Introduction

PFANT is a stellar spectral synthesis software written in Fortran.

The development started with M Spite et al. in France in 1967 (Figure 0). The code formulation is described in (Barbuy 1982), (Cayrel et al. 1991), (Barbuy et al. 2003), and (Coelho et al. 2005).

 |
 | 1967 -- FANTÔME   -- by M Spite et al.
 | 1982 -- FANTOMOL  -- B Barbuy included the computation of molecular lines,
 |                      dissociatipon equilibrium
 | 2003 -- PFANT     -- M-N Perrin: large wavelength coverage,
 |                      inclusion or hydrogen lines
 | 2015 -- PFANT     -- J Trevisan: conversion to Fortran 2003 and optimization;
 |                      documentation; MARCS opacities; Python interface and tools
t|
 V

Figure 0 - Summarized PFANT timeline (Coelho et al. 2005)

Acknowledgement

The source code conversion, the documentation, incorporation of MARCS opacities, and Python development was funded by FAPESP - Research Support Foundation of the State of São Paulo, Brazil (2015-2017).

Contact

For bugs reports, questions, suggestions, etc., please open an issue at the project site on GitHub: http://github.com/trevisanj/PFANT.

References

(Barbuy 1982) Barbuy, B. 1982, PhD Thesis, Université de Paris VII

(Cayrel et al. 1991) Cayrel, R., Perrin, M. N., Barbuy, B., & Buser, R. (1991). A grid of synthetic spectra for the determination of effective temperature, gravity and metallicity of F, G, and K stars. I-Description of the method. II-Application to 41 stellar spectra taken in the Basel field of SA 141. Astronomy and Astrophysics, 247, 108-129.

(Barbuy et al. 2003) Barbuy, B., Perrin, M.-N., Katz, D. et al. 2003, A&A, 404, 661

(Coelho et al. 2005) Coelho, P., Barbuy, B., Meléndez, J., Schiavon, R. P., & Castilho, B. V. (2005). A library of high resolution synthetic stellar spectra from 300 nm to 1.8 μm with solar and α-enhanced composition. Astronomy & Astrophysics, 443(2), 735-746.