dc.creator York, Donald G. en_US dc.creator Thorburn, J. A. en_US dc.creator Hobbs, L. M. en_US dc.creator Oka, T. en_US dc.creator Welty, D. E. en_US dc.creator Snow, T. P. en_US dc.creator Rachford, B. L. en_US dc.creator McCall, Benjamin J. en_US dc.creator Friedman, S. D. en_US dc.creator Sonnentrucker, P. en_US dc.date.accessioned 2006-06-15T20:35:43Z dc.date.available 2006-06-15T20:35:43Z dc.date.issued 2003 en_US dc.identifier 2003-RA-05 en_US dc.identifier.uri http://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.description Author 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 University en_US dc.description.abstract We 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.extent 396364 bytes dc.format.mimetype image/jpeg dc.language.iso English en_US dc.publisher Ohio State University en_US dc.title THE RELATIONSHIP OF MOLECULAR HYDROGEN, ATOMIC HYDROGEN, AND SELECTED DIFFUSE INTERSTELLAR $BANDS^{a}$ en_US dc.type article en_US
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