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Sarod Yatawatta 2018-02-06 13:52:54 +01:00
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README.md
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@ -7,19 +7,19 @@ Warning: this file may be obsolete. use sagecal -h to see up-to-date options.
## Step by Step Introduction:
1a)Calibrate data in the standard way using BBS/CASA or anything else.
###1a)Calibrate data in the standard way using BBS/CASA or anything else.
Use NDPP to average the data in your MS to a few channels (also average in time to about 10sec). Also flag any spikes in the data.
1b)For subtraction of the ATeam from raw data (CasA,CygA,...), no initial calibration is necessary. Just run sagecal on raw data, but it is better to scale the sky model to match the apparent flux of the sources that are being subtracted.
###1b)For subtraction of the ATeam from raw data (CasA,CygA,...), no initial calibration is necessary. Just run sagecal on raw data, but it is better to scale the sky model to match the apparent flux of the sources that are being subtracted.
2) Sky Model:
3a)Make an image of your MS (using ExCon/casapy).
##2) Sky Model:
###2a)Make an image of your MS (using ExCon/casapy).
Use Duchamp to create a mask for the image. Use buildsky to create a sky model. (see the README file on top level directory). Also create a proper cluster file.
Special options to buildsky: -o 1 (NOTE: not -o 2)
Alternatively, create these files by hand according to the following formats.
2b)Cluster file format:
###2b)Cluster file format:
cluster_id chunk_size source1 source2 ...
e.g.
@ -30,26 +30,26 @@ Note: putting -ve values for cluster_id will not subtract them from data.
chunk_size: find hybrid solutions during one solve run. Eg. if -t 120 is used
to select 120 timeslots, cluster 0 will find a solution using the full 120 timeslots while cluster 2 will solve for every 120/3=40 timeslots.
2c)Sky model format:
#name h m s d m s I Q U V spectral_index RM extent_X(rad) extent_Y(rad) pos_angle(rad) freq0
###2c)Sky model format:
\#name h m s d m s I Q U V spectral_index RM extent_X(rad) extent_Y(rad) pos_angle(rad) freq0
or
#name h m s d m s I Q U V spectral_index1 spectral_index2 spectral_index3 RM extent_X(rad) extent_Y(rad) pos_angle(rad) freq0
\#name h m s d m s I Q U V spectral_index1 spectral_index2 spectral_index3 RM extent_X(rad) extent_Y(rad) pos_angle(rad) freq0
e.g.
P1C1 0 12 42.996 85 43 21.514 0.030498 0 0 0 -5.713060 0 0 0 0 115039062.0
P5C1 1 18 5.864 85 58 39.755 0.041839 0 0 0 -6.672879 0 0 0 0 115039062.0
#A Gaussian mjor,minor 0.1375,0.0917 deg diameter -> radius(rad), PA 43.4772 deg (-> rad)
#Position Angle: "West from North (counter-clockwise)" (0 deg = North, 90 deg = West).
#Note: PyBDSM and BBS use "North from East (counter-clockwise)" (0 deg = East, 90 deg = North).
\#A Gaussian mjor,minor 0.1375,0.0917 deg diameter -> radius(rad), PA 43.4772 deg (-> rad)
\#Position Angle: "West from North (counter-clockwise)" (0 deg = North, 90 deg = West).
\#Note: PyBDSM and BBS use "North from East (counter-clockwise)" (0 deg = East, 90 deg = North).
G0 5 34 31.75 22 00 52.86 100 0 0 0 0.00 0 0.0012 0.0008 -2.329615801 130.0e6
#A Disk radius=0.041 deg
\#A Disk radius=0.041 deg
D01 23 23 25.67 58 48 58 80 0 0 0 0 0 0.000715 0.000715 0 130e6
#A Ring radius=0.031 deg
\#A Ring radius=0.031 deg
R01 23 23 25.416 58 48 57 70 0 0 0 0 0 0.00052 0.00052 0 130e6
#A shapelet ('S3C61MD.fits.modes' file must be in the current directory)
\#A shapelet ('S3C61MD.fits.modes' file must be in the current directory)
S3C61MD 2 22 49.796414 86 18 55.913266 0.135 0 0 0 -6.6 0 1 1 0.0 115000000.0
@ -69,7 +69,7 @@ p3=q3/ln(10)^2
...
3)Run sagecal
##3)Run sagecal
Optionally: Make sure your machine has (1/2 working NVIDIA GPU cards or Intel Xeon Phi MICs) to use sagecal.
Recommended usage: (with GPUs)
@ -93,7 +93,7 @@ Eg. If you need to ignore cluster ids '-1', '10', '999', create a text file :
and use it as the 'ignore_file'.
4)Distributed calibration
##4)Distributed calibration
Use mpirun to run sagecal-mpi, example:
mpirun -np 11 -hostfile ./machines --map-by node --cpus-per-proc 8
@ -116,7 +116,7 @@ Note: the number of slaves (-np option) can be lower than the number of MS calib
The rest of the options are similar to sagecal.
5)Solution format
##5)Solution format
All SAGECal solutions are stored as text files. Lines starting with '#' are comments.
The first non-comment line includes some general information, i.e.
freq(MHz) bandwidth(MHz) time_interval(min) stations clusters effective_clusters