A revised orbital ephemeris for HAT-P-9b

Dittmann, Jason; Close, Laird M.; Scuderi, Louis J.; Turner, Jake D.; Stephenson, P. C.

doi:10.1016/j.newast.2011.10.003

Cited by 36 publications

(16 citation statements)

References 22 publications

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“…The data points of all our transits are available in electronic form (see Table 3). For all the transits, the OoT baselines have a photometric root mean squared (rms) value between 1.23 and 6.22 mmag, consistent with previous high S/N transit photometry using the Mont4k on the 1.55-m Kuiper telescope (Dittmann et al 2009b(Dittmann et al , 2012Scuderi et al 2010;Teske et al 2013;Turner et al 2013;Pearson et al 2014;Zellem et al 2015). …”

Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nsupporting

confidence: 86%

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.

109

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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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Section: O B S E Rvat I O N S a N D Data R E D U C T I O Nsupporting

confidence: 86%

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.

109

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“…The seeing ranged from 1.46 00 to 3.19 00 throughout our observation. The Out-of-Transit (OoT) baseline in our transit achieved a photometric root-mean-squared (RMS) value of 2.27 millimagnitude (mmag), which is a typical value for high signal-to-noise (S/N) transit photometry on the 1.55-m Kuiper telescope (Dittmann et al, , 2012Scuderi et al, 2010;Teske et al, 2013). Our observation is summarized in Table 2.…”

Section: Observations and Data Reductionmentioning

confidence: 78%

Photometric observation of HAT-P-16b in the near-UV

2014

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We present the first primary transit light curve of the hot Jupiter HAT-P-16b in the near-UV photometric band. We observed this object on December 29,2012 in order to update the transit ephemeris, constrain its planetary parameters and search for magnetic field interference. Vidotto et al. (2011a) postulate that the magnetic field of HAT-P-16b can be constrained if its near-UV light curve shows an early ingress compared to its optical light curve, while its egress remains unchanged. However, we did not detect an early ingress in our night of observing when using a cadence of 60 seconds and an average photometric precision of 2.26mmag. We find a near-UV planetary radius of Rp=1.274+-0.057RJup which is consistent with its near-IR radius of Rp=1.289+-0.066RJup (Buchhave et al., 2010). We developed an automated reduction pipeline and modeling package to process our data. The data reduction package synthesizes a set of IRAF scripts to calibrate images and perform aperture photometry. The modeling package utilizes the Levenberg-Marquardt minimization algorithm to find a least-squares best fit and a differential evolution Markov Chain Monte Carlo algorithm to find the best fit to the light curve. To constrain the red noise in both fitting models we use the residual permutation (rosary bead) method and time-averaging method.Comment: 9 pages, 3 figures, New Data Reduction Program and Modeling Package. arXiv admin note: text overlap with arXiv:1211.489

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“…The orbital ephemeris in the discovery work was obtained based on four light curves within a time span of only two months (Shporer et al 2009a). Dittmann et al (2012) then derived a new ephemeris with two more observations, extending the time span to two years. In this work, we have added another six light curves, greatly augmenting the time span to a total of eight years.…”

Section: Hat-p-9bmentioning

confidence: 99%

Transiting Exoplanet Monitoring Project (TEMP). V. Transit Follow Up for HAT-P-9b, HAT-P-32b, and HAT-P-36b

Wang

Hinse

et al. 2019

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During the past five years, 6, 7, and 26 transit observations were carried out for the HAT-P-9b, HAT-P-32b, and HAT-P-36b systems, respectively, through the Transiting Exoplanet Monitoring Project network. Combined with the published photometric data and radial-velocity measurements, our new photometry allows us to revisit the system parameters and search for additional close-in planetary companions in these hot Jupiter systems. We measure an updated R P /R * = 0.1260 ± 0.0011 for HAT-P-36 system in the R band, which is 4.5σ larger than the published i-band radius ratio of 0.1186 ± 0.0012. We also perform a transit timing variation (TTV) analysis for each system. Because no significant TTVs were found, we place an upper mass limit on an additional planet for each system.

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A revised orbital ephemeris for HAT-P-9b

Abstract: We present here three transit observations of HAT-P-9b taken on

Cited by 36 publications

References 22 publications

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

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

Photometric observation of HAT-P-16b in the near-UV

Transiting Exoplanet Monitoring Project (TEMP). V. Transit Follow Up for HAT-P-9b, HAT-P-32b, and HAT-P-36b

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