Observations of narrow diffuse interstellar bands toward stars with low reddening

Details Observations of narrow diffuse interstellar bands toward stars with low reddening Observations of narrow diffuse interstellar bands toward stars with low reddening

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..485f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 15, 1984, p. 485-490. Research supported by the Robert A. Welch F

Astronomy and Astrophysics

Astrophysics

15

Abundance, Interstellar Extinction, Interstellar Matter, Molecular Clouds, Cosmic Dust, Diffuse Radiation, Hydrogen Clouds, Interstellar Chemistry, Spectral Line Width, Surface Reactions

Scientific paper

The equivalent widths of the 5780-A, 5797-A, and 6613-A diffuse interstellar bands (DIBs) toward 22 stars with E(B-V) less than 0.1 are determined on the basis of observations obtained with a coude spectrograph and Si-photodiode array on the 2.7-m telescope at McDonald Observatory during June, November, and December, 1982. The results are presented in sample spectra, tables, and graphs and discussed in relation to the N(H2) data of Savage et al. (1977). All three bands are found to be 2-3 times stronger for the group of objects with N(H2) greater than 10 to the 18th/sq cm than for the group with smaller N(H2). Since this observation suggests a molecular origin for the DIBs, but the abundance data argue against a gas-phase molecular carrier, the DIBs are attributed to grain-surface impurity-site/molecular-complex interactions. The proximity of the DIBs to the velocity of the major atomic components is held to rule out the grain-sputtering hypothesis of Smith et al. (1977).

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