J/A+A/623/A143 Code Pegase.3 (Fioc+, 2019)
Pegase.3: A code for modeling the UV-to-IR/submm spectral and chemical
evolution of galaxies with dust.
Fioc M., Rocca-Volmerange B.
<Astron. Astrophys. 623, A143 (2019)>
=2019A&A...623A.143F 2019A&A...623A.143F (SIMBAD/NED BibCode)
ADC_Keywords: Models, evolutionary ; Galaxies
Keywords: galaxies: evolution - galaxies: abundances -
galaxies: stellar content - infrared: galaxies - dust, extinction -
radiative transfer
Abstract:
A code computing consistently the evolution of stars, gas and dust, as
well as the energy they radiate, is required to derive reliably the
history of galaxies by fitting synthetic spectral energy distributions
(SEDs) to multiwavelength observations. The new code Pegase.3
described in this paper extends to the far-infrared/submillimeter the
ultraviolet-to-near-infrared modeling provided by previous versions of
Pegase. It first computes the properties of single stellar populations
at various metallicities. It then follows the evolution of the stellar
light of a galaxy and the abundances of the main metals in the
interstellar medium (ISM), assuming some scenario of mass assembly and
star formation. It simultaneously calculates the masses of the various
grain families, the optical depth of the galaxy and the attenuation of
the SED through the diffuse ISM in spiral and spheroidal galaxies,
using grids of radiative transfer precomputed with Monte Carlo
simulations taking scattering into account. The code determines the
mean radiation field and the temperature probability distribution of
stochastically heated individual grains. It then sums up their spectra
to yield the overall emission by dust in the diffuse ISM. The nebular
emission of the galaxy is also computed, and a simple modeling of the
effects of dust on the SED of star-forming regions is implemented.
The main outputs are ultraviolet-to-submillimeter SEDs of galaxies
from their birth up to 20Gyr, colors, masses of galactic components,
ISM abundances of metallic elements and dust species, supernova rates.
The temperatures and spectra of individual grains are also available.
The paper discusses several of these outputs for a scenario
representative of Milky Way-like spirals. Pegase.3 is fully
documented and its Fortran 95 source files are public. The code should
be especially useful for cosmological simulations and to interpret
future mid- and far-infrared data, whether obtained by JWST, LSST,
Euclid or e-ELT.
Description:
To extract the code from the compressed archive, type
"tar xvf Pegase.3.0.1.tar.gz"
in a terminal. This creates in "./" a directory called "Pegase.3.0.1/"
which contains all the source files of the code.
To read the documentation, open file "doc_Pegase.3.0.1.pdf" in
"Pegase.3.0.1/doc_dir/" with a PDF reader. Have a look at least at
section I ("Getting started") before compiling and running the code.
The text of the free software CeCILL license under which Pegase.3.0.1
is distributed is in the same directory as the documentation. This
directory also contains the paper published in Astronomy &
Astrophysics (file "article_Pegase.3.pdf") and a list of changes with
previous versions of Pegase.3 (file "Changes.txt.html").
To compile the code, go in "Pegase.3.0.1/bin_dir/" and execute the
command 'make' in a terminal. Follow the instructions in section I.2
of the documentation to modify the default settings, in particular if
you need or want to change the Fortran compiler and the link to the
PGPlot graphical library (this library is called by the "plot_*"
executables provided with the code).
To check that the code works without problem on your machine, we
recommend that, for the first execution, you run "./SSPs", "./spectra"
and "./colors" in "Pegase.3.0.1/bin_dir", and that you provide the
same answers as in section I.3 of the documentation.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
Pegase.3.0.1.tar 5280 2607322 Pegase code (all files)
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See also:
http://www.iap.fr/users/fioc/Pegase/Pegase.3 : Pegase.3 Home Page
Acknowledgements:
Michel Fioc, Michel.Fioc(at)iap.fr
(End) Patricia Vannier [CDS] 08-Mar-2019