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Spectroscopy - Coggle Diagram
Spectroscopy
what causes line broadening
natural(quantum)
pressure
thermal
rotational
other motions(turbulence)
the instrument broadens the spectrum too
characteristics of spectral lines
profile(shape)
EW
FWHM
flux
three types of spectra
continuous spectra
absorption line spectra
emission line spectra
grating equation
blazing
the 0th order doesn't takes all the light
specular reflection
incident + output = 2*(blaze angle)
littrow
highest grating efficiency
diffraction
double-slit diffraction
smaller d with larger dispersion
multiple-slit diffraction
SNR defined for spectra
defined for the extracted 1-D spectrum in SNR per pixel or per resolution element
spectral calibration
bias and dark as usual
flat: need to catch the chromatic effect
background subtraction & sky subtraction
spectral typing
OBAFGKM
spectral resolution
R = λ/δλ
low R < 10000; high R > 40000
spectral normalization
removing the cotinuum & blaze
redshift
precise radial velosity
λ_e= λ_0 ∙( 1+z )