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  Na I and Hα absorption features in the atmosphere of MASCARA-2b/KELT-20b

Casasayas-Barris, N., Pallé, E., Yan, F., Chen, G., Albrecht, S., Nortmann, L., et al. (2018). Na I and Hα absorption features in the atmosphere of MASCARA-2b/KELT-20b. Astronomy and Astrophysics, 616.

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Item Permalink: https://hdl.handle.net/21.11116/0000-0005-CE86-C Version Permalink: https://hdl.handle.net/21.11116/0000-0005-CE87-B
Genre: Journal Article

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https://ui.adsabs.harvard.edu/abs/2018A&A...616A.151C (Any fulltext)
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 Creators:
Casasayas-Barris, N.1, Author
Pallé, E.1, Author
Yan, F.1, Author
Chen, G.1, Author
Albrecht, S.1, Author
Nortmann, L.1, Author
Van Eylen, V.1, Author
Snellen, I.1, Author
Talens, G. J. J.1, Author
González Hernández, J. I.1, Author
Rebolo, R.1, Author
Otten, G. P. P. L.1, Author
Affiliations:
1Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners, ou_2421692              

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Free keywords: planetary systems techniques: spectroscopic planets and satellites: atmospheres methods: observational planets and satellites: individual: MASCARA-2b planets and satellites: individual: KELT-20b Astrophysics - Earth and Planetary Astrophysics
 Abstract: We used the HARPS-North high resolution spectrograph (ℛ = 115 000) at Telescopio Nazionale Galileo (TNG) to observe one transit of the highly irradiated planet MASCARA-2b/KELT-20b. Using only one transit observation, we are able to clearly resolve the spectral features of the atomic sodium (Na I) doublet and the Hα line in its atmosphere, which are corroborated with the transmission calculated from their respective transmission light curves (TLC). In particular, we resolve two spectral features centered on the Na I doublet position with an averaged absorption depth of 0.17 ± 0.03% for a 0.75 Å bandwidth with line contrasts of 0.44 ± 0.11% (D2) and 0.37 ± 0.08% (D1). The Na I TLC have also been computed, showing a large Rossiter-McLaughlin (RM) effect, which has a 0.20 ± 0.05% Na I transit absorption for a 0.75 Å passband that is consistent with the absorption depth value measured from the final transmission spectrum. We observe a second feature centered on the Hα line with 0.6 ± 0.1% contrast and an absorption depth of 0.59 ± 0.08% for a 0.75 Å passband that has consistent absorptions in its TLC, which corresponds to an effective radius of Rλ/RP = 1.20 ± 0.04. While the signal- to-noise ratio (S/N) of the final transmission spectrum is not sufficient to adjust different temperature profiles to the lines, we find that higher temperatures than the equilibrium (Teq = 2260 ± 50 K) are needed to explain the lines contrast. Particularly, we find that the Na I lines core require a temperature of T = 4210 ± 180 K and that Hα requires a temperature of T = 4330 ± 520 K. MASCARA-2b, like other planets orbiting A-type stars, receives a large amount of UV energy from its host star. This energy excites the atomic hydrogen and produces Hα absorption, leading to the expansion and abrasion of the atmosphere. The study of other Balmer lines in the transmission spectrum would allow the determination of the atmospheric temperature profile and the calculation of the lifetime of the atmosphere with escape rate measurements. In the case of MASCARA-2b, residual features are observed in the Hβ and Hγ lines, but they are not statistically significant. More transit observations are needed to confirm our findings in Na I and Hα and to build up enough S/N to explore the presence of Hβ and Hγ planetary absorptions. The reduced HARPS spectra are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr/">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsweb.u-strasbg.fr/cgi- bin/qcat?J/A+A/616/A151">http://cdsweb.u-strasbg.fr/cgi- bin/qcat?J/A+A/616/A151</A>

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 Dates: 2018
 Publication Status: Issued
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Title: Astronomy and Astrophysics
Source Genre: Journal
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Pages: - Volume / Issue: 616 Sequence Number: - Start / End Page: - Identifier: -