Hi Steven,
Quote:
Originally Posted by Merlin66
Steven,
OK understood....
What would have been "better" is to take a A type spectrum with exactly the same set up to calibrate the dispersion and then used the identified Balmer lines in the 3C273 spectrum to verify the red shift amount......
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I suggest checking your spectrum image, you may well find you have already captured some A stars in the same field that you can use for wavelength calibration. You can then derive the redshift direct rather than having to assume it. See for example the update in red here when I made the same measurement.
http://www.threehillsobservatory.co..../spectra_3.htm
Cheers
Robin