"Constraining the Size of the Radio Counterpart

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Presentation transcript:

"Constraining the Size of the Radio Counterpart McGill University, June 13th 2017 "Constraining the Size of the Radio Counterpart to the Repeating FRB 121102 Gregg Hallinan, Vikram Ravi E-mail: gh@astro.caltech.edu

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

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

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.

Further developed by Metzger et al. 2017 Both Tendulkar et al. 2017 and Marcote et al. 2017 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.

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

Expected growth of plerion/afterglow Chevalier et al. 1977, Metzger et al. 2017 Crab plerion Distance of FRB 121102 Filled cir- cles, open triangles and squares repre- sent detected on-axis GRBs, Type II and Type Ib/c SNe respectively.

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

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

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

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

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.

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

Summary Constraining the size of the quiescent radio source associated with FRB 121102 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.