title intermediate-ionization x-ray ionized cloud from Lexington 2000
stop column density 16
print line sort wavelength 
print lines column linear 
normalise to "H  1" 1216
print line faint -1
hden 5
iterate
phi(h) 15.477 range 7.353 to 735.3
interpolate (-8 -3)
continue (-6 1.)
continue (-2 14.5)
continue (0.4771 12.7) 
continue (0.8663 10.6)
continue (3.8663 7.6)
continue (6 1)
continue (9 -3)
element abundance helium  -1
element abundance carbon -3.432
element abundance nitrogen -3.959
element abundance oxygen -3.097
element abundance neon -3.959
element abundance magnesium -4.4318
element abundance silicon -4.456
element abundance sulphur -4.7959
element abundance argon -5.4318
element abundance iron -4.398
element lithium off
element beryllium off
element boron off
element fluorine off
element sodium off
element aluminium off
element phosphrous off
element chlorine off
element potasium off
element calcium off
element scandium off
element titanium off
element vanadium off
element chromium off
element manganese off
element cobalt off
element nickel off
element copper off
element zinc off
c
// >>chng 08 oct 18, from 7.543e5 to 7.901e5, include Badnell UTA data 
monitor temperature hydrogen 2 7.901e5 K
save overview "agn_lex00_u0.ovr"
save performance "agn_lex00_u0.per"
save transmitted continuum "agn_lex00_u0.trn" units keV 
c
c agn_lex00_u0.in

This is one of the "warm absorber" simulations presented at the Lexington
2000 meeting on nebulae.  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.

