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Data-driven Modeling of Telluric Features and Stellar Variability with StellarSpectraObservationFitting.jl

  • Authors: Christian Gilbertson, Eric B. Ford, Samuel Halverson, Evan Fitzmaurice, Cullen H. Blake, Gumundur Stefánsson, Suvrath Mahadevan, Jason T. Wright, Jacob K. Luhn, Joe P. Ninan, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien

Christian Gilbertson et al 2026 The Astronomical Journal 172 .

  • Provider: AAS Journals

Caption: Figure 6.

An example of a time-averaged spectrum for an order of NEID data (which includes Ca II H&K ) showing which parts of the spectrum are being used by SSOF after data preprocessing. Different parts of the spectrum are masked for various reasons. The bluer side of this order (order 155 in Table 2) had low SNR (yellow border). Some pixels were masked by the instrumental pipeline (orange border) or had anomalously high observations (green border). Pixels which are never used (red) are surrounded by pixels that are sometimes used (blue). The blue pixels are sometimes ignored when fine-tuning S⊕, S⋆, and v⋆.

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