simutil contains numerous utility methods which can assist users in generic ephemeris and geodesy calculations to aid in performing simulations and other activities in CASA, as well as some methods used internally by simobserve and simanalyze. Several of these tasks directly call the simulator tool in an attempt to lessen the amount of scripting required and to make it easier for the user. It is used by import and instantiation, similarly to testhelper and recipes:

from simutil import simutil


help u.readantenna

Antenna configuration files are important for several tasks in simutil and other simulator tools. Below is an example of a configuration file.

#coordsys=LOC (local tangent plane)
#x     y    z      diam  name
20.  -20.   28.8   12.0  A12S
20.   20.   28.8   12.0  A12N
-20.  -20.   28.8    7.0  A07S
-20.   20.   28.8    7.0  A07N

The observatory, COFA (center of array), coordsys (coordinate system), x, y, z, diam (diameter) and name will be interpreted as header keys or value pairs if they contain "=" and begin with #, and as comments otherwise. Other possible header keys are: zone, datum, or hemisphere. To find the observatory name, one can check the known observatories list by using the measures tool command me.obslist. If an unknown observatory is specified, then one either must use absolute positions (coordsys, XYZ (Cartesian coordinates), UTM (Universal Transverse Mercator)), or specify COFA (longitude and latitude). coordsys can be XYZ (Earth-centered), UTM (easting, northing, and alt), or LOC (xoffset, yoffset, and height). Files for many observatories can be found in: casa.values()[0]['data']+"/alma/simmos".


Tsys and Noise


Noise temperature and efficiencies can be calculated for several telescopes: ALMA, ACA, EVLA, VLA, and SMA. The inputs for simutil.noisetemp method include: telescope, e.g., "ALMA", freq (observing frequency) as a quantity string, e.g., "300GHz", diam (optional - knows diameters for arrays above), e.g., "12m", epsilon = RMS surface accuracy in microns (also optional - this method contains the engineering specification values for each telescope). The outputs produced $\eta_p$ phase efficiency (from Ruze formula), $\eta_s$ spill (main beam) efficiency, $\eta_b$ geometrical blockage efficiency, $\eta_t$ taper efficiency, $\eta_q$ correlator efficiency including quantization, $t_{rx}$ receiver temperature. Where the total antenna efficiency can be calculated from these outputs as such: $\epsilon = \eta_p * \eta_s * \eta_b * \eta_t$.

NOTE: VLA correlator efficiency includes waveguide loss. EVLA correlator efficiency is probably optimistic at 0.88.


This method is used to calculate the noise in an observation by adding noise to visibilities in exactly the same way as sm.corrupt (if doimnoise=True) and also creates a simulated image from which to measure noise. The inputs to calculate sensitivity are: freq, bandwidth = channel width, e.g., "1GHz", etime = exposure time / length of track, e.g., "500sec", integration = scan time, e.g., "10sec", elevation, e.g., "80deg"; either an antennalist (a simobserve-format antenna configuration filename) must be given or the parameters telescope, diam, and nant (number of antennas) must be set. Other optional inputs include: pwv in mm, doimnoise uses the simulator task sm.corrupt to create an MS and image it to measure the noise, integration or integration time (units required) e.g., "10s", debug, method which is equivalent to the mode parameter in the simulator task sm.setnoise (options: "tsys-atm" (default) or "tsys-manual"), tau0 or the zenith atmospheric opacity (must be set if method="tsys-manual"), and t_sky (default=200 (K) when method="tsys-manual").


Geodesy and Antenna Positions

NOTE: For more information on geodesy and pointing and other helper functions that are useful and available, click here.

The ITRF frame mentioned in several of the following tasks is not the official ITRF (International Terrestrial Reference Frame), just a right-handed Cartesian system with X going through 0 latitude and 0 longitude, and Z going through the north pole.


simutil.readantenna is a helper function to read antenna configuration files, using the antab parameter as an input. Outputs will be: earth-centered x,y,z, diameter, name, observatory_name, observatory_measure_dictionary.

NOTE: The observatory_measure_dictionary output was added between CASA 4.7 and 5.0.


When given an antenna configfile, this method will return the zenith baseline lengths.


When given an antenna configfile and freq (in GHz), this method will return the approximate beam size at zenith from the 90th percentile baseline length.


This method returns the nominal ITRF (X, Y, Z) coordinates [m] for a point at geodetic latitude (parameter lat) and longitude (parameter lon) [radians] and elevation [m]. 


When given ITRF Earth-centered (X, Y, Z, using the parameters x, y, and z) coordinates [m] for a point, this method returns geodetic latitude and longitude [radians] and elevation [m]. Elevation is measured relative to the closest point to the (latitude, longitude) on the WGS84 (World Geodetic System 1984) reference ellipsoid.


This method returns the nominal ITRF (X, Y, Z) coordinates [m] for a point at "local" (x, y, z, using the parameters locx, locy, and locz) [m] measured at geodetic latitude (lat) and longitude (longitude) [degrees] and altitude (alt) of the reference point. The "local" (x, y, z) are measured relative to the closest point on the WGS84 reference ellipsoid, with z normal to the ellipsoid and y pointing north.


Given Earth-centered ITRF (X, Y, Z, using the parameters x, y, and z) coordinates [m] and the Earth-centered coords of the center of array (using the parameters cx, cy, and cz), this method returns local (x, y, z) [m] relative to the center of the array, oriented with x and y tangent to the closest point at the COFA (latitude, longitude) on the WGS84 reference ellipsoid, with z normal to the ellipsoid and y pointing north.


Given Earth-centered ITRF (X, Y, Z) coordinates [m] and the name of an known array using the obsname parameter (see me.obslist), the method simutil.itrf2locname returns local (x, y, z) [m] relative to the center of the array, oriented with x and y tangent to the closest point at the COFA (latitude, longitude) on the WGS84 reference ellipsoid, with z normal to the ellipsoid and y pointing north.


This method returns the nominal ITRF (X, Y, Z) coordinates [m] for a point at UTM easting, northing, elevation [m], and zone of a given datum (e.g., 'WGS84') and north/south flag nors ("N" or "S", denotes northern or southern hemisphere). The ITRF frame used is not the official ITRF, just a right-handed Cartesian system with X going through 0 latitude and 0 longitude, and Z going through the north pole.  


The method simutil.utm2long converts UTM coordinates to GPS longitude and latitude (in radians). This task has the following parameters: east, north, zone, datum, and nors.


Pointing and Directions


This method is used to calculate mosaic pointings to cover a region. This returns a hexagonally packed list of pointings determined by the size (either [size[0],size[1]] or [size,size] if a single value is given) parameter separated by parameter spacing and fitting inside an area specified by direction and maptype. If multiple pointings can not be fit to the given parameters, a single pointing will be returned. If direction is a list, the task simply returns the direction and the number of pointings in it. The 3 options for maptype are: "HEX"agonal (default), "SQU"are, and "ALM"A (triangular tiling). The hexagonal packing starts with a horizontal row centered on direction, and the other rows alternate being horizontally offset by a half spacing. For hexagonal or square maptypes, the relmargin (default=0.5) parameter affects the number of pointings returned in the mosaic pattern. For triangular maptypes, the beam parameter is used to determine the number of pointings returned in the mosaic pattern, although this parameter is optional.


This method will read a pointing list from a file using the parameter filename. The input file (ASCII) should contain at least 3 fields separated by a space which specify positions with epoch, RA and Dec (in degrees/minutes/seconds or hours/minutes/seconds). The optional field and time columns should be a list of decimal numbers which specifies integration time at each position (in units of seconds). The lines which start with '#' are ignored and can be used as comment lines. Example of a file:

#Epoch     RA          DEC      TIME(optional)
 J2000 23h59m28.10 -019d52m12.35 10.0
 J2000 23h59m32.35 -019d52m12.35 10.0
 J2000 23h59m36.61 -019d52m12.35 60.0


This method will write a list of pointings out to a file (example above), given by the parameter filename. The optional parameter time can be an array of integration times.


This method will return the average of directions (default=None) as a string, and relative offsets.


This method will return the median of directions (default=None) as a string, and relative offsets.


This method calculates the elevation of a source on a given date, in a given direction, seen from a given telescope. The date should be given in the format YEAR/MO/DY/TI:ME. The time given is referenced with the International Atomic Time, or TAI (from the French name name temps atomique international). Other optional parameters include: usehourangle (boolean parameter which sets or unsets the reference time at transit, essentially centering the plot), ms (uses the information from the OBSERVATION table in the given MeasurementSet and plots the entire range of the observation), and cofa (allows the user to change the center of the array position). The cofa parameter must be set if using an unknown observatory. A list of known observatories can be found by using the measures tool command me.obslist.




This method will plot an image and calculate its statistics. Optional parameters: plot (default True), incell, disprange (low and high values for pl.imshow), bar (show colorbar, default=True), showstats (show stats on the image, default=True).


An alternate antenna configuration plotting routine that takes arrays of x,y=local offset from the array center, z=altitude, d=diameter, and name. This method routine either plots points or, if the array is compact enough to see the diameters, plots to the actual scaled size of the dishes.


simutil.modifymodel is a method that converts a model image into a 4D-coordinate image that can be used in CASA, with axes in space, stokes, spectral order, which the Toolkit requires (e.g., sm.predict in the simulator tool). The input parameters inimage and outimage allow the user to specify the names of the input and output. Values that are absent in the input, or that the user wishes to override, can be input as quantity strings with the in* parameters (inbright, indirection, incell, incenter, inwidth, innchan). e.g., inbright="4Jy/pixel" will scale outimage to have 4Jy/pixel peak, incell="0.2arcsec" will set the cell size in outimage to 0.2arcsec. The flatimage parameter allows one to also generate a flat (2D, integrated intensity) image from inimage, which can be useful for display purposes.


Given a (2D) model (modelflat) image, this method will regrid it to the scale of the outflat image, and convolve it to the beam of the outflat image. This is useful to compare a skymodel with a simulated output image. The optional parameter complist allows the user to import a componentlist to add unresolved components to the outflat image. Information on creating a component list can be found in the CASA guides here.