2014
DOI: 10.1093/mnras/stu1368
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Abstract: Astronomical widefield imaging of interferometric radio data is computationally expensive, especially for the large data volumes created by modern non-coplanar many-element arrays. We present a new widefield interferometric imager that uses the w-stacking algorithm and can make use of the w-snapshot algorithm. The performance dependencies of CASA's wprojection and our new imager are analysed and analytical functions are derived that describe the required computing cost for both imagers. On data from the Murchi… Show more

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Cited by 655 publications
(451 citation statements)
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“…No self‐calibration was performed on this data set. The full‐bandwidth data (30.72MHz) were then imaged and deconvolved using the WSCLEAN algorithm [ Offringa et al , ] to yield images of size 3072 × 3072 pixels, the pixel size being 0.75 . The data were CLEANed up to a maximum of 20,000 iterations.…”
Section: Methodsmentioning
confidence: 99%
“…No self‐calibration was performed on this data set. The full‐bandwidth data (30.72MHz) were then imaged and deconvolved using the WSCLEAN algorithm [ Offringa et al , ] to yield images of size 3072 × 3072 pixels, the pixel size being 0.75 . The data were CLEANed up to a maximum of 20,000 iterations.…”
Section: Methodsmentioning
confidence: 99%
“…Two rounds of self-calibration were then performed on the target scan, the first using a model from the TIFR GMRT Sky Survey (TGSS) Alternative Data Release (TGSS ADR, 9 Intema et al 2017). Multiscale imaging with Briggs 1.0 weighting was then performed using the WSClean tool (Offringa et al 2014). The subband with a central frequency of 150 MHz was flux calibrated using the integrated flux density measurements of point sources from the TGSS ADR.…”
Section: Radio Observationsmentioning
confidence: 99%
“…Much of the raw data processing for this work made use of custom software developed for use with the MWA. These include the algorithm AOFLAGGER for removing radio frequency interference [ Offringa et al , ] and the imaging algorithm WSCLEAN [ Offringa et al , ]. Details of the reduction process for data taken on the 26th and 28th can be found in Loi et al [] and A. Rowlinson et al (Limits on FRBs and other transient sources at 182 MHz using the Murchison Widefield Array, submitted to Monthly Notices of the Royal Astronomical Society , 2015), respectively, which describe the procedure for generating the final total intensity images that we analyze in the current work.…”
Section: Methodsmentioning
confidence: 99%