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Extended CALIFA DR overview
The extended data release of the Calar Alto Legacy Integral Field Area
(CALIFA) survey (eDR) comprises science-grade quality data for 895
galaxies obtained with the PMAS/PPak instrument at the 3.5 m telescope
at the Calar Alto Observatory along the last 12 years, using the V500
setup (3700-7500Å, 6Å/FWHM) and the CALIFA observing strategy. It
includes galaxies of any morphological type, star-formation stage,
covering a wide range of stellar masses (∼10 7 -10 12 M ), at an
average redshift of ∼0.015 (90% within 0.005< z <0.05). Primarily
selected based on the projected size and apparent magnitude, we
demonstrate that it can be volume corrected resulting in a
statistically limited but rep- resentative sample of the population of
galaxies in the nearby Universe. All the data were homogeneous
re-reduced, introducing a set of modifications to the previous
reduction. The most relevant is the development and implementation of
a new cube-reconstruction algorithm that provides with an (almost)
seeing-limited spatial resolution (FWHM PSF ∼1.0 00 ).To illustrate
the usability and quality of the data, we extracted two aperture
spectra for each gañaxy (central 1.5 00 and fully integrated), and
analyze them using pyFIT3D
(Lacerda et al. 2022). We obtain a set of
observational and physical properties of both the stellar populations
and the ionized gas, that have been compared for the two apertures,
exploring their distributions as a function of the stellar masses and
morphologies of the galaxies, comparing with recent results in the
literature.
Finally, we analyze the new dataset using
the pyPipe3D pipeline
(Lacerda et al. 2022), extracting the spatial
resolved distribution for a set of properties of both the ionized gas
emission lines and the stellar population. We distribute the results
of this analysis, including an individual FITs file in the Pipe3D
format for each galaxy and a catalog of integrated, aperture limited
and characteristic properties (e.g., stellar mass, SFR, oxygen
abundances...), and the corresponding slopes of their radial
gradients.
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