frbs and serendipity matthew bailes swinburne university ......matthew bailes swinburne university...
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FRBs and Serendipity Matthew Bailes
Swinburne University of Technology
ARC Laureate Fellow
Photo: Fabian Jankowski
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FRB Discovery n 1967: Early Days (Hewish et al. 1968)
¨ Chart recorders and repeated single pulses
n 1974: Filterbanks + Computers (Hulse & Taylor 1975) ¨ FFT allowed large integration times, bandwidths
n 1982: MSPs (Backer et al. 1982) ¨ Finer filters and more computers
n 2006: RRATs (McLaughlin et al. 2006) ¨ Single pulsed “pulsars”
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Grote Reber’s Radio Data
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Classic Dutch BP diagram B-P Diagram
Millisecond Pulsars
Slow, boring Pulsars
Magnetars
Young Pulsars
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Single Pulse Hunting ‒ Nice (1999)
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Pulsar Dispersion Measures
Lyne’s rule of thumb DM sin b < ~ 45 pc/cc
Computationally
Limited
Magellanic Clouds
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The RRATs ‒ Mc Laughlin et al. 2006
Fluence – 1-15 Jy-ms Luminosity ~ 10-100 Jy kpc2
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Lorimer Burst Discovery (2007)
Motivated by RRATs Manchester et al. (2001) pulsar survey
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2007 Science paper
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The LORIMER BURST (2001 data, published in Lorimer et al. 2007)
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Old 1-bit Hardware RFI algorithm Zapped the Lorimer Burst!
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Pulsar Dispersion Measures
DM sin b < 45 pc/cc
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Doubts:
n Distance of ~300 Mpc? n Brightness ridiculously large (1010 x brighter than RRATs) n It didn’t repeat (!!!) n No-one else could find one.
¨ ATA Fly’s eye survey, Westerbork, old and new Parkes surveys – all nothing
n Where were all the fainter ones???
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Quoting Lorimer et al. (2007)
“Perhaps the most intriguing feature of this burst is its 30-Jy strength. While this has allowed us to make a convincing
case for its extraterrestrial nature, the fact that it is over 100 times our detection threshold makes its uniqueness puzzling.
Often, astronomical sources have a flux distribution that
would naturally lead to many burst detections of lower significance; such events are not observed in our data.”
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And 10 orders of magnitude brighter??
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The “Perytons”: FRB-like events, DM~375?? Burke-Spolaor et al. (2011)
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The “Keane” Burst (2012) n An FRB “in the plane” DM=746 pc/cc.
¨ Possibly galactic event? ¨ Bannister & Madsen(2014) argued against an
extra-galactic event. ¨ Not much scattering?
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HTRU Surveys
n HITRUN Surveys (Keith et al. 2010) n Employed iBOB boards with FPGAs n 1024 x 0.4 MHz channels (340 MHz usable) n 8x frequency resolution, 2-4x time resolution, 2-bit data n Aim was to slice through dispersion
¨ Find MSPs ¨ Higher DM pulsars ¨ Relativistic binaries ¨ Lorimer bursts
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Local Interference is ridiculously correlated between beams Beam 1
Beam 2 Beam 3
Kocz developed eigenvector common RFI removal algorithms
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Use common RFI to remove it
Raw
Clean
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Pulsar Dispersion Measures
DM sin b < 45 pc/cc
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Dispersion Smearing with the Andrew Lyne 3 MHz Filterbanks
n For DM = 375, smear was 3.7 milliseconds n For DM = 1000, smear was 10 milliseconds n For DM = 2500, smear was 25 milliseconds
t = 8.3us BMHz
DMpc / cc
nuGHz!
"#
$
%&−3
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HITRUN Regions
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Success! Thornton et al. (2013) bursts
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FRB 110220 – the first HTRU FRB n DM = 944 cm-3 pc; W = 5.6 ms n Evidence of scatter broadening n But 49 sigma!!! • Bright enough to fit the pulse shape as
a fn. of frequency to find dispersion & scattering indices
EMBARGOED – Thornton et al 2013 (in prep)
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Thornton FRBs n Required hires
filterbanks n Most would have
been smeared out in old filterbanks
n A new phase space was being explored
n ”Four-minute mile”
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Pulsar Dispersion Measures vs FRB DMs
DM sin b < 40 pc/cc
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The Arecibo Burst! (Spitler et al. 2014) n FRB 121102
¨ DM=557 pc/cc ¨ (BTW 557 ~ 1.5 * 375), b~0.0, l~180
n FRB 110523 DM=623 (Masui et al. 2015) ¨ 42 sigma! Large Rotation Measure? GBT! “local”?
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A GBT Burst! n FRB 110523 DM=623 (Masui et al. 2015)
¨ 42 sigma! Large Rotation Measure? Scattering, RM “perfect”
n FRBs exist at 800 MHz! But are FRBs “relatively local”?
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Kulkarni et al. (2014)’s abstract
First, the detection of a single FRB by an interferometer with a kilometer (or longer) baseline will prove that
FRBs are of extraterrestrial origin.
Second, we urge astronomers to pursue observations and understanding of Perytons since they form (at
least) a formidable foreground for the FRBs.
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The Repeating Fast Radio Burst aka “The repeater” (Spitler et al. 2016)
n The Arecibo FRB repeats!
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The repeating Fast Radio Burst (Spitler et al. 2016)
n The Arecibo FRB repeats!!! n Almost certainly a neutron
star – magnetar? ¨ Distance? ¨ Energy? ¨ Scintillation?
n Two classes?
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DM search space n Lorimer et al. DM = 375 n Burke-Spolaor & Bailes searched Edwards et al. and
Jacoby et al. surveys ¨ Max DM was 600! (missed DM > 600 FRB)
n Real-time FRB Heimdall pipeline (Jameson/Barsdell) ¨ Uses GPUs ¨ DM searched up to 1500 pc/cc ¨ Moved to 2000 pc/cc – soon found DM=1912 pc/cc! ¨ Moved to 3000 pc/cc – soon found DM=2600 pc/cc!
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SUPERB Latest Developments (1) n FRB 151206
¨ DM = 1912 pc/cc!
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Latest Developments (3)
n FRB 160102 n DM = 1912 pc/cc!
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Manisha Caleb On behalf of UTMOST collaboration
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The “MOTER” Transient Monitor
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Pulsar detections
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Molonglo FRBs!!!
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FRB Discovery n Required pulsars to be discovered first
¨ Without PSRs, instrumentation incapable of detection
n Data volume so large requires “clever algorithms” to handle it ¨ RFI rejection deleted Lorimer burst, PSR J0437-4715 ¨ DM sin b < 45 ¨ Often blinds us to new discovery space
n PKS MB receiver pivotal in FRB discovery n A proposal to search for FRBs would be rejected by any
sane time assignment committee ¨ “Theoretically impossible”