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The catalog compiled by \citet{Peretto2009a} lists 11,000 IRDCs, but none of the features cataloged will be Nessie-like on its own. The structure-finding algorithm used in the Peretto \& Fuller work is biased toward finding core-like roundish peaks, so a cloud like Nessie forms a connect-the-dots pattern in the Peretto \& Fuller catalog. In fact, Nessie is comprised of $\sim 100$ Peretto \& Fuller sources. So, while the Peretto \& Fuller catalog is tremendously useful to the study of the properties of massive star forming cores, it will only become useful for finding ``bones" when someone applies a clever dot-connecting algorithm to it, and its ilk.  Some very large, and/or very extended, IRDCs, such as the so-called ``Massive Molecular Filament" studied by \citet{Battersby}, are not located along the plane-of-the-sky projected spiral arms. These clouds, which are probably just massive star-forming regions near but not exactly in the Galactic plane, do not appear as straight or highly-elongated as Nessie (cf.the ``wisp" discussed by Li et al.xx \cite{http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1310.3267} \citep {http://adsabs.harvard.edu/abs/2013A%26A...559A..34L}  ), and they may offer a hint at what threshold to set in looking for elongated features as we search for more bones. Futher, once numerical galaxy-simulation modeling resolution catches up to observational resolution, models should be able to say whether they other, non-bone-like, massive IRDCs had their origins long ago in bones, or form in some other way.