@article{fioc_pegase.3_2019,
	title = {The {P}{\textbackslash}'egase.3 code of spectrochemical evolution of galaxies: documentation and complements},
	volume = {1902},
	shorttitle = {The {P}{\textbackslash}'egase.3 code of spectrochemical evolution of galaxies},
	url = {http://adsabs.harvard.edu/abs/2019arXiv190202198F},
	abstract = {P{\textbackslash}'egase.3 is a Fortran 95 code modeling the spectral evolution of 
galaxies from the far-ultraviolet to submillimeter wavelengths. It also
follows the chemical evolution of their stars, gas and dust. For a given
scenario (a set of parameters defining the history of mass assembly, the
star formation law, the initial mass function...), P{\textbackslash}'egase.3
consistently computes the following: * the star formation, infall,
outflow and supernova rates from 0 to 20 Gyr; * the stellar metallicity,
the abundances of main elements in the gas and the composition of dust;
* the unattenuated stellar spectral energy distribution (SED); * the
nebular SED, using nebular continua and emission lines precomputed with
code Cloudy (Ferland et al. 2017); * the attenuation in star-forming
clouds and the diffuse interstellar medium, by absorption and scattering
on dust grains, of the stellar and nebular SEDs. For this, the code uses
grids of the transmittance for spiral and spheroidal galaxies. We
precomputed these grids through Monte Carlo simulations of radiative
transfer based on the method of virtual interactions; * the re-emission
by grains of the light they absorbed, taking into account stochastic
heating. The main innovation compared to P{\textbackslash}'egase.2 is the modeling of
dust emission and its evolution. The computation of nebular emission has
also been entirely upgraded to take into account metallicity effects and
infrared lines. Other major differences are that complex scenarios of
evolution (derived for instance from cosmological simulations), with
several episodes of star formation, infall or outflow, may now be
implemented, and that the detailed evolution of the most important
elements -- not only the overall metallicity -- is followed.},
	urldate = {2019-02-08},
	journal = {arXiv e-prints},
	author = {Fioc, Michel and Rocca-Volmerange, Brigitte},
	month = feb,
	year = {2019},
	keywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},
	pages = {arXiv:1902.02198},
}

{"_id":"4L9pGuZicvSDkqv58","bibbaseid":"fioc-roccavolmerange-theptextbackslashegase3codeofspectrochemicalevolutionofgalaxiesdocumentationandcomplements-2019","author_short":["Fioc, M.","Rocca-Volmerange, B."],"bibdata":{"bibtype":"article","type":"article","title":"The P\\textbackslash'egase.3 code of spectrochemical evolution of galaxies: documentation and complements","volume":"1902","shorttitle":"The P\\textbackslash'egase.3 code of spectrochemical evolution of galaxies","url":"http://adsabs.harvard.edu/abs/2019arXiv190202198F","abstract":"P\\textbackslash'egase.3 is a Fortran 95 code modeling the spectral evolution of galaxies from the far-ultraviolet to submillimeter wavelengths. It also follows the chemical evolution of their stars, gas and dust. For a given scenario (a set of parameters defining the history of mass assembly, the star formation law, the initial mass function...), P\\textbackslash'egase.3 consistently computes the following: * the star formation, infall, outflow and supernova rates from 0 to 20 Gyr; * the stellar metallicity, the abundances of main elements in the gas and the composition of dust; * the unattenuated stellar spectral energy distribution (SED); * the nebular SED, using nebular continua and emission lines precomputed with code Cloudy (Ferland et al. 2017); * the attenuation in star-forming clouds and the diffuse interstellar medium, by absorption and scattering on dust grains, of the stellar and nebular SEDs. For this, the code uses grids of the transmittance for spiral and spheroidal galaxies. We precomputed these grids through Monte Carlo simulations of radiative transfer based on the method of virtual interactions; * the re-emission by grains of the light they absorbed, taking into account stochastic heating. The main innovation compared to P\\textbackslash'egase.2 is the modeling of dust emission and its evolution. The computation of nebular emission has also been entirely upgraded to take into account metallicity effects and infrared lines. Other major differences are that complex scenarios of evolution (derived for instance from cosmological simulations), with several episodes of star formation, infall or outflow, may now be implemented, and that the detailed evolution of the most important elements – not only the overall metallicity – is followed.","urldate":"2019-02-08","journal":"arXiv e-prints","author":[{"propositions":[],"lastnames":["Fioc"],"firstnames":["Michel"],"suffixes":[]},{"propositions":[],"lastnames":["Rocca-Volmerange"],"firstnames":["Brigitte"],"suffixes":[]}],"month":"February","year":"2019","keywords":"Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics","pages":"arXiv:1902.02198","bibtex":"@article{fioc_pegase.3_2019,\n\ttitle = {The {P}{\\textbackslash}'egase.3 code of spectrochemical evolution of galaxies: documentation and complements},\n\tvolume = {1902},\n\tshorttitle = {The {P}{\\textbackslash}'egase.3 code of spectrochemical evolution of galaxies},\n\turl = {http://adsabs.harvard.edu/abs/2019arXiv190202198F},\n\tabstract = {P{\\textbackslash}'egase.3 is a Fortran 95 code modeling the spectral evolution of \ngalaxies from the far-ultraviolet to submillimeter wavelengths. It also\nfollows the chemical evolution of their stars, gas and dust. For a given\nscenario (a set of parameters defining the history of mass assembly, the\nstar formation law, the initial mass function...), P{\\textbackslash}'egase.3\nconsistently computes the following: * the star formation, infall,\noutflow and supernova rates from 0 to 20 Gyr; * the stellar metallicity,\nthe abundances of main elements in the gas and the composition of dust;\n* the unattenuated stellar spectral energy distribution (SED); * the\nnebular SED, using nebular continua and emission lines precomputed with\ncode Cloudy (Ferland et al. 2017); * the attenuation in star-forming\nclouds and the diffuse interstellar medium, by absorption and scattering\non dust grains, of the stellar and nebular SEDs. For this, the code uses\ngrids of the transmittance for spiral and spheroidal galaxies. We\nprecomputed these grids through Monte Carlo simulations of radiative\ntransfer based on the method of virtual interactions; * the re-emission\nby grains of the light they absorbed, taking into account stochastic\nheating. The main innovation compared to P{\\textbackslash}'egase.2 is the modeling of\ndust emission and its evolution. The computation of nebular emission has\nalso been entirely upgraded to take into account metallicity effects and\ninfrared lines. Other major differences are that complex scenarios of\nevolution (derived for instance from cosmological simulations), with\nseveral episodes of star formation, infall or outflow, may now be\nimplemented, and that the detailed evolution of the most important\nelements -- not only the overall metallicity -- is followed.},\n\turldate = {2019-02-08},\n\tjournal = {arXiv e-prints},\n\tauthor = {Fioc, Michel and Rocca-Volmerange, Brigitte},\n\tmonth = feb,\n\tyear = {2019},\n\tkeywords = {Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics},\n\tpages = {arXiv:1902.02198},\n}\n\n","author_short":["Fioc, M.","Rocca-Volmerange, B."],"key":"fioc_pegase.3_2019","id":"fioc_pegase.3_2019","bibbaseid":"fioc-roccavolmerange-theptextbackslashegase3codeofspectrochemicalevolutionofgalaxiesdocumentationandcomplements-2019","role":"author","urls":{"Paper":"http://adsabs.harvard.edu/abs/2019arXiv190202198F"},"keyword":["Astrophysics - Astrophysics of Galaxies","Astrophysics - Instrumentation and Methods for Astrophysics"],"metadata":{"authorlinks":{}}},"bibtype":"article","biburl":"https://bibbase.org/zotero/polyphant","dataSources":["7gvjSdWrEu7z5vjjj"],"keywords":["astrophysics - astrophysics of galaxies","astrophysics - instrumentation and methods for astrophysics"],"search_terms":["textbackslash","egase","code","spectrochemical","evolution","galaxies","documentation","complements","fioc","rocca-volmerange"],"title":"The P\\textbackslash'egase.3 code of spectrochemical evolution of galaxies: documentation and complements","year":2019}