Journal
ASTRONOMY & ASTROPHYSICS
Volume 638, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/202037719
Keywords
planetary systems; planets and satellites; atmospheres; planet-star interactions; planets and satellites; general; planets and satellites; individual; GJ 3470b
Categories
Funding
- German Max-Planck-Gesellschaft (MPG)
- Spanish Consejo Superior de Investigaciones Cientificas(CSIC)
- European Union through FEDER/ERF [FICTS-2011-02]
- Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades
- European FEDER/ERF [ESP2016-80435-C2-2-R, ESP2016-76076-R, BES-2015-074542, AYA2016-79425-C3-1/2/3-P]
- Deutsche Forschungsgemeinschaft [FOR2544]
- National Natural Science Foundation of China [11503088, 11573073, 11573075]
- Natural Science Foundation of Jiangsu Province [BK20190110]
- Priority Program SPP 1992 Exploring the Diversity of Extrasolar Planets [RE 1664/16-1]
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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 aR(p)(lambda)/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, (M) over dot, is confined to a range of 3 x 10(10)g s(-1)forT= 6000 K to 10 x 10(10)g s(-1)forT= 9000 K. We discuss the physical mechanisms and implications of the HeIdetection 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.
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