We propose a deep search for the X-ray and radio afterglow of the kilonova (KN) associated with the binary neutron star merger GW170817 at t>1500 days. The primary scientific objective is to constrain the physical properties of the fastest KN ejecta. UV-Optical-NIR observations of the KN are not useful to this aim as these wavelengths are dominated by thermal emission from the slowest KN material. Coordinated Chandra and VLA observations at t=1500-2000 days hold the key to reveal the emergence of non-thermal radiation from the KN afterglow, which tracks the fastest KN material as it decelerates into the ambient gas and provides crucial information on the still-debated merger dynamics.
|Effective start/end date||1/25/21 → 1/24/24|
- Smithsonian Astrophysical Observatory (GO1-22075X//NAS8-03060)
- National Aeronautics and Space Administration (GO1-22075X//NAS8-03060)
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