A PROGRADE, LOW-INCLINATION ORBIT FOR THE VERY HOT JUPITER WASP-3b

Tripathi, Anjali; Winn, Joshua N.; Johnson, John Asher; Howard, Andrew W.; Halverson, Samuel; Marcy, Geoffrey W.; Holman, Matthew J.; Kleer, K. de; Carter, Joshua A.; Esquerdo, Gilbert A.; Everett, Mark E.; Cabrera, Nicole

doi:10.1088/0004-637x/715/1/421

Cited by 56 publications

(72 citation statements)

References 48 publications

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“…• is close to zero and agrees with the previous results found by Simpson et al (2010) and Tripathi et al (2010). Our value of v sin i = 13.9 ± 0.03 km s −1 is in agreement with the value obtained from the spectroscopic broadening but determined to a much higher level of precision.…”

Section: Discussionsupporting

confidence: 93%

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The Doppler shadow of WASP-3b

Miller

Cameron

Simpson

et al. 2010

A&A

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Context. Hot-Jupiter planets must form at large separations from their host stars where the temperatures are cool enough for their cores to condense. They then migrate inwards to their current observed orbital separations. Different theories of how this migration occurs lead to varying distributions of orbital eccentricity and the alignment between the rotation axis of the star and the orbital axis of the planet. Aims. The spin-orbit alignment of a transiting system is revealed via the Rossiter-McLaughlin effect, which is the anomaly present in the radial velocity measurements of the rotating star during transit due to the planet blocking some of the starlight. In this paper we aim to measure the spin-orbit alignment of the WASP-3 system via a new way of analysing the Rossiter-McLaughlin observations. Methods. We apply a new tomographic method for analysing the time variable asymmetry of stellar line profiles caused by the Rossiter-McLaughlin effect. This new method eliminates the systematic error inherent in previous methods used to analyse the effect. Results. We find a value for the projected stellar spin rate of v sin i = 13.9 ± 0.03 km s −1 which is in agreement with previous measurements but has a much higher precision. The system is found to be well aligned, with λ = 5 +6 −5• which favours an evolutionary history for WASP-3b involving migration through tidal interactions with a protoplanetary disc. From comparison with isochrones we put an upper limit on the age of the star of 2 Gyr.

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Section: Discussionsupporting

confidence: 93%

“…For λ they derived a value of 13 +9 −7 • which agrees with our result. In addition to this Tripathi et al (2010) performed an analysis of a separate set of data and retrieved values that are in good agreement with those found in this study, as can be seen in Table 2.…”

Section: Resultssupporting

confidence: 83%

The Doppler shadow of WASP-3b

Miller

Cameron

Simpson

et al. 2010

A&A

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“…More in general, results obtained from subsets T1-3 (Sloan i) and T5-6 (Sloan g) slightly but significantly disagree with each other, which was already noted by Tripathi et al (2010), who attributed this to the presence of residual red noise.…”

Section: --mentioning

confidence: 54%

“…With the only exception of N3, the final IAC80 light curves have σ 120 = 0.67−0.95 mmag (Table 1, Fig. 2), only slightly higher than that achieved by Gibson et al (2008), Tripathi et al (2010) and Christiansen et al (2011), with space-based or much larger facilities. N6 shows a large amount of red noise of unknown origin, which is probably related to color-dependent systematics caused by variable atmospheric extinction.…”

Section: Iac80 Photometrymentioning

confidence: 82%

“…The RISE camera filter has a custom wideband 500−700 nm, approximately covering both the Johnson R and V passbands. - Tripathi et al (2010): five transits in 2008/2009 (T1-5) from two different telescopes (Fred Lawrence Whipple Observatory FLWO-1.2 m and University of Hawaii UH-2.2 m) and in three Sloan passbands (g, i, z), gathered to complement their high-precision RV measurements. The first two FLWO i transits (T1-2) are partial, the first one missing the first contact by only few minutes.…”

Section: Archival Light Curvesmentioning

confidence: 99%

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Taste

Nascimbeni

Cunial

Murabito

et al. 2012

A&A

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The TASTE project is searching for low-mass planets with the transit timing variation (TTV) technique by gathering high-precision, short-cadence light curves for a selected sample of transiting exoplanets. It has been claimed that the "hot Jupiter" WASP-3b could be perturbed by a second planet. Presenting eleven new light curves (secured at the IAC80 and UDEM telescopes) and re-analyzing thirty-eight archival light curves in a homogeneous way, we show that new data do not confirm the previously claimed TTV signal. However, we bring evidence that measurements are not consistent with a constant orbital period, though no significant periodicity can be detected. Additional dynamical modeling and follow-up observations are planned to constrain the properties of the perturber or to put upper limits to it. We provide a refined ephemeris for WASP-3b and improved orbital/physical parameters. A contact eclipsing binary, serendipitously discovered among field stars, is reported here for the first time.

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ExoClock project: an open platform for monitoring the ephemerides of Ariel targets with contributions from the public

et al. 2021

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The Ariel mission will observe spectroscopically around 1000 exoplanets to further characterise their atmospheres. For the mission to be as efficient as possible, a good knowledge of the planets’ ephemerides is needed before its launch in 2028. While ephemerides for some planets are being refined on a per-case basis, an organised effort to collectively verify or update them when necessary does not exist. In this study, we introduce the ExoClock project, an open, integrated and interactive platform with the purpose of producing a confirmed list of ephemerides for the planets that will be observed by Ariel. The project has been developed in a manner to make the best use of all available resources: observations reported in the literature, observations from space instruments and, mainly, observations from ground-based telescopes, including both professional and amateur observatories. To facilitate inexperienced observers and at the same time achieve homogeneity in the results, we created data collection and validation protocols, educational material and easy to use interfaces, open to everyone. ExoClock was launched in September 2019 and now counts over 140 participants from more than 15 countries around the world. In this release, we report the results of observations obtained until the 15h of April 2020 for 120 Ariel candidate targets. In total, 632 observations were used to either verify or update the ephemerides of 84 planets. Additionally, we developed the Exoplanet Characterisation Catalogue (ECC), a catalogue built in a consistent way to assist the ephemeris refinement process. So far, the collaborative open framework of the ExoClock project has proven to be highly efficient in coordinating scientific efforts involving diverse audiences. Therefore, we believe that it is a paradigm that can be applied in the future for other research purposes, too.

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A PROGRADE, LOW-INCLINATION ORBIT FOR THE VERY HOT JUPITER WASP-3b

Cited by 56 publications

References 48 publications

The Doppler shadow of WASP-3b

The Doppler shadow of WASP-3b

Taste

ExoClock project: an open platform for monitoring the ephemerides of Ariel targets with contributions from the public

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