CLASSY V: The Impact of Aperture Effects on the Inferred Nebular Properties of Local Star-forming Galaxies

Arellano-Córdova, K. Z.; Mingozzi, Matilde; Berg, Danielle A.; James, Bethan L.; Rogers, Noah S. J.; Aloisi, Alessandra; Amorín, R.; Brinchmann, Jarle; Charlot, S.; Chisholm, John; Heckman, Timothy M.; Dubón, Stefany Fabian; Hayes, Matthew; Hernández, Svea; Jones, Tucker; Kumari, Nimisha; Leitherer, Claus; Martin, Crystal L.; Nanayakkara, Themiya; Pogge, Richard W.; Senchyna, Peter; Skillman, Evan D.; Stark, Dan; Wofford, Aida; Xu, Xinfeng

doi:10.3847/1538-4357/ac7854

Cited by 14 publications

(9 citation statements)

References 66 publications

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“…Moreover, the methods used by B16 and B21 to determine the oxygen abundance rely on SDSS and LBT/MODS spectra, respectively. However, according to Arellano-Córdova et al (2022), the differences between the long-slit and IFU spectra are within the uncertainties when the high-ionization-zone temperature T e [O III] is measured directly. These facts lead to the negligible deviation between our result and theirs (0.01 dex; Table 6).…”

Section: Sb Metallicitymentioning

confidence: 97%

Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353

Peng 彭,

Martin,

Thibodeaux

et al. 2023

ApJ

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J1044+0353 is considered a local analog of the young galaxies that ionized the intergalactic medium at high redshift due to its low mass, low metallicity, high specific star formation rate, and strong high-ionization emission lines. We use integral field spectroscopy to trace the propagation of the starburst across this small galaxy using Balmer emission- and absorption-line equivalent widths and find a poststarburst population (∼15–20 Myr) roughly 1 kpc east of the much younger, compact starburst (∼3–4 Myr). Using the direct electron temperature method to map the O/H abundance ratio, we find similar metallicities (1–3σ) between the starburst and poststarburst regions but with a significant dispersion of about 0.3 dex within the latter. We also map the Doppler shift and width of the strong emission lines. Over scales several times the size of the galaxy, we discover a velocity gradient parallel to the galaxy’s minor axis. The steepest gradients (∼30 km s−1 kpc−1) appear to emanate from the oldest stellar association. We identify the velocity gradient as an outflow viewed edge on based on the increased line width and skew in a biconical region. We discuss how this outflow and the gas inflow necessary to trigger the starburst affect the chemical evolution of J1044+0353. We conclude that the stellar associations driving the galactic outflow are spatially offset from the youngest association, and a chemical evolution model with a metal-enriched wind requires a more realistic inflow rate than a homogeneous chemical evolution model.

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Section: Sb Metallicitymentioning

confidence: 97%

Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353

Peng 彭,

Martin,

Thibodeaux

et al. 2023

ApJ

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“…Below, we use the PyNeb package (version 1.1.14; Luridiana et al 2015) in Python to calculate the physical conditions and chemical abundances in s04950, s06355, and s10612. We follow the same procedure and atomic data described in Berg et al (2021) and Arellano-Córdova et al (2022). For Ne and C, we have used the atomic data reported in Arellano-Córdova et al (2020) and Berg et al (2019b), respectively.…”

Section: Electron Temperature and Metallicity Determinationsmentioning

confidence: 99%

A First Look at the Abundance Pattern—O/H, C/O, and Ne/O—in z > 7 Galaxies with JWST/NIRSpec

Arellano-Córdova

Berg

Chisholm

et al. 2022

ApJL

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We analyze the rest-frame near-UV and optical nebular spectra of three z > 7 galaxies from the Early Release Observations taken with the Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope (JWST). These three high-z galaxies show the detection of several strong emission nebular lines, including the temperature-sensitive [O iii] λ4363 line, allowing us to directly determine the nebular conditions and abundances for O/H, C/O, and Ne/O. We derive O/H abundances and ionization parameters that are generally consistent with other recent analyses. We analyze the mass–metallicity relationship (i.e., slope) and its redshift evolution by comparing between the three z > 7 galaxies and local star-forming galaxies. We also detect the C iii] λλ1907, 1909 emission in a z > 8 galaxy from which we determine the most distant C/O abundance to date. This valuable detection of log(C/O) = −0.83 ± 0.38 provides the first test of C/O redshift evolution out to high redshift. For neon, we use the high-ionization [Ne iii] λ3869 line to measure the first Ne/O abundances at z > 7, finding no evolution in this α-element ratio. We explore the tentative detection of [Fe ii] and [Fe iii] lines in a z > 8 galaxy, which would indicate a rapid buildup of metals. Importantly, we demonstrate that properly flux-calibrated and higher-S/N spectra are crucial to robustly determine the abundance pattern in z > 7 galaxies with NIRSpec/JWST.

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“…We used these data to retrieve emission-line ratios involving faint auroral lines, if undetected (S/N < 3) in SDSS spectra. Finally, for galaxies J0808+3948, J0944-0038, J1148+2546, J1323-0132, and J1545+0808, Multi-Object Double Spectographs (MODS) data from the Large Binocular Telescope (LBT), presented in Arellano-Córdova et al 2022, are also available (Paper V hereafter). Information on each of the optical data sets is provided in the following paragraphs.…”

Section: Optical Datamentioning

confidence: 99%

CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era*

Mingozzi

James

Arellano-Córdova

et al. 2022

ApJ

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The Cosmic Origins Spectrograph (COS) Legacy Archive Spectroscopic SurveY (CLASSY) provides the first high-resolution spectral catalog of 45 local high-z analogs in the ultraviolet (UV; 1200–2000 Å) to investigate their stellar and gas properties. Here we present a toolkit of UV interstellar medium (ISM) diagnostics, analyzing the main emission lines of CLASSY spectra (N iv] λ λ1483,87, C iv λλ1548,51, He ii λ1640, O iii]λ λ1661,6, Si iii] λλ1883,92, C iii] λ1907,9). Specifically, our aim is to provide accurate diagnostics for the reddening E(B − V), electron density n e , electron temperature T e , metallicity 12+log(O/H), and ionization parameter log(U), taking the different ISM ionization zones into account. We calibrate our UV toolkit using well-known optical diagnostics, analyzing archival optical spectra for all CLASSY targets. We find that UV density diagnostics estimate n e values that are ∼1–2 dex higher (e.g., n e (C iii]λ λ1907,9) ∼ 104 cm−3) than those inferred from their optical counterparts (e.g., n e ([S ii]λ λ6717,31) ∼ 102 cm−3; n e ([Ar iv]λ λ4714,41) ∼ 103 cm−3). T e derived from the hybrid ratio [O iii] λ1666/λ5007 proves to be reliable, implying differences in determining 12+log(O/H) compared to the optical counterpart O iii] λ4363/[O iii] λ5007 within ∼ ±0.3 dex. We also investigate the relation between the stellar and gas E(B − V), finding consistent values at high specific star formation rates (sSFRs; log ( sSFR ) ≳ − 8 yr−1), while at low sSFRs we confirmed an excess of dust attenuation in the gas. Finally, we investigate UV line ratios and equivalent widths to provide correlations with 12+log(O/H) and log(U), but note that there are degeneracies between the two. With this suite of UV-based diagnostics, we illustrate the pivotal role CLASSY plays in understanding the chemical and physical properties of high-z systems that JWST can observe in the rest-frame UV.

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CLASSY V: The Impact of Aperture Effects on the Inferred Nebular Properties of Local Star-forming Galaxies

Cited by 14 publications

References 66 publications

Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353

Using KCWI to Explore the Chemical Inhomogeneities and Evolution of J1044+0353

A First Look at the Abundance Pattern—O/H, C/O, and Ne/O—in z > 7 Galaxies with JWST/NIRSpec

CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era*

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