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Fraunhofer line comparison table

Subject	has detection procedure	is a kind of	occurs in	has lower energy level	has wavelength	is an instance of	has upper energy level	has series limit	has definition	has specie	has equivalent width	has width
A band		Fraunhofer line	Earth's atmosphere		7600 Å				One of about a dozen of the strongest Fraunhofer lines seen in the Solar spectrum, the A band at 7600 angstoms is due to telluric lines of molecular oxygen in the Earth's atmosphere. (originally thought to originate in the Sun by Fraunhofer)	O2
B band		Fraunhofer line	Earth's atmosphere		7100 Å				Telluric lines due to O2 absorption in Earth's atmosphere, but originally thought to originate in the Sun by Fraunhofer.	O2
D line	narrow absorption lines which don't participate in the periodic Doppler shift of intrinsic absorption lines in a binary star	interstellar line	Sun						Spectral line of neutral sodium, also the strongest interstellar line.	Na I	depends on the amount of absorbing matter between the source and the observer	narrow
E line		Fraunhofer line	Sun		5270 Å				Spectral line consisting of a blend of Fe I and Ca I.	Fe I and Ca I
G band		Fraunhofer line	G star, K star		4303 Å				A band of CH. It is conspicuous in the spectra of G-K stars.	CH
H alpha			Sun	2	6563 Å	Balmer line	3	3647 Å
H beta			Sun	2	4861 Å	Balmer line	4	3647 Å
HK lines		Fraunhofer line	Sun						Two spectral lines of singly ionized calcium. The second strongest interstellar line.	Ca II

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