make_phangs_ssps_isrf_prediction.pro
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PRO make_phangs_ssps_isrf_prediction,source_name=source_name,save=save,help=help
;+
; NAME:
; make_phangs_ssps_isrf_prediction
; CALLING SEQUENCE:
; make_phangs_ssps_isrf_prediction[,source_name=][,/save][,/help]
; PURPOSE:
; predicts the minimum ISRF in voronoi bins
; INPUTS:
; None
; OPTIONAL KEYWORDS:
; save = if set, save the classes
; help = if set, print this help
; OUTPUTS:
; None
; OPTIONAL INPUT:
; source_name = source name (default='ngc0628')
; OPTIONAL OUTPUT:
; None
; PROCEDURE AND SUBROUTINE USED
; ISRF saved is the one predicted by dustem_plugin_phangs_stellar_isrf for each Muse Voronoi bin,
; scaled in amplitude to match the Muse filter data for that Voronoi bin.
; The G0 value computed is wrt the Mathis field at 1 mic.
; SIDE EFFECTS:
; produces file _isrf_min_prediction.sav
; EXAMPLE:
; make_phangs_ssps_isrf_prediction,source_name='ngc0628',/save
; MODIFICATION HISTORY:
; written by Jean-Philippe Bernard
;-
IF keyword_set(help) THEN BEGIN
doc_library,'make_phangs_ssps_isrf_prediction'
goto,the_end
ENDIF
;===== predicts the minimum ISRF in voronoi bins
;===== The prediction is scaled to the Muse filter data observations
win=0L
;window,win,xsize=900,ysize=1000 & win=win+1
;=== This is where the data is read from and the ISRFs will be stored
data_dir=!phangs_data_dir+'/ISRF/WORK/'
use_model='DBP90' ;Example with default keywords uses the DBP90 model
use_polarization=0 ; initialize Dustemwrap in no polarization mode
;== INITIALISE DUSTEM
dustem_init,model=use_model,polarization=use_polarization,show_plots=show_plots
use_source_name='ngc0628'
IF keyword_set(source_name) THEN use_source_name=source_name
CASE use_source_name OF
'ngc0628':BEGIN
object_distance=9.84 ;MPc
object_thickness=0.1 ;kpc
END
'ngc3351':BEGIN
object_distance=9.96 ;MPc
object_thickness=0.1 ;kpc
END
ENDCASE
dustem_define_la_common
obp=[1.1,0,1.15,1]
;dustem_init,show_plots=show_plots
;needed only for NHCO
restore,data_dir+use_source_name+'_jwst_images.sav',/verb
;% RESTORE: Restored variable: JWST_IMAGES.
;% RESTORE: Restored variable: FILTERS.
;% RESTORE: Restored variable: HREF.
;% RESTORE: Restored variable: NHCO.
;needed for stellar parameters and voronoi bin info
restore,data_dir+use_source_name+'_muse_images.sav',/verb
;% RESTORE: Restored variable: ST_TEMPLATES.
;% RESTORE: Restored variable: ST_MUSE_WEIGHTS.
;% RESTORE: Restored variable: VORONOI_ID.
;% RESTORE: Restored variable: AGE_VALUES.
;% RESTORE: Restored variable: METALICITY_VALUES.
;% RESTORE: Restored variable: BINS.
;% RESTORE: Restored variable: HREF.
;=== needed for absolute scaling of ISRF
restore,data_dir+use_source_name+'_muse_filters_data.sav',/verb
;% RESTORE: Restored variable: MUSE_IMAGES.
;% RESTORE: Restored variable: MUSE_FILTERS.
;% RESTORE: Restored variable: HREF.
restore,data_dir+use_source_name+'_muse_seds_muse_pixels.sav',/verb
;% RESTORE: Restored variable: ALL_SEDS.
;% RESTORE: Restored variable: ALL_SEDS_INDICES.
Nvor=max(voronoi_id)
use_NHmap=NHCO ;used NH map in 1.e21 (from CO)
;stop
!quiet=1
t1=systime(0,/sec)
first_vid=0L
lambir=dustem_get_wavelengths(isrf_wavelengths=isrf_wavelengths)
;show_each=10
show_each=100
Nlamb=n_elements(isrf_wavelengths)
ISRFS=dblarr(Nlamb,Nvor)
G0s=dblarr(Nvor)
;==== get Mathis field for G0 calculations
file=!dustem_soft_dir+'/data/ISRF_MATHIS.DAT'
readcol,file,Mathis_wavs,Mathis_ISRF
Mathis_ISRF=interpol(Mathis_ISRF,Mathis_wavs,isrf_wavelengths)
Mathis_1mic=interpol(Mathis_ISRF,isrf_wavelengths,1.0)
FOR vid=first_vid,Nvor-1 DO BEGIN
IF vid mod show_each EQ 0 THEN BEGIN
t2=systime(0,/sec)
delta_t_hr=(t2-t1)/60.^2 ;elapsed time [hr]
frac_perc=vid/Nvor*100
delta_t_remain=delta_t_hr/frac_perc*100.-delta_t_hr ;remaining time [hr]
message,'done '+strtrim(frac_perc)+' % in '+strtrim(delta_t_hr,2)+' hr remaining '+strtrim(delta_t_remain,2)+' hr',/continue
ENDIF
;===== get the SSP weights for the given voronoi bins
weights=phangs_binid2weights(st_muse_weights,vid,st_templates,age_values,metalicity_values,reddening=reddening)
amplitude=1. ;amplitude is set to 1, and will be corrected by G0 below
use_reddening=0. ;This sets Muse reddening to 0. Will be contsrained later
fpd=phangs_stellar_continuum_plugin_weight2params(weights,parameter_values=val,redenning=use_reddening,/force_include_reddening,amplitude=amplitude,/force_include_amplitude)
Nparams=n_elements(val)
key=intarr(Nparams)
FOR i=0L,Nparams-1 DO BEGIN
toto=dustem_parameter_description2type(fpd[i],string_name=string_name,key=one_key)
key[i]=one_key
ENDFOR
;==== compute the prediction stellar continuum for comparison to the Muse filter data.
;==== Here we use the reddening from MUSE
val_sed=val
val_sed[1]=reddening ;for the SED, we use E(B-V)
spectrum=dustem_plugin_phangs_stellar_continuum(key=key,val=val_sed)
sed=interpol(spectrum[*,0],lambir,dustem_filter2wav(muse_filters[0:2]))
muse_sed=(*all_seds[vid]).stokesI
facts=muse_sed/sed
muse_factor=la_mean(facts) ;This takes the average value over the MUSE bands
;print,G0,reddening
;stop
val_isrf=val ;for the ISRF, we use E(B-V)=0
ISRFS[*,vid]=dustem_plugin_phangs_stellar_isrf(key=key,val=val_isrf,object_distance=object_distance,object_thickness=object_thickness)
ISRFS[*,vid]=ISRFS[*,vid]*muse_factor ;=== scale the amplitude of ISRFs to the muse data
;=== compute corresponding G0
G0=interpol(ISRFS[*,vid],isrf_wavelengths,1.)/Mathis_1mic
G0s[vid]=G0
ENDFOR
IF keyword_set(save) THEN BEGIN
file_save=data_dir+use_source_name+'_isrf_min_prediction.sav'
save,ISRFS,G0s,object_distance,object_thickness,use_source_name,file=file_save,/verb
phangs_make_isrf_product,use_source_name,voronoi_id,ISRFS,G0s,object_distance,object_thickness
ENDIF
;cgplot,lindgen(Nvor),G0s,/ylog,yrange=[1.e-5,1],xtit='Voronoi ID',ytit='G0'
stop
the_end:
END