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The Impact of Non-Gaussian Line Spread Functions on Stellar Kinematic Recovery: Consequences for Dynamical Models
The line spread function (LSF) of a spectrograph encodes the inherent broadening of a single spectral line. It is typically reported as a single number, the resolving power $R = λ/Δλ$ with $Δλ$ the FWHM of the LSF. In standard pipelines for extracting stellar kinematics the LSF is assumed to be a wa
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