absorption line Comparison Table

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absorption line comparison table

Subject has discoverer has specie has equivalent width has definition has dicovery date occurs in has detection procedure has wavelength has width

b-lines A triplet of spectral lines of Mg I. λλ 5167-5184 Å

Fraunhofer line Joseph Fraunhofer Absorption line in the spectrum of the Sun, studied by Fraunhofer in 1814. The nine most prominent he labeled with capital letters (from the red end) A. B. C. D. E. F. G. H. and K. The A band and B band are now known to be groups of telluric lines due to O₂ absorption in Earth's atmosphere, and C and F are respectively known as Hα and Hβ. 1814 Sun

h-line Mg II Singly ionized magnesium resonance line. 2803 Å

interstellar line depends on the amount of absorbing matter between the source and the observer Sharp, distinct absorption lines superposed on stellar spectra, produced by the interstellar gas located between the source and the observer. Strongest are the D lines, followed by the H and K lines, and the K I doublet at 7699 and 7644 Å. O stars narrow absorption lines which don't participate in the periodic Doppler shift of intrinsic absorption lines in a binary star narrow

K I doublet potassium (K I) 7699 and 7644 Å

k line Mg II Singly ionized magnesium resonance line. 2795.5 Å

Subject	has discoverer	has specie	has equivalent width	has definition	has dicovery date	occurs in	has detection procedure	has wavelength	has width
b-lines				A triplet of spectral lines of Mg I.				λλ 5167-5184 Å
Fraunhofer line	Joseph Fraunhofer			Absorption line in the spectrum of the Sun, studied by Fraunhofer in 1814. The nine most prominent he labeled with capital letters (from the red end) A. B. C. D. E. F. G. H. and K. The A band and B band are now known to be groups of telluric lines due to O₂ absorption in Earth's atmosphere, and C and F are respectively known as Hα and Hβ.	1814	Sun
h-line		Mg II		Singly ionized magnesium resonance line.				2803 Å
interstellar line			depends on the amount of absorbing matter between the source and the observer	Sharp, distinct absorption lines superposed on stellar spectra, produced by the interstellar gas located between the source and the observer. Strongest are the D lines, followed by the H and K lines, and the K I doublet at 7699 and 7644 Å.		O stars	narrow absorption lines which don't participate in the periodic Doppler shift of intrinsic absorption lines in a binary star		narrow
K I doublet		potassium (K I)						7699 and 7644 Å
k line		Mg II		Singly ionized magnesium resonance line.				2795.5 Å

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