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agn_blr_albedo.in measure rayleigh scattering of Lya
title measure rayleigh scattering of Lya
c model from Korista, K., & Ferland, G. 1998, ApJ, 495, 672
c
c commands controlling continuum =========
agn 6.683 -1.20 -1.20 -0.90
ionization parameter 1.0
c
c commands for density & abundances =========
init file = "ism.ini"
abundances old solar 84
hden 11.0
c
c commands controlling geometry =========
stop total column density = 23.75
c
c other commands for details =========
iterate
c
c commands controlling output =========
normalize to "FeKa" 1.78
print line faint -1
print diffuse continua
print lines inward
punch continuum last "agn_blr_albedo.con" units kev
punch dr "agn_blr_albedo.dr"
punch reflected continuum last "agn_blr_albedo.ref"
punch emitted continuum last "agn_blr_albedo.emt"
c
c must assert the luminosity since change in this
c line would appear to change the rest of the spectrum
c agn_blr_albedo.in
c class blr
c ========================================
This model computes the albedo of a fairly
standard BLR cloud. This is the type of
model that was presented in the BLR albedo
paper by Korista & Ferland, 1998, ApJ 495, 672.
The print diffuse continua command enters continuum
fluxs into the emission line stack.  Pequignot et al. summarized in 2001ASPC..247..533P.
It is necessary to also include the command
no induced processes
to obtain the results presented there.  Pequignot et al. summarized in 2001ASPC..247..533P.
It is necessary to also include the command
no induced processes
to obtain the results presented there.  Pequignot et al. summarized in 2001ASPC..247..533P.
It is necessary to also include the command
no induced processes
to obtain the results presented there. This disables UTA ionization,
a process that was not included in the calculations presented in the paper.
agn_reflector.in model of Compton reflector
title model of Compton reflector
c
c commands controlling continuum =========
c this is a powerlaw that extends into the x-rays, but by default
c has exponential cutoff in FIR
power law -1. hi=1000000000
c the ionization parameter for this powerlaw
ionization parameter 1.
c add background so that FIR/radio does not have zero flux
background
iterate
c
c commands for density & abundances =========
hden 11
c
c commands controlling geometry =========
stop total column density 24
c
c other commands for details =========
constant temper 5
atom h-like element hydrogen levels resolved 10
atom h-like element helium levels resolved 10
c
c commands controlling output =========
print line faint 1
print line inward
print diffuse continuum
c
c this is to produce lines with lots of contrast with the continuum
set PunchLWidth 100 km/sec
c a fig in part 3 of hazy uses data from this model. the fig shows lines
c with above and below linewidth
c set PunchLWidth c
punch continuum last "agn_reflector.con" units kev
punch continuum reflected last "agn_reflector.alb" units kev
punch overview last "agn_reflector.ovr"
punch dr last "agn_reflector.dr"
c
table lines "LineList_BLR.dat"
c agn_reflector.in
c class blr
c ========================================
c
This is a model of the Compton reflector in AGN. It is a
constant temperature since models of this region often make that assumption.
A plot in Part I of Hazy shows the incident and reflected portions of the
continuum. The code will complain that the cloud is Compton thick since it
is not really designed to simulate this situation.
agn_S_curve_grid.in temperature across Spitzer thermal stability S curve
title temperature across Spitzer thermal stability S curve
c
c commands controlling continuum =========
c this is the generic AGN continuum
table agn
c the ionization parameter will be varied
ionization parameter 0.00 vary
grid from 0 to 3 in 0.25 dex steps
c add background so that FIR/radio does not have zero flux
background
iterate
c
c commands for density & abundances =========
c intended to make sim run as fast as possible
hden 8
init file "ism.ini"
element sulphur off
element chlorine off
element argon off
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c commands controlling output
c this produces a very large number of lines in the output mostly
c because Hbeta is very weak in hot gas. Choose Lya as the normalization
c line to make line list smaller
normalize to "totl" 1216
print line faint 10 will be varied
c create file with list of grid parameters
punch grid "agn_S_curve_grid.grd" last
c save average H+ temperature
punch average "agn_S_curve_grid.avr" last
temperature hydrogen 1
end of temperatures
c save heating and cooling
punch heating "agn_S_curve_grid.het" last
punch cooling "agn_S_curve_grid.col" last
punch iron element "agn_S_curve_grid.fe" last
punch xspec atable "agn_S_curve_grid.fit"
c
c
c agn_S_grid.in
c class BLR
c ========================================
c
This computes a series of models that check the temperature
through the S curve in the Fields et al. three-phase model of
ISM stability.
agn_warm_absorber.in simple warm absorber model
title simple warm absorber model
c
c commands controlling continuum =========
table power law
ionization parameter 0
c
c commands for density & abundances =========
hden 6
abundances old solar 84
c
c commands controlling geometry =========
stop column density 22
c
c other commands for details =========
iterate to convergence
c
c commands controlling output =========
print line faint 10
plot continuum range 1 1000
punch continuum "agn_warm_absorber.con" last units kev
punch continuum "agn_warm_absorber.conA" last units Angstroms
punch fine continuum "agn_warm_absorber.finA" last units Angstroms range 61 120 merge 3
punch dr "agn_warm_absorber.dr" last
c this will be the default units, like the printout
punch line optical depths last "agn_warm_absorber_lab.lin"
c this will be the same, in rygbergs
punch line optical depths last "agn_warm_absorber_ryg.lin" units rydberg
c
c warrm_absorber
c class nlr
c ========================================
c
this is a simple warm absorber model. It makes a plot of the
transmitted continuum, and generates a list of lines with
significant optical depths
aperture_beam_int.in test aperture beam command with intensity
title test aperture beam command with intensity
c
c commands for density & abundances =========
hden 0
init file "honly.ini"
c
c other commands for details =========
constant temper 4
c
c commands controlling continuum =========
laser 2
ionization -2
c
c commands controlling geometry =========
stop thickness 10
sphere
aperture beam
c
c commands controlling output =========
c
c aperture_beam_int.in
c class geometry
c ========================================
This is a homogeneous sphere that is especially simple. The model
is a test of the aperture command, a command that simulates observing
part of an extended object. In this case the aperture is a beam
contered on the center of the nebula, with a line of sight
extending through the object.
The code carries along a dummy emission line ("Unit 1") with a constant intensity
of 1e-10 erg cm-3 s-1. The line goes through all of the code's infrastructure,
and when the calculation is complete, the program confirms that the "luminosity"
of the line is the emitting volume times 1e-10. The aperture command
is verified by asserting that the emission line has the correct "luminosity".
In this case the inner radius is not specified so the returned value is unity.
aperture_beam_lum.in test aperture beam command with luminosity
title test aperture beam command with luminosity
c
c commands controlling continuum =========
laser 2
q(h) 31.5
c
c commands for density & abundances =========
hden 0
init file "honly.ini"
c
c commands controlling geometry =========
stop thickness 10
radius 9
sphere
aperture beam
c
c other commands for details =========
constant temper 4
c
c commands controlling output =========
c
c aperture_beam_lum.in
c class geometry
c ========================================
This is a homogeneous sphere that is especially simple. The model
is a test of the aperture command, a command that simulates observing
part of an extended object. In this case the aperture is a beam
contered on the center of the nebula, with a line of sight
extending through the object.
The code carries along a dummy emission line ("Unit 1") with a constant intensity
of 1e-10 erg cm-3 s-1. The line goes through all of the code's infrastructure,
and when the calculation is complete, the program confirms that the "luminosity"
of the line is the emitting volume times 1e-10. The aperture command
is verified by asserting that this emission line has the correct "luminosity".
aperture_slit.in test aperture slit command with luminosity
title test aperture slit command with luminosity
c
c commands controlling continuum =========
laser 2
q(h) 31.5
c
c commands for density & abundances =========
hden 0
init file "honly.ini"
c
c commands controlling geometry =========
radius 9 10
sphere
aperture slit
c
c other commands for details =========
constant temper 4
c
c commands controlling output =========
c
c aperture_slit.in
c class geometry
c ========================================
c
This is a homogeneous sphere that is especially simple. The model
is a test of the aperture command, a command that simulates observing
part of an extended object. In this case the aperture is a long
slit contered on the center of the nebula, extending beyond the outer
reaches of the matter.
The code carries along a dummy emission line ("Unit 1") with a constant intensity
of 1e-10 erg cm-3 s-1. The line goes through all of the code's infrastructure,
and when the calculation is complete, the program confirms that the "luminosity"
of the line is the emitting volume times 1e-10. The aperture command
is verified by asserting that the emission line has the correct "luminosity".
blr_f92.in standard blr cloud in Ferland et al. 1992
title standard blr cloud in Ferland et al. 1992
c
c commands controlling continuum =========
table agn
ionization parameter -1
c
c commands for density & abundances =========
hden 11
abundances old solar 84
c
c commands controlling geometry =========
stop column density 25
c
c other commands for details =========
atom h-like element hydrogen levels resolved 10
atom h-like element helium levels resolved 10
iterate to convergence
c
c commands controlling output =========
print h-like departure hydrogen
print h-like populations hydrogen
print h-like departure helium
print h-like populations helium
plot continuum
normalize to "H 1" 1216 = 105.90
print line faint -2
punch overview last "blr_f92.ovr"
punch convergence reason "blr_f92.cvr"
punch element nitrogen last "blr_f92.nit"
punch element calcium last "blr_f92.ca"
punch dr "blr_f92.dr"
punch transmitted continuum "blr_f92.trn" last
c
c blr_f92.ini
c class blr
c ========================================
This is similar to one of the BLR models presented in Ferland et al. (1992)
for the well-studied Seyfert galaxy NGC 5548. It has a very large column
density and is marginally optically thick to electron scattering. The spectrum
is given relative to Lya, and the intensity of this line is reset to
produce a spectrum that is on the same intensity scale as that paper.
blr_fp89.in final F+P 1989 BLR model table 3
title final F+P 1989 BLR model table 3
c
c commands controlling continuum =========
table agn
ionization parameter -0.5
c
c commands for density & abundances =========
hden 9.5
init file="c84.ini"
abundances old solar 84
c
c commands controlling geometry =========
stop column density 25.5
c
c other commands for details =========
iterate to convergence
failures 2
c
c commands controlling output =========
c set a relatively high faint level since lines relative to Lya=100
print line faint -1
print h-like departure coefficients
plot continuum
normalize to "H 1" 1216 = 85.60
punch heating "blr_fp89.het"
punch convergence reason "blr_fp89.cvr"
punch cooling "blr_fp89.col"
punch overview last "blr_fp89.ovr"
punch element nitrogen last "blr_fp89.nit"
punch results last "blr_fp89.rlt"
punch dr "blr_fp89.dr"
c
c blr_fp89.in
c class blr
c ========================================
Ferland and Persson (1989) presented this calculation of a BLR cloud.
The differences between the present predictions and
those given by FP are largely due to improved treatment
of Balmer line escape and destruction. The spectrum is given relative
to a Lya intensity of 100. The column density is VERY large, to
reproduce intensities of low-ionization lines, especially the Ca II lines.
blr_hizqso.in high Z quasar cloud
title high Z quasar cloud
c
c commands controlling continuum =========
table agn
ionization parameter 1
c
c commands for density & abundances =========
c actual elec den will be about 100x larger
hden 8
abundances starburst 35
c
c commands controlling geometry =========
c this is more gramage than it appears because of high Z
stop column density 21
c
c other commands for details =========
c once elec den fail occurs due to tripping over He+ - He I-front
c code does recover so not a problem. The default for this is 10,
c and is set low because (hopefully) this would never occur
c hydrogen is a minor constituent in this high metallicity gas
c the electron density is well above the hydrogen density
failures 3
iterate 3
c
c commands controlling output =========
normalize "totl" 1909
punch dr "blr_hizqso.dr"
punch convergence reason "blr_hizqso.cvr"
punch overview last "blr_hizqso.ovr"
punch element nitrogen last "blr_hizqso.nit"
punch element chlorine last "blr_hizqso.cl"
punch element iron last "blr_hizqso.fe"
punch element neon last "blr_hizqso.ne"
punch element calcium last "blr_hizqso.ca"
punch element zinc last "blr_hizqso.zn"
punch heating last "blr_hizqso.het"
punch cooling last "blr_hizqso.col"
c
c
c blr_hizqso.in
c class blr
c ========================================
This is a model of a very high metallicty BLR cloud. It checks the
intensities of some of the brigher lines, and is a check that the code
can converge a cloud with this high Z.
Secondary ionization is very important when H is highly ionized,
due to very high He abundance. Sec ionization becomes important
at the He+ - He ionization front, where H+/H is 1e-5.
blr_kk81.in old blr
title old blr
c
c commands controlling continuum =========
interpolate (0 -5) (.05 -5) (.1 0) (1 -0.5) (7.353 -2.233)
continue (735 -3.233) (800 -15) (8.e6 -15)
f(nu) -7.32148
constant gas pressure
c
c commands for density & abundances =========
hden 9.60206
init file="c84.ini"
abundances he-1 c-3.699 n-4 o-3.1549 ne-4 na=-8 mg-4.5229
continue al-10 si-4.4229 s-10 ar-10 ca-10 fe-4.5229 ni=-8
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
failures 2
iterate to convergence
c
c commands controlling output =========
print line faint -1
print ages
normalise "H 1" 1216 100
plot continuum range -3
punch overview last "blr_kk81.ovr"
punch dr last "blr_kk81.dr"
punch continuum last "blr_kk81.con"
punch ionizing continuum "blr_kk81.ion"
c
c
c blr_kk81.in
c class blr
c ========================================
c
This is the "standard" BLR model presented by Kwan and Krolik (1981).
>>refer blr cloud Kwan, J., & Krolik, J. 1981, ApJ, 250, 478
Compare line intensities to previous versions of CLOUDY
by entering into table on page Error! Bookmark not defined..
The code caution that the resulting total pressure was not constant
is to be expected. The KK calculation assumed constant gas pressure,
but internally generature line radiation pressure is significant.
Because of this the sum
of gas plus radiation pressure was not constant although
the gas pressure was.
blr_level2.in test dominant level2 lines
title test dominant level2 lines
c
c commands controlling continuum =========
table agn
ionization -2
c
c commands controlling geometry =========
stop column density 19
c
c commands for density & abundances =========
hden 10
element phosphorus abundance 0
c
c other commands for details =========
iterate
c
c commands controlling output =========
punch overview "blr_level2.ovr"
punch dr "blr_level2.dr"
c
c blr_level2.in
c class blr
c ========================================
This model checks predictions for the "level2" lines. These are
lines that are normally very weak, have Opacity Project wavelengths,
and g-bar collision strengths. Phosphorus is given a large abundance
so that its level2 lines are significant.
blr_n09_p18.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e18 cm2 s-1
title BLR model, density 1e09 cm-3, flux of H-ion phots 1e18 cm2 s-1
c
c commands controlling continuum =========
table agn
phi(h) 18
c
c commands for density & abundances =========
hden 9
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
init "c84.ini"
iterate convergence
c these are to try to speed things up
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n09_p18.ovr" last
punch dr "blr_n09_p18.dr" last
punch convergence reason "blr_n09_p18.cvr"
c
c blr_n09_p18.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n09_p18_Z20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20
title BLR model, density 1e09 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20
c
c commands controlling continuum =========
table agn
phi(h) 18
c
c commands for density & abundances =========
hden 9
abundances starburst 20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate to convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
print h-like hydrogen departure coefficients
punch overview "blr_n09_p18_Z20.ovr"
punch dr "blr_n09_p18_Z20.dr"
punch convergence reason "blr_n09_p18_Z20.cvr"
punch convergence error "blr_n09_p18_Z20.cve"
c
c blr_n09_p18_Z20.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n09_p20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1
title BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1
c
c commands controlling continuum =========
table agn
phi(h) 20
c
c commands for density & abundances =========
hden 9
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
init "c84.ini"
iterate convergence
c these are to try to speed things up
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n09_p18.ovr" last
punch dr "blr_n09_p18.dr" last
punch convergence reason "blr_n09_p18.cvr"
c
c blr_n09_p18.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n09_p20_Z20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1, Z=20
title BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1, Z=20
c
c commands controlling continuum =========
table agn
phi(h) 20
c
c commands for density & abundances =========
abundances starburst 20
hden 9
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
init "c84.ini"
iterate convergence
c these are to try to speed things up
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n09_p20_Z20.ovr" last
punch dr "blr_n09_p20_Z20.dr" last
punch convergence reason "blr_n09_p20_Z20.cvr"
c
c blr_n09_p20_Z20.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
This simulation is optically thin in the Lyman continuum - no H ionization
front is present. As a result it can be difficult to converge.
blr_n09_p22.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1
title BLR model, density 1e09 cm-3, flux of H-ion phots 1e20 cm2 s-1
c
c commands controlling continuum =========
table agn
phi(h) 22
c
c commands for density & abundances =========
hden 9
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
init "c84.ini"
iterate convergence
c these are to try to speed things up
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n09_p22.ovr" last
punch dr "blr_n09_p22.dr" last
punch convergence reason "blr_n09_p22.cvr"
c
c blr_n09_p22.in
c class blr
c ========================================
This is one of the models that sample the LOC plane.
blr_n09_p22_Z20.in BLR model, density 1e09 cm-3, flux of H-ion phots 1e22 cm2 s-1, Z=20
title BLR model, density 1e09 cm-3, flux of H-ion phots 1e22 cm2 s-1, Z=20
c
c commands controlling continuum =========
table agn
phi(h) 22
c
c commands for density & abundances =========
abundances starburst 20
hden 9
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
init "c84.ini"
iterate convergence
c these are to try to speed things up
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n09_p22_Z20.ovr" last
punch dr "blr_n09_p22_Z20.dr" last
punch convergence reason "blr_n09_p22_Z20.cvr"
c
c blr_n09_p22_Z20.in
c class blr
c ========================================
This is one of the models that sample the LOC plane.
blr_n11_p20.in BLR model, density 1e11 cm-3, flux of H-ion phots 1e20 cm2 s-1
title BLR model, density 1e11 cm-3, flux of H-ion phots 1e20 cm2 s-1
c
c commands controlling continuum =========
table agn
phi(h) 20
c
c commands for density & abundances =========
hden 11
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch convergence reason "blr_n11_p20.cvr"
punch overview "blr_n11_p20.ovr" last
punch dr "blr_n11_p20.dr" last
c
c blr_n11_p20.in
c class blr
c ========================================
c
This is one of the 5 models that sample the LOC plane.
blr_n11_p20_Z20.in BLR model, density 1e11 cm-3, flux of H-ion phots 1e20 cm2 s-1, Z=20
title BLR model, density 1e11 cm-3, flux of H-ion phots 1e20 cm2 s-1, Z=20
c
c commands controlling continuum =========
table agn
phi(h) 20
c
c commands for density & abundances =========
hden 11
abundances starburst 20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch cooling "blr_n11_p20_Z20.col"
punch heating "blr_n11_p20_Z20.het"
punch element calcium "blr_n11_p20_Z20.cal"
punch overview "blr_n11_p20_Z20.ovr"
punch dr "blr_n11_p20_Z20.dr"
punch temperature history "blr_n11_p20_Z20.tem"
c
c blr_n11_p20_Z20.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n12_p19.in BLR model, density 1e12 cm-3, flux of H-ion phots 1e19 cm2 s-1
title BLR model, density 1e12 cm-3, flux of H-ion phots 1e19 cm2 s-1
c
c commands for density & abundances =========
c
c commands controlling continuum =========
table agn
phi(h) 19
c
c commands controlling geometry =========
hden 12
stop column density 23
c
c other commands for details =========
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n12_p19.ovr" last
punch dr "blr_n12_p19.dr" last
c
c
c blr_n12_p19.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n12_p19_Z20.in BLR model, density 1e12 cm-3, flux of H-ion phots 1e19 cm2 s-1, Z=20
title BLR model, density 1e12 cm-3, flux of H-ion phots 1e19 cm2 s-1, Z=20
c
c commands controlling continuum =========
table agn
phi(h) 19
c
c commands for density & abundances =========
hden 12
abundances starburst 20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
failures 5
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch convergence reason "blr_n12_p19_Z20.cvr"
punch overview "blr_n12_p19_Z20.ovr" last
punch dr "blr_n12_p19_Z20.dr" last
c
c blr_n12_p19_Z20.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n13_p18.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1
title BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1
c
c this is a very low ionization cloud
c the conditions, and some lines, are surprisingly sensitive
c to the treatment of hydrogen molecules
c
c commands controlling continuum =========
table agn
phi(h) 18
c
c commands for density & abundances =========
hden 13
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate to convergence
c
c commands controlling output =========
normalize to "totl" 1216 100
init "c84.ini"
no level2 lines
punch overview "blr_n13_p18.ovr" last
punch dr "blr_n13_p18.dr" last
punch convergence reason "blr_n13_p18.cvr"
c
c blr_n13_p18.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n13_p18_Z20.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20
title BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20
c
c this is a very low ionization cloud
c the conditions, and some lines, are surprisingly sensitive
c to the treatment of hydrogen molecules
c
c commands controlling continuum =========
phi(h) 18
table agn
c
c commands for density & abundances =========
hden 13
abundances starburst 20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
c this sim needs roughly 10 iterations to converge
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c abort if any failures occur - we want to pass this test
failures 1
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n13_p18_Z20.ovr" last
punch overview "blr_n13_p18_Z20.ovr1"
punch dr "blr_n13_p18_Z20.dr" last
punch convergence reason "blr_n13_p18_Z20.cvr"
c
c
c blr_n13_p18_Z20.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n13_p22.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e22 cm2 s-1
title BLR model, density 1e13 cm-3, flux of H-ion phots 1e22 cm2 s-1
c
c commands controlling continuum =========
table agn
phi(h) 22
c
c commands for density & abundances =========
hden 13
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
print h-like departure hydrogen
print h-like departure helium
normalize to "totl" 1216 100
punch overview "blr_n13_p22.ovr" last
punch dr "blr_n13_p22.dr" last
c
c blr_n13_p22.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_n13_p22_Z20.in BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20
title BLR model, density 1e13 cm-3, flux of H-ion phots 1e18 cm2 s-1, Z=20
c
c commands controlling continuum =========
table agn
phi(h) 22
c
c commands for density & abundances =========
hden 13
abundances starburst 20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate convergence
c these are to try to speed things up
init "c84.ini"
no level2 lines
c
c commands controlling output =========
normalize to "totl" 1216 100
punch overview "blr_n13_p22_Z20.ovr"
punch dr "blr_n13_p22_Z20.dr"
punch heating "blr_n13_p22_Z20.het"
punch cooling "blr_n13_p22_Z20.col"
c
c blr_n13_p22_Z20.in
c class blr
c ========================================
This is one of the 5 models that sample the LOC plane.
blr_nf84.in early model of blr
title early model of blr
c
c commands controlling continuum =========
ionization parameter -1.92
power law -1 100 0.01
c
c commands for density & abundances =========
hden 9.5
init, file="ism.ini"
abundances cameron
stop lyman optical 6
c
c commands controlling geometry =========
c
c other commands for details =========
constant gas pressure
iterate to convergence
c
c commands controlling output =========
print diffuse continuum
plot continuum
punch overview last "blr_nf84.ovr"
punch dr last "blr_nf84.dr"
punch results last "blr_nf84.rlt"
c
table lines "LineList_strong.dat"
c blr_nf84.in
c class blr
c ========================================
c
This is an example of a "conventional" BLR calculation. The parameters are
similar to those of Table 1 of Netzer and Ferland (1984). Notice that the
ratio of Lyalpha to Hbeta ratio is much larger than observed.
>>refer blr model Netzer, H., & Ferland, G. J. 1984, PASP, 96, 593
blr_nf84_45deg.in early model of BLR, with illumination at 45 degree angle
title early model of BLR, with illumination at 45 degree angle
c
c commands controlling continuum =========
ionization parameter -1.92
power law -1 100 0.01
c this continuum is a beam coming in at 45 degrees
illuminate 45 degrees
c
c commands for density & abundances =========
hden 9.5
abundances cameron
stop lyman optical 6
c
c commands controlling geometry =========
c
c other commands for details =========
init file "ism.ini"
constant gas pressure
iterate to convergence
c
c commands controlling output =========
print diffuse continuum
plot continuum
punch overview "blr_nf84_45deg.ovr"
punch dr "blr_nf84_45deg.dr"
punch results last "blr_nf84_45deg.rlt"
c
c blr_nf84_45deg.in
c class blr
c ========================================
c
This is an example of a "conventional" BLR calculation. The parameters are
similar to those of Table 1 of Netzer and Ferland (1984). Notice that the
ratio of Lyalpha to Hbeta ratio is much larger than observed.
>>refer blr model Netzer, H., & Ferland, G. J. 1984, PASP, 96, 593
blr_rnfa.in table 1 of Rees et al. ApJ 347, 648
title table 1 of Rees et al. ApJ 347, 648
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
c commands for density & abundances =========
hden 10
init file="c84.ini"
abundances he -1 c -3.328 n -4.0088 o -3.0809 ne -4 na -20
continue mg -4.3768 al -5.5686 si -4.36653 s -4.76955
continue a -5.4202 ca -5.6383 fe -4.4815 ni -20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate to convergence
c
c commands controlling output =========
normalise "H 1" 1216 = 100
print line faint -1
punch overview last "blr_rnfa.ovr"
punch continuum last "blr_rnfa.con" units microns
punch transmitted continuum last "blr_rnfa.trn" units rydbergs
punch element nitrogen last "blr_rnfa.nit"
punch dr last "blr_rnfa.dr"
punch results last "blr_rnfa.rlt"
c
c blr_rnfa.in
c class blr
c ========================================
c
This is the lower density cloud computed in Rees et al. (1989).
Table 1 of that paper lists the predictions, which were a mean of those
of Hagai Netzer's ION and roughly version 76 of CLOUDY. The lines
are generally still in good agreement with the predictions of that paper.
In particular the changes in the line fluxes shown in Figure 1
of that paper are reproduced quite well.
blr_rnfb.in table 1 of Rees et al. ApJ 347, 648
title table 1 of Rees et al. ApJ 347, 648
c
c blr model from
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
c commands for density & abundances =========
hden 12
init file="c84.ini"
abundances he -1 c -3.328 n -4.0088 o -3.0809 ne -4 na -20
continue mg -4.3768 al -5.5686 si -4.36653 s -4.76955
continue a -5.4202 ca -5.6383 fe -4.4815 ni -20
c
c commands controlling geometry =========
stop column density 23
c
c other commands for details =========
iterate to convergence
c
c commands controlling output =========
print line faint -1
punch overview last "blr_rnfb.ovr"
punch element nitrogen last "blr_rnfb.nit"
punch dr last "blr_rnfb.dr"
punch results last "blr_rnfb.rlt"
normalise "H 1" 1216 = 91.8
c
c blr_rnfb.in
c class blr
c ========================================
c
This is a very dense cloud, and was computed in Rees et al. (1989).
Table 1 of that paper lists the predictions, which were a mean of those of
Hagai Netzer's ION and roughly version 76 of CLOUDY. The lines are
generally still in good agreement with the predictions of that paper.
In particular the changes in the line fluxes shown in Figure 1 of that
paper are reproduced quite well. The fluxes of Lya and Hb are not
reproduced with great precision by this model because of changes in
collision rates for hydrogen and especially the form of the
escape probability function for subordinate lines. As Figure 1 of
RNF showed the line intensities are very sensitive to density for
these parameters.
coll_coronal.in model of active region of solar corona
title model of active region of solar corona
c
c commands controlling continuum =========
c temperature of corona
coronal equilibrium, 2.5e6 K
c assume the sun is a blackbody at 5770K
blackbody 5770 K
luminosity solar linear 1
c
c commands for density & abundances =========
hden log=10
c
c commands controlling geometry =========
c its height above photosphere and thickness
radius 11 thickness = 10
c the gas fully covers the center of symmetry
sphere
c
c other commands for details =========
iterate
c
c commands controlling output =========
normalize to "o 8" 18.97A
punch dr "coll_coronal.dr" last
punch continuum "coll_coronal.con" last units angstroms
c
c
c coll_coronal.in
c class coronal
c ========================================
c
This is a rough model of the solar corona.
The test checks that the coronal equilibrium commands work.
The gas is predominantly collisionally ionized.
coll_heat_only.in test code in limit where ONLY mechanical heating is present
title test code in limit where ONLY mechanical heating is present
c
c commands controlling continuum =========
no photoionization
blackbody 5000 STE
c
c commands controlling geometry =========
stop column density 15
c
c commands for density & abundances =========
hden 10
c
c other commands for details =========
hextra -1.5
iterate
c
c commands controlling output =========
c this command must be tested somewhere
print cooling, zone 5
c output files
punch overview "coll_heat_only.ovr"
punch heating "coll_heat_only.het"
punch cooling "coll_heat_only.col"
punch convergence reason "coll_heat_only.cvr"
punch dr "coll_heat_only.dr"
punch continuum "coll_heat_only.con" units angstroms
c
c
c coll_heat_only.in
c class coronal
c ========================================
This test is an optically thin collisionally ionized gas with no
photoionization at all.
coll_t3.in coronal equilibrium at 10^4 K
title coronal equilibrium at 10^4 K
c
c commands controlling continuum =========
coronal 3
c add component of cosmic rays to drive chemistry
cosmic ray background
c
c other commands for details =========
iterate
c
c commands controlling geometry =========
stop column density 15
c
c commands for density & abundances =========
hden 10
c
c commands controlling output =========
punch overview "coll_t3.ovr"
punch continuum "coll_t3.con" units angstroms
c
c
c coll_t3.in
c class coronal
c ========================================
This tests conditions of collisional equilibrium at low densities.
This is one of a series of sims coll_t?.in which test ionization
over a range of temperatures. This one, unlike the others,
includes cosmic rays. Chemistry is important at this low temperature
and the chemical network will collapse without a source of ionization.
The cosmic rays provide this source of ionization.
coll_t4.in coronal equilibrium at 10^4 K
title coronal equilibrium at 10^4 K
c
c commands controlling continuum =========
coronal 4
c
c other commands for details =========
iterate
c
c commands controlling geometry =========
stop column density 15
c
c commands for density & abundances =========
hden 10
c
c commands controlling output =========
punch overview "coll_t4.ovr"
punch continuum "coll_t4.con" units angstroms
c
c
c coll_t4.in
c class coronal
c ========================================
this tests conditions of collisional equilibrium at low densities
coll_t5.in coronal equilibrium at 10^5 K
title coronal equilibrium at 10^5 K
c
c commands controlling continuum =========
coronal 5
c
c commands controlling geometry =========
stop column density 15
c
c commands for density & abundances =========
hden 10
c
c other commands for details =========
iterate
c
c
c commands controlling output =========
c normalize to strong HeII line
normalize to "He 2" 303.8A
punch overview "coll_t5.ovr"
punch continuum "coll_t5.con" units angstroms
c
table lines "LineList_He_like.dat"
c coll_t5.in
c class coronal
c ========================================
This is a test collisional ionization equilibrium
at 1e5 K.
coll_t6.in coronal equilibrium at 10^6 K
title coronal equilibrium at 10^6 K
c
c commands controlling continuum =========
coronal 6
c
c commands controlling geometry =========
stop column density 15
c
c commands for density & abundances =========
hden 10
c
c other commands for details =========
iterate
c
c commands controlling output =========
normalize to "c 5" 40.27A
c output files
punch overview "coll_t6.ovr"
punch continuum "coll_t6.con" units angstroms
c
c coll_t6.in
c class coronal
c ========================================
This test is an optically thin collisionally ionized gas.
coll_t7.in coronal equilibrium at 10^7 K
title coronal equilibrium at 10^7 K
c
c commands controlling continuum =========
coronal 7
c
c commands controlling geometry =========
stop column density 15
c
c commands for density & abundances =========
hden 10
c
c other commands for details =========
c
normalize to "o 8" 18.97A
c commands controlling output =========
punch overview "coll_t7.ovr"
punch continuum "coll_t7.con" units angstroms
punch cooling "coll_t7.col"
c
c coll_t7.in
c class coronal
c ========================================
Test with only collisional ionization at a
high temperature.
dynamics_orion_flow.in Orion nebula blister with wind
title Orion nebula blister with wind
c
c commands controlling continuum =========
blackbody 40000
phi(h) 13.0
brems 6
phi(h) 10
c
c commands for density & abundances =========
hden 4
abundances hii region no grains
grains orion no qheat single
c
c commands controlling geometry =========
wind -7 km/s advection
c this accounts for matter beyond end of the model
double optical depths
sphere
stop AV 5
stop temperature linear 5
c
c other commands for details =========
iterate 4
magnetic field -4
cosmic rays background
c this has no effect on dynamics, but is to desaturate the lines as per flow
turbulence 8 km/sec no pressure
c try to speed up simulation without hurting dynamics
init "fast.ini"
c use Bakes & Tielens heating
set PAH Bakes
* init "c84.ini"
* failures 5
c
c commands controlling output =========
c want to print line intensities are surface brightness, per arcsec^2
print lines surface brightness arcsec
print diffuse continuum
print line faint -1.5
punch overview "dynamics_orion_flow.ovr" no hash
punch hydrogen 21 cm "dynamics_orion_flow.21cm" no hash
punch dr "dynamics_orion_flow.dr" no hash
punch continuum last "dynamics_orion_flow.con" units microns no hash
punch pressure "dynamics_orion_flow.pre" no hash
punch heating "dynamics_orion_flow.het" no hash
punch cooling "dynamics_orion_flow.col" no hash
punch molecules "dynamics_orion_flow.mol" no hash
punch wind "dynamics_orion_flow.wnd" last
c
c dynamics_orion_flow.in
c class dynamics hii pdr
c ========================================
c
This is a model similar in spirit to the blister geometry H+ region
model computed by Baldwin et al. (1991), but with a D-critical flow.
Many physical processes have been disabled to make this simulationn faster.
Grain physics is not done so the gas temperature is incorrect. The
main purpose is to do a quick test of the dynamical flow with grain
opacities included. The slow directory contains a full simulation
of a flow like Orion.
dynamics_veryfast.in very fast wind model
title very fast wind model
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
c commands for density & abundances =========
hden 9
c this is a set of commands to speed up calc
init file "fast.ini"
c
c commands controlling geometry =========
stop thickness 8.4
c this is a subsonic wind with advection
wind velo -5 advection
c
c other commands for details =========
c absolutely no convergence problems should occur
failures 1
c this degrades the continuum resolution by factor of 3, to
c speed up calc
set continuum resolution 3
iterate 4
c
c commands controlling output =========
punch pressure last "dynamics_veryfast.pre"
punch total opacity last "dynamics_veryfast.opc"
punch ionizing continuum last "dynamics_veryfast.ion"
punch continuum last "dynamics_veryfast.con"
punch dr "dynamics_veryfast.dr"
c
c
c dynamics_veryfast.in
c class dynamics
c ========================================
c
This is meant to be a very fast calculation to
use when running extensive debug-enabled runtimes.
dynamics_veryfast_rec.in very fast wind model
title very fast wind model
c
c commands controlling continuum =========
table agn
ionization parameter -2
c
c commands for density & abundances =========
hden 9
c this is a set of commands to speed up calc
init file "fast.ini"
c
c commands controlling geometry =========
stop thickness 8.4
c this is a subsonic wind with advection
wind velo 5 advection
c
c other commands for details =========
c absolutely no convergence problems should occur
failures 1
c this degrades the continuum resolution by factor of 3, to
c speed up calc
set continuum resolution 3
iterate 4
c
c commands controlling output =========
punch pressure last "dynamics_veryfast_rec.pre"
punch total opacity last "dynamics_veryfast_rec.opc"
punch ionizing continuum last "dynamics_veryfast_rec.ion"
punch continuum last "dynamics_veryfast_rec.con"
punch dr "dynamics_veryfast_rec.dr"
c
c
c dynamics_veryfast_rec.in
c class dynamics
c ========================================
c
This is meant to be a very fast calculation to
use when running extensive debug-enabled runtimes.
dynamics_wind.in test of equations of motion in a very highly ionized wind
title test of equations of motion in a very highly ionized wind
c
c test motion in electron scattering limit
c radiative acceleration (e- only) is 9.54E-7 cm s^-2
c terminal velocity (e- only) is 7.6 km s^-1
c
c commands controlling continuum =========
table agn
luminosiy (total) 45
c
c commands for density & abundances =========
hden 4
c this only includes H and He
init file="hheonly.ini"
c
c commands controlling geometry =========
radius (parsecs) 1
stop thickness (parsecs) -1
c a slow wind velocity, will assert velocity at outer radius
wind velo 0.1 ball
c
c other commands for details =========
c this will speed things up a bit
no level2
no radiation pressure
constant temperature 8
c
c commands controlling output =========
punch pressure "dynamics_wind.pre"
punch wind "dynamics_wind.wnd"
punch dr "dynamics_wind.dr"
c
c dynamics_wind.in
c class limit dynamics
c ========================================
c
This tests the radiative acceleration and terminal velocity of
a wind in which only electron scattering is important. The parameters
were chosen so that electron scattering is the dominant opacity source,
so that the equations can be solved both numerically (in the example)
and analytically (the expected solution given above). In a realistic wind
the gas would be more neutral and line driving would dominate. The force
multiplier, given in the punch wind output, is nearly unity as a result.
Checks:
- The radiative acceleration is correct (e- 9.543910-7 cm s-2).
- The terminal velocity should be 7.57 km s-1.
- Force multiplier near unity (no line driving since so highly ionized).
- Thickness of cloud correct (R-Ro + dr/2 should be 3.086391017 cm).
feii_hin.in test feii in high density limit
title test feii in high density limit
c
c commands controlling continuum =========
black 25000 K
ionization -10
c
c commands for density & abundances =========
hden 18
c force a high electron density to insure collisions dominate
eden 18
c
c commands controlling geometry =========
constant tempera 4
stop zone 1
c
c other commands for details =========
atom feii
iterate
c want to test collision only limit
no induced processes
c
c commands controlling output =========
c
c
c feii_hin.in
c class limit
c ========================================
c
This checks that, at high particle densitites, in which
the gas should be in collisional
equilibrium, the level populations of the large model Fe+ ion
go to the proper values, where the departure coefficients
are all equal to unity.
feii_hirad.in feii in case of high radiation density limit
title feii in case of high radiation density limit
c
c commands controlling continuum =========
black 8000 K lte
c
c commands for density & abundances =========
hden 9
element iron abundance 2
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
atom feii
constant tempera 8000
iterate
c
c commands controlling output =========
punch feii relative populations range 0 200 "feii_hirad.lv1" last
punch feii relative populations range 201 371 "feii_hirad.lv2" last
c
c
c feii_hirad.in
c class limit
c ========================================
c
This checks that, at high radiation densitites, in which
the gas is irradiated by a blackbody in strict thermodynamic
equilibrium, the level populations of the large model Fe+ ion
go to the proper values, where the departure coefficients
are all equal to unity.
feii_pump.in test feii in continuum pumped limit
title test feii in continuum pumped limit
c
c commands controlling continuum =========
black 25000 K
ionization -5
c
c commands for density & abundances =========
hden 10
abundances old solar 84
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
Case B
iterate
constant tempera 4
atom feii
c
c commands controlling output =========
punch feii continuum "feii_pump.con"
c
c feii_pump.in
This is a constant temperature low ionization
cloud, with BLR-like densities, which includes the
large FeII atom. The tests check on the emission
predicted in the Fe II bands.
This model tests the large FeII model in the optically thin,
continuum pumped limit. The zone thickness is set to a
small value (1 cm) so that full continuum hits atom.
feii_ste.in thermal equilibrium of FeII in STE limit
title thermal equilibrium of FeII in STE limit
c
c commands controlling continuum =========
black 8000 K lte
hden 9
c
c commands for density & abundances =========
element iron abundance 2
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
atom feii
iterate
c
c commands controlling output =========
punch feii continuum last "feii_ste.con"
punch feii column density last "feii_ste.col"
punch feii populations all last "feii_ste.pop"
c
c feii_ste.in
c class function
c ========================================
c
This model has a very high iron abundance, 100x H, and most Fe is
in the form of Fe+. It is irradiated by a blackbody in strict
thermodynamic equilibrium. We check that the temperature
of the gas is equal to the radiation temperature, to confirm
that the thermal properties of the model FeII atom obey thermodynamics.
feii_t4.in FeII emission in typical intermediate density photoionzied cloud
title FeII emission in typical intermediate density photoionzied cloud
c
c commands controlling continuum =========
black 5e5K
ionization parameter -2
c
c commands for density & abundances =========
hden 8
element iron abundance 2
element iron ionization -2 0 -2
c
c commands controlling geometry =========
stop thickness 5
c
c other commands for details =========
constant temperature 4
atom feii
iterate 3
c
c commands controlling output =========
set line precision 6
print lines column
print line inward
print line sort wavelength
print line faint 0
punch feii continuum last "feii_t4.con" units angstroms
punch feii inward continuum last "feii_t4.cin" units angstroms
punch feii outward continuum last "feii_t4.cout" units angstroms
punch feii column density last "feii_t4.col"
punch feii populations all last "feii_t4.pop"
punch line emissivity "feii_t4.ems"
Fe2b 2797
Inwd 2797
end of lines
c
c feii_t4.in
c class function
c ========================================
c
This model has a very high iron abundance, 100x H, and most Fe is
in the form of Fe+. it has intermediate density and should produce
and FeII spectrum something like an AGN.
The set line precision 6 increases the number of significant figures
in the wavelengths for each line. This is needed to get the right
FeII inward band.
func_abund_fluc.in check fluctuating heavy-element abundances
title check fluctuating heavy-element abundances
c commands controlling continuum =========
blackbody 5
ionization -2
c
c commands for density & abundances =========
hden 3
c this varies the abundnaces between default and 1e-4 times default,
c over a 1e10 cm period - we will compute half a cycle
fluctuatsion abundances 10.3 0 -4
c
c commands controlling geometry =========
c stop at half a cycle so pick off lowest abundances
stop thickness 10
c
c other commands for details =========
c speed things up a bit
init "c84.ini"
c
c commands controlling output =========
print column density
punch overview "func_abund_fluc.ovr"
punch abundances "func_abund_fluc.abn"
c
c commands giving asserts
c
c func_abund_fluc.in
c class function
c ========================================
c
This checks that the variable abundances option works
func_distance.in check that distance and "print flux earth" commands work
title check that distance and "print flux earth" commands work
c
c commands controlling continuum =========
c luminosity in ionizing radiation, this and distance
c were chosen so that flux at earth assocated with total
c luminoisity of object is 1 erg cm-2 s-1
luminosity 40
laser 2
c
c commands for density & abundances =========
hden 4
init file "honly.ini"
c
c commands controlling geometry =========
stop zone 1
radius 17
c
c other commands for details =========
distance 19.450395
constant temperature 4
c
c commands controlling output =========
c give flux at Earth
print lines, flux at Earth
c
c func_distance.in
c class function
c ========================================
c
Normally the code predicts the intensity or luminosity of
the emission lines. This test confirms that it can predict
the flux recieved at the Earth instead. The model is the simplest
and fastest that can be computed - a H-only constant temperature
single zone. The total luminosity is set to 1e40 erg/s, and the
ionization source is a laser at 2 ryd. With these set, the
total luminosity in ionizing radiation, the total luminoisity in
the incident continuum (the emission line labeled "Inci 0") will be 1e40.
The code will predict the flux at the Earth if both the distance to the
oject is specified with the distance command, and this is requested with
the print flux earth command. The distance was chosen so that the
total flux at the Earth will be 1 erg/s. This is asserted at the
end of the calculation.
func_dlaw.in test model with dlaw table
title test model with dlaw table
c
c commands controlling continuum =========
phi(H) 15
table agn
c
c commands for density & abundances =========
dlaw table radius
continue 16 9
continue 17 7
continue 18 5
continue 19 3
continue 20 1
continue 21 -1
end of dlaw
init "honly.ini"
c
c commands controlling geometry =========
sphere
filling factor -5
radius 17 20
c
c other commands for details =========
constant temperature 4
c
c commands controlling output =========
punch dr "func_dlaw.dr"
punch overveiw "func_dlaw.ovr"
c
c
c func_dlaw.in
c class function
c ========================================
c
this model tests the dlaw density table command
func_fulltrace.in test full trace output
title test full trace output
c
c commands controlling continuum =========
trace h-like hydrogen full no print
stop zone 1
table agn
ionization parameter -0.5
c
c commands for density & abundances =========
hden 9.5
init file="honly.ini"
c
c other commands for details =========
atom h-like element hydrogen collapsed levels 1
c
c commands controlling output =========
c func_fulltrace.in
c class function
c ========================================
this checks that trace output functions correctly
func_globule.in test of globule command
title test of globule command
c
c commands controlling continuum =========
black 40000 K
ionization parameter -1.5
c
c commands for density & abundances =========
globule initial density=5 scale depth=14
init file "ism.ini"
abundances hii region no qheat
c
c commands controlling geometry =========
c
c other commands for details =========
failures 2
no diffuse line pumping
c
c commands controlling output =========
print line faint -1.5
punch overview last "func_globule.ovr"
punch results last "func_globule.rlt"
punch dr "func_globule.dr" last
punch heating "func_globule.het" last
punch cooling "func_globule.col" last
c
c func_globule.in
c class function
c ========================================
c
This model uses the globule command, tests that the zoning logic
works for this extreme case, and that the code is able to converge
the globule model.
func_grid_line_ratios.in test generating line ratios in a grid run
title test generating line ratios in a grid run
c
c commands controlling continuum =====
blackbody 40,000K
ionization parameter -2
c
c commands for density & abundances =====
c these are to speed up the calculation, only do H, O, and Ne
init "honly.ini"
element oxygen on
element neon on
element sulphur on
element oxygen ionization 1 1 1 0.01
element neon ionization 1 1 1 0.01
element sulphur ionization 1 1 1 0.01
c vary the hydrogen density
hden 4 vary
grid 2 6.1 1
c
c other commands for details =======
c these are constant temperature models, vary T
constant temperature 4 vary
grid 4000 17000 3000
stop zone 1
c
c commands controlling output =====
punch line list "func_grid_line_ratios.pun" "func_grid_line_ratios.dat" ratio no hash
punch grid "func_grid_line_ratios.grd"
c
c commands giving (lack of) assert ==========
c
c func_grid_line_line_ratios.in
c class function
c ===================================================
This uses the grid command to compute line ratios for a wide range of
density and temperature. The ionization is set to a uniform value and
only a few elements are included. this makes the calculation faster
and prevents recombination [O III] 4363 from becoming important (there
is no O+3).
These are the line ratios mentioned as limits in the Johnstone et al.
Spitzer cooling flow filament paper (2007).
func_hotgas_coolstar.in test very soft continuum, very hot gas
title test very soft continuum, very hot gas
c
c commands controlling continuum =========
c put in the cosmic background as the only continuum source
CMB
c gas has constant temperature of 1e6 K
constant temperature, t=6
c
c commands for density & abundances =========
hden 10.
c
c commands controlling geometry =========
stop zone 1
c specify a thin cell of gas - 1 cm thick
set dr 0
c
c other commands for details =========
c iterate since gas is optically thin
iterate
c
c commands controlling output =========
c
c func_hotgas_coolstar.in
c class limit
c ========================================
c
This is a test where the CMB is the only continuum source.
It does not extend to energies where the
code needs to work. There are special cases
used in this situation, for continuum addressing,
so this checks whether those still function.
func_ion_increase.in test model where ionization increases with depth
title test model where ionization increases with depth
c
c commands controlling continuum =========
ionization parameter -4
table agn
c
c commands for density & abundances =========
hden 7 -4
init "hheonly.ini"
element oxygen on
element iron on
c
c commands controlling geometry =========
sphere
filling factor -5
radius 17 20
c
c other commands for details =========
constant temperature 4
c
c commands controlling output =========
punch dr "func_ion_increase.dr"
punch overveiw "func_ion_increase.ovr"
punch element oxygen "func_ion_increase.oxy"
punch element iron "func_ion_increase.fe"
c
c
c func_ion_increase.in
c class function
c ========================================
c
This density falls off faster than 1/r^2 so the ionization increases
with depth. Most sims have decreasing rather than increasing ionization.
func_lines.in create output file with list of func_lines
title create output file with list of func_lines
atom h2 levels large
atom feii
test
c
c commands controlling continuum =========
c commands for density & abundances =========
c commands controlling geometry =========
c other commands for details =========
c
c commands controlling output =========
c this creates the file "func_lines.lab that contains a list
c of all emission labels
punch line labels "func_lines.lab"
c this creates the file "func_lines.lis" that contains a list
c of the emission func_lines that are transported.
punch line data "func_lines.lis"
c
c There is nothing extra to assert, since test does include many asserts
c
c func_lines.in
c class function
c ========================================
c
This runs the standard "test" case, and then creates
the line data and labels files. Test by itself includes
many asserts, so no further asserts are needed here.
The file func_lines.lab is a useful list of all lines predicted by the code.
Cut and paste this into other places when you need to find a particular
emission line.
The func_lines lines.dat gives atomic data for all the lines, and their
critical density at 10000 K.
The large H2 and Fe II model atoms are turned on to include their lines.
func_map.in map of heating vs cooling
title map of heating vs cooling
c
c commands controlling continuum =========
table agn
ionization parameter -2.5
c
c commands for density & abundances =========
hden 0
abundances old solar 84
c
c commands controlling geometry =========
set dr 0
stop lyman optical depth -7
stop zone 1
c
c other commands for details =========
c
c commands controlling output =========
c save map information to generate plot for hazy
punch map file="func_map.dta"
set nmaps 100
c
c map.in
c class function
c ========================================
c
This is a test of the continuity of the code over a very large range
of temperature. It was used to produce one of the thermal maps shown in Hazy.
Checks:
- No breaks in the heating and cooling curves where
various approximations change.
func_sdrmin.in test set drmin command
title test set drmin command
c
c commands controlling continuum =========
blackbody 8e4
luminosity 37.5
c
c commands for density & abundances =========
hden 4
c
c commands controlling geometry =========
radius 17
sphere
stop thickness 17.03
stop temperature off
c
c other commands for details =========
set drmin 15.5
cosmic rays background
c
c commands controlling output =========
punch dr "func_sdrmin.dr" last
c
This simulation tests the SET DRMIN command. It is a toy model of a planetary
nebula that is designed to extend into the PDR. The minimum stepsize is
deliberately set much too large so that we would immediately notice if the
command was broken. It also tests if we still hit the correct outer radius
when SET DRMIN is used. Without the SET DRMIN command this sim would need
410 zones (trunk@2760).
func_set_ion.in test impact of setting ionization
title test impact of setting ionization
c
c commands for density & abundances =========
init "ism.ini"
hden 0
element hydrogen ionization 0 1
element helium ionization 0 1 0
element carbon ionization 0 1
element oxygen ionization 0 0.1 0.2 0.3 0.2 0.1 0.1
c
c commands controlling continuum =========
blackbody 5
ionization parameter -2
c
c commands controlling geometry =========
c force model to be 1 cm thick
set dr 0
c
c other commands for details =========
constant temperature 4
stop zone 1
c
c commands controlling output =========
normalize to "O 3" 5007
punch dr "func_set_ion.dr"
c
c
c func_set_ion.in
c class function
c ========================================
c
this script exercies the option to specify the ionization of a species
func_stopline1.in test stop line command
title test stop line command
c
c commands controlling continuum =========
ionization parameter -2
blackbody 50000
c
c commands for density & abundances =========
hden 2
abundances old solar 84
init file "ism.ini"
c test option to turn off elements with small abundances
element limit off -5
c
c commands controlling geometry =========
c stop calc at line ratio, the point of this test
stop line "C 2" 157.6m reaches 0.0358
c
c other commands for details =========
constant temperature 10000 K
c
c commands controlling output =========
punch dr "func_stopline1.dr" last
c
c func_stopline1.in
c class function
c ========================================
c
This is an example of a simple calculation that stops when
a line reaches a specified intensity.
The option to turn off elements with trivial abundances is used.
func_stopline2.in test stop line command
title test stop line command
c
c commands controlling continuum =========
ionization parameter -2
blackbody 50000
c
c commands for density & abundances =========
hden 2
abundances old solar 84
init file "ism.ini"
c
c commands controlling geometry =========
c stop calc at line ratio, the point of this test
stop line "C 2" 157.6m reaches 0.002 relative to "o 3" 5007 A
c
c other commands for details =========
constant temperature 10000 K
c
c commands controlling output =========
normalise to "o 3" 5007
punch dr "func_stopline2.dr" last
c
c func_stopline2.in
c class function
c ========================================
c
this is an example of a simple calculation that stops when
a certain emission line ratio is reached
func_t10.in test very soft continuum, very hot gas
title test very soft continuum, very hot gas
c
c commands controlling continuum =========
table agn
ionization parameters -2
c
c commands for density & abundances =========
hden 1.
c
c commands controlling geometry =========
stop zone 1
c specify a thin cell of gas - 1 cm thick
set dr 0
c
c other commands for details =========
c set constant temperature to high-T limit
constant temperature, t=10 log
c iterate since gas is optically thin
iterate
c
c commands controlling output =========
c
c
c func_t10.in
c class limit
c ========================================
c
This is a test of the highest temperature the code can do.
func_t3.in test low temperature limit of code, 3K
title test low temperature limit of code, 3K
c
c commands controlling continuum =========
table agn
ionization parameters -2
c
c commands for density & abundances =========
hden -1
c
c commands controlling geometry =========
stop zone 1
c specify a thin cell of gas 1 cm thick
set dr 0
c
c other commands for details =========
c set constant temperature to low-T limit
constant temperature, t=3.0 linear
c iterate since gas is optically thin
iterate
c
c commands controlling output =========
c
c
c
c func_t3.in
c class limit
c ========================================
c
This is a test of the lowest temperature the code can do.
It runs a constant temperature of 3K
func_test.in run smoke test
title run smoke test
c commands controlling continuum =========
test
c commands for density & abundances =========
c commands controlling geometry =========
c other commands for details =========
c include this in one test to make sure it works
set continuum shield ferland
c
c commands controlling output =========
c increase precision of all printed wavelengths
set line precision 6
c following will print physical constants used by the code
print constants
c print the past to the data directory
print path
c the citation for the current version of the code
print citation
c following prints column densities
print column density
punch overview "func_test.ovr"
c func_test.in
c class function
c ========================================
c
This runs the smoke test command, which include several asserts.
The tests the behavior of increasing the number of significant figures
in printed wavelengths.
func_testmole.in this runs the standard, one command, test, which contains many asserts
title this runs the standard, one command, test, which contains many asserts
c commands controlling continuum =========
test mole
c
c commands for density & abundances =========
c commands controlling geometry =========
c other commands for details =========
c
c commands controlling output =========
punch overview "func_testmole.ovr"
c func_testmole.in
c class function
c ========================================
c
This runs the "test mole" command, which include several asserts.
func_trans_punch.in first of func_trans_punch/transread pair, punch continuum
title first of func_trans_punch/transread pair, punch continuum
c
c commands controlling continuum =========
ionization parameter -1
table agn
c
c commands for density & abundances =========
hden 10
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
iterate
c
c commands controlling output =========
print incident continuum
punch ionization last "func_trans_punch.ion"
punch continuum last "func_trans_punch.con"
c this continuum will be used by transread.in
punch last transmitted continuum "func_trans_punch.trn"
c
c this contains a large number of asserts that both tests use
init file "trans.dat"
c
c func_trans_punch.in
c class function
c ========================================
c
func_trans_punch.in and transread.in are a pair of
tests that check that the code can punch a transmitted
continuum then read it.
This sim must come before func_trans_read since it
generates the punch file needed by func_trans_read.
Alphabetical order insures this.
func_trans_read.in second of transpunch/transread pair, used transmitted continuum
title second of transpunch/transread pair, used transmitted continuum
c the transmitted continuum produced by func_trans_punch
c
c commands controlling continuum =========
ionization parameter -1
table read "func_trans_punch.trn"
brems 6
ionization parameter -6
c
c commands for density & abundances =========
hden 10
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
iterate
c
c commands controlling output =========
c this contains a large number of asserts used by both commands
init file "trans.dat"
print incident continuum
punch ionization last "func_trans_read.ion"
c
c
c func_trans_read.in
c class function
c ========================================
c
func_trans_punch.in and func_trans_read.in are a pair of
tests that check that the code can punch a transmitted
continuum then read it.
grains_conserve_pp.in test energy conservation with vastly optically thick dust
title test energy conservation with vastly optically thick dust
c
c commands controlling continuum =========
black 500 STE
c
c commands for density & abundances =========
init "honly.ini"
hden 0
grains ism single graphite
c
c commands controlling geometry =========
stop Av 1000
sphere
stop temperature 100K
c
c other commands for details =========
iterate
constant temper 500 K
no grain gas collisional energy exchange
no molecules
cosmic rays background
c
c commands controlling output =========
punch grain temperature "grains_conserve_pp.grntem"
punch continuum units microns "grains_conserve_pp.con"
c
c
c grains_conserve_pp.in
c class limit
c ========================================
c
This tests that multiple absorption / reemission by dust conserves energy
Energy density and grain temperatures should be exactly 500 K
grains_conserve_sp.in test energy conservation with vastly optically thick dust, sphere geometry
title test energy conservation with vastly optically thick dust, sphere geometry
c
c commands controlling continuum =========
black 500 STE
c
c commands for density & abundances =========
init "honly.ini"
hden 3.25 -2
grains ism single graphite
c
c commands controlling geometry =========
radius from 21 to 26
* stop Av 1000
sphere
stop temperature 100K
c
c other commands for details =========
iterate
constant temper 500 K
no grain gas collisional energy exchange
no grain electrons
no molecules
cosmic rays background -10
c
c commands controlling output =========
punch grain temperature "grains_conserve_sp.grntem"
punch continuum units microns "grains_conserve_sp.con"
c
c
c grains_conserve_sp.in
c class limit
c ========================================
c
This tests that multiple absorption / reemission by dust conserves energy
in a spherical geometry.
Radiation density temperature in last zone should be 500 * sqrt(1e21/1e26) = 1.5811 K
grains_hot.in test temperature of gas and dust in high energy density environment
title test temperature of gas and dust in high energy density environment
c
c commands controlling continuum =========
table power law
c intensity of incident radiation field set by its energy density
energy density temp 550 K
c
c commands for density & abundances =========
hden 5.0
init "ism.ini"
c Orion grains and abundances
abundances orion
c
c commands controlling geometry =========
stop zone 1
set drmax 10
c
c other commands for details =========
c
c commands controlling output =========
normalize to "O 8" 18.97A
punch overview "grains_hot.ovr" last
c
c
c grains_hot.in
c class limit
c ========================================
c
This tests the grains in an extreme condition - irradiation by an AGN
near the illuminated face of the molecular torus. The gas is
predominantly heated by the grain electron photo-ejection.
grains_hot_wd01.in test temperature of gas and dust in high energy density environment
title test temperature of gas and dust in high energy density environment
c
c commands controlling continuum =========
table power law
energy density temp 550
c
c commands for density & abundances =========
hden 5.0
init "ism.ini"
abundances orion no grains
grains orion no qheat
c
c revert to WD01 treatment
no grain x-ray treatment
c
c commands controlling geometry =========
stop zone 1
set drmax 10
c
c other commands for details =========
c
c commands controlling output =========
normalize to "O 8" 18.97A
punch overview "grains_hot_wd01.ovr" last
c
c
c grains_hot_wd01.in
c class limit
c ========================================
c
This tests the grains in an extreme condition - irradiation by an AGN
near the illuminated face of the molecular torus. The gas is
predominantly heated by the grains. The grain treatment has been
reverted to Weingartner & Draine, 2001, which is NOT appropriate
for these conditions. It is however a good test whether the old
treatment is not broken....
grains_lte.in check that grains equilibriate at correct temp in ste limit
title check that grains equilibriate at correct temp in ste limit
c this also tests that the code works when H He ionization is ZERO
c
c commands controlling continuum =========
black 3 lte
c
c commands for density & abundances =========
hden 5
eden 5
init file "hheonly.ini"
c need to normalize to some line, oxygen will provide some
element oxygen on
c ism grains with high dust to gas ratio
grain abund 1
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
iterate
c the equilibrium temp would not be correct since small H_2 molecule
c does not go to ste, being an equivalent two-level system
constant temperature 3
c
c commands controlling output =========
normalize to "O 1" 63.17m
punch heating last "grains_lte.het"
punch cooling last "grains_lte.col"
c
c grains_lte.in
c class limit
c ========================================
c
This test irradiates a set of grains with a true blackbody in
strict thermodynamic equilibrium. We expect the grains
(and everything else) to equilibriate at the blackbody temperature.
The gas temperature is forced to the radiation temperature because
the current molecule network (based on ISM approximations) does not
go to LTE in the high-radiation density limit. The calculation
asserts that all grain temperatures are very close to the radiation
temperature.
grains_qheat.in cool atomic ISM with Si grain quantum heating
title cool atomic ISM with Si grain quantum heating
c
c commands controlling continuum =========
table draine
extinguish 20
c
c commands for density & abundances =========
hden 0
c turns on grains with default abundance (log abundance ratio to ism = 0)
c and with quantum heating enabled by default
c (disabled with "no grains qheat" option)
grains 0. "silicate_ism_10.opc"
c
c commands controlling geometry =========
stop zone 1
set dr 0
c
c other commands for details =========
cosmic rays background
iterate
c
c commands controlling output =========
normalize to "C 2" 157.6m
print diffuse continuum
print line faint -2
print line column
punch grains temperature last "grains_qheat.qht"
punch continuum "grains_qheat.con" units microns last
punch two photon continuum "grains_qheat.2nu" units microns
c
c
c grains_qheat.in
c class limit
c ========================================
c
This sim produces dust emission with a Wein trail that is
dominated by quantum heating emission.
grains_temp.in test all grain species temperature
title test all grain species temperature
c
c commands controlling continuum =========
black 50000
ionization parameter -2
c
c commands for density & abundances =========
hden 3
grains_temp "graphite_ism_01.opc"
grains_temp "silicate_ism_01.opc"
grains_temp "graphite_orion_01.opc"
grains_temp "silicate_orion_01.opc"
grains_temp "silicate_0m010.opc"
grains_temp "silicate_0m100.opc"
grains_temp "grey_ism_01.opc"
grains_temp "silicate_1m000.opc"
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
iterate
constant temper 4
c
c commands controlling output =========
c
c
c grains_temp.in
c class limit
c ========================================
c
This turns on all the grain species that are included in the distribution.
A model of an ionized layer is
done and the monitors confirm the resulting grain temperatures.
grains_temp_all.in test all grain species temperature
title test all grain species temperature
c
c commands controlling continuum =========
black 50000
ionization parameter -2
c
c commands for density & abundances =========
hden 3
c this turns on orion-style distributed grains
grains orion
c this turns on ism distributed grains
grains ism
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
constant temper 4
iterate
c
c commands controlling output =========
punch dr "grains_temp_all.dr" last
punch grain charge "grains_temp_all.grnchr" last
punch grain temperature "grains_temp_all.grntem" last
punch grain drift velocity "grains_temp_all.grndft" last
c
c grains_temp_all.in
c class limit
c ========================================
c
This is a relatively quick test of grains.
The Orion and ISM silicate and graphitic grains
are turned on and their equilibrium temperature
checked.
h2_cr.in H2 with background cosmic ray ionization
title H2 with background cosmic ray ionization
c
c commands controlling continuum =========
c this is hot star SED
black 30000
intensity -5. range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c background CR ionization rate of 2.5e-17 s^-1,
cosmic rays, background
c
c commands for density & abundances =========
hden 5
c
c commands controlling geometry =========
set dr 0
stop zone 5
stop temperature 400
c
c other commands for details =========
c failures should not occur
failures 1
atom h2
iterate
c want clean test of CR physics so set constant kinetic temperature
constant temperature 500K
c must turn off line photoexcitation and Solomon process
c since we want to test cr heating and ionization
no induced processes
c
c commands controlling output =========
print column density
print ages
punch overview "h2_cr.ovr" last
punch h2 lines "h2_cr.lin" last all
punch h2 rates "h2_cr.rat" last
punch h2 column density "h2_cr.col" last
c
c
c h2_cr.in
c class limit
c ========================================
c
This test conditions of cosmic ray ionization.
Solar abundances with no dust are assumed so this involves
gas-phase chemistry alone.
The Solomon process is disabled with the "no induced processes' command
so H2 is mainly dissociated by cosmic rays.
This forms a pair with h2_cr_grains, which does include grains.
h2_cr_grains.in background cosmic ray ionization by suprathermal electrons only
title background cosmic ray ionization by suprathermal electrons only
c
c commands controlling continuum =========
c this is hot star continuum
black 30000
intensity -5. range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c background CR ionization rate should be 2.5e-17 s^-1,
c Tielens & Hollenbach 1985; McKee AstroPH 9901370
cosmic rays, background
c
c commands for density & abundances =========
abundances ism
hden 5
c
c commands controlling geometry =========
set dr 0
stop zone 5
stop temperature 400
c
c other commands for details =========
set h2 grain formation thermal pump
atom h2
iterate
constant temperature 500K
c must turn off line photoexcitation
c since we want to test cr heating and ionization
no induced processes
c
c commands controlling output =========
normalize to "H2 " 2.121m
print column density
print ages
punch overview "h2_cr_grains.ovr" last
punch h2 lines "h2_cr_grains.lin" last all
punch h2 rates "h2_cr_grains.rat" last
punch h2 column density "h2_cr_grains.col" last
punch grains H2rates "h2_cr_grains.h2r" last
c
c h2_cr_grains.in
c class limit
c ========================================
c
This tests conditions of cosmic ray ionization and grain formation pumping.
Solomon process is turned off with the "no induced processes" command
so cosmic rays are the main dissociation process.
This forms a pair with h2_cr which does not include grains, so relies
only on gas-phase chemistry.
h2_hminus.in H2 populations in H- dominated limit
title H2 populations in H- dominated limit
c this is one of a pair with h2_solomon.in
c
c commands controlling continuum =========
c this is hot star continuum
black 30000
intensity -5. range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c background CR ionization rate should be 2.5e-17 s^-1,
c Tielens & Hollenbach 1985; McKee AstroPH 9901370
cosmic rays, background
c
c commands for density & abundances =========
c no grains in this sim so H2 forms by H- route
abundances ism no grains
hden 5
c
c commands controlling geometry =========
set dr 0
stop zone 5
stop temperature 400
c
c other commands for details =========
c default is Takahashi 2001 - test thermal distribution here
set h2 grain formation thermal pump
atom h2
iterate
constant temperature 500K
c
c commands controlling output =========
print column density
print ages
punch overview "h2_hminus.ovr" last
punch h2 lines "h2_hminus.lin" last all
punch h2 rates "h2_hminus.rat" last
punch h2 column density "h2_hminus.col" last
c
c h2_hminus.in
c class limit
c ========================================
c
This tests large H2 model in limit of H- formation and Solomon destruction.
h2_pdr_leiden_f1.in low density and flux model 1
title low density and flux model 1
atom H2 He collisions new
c
c commands controlling continuum =========
c Use the Draine 1978 field, for a semi-infinite slab we have to use half
c the requested value, so the actual value
c they want for the model is actually twice the value below
table draine 5
c this is to insure that no H-ionizing radiation strikes the cloud
extinguish 24
c
c commands for density & abundances =========
c hydrogen density
hden 3.
grains ism 1.16 no qheat
c
c commands controlling geometry =========
c
c other commands for details =========
c turn on the large H2 model
atom h2
c turn down the number of convergence failures - there should be none
failures 3
c use leiden initialization file
init file="pdr_leiden.ini"
c This command defines the grain temperature to be a constant 20 Kelvin
constant grain temperature 20
c This sets the gas kinetic temperature to a constant 50 Kelvin
constant temperature 50 linear
c
c commands controlling output =========
c default normalization line is Hbeta, which is not produced by this gas
normalize to "C 2" 157.6m
print line faint -4
punch overview "h2_pdr_leiden_f1.ovr"
punch line emissivity "h2_pdr_leiden_f1.ems"
H2 2.121m
12CO 647.2m
C 2 157.6m
O 1 63.17m
Si 2 34.81m
end of lines
punch leiden lines "h2_pdr_leiden_f1.lin"
punch leiden "h2_pdr_leiden_f1.lei"
punch dr "h2_pdr_leiden_f1.dr"
punch molecules "h2_pdr_leiden_f1.mol"
punch grain physical conditions "h2_pdr_leiden_f1.grn"
punch overview "h2_pdr_leiden_f1.ovr"
punch H2 lines "h2_pdr_leiden_f1.h2lin" all
punch H2 column density "h2_pdr_leiden_f1.h2col"
punch H2 populations matrix zone "h2_pdr_leiden_f1.pop"
punch H2 rates "h2_pdr_leiden_f1.rat"
c
c
c h2_pdr_leiden_f1.in
c class pdr
c ========================================
c
This is one of the tests in Rollig et al. 2007, A&A, 467, 187
h2_solomon.in H2 populations in solomon dominated limit
title H2 populations in solomon dominated limit
c this is a pair with h2_hminus
c
c commands controlling continuum =========
c this is hot star continuum
black 30000
intensity -5. range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c background CR ionization rate should be 2.5e-17 s^-1,
c Tielens & Hollenbach 1985; McKee AstroPH 9901370
cosmic rays, background
c
c commands for density & abundances =========
abundances ism
hden 5
c
c commands controlling geometry =========
set dr 0
stop zone 5
stop temperature 400
c
c other commands for details =========
c default is Takahashi 2001 - test thermal distribution here
set h2 grain formation thermal pump
atom h2
iterate
constant temperature 500K
c
c commands controlling output =========
c don't print so many lines
print line faint 10
print line column
print line sort wavelength
print column density
print ages
punch overview "h2_solomon.ovr" last
punch h2 lines "h2_solomon.lin" last all
punch h2 rates "h2_solomon.rat" last
punch h2 column density "h2_solomon.col" last
c
c h2_solomon.in
c class limit
c ========================================
c
This test H2 in case of grain formation and solomon destruction
h2_t2000.in test large H2 molecule in shock-like conditions
title test large H2 molecule in shock-like conditions
c
c commands controlling continuum =========
c there is a continuum but it is unimportant
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
black 30000
intensity -5 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c must provide source of ionization for chemistry
cosmic rays, background
c
c commands for density & abundances =========
hden 6
grains ism, abundance log 0.16 single
init file="ism.ini"
abundances he -1.01 c -3.52 n-8 o-3.30 ne-8 mg-5.89
continue si -6.10 s -5.10 cl=-7 ar-8 fe -6.60
c
c commands controlling geometry =========
stop zone 10
c force zone thickess to 1 cm
set dr 0
c need to lower stop temperature since gas is cooler than 4000K
stop temperature 3
c
c other commands for details =========
failures 2
atom h2
constant temperature 2000
iterate
c this stop Lymnan line excitation of H, which is then photoionized
c by Balmer continuum
case b
c
c commands controlling output =========
normalize to "H2 " 2.121m
c
punch pdr "h2_t2000.pdr"
punch h2 rates "h2_t2000.rat"
punch h2 column density "h2_t2000.col"
punch h2 lines "h2_t2000.lin" all last
punch h2 populations "h2_t2000.pop" all last
punch raw continuum "h2_t2000.raw"
punch continuum "h2_t2000.con"
punch overview "h2_t2000.ovr"
c
c h2_t2000.in
c class limit
c ========================================
This is a collisionally dominated H2 simulation. The temperature
has been fixed at 2000K and the large molecule turned on. The calculation
checks the returned value of the ortho to para densities.
Cosmic rays and the incident continuum have little effect, the density is high,
so the populations should be close to LTE.
h2_t500.in test large H2 molecule in PDR-like conditions
title test large H2 molecule in PDR-like conditions
c
c commands controlling continuum =========
c first continuum is FIR hot grain continuum produced in
c unmodeled HII Region
blackbody, t = 75 K
intensity -2.7 (total)
c this is hot star continuum
black 30000
intensity -5 range 0.4412 to 1 Ryd
c this will remove all ionizing radiation
extinguish 24 0
c
c commands for density & abundances =========
hden 6
grains ism, abundance log 0.16 single, no qheat
init file="ism.ini"
abundances he -1.01 c -3.52 n-8 o-3.30 ne-8 mg-5.89
continue si -6.10 s -5.10 cl=-7 ar-8 fe -6.60
turbulence 2.7 km/sec
c
c commands controlling geometry =========
stop zone 10
c force zone thickess to 1 cm
sphere
set dr 0
c stop when gas is fully neutral
stop efrac -10
c stop when gas is cold
stop temperature 10 linear
c
c other commands for details =========
failures 2
atom h2
constant temperature 500
iterate
case b
cosmic rays background
c
c commands controlling output =========
normalize to "12CO" 863.0m
c uv lines are strongly pumped by stellar continuum, break out contribution
print line pump
print line optical depths
print line faint -2
print ages
c
punch pdr "h2_t500.pdr"
punch H2 rates "h2_t500.rat"
punch H2 lines "h2_t500.lin" all
punch H2 column density "h2_t500.col"
punch H2 populations "h2_t500.pop"
punch H2 levels "h2_t500.lev"
punch raw continuum "h2_t500.raw"
punch continuum "h2_t500.con"
punch overview "h2_t500.ovr"
c
table lines "LineList_PDR_H2.dat"
c h2_t500.in
c class limit
c ========================================
This is a dense molecular gas with background cosmic rays and the incident
radiation field set to a small value. The lower levels are in LTE.
h_otsopen.in test ots, inward fractions for pure hydrogen, open geo, filling factor
title test ots, inward fractions for pure hydrogen, open geo, filling factor
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 5
init file "honly.ini"
c
c commands controlling geometry =========
stop efrac 0.05 %stop when 5 percent ionized
constant temper 7500
filling factor 0.01
c
c other commands for details =========
c must iterate to get inward line fractions, that are asserted below
iterate
diffuse ots
c not iterating does not affect the solution
no level2
no induced processes (OK)
c
c commands controlling output =========
print diffuse continuum
print line inward
punch overview "h_otsopen.ovr" last
punch dr "h_otsopen.dr" last
punch continuum "h_otsopen.con" last units angstrom
normalize to "Ca B" 4861 = 1 % normalize to exact result
c
c this is an open geometry, so do not expect H atom to exactly be case B
c due to Lyman line leakage. we iterated, so have a good estimate of
c inward and outward fractions, which we test
c h_otsopen.in
c class limit
c ========================================
c
This tests the total emission from a hydrogen Stromgren sphere
using the OTS approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
h_otspp.in plane parallel conservation and hydrogenic emission for pure hydrogen
title plane parallel conservation and hydrogenic emission for pure hydrogen
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 5
init file "honly.ini"
c
c commands controlling geometry =========
sphere static (OK)
stop efrac 0.05 %stop when 5 percent ionized
c
c other commands for details =========
constant temper 7500
no level2
no induced processes (OK)
c needed to prevent 2s / Bal from becoming optically thick
turbulence 20 km/s
diffuse ots
atom h-like levels resolved 10
c
c commands controlling output =========
print diffuse continuum
normalize to "Ca B" 4861 = 1 % normalize to exact result for comp ion struc
punch overview "h_otspp.ovr"
punch dr "h_otspp.dr"
c
c h_otspp.in
c class limit
c ========================================
c
This tests the total emission from a plane parallel pure hydrogen
Stromgren sphere using the OTS approximation. The conservation
of the total number of ionizing photons, and the emitted spectrum,
are all checked.
h_otssp.in spherical conservation and hydrogenic emission for pure hydrogen
title spherical conservation and hydrogenic emission for pure hydrogen
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 5
init file "honly.ini"
c
c commands controlling geometry =========
radius 13
c not iterating does not affect the solution
sphere static (OK)
stop efrac 0.05 %stop when 5 percent ionized
c
c other commands for details =========
constant temper 7500
diffuse ots
no level2
no induced processes (OK)
c
c commands controlling output =========
print diffuse continuum
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "h_otssp.ovr"
punch dr "h_otssp.dr"
c
c h_otssp.in
c class limit
c ========================================
c
This tests the total emission from a spherical pure hydrogen Stromgren sphere
using the OTS approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
h_outopen.in test open geometry
title test open geometry
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 0
init file "honly.ini"
c
c commands controlling geometry =========
stop efrac 0.05 %stop when 5 percent ionized
filling 0.01
c
c other commands for details =========
diffuse outward
iterate
atom h-like levels resolved 15
no level2
no induced processes (OK)
constant temper 4
c
c commands controlling output =========
print diffuse continuum
c normally will not print out inward parts of lines
print line inward
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "h_outopen.ovr" last
punch dr "h_outopen.dr" last
c
c this is an open geometry, so do not expect H atom to exactly be case B
c due to Lyman line leakage. we iterated, so have a good estimate of
c inward and outward fractions, which we test
c h_outopen.in
c class limit
c ========================================
c
This tests the total emission from an open geometry,
hydrogen Stromgren sphere,
using the outward only approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
h_outpp.in plane parallel H-only, close, test hydrogenic emission
title plane parallel H-only, close, test hydrogenic emission
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
c the hydrogen density
hden 5
c an ini file that will include H-only
init file "honly.ini"
c
c commands controlling geometry =========
stop efrac 0.05 %stop when 5 percent ionized
c need this to prevent lyman lines from escaping
sphere static (OK)
c
c other commands for details =========
c prevent continuum pumping of lyman lines
no induced processes (OK)
c must include this to keep Ha optically thin
turbulence 20 km/s
c this is the approximation we are testing
diffuse outward
c force a constant temperature, then give stopping criteria
c if stop were not present model would go to limiting number of zones
constant temper 7500
c increase number of levels to get full emission
atom h-like levels resolved 20
c
c commands controlling output =========
c need to turn this on so that continua at various energies will
c be included in the emission line list
print diffuse continuum
c normalize results to perfect case b - our predictions should
c be close to this
normalize to line "Ca B" 4861
c the output and asserts
punch overview "h_outpp.ovr"
punch dr "h_outpp.dr"
c
c lots of continuum emission points turned on with print diffuse continuum
c energies dominated by two photon emission not included since very
c sensitive to Lya transport
c h_outpp.in
c class limit
c ========================================
c
This tests the total emission from a plane parallel pure hydrogen Stromgren sphere
using the outward only approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
h_outsp.in spherical conservation and hydrogenic emission for pure hydrogen
title spherical conservation and hydrogenic emission for pure hydrogen
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 5
init file "honly.ini"
c
c commands controlling geometry =========
radius 13
c not iterating does not affect the solution
sphere static (OK)
stop efrac 0.05 %stop when 5 percent ionized
c
c other commands for details =========
constant temper 7500
no level2
atom h-like levels resolved 20
no induced processes (OK)
diffuse outward
c
c commands controlling output =========
print diffuse continuum
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "h_outsp.ovr"
punch dr "h_outsp.dr"
c
c lots of continuum emission points turned on with print diffuse continuum
c energies dominated by two photon emission not included since very
c sensitive to Lya transport
c h_outsp.in
c class limit
c ========================================
c
This tests the total emission from a spherical pure hydrogen Stromgren sphere
using the outward only approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
h_t4_conemis.in continuous emission from H atom
title continuous emission from H atom
c
c commands controlling continuum =========
c use laser so that stellar continuum is not in predicted continuum
laser 2
ionization -1
c
c commands for density & abundances =========
c high density to suppress two-photon emission
hden 8
init "honly.ini"
c
c commands controlling geometry =========
c this thisckness is the inverse square of the density, so the
c total emission from the computed slab will in effect have the
c square of the density removed, so predictions will be j pi j / n_e n_p
stop thickness -16
c
c other commands for details =========
c include a large number of levels to capture IR emission
c increase default resolution stored in continuum_mesh.ini
set continuum resolution 0.1
iterate
constant temperature 4
c
c commands controlling output =========
print diffuse continuum
print lines column
punch continuum "h_t4_conemis.con" last no title units microns
punch spectrum "h_t4_conemis.ncon" last no title units microns
c
c h_t4_conemis.in
c class limit
c ========================================
c
This tests the continuous emission from the model H atom. The
gas temperature is 10,000 K and the continuous emissivity
is asserted for a range of wavelengths.
This was used to generate the plot in Hazy 2 comparing the emission
from a pure hydrogen plasma with those of Ferland 1980.
//>>refer HI emission Ferland, G. J. 1980, PASP, 92, 596
h_t4_conemis_lon.in low-den continuous HI emission with 2-nu important
title low-den continuous HI emission with 2-nu important
c
c commands controlling continuum =========
laser 2
ionization -1
c
c commands for density & abundances =========
hden 0
init "honly.ini"
c
c commands controlling geometry =========
stop thickness 0
c
c other commands for details =========
c increase default resolution stored in continuum_mesh.ini
set continuum resolution 0.1
case b
iterate
constant temperature 4
c
c commands controlling output =========
print diffuse continuum
print lines column
punch continuum "h_t4_conemis_lon.con" last units microns
punch two photon continuum "h_t4_conemis_lon.2nu" last rydbergs
punch spectrum "h_t4_conemis_lon.ncon" last units microns
c
c h_t4_conemis_lon.in
c class limit
c ========================================
c
This is a mate to hatomt10.in except that the density is low enough
for two-photon emission to be very imporant in the optical and uv.
h_t4_conemis_thick.in H I continuous emissivity, used for plot in hazy
title H I continuous emissivity, used for plot in hazy
c
c commands controlling continuum =========
black 5
ionization parameter -2
c
c commands for density & abundances =========
c high density to suppress two-photon emission
hden 7
c turn off all elements, except for hydrogen, so that
c we really test hydrogen emission
init file= "honly.ini"
c
c commands controlling geometry =========
c this is necessary to stop model at H ionization front
c constant temperature models will go on to infinity without this
stop efrac -0.8
c
c other commands for details =========
turbulence 200 km/s ; needed to keep balmer lines thin
c increase continuum resolution by factor of ten
set continuum resolution 0.1
c line fluorescense would be very important with above turbulence,
c turn it off
no induced processes
c need large atom to get the many Rydgerg levels in the infrared
c atom h-like levels resolved 10
c what full outward flux so use spherical geometry
sphere
constant temperature 4
c
c commands controlling output =========
c results will be relative to interplated Hummer&Storey Hbeta
c this tests hydrogen atom too
normalize "Ca B" 4861
c by default, the continuum flux at many wavelengths is not printed,
c this turns that information on
print diffuse continuum
c output the predicted continuum
punch emitted continuum last iteration "h_t4_conemis_thick.con" units micron
punch dr last "h_t4_conemis_thick.dr"
c
c h_t4_conemis_thick.in
c class limit
c ========================================
c
This checks that the predicted hydrogen continuum is in good agreement
with exact results in the optically thin nebular limit.
Checks:
- This output was used to generate figure h_t4_conemis_thick in Part I of HAZY.
- Continuum relative to Hbeta should agree with Ferland (1980)
filter averaged results.
- Hbeta should agree with Case B predictions, and Q(H) 4861.
heatomt10.in continuous emission from HeI
title continuous emission from HeI
c
c commands controlling continuum =========
laser 1.9 ryd
ionization -1
c
c commands for density & abundances =========
c need high density to supress two-photon emission
hden 10
c force high density for electrons, He+ density will be the same
set eden 12
c set He/H ratio to 100, He and elec will have same density
element abundance helium 2
init "hheonly.ini"
c
c commands controlling geometry =========
c this thickness will get unit emission when combined with above densities
stop thickness -24
c
c other commands for details =========
iterate
constant temperature 4
c
c commands controlling output =========
print continuum
c
set continuum resolution 0.1
set nFnu diffuse outward, diffuse inward
print continuum
print line faint 1
print line column
punch spectrum "heatomt10.spc" last no title units microns
punch continuum "heatomt10.con" last no title units microns
punch diffuse continuum "heatomt10.dif" last no title units microns
c
c heatomt10.in
c class limit
c ========================================
c
This tests continuous emission from the He I atom.
The laser is used so that the incident continuum
is not included in the total emission.
heatomt10lon.in test low-den continuous emission from H atom, 2-nu is important
title test low-den continuous emission from H atom, 2-nu is important
c
c commands controlling continuum =========
laser 2
ionization -1
c
c commands for density & abundances =========
hden -8
element helium abundance log 3
set eden -5
init "hheonly.ini"
c
c commands controlling geometry =========
stop thickness log 10
c
c other commands for details =========
no scattering opacity
c force all helium to be in He+
element helium ionization -4 0 -4
case b
c increase default resolution stored in continuum_mesh.ini
set continuum resolution 0.1
iterate
constant temperature 4
c
c commands controlling output =========
normalize to "he 1" 4471
print lines column
print diffuse continuum
print lines column
punch continuum "heatomt10lon.con" last units microns
punch diffuse continuum "heatomt10lon.dif" last units microns
punch two photon continuum "heatomt10lon.2nu" last
punch spectrum "heatomt10lon.ncon" last units microns
c
c heatomt10lon.in
c class limit
c ========================================
c
This is a mate to hatomt10.in except that everything is He at low density
heiont10.in continuous emission from HeII
title continuous emission from HeII
c
c commands controlling continuum =========
laser 5 ryd
ionization 1
c
c commands for density & abundances =========
hden 8
set eden 10
element abundance helium 2
init "hheonly.ini"
c
c commands controlling geometry =========
stop thickness -20
c
c other commands for details =========
constant temperature 4
iterate
c increase continuum resolution by factor of ten
set continuum resolution 0.1
set nFnu diffuse outward, diffuse inward
c
c commands controlling output =========
print continuum
print line faint 1
print line column
punch continuum "heiont10.con" last no title units microns
punch spectrum "heiont10.spc" last no title units microns
c
c heiont10.in
c class limit
c ========================================
c
This tests the He II continuous emission. The helium abundance
is very large so that He II overwhelms other emission sources.
 The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
hhe_otssp.in spherical conservation and H-like emission for H and He
title spherical conservation and H-like emission for H and He
c
c commands controlling continuum =========
blackbody 40000
ionization -2
c
c commands for density & abundances =========
hden 5
init file "hheonly.ini"
c
c commands controlling geometry =========
diffuse ots
atom h-like levels resolved 10
radius 13
stop efrac 0.05 %stop when 5 percent ionized
sphere static
c
c other commands for details =========
constant temper 7500
iterate
no level2
no induced processes (OK)
c
c commands controlling output =========
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "hhe_otssp.ovr" last
punch dr "hhe_otssp.dr" last
c
c helium lines
c hhe_otssp.in
c class limit
c ========================================
c
This tests the total emission from a spherical pure H + He-like Stromgren sphere
using the outward only approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked. The geometry is plane paralel.
hhe_outpp.in plane parallel conservation emission for H, He gas
title plane parallel conservation emission for H, He gas
c
c commands controlling continuum =========
blackbody 40000
ionization -2
c
c commands for density & abundances =========
hden 5
init file "hheonly.ini"
c
c commands controlling geometry =========
c open sphere to stop Lya from destroying HeI 23S
sphere
stop efrac 0.05 %stop when 5 percent ionized
c
c other commands for details =========
c need this since will assert helium triplet lines that depend on stable soln
iterate
constant temper 7500
atom h-like element hydrogen levels resolved 10
no level2
no induced processes (OK)
c
c commands controlling output =========
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "hhe_outpp.ovr" last
punch dr "hhe_outpp.dr" last
c
c hhe_outpp.in
c class limit
c ========================================
c
This tests the total emission from a spherical pure hydrogen Stromgren sphere
using the outward only approximation. The conservation of the total number
of ionizing photons, and the emitted spectrum, are all checked.
hhe_outppff.in plane parallel filling factor pure H, He gas
title plane parallel filling factor pure H, He gas
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 5
init file "hheonly.ini"
c
c commands controlling geometry =========
filling factor -1
stop efrac 0.05 %stop when 5 percent ionized
sphere
c
c other commands for details =========
c need this since will assert helium triplet lines that depend on stable soln
iterate
constant temper 7500
no level2
no induced processes (OK)
atom h-like element hydrogen levels resolved 10
c
c commands controlling output =========
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "hhe_outppff.ovr" last
punch dr "hhe_outppff.dr" last
c
c helium lines
c hhe_outppff.in
c class limit
c ========================================
c
This is a plane-parallel constant temperature cloud with only
hydrogen and helium. The gas has a filling factor of 0.1.
Induced processes are turned off and a large H atom is used
so that the hydrogen recombination
spectrum will be close to Case B. The calculation stops beyond the
hydrogen ionization front, because of the stop efrac command (it needs
this since this is a constant temperature calculation, so the usual
lower-temperature stopping criterion does not apply). The asserts
confirm that energy is conserved and that the hydrogen spectrum is correct.
hhe_outsp.in spherical conservation and H-like emission for H, He
title spherical conservation and H-like emission for H, He
c
c commands controlling continuum =========
ionization -2
blackbody 40000
c
c commands for density & abundances =========
hden 5
init file "hheonly.ini"
c
c commands controlling geometry =========
radius 13
stop efrac 0.05 %stop when 5 percent ionized
sphere static
c
c other commands for details =========
iterate
diffuse outward only
constant temper 7500
no level2
no induced processes (OK)
atom h-like element hydrogen levels resolved 10
c
c commands controlling output =========
normalize to "Ca B" 4861 = 1 % normalize to exact result
punch overview "hhe_outsp.ovr" last
punch dr "hhe_outsp.dr" last
c
c helium lines
c
c hhe_outsp.in
c class limit
c ========================================
c
This tests a spherical cloud with only hydrogen and helium.
Diffuse fields are transferred with the outward only approximation.
The asserts check that the ionizing radiation is conserved.
hii_blister.in Lexington 1995 dust-free hii blister region
title Lexington 1995 dust-free hii blister region
c
c commands controlling continuum =========
c a simple blackbody
blackbody 40000
c the flux of H-ionizing photons
phi(h) 13.0
c add the CMB after hot star shape & luminosity specified
CMB
c
c commands for density & abundances =========
hden 4
init file="ism.ini"
c HII region abundance but no dust
abundances hii region no grains
abundances he1 c1 n1 o1 ne1 mg=.0001 si.01 s1 cl1 ar1
continue fe.001
c
c commands controlling geometry =========
sphere
c
c other commands for details =========
c this is to desaturate Lya to prevent excited state photoionization
c from being important - the other codes did not include this important
c physical process
turbulence 10 km/s
c must iterate since optically thick
iterate
c
c commands controlling output =========
normalize to "Ca B" 4861
print line faint .01
print line sum
He 1 5876
totl 2326
C 2 1335
TOTL 1909
N 2 6584
N 2 6548
N 3 57.21m
TOTL 7325
TOTL 3727
O 3 51.80m
O 3 5007
O 3 4959
Ne 2 12.81m
Ne 3 15.55m
Ne 3 3869
Ne 3 3968
S 3 18.67m
S 3 9532
S 3 9069
S 4 10.51m
end of lines
punch overview last "hii_blister.ovr"
punch dr last "hii_blister.dr"
punch results last "hii_blister.rlt"
print line optical depths
c
c
c hii_blister.in
c class hii
c ========================================
This is one of the test cases from the Lexington Meeting suite of
nebulae (Ferland et al. 1995). It is a grain-free hii_blister HII region,
similar to inner regions of the Orion Nebula, except for the
absence of grains.
The set of lines entered with the print line sum command lists
the most powerful coolants in this model. This is one of the
tabulated quantities in the Lexington Meeting, and is a
fundamental test of energy conservation in the code.
The ratio of the sum of these lines to Hb is equivalent to the
Stoy ratio, used for determining stellar temperatures.
The "dielec kludge 0" command is to turn off my estimates of the
DR rates for those elements that had none. This was only to allow
comparison with other calculations that did not make similar estimates.
For an actual calculation I would not include this command, since the
guesses are better than nothing.
the turbulence is to stop the balmer lines from becoming optically
thick since few other codes include an actual H atom, but use
case b instead. The Orion HII region does have an observed turbulence
of about 8 km/s.
This calculation stops near the H+ - H0 ionization front, where
the temperature falls below the default lowest temperature of 4000 K.
This model would have continued into the PDR had a lower temperature
been specified with the STOP LOWEST TEMP command.
hii_coolstar.in dust free cool HII region model, Lexington 1995
title dust free cool HII region model, Lexington 1995
c
c commands controlling continuum =========
black body, T = 20000 K
q(h) 49
c add the CMB after hot star shape & luminosity specified
CMB
c
c commands for density & abundances =========
hden = 2
init file="ism.ini"
abund He-1 C-3.6576 N-4.39794 O-3.481146 ne-4.30103 mg-8
continue si-8 s-5.04576 cl-7 ar-8 fe-8
c
c commands controlling geometry =========
radius = 18.477121
sphere
c this is to go deep to pick up all H recombs
stop efract -2
stop temperature 1,000
c
c other commands for details =========
c must iterate since fine structure lines are optically thick
iterate
c assume there is neutral gas beyond what we compute
double
c
c commands controlling output =========
plot continuum range .1
print line faint .01
c this is the sum of lines in table 2 of the Lexington meeting
print line sum
N 2 6584
N 2 6548
TOTL 3727
Ne 2 12.81m
S 2 6720
S 3 18.67m
S 3 33.47m
S 3 9532
S 3 9069
end of lines
punch overview last "hii_coolstar.ovr"
punch dr last "hii_coolstar.dr"
punch results last "hii_coolstar.rlt"
punch continuum last units microns "hii_coolstar.con"
punch lines, cumulative, "hii_coolstar.cum"
totl 4861
o 3 5007
totl 3727
o 1 6300
end of lines
c
c Hbeta 4.93E36, L(total)4.30xHbeta
c hii_coolstar.in
c class hii
c ========================================
c
This is one of the test cases from the Lexington Meeting suite of nebulae.
It is a grain-free HII region ionized by a very cool star. Hydrogen is
ionized but not helium so this tests the transport of the H Lyman continuum.
The set of lines is entered with the print line sum command to test
energy conservation.
hii_icf.in HII region with negative He/H ICF
title HII region with negative He/H ICF
c
c commands controlling continuum =========
c this is the result of this command
c table star mihalas 46000
c and makes it possible to run these orion sims without
c installing the stellar atmosphere files
table read "star_mihalas_46000.dat"
ionization parameter -2.
c add the CMB after hot star shape & luminosity specified
CMB
c
c commands for density & abundances =========
hden 3
init file "ism.ini"
abundances ism no grains
grains no qheat single
metals and grains 0.320
c
c commands controlling geometry =========
stop efrac -3
stop temperature 15
sphere
c
c other commands for details =========
failures 1
c
c commands controlling output =========
punch overview "hii_icf.ovr" last
punch dr "icr.dr" last
c
c hii_icf.in
c class hii
c ========================================
This is an example of an H II region irradiated
by a hard stellar continuum - one of the Mihalas NLTE stars.
The hard continuum produces a negative He/H ionization
correction factor, as discussed in Ballantyne, Ferland & Martin (2000).
>>refer HeI icf by Ballantyne,D.R., Ferland, G.J., & Martin, P.G., 2000, ApJ 536, 773-777
hii_paris.in "New" Paris meeting HII region
title "New" Paris meeting HII region
c "standard" HII region model of the Pequignot Meudon Conferance
c
c commands controlling continuum =========
black body, T = 40000 K radius = 12.113943
c add the CMB after hot star shape & luminosity specified
CMB
c
c commands for density & abundances =========
hden = 2
init file="ism.ini"
abund he -1 C-3.6576 N-4.39794 O-3.481146 ne-4.30103 mg-8
continue si-8 s-5.04576 cl=-7 ar-8 fe-8
c
c commands controlling geometry =========
radius = 18.477121
sphere
c next two to make sure we pick up all possible H recombination
* stop temperature 600
set temperature floor 1000
c make sure sim goes very deep into cold gas
stop temperature 100K
stop efrac -2
c
c other commands for details =========
c must iterate since fine structure lines are opticall thick
atom h-like element hydrogen levels resolved 10
iterate
c
c commands controlling output =========
normalize to "Ca B" 4861
print column densities
print line optical depths
plot continuum range .1
print line faint 0.01
print line sum
He 1 5876
totl 2326
TOTL 1909
N 2 121.7m
N 2 6584
N 2 6548
N 3 57.21m
TOTL 3727
O 3 5007
O 3 4959
O 3 51.80m
O 3 88.33m
Ne 2 12.81m
Ne 3 15.55m
Ne 3 3869
Ne 3 3968
S 2 6720
S 3 18.67m
S 3 33.47m
S 3 9532
S 3 9069
S 4 10.51m
end of lines
punch overview last "hii_paris.ovr"
punch hydrogen 21 cm last "hii_paris.21cm"
punch results last "hii_paris.rlt"
punch dr last "hii_paris.dr"
c this is to confirm that this commnand works
punch lines emissivity "hii_paris.str" last
TOTL 4861
end lines
c
table lines "LineList_HII.dat"
c hii_paris.in
c class hii
c ========================================
c
This is one of the "standard" models computed at the Paris and Lexington
meetings on photoionization and shock calculations. a bable in hazy
compares the predictions of the current version of CLOUDY with predictions
of a few of the other codes. It is necessary to iterate since some
fine structure lines are optically thick. The set of lines entered
with the print line sum command is used to obtain the total luminosity
in detected lines, a measure of the Stoy temperature.
Checks:
- Hb close to case B, Q(H) 4861, intensities.
- Enter answers in Table Error! Reference source not found..
hlike_c.in H-like C VI case B
title H-like C VI case B
c
c commands controlling continuum =========
table agn
ionization parameter 3
c
c commands for density & abundances =========
hden = 8
init file="ism.ini"
element carbon abundance 1
set eden 9
c
c commands controlling geometry =========
set dr -18
stop zone 1
c
c other commands for details =========
case b hummer no photoionization
no induced processes (OK)
constant temperature = 1.e5
c
c commands controlling output =========
punch results "hlike_c.rlt"
c
c hlike_c.in
c class limit
c ========================================
c
This test case compares the predictions of the multi-level H-like CVI atom
with the Storey and Hummer (1995) results. The set dr command sets the
zone thickness to 1 cm. The case b command sets Lyman line optical depths
to very large values.
Checks:
- Neutral fractions
- H* emissivity
- Relative line intensities
hlike_o.in H-like O VIII case B
title H-like O VIII case B
c
c commands controlling continuum =========
table agn
ionization parameter 4
c
c commands for density & abundances =========
hden = 8
init file="ism.ini"
element oxygen abundance 1
set eden 9
c
c commands controlling geometry =========
c set following so the n^2 dr is unity
set dr -18
stop zone 1
c
c other commands for details =========
case b hummer no photoionization
no induced processes (OK)
constant temperature = 1.e5
c
c commands controlling output =========
punch results "hlike_o.rlt"
c
c caseb_o.in
c class limit
c ========================================
c
This test case compares the predictions of the multi-level H-like O VIII atom
with the Storey and Hummer (1995) results. The set dr command sets the
zone thickness to 1 cm. The case b command sets Lyman line optical depths
to very large values.
Checks:
- Neutral fractions
- H* emissivity
- Relative line intensities
igm_lalpha.in Ly alpha forest cloud
title Ly alpha forest cloud
c
c commands controlling continuum =========
c ionized by cosmic background
c plus quasar/starburst continuum
cmb z=2
table hm05 z = 2
c
c commands for density & abundances =========
hden -2
metals -1.5 ;reduce all heavy elements by 1.5 dex
c
c commands controlling geometry =========
stop neutral column density 15
double ; mimic two-siced photoionization
c
c other commands for details =========
iterate to convergence; must iterate since optically thin
c
c commands controlling output =========
print line faint -1
punch overview last "igm_lalpha.ovr"
punch dr last "igm_lalpha.dr"
punch results last "igm_lalpha.rlt"
c
c on 05 aug 29 changed from old background command to
c cmb 2 plus hm05 z=2 background - all results changed substantially
c igm_lalpha.in
c class igm
c ========================================
c
This example demonstrates the behavior of the code in the low-density limit.
The ionizing source is the cosmic background at a redshift of z = 2.
The cloud is assumed to be optically thin to ionizing radiation,
in keeping with the Gunn-Peterson test, so the double command is included,
and an iteration is performed to converge the optical depth scale.
Continuum fluorescent excitation of lines is important because the cloud
is otically thin.
igm_primal.in cloud with primordial abundances exposed to background at Z=10
title cloud with primordial abundances exposed to background at Z=10
c
c commands controlling continuum =========
background, redshift= 10
c background due to agn from Haardt & Madau 1996 ApJ, 461, 20
c this sets both continuum shape and intensity, actually for z=2
table HM96 old
c
c other commands for details =========
c put in a velocity field to stop Lya from causing stability problems
turbulence 20 km/s
c do a second iteration to establish that it is optically thick downstream
iterate
c this sim should run cleanly - do not accept problems
failures 2
c
c commands for density & abundances =========
c this log of the hydrogen density
hden 5
c stored set of primordial abundances
abundances primordial
c
c commands controlling geometry =========
c we want to shielded face to not be exposed to empty space, but rather
c be just very deep in a dense cloud - this prevents lines from freely
c radiating from the shielded face
double optical depths
c set a lower temperature stopping criterion - default is 4000K
stop temperature 30
c
c commands controlling output =========
c don't want to print lots of faint hydrogen lines
print line faint -3
c some output files with info we want to save
punch temperature history "igm_primal_tem.his"
punch ionizing continuum "igm_primal.ion"
punch hydrogen conditions "igm_primal.mol"
punch heating "igm_primal.het"
punch dr "igm_primal.dr"
punch cooling "igm_primal.col"
punch overview "igm_primal.ovr"
punch results last "igm_primal.rlt"
c
c igm_primal.in
c class hii pdr igm
c ========================================
This is a high redshift cloud irradiated by the cosmic background and AGN light.
H- absorption of the z=10 cosmic background is a MAJOR heating agent
This model is very sensitive to treatment of Lya destruction, since resulting
J-bar is major destruction process for H-, which is the H2 formation route.
Lya ots oscillations could develop and are damped by not reevaluating H-
photo rate after first n times, as in hmole.c
igm_z3.in redshift 1000 recombination epoch
title redshift 1000 recombination epoch
c
c commands controlling continuum =========
c a true blackbody radiation field, in strick thermo equilibrium
blackbody 3000 STE
c
c commands for density & abundances =========
hden 0
abundances primordial
c
c commands controlling geometry =========
stop zone 1
c
c other commands for details =========
case b
iterate
c
c commands controlling output =========
normalize lines to "Ca B" 4861
print ages
print departure coef
print line faint -5
c
c igm_z3.in
c class limit igm
c ========================================
c
This is a model of the universe near the recombination epoch, at
a redshift of a thousand. The gas is exposed to a true blackbody at
3000 K, and the abundances are primordial.
ism.in cloud irradiated by ism background
title cloud irradiated by ism background
c
c commands controlling continuum =========
c this uses the Black continuum with no H-ionizing radiation,
c and with background cosmic rays
table ism
extinguish by a column of 22
c need cosmic rays to provide ionization to the chemistry
cosmic rays, background
c
c commands for density & abundances =========
hden 0
init file="ism.ini"
abundances ism
c
c commands controlling geometry =========
c set sphere since matter in all directions
sphere
stop temperature linear 10
stop thickness 0.1 linear parsecs
c
c other commands for details =========
c this prevents continuum pumping from exciting H0
case b
c this is to converge optical depths
iterate
c this should have no effect since T is larger than 100 K
set temperature floor 100K
c
c commands controlling output =========
c this model has no heavy element molecules, because H2 does not
c really fully form, since Lyman bands are not self-shielded
normalize to 157.6m "C 2"
print line pump
punch overview "ism.ovr" last
punch dr "ism.dr"
punch heating "ism.het"
punch coolign "ism.col"
c
c ism.in
c class ism
c ========================================
TODO - look at temperature struture - it has jitter at about the
level of convergence, up and down. Temp jitter caused by eden jitter.
This model is nearly isothermal, jitter measures noise in solver,
and is great chance to pin this down.
This is a test of the behavior of the code in the extreme of
photoionization by a relatively hard continuum, at low densities.
The continuum is the galactic background, attenuated by a column density
of 10^22 cm-2. Ionization by galactic background cosmic rays is included.
Case b appears since this region is deep in the ISM, and the Lyman lines
are quite thick. This example checks whether the ionization balance,
thermal balance, and electron density sum, are performed correctly in
this limit.
Checks:
- Numerical stability of solution
- Thickness exact
ism_cosmicray.in background cosmic ray ionization by suprathermal electrons only
title background cosmic ray ionization by suprathermal electrons only
c
c commands controlling continuum =========
c background CR H0 ionization rate should be 2.5e-17 s^-1,
c Williams et al. ApJ, 503, 689
cosmic rays, background
c this will be VERY faint black 50000
ionization parameter -25
black 50000
c
c commands for density & abundances =========
hden 5
c
c commands controlling geometry =========
set dr 0
stop zone 1
c
c other commands for details =========
iterate
set temperature floor 1000 K
c turn off molecules to test only ions
no molecules
c must turn off charge transfer and its heating, which would dominate,
c since we want to test cr heating and ionization
no charge transfer
no ctheat
c must turn of photoionization by recombining species,
c since we want to test cr heating and ionization
no photoionization
c any time photoionization is turned off, it is best to also
c turn off induced processes, which include pumping in the lyman lines
no induced processes
c
c commands controlling output =========
print ages
c
c ism_cosmicray.in
c class limit
c ========================================
c
This test conditions of cosmic ray ionization. Molecules and charge transfer
are disabled so that analytical estimates can be made.
ism_grid.in interstellar cloud irradiated by ism background
title interstellar cloud irradiated by ism background
c
c commands controlling continuum =========
c this uses the Black continuum with no H-ionizing radiation,
c and with background cosmic rays
table ism
extinguish by a column of 22
cosmic rays, background
c
c commands for density & abundances =========
hden 0 vary
grid from -3 to 2 in 0.5 dex steps
init file="ism.ini"
c this turns on ism abundances and grains
abundances ism
c
c commands controlling geometry =========
c set sphere since matter in all directions
sphere
stop temperature linear 10
stop thickness 0.1 linear parsecs
stop zone 1
c
c other commands for details =========
c this prevents continuum pumping from exciting H0
case b
c
c commands controlling output =========
c this model has no heavy element molecules, because H2 does not
c really fully form, since Lyman bands are not self-shielded
normalize to 157.6m "C 2"
punch grid "ism_grid.grd" last
punch averages "ism_grid.avr" last
temperature hydrogen 1
end of averages
punch overview "ism_grid.ovr" last
punch dr "ism_grid.dr"
punch heating "ism_grid.het"
punch coolign "ism_grid.col"
punch xspec mtable "ism_grid.fit" range 0.1 3 keV
punch temperature "ism_grid.tem"
c
c this is a special version of the assert that does a series of models
c sert tempe hydro 1 9942 .05 grid 8575 6468 3606 776 304 169 103 66.2 44.1 31.3
c
c ism_grid.in
c class ism
c ========================================
this shows an S-curve calculation - make plot showing density as X-axis
and gas pressure (nT) as y-axis
the gas is ionized by the galactic background. the density varies between
1e-3 and 100 cm-3. this is the full range found in the diffuse ism.
The components that are produced are
CNM - cold neutral medium, density ~ 40 cm-3
WNM - n ~ 0.5 cm-3,
WIM - warm ionized medium, n ~ 0.25 cm-3
HIM - hot ionized medium, n ~ 1e-3 cm-3, calculation DOES NOT
reproduce observed temperature of HIM - we get ~1e4K but
observed is ~1e6 K. HIM is shock, not photo, ionized
ism_hot_brems.in generate continuum due to hot ism in high Z,z starburst
title generate continuum due to hot ism in high Z,z starburst
c
c commands controlling continuum =========
c this sets up coronal equilibrium for temperature and continuum
c cloud is predominantly collisionally ionized
coronal equilibrium, t = 1.e6 K
c
c commands for density & abundances =========
c log of hydrogen density (cm-3), by default a constant density model
hden 1
c chemical composition for a well-evolved star cluster with high Z
c the starburst command generates scale factors that will be used to
c multiply the old solar composition, used in ver 84. this is maintain
c record of physical changes
abundances old solar 84
abundances starburst Z=10 Zsun
c
c commands controlling geometry =========
c the log of the total hydrogen column density, cm-2
stop column density 21
c
c other commands for details =========
c continuum is plotted in Hzay, we me must iterate to predict this
iterate
c
c commands controlling output =========
c normalize to O 7 Lya
normalize to "O 7" 21.60
c this shortens the printout somewhat
print line faint 1
c output options
punch continuum last "ism_hot_brems.con" no title, units keV
punch sulphur ionization "ism_hot_brems.sul"
punch overview last "ism_hot_brems.ovr"
c this is only to document the problem described above
punch dr last "ism_hot_brems.dr"
c
c ism_hot_brems.in
c class ism
c ========================================
c
This model generates a large column constant density cloud
similar to the hot phase of the interstellar medium.
The continuum is punched to generate one of the figures in Part 2 of Hazy.
There is a strange feature between 1.7e-3A and 2.2e-3A that is the N emission
(head starting at 1.7e-3A with O absorption at 2.2e-3A. This model is
strongly enriched in heavies so many metal edges, esp O, are optically thick.
>>TODO 1 the guess of the thickness of the first zone is badly too small,