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"Constraining the Size of the Radio Counterpart

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Presentation on theme: ""Constraining the Size of the Radio Counterpart"— Presentation transcript:

1 "Constraining the Size of the Radio Counterpart
McGill University, June 13th 2017 "Constraining the Size of the Radio Counterpart to the Repeating FRB Gregg Hallinan, Vikram Ravi

2 The Quiescent Radio Source Associated with FRB 121102
Chatterjee et al. 2017

3 Adapted from Frail et al. 2012
Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively. Adapted from Frail et al. 2012

4 Co-located with FRBs to within ~40 pc (Marcote et al 2017)
FRBs originate from a dwarf star-forming galaxy at z~0.19 (Tendulkar et al. 2017) Radio source is offset from the light center of the galaxy (Tendulkar et al. 2017) Co-located with FRBs to within ~40 pc (Marcote et al 2017) Co-located with Hα emission (Bassa et al. 2017; Kokubo et al. 2017) Bassa et al. 2017 Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively.

5 Further developed by Metzger et al. 2017
Both Tendulkar et al and Marcote et al note the similarity of the host galaxy to the hosts of long GRBs and SLSNe-1 Further developed by Metzger et al. 2017 Unified engine for LGRBs, SLSNe-1 and FRBs – a young rapidly spinning magnetar central engine Various constraints suggest age of few decades to a century Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively.

6 Interpreting the radio emission…
A plerion embedded in the supernova remnant, powered by the magnetar Synchrotron emission from a shock formed at the interaction between the supernova ejecta and the circumstellar medium of the progenitor star The late-time, off-axis afterglow of a jet launched at the time of formation of the magnetar Model can be tested by constraining the radio emission source size Differentiate between models – e.g. plerion/afterglow vs LLAGN Constrain the age of a plerion/afterglow

7 Expected growth of plerion/afterglow
Chevalier et al. 1977, Metzger et al. 2017 Crab plerion Distance of FRB Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively.

8 Source resolved at ~2 mas at 1.7 GHz
Limits from VLBI 0.2 mas Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively. Marcote et al. 2017 Source resolved at ~2 mas at 1.7 GHz <0.2 mas at 5 GHz

9 Refractive Scintillation
Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively. Source exhibits variability in the 3 GHz light curve Both variability modulation index and time scale is consistent with refractive scintillation Confirmed by the VLBI resolving the scattering disk

10 Refractive Scintillation
ν0 = transition frequency between strong and weak scattering >38 GHz (NE2001) Θs ∝ ν-11/5 Scattering Disk size Modulation index Refractive Timescale (hours) Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively. Walker et al. 1998 See also Waxman et al. 2017

11 VLA Program Observations at X band (8-12 GHz), Ku band (12-18 GHz) and K band (18-26 GHz) Originally scheduled for D->C reconfiguration (May 15-25) Moved to C configuration – ongoing! 3 Ku band epochs completed on June 8th, 10th and 11th VLBI Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively. X band Ku band K band

12 Strategy Interleave 2 gain calibrators to assess temporal stability
Use bright in-beam source to directly constrain flux of target Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively.

13 June 8th June 10th June 11th Very preliminary… To be taken with a very large grain of salt!

14 Summary Constraining the size of the quiescent radio source associated with FRB is a powerful tool for distinguishing and constraining models Refractive scintillation may be key Observations underway from 8-25 GHz Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively.

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