Self-Consistent Direct Method for Chemical Abundances in High-z Galaxies with JWST
University of Edinburgh（爱丁堡大学）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文研究所）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学计算研究所）
Karla Z. Arellano-Córdova, J. Eduardo Méndez-Delgado, Sophia R. Flury, César Esteban, Kathryn Kreckel, Jorge García-Rojas, Fergus Cullen, Leticia Carigi, Christ… 展开作者
Karla Z. Arellano-Córdova, J. Eduardo Méndez-Delgado, Sophia R. Flury, César Esteban, Kathryn Kreckel, Jorge García-Rojas, Fergus Cullen, Leticia Carigi, Christophe Morisset, F. Fabián Rosales-Ortega, Antonio Peimbert, Thomas M. Stanton, Dirk Scholte
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13 pages, 6 figures. Accepted for publication in MNRAS
The unprecedented rest-frame UV and optical coverage provided by JWST enables simultaneous constraints on the electron density (n$_{\rm e}$) and temperature (T$_{\rm e}$) of ionized gas in galaxies at z>5. We present a self-consistent direct method based on multiple OIII]1661,66) and [OIII] ($λ$4363, and $λ$5007) transitions to characterize the physical conditions of the high-ionization zone. This new approach is insensitive to a wide range of n$_{\rm e}$ due to the high critical densities of the OIII] and [OIII] transitions. Applying this technique to six galaxies at z=5-9, we find electron densities up to n$_{\rm e}$$\sim 3\times 10^{5}$ cm$^{-3}$ and temperatures of T$_{\rm e}$ $\sim 20,000$ K in systems at $z>6$. Accounting for these self-consistent densities changes the derived T$_{\rm e}$ and modifies the inferred metallicities by up to 0.29 dex relative to previous estimates. We discuss the reported N/O overabundances in the high-$z$ galaxies from our sample, which arise entirely from the high N$^{3+}$/H$^{+}$ values inferred from NIV] lines. We point out that a T$_{\rm e}$-stratification, in which the N$^{3+}$ zone has a slightly higher T$_{\rm e}$ than T$_{\rm e}$([OIII]), could substantially reduce the inferred N/O. Quantitatively, if T$_{\rm e}$(N$^{3+}$) were 10\% higher than T$_{\rm e}$([OIII]), this could induce a systematic overestimation of N$^{3+}$/O$^{2+}$ of nearly 50\%. Classical N/O diagnostics such as N$^{+}$/O$^{+}$, due to their critical densities, can significantly impact the inferred N/O abundance in the presence of high-density gas, whereas N$^{2+}$/O$^{2+}$ place these galaxies closer to $z\sim0$ systems in the N/O-O/H plane. Future JWST programs with larger and more diverse samples will be essential to test the universality and robustness of these results.
Precise C-N-O Abundances of Individual Galaxies in the First Billion Years from Ultra-Deep, Rest-UV-to-Optical JWST Spectroscopy
University College London（伦敦大学学院）；University of Kentucky（肯塔基大学）；University of California, Los Angeles（加州大学洛杉矶分校）；University of Geneva（日内瓦大学）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；CNRS, IRAP（法国国家科学研究中心，天体物理研究研究所）
The BoRG-$JWST$ Survey: Abundance and Mass-to-light Ratio of Luminous $z=7-9$ Galaxies from Independent Sight Lines with NIRSpec
University of California, Los Angeles（加州大学洛杉矶分校）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Geneva（日内瓦大学）；California Institute of Technology（加州理工学院）；National Astronomical Research Institute of Thailand (NARIT)（泰国国家天文研究所）；Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所）；Max Planck Institut für Astronomie（马克斯·普朗克天体物理研究所）；University of Melbourne（墨尔本大学）
The First Empirical Calibration of the MIR Abundance Diagnostic Ne$_{23}$ with JWST
Northwestern University（西北大学）；University of Minnesota（明尼苏达大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；University of Edinburgh（爱丁堡大学）；The Ohio State University（俄亥俄州立大学）；Space Telescope Science Institute（太空望远镜科学研究所）；NASA Headquarters（美国国家航空航天局总部）；INAF—Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切尔蒂天文台）
The ALPINE-CRISTAL-JWST Survey: Chemical Abundance Comparison Between the ISM and CGM of Main-Sequence Galaxies at z=4-6
Caltech/IPAC（加州理工学院/IPAC）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所-博洛尼亚天文与空间科学观测站）；Dipartimento di Fisica “Enrico Fermi”, Universitá di Pisa（比萨大学恩里科·费米物理系）；Scuola Internazionale Superiore Studi Avanzati (SISSA)（国际高等研究院）；Istituto Nazionale di Fisica Nucleare (INFN)-Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Istituto di Radioastronomia dell’Istituto Nazionale di Astrofisica (IRA-INAF)（意大利国家天体物理研究所射电天文研究所）；Department of Physics and Astronomy, University of California, Riverside（加州大学河滨分校物理与天文学系）
The JWST EXCELS survey: The ages and abundances of $3<z<5$ massive quiescent galaxies show that downsizing was already in place by $z\simeq4$
SUPA, Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理联盟）；Department of Astronomy, University of California, Berkeley（加州大学伯克利分校天文系）；Armagh Observatory and Planetarium（阿马赫天文馆和天文台）
A first taste of MEAD (Measuring Extinction and Abundances of Dust) -- I. Diffuse Milky Way interstellar dust extinction features in JWST infrared spectra
'Chemical abundances in H II regions and their implications -- Retrospective on: M. Peimbert & R. Costero, Boletin de los Observatorios de Tonantzintla y Tacubaya, Vol. 5, 3, 1969'
MAGAZ3NE: Spatially Resolved Ages and Chemical Abundances of Ultra-Massive Quiescent Galaxies at z $\sim$ 3.5 using JWST/NIRSpec IFU
York University（约克大学）；University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普勒天文学与天体物理研究所）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of California Davis（加州大学戴维斯分校）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Princeton University（普林斯顿大学）
Abundance gradients along the Galactic disc from chemical evolution models
本文研究了银河系盘的形成和化学演化，重点研究了不同银心距下的丰度模式（[ $α$ /Fe] vs. [Fe/H]）、沿盘的现今丰度梯度和丰度梯度的时间演化。我们考虑了Grisoni等人（2017）为太阳邻域开发的银河系圆盘的化学演化模型，包括两个和一个，我们将我们的分析扩展到其他银河系中心距离。特别是，我们研究的过程，主要影响的丰度梯度的形成：由内而外的情况下，一个变星形成效率，径向气体流量。我们比较我们的模型结果与最近的丰度模式沿银河系盘从APOGEE调查和观测到的造父变星，疏散星团，HII地区和PNe的丰度梯度。我们的结论是，由内而外的情况是一个关键因素，但不能是唯一一个解释丰度模式在不同的银河系中心距离和丰度梯度。为了重现薄圆盘中观察到的特征，还需要进一步的因素，如径向气流和变星形成效率。还显示了丰度梯度随时间的演变，但仍不能得出确切的结论。
Two faces of Gaia-Sausage-Enceladus: Mining the chemical abundance space with graph attention networks
INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Dipartimento di Fisica e Astronomia, Università di Padova（帕多瓦大学物理与天文学系）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；INAF - IASF-Milano（意大利国家天体物理研究所米兰天文物理研究所）；University of Birmingham（伯明翰大学）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
