Tutorials

These are optical counterparts to binary neutron star mergers generated by r-process material produced (Metzger 2017). In this framework, we use a POSSIS-based grid of kilonova models spanning the plausible binary neutron star parameter space (Dietrich et al. 2020). There are four parameters:

• the dynamical ejecta mass
• the wind ejecta mass,
• the half opening angle
• the observatoin angle

We use afterglowpy (Ryan et al. 2020), an open-source computational tool modeling forward shock synchrotron emission from relativistic blast waves as a function of jet structure and viewing angle. The model parameters are:

• the isotropic kinetic energy,
• the jet collimation angle,
• the viewing angle,
• the circumburst constant density,
• the spectral slope of the electron distribution,
• the fraction of energy imparted to the electrons by the shock,
• the fraction of energy imparted to the magnetic field,

We use a model from Piro et al. 2021. Following shock breakout, the radiation of shock heated material expands and cools, known as shock cooling emission. The model has parameters:

We rely on a few different models for supernovae from sncosmo. For example, the nugent-hyper model (Levan et al. 2005) used for SN Ib/c supernovae with the stretch and scale set to match the intrinsic (dereddened, rest frame) -band luminosity of SN 1998bw at maximum light. The main free parameter is the absolute magnitude.