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
Output Choice | Output file Suffix or Prefix | Description | |
Standard | prefix=spec | Contains the output emission-line spectrum. | |
Column 1 | Wavelength in Angstroms (A) | ||
Column 2 | Energy (E) in electron volts (eV) | ||
Column 3 | Intensity relative to H-beta=1 | ||
Column 4 | Species responsible for emission-line | ||
Column 5 | Accuracy (see table below) 1=good, 2=average, 3=poor | ||
Standard | prefix=phot | Contains 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 Source | suffix=.sou | Contains the final source spectrum in units of Energy (eV) versus Fnu (ergs/s/cm^2/Hz/sr) | |
NuFnu Spectrum | suffix=.nfn | Contains the final source spectrum in units of nu (Hz) versus nuFnu (ergs/s/cm^2/sr) | |
First Balance | suffix=.bln | Contains the initial ionization balance | |
Column 1 | Atomic number | ||
Column 2 | Ionization state | ||
Column 3 | Fraction of element at this ionization state | ||
Monitor 4 atoms | Prefix=Atomic # | Four files: each contains the fraction of element chosen at each ionization state at each step (shell) through the nebula. | |
Column 1 | Outer radius of shell (cm) | ||
Column 2 | Thickness of shell (cm) | ||
Column 3 | Average temperature in shell (K) | ||
Columns 4-26 | Fraction of element at each ionization state from I-XXVII | ||
Monitor all ions | Prefix=allions | Contains 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. |
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 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 | |
Alpha | Power law model index |
Cut-off | Model cut-off energy (Ryd) |
De | Electron density (cm^-3) |
DH | Hydrogen density (cm^-3) |
DIend | Distance at end of density bounded models (cm) |
(Not applicable to web-based 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 step-size. 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 On-line models |
Int./H-beta | Integrated line intensity divided by the intensity of H-beta |
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 |
Web-based 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 (cm/s) defined as: ionizing photon flux per unit area/ion density . For solar abundance, the ion density, Ndens ~ 1.1*Hdens (hydrogen density) |
QHDH | Ionization 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 |
QHDNin | Ionization parameter at the inner edge of the nebula as defined in QHDN above (cm/s) |
QHDNav | Average ionization parameter as defined in QHDN above(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 optical-depth limited models |
Not applicable to web-based 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. |
Turn-on | Model turn-on energy (Ryd) |
Z-star | Metallicity of mappings internal stellar atmosphere models |
Not applicable to web-based models | |
ZETAef | Alternative (archaic) measure of ionization parameter |