Ultraviolet spectroscopy of interstellar and intergalactic matter

J. Michael Shull

doi:10.1364/AO.19.004002

Applied Optics
Vol. 19,
Issue 23,
pp. 4002-4006
(1980)
•https://doi.org/10.1364/AO.19.004002

Ultraviolet spectroscopy of interstellar and intergalactic matter

J. Michael Shull

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J. Michael Shull, "Ultraviolet spectroscopy of interstellar and intergalactic matter," Appl. Opt. 19, 4002-4006 (1980)

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Abstract

Ultraviolet radiation in absorption and emission provides diagnostics of interstellar and intergalactic matter. After reviewing some basic physical reasons for the importance of UV astronomy, the UV observations of both media, the future uses of high resolution spectrometers in the far UV, and the atomic data required for proper interpretation are discussed. Satellite UV observations have the potential of answering fundamental questions dealing with the nature of the gaseous matter in the outer regions of our galaxy, in neighboring galaxies, and in the intergalactic matter seen in quasar absorption spectra.

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Species	Line (Å)	Diagnostics
H i	1215.670 (Lyman-α)	H column density
D i	949.485 (Lyman-δ)	D/H ratio; cosmological implications
H₂	1049.368 [4–0 R(0)]	H₂ abundance, kinetic temperature,
	1049.961 [4–0 R(1)]	H density, UV radiation field
	1061.697 [4–0 R(5)]
S ii	1259.520
Si ii	1190.418
Fe ii	1144.946	Abundances; tracers of cold neutral clouds
C ii	1036.337
O i	1302.169
N i	1134.165
N ii	1083.990
N ii	1084.562	Abundances; tracers of hot (50,000 K) or photoionized gas; electron density
Si iii	1206.510
C iii	977.026
O vi	1031.945	Tracers of coronal-type (2 × 10⁵ K) gas
	1037.627

Atomic process	Comments
(1) Oscillator strengths for UV lines from ground state	Si ii, Fe ii
(2) Electron collisional excitation^a of permitted and intercombination lines	Ions of C, N, O, Si, S, Ne, and especially Fe
(3) Electron collisional ionization	Ions of C, N, O, Si, S, Ne, and especially Fe
(4) Excitation of H₂ levels (V, J)	H-H₂ and H₂-H₂
(5) Dielectronic recombination rates	Fe ions
(6) Charge transfer to H, He	Exp. measurements for O iii, O iv, C iii, Ne iii, Si iii, N ii, N iii; branching ratios to excited states

Species	Line (Å)	Diagnostics
H i	1215.670 (Lyman-α)	H column density
D i	949.485 (Lyman-δ)	D/H ratio; cosmological implications
H₂	1049.368 [4–0 R(0)]	H₂ abundance, kinetic temperature,
	1049.961 [4–0 R(1)]	H density, UV radiation field
	1061.697 [4–0 R(5)]
S ii	1259.520
Si ii	1190.418
Fe ii	1144.946	Abundances; tracers of cold neutral clouds
C ii	1036.337
O i	1302.169
N i	1134.165
N ii	1083.990
N ii	1084.562	Abundances; tracers of hot (50,000 K) or photoionized gas; electron density
Si iii	1206.510
C iii	977.026
O vi	1031.945	Tracers of coronal-type (2 × 10⁵ K) gas
	1037.627

Atomic process	Comments
(1) Oscillator strengths for UV lines from ground state	Si ii, Fe ii
(2) Electron collisional excitation^a of permitted and intercombination lines	Ions of C, N, O, Si, S, Ne, and especially Fe
(3) Electron collisional ionization	Ions of C, N, O, Si, S, Ne, and especially Fe
(4) Excitation of H₂ levels (V, J)	H-H₂ and H₂-H₂
(5) Dielectronic recombination rates	Fe ions
(6) Charge transfer to H, He	Exp. measurements for O iii, O iv, C iii, Ne iii, Si iii, N ii, N iii; branching ratios to excited states

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