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We present an extensive exploration of the impact of 29 physical parameters in the oxygen abundance for a sample of 299 star-forming galaxies extracted from the extended CALIFA sample. We corroborate that the stellar mass is the physical parameter that better traces the observed oxygen abundance (i.e., the mass-metallicity relation, MZR), while other physical parameters could play a potential role in shaping this abundance, but with a lower significant impact. We find that the functional form that best describes the MZR is a third-order polynomial function. From the residuals between this best functional form and the MZR, we find that once considered the impact of the mass in the oxygen abundance, the other physical parameters do not play a significant secondary role in shaping the oxygen abundance in these galaxies (including the gas fraction or the star formation rate). Our analysis suggests that the origin of the MZR is related to the chemical enrichment evolution of the interstellar medium due, most likely, to the build-up of stellar mass in these star-forming galaxies., 27 pages, 10 figures, 5 tables

Most secular effects produced by stellar bars strongly depend on the pattern speed. Unfortunately, it is also the most difficult observational parameter to estimate. In this work, we measured the bar pattern speed of 97 Milky-Way Analogue galaxies from the MaNGA survey using the Tremaine-Weinberg method. The sample was selected by constraining the stellar mass and morphological type. We improve our measurements by weighting three independent estimates of the disc position angle. To recover the disc rotation curve, we fit a kinematic model to the H$_\alpha$ velocity maps correcting for the non-circular motions produced by the bar. The complete sample has a smooth distribution of the bar pattern speed ($\Omega_{Bar}=28.14^{+12.30}_{-9.55}$ km s$^{-1}$ kpc $^{-1}$), corotation radius ($R_{CR} = 7.82^{+3.99}_{-2.96}$ kpc) and the rotation rate ($\mathcal{R} = 1.35^{+0.60}_{-0.40}$). We found two sets of correlations: (i) between the bar pattern speed, the bar length and the logarithmic stellar mass (ii) between the bar pattern speed, the disc circular velocity and the bar rotation rate. If we constrain our sample by inclination within $30 \degree < i < 60 \degree$ and relative orientation $20\degree, Comment: 19 pages, 20 figures, 2 tables, accepted for publication in MNRAS

Estimating the bar pattern speed (\Om{}) is one of the main challenges faced in understanding the role of stellar bars in galaxy dynamical evolution. This work aims to characterise different uncertainty sources affecting the Tremaine Weinberg (TW)-method to study the correlation between bar and galaxies physical parameters. We use a sample of 15 MaNGA SDSS-IV galaxies and 3 CALIFA galaxies from \cite{Aguerri2015}. We studied the errors related with (i) galaxy centre determination, (ii) disc position angle (PA) emphasising the difficulties triggered by outer non-axisymmetric structures besides the bar, (iii) the slits length and (iv) the spatial resolution. In average, the PA uncertainties range $\sim 15 \%$, the slit length $\sim 9 \%$ and the centring error $\sim 5 \%$. Reducing the spatial resolution increases the sensitivity to the PA error. Through Monte Carlo simulations, we estimate the probability distribution of the \R{} bar speed parameter. The present sample is composed of 7 slow, 4 fast and 7 ultrafast bars, with no trend with morphological types. Although uncertainties and low sample numbers may mask potential correlations between physical properties, we present a discussion of them: We observe an anti-correlation of \Om{} with the bar length and the stellar mass, suggesting that massive galaxies tend to host longer and slower bars. We also observe a correlation of the molecular gas fraction with \R{}, and a weak anti-correlation with \Om{}, suggesting that bars rotate slower in gaseous discs. Confirmation of such trends awaits future studies., Comment: 17 pages, 11 figures, accepted for publication in MNRAS

We used ionized gas and stellar kinematics for 667 spatially resolved galaxies publicly available from the Calar Alto Legacy Integral Field Area survey (CALIFA) third Data Release with the aim of studying kinematic scaling relations as the Tully & Fisher (TF) relation using rotation velocity, Vrot, the Faber & Jackson (FJ) relation using velocity dispersion, σ, and also a combination of Vrot and s through the SK parameter defined as S K 2 = KV rot 2 + σ2 with constant K. Late-type and early-type galaxies reproduce the TF and FJ relations. Some earlytype galaxies also follow the TF relation and some late-type galaxies the FJ relation, but always with larger scatter. On the contrary, when we use the SK parameter, all galaxies, regardless of the morphological type, lie on the same scaling relation, showing a tight correlation with the total stellar mass, M*. Indeed, we find that the scatter in this relation is smaller or equal to that of the TF and FJ relations. We explore different values of the K parameter without significant differences (slope and scatter) in our final results with respect to the case K = 0.5 besides a small change in the zero-point. We calibrate the kinematic S K 2 dynamical mass proxy in order to make it consistent with sophisticated published dynamical models within 0.15 dex. We show that the SK proxy is able to reproduce the relation between the dynamical mass and the stellar mass in the inner regions of galaxies. Our result may be useful in order to produce fast estimations of the central dynamical mass in galaxies and to study correlations in large galaxy surveys. © 2018 The Author(s)., We thank the support by CONACYT grant CB-285080. OV and EA acknowledge support from the PAPIIT grant IN112518. S.F.S. thank PAPIIT-DGAPA-IA101217 (UNAM) project. We would like to thank Damian Mast for his valuable job observing the CALIFA galaxies. Many thanks to Gigi Y. C. Leung from the Max Planck Institute for Astronomy for providing us the stellar and dynamical masses from dynamical models for the 54 galaxies from her study. GvdV acknowledges funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme under grant agreement No 724857 (Consolidator Grant ArcheoDyn).

We report the detection of a highly collimated linear emission-line structure in the spiral galaxy NGC\,232 through the use of integral field spectroscopy data from the All-weather MUse Supernova Integral field Nearby Galaxies (AMUSING) survey. This jet--like feature extends radially from the nucleus and is primarily detected in [oiii]$\lambda$5007 without clear evidence of an optical continuum counterpart. The length of the radial structure projected on sky reaches $\sim 3$ kpc, which makes NGC\,232 the second longest emission-line jet reported. The ionized gas presents extreme [Oiii]/H$\beta$ and [Nii]/H$\alpha$ line ratios, increasing along the jet-like structure. We discuss three possible scenarios to explain the observed structure: (i) direct ionization of in-falling material from the intergalactic medium by the AGN; (ii) photo-ionization by an un-detected optical counter-part of the radio jet and (iii) fast shocks ionization due to the lateral expansion of the radio jet across the ISM. Our analysis favors in-situ ionization., Comment: 7 pages, 2 figures, accepted for publishing in ApJL

We explore the spiral arm structural properties in a large variety of simulated galaxy systems. We study spiral arms arising from isolated barred and unbarred galaxies, as well as from interactions with small satellites. In all these first models, galactic systems are all embedded in a spherical dark matter halo. We also study spiral arms arising from a galactic system embedded in a triaxial dark matter halo. Simulations used in this work have been obtained by using different N-body codes and initial conditions techniques. Our strategy is to study the 3D arm structure through the analysis of pitch angle, along/transverse/vertical density laws and their corresponding scale lengths, and spiral lifetime. Our main results are as follows. First, the radial density profile of all spiral arms analyzed in this work is exponential. This profile resembles the one of the disk but with a scale length that is systematically larger (5%-40%). This result suggests that spiral arm gravitational influence is important beyond the scale radius of the disk. Second, the vertical and transversal density laws of the spiral arms follow a sech2. The vertical scale length is compatible with the one of the disk; this is observed in all spiral arms analyzed here, independently of their origin, i.e., bar, high-order disk perturbation, tidal interaction with satellites, or halo triaxiality. Third, in the triaxial and satellite simulations, spiral arms follow a logarithmic locus all through their lifetime; the remaining models develop transient, recurrent, and short-lived spirals with a nondefined locus. In all cases, spiral arms wind up in their lifetime with a small pitch angle reduction. It is common that newborn spirals inherit the pitch angle of the previous ones; this result challenges the dynamical relevance of arm evolution. Finally, from the analysis of public photometric observations of NGC 2543, we state that the properties of observed spiral arm structure can be consistent with our conclusions. Further and systematic comparisons with observations are needed in order to confirm our results.