We present emission line templates for passively evolving ("retired") galaxies, useful for investigation of the evolution of the ISM in these galaxies, and characterization of their high-temperature source populations. The templates are based on high signal-to-noise ($>800$) co-added spectra ($3700-6800$Å) of $\sim11500$ gas-rich Sloan Digital Sky Survey galaxies devoid of star-formation and active galactic nuclei. Stacked spectra are provided for the entire sample and sub-samples binned by mean stellar age. In Johansson~et al (2014), these spectra provided the first measurements of the He II 4686Å line in passively-evolving galaxies, and the observed He II/H$β$ ratio constrained the contribution of accreting white dwarfs (the "single-degenerate" scenario) to the type Ia supernova rate. In this paper, the full range of unambiguously detected emission lines are presented. Comparison of the observed [O I] 6300Å/H$α$ ratio with photoionization models further constrains any high-temperature single-degenerate scenario for type Ia supernovae (with 1.5 $\lesssim$ T/$10^{5}K$ $\lesssim$ 10) to $\lesssim$3-6\% of the observed rate in the youngest age bin (i.e. highest SN Ia rate). Hence, for the same temperatures, in the presence of an ambient population of post-AGB stars, we exclude additional high-temperature sources with a combined ionizing luminosity of $\approx 1.35\times 10^{30} L_{\odot}/M_{\odot,*}$ for stellar populations with mean ages of 1 - 4 Gyrs. Furthermore, we investigate the extinction affecting both the stellar and nebular continuum. The latter shows about five times higher values. This contradicts isotropically distributed dust and gas that renders similar extinction values for both cases.
Analysis of spatially resolved stellar populations and emission line properties in nearby galaxies with J-PLUS data. II-Results for the M51 group and first comparison with the M101 group
Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）；Universidade Federal de Santa Catarina（圣卡塔琳娜联邦大学）
X-ray stellar feedback in low-metallicity starbursts: Insights from the template starburst galaxy ESO 338-IG04 and its halo
Institute for Physics and Astronomy, University of Potsdam（波茨坦大学物理与天文学研究所）；Department of Physics, University of Arkansas（阿肯色大学物理系）；Arkansas Center for Space and Planetary Sciences, University of Arkansas（阿肯色大学阿肯色空间与行星科学中心）；Department of Astronomy, The Oskar Klein Centre, Stockholm University（斯德哥尔摩大学奥斯卡·克莱因中心天文学系）；Centro de Astrobiología (CAB), INTA–CSIC（西班牙国家航空航天技术研究所-西班牙国家科学研究委员会天体生物学中心）；Department of Astronomy, U. Wisconsin-Madison（威斯康星大学麦迪逊分校天文学系）；ESA, ESAC（欧洲空间局欧洲空间应用与技术中心）
通过研究低金属licity恒星burst星系ESO 338-IG04，发现X射线源对电离光子预算的影响，并预测He II λ4686发射的亮度。
Empirical Near-Infrared Spectral Templates from SPHEREx: Disentangling AGN and Host-Galaxy Emission
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Science and Technology of China（中国科学技术大学）；Guizhou University（贵州大学）
CLUES III: Do User Choices Impact The Results of SED Fitting? Tests of 'Off-The-Shelf' Stellar Population and Dust Extinction Models in the CLUES Sample
JWST reveals a highly ionized nebula powered by an ultraluminous X-ray source with a massive black hole in the metal-poor galaxy Holmberg II
Space Telescope Science Institute（太空望远镜科学研究所）；AURA for ESA, Space Telescope Science Institute（欧洲航天局天文研究联盟，太空望远镜科学研究所）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；Sterrenkundig Observatorium, Universiteit Gent（根特大学天文台）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所（地球物理与化学研究所，西班牙国家研究委员会））；Centro de Astrobiología – Departamento de Astrofísica (CSIC-INTA)（天体生物学中心 - 天体物理学系（西班牙国家研究委员会-国家航空航天技术研究所））
本研究通过JWST光谱观测，首次在ULX Ho II X-1周围探测到[Ne V]和[Ne VI]，直接证实该ULX关联低金属丰度星系中的高度电离星云，其电离由吸积黑洞驱动，电离条件呈各向异性。
