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We report the discovery of a transiting, gas giant circumbinary planet orbiting the eclipsing binary KIC 4862625 and describe our independent discovery of the two transiting planets orbiting Kepler-47. We describe a simple and semi-automated procedure for identifying individual transits in light curves and present our follow-up measurements of the two circumbinary systems. For the KIC 4862625 system, the 0.52 ± 0.018 RJupiter radius planet revolves every ~138 days and occults the 1.47±0.08M⊙, 1.7±0.06 R⊙ F8 IV primary star producing aperiodic transits of variable durations commensurate with the configuration of the eclipsing binary star. Our best-fit model indicates the orbit has a semi-major axis of 0.64 AU and is slightly eccentric, e = 0.1. For the Kepler-47 system, we confirm the results of Orosz et al. Modulations in the radial velocity of KIC 4862625A are measured both spectroscopically and photometrically, i.e., via Doppler boosting, and produce similar results. [ABSTRACT FROM AUTHOR]

A correction to the article "Kepler-413B: A Slightly Misaligned, Neptune-Size Transiting Circumbinary Planet" by V. B. Kostov that was published in the journal in 2014 is presented.

We report the discovery of a transiting, Rp = 4.347 ± 0.099R⊕, circumbinary planet (CBP) orbiting the KeplerK+M eclipsing binary (EB) system KIC 12351927 (Kepler-413) every ∼66 days on an eccentric orbit with ap = 0.355 ± 0.002 AU, ep = 0.118 ± 0.002. The two stars, with MA = 0.820 ± 0.015 M☼, RA = 0.776 ± 0.009 R☼ and MB = 0.542 ± 0.008 M☼, RB = 0.484 ± 0.024 R☼, respectively, revolve around each other every 10.11615 ± 0.00001 days on a nearly circular (eEB = 0.037 ± 0.002) orbit. The orbital plane of the EB is slightly inclined to the line of sight (iEB = 87.°33 ± 0.°06), while that of the planet is inclined by ∼2.°5 to the binary plane at the reference epoch. Orbital precession with a period of ∼11 yr causes the inclination of the latter to the sky plane to continuously change. As a result, the planet often fails to transit the primary star at inferior conjunction, causing stretches of hundreds of days with no transits (corresponding to multiple planetary orbital periods). We predict that the next transit will not occur until 2020. The orbital configuration of the system places the planet slightly closer to its host stars than the inner edge of the extended habitable zone. Additionally, the orbital configuration of the system is such that the CBP may experience Cassini State dynamics under the influence of the EB, in which the planet's obliquity precesses with a rate comparable to its orbital precession. Depending on the angular precession frequency of the CBP, it could potentially undergo obliquity fluctuations of dozens of degrees (and complex seasonal cycles) on precession timescales. [ABSTRACT FROM AUTHOR]

We present measurements of the spin-orbit alignment angle, λ, for the hot Jupiter systems WASP-32, WASP-38, and HAT-P-27/WASP-40, based on data obtained using the HARPS spectrograph. We analyze the Rossiter-McLaughlin effect for all three systems and also carry out Doppler tomography for WASP-32 and WASP-38. We find that WASP-32 (Teff = 6140+90– 100 K) is aligned, with an alignment angle of λ = 10.°5 + 6.4 – 6.5 obtained through tomography, and that WASP-38 (Teff = 6180+40– 60 K) is also aligned, with tomographic analysis yielding λ = 7.°5 + 4.7 – 6.1. The latter result provides an order-of-magnitude improvement in the uncertainty in λ compared to the previous analysis of Simpson et al. We are only able to loosely constrain the angle for HAT-P-27/WASP-40 (Teff = 5190+160– 170 K) to λ = 24.°2 + 76.0 – 44.5, owing to the poor signal-to-noise ratio of our data. We consider this result a non-detection under a slightly updated version of the alignment test of Brown et al. We place our results in the context of the full sample of spin-orbit alignment measurements, finding that they provide further support for previously established trends. [ABSTRACT FROM AUTHOR]