Detection of Fe and evidence for TiO in the dayside emission spectrum of WASP-33b

被引：54

作者：

Cont, D. ^{[1
]}

Yan, F. ^{[1
]}

Reiners, A. ^{[1
]}

Casasayas-Barris, N. ^{[2
,3
,4
]}

Molliere, P. ^{[5
]}

Palle, E. ^{[2
,3
]}

Henning, Th. ^{[5
]}

Nortmann, L. ^{[1
]}

Stangret, M. ^{[2
,3
]}

Czesla, S. ^{[6
]}

Lopez-Puertas, M. ^{[7
]}

Sanchez-Lopez, A. ^{[4
]}

Rodler, F. ^{[8
]}

Ribas, I. ^{[9
,10
]}

Quirrenbach, A. ^{[11
]}

Caballero, J. A. ^{[12
]}

Amado, P. J. ^{[7
]}

Carone, L. ^{[5
]}

Khaimova, J. ^{[1
]}

Kreidberg, L. ^{[5
]}

Molaverdikhani, K. ^{[5
,11
]}

Montes, D. ^{[13
,14
]}

Morello, G. ^{[2
]}

Nagel, E. ^{[6
,15
]}

Oshagh, M. ^{[2
,3
]}

Zechmeister, M. ^{[1
]}

机构：

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

[2] Inst Astrofis Canarias IAC, Calle Via Lactea S-N, Tenerife 38200, Spain

[3] Univ La Laguna, Dept Astrofis, Tenerife 38026, Spain

[4] Leiden Univ, Leiden Observ, Postbus 9513, NL-2300 RA Leiden, Netherlands

[5] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[6] Univ Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany

[7] CSIC, Inst Astrofis Andalucia IAA, Glorieta Astron S-N, Granada 18008, Spain

[8] European Southern Observ ESO, Alonso Cordova 3107,Casilla 19001, Santiago, Chile

[9] CSIC IEEC, Inst Ciencies Espai, Campus UAB,C Can Magrans S-N, Barcelona 08193, Spain

[10] Inst Estudis Espacials Catalunya IEEC, Barcelona 08034, Spain

[11] Heidelberg Univ, Zentrum Astron, Landessternwarte, Konigstuhl 12, D-69117 Heidelberg, Germany

[12] CSIC, INTA, ESAC, Ctr Astrobiol, Camino Bajo Castillo S-N, Madrid 28692, Spain

[13] Univ Complutense Madrid, Fac Ciencias Fis, Dept Fis Tierra & Astrofis, Madrid 28040, Spain

[14] Univ Complutense Madrid, Fac Ciencias Fis, IPARCOS, Inst Fis Particulas & Cosmos, Madrid 28040, Spain

[15] Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany

来源：

ASTRONOMY & ASTROPHYSICS | 2021年 / 651卷

基金：

欧洲研究理事会;

关键词：

planets and satellites: atmospheres; techniques: spectroscopic; planets and satellites: individual: WASP-33b; OPTICAL-TRANSMISSION SPECTRUM; THERMAL INVERSIONS; GIANT EXOPLANET; ORBITAL MOTION; HOT JUPITERS; PHASE CURVE; ATMOSPHERE; TRANSIT; IRON; SPECTROSCOPY;

D O I：

10.1051/0004-6361/202140732

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Theoretical studies predict the presence of thermal inversions in the atmosphere of highly irradiated gas giant planets. Recent observations have identified these inversion layers. However, the role of different chemical species in their formation remains unclear. Aims. We search for the signature of the thermal inversion agents TiO and Fe in the dayside emission spectrum of the ultra-hot Jupiter WASP-33b. Methods. The spectra were obtained with CARMENES and HARPS-N, covering different wavelength ranges. Telluric and stellar absorption lines were removed with SYSREM. We cross-correlated the residual spectra with model spectra to retrieve the signals from the planetary atmosphere. Results. We find evidence for TiO at a significance of 4.9 sigma with CARMENES. The strength of the TiO signal drops close to the secondary eclipse. No TiO signal is found with HARPS-N. An injection-recovery test suggests that the TiO signal is below the detection level at the wavelengths covered by HARPS-N. The emission signature of Fe is detected with both instruments at significance levels of 5.7 sigma and 4.5 sigma, respectively. By combining all observations, we obtain a significance level of 7.3- for Fe. We find the TiO signal at Kp = 248:0+2:0 2:5 km s 1, which is in disagreement with the Fe detection at Kp = 225:0+4:0 3:5 km s 1. The Kp value for Fe is in agreement with prior investigations. The model spectra require different temperature profiles for TiO and Fe to match the observations. We observe a broader line profile for Fe than for TiO. Conclusions. Our results confirm the existence of a temperature inversion layer in the planetary atmosphere. The observed Kp offset and different strengths of broadening in the line profiles suggest the existence of a TiO-depleted hot spot in the planetary atmosphere.

引用

页数：20

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