Simulation Recipes: Difference between revisions
| Line 7: | Line 7: | ||
* model data: Milky Way 13CO from the [http://www.bu.edu/galacticring/ Galactic Ring Survey] on the 14m [http://www.astro.umass.edu/~fcrao/ FCRAO] | * model data: Milky Way 13CO from the [http://www.bu.edu/galacticring/ Galactic Ring Survey] on the 14m [http://www.astro.umass.edu/~fcrao/ FCRAO] | ||
* units: K - first convert to flux surface brightness | * units: K - first convert to flux surface brightness | ||
Jy/Sr = 4x10<sup>23</sup> k T / ( π D<sup>2</sup> Ω ), where Ω | <!-- Jy/Sr = 4x10<sup>23</sup> k T / ( π D<sup>2</sup> Ω ), where Ω --> | ||
<math>\frac{Jy}{Sr} = \frac{4\times 10^{23} k T}{\pi D^2 \Omega}</math>, where <math>\Omega</math> | <math>\frac{Jy}{Sr} = \frac{4\times 10^{23} k T}{\pi D^2 \Omega}</math>, where <math>\Omega</math> | ||
is the beam solid angle. At 110GHz the factor is 2x10<sup>8</sup> | is the beam solid angle. At 110GHz the factor is 2x10<sup>8</sup> | ||
Revision as of 20:17, 16 December 2009
↵ Simulating Observations in CASA
Massively Under Construction
(i.e. don't believe what you see here yet, or ask me when it doesn't make sense :)
Nearby edge-on spiral
Roughly modeled after NGC891
- model data: Milky Way 13CO from the Galactic Ring Survey on the 14m FCRAO
- units: K - first convert to flux surface brightness
[math]\displaystyle{ \frac{Jy}{Sr} = \frac{4\times 10^{23} k T}{\pi D^2 \Omega} }[/math], where [math]\displaystyle{ \Omega }[/math] is the beam solid angle. At 110GHz the factor is 2x108
now we need to decide if this model data will work at the desired pixel scale
- the GRS resolution of 40" at ~10kpc is 0.04" at 10Mpc, so we should be able to do a simulation of observing at ~0.1-0.2".
indicates that for ALMA at 100GHz, configuration 20 is appropriate. - if we intend to set cell=0.04arcsec in simdata, then the cube needs to be multiplied by
2x108 * (.04/206265)2 = 7.9x10-6 to obtain Jy/pixel. The cube peaks at ~3K, so we can perform the simulation with inbright=2.3e-5, which should yield a peak of ~0.3mJy/bm.
will we be dominated by the noise in the input model?
- input noise ~150mK or S/N~20, so at our scaled intensity, ~0.015 mJy/bm. The exposure time calculator says that ALMA will achieve 2.6mJy/bm in 2 hours if we keep the input 212m/s channel width (0.075MHz), so the noise in the input model should not affect our results.
setup:
- the ALMA 12m primary beam is 50" so we'd space a mosaic by 25", but the model cube has 326x357 pixels, or 13 arcsec with our small pixels. That's a lot smaller than the primary beam, so it doesn't matter much what output image size we ask for.
- there are 659 channels in the input cube, so we'll keep the same width and nchan.
here're the simdata inputs : File:Simdata.n891.txt
CASA <> execfile("simdata.ngc891.txt")
CASA <> go simdata
here's the cube with the simdata's scaling and World Coordinate System:
and a spectral profile in the box marked in green on the channel image above
