The gas-to-dust ratio in the Orion nebula

Details The gas-to-dust ratio in the Orion nebula The gas-to-dust ratio in the Orion nebula

Nov 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974hrgc.conf..191p&link_type=abstract

H II regions and the galactic centre : proceedings of the Eighth ESLAB Symposium, 4-7 June 1974, Frascati, Italy, p. 191-194 (SE

Physics

Cosmic Dust, Interstellar Gas, Nebulae, Orion Constellation, Electron Density (Concentration), H Beta Line, Image Tubes, Spectrographs, Stellar Spectra

Scientific paper

About 60 spectra were obtained using an image tube with the nebular spectrograph of the Asiago 122 cm reflector, in a position W-E from north of the Trapezium across the star P1925 into the bay area of the Orion nebula. Twenty-five spectra were selected for accurate measurements of the H beta intensity and of the electron density by the (S2) 6730/6716 intensity line ratio. The results are interpreted in terms of well-mixed gas and dust, not only in the central bright regions, but even in the bay area, where the coefficient of dust extinction counted per electron is found to be larger than in the bright center of the nebula.

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