File:The first full spectral energy distribution of a Y-dwarf.jpg

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English: Figure 2. The first full spectral energy distribution (black) from 1–21 μm of a Y dwarf (WISE 0359−54), with key molecular features identified (color). It consists of merged and calibrated JWST spectra and photometry (F1500W, F1800W, and F2100W), in dimensions of fν The transition between the NIRSpec and MIRI LRS spectra occurs at 5.14 μm and can be seen easily by the change in resolving power. The FWHM of the photometric bandpasses are marked with horizontal bars, while the vertical bars on the photometric points represent the 1σ flux density error. The typical signal-to-noise of the NIRSpec and MIRI LRS spectra are ∼20 and ∼100, respectively. (The data used to create this figure are available.)
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Source https://doi.org/10.3847/2041-8213/ace32c
Author The First JWST Spectral Energy Distribution of a Y Dwarf, Samuel A. Beiler et al 2023 ApJL 951 L48

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