Simulating Observations in CASA 4.0: Difference between revisions
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=== Step-by-Step Simulations === | === Step-by-Step Simulations === | ||
simobserve and simanalyze can be broken down into a series of steps, each of which is modular. As long as you follow a few conventions about filenames, you can run each | <tt>simobserve</tt> and <tt>simanalyze</tt> can be broken down into a series of steps, each of which is modular. As long as you follow a few conventions about filenames, you can run each step independently and optionally. For example, using <tt>simobserve</tt>, you can modify the sky model, then predict ACA visibilities, then run again to predict 12m interferometer visibilities. With simanalyze you can image and analyze both the ACA and ATCA measurement sets together. You can run interactive clean yourself, and, minding your filenames, you can run simanalyze just to calculate a difference image and analyze the results. | ||
The major steps involved in simulating data with CASA are: | The major steps involved in simulating data with CASA are: | ||
Revision as of 19:34, 7 November 2012
UNDER DEVELOPMENT
- This guide is applicable to CASA version 4.0. For older versions of CASA please see Simulating Observations in CASA 3.4.
Introduction
The task simobserve can be used to simulate an observation in CASA. simobserve turns a model of the sky (2 to 4 dimensions including frequency and polarization) into the visibilities that would be measured with ALMA, (J)VLA, CARMA, SMA, ATCA, PdB, et cetera. simobserve can also add thermal noise (from receiver, atmosphere, and ground) to the visibilities. simobserve uses the aatm atmospheric model, a thin wrapper of Juan Pardo's ATM library, to accurately calculate all atmospheric corruption terms (noise, phase delay) as a function of frequency and site characteristics.
After creating the visibilities, task simanalyze will produce a cleaned image of the model visibilities. It will compare that image with your input convolved with the output clean beam, and then calculate a fidelity image.
Taskname History The simulation tasks have been under significant revision and development.
- In CASA 3.3 simobserve and simanalyze were named sim_observe and sim_analyze, respectively.
- In CASA 3.4 and earlier, the functionality of both tasks was contained in task simdata, which is now obsolete.
ALMA Simulations and Proposals
Although simobserve can simulate data for many instruments, this guide (and the tutorials linked below) focuses in particular on simulating ALMA observations. ALMA is still under construction. We will update CASA's simulation tasks and tools as ALMA commissioning proceeds. During this period, we expect the noise properties of the telescope to be increasingly better characterized, and its configurations to be refined.
Rigorous verification of the noise calculations between simobserve and the ALMA sensitivity calculator are performed periodically. (The ALMA Observation Preparation Tool uses the same algorithm as the ALMA sensitivity calculator.) The most recent such verification was performed during August 2012.
The noise in a synthesis image is dependent on the imaging and deconvolution parameters; therefore small differences between the simple radiometer-equation based ALMA sensitivity calculator and simobserve/simanalyze are to be expected. See NAASC memo 102 for more discussion.
Larger differences between the radiometer equation and a simulation may also result in a simulated image that is limited by dynamic range. It is for this reason that ALMA users should consider running a simulation when applying for telescope time. The results of the simulation can be a strong support to one's observing proposal, as a way to demonstrate the scientific feasibility of the observing plan.
Finally, simobserve will not be able to provide realistic results if the pixel size of the input sky model is comparable to, or larger than, the simulated output clean beam.
Users should be aware of the Observation Support Tool (OST) [1]. This is a web-based interface to an ALMA simulator hosted by the University of Manchester, UK. Like simobserve, the OST is based on the CASA sm toolkit. However, the OST and simobserve use different wrapper scripts and employ different treatment of atmospheric effects. Comparisons to the ALMA sensitivity calculator made in March 2011 suggest that both simobserve and the OST give similar noise level for observations in bands 3 through 8. However, the results of the two tools diverge in bands 9 and 10.
Values from simobserve or the OST should not be used to calculate exposure times for ALMA Science Goals. Only values from the ALMA sensitivity calculator should be used for this purpose, as it is the ALMA sensitivity calculator that will be used in the technical assessment of ALMA proposals. However, the results of simulations may be helpful to support a request for more observing time than is required by the sensitivity calculator, in order to obtain better uv-plane coverage.
Tutorials
| Simulation Guide for New Users (CASA 4.0) | 
|
|---|---|
| A fully annotated tutorial that uses a Spitzer SAGE 8 micron continuum image of 30 Doradus and scales it to greater distance. A good place for new users to start. | |
| Protoplanetary Disk Simulation (CASA 4.0) | 
|
| A sky model with a lightly annotated script that simulates a protoplanetary disk. Uses a theoretical model of dust continuum from Sebastian Wolff, scaled to the distance of a nearby star. This is another fairly generic simulation - if you're short on time, you probably don't need to go through this one and the New Users guide, but it can be useful to go through multiple examples. | |
| Simulation Guide Component Lists (CASA 4.0) | 
|
| Tutorial for simulating data based on multiple sources (using both a FITS image and a component list). If you are interested in simulating from a list of simple sources (point, Gaussian, disk), rather than or in addition to a sky model image, then read the considerations here. | |
| Einstein-Face (CASA 4.0) | 
|
| A sky model and lightly annotated script that simulates the face of Einstein as seen by ALMA. This simulation is particularly useful for those who wish to better understand spatial filtering by an interferometer, but doesn't demonstrate new capabilities of the simulation tasks beyond those described above. | |
| ACA Simulation (CASA 4.0) | 
|
| A tutorial for simulating ALMA observations that use multiple configurations or use the
12-meter array in combination with the ALMA Compact Array. Of particular interest to those wishing to explore multi-component ALMA observations and their combination and e.g. whether the ACA improves your scientific fidelity. |
Example Input and Output
Several examples of input model images are showcased here: Sim Inputs.
Several examples of simanalyze output images are showcased here: Sim Outputs.
Advanced CASA Simulation
Step-by-Step Simulations
simobserve and simanalyze can be broken down into a series of steps, each of which is modular. As long as you follow a few conventions about filenames, you can run each step independently and optionally. For example, using simobserve, you can modify the sky model, then predict ACA visibilities, then run again to predict 12m interferometer visibilities. With simanalyze you can image and analyze both the ACA and ATCA measurement sets together. You can run interactive clean yourself, and, minding your filenames, you can run simanalyze just to calculate a difference image and analyze the results.
The major steps involved in simulating data with CASA are:
- simobserve
- Modify Model - relabel (scale) the spectral and spatial coordinates and brightness of the sky model image.
- Set Pointings - calculate a mosaic of pointings and save in a text file. You could also make the text file yourself.
- Predict - Calculate visibilities for a specified array on a specified day.
- Corrupt - Corrupt the measurement set with thermal noise, phase noise, cross-polarization, etc.
- simanalyze
Under the Hood: The sm Tool
simobserve calls methods in the sm tool. For advanced users, sm has methods that can add phase delay variations, gain fluctuations and drift, cross-polarization, and (coming soon) bandpass and pointing errors to simulated data. sm also has more flexibility in adding thermal noise than simobserve. The tutorials linked from this page describe the simulation of data using the task interface only. To learn more about sm, see the CASA Toolkit Reference Manual.
Ephemeris and Geodesy
Generic ephemeris and geodesy calculations can be done using CASA Python module simutil.py.
Warning: CLEAN Bias
As is the case for real images, cleaning images produced by simobserve can lead to a spurious decrease in object fluxes and noise on the image ("clean bias"). This is particularly true for observations with poor coverage of the uv-plane, i.e. using telescopes with small numbers of antennas, such as the ALMA Early Science configurations, and/or in short "snapshot" observations. Users should always clean images with care, using a small number of iterations and/or a conservative (3-5sigma) threshold and boxing bright sources.
User Feedback
We welcome input on developing the CASA simulator. Contact "rindebet at nrao.edu" if you would like to volunteer your input.
