Evidence of Ongoing Radial Migration in NGC 6754: Azimuthal Variations of the Gas Properties

Sánchez-Menguiano, L.; Sánchez, S. F.; Kawata, Daisuke; Chemin, L.; Pérez, I.; Ruiz-Lara, T.; Sánchez‐Blázquez, P.; Galbany, L.; Anderson, J. P.; Grand, Robert J. J.; Minchev, Ivan; Gómez, Facundo A.

doi:10.3847/2041-8205/830/2/l40

Cited by 67 publications

(94 citation statements)

References 47 publications

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“…So far it comprises ∼328 galaxies, being the core of the current compilation. This sample has been used to explore different science topics: (i) the radial profiles of the oxygen abundances in galaxies (Sánchez-Menguiano et al 2018), and its azimuthal variation (Sánchez et al 2015;Sánchez-Menguiano et al 2016); (ii) extended ionized gas fillaments associated to galaxy interactions (Prieto et al 2016a); (iii) the discovery of new strong lenses (Galbany et al 2018), and the optical counterpart of a radio-jet (López-Cobá et al 2017a); (iv) the derivation of main galaxy kinematic parameters such as velocity and velocity dispersion by different approaches (Bellocchi et al 2019); (v) individual type II supernova (Meza et al 2019); (vi) ionized gas tails (Boselli et al 2018); besides (vi) the local environment of supernovae, i.e., the major goal of the survey (Galbany et al 2016;Krühler et al 2017).…”

Section: The Amusing++ Samplementioning

confidence: 99%

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

López-Cobá¹,

Sánchez²,

Anderson

et al. 2020

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We present here AMUSING++; the largest compilation of nearby galaxies observed with the MUSE integral field spectrograph so far. This collection consists of 635 galaxies from different MUSE projects covering the redshift interval 0.0002 < z < 0.1. The sample and its main properties are characterized and described in here. It includes galaxies of almost all morphological types, with a good coverage in the color-magnitude diagram, within the stellar mass range between 10 8 to 10 12 M , and with properties resembling those of a diameter-selected sample. The AMUSING++ sample is therefore suitable to study, with unprecendent detail, the properties of nearby galaxies at global and local scales, providing us with more than 50 million individual spectra. We use this compilation to investigate the presence of galactic outflows. We exploit the use of combined emission-line images to explore the shape of the different ionized components and the distribution along classical diagnostic diagrams to disentangle the different ionizing sources across the optical extension of each galaxy. We use the cross correlation function to estimate the level of symmetry of the emission lines as an indication of the presence of shocks and/or active galactic nuclei. We uncovered a total of 54 outflows, comprising ∼8% of the sample. A large number of the discovered outflows correspond to those driven by active galactic nuclei (∼60%), suggesting some bias in the selection of our sample. No clear evidence was found that outflow host galaxies are highly star-forming, and outflows appear to be found within all galaxies around the star formation sequence.

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Section: The Amusing++ Samplementioning

confidence: 99%

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

López-Cobá¹,

Sánchez²,

Anderson

et al. 2020

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“…Since then, new works on the gas-phase abundance distribution based on MUSE data have arisen (e.g. Kreckel et al 2016;Sánchez-Menguiano et al 2016a;Vogt et al 2017), confirming the potential of this instrument for such studies.…”

Section: Introductionmentioning

confidence: 97%

“…IFS surveys have also allowed us to find a relation between the inner abundance drop presented in spiral galaxies and the galaxy mass, being this feature more common in more massive galaxies (Sánchez-Menguiano et al 2016b). Regarding the study of azimuthal abundance variations in spiral galaxies, Zinchenko et al (2016) suggested that there is no significant global azimuthal asymmetry in the oxygen abundance distribution, establishing a limit of ∼ 0.05 dex for these asymmetries, although works analysing in detail individual galaxies indicate otherwise (Sánchez-Menguiano et al 2016a;Vogt et al 2017).…”

Section: Introductionmentioning

confidence: 99%

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Sánchez-Menguiano

Sanchez

Pérez

et al. 2018

A&A

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146

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We characterised the oxygen abundance radial distribution of a sample of 102 spiral galaxies observed with VLT/MUSE using the O3N2 calibrator. The high spatial resolution of the data allowed us to detect 14345 H ii regions with the same image quality as with photometric data, avoiding any dilution effect. We developed a new methodology to automatically fit the abundance radial profiles, finding that 55 galaxies of the sample exhibit a single negative gradient. The remaining 47 galaxies also display, as well as this negative trend, either an inner drop in the abundances (21), an outer flattening (10), or both (16), which suggests that these features are a common property of disc galaxies. The presence and depth of the inner drop depends on the stellar mass of the galaxies with the most massive systems presenting the deepest abundance drops, while there is no such dependence in the case of the outer flattening. We find that the inner drop appears always around 0.5 r e , while the position of the outer flattening varies over a wide range of galactocentric distances. Regarding the main negative gradient, we find a characteristic slope in the sample of α O/H = − 0.10 ± 0.03 dex/r e . This slope is independent of the presence of bars and the density of the environment. However, when inner drops or outer flattenings are detected, slightly steeper gradients are observed. This suggests that radial motions might play an important role in shaping the abundance profiles. We define a new normalisation scale ('the abundance scale length', r O/H ) for the radial profiles based on the characteristic abundance gradient, with which all the galaxies show a similar position for the inner drop (∼ 0.5 r O/H ) and the outer flattening (∼ 1.5 r O/H ). Finally, we find no significant dependence of the dispersion around the negative gradient with any property of the galaxies, with values compatible with the uncertainties associated with the derivation of the abundances.

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“…In this regard, the advent of Integral Field Spectroscopy (IFS) instruments combining large field-of-views (FoV) and high spatial resolution has meant a revolution in the progress of 2D abundance distribution studies. Since then, a growing number of works have been able to detect such elusive variations in individual galaxies: NGC 6754 (Sánchez-Menguiano et al 2016b, see also Sánchez et al 2015), NGC 1365 (Ho et al 2017), HCG 91c (Vogt et al 2017), and NGC 2997 (Ho et al 2018). The magnitude of the reported variations differ from study to study (from 0.06 in NGC 2997 to 0.4 dex in NGC 1365), but in all cases more metal-rich gas has been observed associated with the spiral structure.…”

Section: Introductionmentioning

confidence: 99%

Arm–interarm gas abundance variations explored with MUSE: the role of spiral structure in the chemical enrichment of galaxies

Sánchez-Menguiano

Sánchez

Pérez

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Spiral arms are the most characteristic features of disc galaxies, easily distinguishable due to their association with ongoing star formation. However, the role of spiral structure in the chemical evolution of galaxies is unclear. Here we explore gas-phase abundance variations between arm and interarm regions for a sample of 45 spiral galaxies using high spatial resolution VLT/MUSE Integral Field Spectroscopy data. We report the presence of more metal-rich H ii regions in the spiral arms with respect to the corresponding interarm regions for a large subsample of galaxies (45 − 65% depending on the adopted calibrator for the abundance derivation). A small percentage of the sample is observed to display the opposite trend, that is, more metal-poor H ii regions in the spiral arms compared to that of the interarms (5−20% depending on the calibrator). We investigate the dependence of the variations with three galaxy properties: the stellar mass, the presence of bars, and the flocculent/grand design appearance of spiral arms. In all cases, we observe that the arm-interarm abundance differences are larger (positive) in more massive and grand-design galaxies. This is confirmed by an analogous spaxel-wise analysis, which also shows a noticeable effect of the presence of galactic bars, with barred systems presenting larger (positive) arm-interarm abundance variations than unbarred systems. The comparison of our results with new predictions from theoretical models exploring the nature of the spirals would highly impact on our knowledge on how these structures form and affect their host galaxies.

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Evidence of Ongoing Radial Migration in NGC 6754: Azimuthal Variations of the Gas Properties

Cited by 67 publications

References 47 publications

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

The AMUSING++ Nearby Galaxy Compilation. I. Full Sample Characterization and Galactic-scale Outflow Selection

The shape of oxygen abundance profiles explored with MUSE: evidence for widespread deviations from single gradients

Arm–interarm gas abundance variations explored with MUSE: the role of spiral structure in the chemical enrichment of galaxies

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