From nebular to pynebular: a new package for the analysis of emission lines
1
nebular is being migrated to a new environment, to make it more powerful and user-friendly... Nebular, a long-time reference package for the analysis of emission lines, started as a simple Fortran program and evolved into a powerful IRAF package. In essence, nebular works by solving the equilibrium equations for an n-level atom. These are some of the things nebular is able to compute: - physical conditions from suitable dignostic line ratios. - level populations, critical densities and line emissivities - 3-zone nebula models from sets of line ratios - dereddened line intensities Now nebular is being recasted in python and will become pyneb. pyneb is being designed to be more user-friendly and powerful than its predecessor. Here are some of the improvements: Fully user-selectable atomic data Fully user-defined and more numerous diagnostics hey! there's IR lines too! Emission maps as a function of temperature and density Full access to input data or intermediate quantities Contour maps of diagnostic line ratios as a function of T e and N e One of them is a tool for the Dynamic plotting of extinction and YES! a web interface: a long way to go, but here's a prototype: And there are many, many more features we intend to implement... for example: - Computation of elemental abundance using ICFs. - User-selectable and user-definable ICFs - Tools to perform error analysis of N e , T e and abundances - Ionic abundances for He and other elements from recombination lines Wanna be a beta tester? Sign here or send us an email ([email protected]) Valentina Luridiana vale AT iac.es ChristopheMorisset [email protected] Dick Shaw shaw AT noao.edu References De Robertis, M. M., Dufour, R. J., & Hunt, R. W. 1987, JRASC, 81, 195 Shaw, R. A., de La Pena, M. D., Katsanis, R. M., & Williams, R. E. 1998, in ADASS VII, R. Albrecht, R. N. Hook, & H. A. Bushouse eds, ASP Conf. Series, 145, 192 Shaw, R. A., & Dufour, R. J. 1995, PASP, 107, 896 Acknowledgments: Manuel Núñez-Díaz kindly gave us his HH 204 data Wishing a particular feature was there? Tell us or describe it here:
description
Poster presented by . Luridiana, C. Morisset, R.A. Shaw, D. Díaz-González at the IAU Symposium 283, Planetary Nebulae: an Eye to the Future, 25-29 July 2011, Tenerife, Spain.
Transcript of From nebular to pynebular: a new package for the analysis of emission lines
nebular is being migrated to a new environment, to make it more powerful and user-friendly...
Nebular, a long-time reference package for the analysis of emission lines, started as a simple Fortran program and evolved into a powerful IRAF package.
In essence, nebular works by solving the equilibrium equations for an n-level atom.
These are some of the things nebular is able to compute: - physical conditions from suitable dignostic line ratios. - level populations, critical densities and line emissivities - 3-zone nebula models from sets of line ratios - dereddened line intensities
Now nebular is being recasted in python and will become pyneb.
pyneb is being designed to be more user-friendly and powerful than its predecessor. Here are some of the improvements:
Fully user-selectable atomic data
Fully user-defined and more numerous diagnostics
hey
!
the
re's
IR
lines
too
!
Emission maps as a function of temperature and density
Full access to input data or intermediate quantities
Contour maps of diagnostic line ratios as a function of Te and Ne
One of them is a tool for the Dynamic plotting of extinction
and YES! a web interface: a long way to go, but here's a prototype:
And there are many, many more features we intend to implement... for example:
- Computation of elemental abundance using ICFs. - User-selectable and user-definable ICFs - Tools to perform error analysis of Ne, Te and abundances - Ionic abundances for He and other elements from recombination lines
Wanna be a beta tester? Sign here or send us an email ([email protected]) Valentina Luridiana (vale AT iac.es ChristopheMorisset [email protected]
Dick Shaw: shaw@ AT noao.edu
References De Robertis, M. M., Dufour, R. J., & Hunt, R. W. 1987, JRASC, 81, 195 Shaw, R. A., de La Pena, M. D., Katsanis, R. M., & Williams, R. E. 1998, in ADASS VII, R. Albrecht, R. N. Hook, & H. A. Bushouse eds, ASP Conf. Series, 145, 192 Shaw, R. A., & Dufour, R. J. 1995, PASP, 107, 896 Acknowledgments: Manuel Núñez-Díaz kindly gave us his HH 204 data
Wishing a particular feature was there? Tell us or describe it here:
![Variation of fluxes of RR Tel emission lines measured in …arXiv:0811.4557v1 [astro-ph] 27 Nov 2008 Variation of fluxes of RR Tel emission lines measured in 2000 with respect to](https://static.fdocuments.in/doc/165x107/60d5cc16040a5c7bbf062244/variation-of-iuxes-of-rr-tel-emission-lines-measured-in-arxiv08114557v1-astro-ph.jpg)
