The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica
The ASTEP (Antarctica Search for Transiting ExoPlanets) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted...
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ftdatacite:10.48550/arxiv.1303.0973 2023-05-15T13:33:36+02:00 The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica Abe, L. Gonçalves, I. Agabi, A. Alapini, A. Guillot, T. Mékarnia, D. Rivet, J. -P. Schmider, F. -X. Crouzet, N. Fortney, J. Pont, F. Barbieri, M. Daban, J. -B. Fanteï-Caujolle, Y. Gouvret, C. Bresson, Y. Roussel, A. Bonhomme, S. Robini, A. Dugué, M. Bondoux, E. Péron, S. Petit, P. -Y. Szulágyi, J. Fruth, T. Erikson, A. Rauer, H. Fressin, F. Valbousquet, F. Blanc, P. -E. van Suu, A. Le Aigrain, S. 2013 https://dx.doi.org/10.48550/arxiv.1303.0973 https://arxiv.org/abs/1303.0973 unknown arXiv https://dx.doi.org/10.1051/0004-6361/201220351 arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences article-journal Article ScholarlyArticle Text 2013 ftdatacite https://doi.org/10.48550/arxiv.1303.0973 https://doi.org/10.1051/0004-6361/201220351 2022-04-01T13:23:02Z The ASTEP (Antarctica Search for Transiting ExoPlanets) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. The WASP-19 system was observed during 24 nights in May 2010. The photometric variability level due to starspots is about 1.8% (peak-to-peak), in line with the SuperWASP data from 2007 (1.4%) and larger than in 2008 (0.07%). We find a rotation period of WASP-19 of 10.7 +/- 0.5 days, in agreement with the SuperWASP determination of 10.5 +/- 0.2 days. Theoretical models show that this can only be explained if tidal dissipation in the star is weak, i.e. the tidal dissipation factor Q'star > 3.10^7. Separately, we find evidence for a secondary eclipse of depth 390 +/- 190 ppm with a 2.0 sigma significance, a phase consistent with a circular orbit and a 3% false positive probability. Given the wavelength range of the observations (420 to 950 nm), the secondary transit depth translates into a day side brightness temperature of 2690(-220/+150) K, in line with measurements in the z' and K bands. The day side emission observed in the visible could be due either to thermal emission of an extremely hot day side with very little redistribution of heat to the night side, or to direct reflection of stellar light with a maximum geometrical albedo Ag=0.27 +/- 0.13. We also report a low-frequency oscillation well in phase at the planet orbital period, but with a lower-limit amplitude that could not be attributed to the planet phase alone, and possibly contaminated with residual lightcurve trends. : Accepted for publication in Astronomy and Astrophysics, 13 pages, 13 figures Text Antarc* Antarctica DataCite Metadata Store (German National Library of Science and Technology) Austral |
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Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences |
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Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences Abe, L. Gonçalves, I. Agabi, A. Alapini, A. Guillot, T. Mékarnia, D. Rivet, J. -P. Schmider, F. -X. Crouzet, N. Fortney, J. Pont, F. Barbieri, M. Daban, J. -B. Fanteï-Caujolle, Y. Gouvret, C. Bresson, Y. Roussel, A. Bonhomme, S. Robini, A. Dugué, M. Bondoux, E. Péron, S. Petit, P. -Y. Szulágyi, J. Fruth, T. Erikson, A. Rauer, H. Fressin, F. Valbousquet, F. Blanc, P. -E. van Suu, A. Le Aigrain, S. The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica |
topic_facet |
Earth and Planetary Astrophysics astro-ph.EP FOS Physical sciences |
description |
The ASTEP (Antarctica Search for Transiting ExoPlanets) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. The WASP-19 system was observed during 24 nights in May 2010. The photometric variability level due to starspots is about 1.8% (peak-to-peak), in line with the SuperWASP data from 2007 (1.4%) and larger than in 2008 (0.07%). We find a rotation period of WASP-19 of 10.7 +/- 0.5 days, in agreement with the SuperWASP determination of 10.5 +/- 0.2 days. Theoretical models show that this can only be explained if tidal dissipation in the star is weak, i.e. the tidal dissipation factor Q'star > 3.10^7. Separately, we find evidence for a secondary eclipse of depth 390 +/- 190 ppm with a 2.0 sigma significance, a phase consistent with a circular orbit and a 3% false positive probability. Given the wavelength range of the observations (420 to 950 nm), the secondary transit depth translates into a day side brightness temperature of 2690(-220/+150) K, in line with measurements in the z' and K bands. The day side emission observed in the visible could be due either to thermal emission of an extremely hot day side with very little redistribution of heat to the night side, or to direct reflection of stellar light with a maximum geometrical albedo Ag=0.27 +/- 0.13. We also report a low-frequency oscillation well in phase at the planet orbital period, but with a lower-limit amplitude that could not be attributed to the planet phase alone, and possibly contaminated with residual lightcurve trends. : Accepted for publication in Astronomy and Astrophysics, 13 pages, 13 figures |
format |
Text |
author |
Abe, L. Gonçalves, I. Agabi, A. Alapini, A. Guillot, T. Mékarnia, D. Rivet, J. -P. Schmider, F. -X. Crouzet, N. Fortney, J. Pont, F. Barbieri, M. Daban, J. -B. Fanteï-Caujolle, Y. Gouvret, C. Bresson, Y. Roussel, A. Bonhomme, S. Robini, A. Dugué, M. Bondoux, E. Péron, S. Petit, P. -Y. Szulágyi, J. Fruth, T. Erikson, A. Rauer, H. Fressin, F. Valbousquet, F. Blanc, P. -E. van Suu, A. Le Aigrain, S. |
author_facet |
Abe, L. Gonçalves, I. Agabi, A. Alapini, A. Guillot, T. Mékarnia, D. Rivet, J. -P. Schmider, F. -X. Crouzet, N. Fortney, J. Pont, F. Barbieri, M. Daban, J. -B. Fanteï-Caujolle, Y. Gouvret, C. Bresson, Y. Roussel, A. Bonhomme, S. Robini, A. Dugué, M. Bondoux, E. Péron, S. Petit, P. -Y. Szulágyi, J. Fruth, T. Erikson, A. Rauer, H. Fressin, F. Valbousquet, F. Blanc, P. -E. van Suu, A. Le Aigrain, S. |
author_sort |
Abe, L. |
title |
The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica |
title_short |
The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica |
title_full |
The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica |
title_fullStr |
The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica |
title_full_unstemmed |
The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica |
title_sort |
secondary eclipses of wasp-19b as seen by the astep 400 telescope from antarctica |
publisher |
arXiv |
publishDate |
2013 |
url |
https://dx.doi.org/10.48550/arxiv.1303.0973 https://arxiv.org/abs/1303.0973 |
geographic |
Austral |
geographic_facet |
Austral |
genre |
Antarc* Antarctica |
genre_facet |
Antarc* Antarctica |
op_relation |
https://dx.doi.org/10.1051/0004-6361/201220351 |
op_rights |
arXiv.org perpetual, non-exclusive license http://arxiv.org/licenses/nonexclusive-distrib/1.0/ |
op_doi |
https://doi.org/10.48550/arxiv.1303.0973 https://doi.org/10.1051/0004-6361/201220351 |
_version_ |
1766043597491142656 |