Simulation of cosmology

Equation 2.8 , gives us the expression of the flux of an object according to its shift towards the red. We thus can, knowing the spectral shift of our object, to calculate the flux awaited for values given of the cosmological parameters.

We chose in simulation to use cosmology `` standard '', i.e. , that determined by perlmutter1999 for a flat universe with values of $0.72$. This parameterization is only one suitability and has only influence on the shape of the lightcurve. Only total standardization is modified.

The second influence of cosmology is the redshift which results by a spectral shift and a time-scale of the lightcurve of the supernova (see chapter 2 ). These two effects will be taken into account during simulation.

Provide with cosmology, of the owner of spectrum of supernovæ of correctly standardized the Ia type and effective filters, we are able to simulate the lightcurve of a supernova given to a shift towards the red given.