A SEARCH FOR FAST RADIO BURSTS WITH THE GBNCC SURVEY. PRAGYA CHAWLA McGill University (On Behalf of the GBNCC Collaboration)
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1 A SEARCH FOR FAST RADIO BURSTS WITH THE GBNCC SURVEY PRAGYA CHAWLA McGill University (On Behalf of the GBNCC Collaboration)
2 P. Chawla 1, V. M. Kaspi 1, A. Josephy 1, K. M. Rajwade 2, D. R. Lorimer 2,3, A. M. Archibald 4, M. E. DeCesar 5, J. W. T. Hessels 4,6, D. L. Kaplan 7, C. Karako-Argaman 1, V. I. Kondratiev 4,8, L. Levin 9, R. S. Lynch 3, M. A. McLaughlin 2, S. M. Ransom 10, M. S. E. Roberts 11, I. H. Stairs 12, K. Stovall 13, J. K. Swiggum 7 and J. van Leeuwen 4,6 1 Department of Physics & McGill Space Institute, McGill University 2 Department of Physics and Astronomy, West Virginia University 3 National Radio Astronomy Observatory, Green Bank 4 ASTRON, the Netherlands Institute for Radio Astronomy 5 Department of Physics, Lafayette College 6 Anton Pannekoek Institute for Astronomy, University of Amsterdam 7 Department of Physics, University of Wisconsin-Milwaukee 8 Astro Space Center, Lebedev Physical Institute, Russian Academy of Sciences 9 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester 10 National Radio Astronomy Observatory, Charlottesville 11 New York University, Abu Dhabi 12 Department of Physics and Astronomy, University of British Columbia 13 National Radio Astronomy Observatory, Socorro 2017, ApJ, Submitted, arxiv:
3 LOW-FREQUENCY SEARCHES FOR FRBs All known FRBs have been detected at frequencies > 700 MHz. Scattering, spectral index and free-free absorption could be possible reasons for non-detection at low frequencies. Low-frequency surveys with LOFAR, MWA and Arecibo have not resulted in any detections. 3
4 THE GBNCC PULSAR SURVEY Operates at 350 MHz with a bandwidth of 100 MHz. Conducted using the 100-m diameter Green Bank Telescope. The analysis pipeline (Stovall et al. 2014) based on PRESTO (Ransom 2001) includes: RFI Removal Dedispersion Single Pulse Search GBNCC Survey Parameters Sampling Time Integration Time Gain System Temperature Bandwidth Number of Freq. Channels Channel Bandwidth θ FWHM μs 120 s 2 K/Jy 23 K 100 MHz MHz 36 arcmin Sky Coverage δ > -40 4
5 SURVEY OBSERVATIONS Maximum DM for FRB search = 3000 pc cm -3 (for pointings). GBNCC Pointings Searched to DM = 3000 pc cm pointings searched to a DM of 500 pc cm -3 have maximum Galactic DM along LOS < 100 pc cm -3. Total observing time for all pointings = 84 days. 5
6 SURVEY OBSERVATIONS Maximum DM for FRB search = 3000 pc cm -3 (for pointings). GBNCC Pointings Searched to DM = 500 pc cm pointings searched to a DM of 500 pc cm -3 have maximum Galactic DM along LOS < 100 pc cm -3. Total observing time for all pointings = 84 days. 6
7 THE SEARCH FOR FRBs Single pulse events at DM > 2 DM MW were processed with the grouping and rating algorithm, RRATtrap. All GBNCC Pointings Searched for FRBs RRATtrap (Karako-Argaman et al. 2015) was developed to detect Rotating RAdio Transients (RRATs). Enabled discovery of 10 new RRATs in GBNCC data. RRATtrap output was inspected and no FRBs were detected. 7
8 CALCULATION OF FRB RATE Assuming Poisson statistics, field of view = 0.41 sq. deg for the GBT beam and a threshold flux density of 0.63 Jy for a pulse of intrinsic width = 5 ms. We place a 95% confidence upper limit on FRB rate = 3.6 x 10 3 FRBs sky -1 day -1 at 350 MHz. 8
9 CONSTRAINING SPECTRAL INDICES OF FRBs Assuming a power-law flux density model for FRBs: Varying the index γ of the log N log S function of the FRB population (γ = 0.8, 1.2 and 1.5) such that: Performing Monte Carlo simulations of FRB flux density distribution consistent with the 1.4-GHz rate estimate reported for the Parkes surveys by Crawford et al. (2016) (3.3 x 10 3 FRBs sky -1 day -1 ) 9
10 ABSENCE OF SCATTERING AND FREE-FREE ABSORPTION Generate 1.4-GHz flux density distribution (γ = 0.8, 1.2 or 1.5) Scale distribution to 350 MHz by sampling α from a normal distribution (σ = 0.5) Compute 350-MHz FRB rate above S = 0.63 Jy from the resulting distribution For constraining spectral index, α lim, computed 350-MHz FRB rate = 95% confidence GBNCC upper limit γ α lim
11 SCATTERING Generate 1.4-GHz flux density distribution Scale distribution to 350 MHz by sampling α from a normal distribution Assign t scatt drawn from a lognormal distribution to each detectable FRB (S > 0.65 Jy) Is t scatt for all FRBs > 100 ms? TRUE Increase mean of lognormal dist. FALSE Mean scattering time for spectral index α = mean of lognormal dist. Given the observed range of scattering times and FRB rate, R, at 1.4 GHz, γ α lim
12 PREDICTING FRB DETECTION RATES FOR OTHER SURVEYS Based on flux density distribution consistent with 1.4- GHz rate estimate for Parkes surveys. Distribution scaled to each survey s center freq. by sampling α from a normal distribution. Scattering time for each FRB drawn from a lognormal distribution. 12
13 PREDICTING FRB DETECTION RATES FOR OTHER SURVEYS Based on flux density distribution consistent with 1.4- GHz rate estimate for Parkes surveys. Distribution scaled to each survey s center freq. by sampling α from a normal distribution. Scattering time for each FRB drawn from a lognormal distribution. γ =
14 PREDICTING FRB DETECTION RATES FOR OTHER SURVEYS Limits on bursts per hour arise because of range of spectral indices considered (α lim < α < +2). No free-free absorption assumed. γ =
15 PREDICTING FRB DETECTION RATES FOR OTHER SURVEYS Predictions consistent with upper limits reported for FRB searches with MWA (Tingay et al. 2015, Rowlinson et al. 2016), LOFAR (Coenen et al. 2014, Karastergiou et al. 2016), AO327 (Deneva et al. 2016) and UTMOST (Caleb et al. 2016). γ =
16 SUMMARY No FRBs were detected in GBNCC pointings amounting to a total observing time of 84 days. We place a 95% confidence upper limit on the FRB rate of 3.6 x 10 3 FRBs sky -1 day -1 above 0.63 Jy at 350 MHz. Non-detection with GBNCC is consistent with 1.4-GHz rate estimate for α > in the absence of scattering and free-free absorption and α > -0.3 in the presence of scattering, for γ = 1.5. We predict CHIME to detect 3-54 bursts per day assuming the Crawford et al. rate estimate, for γ =
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