ASKAP Continuum and Polarization Data Processing Workgroup
The intention of this group is to bring together members of the ASKAP Science Data Processing (SDP) group and members of ASKAP science survey teams including EMU, POSSUM, VAST and anyone else who is interested in joining.
Our current goals are to contribute to commissioning the end-to-end ASKAPsoft pipeline and to ensure that it is meeting the needs of our early science data requirements. I encourage all survey teams to participate in this process since we are all reliant on the performance of the up-front stages of the pipeline. Use of ASKAPsoft is not mandatory, since anything we can learn about the ASKAP data and how to most effectively deal with it will be useful, but I encourage everyone to try out the end-to-end processing pipeline or at least to familiarize themselves with it here.
I will maintain a table below with candidate test data sets that I suggest we focus on. I will link each data set to its own page so we can discuss our results and compare notes.
Field Name |
SBID |
Cal SBID |
Notes |
LMC |
1997 |
1995 |
closepack36 footprint. only 30 beams ingested. A-B-C interleaving. 10+ hours. 48 MHz BW @ 1400 MHz |
CDFS |
2102 |
2099 |
square_6x6 footprint. 36 beams. A-B interleaving. 10+ hours. 48 MHz BW @ 1032 MHz |
CDFS |
2107 |
2104 |
square_6x6 footprint. 36 beams. A-B interleaving. 10+ hours. 48 MHz BW @ 1032 MHz |
I also created a directory on the Pawsey file system where we can share our imaging results, /group/astronomy856/images
And I have also compiled a list of suggested projects here:
- tuning the different steps of flagging
- summarizing / visualizing the amount of data flagged
- improving the bandpass solutions
- tuning the imaging and deconvolution parameters
- improving model image made by selavy+cmodel
- tuning the self-calibration process
- improving the linear mosaicking
- external validation, i.e., comparison with priors
- internal validation, i.e., self-consistency
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