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 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:
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RA (2000) DE Designation(s)
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23 13 58.76 +08 45 40.6 WASP-52 = WASP-52
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File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
list.dat 50 12 Details of the transit observations presented
in this work
phot/* . 12 Individual transit files
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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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" Obs.date Observation date
48- 50 I3 --- Nobs Number of observations
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Byte-by-byte Description of file: phot/*
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Bytes Format Units Label Explanations
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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
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Acknowledgements:
Luigi Mancini, lmancini(at)roma2.infn.it, University of Rome Tor Vergata
(End) Luigi Mancini [Rome univ. Italy], Patricia Vannier [CDS] 26-Mar-2018