Content-type: text/html Manpage of obsrms

obsrms

Section: User Commands (1)
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NAME

obsrms - Calculate theoretical rms for telescope array observations.  

PERSON RESPONSIBLE

mchw  

CATEGORIES

image analysis  

DESCRIPTION

OBSRMS - Calculate theoretical rms for telescope array observations. The MIRIAD task TELEPAR provides typical values for Tsys and Jy/K. for several observatories.  

PARAMETERS

tsys
SSB system temperature (Kelvin). Default=300 K. Tsys includes the loss through the atmosphere.
jyperk
Antenna gain in units Jy/K. Default=150 Jy/K.
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.
lambda
wavelength in millimeters. Default=3 mm.
freq
freq (GHz) can be used to compute lambda. Default=0 GHz, uses lambda.
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
nants
Number of antennas in array. Single antenna is OK too. Default=9.
bw
Bandwidth in MHz used for continuum observations. Default=800 MHz.
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.
inttime
Total Integration time on source in minutes. Default=1 minute.
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
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.


 

Index

NAME
PERSON RESPONSIBLE
CATEGORIES
DESCRIPTION
PARAMETERS

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Time: 18:35:38 GMT, July 05, 2011