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Intensity Conserving Spectral FittingThe detailed shapes of spectral line profiles provide valuable information about the emitting plasma, especially when the plasma contains an unresolved mixture of velocities, temperatures, and densities. As a result of finite spectral resolution, the intensity measured by a spectrometer is the average intensity across a wavelength bin of non-zero size. It is assigned to the wavelength position at the center of the bin. However, the actual intensity at that discrete position will be different if the profile is curved, as it invariably is. Standard fitting routines (spline, Gaussian, etc.) do not account for this difference, and this can result in significant errors when making sensitive measurements. Detection of asymmetries in solar coronal emission lines is one example. Removal of line blends is another. We have developed an iterative procedure that corrects for this effect. It can be used with any fitting function, but we employ a cubic spline in a new analysis routine called Intensity Conserving Spline Interpolation (ICSI). As the name implies, it conserves the observed intensity within each wavelength bin, which ordinary fits do not. Given the rapid convergence, speed of computation, and ease of use, we suggest that ICSI be made a standard component of the processing pipeline for spectroscopic data.
Document ID
20170003745
Document Type
Reprint (Version printed in journal)
Authors
Klimchuk, J. A. (NASA Goddard Space Flight Center Greenbelt, MD United States)
Patsourakos, S. (Ioannina Univ. Greece)
Tripathi, D. (Inter-University Centre for Astronomy and Astrophysics (IUCAA) Pune, India)
Date Acquired
April 20, 2017
Publication Date
December 15, 2015
Publication Information
Publication: Solar Physics
Volume: 291
Issue: 1
ISSN: 0038-0938
Subject Category
Astrophysics
Numerical Analysis
Report/Patent Number
GSFC-E-DAA-TN41088
Distribution Limits
Public
Copyright
Other