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

MODEL DESIGNATION: -- an identifier you want to assign to the model. This must consist only of alphanumeric characters and if required, the underscore character '_'. You will find this name in each header of the output files.

CHEMICAL COMPOSITION OF THE GAS: -- specify the elemental abundances of the gas. The default solar set of abundances from Anders & Grevesse (1989) is shown in the boxes on the right-hand side of the input form.

DEFAULT ABUNDANCES: -- use the default set of abundances as given in the boxes on the right and scale by the metal abundance to a common fraction of solar. H and He are kept fixed and all metals are multiplied by the Z value in the pull-down menu. More detailed abundance sets should be entered into the itemized boxes (such as those requiring a secondary nature of Nitrogen for specific metallicities).

TAILORED ABUNDANCES: -- enter individual abundances for the 16 elements as desired. Units: logarithmic with hydrogen = 0.0.

INCLUSION OF DUST: -- if the include button is checked, dust is considered in Mappings, and all the dust related input parameters must be specified. Otherwise they are ignored.

DUST DEPLETION: -- specify the depletion factors for the 16 elements listed.

DEFAULT DEPLETION FACTORS: -- use the default depletion factors as given in the boxes on the right.

INDIVIDUAL DEPLETION FACTORS: -- enter individual depletion factors in logarithmic units for the 16 elements as desired. Depletion factors are defined as the fraction of each element in gas phase compared to the fraction in dust. Undepleted elements have depletion factors of 1.00, and fully depleted elements have depletion factors of 0.00. Negative values are assumed to be in logarithmic form.

GRAIN DISTRIBUTION MODEL: -- characterize the dust properties by the model of Mathis, Rumpl, & Nordsiek (1977). Other options for the distribution function will be added in the future.

CALCULATION OF THE DUST SED: -- switch to enable or disable the calculation of the IR flux distribution of the dust and the dust temperature. Since this step is very time consuming, it should only be turned on if infrared fluxes are required.

IONIZING RADIATION FIELD: -- select which ionizing radiation field to use. Choices are a blackbody or power-law. For an ionizing radiation field from the stellar-population synthesis model Starburst99, please use the Starburst99-Mappings portal webpage. This page includes the Starburst99 input parameters in addition to the Mappings input parameters.

BLACKBODY RADIATION FIELD: -- blackbody radiation field defined by its temperature in degrees Kelvin. This is the appropriate choice for photoionization by a single stellar source.

POWER-LAW RADIATION FIELD: -- power-law radiation field defined as

, where alpha is the power-law index given by the user (default=-1.4; suitable for an AGN). The constant c is determined by scaling the ionizing radiation field by either the ionization parameter, luminosity or radius below (the latter two can only be entered for spherical models).

SELECTION OF THE GEOMETRY: -- specify either spherically symmetric or plane-parallel geometry. The choice affects which additional input parameters are necessary for scaling the ionizing radiation field. The parameters below the geometry buttons for either geometry should be used. The default is spherical geometry.

RADIUS OF THE STELLAR SOURCE [SOLAR RADII]: -- this is the first of the 3 scaling options. It is most useful if a single stellar source ionizes the HII region. Enter the stellar radius in R_sol, and the scaled Starburst99 spectrum is used to simulate a single star of that radius and having the Starburst99 spectral shape.

TOTAL LUMINOSITY THE STELLAR SOURCE [log (erg/s)]: -- this is the second of the 3 scaling options. Enter the bolometric luminosity of the star, star cluster, or stellar population. .

IONIZING LUMINOSITY THE STELLAR SOURCE [log (erg/s)]: -- this is the third of the 3 scaling options. Enter the ionizing luminosity (below 912 A) of the star or star cluster.

INNER BOUNDARY CONDITION OF THE HII REGION: -- the scaled spectrum for a spherical geometry requires an additional input parameter: the inner radius of the HII region. One of the following three must be chosen.

DISTANCE OF THE INNER EDGE OF THE HII REGION [pc]: -- the first option is to give the distance between the ionizing star or star cluster and the inner surface of the HII region.

INNER EDGE AS A FRACTION OF THE STROMGREN RADIUS: -- the second option is to give the distance as a fraction of the total size defined by the Stromgren radius.

INNER EDGE VIA THE IONIZATION PARAMETER: -- the third option is to define the inner edge via the logarithm of the desired ionization parameter (U). The ionization parameter is dimensionless and is defined as U=ionizing photon flux per unit area/(hydrogen density * c).

INNER EDGE VIA THE BOLOMETRIC FLUX [log (ergs/s/cm^2)] : -- For plane parallel models, one can define the inner edge via the bolometric flux. Bolometric flux is defined here as the total energy incident on one cubic centimeter of the inner surface of the nebula per second.

INNER EDGE VIA THE IONIZING FLUX [log (ergs/s/cm^2)]: -- For plane parallel models, one can define the inner edge via the ionizing flux. Ionizing flux is defined here as the ionizing energy incident on one cubic centimeter of the inner surface of the nebula per second.

INITIAL IONIZATION PARAMETER: -- For plane-parallel geometry, the flux at the inner edge of the nebula can be defined by the logarithm of the dimensionless ionization parameter (U). The ionization parameter is defined as U=ionizing photon flux per unit area/(hydrogen density * c).

DENSITY STRUCTURE: -- the density structure can be isochoric or isobaric. In the former case, it is specified by the density, and in the latter by pressure and temperature. A filling factor can be chosen for either case.

ELECTRON DENSITY [cm^-3]: -- enter the electron density if the structure is isochoric.

PRESSURE: -- enter the dimensionless pressure in units of 10⁵ if the structure is isobaric.

TEMPERATURE [10⁴ K]: -- enter the mean temperature in units of 10⁴ K if the structure is isobaric.

FILLING FACTOR: -- enter the filling factor for either density option.

OUTPUT FILES: -- these are the options to generate various outputs, ranging from the minimum to the very detailed output. All files are described in more detail below.

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 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.

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.

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

(October 17th 2002) - Lisa Kewley

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