THE SUB-SATURN MASS TRANSITING PLANET HAT-P-12b

Lee, Jae Woo; Youn, Jae-Hyuck; Lee, Chung-Uk; Hinse, T. C.

doi:10.1088/0004-6256/143/4/95

Cited by 28 publications

(32 citation statements)

References 30 publications

(33 reference statements)

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“…For the Hartman et al (2009) light curves, we achieve excellent agreement in the parameters, but find error bars that are higher by up to a factor of 2. The Lee et al (2012) results, which were also derived with JKTEBOP, are reproduced as well, however our error estimation yields values higher by a factor of 2 for the planet-to-star radius ratio and 10 for the orbital inclination. The source of this discrepancy remains unexplained.…”

Section: Re-analysis Of the Literature Datasupporting

confidence: 69%

“…There are also a handful of examples of candidates or confirmed multiplanet systems with a hot Jupiter, where indications or evidence of another companion was achieved with the radial velocity method, see Hartman et al (2014) and references therein. Lee et al (2012) found variations in the transit times of HAT-P-12b that are significantly larger than their error values. We use our sample of transit observations to follow up on this potential TTV detection.…”

Section: Introductionmentioning

confidence: 64%

“…The source of this discrepancy remains unexplained. The J-band light curve from Sada et al (2012) shows rather complex Lee et al (2012) deviations from the symmetric transit shape and was originally detrended by a fifth-order polynomial over time fitted to the outof-transit data. The uncertainty of this polynomial was not included in the transit parameter error estimation.…”

Section: Re-analysis Of the Literature Datamentioning

confidence: 99%

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Broad-band spectrophotometry of the hot Jupiter HAT-P-12b from the near-UV to the near-IR

Mallonn

Nascimbeni

Weingrill

et al. 2015

A&A

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Context. The detection of trends or gradients in the transmission spectrum of extrasolar planets is possible with observations at very low spectral resolution. Transit measurements of sufficient accuracy using selected broad-band filters allow for an initial characterization of the atmosphere of the planet. Aims. We want to investigate the atmosphere of the hot Jupiter HAT-P-12b for an increased absorption at the very blue wavelength regions caused by scattering. Furthermore, we aim for a refinement of the transit parameters and the orbital ephemeris. Methods. We obtained time series photometry of 20 transit events and analyzed them homogeneously, along with eight light curves obtained from the literature. In total, the light curves span a range from 0.35 to 1.25 microns. During two observing seasons over four months each, we monitored the host star to constrain the potential influence of starspots on the derived transit parameters. Results. We rule out the presence of a Rayleigh slope extending over the entire optical wavelength range, a flat spectrum is favored for HAT-P-12b with respect to a cloud-free atmosphere model spectrum. A potential cause of such gray absorption is the presence of a cloud layer at the probed latitudes. Furthermore, in this work we refine the transit parameters, the ephemeris and perform a TTV analysis in which we found no indication for an unseen companion. The host star showed a mild non-periodic variability of up to 1%. However, no stellar rotation period could be detected to high confidence.

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Section: Re-analysis Of the Literature Datasupporting

confidence: 69%

Section: Introductionmentioning

confidence: 64%

Section: Re-analysis Of the Literature Datamentioning

confidence: 99%

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Broad-band spectrophotometry of the hot Jupiter HAT-P-12b from the near-UV to the near-IR

Mallonn

Nascimbeni

Weingrill

et al. 2015

A&A

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“…A summary of the observations is listed in Table 1, where we present observing interval, numbers of nights, CCD type, field of view (FOV), and numbers of observed points. The instruments and reduction methods for the FLI IMG4301E and ARC 4K CCD cameras are the same as those described by Lee et al (2009bLee et al ( , 2012b. In order to make an optimal artificial comparison source during our observing runs, we monitored a few tens of stars imaged on the chip at the same time as the eclipsing pair.…”

Section: New Long-term Observations and Eclipse Timesmentioning

confidence: 99%

The pulsating sdB+M eclipsing system NY Virginis and its circumbinary planets

Lee¹,

Hinse²,

Youn³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We searched for circumbinary planets orbiting NY Vir in historical eclipse times including our long-term CCD data. Sixty-eight times of minimum light with accuracies better than 10 s were used for the ephemeris computations. The best fit to those timings indicated that the orbital period of NY Vir has varied due to a combination of two sinusoids with periods of P 3 =8.2 yr and P 4 =27.0 yr and semi-amplitudes of K 3 =6.9 s and K 4 =27.3 s, respectively. The periodic variations most likely arise from a pair of light-time effects due to the presence of third and fourth bodies that are gravitationally bound to the eclipsing pair. We have derived the orbital parameters and the minimum masses, M 3 sin i 3 = 2.8 M Jup and M 4 sin i 4 = 4.5 M Jup , of both objects. A dynamical analysis suggests that the outer companion is less likely to orbit the binary on a circular orbit. Instead we show that future timing data might push its eccentricity to moderate values for which the system exhibits long-term stability. The results demonstrate that NY Vir is probably a star-planet system, which consists of a very close binary star and two giant planets. The period ratio P 3 /P 4 suggests that a long-term gravitational interaction between them would result in capture into a nearly 3:10 mean motion resonance. When the presence of the circumbinary planets is verified and understood more comprehensively, the formation and evolution of this planetary system should be advanced greatly.

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“…The observations will also be focused to check possible out-ofeclipse and color brightness variations which would indi- www.an-journal.org Lee et al (2012).…”

Section: Observing Network and First Observationsmentioning

confidence: 99%