The atmosphere of WASP-17b: Optical high-resolution transmission spectroscopy
The atmosphere of WASP-17b: Optical high-resolution transmission spectroscopy
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WASP-17b 的大气层：光学高分辨率透射光谱
DOI：
10.1051/0004-6361/201732029
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发表时间：
2017
影响因子：
6.5
通讯作者：
Khalafinejad
中科院分区：
文献类型：
--
作者：
Khalafinejad
High-resolution transmission spectroscopy is a method for understanding the chemical and physical properties of upper exoplanetary atmospheres. Due to large absorption cross-sections, resonance lines of atomic sodium D-lines (at 5889.95 and 5895.92 Å) produce large transmission signals. Our aim is to unveil the physical properties of WASP-17b through an accurate measurement of the sodium absorption in the transmission spectrum. We analyze 37 high-resolution spectra observed during a single transit of WASP-17b with the MIKE instrument on the 6.5 mMagellanTelescopes. We exclude stellar flaring activity during the observations by analyzing the temporal variations of Hαand Ca II infrared triplet (IRT) lines. We then obtain the excess absorption light curves in wavelength bands of 0.75, 1, 1.5, and 3 Å around the center of each sodium line (i.e., the light curve approach). We model the effects of differential limb-darkening, and the changing planetary radial velocity on the light curves. We also analyze the sodium absorption directly in the transmission spectrum, which is obtained by dividing in-transit by out-of-transit spectra (i.e., the division approach). We then compare our measurements with a radiative transfer atmospheric model. Our analysis results in a tentative detection of exoplanetary sodium: we measure the width and amplitude of the exoplanetary sodium feature to beσNa= (0.128 ± 0.078) Å and ANa= (1.7 ± 0.9)% in the excess light curve approach andσNa= (0.850 ± 0.034) Å and ANa= (1.3 ± 0.6)% in the division approach. By comparing our measurements with a simple atmospheric model, we retrieve an atmospheric temperature of 1550 K and radius (at 0.1 bar) of 1.81 ± 0.02RJupfor WASP-17b.
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