Observations of O VI Emission from the Diffuse Interstellar Medium toward l = 113°, b = 71°

Details Observations of O VI Emission from the Diffuse Interstellar Medium toward l = 113°, b = 71° Observations of O VI Emission from the Diffuse Interstellar Medium toward l = 113°, b = 71°

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...569..758s&link_type=abstract

The Astrophysical Journal, Volume 569, Issue 2, pp. 758-765.

Astronomy and Astrophysics

Astronomy

20

Galaxy: General, Galaxy: Halo, Ism: General, Ism: Individual: Name: Local Bubble, Ultraviolet: Ism

Scientific paper

Emission from O VI (λλ1032, 1038) in the diffuse interstellar medium was observed in two, long Far Ultraviolet Spectroscopic Explorer (FUSE) observations at l~=113.0d and b~=70.7d (near the quasar HS 1307+4617). The observed intensities are 2580+/-380 (random) +/-360 (systematic) and 1100+/-160 (random) +/-160 (systematic) photons cm-2 s-1 sr-1 in the 1032 and 1038 Å emission lines, respectively. The electron density, thermal pressure, and depth of the emitting gas are calculated from the observed intensities. The velocity of the emitting material is about +10 km s-1 relative to the local standard of rest and less than +30 km s-1 relative to the H I along the line of sight. The similarity suggests that the highly ionized gas is quiescent and not recently shock heated. Emission from the C II 3 s2 S1/2 to 2p2 P3/2 transition at 1037 Å is also observed, and upper limits are placed on the intensities of ultraviolet line emission from C I, C III, N I, N II, Mg II, Si II, S II, S III, S IV, S VI, Fe II, and Fe III.

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