CHAOS. VII. A Large-scale Direct Abundance Study in M33

Rogers, Noah S. J.; Skillman, Evan D.; Pogge, Richard W.; Berg, Danielle A.; Croxall, K. V.; Bartlett, Jordan; Arellano-Córdova, K. Z.; Moustakas, John

doi:10.3847/1538-4357/ac947d

Cited by 14 publications

(15 citation statements)

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“…Within the set of T e -T e between the low-and intermediateionization zones, we observed that the comparisons between T e,[S III] -T e,[O II] and T e,[S III] -T e,[S II] largely agree with those from Zurita et al (2021). However, similarly to recent studies (Berg et al 2015(Berg et al , 2020Zurita et al 2021;Rogers et al 2021Rogers et al , 2022, we observed that the T e -T e trend between T e,[N II] and T e,[S III] exhibits the lowest scatter and agrees with many of the literature trends presented in Figure 9 Judged from the oxygen CEL and RL temperatures, the high-ionization zone is expected to be most affected by temperature fluctuations, due to its proximity to sources of feedback (Méndez-Delgado et al 2023a). To what degree the intermediate-ionization zone temperatures are affected is unclear (Méndez-Delgado et al 2023b).…”

Section: T E[n Ii] and T E[s Iii] As Accurate Tracers Of H II Region ...supporting

confidence: 85%

Investigating the Drivers of Electron Temperature Variations in H ii Regions with Keck-KCWI and VLT-MUSE

Rickards Vaught,

Sandstrom,

Belfiore

et al. 2024

ApJ

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H ii region electron temperatures are a critical ingredient in metallicity determinations, and recent observations have revealed systematic variations in the temperatures measured using different ions. We present electron temperatures (T e ) measured using the optical auroral lines ([N ii]λ5756, [O ii]λ λ7320, 7330, [S ii]λ λ4069, 4076, [O iii]λ4363, and [S iii]λ6312) for a sample of H ii regions in seven nearby galaxies. We use observations from the Physics at High Angular resolution in Nearby Galaxies survey (PHANGS) obtained with integral field spectrographs on Keck (Keck Cosmic Web Imager) and the Very Large Telescope (Multi-Unit Spectroscopic Explorer). We compare the different T e measurements with H ii region and ISM environmental properties such as electron density, ionization parameter, molecular gas velocity dispersion, and stellar association/cluster mass and age obtained from PHANGS. We find that the temperatures from [O ii] and [S ii] are likely overestimated due to the presence of electron density inhomogeneities in H ii regions. We measure high [O iii] temperatures in a subset of regions with high molecular gas velocity dispersion and low ionization parameter, which may be explained by the presence of low-velocity shocks. In agreement with previous studies, the T e–T e between [N ii] and [S iii] temperatures have the lowest observed scatter and follow predictions from photoionization modeling, which suggests that these tracers reflect H ii region temperatures across the various ionization zones better than [O ii], [S ii], and [O iii].

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Section: T E[n Ii] and T E[s Iii] As Accurate Tracers Of H II Region ...supporting

confidence: 85%

Investigating the Drivers of Electron Temperature Variations in H ii Regions with Keck-KCWI and VLT-MUSE

Rickards Vaught,

Sandstrom,

Belfiore

et al. 2024

ApJ

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“…Table 3 reports the physical conditions measured in D40. The direct T e in D40, T e [O III] = 13,200 ± 500 K and T e [S III] = 14,700 ± 1400 K, are plotted in Figure 2 alongside T e measurements in extragalactic H II regions (from Berg et al 2020;Rogers et al 2021Rogers et al , 2022 and low-metallicity dwarf galaxies (Berg et al 2021;Izotov et al 2021;Arellano-Córdova et al 2022b;Thuan et al 2022). The empirical T e -T e scaling relation of Rogers et al (2021) and photoionization model relation of Garnett (1992) (2021).…”

Section: Electron Temperature and Densitymentioning

confidence: 99%

“…This auroral line permits a direct measurement of T e [O III], which primarily traces the gas containing high-ionization ions such as O 2+ and Ne 2+ . However, a lack of T e in other ionization zones can significantly bias direct abundance measurements (Arellano-Córdova & Rodríguez 2020;Rogers et al 2022). Particularly, robust S 2+ and Ar 2+ abundances require a measurement of T e [S III], which has not been made in a galaxy at z > 0.2.…”

Section: Introductionmentioning

confidence: 99%

CECILIA: Direct O, N, S, and Ar Abundances in Q2343-D40, a Galaxy at z ∼ 3

Rogers,

Strom,

Rudie

et al. 2024

ApJL

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Measurements of chemical abundances in high-z star-forming (SF) galaxies place important constraints on the enrichment histories of galaxies and the physical conditions in the early Universe. The James Webb Space Telescope (JWST) is beginning to enable direct chemical abundance measurements in galaxies at z > 2 via the detection of the faint T e -sensitive auroral line [O iii] λ4364. However, abundances of other elements (e.g., S and Ar) in high-z galaxies remain unconstrained owing to a lack of T e data and wavelength coverage. Here we present multiple direct abundances in Q2343-D40, a galaxy at z = 2.9628 ± 0.0001 observed with JWST/NIRSpec as part of the CECILIA program. We report the first simultaneous measurement of T e [O iii] and T e [S iii] in a high-z galaxy, finding good agreement with the temperature trends in local SF systems. We measure a gas-phase metallicity of 12+log(O/H) = 8.07 ± 0.06, and the N/O abundance, log(N/O) = −1.37 ± 0.21, is indicative of primary nucleosynthesis. The S/O and Ar/O relative abundances, log(S/O) = −1.88 ± 0.10 and log(Ar/O) = −2.80 ± 0.12, are both >0.3 dex lower than the solar ratios. However, the relative Ar2+/S2+ abundance is consistent with the solar ratio, suggesting that the relative S-to-Ar abundance does not evolve significantly with redshift. Recent nucleosynthesis models find that significant amounts of S and Ar are produced in Type Ia supernovae, such that the S/O and Ar/O abundances in Q2343-D40 could be the result of predominantly core-collapse supernova enrichment. Future JWST observations of high-z galaxies will uncover whether S/O and Ar/O are sensitive to the timescales of these different enrichment mechanisms.

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“…Before JWST, the majority of α-element abundance measurements were limited to H II regions and star-forming galaxies (SFGs) from the local Universe (e.g., Izotov et al 2006Izotov et al , 2011Guseva et al 2011;Gusev et al 2012;Croxall et al 2016;Berg et al 2018Berg et al , 2019Kumari et al 2019;Díaz & Zamora 2022;Domínguez-Guzmán et al 2022;Rogers et al 2022). In general, many studies report little-to-no variation between αelements with respect to O and metallicity (e.g., Kennicutt et al 2003a;Izotov et al 2006;Berg et al 2021;Rogers et al 2022), with the exception of S/O, which has been seen to decrease significantly as metallicity increases (e.g., S/O versus O/H, Izotov et al 2006;Guseva et al 2011;Amayo et al 2021;Díaz & Zamora 2022).…”

Section: Introductionmentioning

confidence: 99%

CLASSY. IX. The Chemical Evolution of the Ne, S, Cl, and Ar Elements

Arellano-Córdova,

Berg,

Mingozzi

et al. 2024

ApJ

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To study the chemical evolution across cosmic epochs, we investigate Ne, S, Cl, and Ar abundance patterns in the Cosmic Origins Spectrograph Legacy Archive Spectroscopic SurveY (CLASSY). CLASSY comprises local star-forming galaxies (SFGs; 0.02 < z < 0.18) with enhanced star formation rates, making them strong analogues to high-z SFGs. With direct measurements of electron temperature, we derive accurate ionic abundances for all elements and assess ionization correction factors (ICFs) to account for unseen ions and derive total abundances. We find Ne/O, S/O, Cl/O, and Ar/O exhibit constant trends with gas-phase metallicity for 12+log(O/H) < 8.5 but significant correlation for Ne/O and Ar/O with metallicity for 12+log(O/H) > 8.5, likely due to ICFs. Thus, the applicability of the ICFs to integrated spectra of galaxies could bias results, underestimating true abundance ratios. Using CLASSY as a local reference, we assess the evolution of Ne/O, S/O, and Ar/O in galaxies at z > 3, finding no cosmic evolution of Ne/O, while the lack of direct abundance determinations for S/O and Ar/O can bias the interpretation of the evolution of these elements. We determine the fundamental metallicity relationship (FMR) for CLASSY and compare to the high-redshift FMR, finding no evolution. Finally, we perform the first mass–neon relationship analysis across cosmic epochs, finding a slight evolution to high Ne at later epochs. The robust abundance patterns of CLASSY galaxies and their broad range of physical properties provide essential benchmarks for interpreting the chemical enrichment of the early galaxies observed with the JWST.

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CHAOS. VII. A Large-scale Direct Abundance Study in M33

Cited by 14 publications

References 100 publications

Investigating the Drivers of Electron Temperature Variations in H ii Regions with Keck-KCWI and VLT-MUSE

Investigating the Drivers of Electron Temperature Variations in H ii Regions with Keck-KCWI and VLT-MUSE

CECILIA: Direct O, N, S, and Ar Abundances in Q2343-D40, a Galaxy at z ∼ 3

CLASSY. IX. The Chemical Evolution of the Ne, S, Cl, and Ar Elements

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