Transit timing analysis in the HAT-P-32 system

Seeliger, Martin; Dimitrov, D.; Kjurkchieva, D.; Mallonn, M.; Fernández, M.; Kitze, M.; Casanova, V.; Maciejewski, G.; Ohlert, J.; Schmidt, J.; Pannicke, A.; Puchalski, D.; Göǧüş, E.; Güver, T.; Bilir, S.; Ak, T.; Hohle, M. M.; Schmidt, T. O. B.; Errmann, R.; Jensen, Eric L. N.; Cohen, David H.; Marschall, Laurence A.; Saral, G.; Bernt, I.; Derman, E.; Gałan, C.; Neuhäuser, R.

doi:10.1093/mnras/stu567

Cited by 47 publications

(38 citation statements)

References 42 publications

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“…We find our results for the planet parameters to be consistent with the literature values. The difference in radius ratio compared to the results of Hartman et al (2011) and Seeliger et al (2014) might be explained by the different wavelength region probed in this study but is more likely caused by the transit depth dilution from additional flux of the M-dwarf companion HAT-P-32B, which was not accounted for in these two studies. A rough dilution correction of the given radius ratios using…”

Section: Results and Discussion Of The White Light Curvescontrasting

confidence: 71%

“…Not fixing the values but letting them vary in their uncertainty intervals did not change our final results for the relative wavelength-dependent change in radius ratio, but did only offset the exact value around which the narrow band radius ratios and limb darkening coefficients varied. The same held true when we fixed the wavelengthindependent and white light transit parameters to the literature values provided by Gibson et al (2013b), Hartman et al (2011) or Seeliger et al (2014. Between these tested configurations adopting our best fit Run 1 white light parameters did yield the lowest overall χ 2 .…”

Section: Analysis Of the Color Light Curves Of Runmentioning

confidence: 53%

“…The red noise factor used to inflate the error bars of our results is β = 1.345. For comparison the planet parameters obtained from three recent works (Hartman et al 2011) (e ≡ 0), (Gibson et al 2013b) and (Seeliger et al 2014) are listed. (a) Value derived from the ephemeris information given in respective papers.…”

Section: Parametermentioning

confidence: 99%

“…They found a long trend signal for HAT-P-32A pointing to the existence of yet another body in the system. A transit timing variation (TTV) study of 45 transit events by Seeliger et al (2014) looking for evidence of an additional body found no evidence for variations larger than 1.5 min. Gibson et al (2013b) obtained a ground-based optical transmission spectrum of HAT-P-32Ab using Gemini North/GMOS.…”

Section: Introductionmentioning

confidence: 99%

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The GTC exoplanet transit spectroscopy survey

Nortmann

Pallé

Murgas

et al. 2016

A&A

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We observed the hot Jupiter HAT-P-32b (also known as HAT-P-32Ab) to determine its optical transmission spectrum by measuring the wavelength-dependent planet-to-star radius ratios in the region between 518 -918 nm. We used the OSIRIS instrument at the GTC in long slit spectroscopy mode, placing HAT-P-32 and a reference star in the same slit and obtaining a time series of spectra covering two transit events. Using the best quality data set, we were able to yield 20 narrow-band transit light curves, with each passband spanning a 20 nm wide interval. After removal of all systematic noise signals and light curve modeling the uncertainties for the resulting radius ratios lie between 337 and 972 ppm. The radius ratios show little variation with wavelength suggesting a high altitude cloud layer masking any atmospheric features. Alternatively, a strong depletion in alkali metals or a much smaller than expected planetary atmospheric scale height could be responsible for the lack of atmospheric features. Our result of a flat transmission spectrum is consistent with a previous ground-based study of the optical spectrum of this planet. This agreement between independent results demonstrates that ground-based measurements of exoplanet atmospheres can give reliable and reproducible results despite the fact that the data often is heavily affected by systematic noise, as long as the noise source is well understood and properly corrected. We also extract an optical spectrum of the M-dwarf companion HAT-P-32B. Using PHOENIX stellar atmosphere models we determine an effective temperature of T eff = 3187 +60 −71 K, slightly colder than previous studies relying only on broadband infra-red data.

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Section: Results and Discussion Of The White Light Curvescontrasting

confidence: 71%

Section: Analysis Of the Color Light Curves Of Runmentioning

confidence: 53%

Section: Parametermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The GTC exoplanet transit spectroscopy survey

Nortmann

Pallé

Murgas

et al. 2016

A&A

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“…After the discovery of a group of inflated planets (e.g. WASP-17b, TrES-4b and HAT-P-32, Anderson et al 2011;Sozzetti et al 2015;Seeliger et al 2014), several theories invoking tidal friction, enhanced atmospheric opacities, turbulent mixing, ohmic dissipation, windshocks, or more exotic mechanisms have been proposed to account for the slow cooling rate of these planets, resulting in an unexpectedly large radius (see e.g. Baraffe et al 2014;Spiegel & Burrows 2013;Ginzburg & Sari 2015, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry

Ciceri

Mancini

Southworth

et al. 2015

A&A

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Context. Accurate and repeated photometric follow-up observations of planetary transit events are important to precisely characterize the physical properties of exoplanets. A good knowledge of the main characteristics of the exoplanets is fundamental in order to trace their origin and evolution. Multi-band photometric observations play an important role in this process. Aims. By using new photometric data, we computed precise estimates of the physical properties of two transiting planetary systems at equilibrium temperatures of ∼2000 K. Methods. We present new broadband, multi-colour photometric observations obtained using three small class telescopes and the telescope-defocussing technique. In particular we obtained 11 and 10 light curves covering 8 and 7 transits of HAT-P-23 and WASP-48, respectively. For each of the two targets, one transit event was simultaneously observed through four optical filters. One transit of WASP-48 b was monitored with two telescopes from the same observatory. The physical parameters of the systems were obtained by fitting the transit light curves with jktebop and from published spectroscopic measurements.Results. We have revised the physical parameters of the two planetary systems, finding a smaller radius for both HAT-P-23 b and WASP-48 b, R b = 1.224 ± 0.037 R Jup and R b = 1.396 ± 0.051 R Jup , respectively, than those measured in the discovery papers (R b = 1.368 ± 0.090 R Jup and R b = 1.67 ± 0.10 R Jup ). The density of the two planets are higher than those previously published (ρ b ∼ 1.1 and ∼0.3 ρ jup for HAT-P-23 and WASP-48, respectively) hence the two hot Jupiters are no longer located in a parameter space region of highly inflated planets. An analysis of the variation of the planet's measured radius as a function of optical wavelength reveals flat transmission spectra within the experimental uncertainties. We also confirm the presence of the eclipsing contact binary NSVS-3071474 in the same field of view of WASP-48, for which we refine the value of the period to be 0.459 d.

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Near‐ultraviolet transit photometry of HAT‐P‐32 b with the Large Binocular Telescope: Silicate aerosols in the planetary atmosphere

Mallonn

Wakeford

2017

Astron Nachr

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Broad-band exoplanet transit photometry can characterize the planetary atmosphere when observed at multiple selected filters. This observing technique can reveal gradients in the spectra of extrasolar planets, for example, the slope of decreasing opacity from short to long optical wavelengths caused by aerosol scattering. In this work, we observed a transit of the hot Jupiter HAT-P-32 b in the shortest wavelength possible from the ground using the Large Binocular Telescope (LBT). The data comprise the best quality ground-based U-band measurement taken so far of an exoplanet transit. Compared to broad-band observations of intermediate and long optical wavelengths published previously, a clear scattering slope in the planetary transmission spectrum is revealed. Most likely, the scattering particles are magnesium silicate aerosols larger than 0.1 μm. We define a spectral index to compare this scattering feature of HAT-P-32 b with published results of other exoplanets. It turns out to be very typical in amplitude within the compared sample. Furthermore, we searched for correlation in this sample of the spectral index with planetary equilibrium temperature, surface acceleration, and stellar activity indicator, but could not find any.

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Transit timing analysis in the HAT-P-32 system

Cited by 47 publications

References 42 publications

The GTC exoplanet transit spectroscopy survey

The GTC exoplanet transit spectroscopy survey

Physical properties of the HAT-P-23 and WASP-48 planetary systems from multi-colour photometry

Near‐ultraviolet transit photometry of HAT‐P‐32 b with the Large Binocular Telescope: Silicate aerosols in the planetary atmosphere

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