no code implementations • 8 Mar 2021 • A. Ridolfi, T. Gautam, P. C. C. Freire, S. M. Ransom, S. J. Buchner, A. Possenti, V. Venkatraman Krishnan, M. Bailes, M. Kramer, B. W. Stappers, F. Abbate, E. D. Barr, M. Burgay, F. Camilo, A. Corongiu, A. Jameson, P. V. Padmanabh, L. Vleeschower, D. J. Champion, M. Geyer, A. Karastergiou, R. Karuppusamy, A. Parthasarathy, D. J. Reardon, M. Serylak, R. M. Shannon, R. Spiewak
The other three new binary pulsars (NGC 6624G, M62G, and Ter 5 an) are in wider ($> 0. 7$ days) orbits, with companions that are likely to be white dwarfs or neutron stars.
High Energy Astrophysical Phenomena
1 code implementation • 12 Nov 2018 • V. Morello, E. D. Barr, S. Cooper, M. Bailes, S. Bates, N. D. R. Bhat, M. Burgay, S. Burke-Spolaor, A. D. Cameron, D. J. Champion, R. P. Eatough, C. M. L. Flynn, A. Jameson, S. Johnston, M. J. Keith, E. F. Keane, M. Kramer, L. Levin, C. Ng, E. Petroff, A. Possenti, B. W. Stappers, W. van Straten, C. Tiburzi
We have also introduced an outlier detection algorithm for efficient radio-frequency interference (RFI) mitigation on folded data, a new approach that enabled the discovery of pulsars previously masked by RFI.
Instrumentation and Methods for Astrophysics High Energy Astrophysical Phenomena
1 code implementation • 14 Jun 2017 • E. F. Keane, E. D. Barr, A. Jameson, V. Morello, M. Caleb, S. Bhandari, E. Petroff, A. Possenti, M. Burgay, C. Tiburzi, M. Bailes, N. D. R. Bhat, S. Burke-Spolaor, R. P. Eatough, C. Flynn, F. Jankowski, S. Johnston, M. Kramer, L. Levin, C. Ng, W. van Straten, V. Venkatraman Krishnan
We report on the observational setup, data analysis, multi-wavelength/messenger connections, survey sensitivities to pulsars and fast radio bursts and the impact of radio frequency interference.
Instrumentation and Methods for Astrophysics High Energy Astrophysical Phenomena
1 code implementation • 30 Jun 2010 • M. J. Keith, A. Jameson, W. van Straten, M. Bailes, S. Johnston, M. Kramer, A. Possenti, S. D. Bates, N. D. R. Bhat, M. Burgay, S. Burke-Spolaor, N. D'Amico, L. Levin, P. L. McMahon, S. Milia, B. W. Stappers
Installation of a digital backend allows us to record 400 MHz of bandwidth for each beam, split into 1024 channels and sampled every 64 us.
High Energy Astrophysical Phenomena Solar and Stellar Astrophysics