151 research outputs found
Separate ways: The Mass-Metallicity Relation does not strongly correlate with Star Formation Rate in SDSS-IV MaNGA galaxies
We present the integrated stellar mass-metallicity relation (MZR) for more
than 1700 galaxies included in the integral field area SDSS-IV MaNGA survey.
The spatially resolved data allow us to determine the metallicity at the same
physical scale (effective radius in arcsecs, ) using a
heterogeneous set of ten abundance calibrators. Besides scale factors, the
shape of the MZR is similar for all calibrators, consistent with those reported
previously using single-fiber and integral field spectroscopy. We compare the
residuals of this relation against the star formation rate (SFR) and specific
SFR (sSFR). We do not find a strong secondary relation of the MZR with either
SFR or the sSFR for any of the calibrators, in contrast with previous
single-fiber spectroscopic studies. Our results agree with an scenario in which
metal enrichment happens at local scales, with global outflows playing a
secondary role in shaping the chemistry of galaxies and cold-gas inflows
regulating the stellar formation.Comment: 10 pages, 9 Figures. Accepted for publication in Ap
The Calar Alto Legacy Integral Field Area Survey: extended and remastered data release
This paper describes the extended data release of the Calar Alto Legacy
Integral Field Area (CALIFA) survey (eDR). It 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 (3700-7500{\AA}, 6{\AA}/FWHM) and the CALIFA observing strategy. It
includes galaxies of any morphological type, star-formation stage, a wide range
of stellar masses (10 10 Msun ), at an average redshift of
0.015 (90\% within 0.005z0.05). Primarily selected based on the
projected size and apparent magnitude, we demonstrate that it can be volume
corrected resulting in a statistically limited but representative 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").To illustrate the usability and
quality of the data, we extracted two aperture spectra for each galaxy (central
1.5" and fully integrated), and analyze them using pyFIT3D. 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. DATA RELEASE:
http://ifs.astroscu. unam.mx/CALIFA_WEB/public_html/Comment: 30 pages, 26 figures, accepted for publishing in the MNRA
The local and global relations between , and that regulate star-formation
Star-formation is one of the main processes that shape galaxies, defining its
stellar population and metallicity production and enrichment. It is nowadays
known that this process is ruled by a set of relations that connect three
parameters: the molecular gas mass, the stellar mass and the star-formation
rate itself. These relations are fulfilled at a wide range of scales in
galaxies, from galaxy wide to kpc-scales. At which scales they are broken, and
how universal they are (i.e., if they change at different scales or for
different galaxy types) it is still an open question. We explore here how those
relations compare at different scales using as proxy the new analysis done
using Integral Field Spectroscopy data and CO observations data from the
EDGE-CALIFA survey and the AMUSSING++ compilation.Comment: 8 pages, 3 figures, 1 table, proceedings of the IAU Symposium 373:
Resolving the Rise and Fall of Star Formation in Galaxie
The Calar Alto Legacy Integral Field Area Survey: spatial resolved properties
We present the analysis performed using the pyPipe3D pipeline for the 895
galaxies that comprises the eCALIFA data release Sanchez et al. submitted, data
with a significantly improved spatial resolution (1.0-1.5"/FWHM). We include a
description of (i) the analysis performed by the pipeline, (ii) the adopted
datamodel for the derived spatially resolved properties and (iii) the catalog
of integrated, characteristics and slope of the radial gradients for a set of
observational and physical parameters derived for each galaxy. We illustrate
the results of the analysis (i) using the NGC\,2906 as an archetypal galaxy,
showing the spatial distribution of the different derived parameters and
exploring in detail the properties of the ionized gas, and (ii) showing
distribution of the spatial resolved ionized gas across the classical
[OIII]/H vs. [NII]/H for the whole galaxy sample. In general our
results agree with previous published ones, however, tracing radial patterns
and segregating individual ionized structures is improved when using the
current dataset. All the individual galaxy dataproducts and the catalog
discussed along this article are distributed as part of the eCALIFA data
release http://ifs.astroscu.unam.mx/CALIFA_WEB/public_html/Comment: 47 pages, 8 tables, 9 figures, submitted the 12th of April 2023 to
RMxA
The WHaD diagram: Classifying the ionizing source with one single emission line
The usual approach to classify the ionizing source using optical spectroscopy
is based on the use of diagnostic diagrams that compares the relative strength
of pairs of collisitional metallic lines (e.g., [O iii] and [N ii]) with
respect to recombination hydrogen lines (e.g., H{\beta} and H{\alpha}). Despite
of being accepted as the standard procedure, it present known problems,
including confusion regimes and/or limitations related to the required
signal-to-noise of the involved emission lines. These problems affect not only
our intrinsic understanding of inter-stellar medium and its poroperties, but
also fundamental galaxy properties, such as the star-formation rate and the
oxygen abundance, and key questions just as the fraction of active galactic
nuclei, among several others. We explore the existing alternatives in the
literature to minimize the confusion among different ionizing sources and
proposed a new simple diagram that uses the equivalent width and the velocity
dispersion from one single emission line, H{\alpha}, to classify the ionizing
sources. We use aperture limited and spatial resolved spectroscopic data in the
nearby Universe (z{\sim}0.01) to demonstrate that the new diagram, that we
called WHaD, segregates the different ionizing sources in a more efficient way
that previously adopted procedures. A new set of regions are defined in this
diagram to select betweeen different ionizing sources. The new proposed diagram
is well placed to determine the ionizing source when only H{\alpha} is
available, or when the signal-to-noise of the emission lines involved in the
classical diagnostic diagrams (e.g., H{\beta}).Comment: 10 pages, 5 figures, accepted for publishing in A&
Census of HII regions in NGC 6754 derived with MUSE: Constraints on the metal mixing scale
We present a study of the HII regions in the galaxy NGC 6754 from a two
pointing mosaic comprising 197,637 individual spectra, using Integral Field
Spectrocopy (IFS) recently acquired with the MUSE instrument during its Science
Verification program. The data cover the entire galaxy out to ~2 effective
radii (re ), sampling its morphological structures with unprecedented spatial
resolution for a wide-field IFU. A complete census of the H ii regions limited
by the atmospheric seeing conditions was derived, comprising 396 individual
ionized sources. This is one of the largest and most complete catalogue of H ii
regions with spectroscopic information in a single galaxy. We use this
catalogue to derive the radial abundance gradient in this SBb galaxy, finding a
negative gradient with a slope consistent with the characteristic value for
disk galaxies recently reported. The large number of H ii regions allow us to
estimate the typical mixing scale-length (rmix ~0.4 re ), which sets strong
constraints on the proposed mechanisms for metal mixing in disk galaxies, like
radial movements associated with bars and spiral arms, when comparing with
simulations. We found evidence for an azimuthal variation of the oxygen
abundance, that may be related with the radial migration. These results
illustrate the unique capabilities of MUSE for the study of the enrichment
mechanisms in Local Universe galaxies.Comment: 13 pages, 7 Figurs, accepted for publishing in A&
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