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Larger and faster: revised properties and a shorter orbital period for the WASP-57 planetary system from a pro-am collaboration

Southworth, John; Mancini, L.; Tregloan-Reed, J.; Calchi Novati, S.; Ciceri, S.; D'Ago, G.; Delrez, L.; Dominik, M.; Evans, D.F.; Gillon, M.; Jehin, E.; Jørgensen, U.G.; Haugbølle, T.; Lendl, M.; Arena, C.; Barbieri, L.; Barbieri, M.; Corfini, G.; Lopresti, C.; Marchini, A.; Marino, G.; Alsubai, K.A.; Bozza, V.; Bramich, D.M.; Figuera Jaimes, R.; Hinse, T.C.; Th. Henning; Hundertmark, M.; Juncher, D.; Korhonen, H.; Popovas, A.; Rabus, M.; Rahvar, S.; Schmidt, R.W.; Skottfelt, J.; Snodgrass, C.; Starkey, D.; Surdej, J.; Wertz, O.

Larger and faster: revised properties and a shorter orbital period for the WASP-57 planetary system from a pro-am collaboration Thumbnail


Authors

L. Mancini

J. Tregloan-Reed

S. Calchi Novati

S. Ciceri

G. D'Ago

L. Delrez

M. Dominik

D.F. Evans

M. Gillon

E. Jehin

U.G. Jørgensen

T. Haugbølle

M. Lendl

C. Arena

L. Barbieri

M. Barbieri

G. Corfini

C. Lopresti

A. Marchini

G. Marino

K.A. Alsubai

V. Bozza

D.M. Bramich

R. Figuera Jaimes

T.C. Hinse

Th. Henning

M. Hundertmark

D. Juncher

H. Korhonen

A. Popovas

M. Rabus

S. Rahvar

R.W. Schmidt

J. Skottfelt

C. Snodgrass

D. Starkey

J. Surdej

O. Wertz



Abstract

Transits in the WASP-57 planetary system have been found to occur half an hour earlier than expected. We present 10 transit light curves from amateur telescopes, on which this discovery was based, 13 transit light curves from professional facilities which confirm and refine this finding, and high-resolution imaging which show no evidence for nearby companions. We use these data to determine a new and precise orbital ephemeris, and measure the physical properties of the system. Our revised orbital period is 4.5 s shorter than found from the discovery data alone, which explains the early occurrence of the transits. We also find both the star and planet to be larger and less massive than previously thought. The measured mass and radius of the planet are now consistent with theoretical models of gas giants containing no heavy-element core, as expected for the subsolar metallicity of the host star. Two transits were observed simultaneously in four passbands. We use the resulting light curves to measure the planet’s radius as a function of wavelength, finding that our data are sufficient in principle but not in practise to constrain its atmospheric properties. We conclude with a discussion of the current and future status of transmission photometry studies for probing the atmospheres of gas-giant transiting planets.

Journal Article Type Article
Acceptance Date Sep 18, 2015
Online Publication Date Oct 16, 2015
Publication Date Dec 11, 2015
Publicly Available Date Mar 28, 2024
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 454
Issue 3
Pages 3094 -3107
DOI https://doi.org/10.1093/mnras/stv2183
Keywords astrophysics, stars, fundamental parameters, individual, WASP-57, planetary systems
Publisher URL http://dx.doi.org/10.1093/mnras/stv2183

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