Using the largest sample of galaxies observed with an optical integral field unit (IFU, the SDSS-IV MaNGA survey, ≈10000 targets), we derive the radial distribution of the physical properties ...obtained from the stellar continuum and the ionized-gas emission lines. Given the large sample, we are able to explore the impact of the total stellar mass and morphology by averaging those radial distributions for different bins of both global properties. In general, we find that most of the properties exhibit a negative gradient, with a secondary impact by global properties. Our results confirm the intimate interplay between the properties of the stellar component and those of the ionized gas at local (kpc) scales to set the observed radial gradients. The resemblance of the gradients for similar global properties indicates statistical similar histories of star formation and chemical enrichment, with an initial radial gas distribution following the potential of the galaxy.
We present P 3D, an analysis pipeline based on the FIT3D fitting tool, developed to explore the properties of the stellar populations and ionized gas of integral field spectroscopy (IFS) data. P 3D ...was created to provide coherent, simple to distribute, and comparable dataproducts, independently of the origin of the data, focused on the data of the most recent IFU surveys (e.g., CALIFA, MaNGA, and SAMI), and the last generation IFS instruments (e.g., MUSE). In this article we describe the different steps involved in the analysis of the data, illustrating them by showing the dataproducts derived for NGC 2916, observed by CALIFA and P-MaNGA. As a practical example of the pipeline we present the complete set of dataproducts derived for the 200 datacubes that comprises the V500 setup of the CALIFA Data Release 2 (DR2), making them freely available through the network. Finally, we explore the hypothesis that the properties of the stellar populations and ionized gas of galaxies at the effective radius are representative of the overall average ones, finding that this is indeed the case.
Abstract
We present a new code named pyhiiextractor, which detects and extracts the main features (positions and radii) of clumpy ionized regions, i.e. candidate H ii regions, using $\rm {H}\,\alpha$ ...emission line images. Our code is optimized to be used on the dataproducts provided by the pipe3d pipeline (or dataproducts with such a format), applied to high-spatial resolution integral field spectroscopy data (like that provided by the AMUSING++ compilation, using muse). The code provides the properties of both the underlying stellar population and the emission lines for each detected H ii candidate. Furthermore, the code delivers a novel estimation of the diffuse ionized gas (DIG) component, independent of its physical properties, which enables a decontamination of the properties of the H ii regions from the DIG. Using simulated data, mimicking the expected observations of spiral galaxies, we characterize pyhiiextractor and its ability to extract the main properties of the H ii regions (and the DIG), including the line fluxes, ratios, and equivalent widths. Finally, we compare our code with other such tools adopted in the literature, which have been developed or used for similar purposes: pyhiiexplorer, sourceextractor, hiiphot, and astrodendro. We conclude that pyhiiextractor exceeds the performance of previous tools in aspects such as the number of recovered regions and the distribution of sizes and fluxes (an improvement that is especially noticeable for the faintest and smallest regions). pyhiiextractor is therefore an optimal tool to detect candidate H ii regions, offering an accurate estimation of their properties and a good decontamination of the DIG component.
Abstract
We compare the CO(1–0) and H
α
kinematics in 34 nearby galaxies, selected from the ALMaQUEST and EDGE-CALIFA surveys. We use 3D-Barolo, a 3D tilted-ring model, to derive the CO and H
α
...rotation curves. Before comparing rotation curves in the 34 nearby galaxies, we found systematics between the MaNGA and CALIFA data using eight MaNGA-CALIFA overlapping galaxies. We assume the rotation curves based on the MaNGA data are accurate and made the corresponding correction to the CALIFA data. Our result shows that ∼56% (19/34) of our galaxies present slower H
α
rotation curves compared to the CO rotation curves, with a median value of 6.5 km s
−1
. The remaining galaxies (15/34) show consistent CO–H
α
rotation velocity within uncertainties. As a result, the H
α
rotation may underestimate the total dynamical mass by 6% for a circular velocity of 200 km s
−1
(the median value in our sample). Furthermore, the difference in the velocity between the CO and H
α
rotational velocity is found to correlate with the difference in velocity dispersion between CO and H
α
, suggesting that gas pressure plays a role in the discrepancy in velocity. After incorporating the effect of pressure support due to the turbulent gas motion into our sample, the median value of the difference in the velocities decreases to 1.9 km s
−1
, which in turn reduces the underestimation of the dynamical mass to ∼2%. Finally, we also investigate the role that the extraplanar diffuse ionized gas plays in the discrepancy in the velocity of CO–H
α
.
We present a new code named pyHIIextractor, which detects and extracts the main features (positions and radii) of clumpy ionized regions, i.e. candidate HII regions, using H{\alpha} emission line ...images. Our code is optimized to be used on the dataproducts provided by the Pipe3D pipeline (or dataproducts with such a format), applied to high spatial resolution Integral Field Spectroscopy data (like that provided by the AMUSING++ compilation, using MUSE). The code provides the properties of both the underlying stellar population and the emission lines for each detected H ii candidate. Furthermore, the code delivers a novel estimation of the diffuse ionized gas (DIG) component, independent of its physical properties, which enables a decontamination of the properties of the HII regions from the DIG. Using simulated data, mimicking the expected observations of spiral galaxies, we characterise pyHIIextractor and its ability to extract the main properties of the H ii regions (and the DIG), including the line fluxes, ratios and equivalent widths. Finally, we compare our code with other such tools adopted in the literature, which have been developed or used for similar purposes: pyhIIexplorer, SourceExtractor, HIIphot, and astrodendro. We conclude that pyHIIextractor exceeds the performance of previous tools in aspects such as the number of recovered regions and the distribution of sizes and fluxes (an improvement that is especially noticeable for the faintest and smallest regions). pyHIIextractor is therefore an optimals tool to detect candidate HII regions, offering an accurate estimation of their properties and a good decontamination of the DIG component.
Using the largest sample of galaxies observed with an optical integral field unit (IFU, the SDSS-IV MaNGA survey, \(\sim\)10000 targets), we derive the radial distribution of the physical properties ...obtained from the stellar continuum and the ionized-gas emission lines. Given the large sample, we are able to explore the impact of the total stellar mass and morphology by averaging those radial distributions for different bins of both global properties. We use a piece-wise analysis to characterize the slopes of the gradients from those properties at different galactocentric distances. In general we find that most of the properties -- derived from both the stellar continuum and the ionized gas emission lines -- exhibit a negative gradient with a secondary impact by global properties such as the total stellar mass or morphology. Our results confirm the intimate interplay between the properties of the stellar component and those of the ionized gas at local (kpc) scales in order to set the observed gradients. Furthermore, the resemblance of the gradients for similar global properties (in particular for the stellar parameters) indicates statistical similar histories of star formation and chemical enrichment with an initial radial gas distribution following the potential of the galaxy.
We present an updated version of the mass--metallicity relation (MZR) using integral field spectroscopy data obtained from 734 galaxies observed by the CALIFA survey. These unparalleled spatially ...resolved spectroscopic data allow us to determine the metallicity at the same physical scale (\(\mathrm{R_{e}}\)) for different calibrators. We obtain MZ relations with similar shapes for all calibrators, once the scale factors among them are taken into account. We do not find any significant secondary relation of the MZR with either the star formation rate (SFR) or the specific SFR for any of the calibrators used in this study, based on the analysis of the residuals of the best fitted relation. However we do see a hint for a (s)SFR-dependent deviation of the MZ-relation at low masses (M\(<\)10\(^{9.5}\)M\(_\odot\)), where our sample is not complete. We are thus unable to confirm the results by Mannucci et al. (2010), although we cannot exclude that this result is due to the differences in the analysed datasets. In contrast, our results are inconsistent with the results by Lara-Lopez et al. (2010), and we can exclude the presence of a SFR-Mass-Oxygen abundance Fundamental Plane. These results agree with previous findings suggesting that either (1) the secondary relation with the SFR could be induced by an aperture effect in single fiber/aperture spectroscopic surveys, (2) it could be related to a local effect confined to the central regions of galaxies, or (3) it is just restricted to the low-mass regime, or a combination of the three effects.
La colectomía en la colitis ulcerosa (CU), es una decisión terapéutica que se asocia con distintos aspectos de su evolución y no exenta de morbilidad. Objetivo Describir la causa, tipo de ...intervención y mortalidad asociada de 33 ptes que han sufrido colectomía en nuestra cohorte histórica de 636 CU, desde el diag hasta el 31 de Dic 2006 o la muerte. Métodos Estudio epidemiológico descriptivo, poblacional, prospectivo. Incluimos 33 ptes (48,48% mujeres) intervenidos, de la cohorte de 636 ptes con CU, en el Área Sanitaria V de Gijón. Media de seguimiento de 12,90 años (en ptes vivos 15,68 años y muertos de 4,25 años). La Colectomía se clasifica como colectomía con ileostomía (CT+I), o con anatomosis ileo-rectal (CT-AIR), panproctocolectomía con ileostomía (PTC+I), panproctocolectomía con reservorio (PTC+R), y Colectomía parcial+colostomía(CP+C). Definimos cirugía precoz como intervención realizada en los primeros 2 años de enfermedad y cirugía urgente como la realizada 24 horas después de la decisión de operar. Mortalidad perioperatoria, la que se produce durante el año siguiente a la cirugía. Causas de Intervención: enf Aguda Grave, Crónica refractaria, Hemorragia Masiva y otras. Resultados Se han realizado 60 cirugías en 33 ptes (media: 1,81 cirugías /ptes; rango: 1 a 6). Causas de intervención: enf Aguda Grave, 18 (54,54%), Crónica refractaria, 9 (27,27%), Hemorragia Masiva, 5 (15,15%) y displasia, 1(3,03%). Tipo de Intervención: CT+I, 4 (12,12%); CT-AIR, 3 (9,09%); PTC+I, 18 (54,54%); PTC+R, 3 (9,09%) y CP+C, 5 (15,15%). Cirugía precoz, 19(57,57%). Cirugía urgente 24 (72,72%). Ningún cáncer colorectal. Mueren 8 ptes (24,24%); Mortalidad peri-operatoria, 7 (87,5%). La mortalidad se asocia con extensión (7 pancolitis 87,5%), negativamente con el hab de fumar (6 no fum y 1 ex-fumador) y cirugía precoz (6 pacientes 75%) y cirugía urgente (6 casos 25%). 2 de 13 (15,38%) pacientes operados mueren antes de 1990 y 6 de 20 (30%) después de 1991. Conclusiones Destacamos que la mayoría de los ptes se intervienen por complicación aguda grave con cirugía urgente. La tasa de mortalidad es alta, asociada a intervención urgente y precoz.
