# Difference between revisions of "Simulation Recipes"

From CASA Guides

(→Nearby edge-on spiral) |
(→Nearby edge-on spiral) |
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* 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 | ||

− | <math>\frac{Jy}{Sr} = \frac{4\times 10^{23} k T}{\pi D^2 | + | <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 <math>2x10^8</math> |

− | now we need to decide if this model data will work at the desired pixel scale | + | 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". [[File:Beamsummary.png]] indicates that for ALMA at 100GHz, configuration 20 is appropriate. | * 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". [[File:Beamsummary.png]] indicates that for ALMA at 100GHz, configuration 20 is appropriate. | ||

* if we intend to set <tt>cell=0.04arcsec</tt> in <tt>simdata</tt>, then the cube needs to be multiplied by | * if we intend to set <tt>cell=0.04arcsec</tt> in <tt>simdata</tt>, then the cube needs to be multiplied by | ||

<math>2x10^8 * (.04/206265)^2 = 7.9x10^{-6}</math> to obtain Jy/pixel. The cube peaks at ~3K, so we can perform the simulation with <tt>inbright=2.3e-5</tt> | <math>2x10^8 * (.04/206265)^2 = 7.9x10^{-6}</math> to obtain Jy/pixel. The cube peaks at ~3K, so we can perform the simulation with <tt>inbright=2.3e-5</tt> | ||

+ | |||

+ | will we be dominated by the noise in the input model? | ||

+ | * input noise ~150mK or S/N~20, so at our scaled intensity, a few mJy/bm. The exposure time calculator says that ALMA will achieve 1.3mJy/bm in an hour, so we should set this up as a half hour snapshot. |

## Revision as of 14:04, 16 December 2009

## 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]\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 [math]2x10^8[/math]

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

[math]2x10^8 * (.04/206265)^2 = 7.9x10^{-6}[/math] to obtain Jy/pixel. The cube peaks at ~3K, so we can perform the simulation with `inbright=2.3e-5`

will we be dominated by the noise in the input model?

- input noise ~150mK or S/N~20, so at our scaled intensity, a few mJy/bm. The exposure time calculator says that ALMA will achieve 1.3mJy/bm in an hour, so we should set this up as a half hour snapshot.