. Additionally, the range of possible orbital radii of exomoons of the known transiting exoplanets, with two exceptions, is below 8 Jupiter-radii and therefore rather small.

show abstract

An ingress and a complete transit of HD 80606 b

Cited by 10 publications

References 15 publications

Observation of the full 12-hour-long transit of the exoplanet HD 80606b

Observation of the full 12-hour-long transit of the exoplanet HD 80606b

The Penn State-Toruń Centre for Astronomy Planet Search stars

Limits on the orbits and masses of moons around currently-known transiting exoplanets

Contact Info

Product

Resources

About