This repository contains the emission line fluxes predicted with the Cloudy photoionization code version 17.01 (Ferland et al. 2017) for the star-forming models described in Section 3.1 of Calabro et al. (2023): https://arxiv.org/abs/2306.08605
We use for the calculations the package pyCloudy v.0.9.11: https://github.com/Morisset/pyCloudy/tree/0.9.11.
In all cases, the incident radiation field shape is obtained with BPASS stellar population models (Eldridge et al. 2017), assuming a Salpeter IMF with an upper mass limit of 300 Msun , stellar metallicity equal to the gas phase metallicity of the surrounding gas cloud, and continuous star-formation history with age of
The table joined_table_SF_models.txt in the repository contains the predictions of the line intensity (in units of erg/s, obtained with the command 'get_emis_vol' in pycloudy, and scaled to an
column name | description |
---|---|
dens | gas density of the cloud (in units of |
met | gas-phase metallicity |
OH | corresponding oxygen abundance of the cloud (12+log(O/H)) |
logU | ionization parameter |
Currently, the flux predictions are available for the following emission lines, in order of increasing wavelength :
column name | emission line |
---|---|
CII_1335 | [CII] |
CIV_1551 | CIV |
HeII_1640 | HeII |
CIII_1909 | CIII] |
Hbeta | |
OIII_5007 | [OIII] |
Halpha | |
NII_6583 | [NII] |
SIII_9531 | [SIII] |
CI_9850 | [CI] |
HeI_10830 | HeI |
PaGamma | |
PII_1188 | [PII] |
FeII_1257 | [FeII] |
PaBeta | |
FeII_132 | [FeII] |
FeII_164 | [FeII] |
PaAlpha |