Transit Analysis Package: An IDL Graphical User Interface for Exoplanet Transit Photometry

Gazak, J. Zachary; Johnson, John Asher; Tonry, J.; Dragomir, Diana; Eastman, Jason D.; Mann, Andrew W.; Agol, Eric

doi:10.1155/2012/697967

Cited by 141 publications

(117 citation statements)

References 32 publications

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“…The Transit Analysis Package (Gazak et al 2012) was employed to determine mid-transit times and their uncertainties for individual epochs. The transit parameters such as the orbital inclination, scaled semi-major axis, ratio of planetary to stellar radii, and coefficients of the quadratic limb-darkening (LD) law for R-band data were taken from Maciejewski et al (2013).…”

Section: Observations and Data Processingmentioning

confidence: 99%

Departure from the constant-period ephemeris for the transiting exoplanet WASP-12 b

Maciejewski

Dimitrov

Fernández

et al. 2016

A&A

131

148

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Aims. Most hot Jupiters are expected to spiral in toward their host stars because the angular momentum of the orbital motion is transferred to the stellar spin. Their orbits can also precess as a result of planet-star interactions. Calculations show that both effects might be detected for the very-hot exoplanet WASP-12 b using the method of precise transit-timing over a time span of about 10 yr. Methods. We acquired new precise light curves for 29 transits of WASP-12 b, spannning four observing seasons from November 2012 to February 2016. New mid-transit times, together with those from the literature, were used to refine the transit ephemeris and analyze the timing residuals. Results. We find that the transit times of WASP-12 b do not follow a linear ephemeris with a 5σ confidence level. They may be approximated with a quadratic ephemeris that gives a change rate in the orbital period of (−2.56 ± 0.40) × 10 −2 s yr −1 . The tidal quality parameter of the host star was found to be equal to 2.5 × 10 5 , which is similar to theoretical predictions for Sun-like stars. We also considered a model in which the observed timing residuals are interpreted as a result of the apsidal precession. We find, however, that this model is statistically less probable than the orbital decay.

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Section: Observations and Data Processingmentioning

confidence: 99%

Departure from the constant-period ephemeris for the transiting exoplanet WASP-12 b

Maciejewski

Dimitrov

Fernández

et al. 2016

A&A

131

148

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“…The common-mode systematics S w were derived after dividing the white-color light curve by the best-fitting transit model T (p). The transit analysis package (TAP; Gazak et al 2012), which is customized for our purposes, was employed to perform the Markov chain Monte Carlo analysis. The correlated noise was taken into account by the wavelet-based likelihood function proposed by Carter & Winn (2009).…”

Section: Light-curve Analysismentioning

confidence: 99%

Feature-rich transmission spectrum for WASP-127b

Πάλλη

Chen

Nowak

et al. 2017

A&A

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Context. WASP-127b is a planet with one of the lowest densities discovered to date. With a sub-Saturn mass (M p = 0.18 ± 0.02 M J ) and super-Jupiter radius (R p = 1.37 ± 0.04 R J ), it orbits a bright G5 star that is about to leave the main-sequence. Aims. We aim to explore the atmosphere of WASP-127b in order to retrieve its main atmospheric components, and to find hints for its intriguing inflation and evolutionary history. Methods. We used the ALFOSC spectrograph at the NOT telescope to observe a low-resolution (R ∼ 330, seeing limited) long-slit spectroscopic time series during a planetary transit, and present here the first transmission spectrum for WASP-127b. Results. We find a strong Rayleigh slope at blue wavelengths and a hint of Na absorption, although the quality of the data does not allow us to claim a detection. At redder wavelengths the absorption features of TiO and VO are the best explanation to fit the data. Conclusions. Although observations with a higher signal-to-noise ratio are needed to conclusively confirm the absorption features, WASP-127b seems to posses a cloud-free atmosphere and is one of the best targets on which to perform further characterization studies in the near future.

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“…Using artificial data, we perform several different comparison tests of EXOMOP with two different publicly available modelling software packages: the Transit Analysis Package 6 (TAP; Mandel & Agol 2002;Carter & Winn 2009;Gazak et al 2012;Eastman et al 2013) and JKTEBOP 7 (Southworth et al 2004a,b). We also test if the errors we calculate using EXOMOP are reliable by comparing the errors to analytic estimates.…”

Section: Exomop Model Comparisonmentioning

confidence: 99%

Ground-based near-UV observations of 15 transiting exoplanets: constraints on their atmospheres and no evidence for asymmetrical transits

Turner

Pearson

Biddle

et al. 2016

Mon. Not. R. Astron. Soc.

101

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Transits of exoplanets observed in the near-UV have been used to study the scattering properties of their atmospheres and possible star-planet interactions. We observed the primary transits of 15 exoplanets (CoRoT-1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-16b, HAT-P-22b, TrES2b, in the near-UV and several optical photometric bands to update their planetary parameters, ephemerides, search for a wavelength dependence in their transit depths to constrain their atmospheres, and determine if asymmetries are visible in their light curves. Here, we present the first ground-based near-UV light curves for 12 of the targets (CoRoT1b, GJ436b, HAT-P-1b, HAT-P-13b, HAT-P-22b, TrES-2b, TrES-4b, WASP-1b, WASP-33b, WASP-36b, WASP-48b, and WASP-77Ab). We find that none of the near-UV transits exhibit any non-spherical asymmetries, this result is consistent with recent theoretical predictions by Ben-Jaffel et al. and Turner et al. The multiwavelength photometry indicates a constant transit depth from near-UV to optical wavelengths in 10 targets (suggestive of clouds), and a varying transit depth with wavelength in 5 targets (hinting at Rayleigh or aerosol scattering in their atmospheres). We also present the first detection of a smaller near-UV transit depth than that measured in the optical in WASP-1b and a possible opacity source that can cause such radius variations is currently unknown. WASP-36b also exhibits a smaller near-UV transit depth at

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Transit Analysis Package: An IDL Graphical User Interface for Exoplanet Transit Photometry

Cited by 141 publications

References 32 publications

Departure from the constant-period ephemeris for the transiting exoplanet WASP-12 b

Departure from the constant-period ephemeris for the transiting exoplanet WASP-12 b

Feature-rich transmission spectrum for WASP-127b

Ground-based near-UV observations of 15 transiting exoplanets: constraints on their atmospheres and no evidence for asymmetrical transits

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