THE PERSISTENT RADIO SOURCE ASSOCIATED WITH FRB121102 R.S. Wharton - - PowerPoint PPT Presentation

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THE PERSISTENT RADIO SOURCE ASSOCIATED WITH FRB121102 R.S. Wharton - - PowerPoint PPT Presentation

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THE PERSISTENT RADIO SOURCE ASSOCIATED WITH FRB121102 R.S. Wharton Scintillometry 2019 05 Nov 2019 L. Spitler (MPIfR), J. Cordes (Cornell), S. Chatterjee (Cornell), P . Demorest (NRAO), Bryan Butler (NRAO), Sarah Burke- Spolaor (NRAO),

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SLIDE 1

R.S. Wharton Scintillometry 2019 05 Nov 2019

  • L. Spitler (MPIfR), J. Cordes (Cornell), S. Chatterjee (Cornell),

P . Demorest (NRAO), Bryan Butler (NRAO), Sarah Burke- Spolaor (NRAO), Casey Law (Caltech), D. Michilli (McGill), J. Lazio (JPL/Caltech), G. Bower (ASIAA), ….

THE PERSISTENT RADIO SOURCE ASSOCIATED WITH FRB121102

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SLIDE 2

What are FRBs?

Two Main Strategies:

1) Population Statistics 2) Localization

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SLIDE 3

Arcsecond Localizations

What Do We Get?

  • Redshift
  • Galaxy Mass
  • Galaxy Star Formation Rate

FRB 121102 FRB 180924 FRB 190523 FRB 181112

Chatterjee et al. (2017) Bannister et al. (2019) Ravi et al. (2019) Prochaska et al. (2019)

Image from: Bassa et al. (2017)

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FRB 121102

First Arecibo FRB – Kind of interesting! First Repeating FRB –VERY interesting!

Excellent Target for Localization

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SLIDE 5

FRB 121102

More Info: realfast.io

Δ𝜄 ≈ 100 mas

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SLIDE 6

FRB 121102

“Persistent Radio Source”

  • 𝑇 ≈ 200 𝜈Jy at 3 GHz
  • Compact on mas scales
  • Some (~10%) variability

12 5:32:00 48 31:36 12:00 +33:09:00 06:00

Optical Counterpart

  • T

endulkar et al. (2017)

  • Dwarf Galaxy
  • 𝑨 = 0.193 𝐸5 = 972 Mpc
  • 𝑁∗ ∼ 10=𝑁⊙
  • 𝑇𝐺𝑆 ≈ 0.4𝑁⊙ yrCD

VLA 3 GHz

Gemini r-band

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SLIDE 7

FRB 121102

1′′

Host Galaxy

HST Imaging (Bassa et al. 2017) Offset Star Forming Region Low Metallicity Similar to SLSNe and LGRBs?

Adapted from Bassa et al. (2017)

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SLIDE 8

FRB 121102 Marcote et al. (2017)

EVN Imaging

  • 𝜄 ≤ 0.7 pc (0.2 mas at 5 GHz)
  • 𝜄 ∼ 2 − 4 mas at 1.7 GHz

Burst – PRS Separation

  • EVN+Arecibo 1.7 GHz
  • Detected 4 bursts
  • Δ𝜄 ≤ 12 mas

(Δ𝑦 ≤ 40 pc)

12 mas = 40 pc

Adapted from Marcote et al. (2017)

PRS smaller than 1 pc and coincident with FRB to 40 pc (projected)!

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SLIDE 9

FRB 121102

Michilli et al. (2018)

Michilli et al. (2018)

Measured burst RMs Found RM ∼ +10Rrad mCT Burst source resides in an extreme magneto-ionic environment

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SLIDE 10

Models

FRB Source Persistent Radio Source Magnetized Plasma

Magnetar Nebula Galactic Center (unrelated) Galactic Center (related)

Piro (2016) Metzger et al. (2017) Margalit & Metzger (2018) + more Eatough et al. (2013) Desvignes et al. (2018) Zhang (2018) Vieyro et al. (2017) Katz (2017)

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SLIDE 11

What is the PRS?

How do we differentiate models?

1) Time Evolution of Burst Properties (RM, DM, …) 2) Time Evolution of PRS Properties (flux, spectra) 3) Measure RM of PRS 4) Measure size of PRS or separation with FRB

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SLIDE 12

Time Evolution of Rotation Measure

Nebula – Margalit & Metzger (2018) GC Magnetar – Desvignes et al. (2018)

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Time Evolution of Rotation Measure

Nebula – Margalit & Metzger (2018) GC Magnetar – Desvignes et al. (2018)

Burst RMs

Decrease by ~30%

  • L. Spitler, D. Michilli,
  • J. Hessels, A. Seymour,
  • G. Hilmarsson
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SLIDE 14

Time Evolution of Dispersion Measure

Nebula – Margalit & Metzger (2018) GC Magnetar – Desvignes et al. (2018)

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SLIDE 15

Time Evolution of Dispersion Measure

Nebula – Margalit & Metzger (2018)

Burst DMs

Increases (!) by ~1%

  • L. Spitler, D. Michilli,
  • J. Hessels, A. Seymour,
  • G. Hilmarsson

GC Magnetar – Desvignes et al. (2018)

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Time Evolution of PRS Flux Density

Nebula – Margalit & Metzger (2018) Sgr A* – Macquart & Bower (2006)

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Time Evolution of PRS Flux Density

Nebula – Margalit & Metzger (2018) Sgr A* – Macquart & Bower (2006)

VLA 3 GHz

Variability ~10% 80+ hours over 2 years New Obs Soon. Will get to 4 year baseline

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SLIDE 18

Time Evolution of PRS Spectrum

Measured spectrum from 1-20 GHz on 3 epochs

Δ𝑢 = 3 days Δ𝑢 ≈ 460 days

Broadly Consistent

Bryan Butler, Sarah Burke-Spolaor, Shami Chatterjee, Jim Cordes, Paul Demorest, Joe Lazio, +

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SLIDE 19

Measure RM of PRS

Want to measure very large RM (10W rad mCT) in pretty faint source (∼ 100 𝜈Jy) Need linear pol’n of >3% VLA from 8-12 GHz 4 x 5 hr obs (3 consecutive) Work in Progress …

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SLIDE 20

Measure Size?

Margalit & Metzger (2018)

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Models

FRB Source Persistent Radio Source Magnetized Plasma

Magnetar Nebula Galactic Center (unrelated) Galactic Center (related)

Piro (2016) Metzger et al. (2017) Margalit & Metzger (2018) + more Eatough et al. (2013) Desvignes et al. (2018) Zhang (2018) Vieyro et al. (2017) Katz (2017)

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SLIDE 22

Thanks!

10 05 5:32:00 55 31:50 11:00 33:10:00 09:00 08:00 07:00