no code implementations • 9 Dec 2020 • F. Jankowski, M. Berezina, B. W. Stappers, E. D. Barr, M. C. Bezuidenhout, M. Caleb, L. N. Driessen, M. Malenta, V. Morello, K. M. Rajwade, S. Sanidas, M. P. Surnis
Rapid data processing is essential for us to be able to retain high-resolution data of the bursts, to localise them, and to minimise the delay for follow-up observations.
Instrumentation and Methods for Astrophysics High Energy Astrophysical Phenomena
1 code implementation • 31 Mar 2020 • Devansh Agarwal, D. R. Lorimer, M. P. Surnis, X. Pei, A. Karastergiou, G. Golpayegani, D. Werthimer, J. Cobb, M. A. McLaughlin, S. White, W. Armour, D. H. E. MacMahon, A. P. V. Siemion, G. Foster
Depending on the observing mode, this translates to peak flux sensitivities in the range 0. 14--0. 89~Jy.
Instrumentation and Methods for Astrophysics
