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Multi-segment and Echelle stellar spectra processing issues and how to solve them

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arxiv 2112.01468 v1 pith:AN5RI3BY submitted 2021-12-02 astro-ph.IM

Sviatoslav Borisov , Igor Chilingarian , Evgenii Rubtsov , Kirill Grishin , Ivan Katkov , Vladimir Goradzhanov , Anton Afanasiev , Anna Saburova
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Anastasia Kasparova Ivan Zolotukhin
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keywords spectrastellarqualitycalibrationechellepopulationproceduressynthesis
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High-quality stellar spectra are in great demand now - they are the most important ingredient in the stellar population synthesis to study galaxies and star clusters. Here we describe the procedures to increase the quality of flux calibration of stellar spectra. We use examples of NIR intermediate-resolution Echelle spectra collected with the Folded InfraRed Echellete (R~6500, Magellan Baade) and high-resolution UV-optical spectra observed with UVES (R~80000, ESO VLT). By using these procedures, we achieved the quality of the global spectrophotometric calibration as good as 1-2%, which fulfills the requirements for the quality of stellar spectra intended to be used in the stellar population synthesis

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