<i>MOST</i>SPACE TELESCOPE PHOTOMETRY OF THE 2010 JANUARY TRANSIT OF EXTRASOLAR PLANET HD80606b

Roberts, Jessica; Barnes, Jason W.; Rowe, Jason F.; Fortney, Jonathan J.

doi:10.1088/0004-637x/762/1/55

Cited by 37 publications

(3 citation statements)

References 17 publications

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“…A few days after again with Spitzer, Hébrard et al (2011) observed the whole transit of January 2010 with a mid-time accuracy of ±85 seconds. Roberts et al (2013) observed the same transit with the MOST satellite and reached a lower accuracy of ±294 seconds. All the other available observations were made from the ground in February 2009 (Moutou et al 2009;Garcia-Melendo & McCullough 2009;Fossey et al 2009;Hidas et al 2010), June 2009(Winn et al 2009, or January 2010 (Shporer et al 2010) and could only observe partial portions of transits with a given telescope; so their accuracies on the mid-transit times were ±310 seconds or even poorer.…”

Section: Conclusion and Discussionmentioning

confidence: 84%

Detecting the general relativistic orbital precession of the exoplanet HD 80606b

Blanchet

Hébrard

Larrouturou

2019

A&A

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We investigate the relativistic effects in the orbital motion of the exoplanet HD 80606b with a high eccentricity of e 0.93. We propose a method to detect these effects (notably the orbital precession) based on measuring the successive eclipse and transit times of the exoplanet. In the case of HD 80606b, we find that in ten years (after approximately 33 periods) the instants of transits and eclipses are delayed with respect to the Newtonian prediction by about three minutes due to relativistic effects. These effects can be detected by comparing at different epochs the time difference between a transit and the preceding eclipse, and should be measurable by comparing events already observed on HD 80606 in 2010 with the Spitzer satellite together with those to be observed in the future with the James Webb Space Telescope.

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Section: Conclusion and Discussionmentioning

confidence: 84%

Detecting the general relativistic orbital precession of the exoplanet HD 80606b

Blanchet

Hébrard

Larrouturou

2019

A&A

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“…Figure 2a shows the relative polarimetric amplitude of a transit versus R p /R * for R p /R * < 0.5 and b = 0. We adopt HD 80606 limb darkening coefficients (Roberts et al 2013, c 1 = 0.742 and c 2 = 0.458), as well as 460 nm solar limb polarization profile coefficients (Faurobert et al 2001, P 1 = 0.87% and k = 70), because limb polarization is difficult to measure for most stars.…”

Section: Scaling With Planet/star Radius Ratiomentioning

confidence: 99%

“…The POLISH2 polarimeter at the Lick Observatory Shane 3-m telescope uses two photoelastic modulators to simultaneously measure Stokes I, Q, U , and V (see Wiktorowicz & Matthews 2008;Wiktorowicz 2009 for the prototype POLISH). Using this system, we obtain B band observations during a transit ingress of HD 80606b (first contact 06:17 UT, February 1, 2013: H10; Shporer et al 2010;Roberts et al 2013). We also obtain 4.9 hours of control data during the previous night to complement the 7.1 hour observation during transit.…”

Section: Observationsmentioning

confidence: 99%

Toward the Detection of Exoplanet Transits With Polarimetry

Wiktorowicz¹,

Laughlin

2014

ApJ

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In contrast to photometric transits, whose peak signal occurs at mid-transit due to occultation of the brightest region of the disk, polarimetric transits provide a signal upon ingress and egress due to occultation of the polarized stellar limb. Limb polarization, the bright corollary to limb darkening, arises from the 90 • scattering angle and low optical depth experienced by photons at the limb. In addition to the ratio R p /R * , the amplitude of a polarimetric transit is expected to be controlled by the strength and width of the stellar limb polarization profile, which depend on the scattering-tototal opacity ratio at the stellar limb. We present a short list of the systems providing the highest expected signal-to-noise ratio for detection of this effect, and we draw particular attention to HD 80606b. This planet is spin/orbit misaligned, has a three-hour ingress, and has a bright parent star, which make it an attractive target. We report on test observations of an HD 80606b ingress with the POLISH2 polarimeter at the Lick Observatory Shane 3-m telescope. We conclude that unmodeled telescope systematic effects prevented polarimetric detection of this event. We outline a roadmap for further refinements of exoplanet polarimetry, whose eventual success will require a further factor of ten reduction in systematic noise.

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The Exoplanet Handbook

Perryman¹

2018

177

149

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MOSTSPACE TELESCOPE PHOTOMETRY OF THE 2010 JANUARY TRANSIT OF EXTRASOLAR PLANET HD80606b

Cited by 37 publications

References 17 publications

Detecting the general relativistic orbital precession of the exoplanet HD 80606b

Detecting the general relativistic orbital precession of the exoplanet HD 80606b

Toward the Detection of Exoplanet Transits With Polarimetry

The Exoplanet Handbook

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