M51 at z = 0.1: Difference between revisions
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# in bash (or other unix shell) | # in bash (or other unix shell) | ||
gunzip NGC5194.bima.12m.cm.fits | gunzip NGC5194.bima.12m.cm.fits | ||
</source> | |||
Load these data into CASA. For later convenience, we'll store the name of the resulting measurement set into the python global <tt>cubeName</tt>. | |||
<source lang="python"> | |||
cubeName = 'm51-song' | |||
importfits(fitsimage='NGC5194.bima12m.cm.fits', imagename=cubeName) | |||
</source> | </source> | ||
Revision as of 14:52, 29 April 2010
This article is under construction. Watch this space!
Overview
This tutorial presents a simulation of ALMA observations of a well-known galaxy, M51, as it would be observed at redshift z = 0.1.
The goal of this tutorial is to provide a complete run-through of a relatively simple simulation. Included in this simulation are the effects of (u, v) sampling of a 50-antenna ALMA, the primary beam of the ALMA antennas, and thermal noise levels appropriate for the ALMA site. Calibration overheads are not included, nor is phase noise owing to a varying troposphere. As such, this simulation should be viewed as somewhat optimistic.
For this tutorial, we'll use the BIMA SONG observations of M51 as the basis for the model. Grab the file NGC5194.bima12m.cm.fits.gz and uncompress it in a working directory.
# in bash (or other unix shell)
gunzip NGC5194.bima.12m.cm.fits
Load these data into CASA. For later convenience, we'll store the name of the resulting measurement set into the python global cubeName.
cubeName = 'm51-song'
importfits(fitsimage='NGC5194.bima12m.cm.fits', imagename=cubeName)
