Abstract
We explore via spectroscopic modeling whether the highly correlated diffuse interstellar bands at 6613.6 and 6196.0 Å might originate from a single molecule. Efforts were made to simulate the band contours of the DIBs along the three lines-of-sight, which have been observed by others at high resolution: HD179406, HD174165, and Her 36. Reasonable simultaneous fits were obtained using a prolate symmetric top molecule that exhibits transitions of two different band types, type-a parallel and type-b perpendicular bands. Two different excited states of a long- or heavy-chain, forked molecule are proposed. A minimum number of adjustable parameters were used including ground and excited state \(A\) and \(B\) rotational constants, an excited state centrifugal distortion constant, and three different rotational excitation temperatures. Points in favor and against the hypothesis are discussed.
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Acknowledgements
We thank Erik Hoy for help with the early calculations and David Dixon for references to the iron cluster data. The DIB spectra from HD179406 and HD147165 are reproduced with permission from Jacob Krełowski; that from 36 Her is reproduced with permission from Julie Dahlstrom.
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Glinski, R.J., Eller, M.W. On a common carrier hypothesis for the 6613.6 and 6196.0 Å diffuse interstellar bands. Astrophys Space Sci 361, 305 (2016). https://doi.org/10.1007/s10509-016-2878-x
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DOI: https://doi.org/10.1007/s10509-016-2878-x