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--- lc_generation [2022/02/11 09:45]
theoastro
+++ lc_generation [2023/06/02 17:05] (current)
theoastro
@@ Line 12: / Line 12: @@
 Note that the parameters vary from model to model - an overview can be found [[https://github.com/nuclear-multimessenger-astronomy/nmma/blob/c9f55663f27625ca7c3aa1b8d74dcb231ca060e7/nmma/em/model.py#L16|here]]. Some models such as ''Bu2019lm'' require to embed a SVD grid for light curve computation which can be found [[https://github.com/nuclear-multimessenger-astronomy/nmma/tree/main/svdmodels|here]]. With these, a light curve object can be instantiated as follows:
-  t = np.arange(tmin=0.1, tmax=20.0 ,deltat=0.1)
+  tmin=0.1
+  tmax=20.0
+  deltat=0.1
+  t = np.arange(tmin, tmax, deltat)
   lc_model = nmma.em.model.SVDLightCurveModel(model='Bu2019lm', sample_times = t, svd_path = "nmma/svdmodels/", parameter_conversion=None, mag_ncoeff=None,  lbol_ncoeff=None)
@@ Line 22: / Line 25: @@
     'inclination_EM': 0,
     'luminosity_distance': 40}
-  lbol, mag= lc_model.generate_lightcurve(t, params)
+  lbol, mag= lc_model.generate_lightcurve(t, params_range)
 Through the filter keys such as u,g,r,i,z,y,J,H,K, the light curves in different photometric bands can be obtained, e.g., using ''mag['u']''. An example plot of kilonova light curves in different photometric bands is shown below for AT2017gfo.
@@ Line 31: / Line 34: @@
 === Gamma-ray burst afterglows  ===
 In order to compute GRB afterglow light curves, NMMA uses the model ''TrPi2018'' from [[https://afterglowpy.readthedocs.io/en/latest/#|afterglowpy]]  and enables a GRB afterglow light curve generation on a fixed time grid.
-  from nmma.em import utils
+  import nmma.em.model
-  params = {
+  t_day = np.arange(1., 950., 1.)
-    'E0': 10**50.,
+  grb_model = nmma.em.model.GRBLightCurveModel(t_day, resolution=12, jetType=0)
+  params_range = {
+    'inclination_EM': 0,
+    'log10_E0': 50.,
     'thetaCore': 0.05,
     'thetaWing': 0.01,
-    'n0':10**(-4.5),
+    'log10_n0':-4.5,
     'p':2.160,
-    'epsilon_e':10**(-1.6),
+    'log10_epsilon_e':-1.6,
-    'epsilon_B':10**(-2),
+    'log10_epsilon_B':-2.,
-    'jetType': 0,
+    'luminosity_distance': 40,}
-    'specType': 0,
-    'thetaObs': 0.,
-    'xi_N': 1.0,
-    'd_L': 1.234e+26,}
-  tmin = 1.
-  tmax = 950.
-  deltat = 1.
-  t = np.arange(tmin, tmax, deltat)
-  t_day, lbol, mag_abs = utils.grb_lc(t, Ebv=0., param_dict=params)
+  lbol, mag = grb_model.generate_lightcurve(t_day, params_range)
 GRB afterglow light curves can be accessed with the filter keys ''X-ray-5keV'' and ''X-ray-1keV'', e.g. ''mag_abs['X-ray-5keV']''.
 === Shock-cooling supernovae  ===
-NMMA uses a model from [[https://arxiv.org/pdf/2007.08543|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:
+NMMA uses a model from [[https://arxiv.org/pdf/2007.08543|Piro et al. 2021]]. Following a shock breakout, the radiation of shock heated material expands and cools, known as shock cooling emission. The emission in different spectral regimes can be computed as follows:
+  t = np.arange(tmin=0.1, tmax=10., deltat=0.1)
+  sn_model = nmma.em.model.ShockCoolingLightCurveModel(sample_times = t, parameter_conversion=None, model="Piro2021")
+  params_range = {
+    'log10_Menv': 30,
+    'log10_Renv': 20,
+    'log10_Ee': 49.,
+    'luminosity_distance': 1.234e+24,}
+  lbol, mag = sn_model.generate_lightcurve(t, params_range)

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