Radio Emission from Embryonic Super-Luminous Supernova Remnants Kazumi Kashiyama1 Kohta Murase2,3 1University of Tokyo 2Pennsylvania State University 3Kyoto University Conor Omand1 http://www.councilchronicle.com/gamma-ray-pulsar-was-found-in-tarantula-nebula/22702/ Sept 7/2017 高エネルギー宇宙物理学研究会 2017

Background/Motivation Proto-NS thought to power SLSN (and other transients) Quasi-thermal radiation can’t differentiate engines, non-thermal can (PWNe emission) FRB 121102 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

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? http://images.nrao.edu/583 http://images.nrao.edu/Telescopes/VLA/307 Sept 7/2017 高エネルギー宇宙物理学研究会 2017

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

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

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

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

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

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