CALIM 2011

Session

Calibration 2of2

26 Jul 2011, 08:00

Lovell seminar room 3.225 (SPDO, University of Manchester)

14. Single dish polarization calibration results using KAT-7

Dr Mattieu de Villiers (SKA SA)

26/07/2011, 08:00

This presentation will show early single dish polarization calibration results using KAT-7. Two methods of observation, namely radial and raster scans, are compared. Direction dependent beam pattern results as well as on-axis calibration solutions for leakages will be shown.

15. Fringe Fitting in Casa

Mr Stephen Bourke (JIVE)

26/07/2011, 08:40

In general, VLBI networks need to calibrate with additional terms over complex gain, namely, delay and rate. This type of calibration, known as fringe fitting has also been found beneficial and in some cases necessary with interferometers other then traditional VLBI networks. The use of AIPS for fringe fitting is well established however many of the new or upgraded telescopes use the...

18. Next-generation calibration: John Q. Astronomer's perspective

Dr Heywood Ian (University of Oxford)

26/07/2011, 09:20

The reduction, calibration and imaging of data from the SKA and its pathfinders will necessarily be automated on dedicated high-performance computing facilities instead of manual operations performed on the desktop PC of the lucky astronomer, as has been the story so far. This is already partially realised by the LOFAR project which offers observers and analysts access to a dedicated data...

20. Solving for primary beams, pointing errors, and The Westerbork Wobble

Dr Oleg Smirnov (ASTRON)

26/07/2011, 10:20

I will present recent results on dealing with beam-related DDEs and the associated calibration artefacts in WSRT data. An algorithm conceptually similar to pointing selfcal, but amenable to any kind of beamshape (including empirical beamshapes specified as e.g. FITS files), and able to solve for parameters of the primary beam, has been implemented in MeqTrees. This has been applied to a...

35. Complex Factor Analysis

Mr Ahmad Mouri Sardarabadi (Delft University of Technology)

26/07/2011, 11:00

Many techniques for array processing assume either that the system has a calibrated array or that the noise covariance matrix is known. If the noise covariance matrix is unknown, training or other calibration techniques are used to find it. Here another approach to the problem of unknown noise covariance is presented. The factor analysis (FA) model is used to model the data. In order to...