The SDSS-V Local Volume Mapper (LVM): Scientific Motivation and Project Overview
Niv Drory, Guillermo A. Blanc, Kathryn Kreckel, Sebastian F. Sanchez, Alfredo Mejia-Narvaez, Evelyn J. Johnston, Amy M. Jones, Eric W. Pellegrini, Nicholas P. K… 展开作者
Niv Drory, Guillermo A. Blanc, Kathryn Kreckel, Sebastian F. Sanchez, Alfredo Mejia-Narvaez, Evelyn J. Johnston, Amy M. Jones, Eric W. Pellegrini, Nicholas P. Konidaris, Tom Herbst, Jose Sanchez-Gallego, Juna A. Kollmeier, Florence de Almeida, Jorge K. Barrera-Ballesteros, Dmitry Bizyaev, Joel R. Brownstein, Mar Canal i Saguer, Brian Cherinka, Maria-Rosa L. Cioni, Enrico Congiu, Maren Cosens, Bruno Dias, John Donor, Oleg Egorov, Evgeniia Egorova, Cynthia S. Froning, Pablo Garcia, Simon C. O. Glover, Hannah Greve, Maximilian Haeberle, Kevin Hoy, Hector Ibarra, Jing Li, Ralf S. Klessen, Dhanesh Krishnarao, Nimisha Kumari, Knox S. Long, Jose Eduardo Mendez-Delgado, Silvia Anastasia Popa, Solange Ramirez, Hans-Walter Rix, Aurora Mata Sanchez, Ravi Sankrit, Natascha Sattler, Conor Sayres, Amrita Singh, Guy Stringfellow, Stefanie Wachter, Elizabeth Jayne Watkins, Tony Wong, Aida Wofford
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29 pages, 12 figures, accepted for publication in The Astronomical Journal
We present the Sloan Digital Sky Survey V (SDSS-V) Local Volume Mapper (LVM). The LVM is an integral-field spectroscopic survey of the Milky Way, Magellanic Clouds, and of a sample of local volume galaxies, connecting resolved pc-scale individual sources of feedback to kpc-scale ionized interstellar medium (ISM) properties. The 4-year survey covers the southern Milky Way disk at spatial resolutions of 0.05 to 1 pc, the Magellanic Clouds at 10 pc resolution, and nearby large galaxies at larger scales totaling $>4300$ square degrees of sky, and more than 55M spectra. It utilizes a new facility of alt-alt mounted siderostats feeding 16 cm refractive telescopes, lenslet-coupled fiber-optics, and spectrographs covering 3600-9800A at R ~ 4000. The ultra-wide field IFU has a diameter of 0.5 degrees with 1801 hexagonally packed fibers of 35.3 arcsec apertures. The siderostats allow for a completely stationary fiber system, avoiding instability of the line spread function seen in traditional fiber feeds. Scientifically, LVM resolves the regions where energy, momentum, and chemical elements are injected into the ISM at the scale of gas clouds, while simultaneously charting where energy is being dissipated (via cooling, shocks, turbulence, bulk flows, etc.) to global scales. This combined local and global view enables us to constrain physical processes regulating how stellar feedback operates and couples to galactic kinematics and disk-scale structures, such as the bar and spiral arms, as well as gas in- and out-flows.
SDSS-V Local Volume Mapper (LVM): The Integrated Light and Internal Rotation of Omega Centauri
European Southern Observatory（欧洲南方天文台）；Apache Point Observatory（阿帕奇点天文台）；Department of Astrophysics, University of Vienna（维也纳大学天体物理系）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学中心天文计算研究所）；Instituto de Astrofísica, Departamento de Física y Astronomía, Facultad de Ciencias Exactas, Universidad Andres Bello（安德斯·贝略大学精确科学学院物理学与天文学系天体物理研究所）；Centro de investigación en Astronomía, Facultad de Ingeniería, Ciencia y Tecnología, Universidad Bernardo O’Higgins（贝尔纳多·奥希金斯大学工程、科学与技术学院天文学研究中心）；Instituto de Astronomía, Universidad Ca（卡塔大学天体物理研究所）
SDSS-V Local Volume Mapper (LVM): Dithered Data Cube Reconstruction with 3dcubegen
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）；Universidad Andrés Bello（安德烈斯贝略大学）；Institute of Astrophysics, Facultad de Ciencias Exactas, Universidad Andrés Bello（安德烈斯贝略大学精确科学学院天体物理研究所）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Cátedras CONAHCYT. Universidad Nacional Autónoma de México, Instituto de Astronomía（墨西哥国家科学技术委员会讲席教授项目，墨西哥国立自治大学天文研究所）；Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学中心天文计算研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；New York University Abu Dhabi（纽约大学阿布扎比分校）；Universidad Diego Portales（迭戈波塔莱斯大学）；Universidad de Chile（智利大学）；Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学射电天文学与天体物理研究所）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Departamento de Astronomía, Universidad de Chile（智利大学天文学系）；Department of Astronomy, University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校天文学系）
SDSS-V LVM: Detectability of Wolf-Rayet stars and their He II ionizing flux in low-metallicity environments I. The weak-lined, early-type WN3 stars in the SMC
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut（海德堡大学天文中心，天文计算研究所）；Department of Physics and Astronomy, University of Utah（犹他大学物理与天文学系）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理学系）；The Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Space Telescope Science Institute（太空望远镜科学研究所）；McDonald Observatory, The University of Texas at Austin（德克萨斯大学奥斯汀分校麦克唐纳天文台）；Univ. Diego Portales, Inst. de Estudios Astrofísicos（迭戈帕托莱斯大学，天体物理研究所）
SDSS-V LVM: Revealing the Physical and Chemical Structure of the Helix Nebula
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学射电天文与天体物理研究所）；Universidad Nacional Autónoma de México. Instituto de Astronomía（墨西哥国立自治大学天文研究所）；Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México（墨西哥国立自治大学物理科学研究所）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Institute of Astrophysics, Facultad de Ciencias（科学学院天体物理研究所）
SDSS-V LVM: Resolving Physical Conditions in the Trifid Nebula
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学计算研究所）；Instituto de Astronomía, Universidad Nacional Autónoma de México（墨西哥国立自治大学天文学研究所）；Instituto de Ciencias Físicas, Universidad Nacional Autónoma de México（墨西哥国立自治大学物理科学研究所）；New York University Abu Dhabi（纽约大学阿布扎比分校）；Center for Astrophysics and Space Science, NYU Abu Dhabi（纽约大学阿布扎比分校天体物理学与空间科学中心）
Unified Spectrospatial Forward Models: Spatially Continuous Maps of Weak Emission Lines in the Rosette Nebula with SDSS-V LVM
Monash University（莫纳什大学）；Flatiron Institute（平托研究所）；University of Washington（华盛顿大学）；Princeton University（普林斯顿大学）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；New Mexico State University（新墨西哥州立大学）；University of Toronto（多伦多大学）；Canadian Institute for Advanced Research（加拿大高级研究院）
SDSS-V LVM: A spatially resolved study of the physical conditions and the chemical abundance discrepancy in the Lagoon Nebula (M 8)
Universidad de Chile（智利大学）；Carnegie Institution for Science（卡内基科学研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Universidad Nacional Autónoma de México（墨西哥国立自治大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；European Southern Observatory（欧洲南方天文台）；Universität Heidelberg（海德堡大学）
SDSS-V LVM: Verifying what, and where, the 'Galactic Center' Lobe is
Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg（海德堡大学天文学计算研究所）；McDonald Observatory, The University of Texas at Austin（德克萨斯大学奥斯汀分校麦克唐纳天文台）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Departamento de Astronomía, Universidad de Chile（智利大学天文学系）；Universidad Nacional Autónoma de México, Instituto de Astronomía（墨西哥国立自治大学天文学研究所）；Apache Point Observatory and New Mexico State University（新墨西哥州立大学阿帕奇点天文台）；Sternberg Astronomical Institute, Moscow State University（莫斯科国立大学斯登伯格天文研究所）；Department of Physics and Astronomy, University of Utah（犹他大学物理与天文学系）；Universidad Católica del Norte（北天主教学会大学）
The SDSS-V Black Hole Mapper Reverberation Mapping Project: Multi-Line Dynamical Modeling of a Highly Variable Active Galactic Nucleus with Decade-long Light Curves
The SDSS-V Black Hole Mapper Reverberation Mapping Project: Light Echoes of the Coronal Line Region in a Luminous Quasar
University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；National Center for Supercomputing Applications（国家超级计算应用中心）；University of Washington（华盛顿大学）；The Pennsylvania State University（宾夕法尼亚州立大学）；York University（约克大学）；University of St. Andrews（圣安德鲁斯大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；University of Connecticut（康涅狄格大学）；Space Telescope Science Institute（空间望远镜科学研究所）；Tel Aviv University（特拉维夫大学）
The Twentieth Data Release of the Sloan Digital Sky Survey: First All-Sky BOSS Spectra, eROSITA-SDSS-V Mapper Coordinated Observations, and a Preview of the Local Volume Mapper
Sloan Digital Sky Survey（斯隆数字巡天）；Department of Astronomy, University of Virginia（弗吉尼亚大学天文学系）；Department of Physics and Astronomy, California State University, San Bernardino（加州州立大学圣贝纳迪诺分校物理与天文学系）；Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh（爱丁堡大学皇家天文台天体物理学研究所）；Universidad Nacional Autónoma de México. Instituto de Astronomía（墨西哥国立自治大学天文学研究所）；Department of Astronomy and Astrophysics, University of Chicago（芝加哥大学天文学与天体物理学系）；Department of Astronomy, University of Washington（华盛顿大学天文学系）；Department of Astronomy & Institute for Astrophysical Research, Boston University（波士顿大学天文学系及天体物理研究所）；Las Campanas Observatory（拉斯坎帕纳斯天文台）
Payne4GAIN: NLTE Corrections for Red Giants in Milky Way Mapper using H-Band Neural Network Emulators
University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Joint Institute for Nuclear Astrophysics（联合核天体物理研究所）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Heidelberg University（海德堡大学）；University of Florida（佛罗里达大学）；The Ohio State University（俄亥俄州立大学）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理中心）；Monash University（蒙纳士大学）；University of Colorado（科罗拉多大学）；Universidad Bernardo O’Higgins（贝尔纳多·奥希金斯大学）
The Nineteenth Data Release of the Sloan Digital Sky Survey
Sloan Digital Sky Survey（斯隆数字巡天）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Virginia（弗吉尼亚大学）；University of Edinburgh（爱丁堡大学）；Universidad de Chile（智利大学）；Universitat de Barcelona (UB)（巴塞罗那大学）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究所）；University of Washington（华盛顿大学）
The Open Cluster Chemical Abundances and Mapping Survey XI. First Gradients from SDSS/MWM BOSS Determined Clusters
Texas Christian University（德克萨斯基督教大学）；Vanderbilt University（范德堡大学）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of Arizona（亚利桑那大学）；Observatório Nacional/MCTIC（国家天文台/科技情报部）；University of Utah（犹他大学）
The eROSITA Final Equatorial Depth Survey (eFEDS): SDSS spectroscopic observations of X-ray sources
Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Excellence Cluster ORIGINS（ORIGINS卓越集群）；Max Planck Institut für Astronomie（马克斯·普朗克天体物理研究所）；Dipartimento di Fisica e Astronomia, Università di Bologna（博洛尼亚大学物理与天文系）；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）；Department of Astronomy, University of Science and Technology of China（中国科学技术大学天文学系）；Department of Astronomy, University of Washington（华盛顿大学天文学系）；Instituto de Alta Investigación, Universidad de Tarapacá（塔拉帕卡大学高等研究院）
