Commit cf92aab30bc49c80ce3b5315b2b7194204be64d6
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src/idl/dustem_fit_sed_polsed_readme.pro
| ... | ... | @@ -42,12 +42,13 @@ PRO dustem_fit_sed_polsed_readme,postcript=postcript,mode=mode,help=help |
| 42 | 42 | ; Contact J.-Ph. Bernard (Jean-Philippe.Bernard@cesr.fr) in case of problems. |
| 43 | 43 | ;- |
| 44 | 44 | |
| 45 | - | |
| 46 | 45 | IF keyword_set(help) THEN BEGIN |
| 47 | 46 | doc_library,'dustem_fit_sed_polsed_readme' |
| 48 | 47 | goto,the_end |
| 49 | 48 | ENDIF |
| 50 | 49 | |
| 50 | +dustem_define_la_common | |
| 51 | + | |
| 51 | 52 | ;=== initialise dustem |
| 52 | 53 | ;dustem_init,mode='COMPIEGNE_ETAL2010',/pol |
| 53 | 54 | use_mode='G17_MODELA' | ... | ... |
src/idl/dustem_fit_sed_readme.pro
| ... | ... | @@ -152,30 +152,29 @@ CASE use_model OF |
| 152 | 152 | ;ORIGINAL LINES |
| 153 | 153 | |
| 154 | 154 | ;parameter description of parameters to be fitted |
| 155 | -; pd = [ $ | |
| 156 | -; '(*!dustem_params).gas.G0', $ ;G0 | |
| 157 | -; 'dustem_create_continuum_2', $ ;intensity of NIR continuum | |
| 158 | -; | |
| 159 | -; ;'!dustem_isrf_star_add[0].distance', $ ;distance of first stellar contribution to ISRF | |
| 160 | -; '!dustem_isrf_star_add[0].amplitude', $ ;amplitude of first stellar contribution to ISRF | |
| 161 | -; '(*!dustem_params).grains(0).mdust_o_mh',$ ;PAH0 mass fraction | |
| 162 | -; '(*!dustem_params).grains(1).mdust_o_mh',$ ;PAH1 mass fraction | |
| 163 | -; '(*!dustem_params).grains(2).mdust_o_mh', $ ;amCBEx | |
| 164 | -; '(*!dustem_params).grains(3).mdust_o_mh', $ ;amCBEx | |
| 165 | -; '(*!dustem_params).grains(4).mdust_o_mh' $ | |
| 166 | -; ] | |
| 167 | -; ;initial parameter values for parameters to be fitted | |
| 168 | -; iv = [ $ | |
| 169 | -; 1.0, $ | |
| 170 | -; 0.002, $ ;intensity of NIR continuum | |
| 171 | -; ;0.003, $ ;distance of first stellar contribution to ISRF | |
| 172 | -; 1.e-3, $ ;amplitude of first stellar contribution to ISRF | |
| 173 | -; 7.8e-4, $ ;mass fraction of PAH0 | |
| 174 | -; 7.8e-4, $ ;mass fraction of PAH1 | |
| 175 | -; 1.65e-4, $ ;mass fraction of amCBEx | |
| 176 | -; 1.45e-3, $ ;mass fraction of amCBEx | |
| 177 | -; 7.8e-3 $ ;mass fraction of | |
| 178 | -; ] | |
| 155 | + pd = [ $ | |
| 156 | + '(*!dustem_params).gas.G0', $ ;G0 | |
| 157 | + 'dustem_create_continuum_2', $ ;intensity of NIR continuum | |
| 158 | + ;'!dustem_isrf_star_add[0].distance', $ ;distance of first stellar contribution to ISRF | |
| 159 | + ;'!dustem_isrf_star_add[0].amplitude', $ ;amplitude of first stellar contribution to ISRF | |
| 160 | + '(*!dustem_params).grains(0).mdust_o_mh',$ ;PAH0 mass fraction | |
| 161 | + '(*!dustem_params).grains(1).mdust_o_mh',$ ;PAH1 mass fraction | |
| 162 | + '(*!dustem_params).grains(2).mdust_o_mh', $ ;amCBEx | |
| 163 | + '(*!dustem_params).grains(3).mdust_o_mh', $ ;amCBEx | |
| 164 | + '(*!dustem_params).grains(4).mdust_o_mh' $ | |
| 165 | + ] | |
| 166 | + ;initial parameter values for parameters to be fitted | |
| 167 | + iv = [ $ | |
| 168 | + 1.0, $ | |
| 169 | + 0.002, $ ;intensity of NIR continuum | |
| 170 | + ;0.003, $ ;distance of first stellar contribution to ISRF | |
| 171 | + ;1.e-3, $ ;amplitude of first stellar contribution to ISRF | |
| 172 | + 7.8e-4, $ ;mass fraction of PAH0 | |
| 173 | + 7.8e-4, $ ;mass fraction of PAH1 | |
| 174 | + 1.65e-4, $ ;mass fraction of amCBEx | |
| 175 | + 1.45e-3, $ ;mass fraction of amCBEx | |
| 176 | + 7.8e-3 $ ;mass fraction of | |
| 177 | + ] | |
| 179 | 178 | |
| 180 | 179 | ;NEW LINES |
| 181 | 180 | |
| ... | ... | @@ -199,59 +198,59 @@ CASE use_model OF |
| 199 | 198 | ; '(*!dustem_params).grains(4).mdust_o_mh' $ |
| 200 | 199 | ; ] |
| 201 | 200 | |
| 202 | - pd = [ $ | |
| 203 | - ;'(*!dustem_params).G0', $ ;G0 | |
| 204 | - '(*!dustem_params).grains(0).mdust_o_mh',$ ;PAH0 mass fraction | |
| 205 | - '(*!dustem_params).grains(1).mdust_o_mh',$ ;PAH1 mass fraction | |
| 206 | - '(*!dustem_params).grains(2).mdust_o_mh', $ ;amCBEx | |
| 207 | - '(*!dustem_params).grains(3).mdust_o_mh', $ ;amCBEx | |
| 208 | - '(*!dustem_params).grains(4).mdust_o_mh', $ | |
| 209 | - ;'dustem_create_continuum_2', $ ;intensity of NIR continuum | |
| 210 | - 'dustem_create_stellar_population_O63',$ ; distance to the O6 stellar population | |
| 201 | + ; pd = [ $ | |
| 202 | + ; ;'(*!dustem_params).G0', $ ;G0 | |
| 203 | + ; '(*!dustem_params).grains(0).mdust_o_mh',$ ;PAH0 mass fraction | |
| 204 | + ; '(*!dustem_params).grains(1).mdust_o_mh',$ ;PAH1 mass fraction | |
| 205 | + ; '(*!dustem_params).grains(2).mdust_o_mh', $ ;amCBEx | |
| 206 | + ; '(*!dustem_params).grains(3).mdust_o_mh', $ ;amCBEx | |
| 207 | + ; '(*!dustem_params).grains(4).mdust_o_mh', $ | |
| 208 | + ; ;'dustem_create_continuum_2', $ ;intensity of NIR continuum | |
| 209 | + ; 'dustem_create_stellar_population_O63',$ ; distance to the O6 stellar population | |
| 211 | 210 | |
| 212 | - ;'dustem_create_stellar_population_O64',$ ; amplitude of the O6 stellar population | |
| 211 | + ; ;'dustem_create_stellar_population_O64',$ ; amplitude of the O6 stellar population | |
| 213 | 212 | |
| 214 | - ;'dustem_create_stellar_population_O65',$ ; number of stars of the O6 stellar population | |
| 215 | - 'dustem_create_stellar_population_B43'$ ; distance to the B4 stellar population | |
| 213 | + ; ;'dustem_create_stellar_population_O65',$ ; number of stars of the O6 stellar population | |
| 214 | + ; 'dustem_create_stellar_population_B43'$ ; distance to the B4 stellar population | |
| 216 | 215 | |
| 217 | - ;;'dustem_create_stellar_population_B44',$ ; amplitude of the B4 stellar population | |
| 216 | + ; ;;'dustem_create_stellar_population_B44',$ ; amplitude of the B4 stellar population | |
| 218 | 217 | |
| 219 | - ;'dustem_create_stellar_population_B45'$ ; number of stars of the B4 stellar population | |
| 220 | - ] | |
| 218 | + ; ;'dustem_create_stellar_population_B45'$ ; number of stars of the B4 stellar population | |
| 219 | + ; ] | |
| 221 | 220 | |
| 222 | 221 | |
| 223 | 222 | ;initial parameter values for parameters to be fitted |
| 224 | -; iv = [ $ | |
| 225 | -; 1., $ ;G0 | |
| 226 | -; 7.8e-4, $ ;mass fraction of PAH0 | |
| 227 | -; 7.8e-4, $ ;mass fraction of PAH1 | |
| 228 | -; 1.65e-4, $ ;mass fraction of amCBEx | |
| 229 | -; 1.45e-3, $ ;mass fraction of amCBEx | |
| 230 | -; 7.8e-3, $ ;mass fraction of big grains? | |
| 231 | -; 0.002, $ ;intensity of NIR continuum | |
| 232 | -; 10.,$ | |
| 233 | -; ;;1.,$ | |
| 234 | -; 1.,$ | |
| 235 | -; 10.,$ | |
| 236 | -; ;;1.,$ | |
| 237 | -; 1.$ | |
| 238 | -; ] | |
| 223 | + ; iv = [ $ | |
| 224 | + ; 1., $ ;G0 | |
| 225 | + ; 7.8e-4, $ ;mass fraction of PAH0 | |
| 226 | + ; 7.8e-4, $ ;mass fraction of PAH1 | |
| 227 | + ; 1.65e-4, $ ;mass fraction of amCBEx | |
| 228 | + ; 1.45e-3, $ ;mass fraction of amCBEx | |
| 229 | + ; 7.8e-3, $ ;mass fraction of big grains? | |
| 230 | + ; 0.002, $ ;intensity of NIR continuum | |
| 231 | + ; 10.,$ | |
| 232 | + ; ;;1.,$ | |
| 233 | + ; 1.,$ | |
| 234 | + ; 10.,$ | |
| 235 | + ; ;;1.,$ | |
| 236 | + ; 1.$ | |
| 237 | + ; ] | |
| 239 | 238 | ; |
| 240 | 239 | |
| 241 | - iv = [ $ | |
| 242 | - 7.8e-4, $ ;mass fraction of PAH0 | |
| 243 | - 7.8e-4, $ ;mass fraction of PAH1 | |
| 244 | - 1.65e-4, $ ;mass fraction of amCBEx | |
| 245 | - 1.45e-3, $ ;mass fraction of amCBEx | |
| 246 | - 7.8e-3, $ ;mass fraction of big grains? | |
| 247 | - ;0.002, $ ;intensity of NIR continuum | |
| 248 | - 10.,$ | |
| 249 | - ;;1.,$ | |
| 250 | - ;1.,$ | |
| 251 | - 10.$ | |
| 252 | - ;;1.,$ | |
| 253 | - ;1.$ | |
| 254 | - ] | |
| 240 | + ; iv = [ $ | |
| 241 | + ; 7.8e-4, $ ;mass fraction of PAH0 | |
| 242 | + ; 7.8e-4, $ ;mass fraction of PAH1 | |
| 243 | + ; 1.65e-4, $ ;mass fraction of amCBEx | |
| 244 | + ; 1.45e-3, $ ;mass fraction of amCBEx | |
| 245 | + ; 7.8e-3, $ ;mass fraction of big grains? | |
| 246 | + ; ;0.002, $ ;intensity of NIR continuum | |
| 247 | + ; 10.,$ | |
| 248 | + ; ;;1.,$ | |
| 249 | + ; ;1.,$ | |
| 250 | + ; 10.$ | |
| 251 | + ; ;;1.,$ | |
| 252 | + ; ;1.$ | |
| 253 | + ; ] | |
| 255 | 254 | |
| 256 | 255 | |
| 257 | 256 | |
| ... | ... | @@ -273,11 +272,11 @@ CASE use_model OF |
| 273 | 272 | ;llims =[1e-5 ,0. ,0. ,0. ,0. ,0. ,0. ,1. ,0. , 1. ,0. ] |
| 274 | 273 | |
| 275 | 274 | ;llims =[0. ,0. ,0. ,0. ,0. ,0. ,1. ,0. , 1. ,0. ] |
| 276 | - llims =[0. ,0. ,0. ,0. ,0. ,1. , 1. ] | |
| 275 | + ;llims =[0. ,0. ,0. ,0. ,0. ,1. , 1. ] | |
| 277 | 276 | |
| 278 | 277 | ulimed=replicate(0,Npar) |
| 279 | 278 | llimed=replicate(1,Npar) |
| 280 | - ;llims=replicate(0.,Npar) | |
| 279 | + llims=replicate(0.,Npar) | |
| 281 | 280 | |
| 282 | 281 | |
| 283 | 282 | ;=== Fixed parameters |
| ... | ... | @@ -383,7 +382,8 @@ dustem_init_plugins, pd ;initializing the scopes of the plugins to be read later |
| 383 | 382 | |
| 384 | 383 | ;=== RUN fit |
| 385 | 384 | tol=1.e-16 |
| 386 | -use_Nitermax=50 ;maximum number of iteration. This is the criterium which will stop the fit procedure , NOTA BENE: 3 iterations aren't enough to fit the entirety of the newly added stellar population parameters. | |
| 385 | +;use_Nitermax=50 ;maximum number of iteration. This is the criterium which will stop the fit procedure , NOTA BENE: 3 iterations aren't enough to fit the entirety of the newly added stellar population parameters. | |
| 386 | +use_Nitermax=5 ;maximum number of iteration. This is the criterium which will stop the fit procedure , NOTA BENE: 3 iterations aren't enough to fit the entirety of the newly added stellar population parameters. | |
| 387 | 387 | IF keyword_set(itermax) THEN use_Nitermax=itermax |
| 388 | 388 | |
| 389 | 389 | t1=systime(0,/sec) | ... | ... |