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JWST COMPASS: NIRSpec/G395H Transmission Observations of the Sub-Neptune HD 15337 c

  • Authors: Nicole L. Wallack, Peter Gao, Michael Greklek-McKeon, Annabella Meech, Artyom Aguichine, Munazza K. Alam, Lili Alderson, Natasha E. Batalha, Natalie M. Batalha, Anna Gagnebin, Tyler A. Gordon, James Kirk, Mercedes López-Morales, Sarah E. Moran, Jea Iyanla Redai, Nicholas Scarsdale, Johanna Teske, Hannah R. Wakeford, Nicholas F. Wogan, Angie Wolfgang

Nicole L. Wallack et al 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 11.

Nonphysical model fits to the combined (left), visit 1 (middle), and visit 2 (right) Eureka! data reductions for the (top to bottom) flat, step function, slope, and NRS1 and NRS2 Gaussian models, respectively. For each panel, the data are given by the points, the 1σ bounds of the best-fit models are given by the inner, darker bands, and the 3σ bounds are given by the outer, lighter bands. For the flat, step function, and slope models the best-fit parameter values and associated uncertainties are given in the figure, where D is the average transit depth across both detectors, D2 is the average NRS2 transit depth, and ΔD is the offset between the NRS1 and NRS2 detectors; those of the Gaussian models are given in Table 5.

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