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J/MNRAS/465/843     Light curves of WASP-52                  (Mancini+, 2017)

Orbital alignment and star-spot properties in the WASP-52 planetary system. Mancini L., Southworth J., Raia G., Tregloan-Reed J., Molliere P., Bozza V., Bretton M., Bruni I., Ciceri S., D'Ago G., Dominik M., Hinse T.C., Hundertmark M., Jorgensen U.G., Korhonen H., Rabus M., Rahvar S., Starkey D., Calchi Novati S., Figuera Jaimes R., Henning T., Juncher D., Haugbolle T., Kains N., Popovas A., Schmidt R.W., Skottfelt J., Snodgrass C., Surdej J., Wertz O. <Mon. Not. R. Astron. Soc., 465, 843-857 (2017)> =2017MNRAS.465..843M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Exoplanets ; Photometry Keywords: techniques: photometric - stars: fundamental parameters - stars: individual: WASP-52 - planetary systems Abstract: We report 13 high-precision light curves of eight transits of the exoplanet WASP-52 b, obtained by using four medium-class telescopes, through different filters, and adopting the defocussing technique. One transit was recorded simultaneously from two different observatories and another one from the same site but with two different instruments, including a multiband camera. Anomalies were clearly detected in five light curves and modelled as star-spots occulted by the planet during the transit events. We fitted the clean light curves with the JKTEBOP code, and those with the anomalies with the PRISM+gemc codes in order to simultaneously model the photometric parameters of the transits and the position, size and contrast of each star-spot. We used these new light curves and some from the literature to revise the physical properties of the WASP-52 system. Star-spots with similar characteristics were detected in four transits over a period of 43 d. In the hypothesis that we are dealing with the same star-spot, periodically occulted by the transiting planet, we estimated the projected orbital obliquity of WASP-52 b to be λ=3.8±8.4°. We also determined the true orbital obliquity, ψ=20±50°, which is, although very uncertain, the first measurement of ψ purely from star-spot crossings. We finally assembled an optical transmission spectrum of the planet and searched for variations of its radius as a function of wavelength. Our analysis suggests a flat transmission spectrum within the experimental uncertainties. Description: Light curves of transit events of the extrasolar planet WASP-52b. One of the datasets was obtained using the Cassini 1.52m Telescope (Gunn r) at the Astronomical Observatory of Bologna in Loiano (Italy). Three of the datasets were obtained using the Zeiss 1.23m telescope (Cousins R and Cousins I) at the German-Spanish Astronomical Centre at Calar Alto (Spain). Four of the datasets were obtained using the MPG 2.2m telescope (Sloan g, Sloan r, Sloan i, Sloan z) at the ESO Observatory in La Silla (Chile). Four of the datasets were obtained using the 1.54m Danish Telescope at the ESO Observatory in La Silla (Chile). Objects: ---------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------- 23 13 58.76 +08 45 40.6 WASP-52 = WASP-52 ---------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 50 12 Details of the transit observations presented in this work phot/* 37 12 Individual transit files
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 11 A11 --- FileName Name of the table with photometry in subdirectory phot 13- 25 A13 --- Tel Telescope 27- 35 A9 --- Filt Filter 37- 46 A10 "date" Observation date 48- 50 I3 --- Nobs Number of observations
Byte-by-byte Description of file: phot/*
Bytes Format Units Label Explanations
1- 12 F12.6 d BJD Barycentric JD for the midpoint of observation (TDB) (BJD-2400000) 17- 25 F9.6 mag mag Differential magnitude of the target 30- 37 F8.6 mag e_mag Measurement error of the magnitude
Acknowledgements: Luigi Mancini, lmancini(at), University of Rome Tor Vergata
(End) Luigi Mancini [Rome univ. Italy], Patricia Vannier [CDS] 26-Mar-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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