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High-resolution Spectroscopic Detection of TiO and a Stratosphere in the Day-side of WASP-33b

• Authors: Stevanus K. Nugroho, Hajime Kawahara, Kento Masuda, Teruyuki Hirano, Takayuki Kotani, and Akito Tajitsu

2017 The Astronomical Journal 154 221.

• Provider: AAS Journals

Caption: Figure 7.

(a) The colored line is an example of the blue CCD spectrum of WASP-33 after standard reduction. Different colors mean different orders. The black line is the Coelho model spectrum. (b) The barycentric-corrected RV of WASP-33 during the observation (red star), as a result of combining the RV of each order that has the highest cross-correlation signal. The blue line is the weighted median combination of all frames that was taken as the RV of WASP-33. The error bar is the 1σ scatter across the observation time.