A grid of PDR and XDR models
by:
Rowin Meijerink (rowin@astro.berkeley.edu)
Marco Spaans (spaans@astro.rug.nl)

Purpose
To interpret atomic and molecular line emissions from irradiated gas in galaxy centers.

Grid
The PDR grid comprises the following ranges:
Range Density (cm-3) Radiation field (G0) Cloudsize (pc)
I 102-103 100.5-103 50
II 103-104 101-104 10
III 104-106.5 102-105 1

The XDR grid comprises the following ranges:
Range Density (cm-3) Radiation field (erg s-1 cm-2) Cloudsize (pc)
I 102-103 0.016-1.6 50
II 103-104 0.16-16 10
III 104-106.5 1.6-160 1

Line list
Atomic species:
[CII] 158mum
[SiII] 35mum
[CI] 609, 369, 230mum
[OI] 63, 145, 44mum
[S] 25, 57, 17mum
[FeII] 25, 35, 16mum
[SiI] 130, 68, 45mum

 Molecular species
CO, 13CO, HCN, HNC, HCO+, CS and SiO

Format
All data are in tabular form according to the following format:

atomic fine-structure lines (in units of erg cm-2 s-1 sr-1)
distance[cm], [CII], [SiII], [CI], [OI], [S], [FeII], [SiI]
The *tar.gz can be found here:
XDR range I, II, and III
PDR all ranges

molecular rotational lines (in units of erg cm-2 s-1,  so one has to divide by 2 pi to obtain the same units as for the atomic lines)
distance[cm], n rotational lines (where n varies, lines are in increasing order so J=1-0, 2-1, etc.)
The *tar.gz can be found here:
CO:     XDR range I, II, and III
            PDR range I, II,  and III
13CO:  XDR range I, II, and III
            PDR range I, II, and III
HCN:  XDR range III
            PDR range III
HNC:  XDR range III
            PDR range III
HCO+: XDR range III
             PDR range III
CS:       XDR range III
             PDR range III
SiO:      XDR range III
              PDR range III
   
Bibliography
Here you find the description of the codes that where used to compute the PDR and XDR model grid and the description of the models available on this site. When using these models, please cite these articles.

Additional models
Also available are models with an enhanced cosmic ray rate (5×10-15s-1), which are described in the following letter.

Furthermore, chemical abundances and temperatures as a function of depth for all models are available on a collaborative basis.