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lc_generation [2022/02/11 12:21]
theoastro 		lc_generation [2023/06/02 17:05] (current)
theoastro
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 NMMA enables to generate electromagnetic light curves in different electromagnetic regimes. For the light curve generation, the user can select among different models. The current version of NMMA includes three kilonova light curve models and enables to compute Gamma-ray burst afterglow light curves which is based on the model [[https://afterglowpy.readthedocs.io/en/latest/#|afterglowpy]] published by [[ https://arxiv.org/pdf/1909.11691|[1]]].  NMMA enables to generate electromagnetic light curves in different electromagnetic regimes. For the light curve generation, the user can select among different models. The current version of NMMA includes three kilonova light curve models and enables to compute Gamma-ray burst afterglow light curves which is based on the model [[https://afterglowpy.readthedocs.io/en/latest/#|afterglowpy]] published by [[ https://arxiv.org/pdf/1909.11691|[1]]]. 
  
-**=== Kilonovae  ===**+=== Kilonovae  ===
 For kilonova light curve generation, the following models are available in NMMA: For kilonova light curve generation, the following models are available in NMMA:
   *   ''Bu2019nsbh'' - a BH-NS model,    *   ''Bu2019nsbh'' - a BH-NS model, 
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 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: 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)   lc_model = nmma.em.model.SVDLightCurveModel(model='Bu2019lm', sample_times = t, svd_path = "nmma/svdmodels/", parameter_conversion=None, mag_ncoeff=None,  lbol_ncoeff=None)
  
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     'inclination_EM': 0,     'inclination_EM': 0,
     'luminosity_distance': 40}     '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. 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.
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 === Gamma-ray burst afterglows  === === 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.  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,     'thetaCore': 0.05,
     'thetaWing': 0.01,     'thetaWing': 0.01,
-    'n0':10**(-4.5),+    'log10_n0':-4.5,
     'p':2.160,     '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']''. 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  === === 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)
  
Last modified: le 2022/02/11 12:21

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