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lc_comb_inference [2022/05/18 13:17]
theoastro |
lc_comb_inference [2023/06/16 13:14] (current)
theoastro |
| === Example: BNS source === | === Example: BNS source === |
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| If we assume a BNS source, we can use the model ''TrPi2018'' for modelling Gamma-ray burst afterglows along with the kilonova model ''Bu2019lm''. To run a joint inference with these 2 models, we use the [[GRB211211A-data|observed data]] ''GRB211211A.txt'', an adapted [[prior-GRB211211A|prior file]] which includes prior settings for both models and the [[https://github.com/nuclear-multimessenger-astronomy/nmma/tree/main/svdmodels|SVD grid]] for the ''Bu2019lm'' kilonova model. The joint inference can be started using the command: | If we assume a BNS source, we can use the model ''TrPi2018'' for modelling Gamma-ray burst afterglows along with the kilonova model ''Bu2019lm''. To run a joint inference with these 2 models, we use the [[GRB211211A-data|observed data]] ''GRB211211A.txt'', an adapted [[prior-GRB211211A|prior file]] which includes prior settings for both models and the [[https://github.com/nuclear-multimessenger-astronomy/nmma/tree/main/svdmodels|model grid]] for the ''Bu2019lm'' kilonova model. The joint inference can be started using the command: |
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| mpiexec -np 16 light_curve_analysis --model Bu2019lm,TrPi2018 --svd-path ./ --interpolation_type sklearn_gp --outdir outdir --label GRB211211A --prior ./Bu2019lm_TrPi2018GRB211211A.prior --tmin 0.1 --tmax 14 --dt 0.1 --error-budget 1 --nlive 1024 --Ebv-max 0 --trigger-time 59559.54791666667 --data ./GRB211211A.txt --plot --filters u,g,r,i,J,K --xlim 0,14 --ylim 26,16 | mpiexec -np 16 light_curve_analysis --model Bu2019lm,TrPi2018 --svd-path /nmma/svdmodels/ --interpolation_type sklearn_gp --outdir outdir --label GRB211211A --prior ./Bu2019lm_TrPi2018GRB211211A.prior --tmin 0.01 --tmax 10 --dt 0.01 --error-budget 1 --nlive 1024 --Ebv-max 0 --trigger-time 59559.54791666667 --data ./GRB211211A.txt --plot --filters u,g,r,i,J,K --xlim 0,14 --ylim 26,16 |
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| The joint Bayesian inference using both model yields posterior samples for the source paramaters describing the kilonova and GRB afterglow and are shown below. | The joint Bayesian inference using both model yields posterior samples for the source parameters describing the kilonova and GRB afterglow. Some of the source parameter posteriors are shown below. |
| | {{:grb211211a_bns_bu2019_trpi2018.jpg}} |
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| {{:GRB211211A_BNS_Bu2019_TrPi2018.png}} | === Example: NSBH source === |
| | For the assumption that also a NSBH source could produce a signal such as GRB211211A, we use a NSBH-kilonova model ''Bu2019nsbh'' and again the model ''TrPi2018'' for modelling Gamma-ray burst afterglows. We use the same observational data and adapt the [[prior-Bunsbh-GRB211211A|prior]] setting for the ''Bu2019nsbh'' model. To run tje joint inference with these 2 models, run the command: |
| | mpiexec -np 16 light_curve_analysis --model Bu2019nsbh,TrPi2018 --svd-path /nmma/svdmodels/ --interpolation_type sklearn_gp --outdir outdir --label GRB211211A_NSBH --prior ./Bu2019nsbh_TrPi2018_GRB211211A.prior --tmin 0.01 --tmax 10 --dt 0.01 --error-budget 1 --nlive 1024 --Ebv-max 0 --trigger-time 59559.54791666667 --data ./GRB211211A.txt --plot --filters u,g,r,i,J,K --xlim 0,14 --ylim 26,16 |
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| === Example: NSBH source === | |
| source: kilonova analyzed with Bu2019lm and GRB afterglow anaylzed with TrPi2018 | |
