Adding to this thread some gory technical details that I would like to remember...
At
https://www.cloudynights.com/topic/8660 ... ry12555752 , Lou Jost mentions that some nonlinear stretching was necessary to bring various representations into alignment.
I was intrigued to see that in my data, only linear operations were needed. The explanation is that for spectra from a diffraction grating, offset from the optical axis is linear in wavelength, per the formulas at
https://en.wikipedia.org/wiki/Diffraction_grating#Theory_of_operation . So, it is only necessary to know the wavelengths of two points on the spectrum, and all other wavelength are simple to compute.
Here is an incredibly ugly montage of the spectrum collected by my Canon R7 (color band in the middle, lines intensified by strong USM filtering), overlaid on the annotated spectrum at
https://upload.wikimedia.org/wikipedia/commons/7/7d/Fraunhofer_lines_DE.svg , also overlaid by the graph at
https://upload.wikimedia.org/wikipedia/commons/e/e4/Solar_spectral_irradiance.svg , both linked from
https://en.wikipedia.org/wiki/Fraunhofer_lines .
The pixel coordinates of certain major Fraunhofer lines (G,F,b1,E2,D2+D1,C) are pretty clear in my raw data. Working from the known wavelengths of those and the linearity of the spectroscope, I measured the actual wavelengths of my red and blue laser pointers. Those turned out to be blue = 407.2 nm (label says 405 +- 10) and red = 653.5 nm (label says 650 +-10). I assume these wavelengths will vary depending on environmental conditions, but I have no idea by how much or because of what conditions. If anybody knows these things, I would be interested in learning.
Edited to add... I see that I haven't shown any raw data for daylight. That looks like this:
--Rik