The newest generation of integral field unit spectrographs brings three-dimensional mapping of nearby galaxies one step closer. While the focus up to this point was mostly on stars and ionised gas, it is also possible to look at dust in a new, more complete way. Using MUSE science verification observations of NGC 5626, we map the interstellar matter in this dusty lenticular. We use the resolving power of MUSE to measure the optical attenuation with a spectral resolution of 6.25 Å, at physical scales of 0.1-1 kpc. The integrated attenuation curve of NGC 5626 shows a smooth, slightly steeper than Milky Way and SMC attenuation curves. Several sharp features are superimposed: we measure lower attenuation at spectral emission lines and higher attenuation for the sodium line doublet. No correlation was observed between sodium line strength and reddening by dust on spatially resolved scales. Additionally, the continuum attenuation was found to be independent from the Balmer decrement (tracing ionised gas attenuation). We model and interpret the variations in the attenuation curves of each spatial resolution element of NGC 5626. We find that the amount and distribution of dust along the line-of-sight is highly degenerate with any variation in the intrinsic extinction law. Our analysis shows that the interstellar matter in NGC 5626 resides in a regular and well-settled disk. Our results preach caution in the application of simple recipes to de-redden global galaxy spectra and underlines the need for more realistic dust geometries when constructing such correction formulas.
Less than the sum of its parts: the dust-corrected H$α$ luminosity of star-forming galaxies explored at different spatial resolutions with MaNGA and MUSE
Tidal pre-conditioning and ram-pressure stripping in NGC 1427A. Deep VLT/MUSE spectroscopy and FUV-to-radio observations trace a Fornax Cluster dwarf in transformation
Pontificia Universidad Católica de Chile（智利天主教 Pontificia 大学）；Centro Espacial Nacional, Fuerza Aérea de Chile（智利空军国家航天中心）；University of Vienna（维也纳大学）；European Southern Observatory（欧洲南方天文台）；University of Minnesota（明尼苏达大学）；Carnegie Observatories（卡内基观测站）；Gemini Observatory（双子座天文台）；Universidad Diego Portales（迭戈·波特莱斯大学）
M^3D: Mosaicking M33 with MUSE datacubes I. Unveiling the diversity of HII regions in M33 with MUSE
Università di Firenze（佛罗伦萨大学）；Center for Astrophysics | Harvard & Smithsonian（哈佛史密森天体物理中心）；National Radio Astronomy Observatory（国家射电天文台）；University of Zagreb（萨格勒布大学）；Ecole Polytechnique Federale de Lausanne（洛桑联邦理工学院）
The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales
Leiden Observatory, Leiden University（莱顿天文台，莱顿大学）；Leibniz-Institut für Astrophysik Potsdam (AIP)（波茨坦阿诺德·爱因斯坦研究所 (AIP)）；European Southern Observatory（欧洲南方天文台）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；Institut für Physik und Astronomie, Universität Potsdam（波茨坦大学物理与天文学研究所）；Department of General Systems Studies, Graduate School of Arts and Sciences, The University of Tokyo（东京大学人文社会系研究科综合系统科学专攻）
The MAGPI Survey: Emission Line Products Data Release and the Role of Spectroscopic Aperture Covering Fraction on the Balmer Decrement-Stellar Mass Relation
Predicting ionised gas emission in 3D with SKIRT. I. Framework and validation
Department of Physics and Astronomy, Proeftuinstraat 86 N3, B-9000 Ghent, Belgium（根特大学物理与天文学系）；Department of Physics, The University of Texas at Dallas, Richardson, Texas 75080, USA（德克萨斯大学达拉斯分校物理系）；Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, Cambridge CB3 0HE, UK（剑桥大学卡文迪许实验室）
A quasar hatching from a buried red phase at z = 3.7
University of Arizona（亚利桑那大学）；University of Michigan（密歇根大学）；University of California, Riverside（加州大学河滨分校）；The University of Tokyo（东京大学）；University of Cambridge（剑桥大学）；Space Telescope Science Institute（太空望远镜科学研究所）；University College London（伦敦大学学院）
研究 z = 3.7 的红类星体“幼体”，通过多波长数据如 JWST 等观测，发现其活动核部分暴露，有宽发射线等特征，核附近有致密气体，多相气体被加速，连续谱呈红色且下降，为探索类星体过渡阶段提供独特机会。
DIGging into HII regions: the role of ionizing photon leakage and spectral hardening in coupling HII regions and diffuse ionized gas
Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理与宇宙学研究所）；Center for Decoding the Universe, Stanford University（斯坦福大学解码宇宙中心）；Racah Institute of Physics, The Hebrew University of Jerusalem（耶路撒冷希伯来大学拉卡物理学研究所）；Universität Heidelberg, Zentrum für Astronomie, Astronomisches Rechen-Institut（海德堡大学天文中心计算天文研究所）；Observatories of the Carnegie Institution for Science（卡内基科学学会天文台）；Department of Astronomy & Astrophysics, University of California, San Diego（加州大学圣地亚哥分校天文学与天体物理学系）；Department of Astronomy and Joint Space-Science Institute, University of Maryland, College Park（马里兰大学学院公园分校天文学系与联合空间科学研究所）；Departamento de Astronomía, Universidad de Chile（智利大学天文学系）；Max-Planck-Instit（马克斯·普朗克研究所）
Low-power jet-ISM coupling and disk-plane perturbations in the edge-on Seyfert galaxy NGC 4388
Università di Firenze（佛罗伦萨大学）；INAF - Arcetri Astrophysical Observatory（意大利国家天体物理研究所-阿切特里天文台）；Scuola Normale Superiore（比萨高等师范学院）；Center for Physical Sciences and Technology（物理与技术研究中心）；Instituto de Alta Investigación, Universidad de Tarapacá（塔拉帕卡大学高级研究所）；Dipartimento di Fisica e Astronomia, Università di Bologna（博洛尼亚大学物理与天文系）；INAF – Istituto di Radioastronomia（意大利国家天体物理研究所无线电天文研究所）；European Southern Observatory（欧洲南方天文台）
