Task: obsrms Purpose: Calculate theoretical rms for telescope array observations. Categories: image analysis OBSRMS - Calculate theoretical rms for telescope array observations. The MIRIAD task TELEPAR provides typical values for Tsys and Jy/K. for several observatories. Key: tsys SSB system temperature (Kelvin). Default=300 K. Tsys includes the loss through the atmosphere. Key: jyperk Antenna gain in units Jy/K. Default=150 Jy/K. Key: antdiam Antenna diameter (m), and aperture efficiency can be used to calculate jyperk. If only one value is given then the aperture efficiency used is 0.6. Default=0,0.6 i.e. use jyperk value. Key: lambda wavelength in millimeters. Default=3 mm. Key: freq freq (GHz) can be used to compute lambda. Default=0 GHz, uses lambda. Key: theta Beamsize in arcsec. Two values may be given for the beam FWHM. If only one value is given it is used for both axes. Default=1,1 Key: nants Number of antennas in array. Single antenna is OK too. Default=9. Key: bw Bandwidth in MHz used for continuum observations. Default=800 MHz. Key: deltav Velocity resolution in km/s can be used to compute bandwidth for spectral line observations. Default=0 km/s, i.e. use bandwidth value. Key: inttime Total Integration time on source in minutes. Default=1 minute. Key: coreta Correlator efficiency factor. A perfect correlator has coreta=1. 2-, 3-, and 4-level correlators have coreta=0.64, 0.81, and 0.88 respectively. (see Thompson, Moran, and Swenson, p229). Default=0.88 Key: rmsphase RMS phase noise (degrees). Phase noise reduces the signal, effectively increasing the observed RMS noise in the data by a factor exp(rmsphase(radians)**2/2.). For strong sources atmospheric phase noise can be removed by selfcalibration. Default=0. degrees. i.e. perfect data.

Generated by miriad@atnf.csiro.au on 21 Jun 2016