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Mappings IIId Output Files 

Note: MappingsIII has been developed over two decades by many people. The variations in naming convention and units reflect this. Work is currently underway to introduce more consistency to the Mappings output naming convention.

ABUND  Abundance 
Accuracy  This parameter reflects the reliability of the atomic data used to estimate the emissionline fluxes. 
1 = Accurate to 10% (Hydrogenic lines only)  
2 = Average reliability  
3 = Poor reliability (old data, many atomic levels, or radiative transfer problems  
Alpha  Power law model index 
Cutoff  Model cutoff energy (Ryd) 
De  Electron density (cm^3) 
DH  Hydrogen density (cm^3) 
DIend  Distance at end of density bounded models (cm) 
(Not applicable to webbased models)  
DISav  Average radius of each shell (cm) 
DIST.Ave.  Average radius of each shell (cm) 
DISfin  Final radius of the nebula (cm) 
DISout  Radius at the outer edge of each shell (cm) 
DILUav  Average geometric dilution factor. For plane parallel models, DILUav will be 0.5. For spherical models, it will be close to zero 
DLOsav  Average differential loss between heating and cooling. This should be close to zero if energy has been conserved in the model 
Dn  Ion density (cm^3) 
Dnum  Ion density (cm^3) 
dr  thickness of each shell (cm) 
dR  thickness of each shell (cm) 
dTau  Model stepsize. Default=0.03 
dVol  Nebula volume in each shell (cm^3) 
El.Dens  Electron density (cm^3) 
Ending  Model ending = A (fraction of HI = 99%) 
FHI  Fraction of HI in each shell of the nebula 
FHII  Fraction of HII in each shell of the nebula 
FHXF  Final fraction of HII at the end of the nebula 
Fill.F. or F.F.  Filling factor 
Fren  Required final fraction of ionized hydrogen at model end (1%) 
FQHeI  Flux of He+ ionizing photons(photons/s/cm^2) 
FQHeII  Flux of He++ ionizing photons(photons/s/cm^2) 
FQHI  Flux of H+ ionizing photons(photons/s/cm^2) 
FQtot  Total Flux of ionizing photons(photons/s/cm^2) 
Hden  Hydrogen density (cm^3) 
Hdens  Hydrogen density (cm^3) 
Ielen  Atomic number of element whose ionized fraction determines the model ending (this is always hydrogen=1). 
Input  Will always read `interactive' for Mappings Online models 
Int./Hbeta  Integrated line intensity divided by the intensity of Hbeta 
Jden  Density model chosen by user: c=isochoric, b=isobaric 
Jeq  Equilibrium model chosen (always E) 
Jgeo  Geometry model chosen by user: s=spherical, p=plane parallel 
Jpoen  Ionization state of required model ending 
Webbased models: 1 (99% HI)  
MOD  model choice: X=external, B=blackbody, P=power law 
Ndens  Ion density (cm^3). For solar abundance, Ndens ~ 1.1*Hdens (hydrogen density) 
nH  Hydrogen density (cm^3) 
ne  Electron density (cm^3) 
Output  Output photoionization file (See description in the Table above) 
P5  Photoionization model version IIId used 
QHDN  Ionization parameter 
QHDH  Ionization parameter as above (cm/s) 
QHDNin  Ionization parameter at the inner edge of the nebula (cm/s) 
QHDNav  Average ionization parameter (cm/s) 
Remp  Initial radius of the nebula (cm) 
Rmax  Maximum radius of model (cm) 
Rsou  Source Radius (cm) 
Run  Model designation entered by user 
Tauen  Optical depth at model end for opticaldepth limited models 
Not applicable to webbased moels  
TauXF  Optical depth at Hydrogen edge (912A): optically thick if TauXF > 1, optically thin if TauXF < 1 
Teav  Average electron temperature (K) 
Te Ave.  Average electron temperature (K) 
Teini  Initial electron temperature (K) 
Temp  Blackbody model temperature (K) 
Tend  Temperature at model end (K) 
Tfinal  Temperature at model end (K) 
TOTLOSS  Total energy losses + total heating. This should be close to zero if energy has been conserved in the model. 
Turnon  Model turnon energy (Ryd) 
Zstar  Metallicity of mappings internal stellar atmosphere models 
Not applicable to webbased models  
ZETAef  Alternative (archaic) measure of ionization parameter 