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. 2023 Jan 9;614(7949):670–675. doi: 10.1038/s41586-022-05674-1

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© The Author(s) 2023

Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article’s Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article’s Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.

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Extended Data Fig. 3 — The insets highlight the peak of the spectra. The supreme-SPOON spectra are scaled by a factor of 72 to compare the overall shape of the spectra, rather than the extracted flux counts. a, The extracted stellar spectra from order 1. All pipelines are in relatively good agreement, whereas the shape of the iraclis data changes slightly at λ < 1.1 μm. This is probably owing to different traces that were used in the spectral extraction routine. b, The extracted stellar spectra from order 2. Differences at λ = 0.725 and 0.860 μm are because of differences in removing zeroth-order contaminants in the background. The iraclis pipeline does not extract data past λ > 0.85 μm, which is where the order overlap region begins. Across all pipelines, the shape of the spectra, as well as overall absorption features, cosmic-ray-removal techniques and noise levels are consistent. (https://github.com/afeinstein20/wasp39b_niriss_paper/blob/main/scripts/edfigure3.py).