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dc.creatorYork, Donald G.en_US
dc.creatorThorburn, J. A.en_US
dc.creatorHobbs, L. M.en_US
dc.creatorOka, T.en_US
dc.creatorWelty, D. E.en_US
dc.creatorSnow, T. P.en_US
dc.creatorRachford, B. L.en_US
dc.creatorMcCall, Benjamin J.en_US
dc.creatorFriedman, S. D.en_US
dc.creatorSonnentrucker, P.en_US
dc.date.accessioned2006-06-15T20:35:43Z
dc.date.available2006-06-15T20:35:43Z
dc.date.issued2003en_US
dc.identifier2003-RA-05en_US
dc.identifier.urihttp://hdl.handle.net/1811/20840
dc.description$^{a}$Based on observations from the APO 3.5-meter telescope, owned and operated by the Astrophysical Research Consortium.en_US
dc.descriptionAuthor Institution: University of Chicago, Astronomy \& Astrophysics Center; Center for Astrophysics and Space Astronomy, University of Colorado; Department of Astronomy, University of California; Department of Astronomy, Space Telescope Science Institute;; Department of Physics \& Astronomy, Johns Hopkins Universityen_US
dc.description.abstractWe have conducted an exhaustive astronomical observing campaign aimed at developing a high-quality, uniform set of spectra of the diffuse interstellar bands (DIBs), with the goal of refining physical and chemical constraints that may ultimately help in the identification of the specific carriers of the DIBs. In the present study we have analyzed the correlations between molecular and atomic hydrogen and five selected DIBs, which include the strongest DIB (at 4428{\AA}); three prominent DIBs that have been included in many previous surveys ($\lambda\lambda 5780, 5797$, and 6284); and one DIB (4963{\AA}) that represents a new class identified by our survey as being closely associated with diatomic carbon (Thorburn \emph{et al}. 2003, ApJ, 584, 339; see also the Thorburn et al. paper in this symposium, presented by T. Oka). We find that the 5780 and 6284{\AA} DIBs correlate very strongly with atomic hydrogen but extremely weakly with molecular hydrogen, suggesting that the carriers of these two DIBs do not co-exist with $H_{2}$. The correlations between the DIBs at 4428, 5797, and 4963 {\AA} and atomic and molecular hydrogen are more complex, but also suggest that there is no strong connection with molecular hydrogen. We discuss an empirical picture in which most of the DIB carriers form in low-density atomic gas while $H_{2}$ and possibly the ``$C_{2}$ DIBs'' arise in denser regions. One possible chemical interpretation is that the carriers of the traditional DIBs may be primary ions, which would be efficiently converted to protonated ions by hydrogen abstraction reactions in the presence of $H_{2}$, whereas the carriers of the ""$C_{2}$ DIBs"" do not react with $H_{2}$.en_US
dc.format.extent396364 bytes
dc.format.mimetypeimage/jpeg
dc.language.isoEnglishen_US
dc.publisherOhio State Universityen_US
dc.titleTHE RELATIONSHIP OF MOLECULAR HYDROGEN, ATOMIC HYDROGEN, AND SELECTED DIFFUSE INTERSTELLAR $BANDS^{a}$en_US
dc.typearticleen_US


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