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         title="Permalink to Late Night Ideas, Oct 6 2013">Late Night Ideas, Oct 6 2013</a></h2>
 
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    <abbr class="published" title="2013-10-07T01:00:00-06:00">
      2013/10/07
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    <address class="vcard author">
      By <a class="url fn" href="https://keflavich.github.io/blog/author/adam-ginsburg.html">Adam Ginsburg</a>
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  <div class="entry-content">
    <p>Coffee at 7 pm usually isn't a problem...</p>
<blockquote>
<ol class="arabic simple">
<li>Dendrogram analysis of turbulent simulations.  What do the structures look
like?  Mostly for visualization in a talk, but perhaps the start of a paper.
Are the high-density substructures too small to collapse?  Too hot?</li>
<li>A deep GBT+AO observation of the center of the G49 40km/s cloud.  Can we
perform the same measurement as I did originally against a uniform
backlight?  Will that provide new information</li>
<li>Corollary to 2: In simulations, what effect does a varying size and
brightness backlight have on the inferred density?</li>
<li>Measure the distance to the G49 cloud with NIR extinction.  Keep working
with Jonathan Foster on that...</li>
<li>Test the Cepheid / RR Lyrae distance method on the G49 cloud.  It's close
enough that the targets should be bright.  Start off with 1-hour pilot
(DD?) on the most distant star with a &quot;guaranteed&quot; CO detection, then
propose a longer project to begin using the bisector approach to determine
its true distance.</li>
<li>Eta Car ALMA.  Basically, same thing, but now invoke the SN 1987A CO
detection.  Eta is the closer laboratory, and it must have similar shock
physics...</li>
<li>H3+ in the CMZ with Juergen.  Talk to Tom Geballe about H3+ and CO
absorption.  Is it possible to measure CO absorption to red giants?</li>
</ol>
</blockquote>

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