Deconvolution of Spectra for Near-Infrared Astronomical Instruments

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SUMMARY

The discussion centers on the need for deconvolution techniques in long slit spectroscopy for near-infrared astronomical instruments, specifically between 0.950 and 2.2 microns with a resolution of R=30. The primary challenge is the convolution of steep spectral features with the line spread function (LSF), which is modeled as a sinc function. Variations in LSF width across wavelengths complicate the observation of rapid flux changes. Participants suggest exploring various deconvolution methods to partially correct these convolution effects.

PREREQUISITES
  • Understanding of long slit spectroscopy techniques
  • Familiarity with line spread functions (LSF) and their mathematical representation
  • Knowledge of deconvolution methods applicable in spectroscopy
  • Experience with near-infrared instrumentation and its spectral range
NEXT STEPS
  • Research deconvolution algorithms such as Wiener deconvolution and Richardson-Lucy deconvolution
  • Explore the mathematical modeling of line spread functions in spectroscopy
  • Investigate software tools for spectral analysis, such as IRAF or Python libraries like SciPy
  • Study case studies on deconvolution applications in astronomical spectroscopy
USEFUL FOR

Astronomers, optical engineers, and researchers involved in spectroscopy who are looking to enhance the accuracy of spectral data obtained from near-infrared instruments.

Deckard
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Hi,

I am working on long slit spectroscopy for an astronomical instrument, and I think I need deconvolution, but I am not sure, so maybe you will be able to answer me :) Currently those are only simulations. I work in near-infrared (0.950 -> 2.2 micron) with a low resolution (R=30).

My problem is that the spectrum I am supposed to observe can be very steep (ie I can have a quick flux variation between \lambda and \lambda+\delta\lambda), but when I watch them through my instrument, this spectrum is convolved with the slit LSF (line spread function), which is a sinc function (sinc(x)=sin(\pi x)/\pi x). Of course the width of the LSF varies acording to wavelength, and then is much larger at 0.95 micron than at 2.2 micron. And when I observe a steep change in the spectrum through the spectrograph, the change is much less steeper because it has been convolved with the LSF which is less steeper.

Are there some deconvolution methods that can correct, at least partialy what I describe?

I hpe what I say is making sense. If it's not I can post some picture to illustrate this. Thanks a lot in advance.

-- Arthur;
 
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Deconvolution. With applications in spectroscopy, PA Jansson - New York: Academic Press, 1984, edited by Jansson, Peter A., 1984

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