2018A&A...616A.151C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST01:57:56

2018A&A...616A.151C - Astronomy and Astrophysics, volume 616A, 151-151 (2018/8-1)

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

CASASAYAS-BARRIS N., PALLE E., YAN F., CHEN G., ALBRECHT S., NORTMANN L., VAN EYLEN V., SNELLEN I., TALENS G.J.J., GONZALEZ HERNANDEZ J.I., REBOLO R. and OTTEN G.P.P.L.

Abstract (from CDS):

We used the HARPS-North high resolution spectrograph (R=115000) 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 (NaI) 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 NaI doublet position with an averaged absorption depth of 0.17±0.03% for a 0.75Å bandwidth with line contrasts of 0.44±0.11% (D2) and 0.37±0.08% (D1). The NaI TLC have also been computed, showing a large Rossiter-McLaughlin (RM) effect, which has a 0.20±0.05% NaI transit absorption for a 0.75Å 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 0.75Å 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±50K) are needed to explain the lines contrast. Particularly, we find that the Na I lines core require a temperature of T=4210±180K and that Hα requires a temperature of T=4330±520K. 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.

Abstract Copyright: © ESO 2018

Journal keyword(s): planetary systems - techniques: spectroscopic - planets and satellites: atmospheres - methods: observational - planets and satellites: individual: MASCARA-2b - planets and satellites: individual: KELT-20b

VizieR on-line data: <Available at CDS (J/A+A/616/A151): tsm2bna.dat tsm2bha.dat lcm2bna.dat lcm2bha.dat>

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME G Cloud Cld 03 00 +50.2           ~ 64 0
2 WASP-49b Pl 06 04 21.4734612842 -16 57 55.108837741           ~ 33 1
3 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3027 0
4 NAME Mic Cloud Cld 18 10 +13.           ~ 7 0
5 * 5 Vul * 19 26 13.2462609696 +20 05 51.839397272   5.585 5.591     A0V 69 0
6 HD 185603 * 19 38 38.7352870670 +31 13 09.215701765   7.67 7.58     A0 16 0
7 HD 185603b Pl 19 38 38.7352870670 +31 13 09.215701765           ~ 33 0
8 HD 189733b Pl 20 00 43.7130382888 +22 42 39.071811263           ~ 1082 1
9 BD-05 5432b Pl 21 00 06.1969250596 -05 05 40.037007561           ~ 40 1
10 HD 209458b Pl 22 03 10.7729598762 +18 53 03.548248479           ~ 1468 1

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2020.07.10-01:57:57

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