grburgess/cosmogrb

A cosmological GRB light curve simulator. Because, why not?

status

cosmogrb

Idea

This simulates a cosmological population of GRBs in the Universe from a given space and luminosity distribution.

Light curves / lightcurves

After simulation, a realistic background and temporally evolving spectrum are created. These are then sampled at the single photon level, pushed through the detector responses, simulated with real dead time, and pushed into FITS Event files.

Cool?

import matplotlib.pyplot as plt
%matplotlib inline
from jupyterthemes import jtplot

import cosmogrb

You do not have threeML installed

Demo of Creating a GBM GRB

Instantiate the GRB with its parameters

grb = cosmogrb.GBMGRB_CPL(
    ra=312.0,
    dec=-62.0,
    z=1.0,
    peak_flux=5e-7,
    alpha=-0.66,
    ep=500.0,
    tau=2.0,
    trise=1.0,
    tdecay=1.,
    duration=80.0,
    T0=0.1,
)

Examine the latent lightcurve

time = np.linspace(0, 20, 100)

grb.display_energy_integrated_light_curve(time);

energy = np.logspace(1, 3, 100)

grb.display_energy_dependent_light_curve(time, energy, cmap='magma')

Simulate the GRB

grb.go(n_cores=6)

Save the GRB to an HDF5 file

grb.save('test_grb.h5')

Reload the GRB

grb_reload = cosmogrb.GRBSave.from_file('test_grb.h5')

fig, axes = plt.subplots(4,4,sharex=True,sharey=False,figsize=(15,15))
row=0
col = 0
for key in grb_reload.keys:
    ax = axes[row][col]
    
    lightcurve = grb_reload[key]['lightcurve']
    
    lightcurve.display_lightcurve(dt=2, ax=ax,lw=.8)
    lightcurve.display_source(ax=ax,lw=.8)
    lightcurve.display_background(ax=ax,lw=.8)
    
    if col < 3:
        col+=1
    else:
        row+=1
        col=0
    
    

fig, axes = plt.subplots(4,4,sharex=False,sharey=False,figsize=(15,15))
row=0
col = 0

for key in grb_reload.keys:
    ax = axes[row][col]
    
    lightcurve = grb_reload[key]['lightcurve']
    
    lightcurve.display_count_spectrum(tmin=0, tmax=5, ax=ax)
    lightcurve.display_count_spectrum_source(tmin=0, tmax=5, ax=ax)
    lightcurve.display_count_spectrum_background(tmin=0, tmax=5, ax=ax)

    if col < 3:
        col+=1
    else:
        row+=1
        col=0

Convert HDF5 to standard FITS files

cosmogrb.grbsave_to_gbm_fits("test_grb.h5")
!ls SynthGRB_*

SynthGRB_b0.fits      SynthGRB_n3.fits      SynthGRB_n7rsp_n7.rsp

SynthGRB_b0.rsp       SynthGRB_n3.rsp       SynthGRB_n8.fits

SynthGRB_b0rsp_b0.rsp SynthGRB_n3rsp_n3.rsp SynthGRB_n8.rsp

SynthGRB_b1.rsp       SynthGRB_n4.fits      SynthGRB_n8rsp_n8.rsp

SynthGRB_b1rsp_b1.rsp SynthGRB_n4.rsp       SynthGRB_n9.fits

SynthGRB_n0.fits      SynthGRB_n4rsp_n4.rsp SynthGRB_n9.rsp

SynthGRB_n0.rsp       SynthGRB_n5.fits      SynthGRB_n9rsp_n9.rsp

SynthGRB_n0rsp_n0.rsp SynthGRB_n5.rsp       SynthGRB_na.fits

SynthGRB_n1.fits      SynthGRB_n5rsp_n5.rsp SynthGRB_na.rsp

SynthGRB_n1.rsp       SynthGRB_n6.fits      SynthGRB_narsp_na.rsp

SynthGRB_n1rsp_n1.rsp SynthGRB_n6.rsp       SynthGRB_nb.fits

SynthGRB_n2.fits      SynthGRB_n6rsp_n6.rsp SynthGRB_nb.rsp

SynthGRB_n2.rsp       SynthGRB_n7.fits      SynthGRB_nbrsp_nb.rsp

SynthGRB_n2rsp_n2.rsp SynthGRB_n7.rsp