Spectral resolution calculator full#

The sensitivity calculator has been extended to include basic point source sensitivity and confusion estimates based on a tabulated selection of cuts in the uv domain for both bands. Failing to do so may result in flux scale errors on slightly extended emission. Since CLEAN fits the main lobe of the PSF for a restoring beam it is necessary to sufficiently taper off the long spacings when imaging to ensure that the main lobe is sufficiently Gaussian-like for the restoring step to be successful.

the MFS CLEAN implemented in DDFacet / WSClean or CASA). 2014).ġWe assume that the vast majority of our users will use variants of the CLEAN algorithm (e.g. We estimate the major axis of the restoring beam, as fitted with the WSClean imager (Offringa et al. This represents a fundamental limit to continuum detections with MeerKAT. However after sufficient integration time, depending on the beam size, the field will become dominated by confusion noise. Pure thermal noise will scale as a function of integration time. For more information, please see our pages on dynamic range and direction-dependent effects.

Spectral resolution calculator full#

Residual calibration errors do not scale with time, though a full uv track will improve the point spread function (PSF), reducing noise due to sidelobes from bright sources. The calculator therefore also offers standard imaging robust and tapering factors (see below). However, in practice, we don’t often use natural weighting, particularly for continuum point source observations where high resolution is important. Here is the number of antennas, is the total (unflagged) bandwidth available and is the total integration time on the source.