The atmosphere of HD 209458b seen with ESPRESSO No detectable planetary absorptions at high resolution

被引：48

作者：

Casasayas-Barris, N. ^{[1
,2
]}

Palle, E. ^{[1
,2
]}

Stangret, M. ^{[1
,2
]}

Bourrier, V. ^{[3
]}

Tabernero, H. M. ^{[4
]}

Yan, F. ^{[5
]}

Borsa, F. ^{[6
]}

Allart, R. ^{[3
]}

Zapatero Osorio, M. R. ^{[7
]}

Lovis, C. ^{[3
]}

Sousa, S. G. ^{[4
]}

Chen, G. ^{[8
]}

Oshagh, M. ^{[1
,2
]}

Santos, N. C. ^{[4
,9
]}

Pepe, F. ^{[3
]}

Rebolo, R. ^{[1
,2
,13
]}

Molaro, P. ^{[11
,12
]}

Cristiani, S. ^{[11
]}

Adibekyan, V. ^{[4
,9
]}

Alibert, Y. ^{[10
]}

Allende Prieto, C. ^{[1
,2
]}

Bouchy, F. ^{[3
]}

Demangeon, O. D. S. ^{[4
,9
,16
]}

Di Marcantonio, P. ^{[11
]}

D'Odorico, V. ^{[11
,12
]}

Ehrenreich, D. ^{[3
]}

Figueira, P. ^{[4
,14
]}

Genova Santos, R. ^{[1
,2
]}

Gonzalez Hernandez, J. I. ^{[1
,2
]}

Lavie, B. ^{[1
,3
]}

Lillo-Box, J. ^{[14
]}

Lo Curto, G. ^{[15
]}

Martins, C. J. A. P. ^{[4
,16
]}

Mehner, A. ^{[17
]}

Micela, G. ^{[18
]}

Nunes, N. J. ^{[19
]}

Poretti, E. ^{[6
,20
]}

Sozzetti, A. ^{[21
]}

Suarez Mascareno, A. ^{[1
,2
]}

Udry, S. ^{[3
]}

机构：

[1] Inst Astrofis Canarias, Via Lactea S-N, Tenerife 38205, Spain

[2] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[3] Univ Geneva, Observ Astron, Chemin Pegasi 51b, CH-1290 Sauverny, Switzerland

[4] Univ Porto, Inst Astrofis & Ciencias Espaco, CAUP, Rua Estrelas, P-4150762 Porto, Portugal

[5] Georg August Univ, Inst Astrophys, Friedrich Hund Pl 1, D-37077 Gottingen, Germany

[6] INAF Osservatorio Astron Brera, Via Bianchi 46, I-23807 Merate, Italy

[7] Ctr Astrobiol CSIC INTA, Carretera Ajalvir,Km 4, Madrid 28850, Spain

[8] Chinese Acad Sci, Purple Mt Observ, Key Lab Planetary Sci, Nanjing 210023, Peoples R China

[9] Univ Porto, Fac Ciencias, Dept Fis & Astron, Rua Campo Alegre, P-4169007 Porto, Portugal

[10] Univ Bern, Inst Phys, Sidlerstr 5, CH-3012 Bern, Switzerland

[11] INAF Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy

[12] Inst Fundamental Phys Universe, Via Beirut 2, I-34151 Trieste, Italy

[13] CSIC, Madrid, Spain

[14] Ctr Astrobiol CSIC INTA, ESAC Campus, Madrid 28692, Spain

[15] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[16] Univ Porto, Ctr Astrofis, Rua Estrelas, P-4150762 Porto, Portugal

[17] European Southern Observ, Alonso de Cordova 3107, Vitacura, Region Metropol, Chile

[18] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy

[19] Univ Lisbon, Fac Ciencias, Inst Astrofis & Ciencias Espaco, P-1749016 Lisbon, Portugal

[20] INAF Fdn Galileo Galilei, Rambla Jose Ana Fernandez Perez 7, Tenerife 38712, Spain

[21] INAF Osservatorio Astrofis Torino, Via Osservatorio 20, I-10025 Pino Torinese, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 647卷

基金：

中国国家自然科学基金; 瑞士国家科学基金会; 欧洲研究理事会;

关键词：

planets and satellites: individual: HD 209458b; planets and satellites: atmospheres; methods: observational; techniques: spectroscopic; TRANSMISSION SPECTROSCOPY; MODEL ATMOSPHERES; SODIUM-ABSORPTION; OPTICAL-SPECTRUM; HOT; PARAMETERS; EXOPLANETS; SEARCH; MASS; TIO;

D O I：

10.1051/0004-6361/202039539

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We observed two transits of the iconic gas giant HD 209458b between 380 and 780 nm, using the high-resolution ESPRESSO spectrograph. The derived planetary transmission spectrum exhibits features at all wavelengths where the parent star shows strong absorption lines, for example, NaI, MgI, FeI, FeII, CaI, VI, H alpha, and KI. We interpreted these features as the signature of the deformation of the stellar line profiles due to the Rossiter-McLaughlin effect, combined with the centre-to-limb effects on the stellar surface, which is in agreement with similar reports recently presented in the literature. We also searched for species that might be present in the planetary atmosphere but not in the stellar spectra, such as TiO and VO, and obtained a negative result. Thus, we find no evidence of any planetary absorption, including previously reported NaI, in the atmosphere of HD 209458b. The high signal-to-noise ratio in the transmission spectrum (similar to 1700 at 590 nm) allows us to compare the modelled deformation of the stellar lines in assuming different one-dimensional stellar atmospheric models. We conclude that the differences among various models and observations remain within the precision limits of the data. However, the transmission light curves are better explained when the centre-to-limb variation is not included in the computation and only the Rossiter-McLaughlin deformation is considered. This demonstrates that ESPRESSO is currently the best facility for spatially resolving the stellar surface spectrum in the optical range using transit observations and carrying out empirical validations of stellar models.

引用

页数：19

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