On a common carrier hypothesis for the 6613.6 and 6196.0 {\AA} diffuse
  interstellar bands
  We explore via spectroscopic modeling whether the highly correlated diffuse
interstellar bands at 6613.6 and 6196.0 {\AA} 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.
