FRB : A Repeating Fast Radio Burst. Laura Spitler 20. June 2016 Bonn Workshop IX

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1 FRB : A Repeating Fast Radio Burst Laura Spitler 20. June 2016 Bonn Workshop IX 1

2 Fast Radio Bursts (FRB): An Overview 17 Published Sources Parkes (15) Arecibo (1) GBT (1) Broadband radio pulses showing frequencydependent dispersion consistent with propagation through the cold, ISM. Observed widths: ~1 to 10 msec Peak flux densities: ~0.2 to 30 Jy (Lorimer et al. Science, 2007) Most discovered off the Galactic plane Observed dispersion measures (DM) greater than the maximum expected from the Galaxy. Most likely extragalactic 2

3 Dispersion: DM = D 0 n e dl t 1 t 2 DM 1 ν ν 2 2 (Credit: Jim Cordes) NE2001 is the standard model for the Galactic electron distribution Estimate of DMmax from Galaxy DMobs/DMmax ~

4 FRB : Arecibo FRB Discovered in Pulsar ALFA survey with the Arecibo Observatory using the 7-pixel L-band feed array DMobs = 558 pc cm-3 DMNE2001 = 188 pc cm-3 Near Galactic anti-center: l = 175o & b = 0o No observable pulse broadening (τd ~ 6 μsec) Spitler et al, ApJ, 2014 Positive spectral index: sidelobe detection? 4

5 Pulsar ALFA (PALFA) Survey Survey for pulsars in the Galactic plane (b<5 o ). ALFA (Arecibo L-band feed array): 7-pixel receiver, 300 MHz bandwidth Mock spectrometers Arecibo Observatory: 305 meters P. Scholz (McGill), J. W. T. Hessels (ASTRON/U of Amsterdam), S. Chatterjee (Cornell), J. M. Cordes (Cornell), V. M. Kaspi (McGill), R. S. Wharton (Cornell), S. Bogdanov (Columbia), F. Camilo (Columbia,SASKA), F. Crawford (F&M College), J. Deneva (NRL), J. van Leeuwen (ASTRON/U of Amsterdam), R. Lynch (NRAO), E. C. Madsen (McGill), M. A. McLaughlin (UWV), M. Mickaliger (Jodrell), E. Parent (McGill), C. Patel (McGill), S. M. Ransom (NRAO), A. Seymour (Arecibo), I. H. Stairs(UBC,McGill), B. W. Stappers (Jodrell), & S. P. Tendulkar (McGill) 5

6 10 new bursts discovered in follow-up observations with Arecibo Discovery burst 17 May 2015: Beam 2 2 June 2015: Beam 2 Spectral variation intrinsic Episodic No obvious periodicity Δνd ~ GHz 2 June 2015: Beam 6 (Spitler et al, Nature, 2016) 6

7 Beam positions of discovery and follow-up observations Black circles: Discovery pointing Red: Beam 0 of interleaved pointings Blue: Beams 1-6 of interleaved pointings Yellow circles: Beams with detections Dotted yellow circles: Other six beams from a pointing with a detection (Spitler et al, Nature, 2016) 7

8 (Spitler et al, Nature, 2016) 8

9 Extensive follow-up Observations new bursts detected with Arecibo in early May 40 additional hours with the VLA Scholz et al., submitted arxiv:

10 UPPI bursts Coherently dedispersed filterbanks GBT+GUPPI Bursts Scholz et al., submitted arxiv: AO+PUPPI Burst 17 10

11 UPPI bursts Coherently dedispersed filterbanks GBT+GUPPI Bursts Scholz et al., submitted arxiv: AO+PUPPI Burst 17 11

12 FWHM region of ALFA beam positions Best and conservative average position VLA 1.6 GHz Chandra No associated high energy counterpart No unmodeled Galactic emission WISE 22 μm IPHAS Hα VLA1 and VLA2 are AGN. 5σ limit is Smax = 0.3 mjy. Scholz et al., submitted arxiv:

13 What produces FRBs? Collapse of supra-massive neutron stars (Falcke & Rezzolla 2014) Merger of binary white dwarfs (Kashiyama et al 2013) Merger of two neutron stars (Hansen & Lyutikov 2001, Totani 2013) Superconducting cosmic strings (e.g. Vachaspati 2008) Evaporating primordial black holes (Rees 1977) Quark Nova (Shand et al. 2015) Black hole battery (Mingarelli, Levin, Lazio 2015) Dark matter-induced collapse of neutron stars (Fuller & Ott 2015) Magnetospheric collapse of a Kerr-Newman black hole (Liu et al. 2016) Flaring stars (e.g. Loeb et al 2013) Magnetar radio bursts (e.g. Popov 2007, 2013; Lyubarsky 2014) Supergiant pulses from NSs (e.g. Cordes and Wasserman 2016, Lyutikov 2016) Pulsar + planet (Mottez & Zarka 2014) Pulsar in asteroid field (Dai et al 2016) Mass transfer in a WD-NS system (Gu et al 2016) Non-repeating Repeating 13

14 What produces FRBs? Collapse of supra-massive neutron stars (Falcke & Rezzolla 2014) Merger of binary white dwarfs (Kashiyama et al 2013) Merger of two neutron stars (Hansen & Lyutikov 2001, Totani 2013) Superconducting cosmic strings (e.g. Vachaspati 2008) Evaporating primordial black holes (Rees 1977) Quark Nova (Shand et al. 2015) Black hole battery (Mingarelli, Levin, Lazio 2015) Dark matter-induced collapse of neutron stars (Fuller & Ott 2015) Magnetospheric collapse of a Kerr-Newman black hole (Liu et al. 2016) Flaring stars (e.g. Loeb et al 2013) Magnetar radio bursts (e.g. Popov 2007, 2013; Lyubarsky 2014) Supergiant pulses from NSs (e.g. Cordes and Wasserman 2016, Lyutikov 2016) Pulsar + planet (Mottez & Zarka 2014) Pulsar in asteroid field (Dai et al 2016) Mass transfer in a WD-NS system (Gu et al 2016) Non-repeating Repeating 14

15 Why is this the only repeater? Multiple classes? Arecibo is more sensitive Smax,FRB = mjy Smin,Parkes ~ 200 mjy (brightest 1 or 2 bursts) Re-/Non-detection rates: AO: 11 bursts in ~22 hrs Parkes: Lorimer burst 1 (~100 hrs), FRB (~78 hrs), FRB (~34 hrs) 1 Lorimer et al., Ravi, Shannon, Jameson Petroff, et al., 2015 FRB is observed through the Galactic plane Are bursts discovered out of the plane boosted by interstellar scintillations? Pulses from FRB are temporally resolved The widths of Parkes and GBT bursts can be modeled with instrumental effects and scattering 15

16 Conclusions FRB is the first FRB shown to repeat The bursts have complex spectra and pulse shapes, as well as episodic emission. No obvious periodicity seen. No high energy counterpart Deep radio, infrared, and Hα images rule out Galactic emission Rules out all models requiring a cataclysmic event -> neutron star origin 16

17 Limit on un-modeled Galactic contribution to DM VLA 1.6 GHz Deepest radio image: Excludes Galactic free-free emission Widefield Infrared Survey Explorer: No HII regions WISE 22 μm Isaac Newton Telescope Photometric Hα survey: No SNR or planetary nebula IPHAS Hα Scholz et al., submitted arxiv:

18 High energy observations 39.5 ksec observation Chandra Source 1 within best position Probability of having an unrelated x-ray source ~1. No variability seen Swift: 3 observations; no sources within 6 region Archival Swift BAT, Fermi GBM, MAXI, INTEGRAL: No hard X-ray or soft gamma-ray bursts Fermi LAT Point Source Catalog: No gamma-ray point sources Scholz et al., submitted arxiv:

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