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A He I upper atmosphere around the warm Neptune GJ 3470 b

Palle, E. ; Nortmann, L. ; Casasayas-Barris, N. ; Lampón, M. ; López-Puertas, M. ; Caballero, J. A. ; Sanz-Forcada, J. ; Lara, L. M. ; Nagel, E. ; Yan, F. ; Alonso-Floriano, F. J. ; Amado, P. J. ; Chen, G. ; Cifuentes, C. ; Cortés-Contreras, M. ; Czesla, S. ; Molaverdikhani, K. ; Montes, D. ; Passegger, V. M. ; Quirrenbach, A. ; Reiners, A. ; Ribas, I. ; Sánchez-López, A. ; Schweitzer, A. ; Stangret, M. ; Zapatero Osorio, M. R. ; Zechmeister, M.

Astronomy and astrophysics (Berlin), 2020-06, Vol.638, p.A61 [Periódico revisado por pares]

Heidelberg: EDP Sciences

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Título:
A He I upper atmosphere around the warm Neptune GJ 3470 b
Autor: Palle, E. ; Nortmann, L. ; Casasayas-Barris, N. ; Lampón, M. ; López-Puertas, M. ; Caballero, J. A. ; Sanz-Forcada, J. ; Lara, L. M. ; Nagel, E. ; Yan, F. ; Alonso-Floriano, F. J. ; Amado, P. J. ; Chen, G. ; Cifuentes, C. ; Cortés-Contreras, M. ; Czesla, S. ; Molaverdikhani, K. ; Montes, D. ; Passegger, V. M. ; Quirrenbach, A. ; Reiners, A. ; Ribas, I. ; Sánchez-López, A. ; Schweitzer, A. ; Stangret, M. ; Zapatero Osorio, M. R. ; Zechmeister, M.
Assuntos: Absorption ; Atmospheric models ; Chemical composition ; Extrasolar planets ; Gas giant planets ; Light curve ; Night ; Planetary atmospheres ; Planetary systems ; Radiative transfer ; Signal to noise ratio ; Transit ; Upper atmosphere ; Weather
É parte de: Astronomy and astrophysics (Berlin), 2020-06, Vol.638, p.A61
Descrição: High resolution transit spectroscopy has proven to be a reliable technique for the characterization of the chemical composition of exoplanet atmospheres. Taking advantage of the broad spectral coverage of the CARMENES spectrograph, we initiated a survey aimed at characterizing a broad range of planetary systems. Here, we report our observations of three transits of GJ 3470 b with CARMENES in search of He (2 3 S) absorption. On one of the nights, the He  I region was heavily contaminated by OH − telluric emission and, thus, it was not useful for our purposes. The remaining two nights had a very different signal-to-noise ratio (S/N) due to weather. They both indicate the presence of He (2 3 S) absorption in the transmission spectrum of GJ 3470 b, although a statistically valid detection can only be claimed for the night with higher S/N. For that night, we retrieved a 1.5 ± 0.3% absorption depth, translating into a R p ( λ )∕ R p = 1.15 ± 0.14 at this wavelength. Spectro-photometric light curves for this same night also indicate the presence of extra absorption during the planetary transit with a consistent absorption depth. The He (2 3 S) absorption is modeled in detail using a radiative transfer code, and the results of our modeling efforts are compared to the observations. We find that the mass-loss rate, Ṁ , is confined to a range of 3 × 10 10 g s −1 for T = 6000 K to 10 × 10 10 g s −1 for T = 9000 K. We discuss the physical mechanisms and implications of the He  I detection in GJ 3470 b and put it in context as compared to similar detections and non-detections in other Neptune-size planets. We also present improved stellar and planetary parameter determinations based on our visible and near-infrared observations.
Editor: Heidelberg: EDP Sciences
Idioma: Inglês

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A He I upper atmosphere around the warm Neptune GJ 3470 b

Heidelberg: EDP Sciences

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A He I upper atmosphere around the warm Neptune GJ 3470 b