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Catherine Zucker edited By_overlaying_the_HO.tex
about 9 years ago
Commit id: c186d918686fb8c84e5045465ef19809f710275a
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By overlaying the HOPS, MALT90, BGPS, and GRS determined velocities on a p-v diagram of CO emission, we determine whether these filaments are physical spines or simply a chance projection of mid-infrared extinction features along our line-of-sight. For this study, we use the whole-galaxy \citet{Dame_2001} CO survey to locate each of the arms in p-p-v space. Of the approximately fifteen candidates identified visually, ten of these candidates are within 10 km/s of the Scutum-Centaurus and Norma-Cygnus arms. The central coordinates for these ten filaments, along with their average lengths, LSR velocities, and distances, are listed in table \ref{tab:candidates}. We plot these ten candidates in p-p-v space, as shown in figure \ref{fig:skeleton}. In addition to showing our Bone candidates, we show several different predictions of the positions of two spiral arms toward the inner Galaxy in longitude-velocity space, from \citet{Dame_2011}, \citet{Sanna_2014}, \citet{Shane_1972}, and \citet{Vallee_2008}. For reference, we note that the new BeSSeL (maser) results from \citet{Sato_2014} in the first quadrant favor the oldest, HI-based \citet{Shane_1972}, fits for the Scutum arm.
\cite{Sanna_2014}