sections:
FINISH HELIUM
TO RELEASE C96
HIGH PRIORITY
MEDIUM PRIORITY
PDR physics

02 apr 10, 43 fixits
02 apr 17, 45
02 may 05, 41
02 may 10, 25
02 may 16, 19

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critical

Peter Martin's comments on the web site

add perl script check on PROBLEM into special file

complete new brems - free-free heating, freeht.c, and cooling, in coolr.c line 285

two photon in rtdiffuse - search on TODO

no molecular asserts in many orion pdr, or th models

===================================================================
FINISH HELIUM

helium - see helium.txt 

helike.lgUseOld = FALSE; use this variable to make full set of new he-like physics complete - /*this one - use new atom */

when old he is finally turned off, confirm that new helium respects very low levels of ionization of helium itself, good model is lowion_low.in - code should never turn off He+ since so important for molecular clouds.  

he.in in bugs - run just one zone, as density increases old and new hei gets worse,  run with n = 2 very good agreement, n = 5 bad

helike - names of routines at start of program do not match with what is actually within the file, as Ryan to fix
	
g-bar paper from 1995 for all other he cs
Romanik 1988 has dr for he iso seq

incorporate sampson collision strengths

helium - be careful when replacing hei1 and hei3 - what should they really be?
23s or 11s populations?  if so, use those real numbers not sum
check all total hei xIonFracs[0][ipHELIUM] - should actually
be 11s??  proton 1-3 collisions
table of collision strengths is not complete - fill in fake cs before calling it, with typical
cs, so that complete collision set in code

he - hei must be solved in totally molecular environments due to co ct dest 

====================================================================
TO RELEASE C96

kill electron scattering line array
kill default title on punch

new DR rates from W Mich, also Badnell?
get all Savin rates from him

Bahar fe rates
Kaspi et al. 2001, either ApJ 554, 216 or 535, 14 (second one first)
Behar & Netzer 2002, ApJ 570 165
Behar, Sako, & Kahn, 2001, ApJ 563, 497

do something about new oxygen abundance

The optical depth in the HeII 3 cm line -- occurs in conserve.out
check 21 cm, heii lines, agree, remove main lines, rely on hyperfine lines
21 cm - remove from level 1, use info in hfs line, check e, H cs for H 21 cm, 
	put printout of hfs line optical depths, check 21 cm/Hb ratio vs density, paper?
he 21-cm-like transition has wrong abundance - multiply by ratio of isotopic line 216 hydrogenic.c,
take from hyperfine.dat??

p2k models all have dielectronic kludge 0 0 1 1 =-> should this be default?
nahar s3 -> s2, 9% larger than verner, s4 ->s3 5x larger
ar 5->4 8.3x 

FeII two versions of cloudy agree
check fixit in pop371 

two photon induced left incomplete,
	values for he iso seq
	emission from he iso seq
	induced rates correctly

====================================================================
HIGH PRIORITY

following not tested in tsuite: fabden, parseagn, dlaw, fileball, ratio, table abund, table table den
cext, cylinder, energy density, force te, hext, illuminate, neutrons

get rid of reference with ITRDIM, malloc when iterations are known 

use new he ct file for helium charge transfer

extend asster h-like departure coef to all do he-like - simply have var with ipISO

get rid of existing lowest 16 level feii, use verner instead, pequignot uses 46 level atom - do this

check what types of data are in chianti

why the negative rec cool topoff in iso_cool?  look for string "RecCoolError lt 0 in iso_cool" will only print if significant error, rel to cooling */

grep on "lya heating hittt", in heatsum, if never occurs, remove this logic, probably bogus 

xspec integration

CO turned off and on in grid I ran in india

incorporate tlusty and wm-basic (pouldrach) model atmospheres

script on alpha, del *.o so that when routines renamed, there is no conflict

dusty torus convergence failures

post peter vh's small sample on .net web site, ask how to speed it up.  run same thing on P3

define differences between cloudy and three reflected spectra of compton thick matter in lex meeting book

CO - csupra now destroys CO but does not create anything in the matrix.  Should it be CO+?
what does high energy light do?  

is rayleigh scattering added as a excitation process for lya - think not but could be important

FeXIII 1216 line under Lya

tarter thesis has good description of diffuse fields in outward only

widla called in pressurechange never does special lya - always uses widlin - could this bew major problem with lya width?

Lya dest prob is nearly always the low-end limit of 1e-8 in kk.in

full test suite with eden solver new, conserv.in failed with excessive eden failures

blister.in fails with impossible bracket with set temp solver new

Fix so that very high temperature exits like very low temperature

what is difference between hden and IonFracs[0][0]

get x-ray models strong lines to agree with exact wavelengths/energies

get new temp, eden solvers integrated into code

trace set eeden ot cofirm it still works

newdata has NII and NIII collision strength data - put into code

Stancil et al. O+ ct, A&A sup 140, 225, also Pequignot CT excitation of OI

Tayal 2000, ApJ 544, 575, has collision strengths for Fe10- 11, 13, expand
Fe10 to three level atom 

reinstate conpump routine that Hagai and I played with

Kaastra sent paper with lines from fluorescence, in cloudy/atomic data dir - put them in

way to enter J into continuum array, directly

longer input lines as per Fischer

boron-sequence, put in NeVI - Ca21 

NeVII 465A, Berrington et al, 1985, at dat nuc dat tab 33, 195

Fe15, 283A, better cs in Pradhan ADNDT 40, 335
Mg9 368, Berrington, 1994, ADNDT 57, many articles

hazy_coolcurve.c crashes if init te lowered to 3.4

==================================================================

MEDIUM PRIORITY

hydrogenic - electron scat escape prob is not used, set to zero

putline does not need to call linadd

limits to how low an ionization could be done with H level atom were influenced by bug in float/double.  
reconsider all this with harder bounds

level3 does not consider the pumping component before giving up because gas too cool.  
As result it underestimates some lines.

no molecules command - change to set H2 formation rate to be very small

H2 - update photo cs to Yan et al. include H2 photoioniz as dest process 

molecular data base in Millar et al. A&AS 121, 139 - study paper, has lots of details, update cloudy to include all this

look at secondary ionization in Dalgarno et al. 1999, apj sup

put in cobe background tempeature into cloudy/hazy

add electron scattering escape to Lya only, since it is so important and such a problem in grain free case

add option for abundances to be on log scale where H is 12
also to not print abundances as logs

old oi photo into excited states - does it still exist?

new oi ct data

put in mewe line yields for all elements so that all fluor lines are predicted for axaf

keenan atomic data 
!G-bar cooling lines reached 7.29e+001% of the local cooling.  Line=Fe15  282A

go over vanHoof2do.txt and put in his suggested additions

move comments now in linedata.old into data file level1.dat, modify getdata so that it
	counts number of level1 lines and mallocs the right sized array.  skip over comments

make sure that every command in hazy is used at least one in a test case

heii bowen problem should be done correctly

====================================================================

PDR physics

[OI] production in flow from OH, Stoerzer & Hollenbach 1998

new molecular reactions in table 1 of Hollenbach takahashi & tielens apj 377, 192

check CO pops go to lte

TH85 says that charge transfer between C+ and S and Si are important

H2 collision, Martin & Mandy

advectioon into pdrs, Storzer & Hollenback ApJ recent,
Goldsmith & Sternberg '9

Maloney & Hollenback 1996, XDR, xrays into pdrs

sternberg & neufeld, '99, H2 physics

