Spectro-photometric decomposition of galaxy structural components. (arXiv:1901.08075v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mendez_Abreu_J/0/1/0/all/0/1">J. Méndez-Abreu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_S/0/1/0/all/0/1">S. F. Sánchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lorenzo_Caceres_A/0/1/0/all/0/1">A. de Lorenzo-Cáceres</a>
Galaxies are complex systems made up of different structural components such
as bulges, discs, and bars. Understanding galaxy evolution requires unveiling,
independently, their history of stellar mass and metallicity assembly. We
introduce C2D, a new algorithm to perform spectro-photometric multi-component
decompositions of integral field spectroscopy (IFS) datacubes. The galaxy
surface-brightness distribution at each wavelength (quasi-monochromatic image)
is fitted using GASP2D, a 2D photometric decomposition code. As a result, C2D
provides both a characteristic one-dimensional spectra and a full datacube with
all the spatial and spectral information for every component included in the
fit. We show the basic steps of the C2D spectro-photometric fitting procedure,
tests on mock datacubes demonstrating its reliability, and a first application
of C2D to a sample of three early-type galaxies (ETGs) observed within the
CALIFA survey. The resulting datacubes from C2D are processed through the
PIPE3D pipeline obtaining both the stellar populations and ionised gas
properties of bulges and discs. This paper presents an overview of the
potential of C2D+PIPE3D to unveil the formation and evolution of galaxies.
Galaxies are complex systems made up of different structural components such
as bulges, discs, and bars. Understanding galaxy evolution requires unveiling,
independently, their history of stellar mass and metallicity assembly. We
introduce C2D, a new algorithm to perform spectro-photometric multi-component
decompositions of integral field spectroscopy (IFS) datacubes. The galaxy
surface-brightness distribution at each wavelength (quasi-monochromatic image)
is fitted using GASP2D, a 2D photometric decomposition code. As a result, C2D
provides both a characteristic one-dimensional spectra and a full datacube with
all the spatial and spectral information for every component included in the
fit. We show the basic steps of the C2D spectro-photometric fitting procedure,
tests on mock datacubes demonstrating its reliability, and a first application
of C2D to a sample of three early-type galaxies (ETGs) observed within the
CALIFA survey. The resulting datacubes from C2D are processed through the
PIPE3D pipeline obtaining both the stellar populations and ionised gas
properties of bulges and discs. This paper presents an overview of the
potential of C2D+PIPE3D to unveil the formation and evolution of galaxies.
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