Flame: A Flexible Data Reduction Pipeline for Near-Infrared and Optical Spectroscopy

TL;DR

Flame is a versatile, modular data reduction pipeline designed for near-infrared and optical spectroscopic observations, enabling flexible calibration, rectification, and sky subtraction across various instruments.

Contribution

It introduces a flexible, modular architecture for spectroscopic data reduction that simplifies calibration and rectification processes for diverse instruments.

Findings

Successfully applied to LUCI and LRIS data.

Achieves accurate wavelength calibration with minimal interpolation.

Effectively corrects spatial misalignments during rectification.

Abstract

We present flame, a pipeline for reducing spectroscopic observations obtained with multi-slit near-infrared and optical instruments. Because of its flexible design, flame can be easily applied to data obtained with a wide variety of spectrographs. The flexibility is due to a modular architecture, which allows changes and customizations to the pipeline, and relegates the instrument-specific parts to a single module. At the core of the data reduction is the transformation from observed pixel coordinates (x, y) to rectified coordinates (lambda, gamma). This transformation consists in the polynomial functions lambda(x,y) and gamma(x,y) that are derived from arc or sky emission lines and slit edge tracing, respectively. The use of 2D transformations allows one to wavelength calibrate and rectify the data using just one interpolation step. Furthermore, the gamma(x,y) transformation includes also the spatial misalignment between frames, which can be measured from a reference star observed simultaneously with the science targets. The misalignment can then be fully corrected during the rectification, without having to further resample the data. Sky subtraction can be performed via nodding and/or modeling of the sky spectrum; the combination of the two methods typically yields the best results. We illustrate the pipeline by showing examples of data reduction for a near-infrared instrument (LUCI at the Large Binocular Telescope) and an optical one (LRIS at the Keck telescope).