Azimuthal variations of gas-phase oxygen abundance in NGC 2997

Ho, I-Ting; Meidt, Sharon E.; Kudritzki, Rolf‐Peter; Groves, Brent; Seibert, Mark; Madore, Barry F.; Schinnerer, E.; Kewley, Lisa J.

doi:10.1051/0004-6361/201833262

Cited by 54 publications

(52 citation statements)

References 61 publications

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“…Comparing the abundance distribution of the arm and interarm regions of the galaxies, we find more metal-rich H ii regions in the spiral arms with respect to the interarm area for a large subsample of galaxies (45% using the M13 calibration, 65% for D13). This is in agreement with previous studies on individual galaxies (Sánchez-Menguiano et al 2016a;Vogt et al 2017;Ho et al 2017Ho et al , 2018. Particularly relevant is the compatibility found between the range of values obtained here (up to 0.08 dex) and the one derived by Ho et al (2018) for NGC 2997 following a similar methodology.…”

Section: Discussionsupporting

confidence: 93%

“…This is in agreement with previous studies on individual galaxies (Sánchez-Menguiano et al 2016a;Vogt et al 2017;Ho et al 2017Ho et al , 2018. Particularly relevant is the compatibility found between the range of values obtained here (up to 0.08 dex) and the one derived by Ho et al (2018) for NGC 2997 following a similar methodology. In addition, surprisingly, we observe the opposite trend in a small percentage of the sample, that is, more metal-poor H ii regions in the spiral arms compared to the interarm region.…”

Section: Discussionsupporting

confidence: 93%

“…However, we note that these differences are averaged over the whole arm and interarm areas, whereas in most of previous studies the provided values represent the maxima of the detected variations. Ho et al (2018), following a similar methodology to separate arm and interarm areas, report abundance differences in NGC 2997 of 0.02 dex when the same calibrator is used, totally compatible with the range of values obtained here.…”

Section: Discussionsupporting

confidence: 87%

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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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Section: Discussionsupporting

confidence: 93%

Section: Discussionsupporting

confidence: 93%

Section: Discussionsupporting

confidence: 87%

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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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“…Figure 8 (left) shows a large scatter across this measure, but most galaxies show clustering on ∼300 pc scales of the reduced metallicity regions while enhanced metallicity regions are more widely distributed (n 3 ∼ 400-600 pc; see also Figure 7). This suggests a connection between clustering and mixing, where isolated young regions with a history of star formation have the chance to become enriched (Ho et al 2017(Ho et al , 2018. We further compare the clustering of the outliers in relation to the full HII region population (Figure 8, right), relative to the average, and again find that the HII regions with enhanced metallicities are less clustered.…”

Section: Physical Conditions Of Regions With Enhanced and Reduced Abumentioning

confidence: 82%

Mapping Metallicity Variations across Nearby Galaxy Disks

Kreckel

Blanc

et al. 2019

ApJ

169

196

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The distribution of metals within a galaxy traces the baryon cycle and the buildup of galactic disks, but the detailed gas phase metallicity distribution remains poorly sampled. We have determined the gas phase oxygen abundances for 7,138 HII regions across the disks of eight nearby galaxies using VLT/MUSE optical integral field spectroscopy as part of the PHANGS-MUSE survey. After removing the first order radial gradients present in each galaxy, we look at the statistics of the metallicity offset (∆O/H) and explore azimuthal variations. Across each galaxy, we find low (σ=0.03-0.05 dex) scatter at any given radius, indicative of efficient mixing. We compare physical parameters for those HII regions that are 1σ outliers towards both enhanced and reduced abundances. Regions with enhanced abundances have high ionization parameter, higher Hα luminosity, lower Hα velocity dispersion, younger star clusters and associated molecular gas clouds show higher molecular gas densities. This indicates recent star formation has locally enriched the material. Regions with reduced abundances show increased Hα velocity dispersions, suggestive of mixing introducing more pristine material. We observe subtle azimuthal variations in half of the sample, but can not always cleanly associate this with the spiral pattern. Regions with enhanced and reduced abundances are found distributed throughout the disk, and in half of our galaxies we can identify subsections of spiral arms with clearly associated metallicity gradients. This suggests spiral arms play a role in organizing and mixing the ISM.

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“…Given the strong correlation with spiral pattern, these authors find that the observed abundance variations are due to the mixing and dilution processes driven by the spiral density waves. On the other hand, the TYPHOON program has also reported a much smaller magnitude of 0.06 dex azimuthal variations for the unbarred spiral galaxy NGC 2997 (Ho et al 2018).…”

Section: Azimuthal Variationsmentioning

confidence: 98%

CHAOS IV: Gas-phase Abundance Trends from the First Four CHAOS Galaxies

Berg

Pogge

Skillman

et al. 2020

ApJ

117

140

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The chemical abundances of spiral galaxies, as probed by H II regions across their disks, are key to understanding the evolution of galaxies over a wide range of environments. We present LBT/MODS spectra of 52 H II regions in NGC3184 as part of the CHemical Abundances Of Spirals (CHAOS) project. We explore the direct-method gas-phase abundance trends for the first four CHAOS galaxies, using temperature measurements from one or more auroral line detections in 190 individual H II regions. We find the dispersion in T e − T e relationships is dependent on ionization, as characterized by F λ5007 /F λ3727 , and so recommend ionization-based temperature priorities for abundance calculations. We confirm our previous results that [N II] and [S III] provide the most robust measures of electron temperature in low-ionization zones, while [O III] provides reliable electron temperatures in highionization nebula. We measure relative and absolute abundances for O, N, S, Ar, and Ne. The four CHAOS galaxies marginally conform with a universal O/H gradient, as found by empirical IFU studies when plotted relative to effective radius. However, after adjusting for vertical offsets, we find a tight universal N/O gradient of α N/O = −0.33 dex/R e with σ tot. = 0.08 for R g /R e < 2.0, where N is dominated by secondary production. Despite this tight universal N/O gradient, the scatter in the N/O-O/H relationship is significant. Interestingly, the scatter is similar when N/O is plotted relative to O/H or S/H. The observable ionic states of S probe lower ionization and excitation energies than O, which might be more appropriate for characterizing abundances in metal-rich H II regions. Spectral ReductionsFor a detailed description of the data reduction procedures we refer the reader to (B15). Here, we only note the primary points of our data processing. Spectra were reduced and analyzed using the beta-version of the MODS reduction pipeline 1 which runs within the XIDL 2 reduction package. Given that the bright disks of CHAOS galaxies can complicate local sky subtraction, 1

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Azimuthal variations of gas-phase oxygen abundance in NGC 2997

Cited by 54 publications

References 61 publications

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

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

Mapping Metallicity Variations across Nearby Galaxy Disks

CHAOS IV: Gas-phase Abundance Trends from the First Four CHAOS Galaxies

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