Carbon, nitrogen and oxygen abundance gradients in M101 and M31

Esteban, C.; Bresolin, Fabio; García‐Rojas, J.; Cipriano, L. Toribio San

doi:10.1093/mnras/stz3134

Cited by 45 publications

(61 citation statements)

References 75 publications

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“…An alternative way to stellar spectroscopy is to measure the chemical composition of H II regions and planetary nebulae from their optical and ultraviolet emission-line spectra, both collisional excited lines, for oxygen and nitrogen, and recombination lines, for carbon and oxygen (e.g., Deharveng et al, 2000;Esteban et al, 2017, Esteban et al, 2019Stanghellini and Haywood, 2018;Arellano-Córdova et al, 2020;Esteban et al, 2020;Stanghellini et al, 2020). Abundances of H II regions and planetary nebulae are excellent probes of the radial abundance gradient of the Milky Way (e.g., Esteban et al, 2017Arellano-Córdova et al, 2020;Stanghellini et al, 2020).…”

Section: The Galactic Evolution Of Cnomentioning

confidence: 99%

Light Elements in the Universe

Randich

Magrini

2021

Front. Astron. Space Sci.

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Due to their production sites, as well as to how they are processed and destroyed in stars, the light elements are excellent tools to investigate a number of crucial issues in modern astrophysics: from stellar structure and non-standard processes at work in stellar interiors to age dating of stars; from pre-main sequence evolution to the star formation histories of young clusters and associations and to multiple populations in globular clusters; from Big Bang nucleosynthesis to the formation and chemical enrichment history of the Milky Way Galaxy and its populations, just to cite some relevant examples. In this paper, we focus on lithium, beryllium, and boron (LiBeB) and on carbon, nitrogen, and oxygen (CNO). LiBeB are rare elements, with negligible abundances with respect to hydrogen; on the contrary, CNO are among the most abundant elements in the Universe, after H and He. Pioneering observations of light-element surface abundances in stars started almost 70 years ago and huge progress has been achieved since then. Indeed, for different reasons, precise measurements of LiBeB and CNO are difficult, even in our Sun; however, the advent of state-of-the-art ground- and space-based instrumentation has allowed the determination of high-quality abundances in stars of different type, belonging to different Galactic populations, from metal-poor halo stars to young stars in the solar vicinity and from massive stars to cool dwarfs and giants. Noticeably, the recent large spectroscopic surveys performed with multifiber spectrographs have yielded detailed and homogeneous information on the abundances of Li and CNO for statistically significant samples of stars; this has allowed us to obtain new results and insights and, at the same time, raise new questions and challenges. A complete understanding of the light-element patterns and evolution in the Universe has not been still achieved. Perspectives for further progress will open up soon thanks to the new generation instrumentation that is under development and will come online in the coming years.

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Section: The Galactic Evolution Of Cnomentioning

confidence: 99%

Light Elements in the Universe

Randich

Magrini

2021

Front. Astron. Space Sci.

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“…O, N, S) for thousands of local Hii regions and star forming galaxies (e.g. Smith 1975;Peimbert et al 1978;Torres-Peimbert et al 1989;Garnett et al 1997;van Zee et al 1998;Kennicutt et al 2003;Bresolin et al 2004;Hägele et al 2006Hägele et al , 2011Hägele et al , 2012Zurita & Bresolin 2012;Croxall et al 2016;Lin et al 2017;Fernández et al 2018;Esteban et al 2020;Berg et al 2020, among others) and for some objects at high redshifts (z > 1; e.g. Sanders et al 2016Sanders et al , 2020Gburek et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Chemical abundances of Seyfert 2 AGNs – III. Reducing the oxygen abundance discrepancy

Dors

Maiolino

Cardaci

et al. 2020

Monthly Notices of the Royal Astronomical Society

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ABSTRACT We investigate the discrepancy between oxygen abundance estimations for narrow-line regions of active galactic nuclei (AGNs) type Seyfert 2 derived using direct estimations of the electron temperature (Te-method) and those derived using photoionization models. In view of this, observational emission-line ratios in the optical range ($3000 \: \lt \: \lambda (\mathring{\rm A}) \: \lt 7000$) of Seyfert 2 nuclei compiled from the literature were reproduced by detailed photoionization models built with the cloudy code. We find that the derived discrepancies are mainly due to the inappropriate use of the relations between temperatures of the low (t2) and high (t3) ionization gas zones derived for H ii regions in AGN chemical abundance studies. Using a photoionization model grid, we derived a new expression for t2 as a function of t3 valid for Seyfert 2 nuclei. The use of this new expression in the AGN estimation of the O/H abundances based on Te-method produces O/H abundances slightly lower (about 0.2 dex) than those derived from detailed photoionization models. We also find that the new formalism for the Te-method reduces by about 0.4 dex the O/H discrepancies between the abundances obtained from strong emission-line calibrations and those derived from direct estimations.

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“…Table 2 also provides the regions which contain C II λ4267 Å detections. This recombination line allows for the determination of C ++ abundances (for example, Esteban et al 2009Esteban et al , 2020Skillman et al 2020), but we reserve a study of the recombination line abundances in multiple galaxies for a future study.…”

Section: Data Acquisitionmentioning

confidence: 99%

“…The error in their inferred T e [O II] values is assumed to be 300 K, citing the magnitude of the uncertainties in Kennicutt et al (2003a) as justification for this choice. Finally, Esteban et al (2020) used the empirical, linear T e -T e relations from Esteban et al (2009) when necessary, and standard propagation of errors is applied, without a lower limit, to obtain the uncertainties on the inferred temperatures.…”

Section: Application Of Chaos T E -T E Relationsmentioning

confidence: 99%

CHAOS VI: Direct Abundances in NGC 2403

Rogers,

Skillman,

Pogge

et al. 2021

Preprint

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We report the direct abundances for the galaxy NGC 2403 as observed by the CHemical Abundances Of Spirals (CHAOS) project. Using the Multi-Object Double Spectrograph on the Large Binocular Telescope, we observe two fields with Hii regions that cover an R g /R e range of 0.18 to 2.31. 32 Hii regions contain at least one auroral line detection, and we detect a total of 122 temperature-sensitive auroral lines. Here, for the first time, we use the intrinsic scatter in the T e -T e diagrams, added in quadrature to the uncertainty on the measured temperature, to determine the uncertainty on an electron temperature inferred for one ionization zone from a measurement in a different ionization zone. We then use all available temperature data within an Hii region to obtain a weighted average temperature within each ionization zone. We re-derive the oxygen abundances of all CHAOS galaxies using this new temperature prioritization method, and we find that the gradients are consistent with the results of Berg et al. (2020). For NGC 2403, we measure a direct oxygen abundance gradient of −0.09(±0.03) dex/R e , with an intrinsic dispersion of 0.037(±0.017) dex, and an N/O abundance gradient of −0.17(±0.03) dex/R e with an intrinsic dispersion of 0.060(±0.018) dex. For direct comparison, we use the line intensities from the study of NGC 2403 by Berg et al. (2013), and find their recomputed values for the O/H and N/O gradients are consistent with ours.

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Carbon, nitrogen and oxygen abundance gradients in M101 and M31

Cited by 45 publications

References 75 publications

Light Elements in the Universe

Light Elements in the Universe

Chemical abundances of Seyfert 2 AGNs – III. Reducing the oxygen abundance discrepancy

CHAOS VI: Direct Abundances in NGC 2403

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