Observational data
In contrast to synthetic data, NMMA can make use of observational data both from electromagnetic and gravitational-wave observations. In order to make sure that the NMMA framework can smoothly read in and interpret observed signals, a short description of the data structure can be found below.
Electromagnetic data
Observatories provide observational data as a measured flux or as spectral flux density which needs to be converted to the AB magnitude system in order to be used within NMMA. It is important to distinguish between different spectral filters in order to run a consistent analysis. Current available filters can be checked in utils.py. A specific flux or respective magnitude measurement comes along with a specific time stamp which needs to be in the ISOT time format. For further details, see here.
Example: Some data for kilonova AT2017gfo
2017-08-18T00:00:00.000 g 17.41000 0.02000 2017-08-18T00:00:00.000 r 17.56000 0.04000 2017-08-18T00:00:00.000 i 17.48000 0.03000 2017-08-18T00:00:00.000 z 17.59000 0.03000
The first column represents the ISOT time, followed by the filter or spectral regime in the second column, the measured AB magnitude and its respective error are given in the third and fourth column. This data structure detailed above is also applicable for other astrophysical sources (SNe, GRBs) or models implemented in NMMA.
