Enviar artigo por via de e-mail Exoplanet Studies. Photometric Analysis of the Transmission Spectra of Selected Exoplanets
- Autores: Valyavin G.G.1, Gadelshin D.R.1, Valeev A.F.1, Burlakova T.E.1, Antonyuk K.A.2, Galazutdinov G.A.1,3,4, Pit N.V.2, Moskvitin A.S.1, Sokov E.N.1,4, Sokova I.A.4, Lee B.5, Han I.5, Lendl M.6, Fossati L.6, Grauzhanina A.O.1, Fatkhullin T.A.1
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Afiliações:
- Special Astrophysical Observatory
- Crimean Astrophysical Observatory
- Instituto de Astronomia
- Main (Pulkovo) Observatory
- Korea Astronomy and Space Science Institute
- Space Research Institute
- Edição: Volume 73, Nº 2 (2018)
- Páginas: 225-234
- Seção: Article
- URL: https://journals.rcsi.science/1990-3413/article/view/212671
- DOI: https://doi.org/10.1134/S1990341318020086
- ID: 212671
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Resumo
We present the results of ground based observations and model analysis of transits of exoplanets WASP-33b, WASP-43b, WASP-104b, and HD 219134b. Broadband transmission spectra (dependence of the observed radii on wavelength) have been plotted for all exoplanets, ranging from the near-UV to the IR region. We show that the transmission spectrum of WASP-33b is, within errors, flat in the range of 3800 Å to 12 000 Å. The derived broadband spectrum of WASP-43b is also flat in the first approximation, although other authors have reported the presence of absorption lines of various chemical elements in the narrow bands. Model spectra of WASP-43b taken from the literature and based on IR data allowed us to obtain a direct estimate of its nighttime temperature. We present and analyze the results of ground based observations which confirm the discovery of a transiting super-Earth in the HD 219134 star system. Signs of this planet’s existence were discovered earlier during the radial velocity analysis of the star, as well as transit observations with the Spitzer space telescope in the IR.At the estimated time, we registered a transit in the near-UV range several times. The transit depth measured in the U-band of the Johnson photometric system amounts to 0.13% ± 0.027%, which is deeper than the one based on Spitzer measurements. We discuss the possible causes of this difference.
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Sobre autores
G. Valyavin
Special Astrophysical Observatory
Autor responsável pela correspondência
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
D. Gadelshin
Special Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
A. Valeev
Special Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
T. Burlakova
Special Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
K. Antonyuk
Crimean Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nauchniy, 298409
G. Galazutdinov
Special Astrophysical Observatory; Instituto de Astronomia; Main (Pulkovo) Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167; Av. Angamos 0610, Antofagasta; Saint Petersburg, 196140
N. Pit
Crimean Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nauchniy, 298409
A. Moskvitin
Special Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
E. Sokov
Special Astrophysical Observatory; Main (Pulkovo) Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167; Saint Petersburg, 196140
I. Sokova
Main (Pulkovo) Observatory
Email: gvalyavin@sao.ru
Rússia, Saint Petersburg, 196140
B.-C. Lee
Korea Astronomy and Space Science Institute
Email: gvalyavin@sao.ru
República da Coreia, Daejeon, 34055
I. Han
Korea Astronomy and Space Science Institute
Email: gvalyavin@sao.ru
República da Coreia, Daejeon, 34055
M. Lendl
Space Research Institute
Email: gvalyavin@sao.ru
Áustria , Graz, A-8042
L. Fossati
Space Research Institute
Email: gvalyavin@sao.ru
Áustria , Graz, A-8042
A. Grauzhanina
Special Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
T. Fatkhullin
Special Astrophysical Observatory
Email: gvalyavin@sao.ru
Rússia, Nizhnii Arkhyz, 369167
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