Volume 452, Number 1, June II 2006
|Page(s)||269 - 272|
|Section||Interstellar and circumstellar matter|
|Published online||17 May 2006|
Measuring interstellar gas-phase D/H ratios in the presence of H2
National Radio Astronomy Observatory, 520 Edgemont Road, 22903-2475 Charlottesville, VA, USA e-mail: firstname.lastname@example.org
Accepted: 21 February 2006
Aims.To clarify the circumstances under which it is acceptable to approximate the interstellar gas-phase D/H ratio by D I/H I.
Methods.Observed column densities of H I, D I, H2 and HD are compared for six lines of sight having appreciable fractions of H2.
Results.The overall fraction of deuterium in HD varies by a factor 3-4 but is found to be much smaller than the fraction of H in H2 in all cases, implying that deuterium appears as D I and N(D I)/N(H I) exceeds the gas-phase D/H ratio in H2-bearing gas.
Conclusions.Deuterium in H2-bearing gas contributes to the observed D I absorption and the D/H ratio should be inferred from N(D)/N(H) where N(D) = (N(D I) + N(HD)), N(H) = N(H I) + 2N(H2): failure to do so biases the resulting D/H ratio upward, typically by 5%-15% in present data. Along sightlines with multiple kinematic components having different molecular fractions, fractionation can cause velocity differences between D I and H I profiles. Shifts between H2 and HD velocity centroids may arise when the molecule-bearing gas has kinematic substructure reflecting regions of different ionization balance and HD/H2 ratios.
Key words: ISM: abundances / ISM: atoms / ISM: molecules
© ESO, 2006
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