The Challenges of Observing, Calibrating, and Modeling Stellar Spectral Energy Distributions. (arXiv:1903.06859v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Prieto_C/0/1/0/all/0/1">Carlos Allende Prieto</a> (Instituto de Astrofisica de Canarias)
While optical and quantum efficiency are on the rise, and spectrographs
becoming massively multiplexed, measuring spectral energy distributions of
astronomical sources with accuracy remains a challenge. In addition to
atmospheric refraction, extinction, variability, and limited apertures of
instrument entrance slits and optical fibers, accurate calibration is hampered
by issues such as a limited choice of reliable standard stars. Modeling stellar
spectral energy distributions has seen good progress, but some weaknesses
survive, especially for late-type stars. This article provides an overview of
these matters and discusses observation, calibration, and modeling strategies
for future large spectroscopic surveys.
While optical and quantum efficiency are on the rise, and spectrographs
becoming massively multiplexed, measuring spectral energy distributions of
astronomical sources with accuracy remains a challenge. In addition to
atmospheric refraction, extinction, variability, and limited apertures of
instrument entrance slits and optical fibers, accurate calibration is hampered
by issues such as a limited choice of reliable standard stars. Modeling stellar
spectral energy distributions has seen good progress, but some weaknesses
survive, especially for late-type stars. This article provides an overview of
these matters and discusses observation, calibration, and modeling strategies
for future large spectroscopic surveys.
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