How to run a MappingsIIId photoionization model

Model parameters can be entered using the web-based form. The parameters are described below. If you are not sure about an input parameter, start outwith the default value. Mappings IIId runs the models in a queue during the evenings. Upon completion, an email will be sent notifying the user that model has run. The user can then retrieve the output files from the Mappings IIId website



The output

Once the run is finished, you will be notified by e-mail. If everything went well, you should find the output files in the output directory. The e-mail gives you all the information you need to locate the files and the retrieve them.

Mappings IIId output files



Output ChoiceOutput file Suffix or PrefixDescription
Standardprefix=specContains the output emission-line spectrum.
Column 1Wavelength in Angstroms (A)
Column 2Energy (E) in electron volts (eV)
Column 3Intensity relative to H-beta=1
Column 4Species responsible for emission-line
Column 5Accuracy (see table below) 1=good, 2=average, 3=poor
Standardprefix=photContains the model parameters, detailed description of the radiation field and fraction of various ions at each distance step in the model, the average state of ionization of each distance, average distance of each ionization state, average ionic temperatures,integrated column densities, average ionic electron densities.
Final Sourcesuffix=.souContains the final source spectrum in units of Energy (eV) versus Fnu (ergs/s/cm^2/Hz/sr)
NuFnu Spectrumsuffix=.nfnContains the final source spectrum in units of nu (Hz) versus nuFnu (ergs/s/cm^2/sr)
First Balancesuffix=.blnContains the initial ionization balance
Column 1Atomic number
Column 2Ionization state
Column 3Fraction of element at this ionization state
Monitor 4 atomsPrefix=Atomic #Four files: each contains the fraction of element chosen at each ionization state at each step (shell) through the nebula.
Column 1Outer radius of shell (cm)
Column 2Thickness of shell (cm)
Column 3Average temperature in shell (K)
Columns 4-26Fraction of element at each ionization state from I-XXVII
Monitor all ionsPrefix=allionsContains the fraction of all elements at each ionization state at each step (or shell) through the nebula. Also gives the abundance used. Allions is a very large file and should only be requested if specifically required.



Description of names and acronyms in 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.

ABUNDAbundance
AccuracyThis parameter reflects the reliability of the atomic data used to estimate the emission-line fluxes.
1 = Accurate to 10% (Hydrogenic lines only)
2 = Average reliability
3 = Poor reliability (old data, many atomic levels, or radiative transfer problems
AlphaPower law model index
Cut-offModel cut-off energy (Ryd)
DeElectron density (cm^-3)
DHHydrogen density (cm^-3)
DIendDistance at end of density bounded models (cm)
(Not applicable to web-based models)
DISavAverage radius of each shell (cm)
DIST.Ave.Average radius of each shell (cm)
DISfinFinal radius of the nebula (cm)
DISoutRadius at the outer edge of each shell (cm)
DILUavAverage geometric dilution factor. For plane parallel models, DILUav will be 0.5. For spherical models, it will be close to zero
DLOsavAverage differential loss between heating and cooling. This should be close to zero if energy has been conserved in the model
DnIon density (cm^-3)
DnumIon density (cm^-3)
drthickness of each shell (cm)
dRthickness of each shell (cm)
dTauModel step-size. Default=0.03
dVol Nebula volume in each shell (cm^3)
El.DensElectron density (cm^-3)
EndingModel ending = A (fraction of HI = 99%)
FHIFraction of HI in each shell of the nebula
FHIIFraction of HII in each shell of the nebula
FHXFFinal fraction of HII at the end of the nebula
Fill.F. or F.F.Filling factor
FrenRequired final fraction of ionized hydrogen at model end (1%)
FQHeIFlux of He+ ionizing photons(photons/s/cm^2)
FQHeIIFlux of He++ ionizing photons(photons/s/cm^2)
FQHIFlux of H+ ionizing photons(photons/s/cm^2)
FQtotTotal Flux of ionizing photons(photons/s/cm^2)
HdenHydrogen density (cm^-3)
HdensHydrogen density (cm^-3)
IelenAtomic number of element whose ionized fraction determines the model ending (this is always hydrogen=1).
InputWill always read `interactive' for Mappings On-line models
Int./H-betaIntegrated line intensity divided by the intensity of H-beta
JdenDensity model chosen by user: c=isochoric, b=isobaric
JeqEquilibrium model chosen (always E)
JgeoGeometry model chosen by user: s=spherical, p=plane parallel
JpoenIonization state of required model ending
Web-based models: 1 (99% HI)
MODmodel choice: X=external, B=blackbody, P=power law
NdensIon density (cm^-3). For solar abundance, Ndens ~ 1.1*Hdens (hydrogen density)
nHHydrogen density (cm^-3)
neElectron density (cm^-3)
OutputOutput photoionization file (See description in the Table above)
P5Photoionization model version IIId used
QHDNIonization parameter (cm/s) defined as:
ionizing photon flux per unit area/ion density .
For solar abundance, the ion density, Ndens ~ 1.1*Hdens (hydrogen density)
QHDHIonization parameter (cm/s) defined as:
ionizing photon flux per unit area/hydrogen density.
Note: the dimensionless ionization parameter is defined as U=QHDH/c, not as QHDN/c
QHDNinIonization parameter at the inner edge of the nebula as defined in QHDN above (cm/s)
QHDNavAverage ionization parameter as defined in QHDN above(cm/s)
RempInitial radius of the nebula (cm)
RmaxMaximum radius of model (cm)
RsouSource Radius (cm)
RunModel designation entered by user
TauenOptical depth at model end for optical-depth limited models
Not applicable to web-based moels
TauXFOptical depth at Hydrogen edge (912A): optically thick if TauXF > 1, optically thin if TauXF < 1
TeavAverage electron temperature (K)
Te Ave.Average electron temperature (K)
TeiniInitial electron temperature (K)
TempBlackbody model temperature (K)
TendTemperature at model end (K)
TfinalTemperature at model end (K)
TOTLOSSTotal energy losses + total heating. This should be close to zero if energy has been conserved in the model.
Turn-onModel turn-on energy (Ryd)
Z-starMetallicity of mappings internal stellar atmosphere models
Not applicable to web-based models
ZETAefAlternative (archaic) measure of ionization parameter

(October 17th 2002) - Lisa Kewley