The FRB Population: Observations and Theory

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1 The FRB Population: Observations and Theory Dr. Emily Petroff ASTRON Aspen Winter Conference on FRBs 12 February,

2 What do we talk about when we talk about population 26 known FRB sources 18 published, 8 unpublished Out of ~1000s occurring every day Properties of the observed population What do they tell us about FRBs? How these can constrain theory? Sources that live at the edges

3 Observational basics What do we measure? DM pulse width S/N*, (flux, fluence) scatter broadening DM index scattering index spectral index* polarization rotation measure Thornton et al.(2013) *these depend heavily on where the FRB is located in the primary beam

4 Observations guiding theory From these parameters we want: Progenitors! Emission region size? Energetics Distances, redshifts Emission mechanism Local density + B field Host galaxy IGM information Galactic effects Brightness distribution

5

6 Outline Observational constraints on theory from specific FRBs: and what these bursts can teach us re: physical properties of FRBs A new way to view the population - FRBCAT and new plotting tools Discussion

7 FRB re: Progenitors A repeating FRB! 100+ pulses seen Same DM to within a few % Pulses with varying width/structure Detected from 5 GHz GHz Localized to a host galaxy (z~ (8)) Spitler et al. 2016

8 re: Progenitors Limits: Extragalactic!! Non-cataclysmic progenitor Energy ~ erg Associated with stable radio source Located in dwarf galaxy Chatterjee et al. 2017

9 re: Progenitors No other FRBs seen to repeat Best constraints from FRB in 170 hours, FRB /110220: >50 Hours Multiple progenitors? No robust evidence for two progenitors based on any other observed parameters BUT there are differences between FRB and many others in the population: width, frequency structure Different behavior at different source ages? Observational reasons: unlucky observing times, Parkes sensitivity, caught the brightest pulses in the pulse energy distribution

10 re: Emission region size Light travel time Example: Crab nano-shot pulses 2 ns = 0.6 m light travel time Narrowest bursts give us this constraint FRB : 0.35 ms = 105 km Many other FRB pulses unresolved in width when taking scattering time into account FRB ; Ravi et al. 2016

11 re: Redshift Looking at the FRB DM excess z DM excess /1200 Very basic, lots of assumptions, for IGM after He re-ionization (z < 3) No precise relation, but some indication of path of FRB Constrain bounds of population with both high and low DM FRBs Ioka 2003

12 re: Redshift Using DM as an indicator for distance: 0.05 < z < 2.1 Heavily depends on density of progenitor region and models for DM-redshift relation Most FRBs still have DMs between 500 and 1,000 pc/ cm 3

13 re: Emission mechanism First polarization results suggest coherent emission (but we probably knew that already) FRB FRB FRB FRB

14 re: Local magnetic field Two conflicting pictures FRB High fractional linear polarization RM much higher than estimated foreground Ordered magnetic field local to progenitor or in host galaxy FRB High fractional linear polarization Low RM consistent with estimates of Galactic foreground No ordered magnetic field in addition to Galactic contribution RM may give greatest insights into local environment!

15 re: Galactic effects HTRU int HTRU high RRATs FRB follow up SUPERB P574 Total N FRBs See Shivani s talk for more on this!

16 re: Galactic effects Growing number of detections in the Galactic Plane It can take 3x or 4x the observing to find an FRB in the plane Possible explanation: scintillation boosting in Galactic halo (Macquart & Johnston 2015) could have huge implications for measured vs intrinsic values (flux, spectral index) Models must take this into account

17 re: Brightness distribution No immediately obvious correlation between DM and S/N S/N No evidence in data for standard candles DM

18 Bringing it all together Each of these parameters gives us one angle of information Need to combine all angles to get a fuller picture of the physics behind FRBs Only a handful of measurements for each parameter with such a small population of FRBs Fortunately that s about to change

19 The big bright future

20

21

22 FRBCAT: A population Petroff et al. (2016)

23 FRBCAT: A population tool Expanding the functionality of the catalogue What features would you like to see? What functionality? Feedback welcome! A quick demo!

24 Discussion Questions What if FRBs arise from multiple populations? What will the most constraining parameters be for theorists going forward? How do we describe and name this growing population? Tradeoffs of two different types of experiments to find FRBs: High volume, poor localization vs. Rare detections, precise localization Other discussion points?

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