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>1000 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=1000-2000 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||12/14/20 → 12/13/22|
- Smithsonian Astrophysical Observatory (GO0-21066X//NAS8-03060)
- National Aeronautics and Space Administration (GO0-21066X//NAS8-03060)