Constraining the size of the carrier of the $\lambda$5797.1 diffuse
  interstellar band
  The diffuse interstellar band (DIB) at 5797.1 \AA\ is simulated based on
three premises: (1) The carrier of the DIB is polar as concluded by T. Oka et
al. from the anomalous spectrum toward Herschel 36. (2) The sharp central
feature observed by P. J. Sarre's group is the $Q$-branch of a parallel band of
a prolate top. (3) The radiative temperature of the environment is $T_r$=2.73
K.
  A $^2 \Pi \leftarrow$ $^2\Pi$ transition of a linear radical is simulated.
Results depend on 10 parameters, with the rotational constant $B$ being the
most critical. Comparisons of calculated spectra with observed data constrain
$B$, which in turn constrains the number of heavy atoms to 5 $\leq n \leq 7$.
Upper limits based on the Her 36 spectrum and lower limits based on stability
against photodissociation are also discussed. The latter is based on the
assumption that the DIB molecules are produced top-down from the breakdown of
dust rather than bottom-up by chemical reactions.
  A difficulty with this limit is that J. P. Maier's laboratory has observed
many molecules within this size range, some of which have been tested
astronomically. Candidates are discussed in light of many prolate tops observed
by the P. Thaddeus and M. C. McCarthy microwave group.
