1. Radio Emission from Embryonic Super-Luminous Supernova Remnants
Kazumi Kashiyama1
Kohta Murase2,3
1University of Tokyo
2Pennsylvania State University
3Kyoto University
Conor Omand1
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

2. Background/Motivation
Proto-NS thought to power SLSN (and other transients)
Quasi-thermal radiation can’t differentiate engines, non-thermal can (PWNe emission)
FRB localized to host galaxy similar to SLSN
Want to connect GRBs, FRB, SLSN, hypernovae, and Type Ibc SN under one model
Gal-Yam A., 2012, Sci, 337, 927
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

3. Purpose
Want to see if emission is detectable by VLA (~1 GHz) or ALMA (~100 GHz)
First, need to fit optical light curves to six previous SLSN to determine model parameters
Then, determine the radio spectra and fluxes and examine:
Time evolution
Frequency dependence
Dependence on pulsar and environmental parameters
Are detections feasible?
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

4. Model Overview
Models were previously developed: Murase+ (2015, 2016), Kashiyama+ (2016)
Six parameters, but three held constant (MNi, ESN, κ), so three free (P, B, Mej)
(P, B, Mej) are degenerate, give a family of solutions
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

5. Model Physics Pulsar spin down:
Acceleration of the ejecta by magnetized wind:
Electron acceleration, cooling, and pair cascades:
56Ni and 56Co decay:
Calibrated against analytical Arnett model
Kashiyama K. et al., 2016, ApJ, 818, 94
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

6. Results (Optical fitting)
Fitting of optical light curves
Determination of Pmax (SN2011ke)
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

7. Results (Radio emission)
Broadband Spectra
Intrinsic Light Curves
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

8. Results (Radio emission)
P = 1 ms
P = Pmax
1 GHz
100 GHz
Sept 7/2017
高エネルギー宇宙物理学研究会 2017

9. Summary
Determined pulsar and ejecta parameters for six SLSN by fitting optical light curves, and calculated radio flux.
Found that 4-6 SLSN could be visible in ALMA band after ~ 1 yr, 2-5 could be visible in VLA band after ~ 10 yrs
Progress underway to determine if dust in ejecta can produce a similar sub-mm signal
Proposal submitted to ALMA to search for this non- thermal signal in two SLSN (accepted)
Sept 7/2017
高エネルギー宇宙物理学研究会 2017