The Airborne Infrared Spectrometer: Development, Characterization, and the 21 August 2017 Eclipse Observation

Samra, Jenna E.; Marquez, Vanessa; Cheimets, Peter; DeLuca, Edward E.; Golub, Leon; Hannigan, James W.; Madsen, Chad A.; Vira, Alisha; Adams, Arn

doi:10.48550/arxiv.2105.09419

Cited by 2 publications

(2 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Our four selected coronal line emission profiles are synthesized using CLE and scaled based on theoretical or observed literature intensities. The available literature has debated over which conditions coronal line intensities can be measured from ground instrumentation or airborne instrumentation or via balloon flights (e.g., Kuhn et al 1999;Lin et al 2004;Penn 2014;Samra et al 2018;Judge et al 2019;Samra et al 2021). Theoretical calculations for coronal line intensities at heights of ∼1.1 R e were computed by Judge (1998) and adapted by us in Table 1.…”

Section: Observations Instrumentation and Modelingmentioning

confidence: 99%

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

Ali

Paraschiv

Reardon

et al. 2022

ApJ

View full text Add to dashboard Cite

The infrared solar spectrum contains a wealth of physical data about the Sun and is being explored using modern detectors and technology with new ground-based solar telescopes. One such instrument will be the ground-based Cryogenic Near-IR Spectro-Polarimeter of the Daniel K. Inouye Solar Telescope (DKIST), which will be capable of sensitive imaging of the faint infrared solar coronal spectra with full Stokes I, Q, U, and V polarization states. Highly ionized magnetic dipole emission lines have been observed in galaxies and the solar corona. Quantifying the accuracy of spectral inversion procedures requires a precise spectroscopic calibration of observations. A careful interpretation of the spectra around prominent magnetic dipole lines is essential for deriving physical parameters and particularly for quantifying the off-limb solar coronal observations from DKIST. In this work, we aim to provide an analysis of the spectral regions around the infrared coronal emission lines of Fe xiii 1074.68 nm, Fe xiii 1079.79 nm, Si x 1430.10 nm, and Si ix 3934.34 nm, aligning with the goal of identifying solar photospheric and telluric lines that will help facilitate production of reliable inversions and data products from four sets of solar coronal observations. The outputs can be integrated in processing pipelines to produce level 2 science-ready data.

show abstract

Section: Observations Instrumentation and Modelingmentioning

confidence: 99%

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

Ali

Paraschiv

Reardon

et al. 2022

ApJ

View full text Add to dashboard Cite

show abstract

“…The available literature has debated over which conditions coronal line intensities can be measured from ground instrumentation, airborne instrumentation or via balloon flights (e.g. Kuhn et al 1999;Lin et al 2004;Penn 2014;Samra et al 2018;Judge et al 2019;Samra et al 2021). Theoretical calculations for coronal line intensities at heights of ∼1.1R were computed by Judge (1998), and adapted by us in Table 1.…”

Section: Observations Instrumentation and Modelingmentioning

confidence: 99%

A spectroscopic survey of infrared 1-4μm spectra in regions of prominent solar coronal emission lines of Fe XIII, Si X, and Si IX

Ali,

Paraschiv,

Reardon

et al. 2022

Preprint

View full text Add to dashboard Cite

The infrared solar spectrum contains a wealth of physical data about the Sun and is being explored using modern detectors and technology with new ground-based solar telescopes. One such instrument will be the ground-based Cryogenic Near-IR Spectro-Polarimeter of the Daniel K. Inouye Solar Telescope that will be capable of sensitive imaging of the faint infrared solar coronal spectra with full Stokes I, Q, U, and V polarization states. Highly ionized magnetic dipole emission lines have been observed in galaxies and the solar corona. Quantifying the accuracy of spectral inversion procedures requires a precise spectroscopic calibration of observations. A careful interpretation of the spectra around prominent magnetic dipole lines is essential for deriving physical parameters, and particularly, for quantifying the off-limb solar coronal observations from DKIST. In this work, we aim to provide an analysis of the spectral regions around the infrared coronal emission lines of Fe XIII 1074.68 nm, Fe XIII 1079.79 nm, Si X 1430.10 nm, and Si IX 3934.34 nm, aligning with the goal of identifying solar photospheric and telluric lines that will help facilitate production of reliable inversions and data products from four sets of solar coronal observations. The outputs will be integrated in the processing pipeline to produce Level-2 science-ready data that will be made available to DKIST observers.

show abstract

The Airborne Infrared Spectrometer: Development, Characterization, and the 21 August 2017 Eclipse Observation

Cited by 2 publications

References 24 publications

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

A Spectroscopic Survey of Infrared 1–4 μm Spectra in Regions of Prominent Solar Coronal Emission Lines of Fe XIII, Si X, and Si IX

A spectroscopic survey of infrared 1-4μm spectra in regions of prominent solar coronal emission lines of Fe XIII, Si X, and Si IX

Contact Info

Product

Resources

About