PNe*

These sets of models are available in both the old 3MdB and the new 3MdB_17 databases.

In the 3MdB_17 database, all the models are run with Cloudy 17.01, and the reference of the models is PNe_2020. More effective temperatures are used:

• in the Blackbody as ionizing SED (in kK): 25, 30, 35, 40, 50, 60, 70, 75, 80, 90, 100, 110, 120, 125, 130, 140, 150, 160, 170, 180, 190, 200, 210, 220, 230, 240, 250, 260, 270, 280, 290, and 300.
• in the models with a Thomas Rauche SED: 50, 60, 70, 75, 80, 90, 100, 110, 120, 125, 130, 140, 150, 160, 170, and 180.

All the models in 3MdB_17 have been obtained with Constant density (i.e. no Gaussian density law as in PNe_2014). A total of 724,386 models are in 3MdB_17, from which 116,121 have com6 =1 (see below).

The python script used to generate the models is there: https://github.com/Morisset/pyCloudy/blob/master/pyCloudy/3MdB_17/make_PNe_20.py

In the 3MdB database, the references are PNe_2014 (run with Cloudy c10), PNe_2014_c13 and PNe_2016, both obtained with Cloudy c13.

This project is associated with the papers by Delgado-Inglada, G., Morisset, C. and Stasinska, G. see http://adsabs.harvard.edu/abs/2014MNRAS.440..536D.

A second paper is dealing with the ICFs for the ions not treated in Paper I.

The coms columns in tab contain:

• com1: 'BB' or 'TR' for BlackBody or Thomas Rauch atmosphere models respectively, for the SED
• com2: 'C' or 'G1' for constant or Gaussian density law resp.
• com3: 'R', 'M20', 'M40', 'M60', 'M80' for Radiation-, 20%, 40%, 60% and 80% Matter-bounded models.
• com4: 'S', 'L', 'H', 'VH' for Solar, Low, High and Very High abundances.
• com5: 'N' or 'D' for No dust and Dusty models resp.
• com6: '0' and '1' for non selected and selected models resp. The selected models are the ones used in the Paper I, that is the ones fitting all the following criteria:
  • (log(L) < 4.2) & (log(L) > 3.4 | Tstar > 1e5) & (log(L) > 1.5e-5 * Tstar-0.25), where L is the bolometric luminosity in solar units and Tstar is in K.
  • Hmass < 1 solar mass
  • 2e53 < nH * Rout**3 < 3e56, where nH is the mean Hydrogen density and Rout is the outer radius in cm.
  • 1e-15 < Hbeta / (4.pi.Rout.206265)**2 < 1e-11 , where Hbeta is the Hbeta luminosity in erg/s and Rout the outer radius in cm.

The script used to generate the inputs of the grids, as well as the one used to make some of the figures for the paper Delgado-Inglada et al. 2014 are attached to this post.

Formats of the "com" fields: