Can intrinsic alignments of elongated low-mass galaxies be used to map the cosmic web at high redshift?
Viraj Pandya, Joel Primack, Peter Behroozi, Avishai Dekel, Haowen Zhang, Elliot Eckholm, Sandra M. Faber, Henry C. Ferguson, Mauro Giavalisco, Yicheng Guo, Nimi… 展开作者
Viraj Pandya, Joel Primack, Peter Behroozi, Avishai Dekel, Haowen Zhang, Elliot Eckholm, Sandra M. Faber, Henry C. Ferguson, Mauro Giavalisco, Yicheng Guo, Nimish Hathi, Dritan Kodra, Anton M. Koekemoer, David C. Koo, Jeffrey Newman, Arjen van der Wel
Hubble Space Telescope observations show that low-mass ($M_*=10^9-10^{10}M_{\odot}$) galaxies at high redshift ($z=1.0-2.5$) tend to be elongated (prolate) rather than disky (oblate) or spheroidal. This is explained in zoom-in cosmological hydrodynamical simulations by the fact that these galaxies are forming in cosmic web filaments where accretion happens preferentially along the direction of elongation. We ask whether the elongated morphology of these galaxies allows them to be used as effective tracers of cosmic web filaments at high redshift via their intrinsic alignments. Using mock lightcones and spectroscopically-confirmed galaxy pairs from the CANDELS survey, we test two types of alignments: (1) between the galaxy major axis and the direction to nearby galaxies of any mass, and (2) between the major axes of nearby pairs of low-mass, likely prolate, galaxies. The mock lightcones predict strong signals in 3D real space, 3D redshift space, and 2D projected redshift space for both types of alignments (assuming prolate galaxy orientations are the same as those of their host prolate halos), but we do not detect significant alignment signals in CANDELS observations. However, we show that spectroscopic redshifts have been obtained for only a small fraction of highly elongated galaxies, and accounting for spectroscopic incompleteness and redshift errors significantly degrades the 2D mock signal. This may partly explain the alignment discrepancy and highlights one of several avenues for future work.
Impact of Cosmic Filaments on Galaxy Morphological Evolution and Predictions of Early Cosmic Web Structure for Roman
Space Telescope Science Institute（太空望远镜科学研究所）；New Mexico State University（新墨西哥州立大学）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；Canadian Institute for Theoretical Astrophysics, University of Toronto（多伦多大学加拿大理论天体物理研究所）；Columbia Astrophysics Laboratory, Columbia University（哥伦比亚大学哥伦比亚天体物理学实验室）；Johns Hopkins University（约翰斯·霍普金斯大学）
Spin-filament alignments to unravel galaxy evolution and model intrinsic alignments
The University of Sydney（悉尼大学）；Sorbonne Université（索邦大学）；CNRS（法国国家科学研究中心）；Univ Lyon1（里昂第一大学）；Ens de Lyon（巴黎高等师范学院里昂分校）；INAF-Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；EPFL（洛桑联邦理工学院）；University of Vienna（维也纳大学）；Australian National University（澳大利亚国立大学）；Swinburne University of Technology（斯威本科技大学）；Aix Marseille Univ（艾克斯-马赛大学）
Properties of Barred Galaxies with the Environment: II. The case of the Cosmic Web around the Virgo cluster
Universidad de La Serena（拉塞雷纳大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad de La Laguna（拉古纳大学）；Universidad de Atacama（阿塔卡马大学）；Universidad Técnica Federico Santa Maria（费德里科·圣玛丽亚理工大学）；Centro de Estudios de Física del Cosmos de Aragón (CEFCA)（阿拉贡宇宙物理研究中心）；CSIC（西班牙国家科学研究委员会）
The invariance of group occupation across the cosmic web
Universidad Técnica Federico Santa María（技术费德里科·圣玛丽亚大学）；CONICET. Instituto de Astronomía Teórica y Experimental (IATE)（阿根廷国家科学研究委员会理论及实验天文学研究所）；Universidad Nacional de Córdoba (UNC). Observatorio Astronómico de Córdoba (OAC)（科尔多瓦国立大学科尔多瓦天文台）
Where Galaxies Point: First Measurement of the Large-Scale Axial Intrinsic Alignment
Zhejiang University（浙江大学）；Centro Brasileiro de Pesquisas Físicas（巴西物理研究中心）；Universidade Federal do Rio de Janeiro（里约热内卢联邦大学）；Observatório Nacional（国家天文台）；Universidade Federal do Rio Grande（里奥格兰德联邦大学）；Universidade Federal de Ouro Preto（欧罗普雷图联邦大学）；INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）
A Mysteriously Tight H$α$-[O III] Correlation and Non-Case B Balmer Decrements Revealed by the Spectra from the James Webb Space Telescope NIRSpec Instrument
A 15 Mpc rotating galaxy filament at redshift z = 0.032
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理学）；Department of Physics and Astronomy, University of the Western Cape（西开普敦大学物理与天文学系）；Department of Physics and Electronics, Rhodes University（罗德岛大学物理与电子学系）；South African Radio Astronomy Observatory（南非射电天文台）；Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire（赫特福德大学物理、天文学与数学学院天体物理研究中心）；School of Physics, H.H. Wills Physics Laboratory, Tyndall Avenue, University of Bristol（布里斯托大学H.H.威尔斯物理实验室）；Institute for Astronomy, University of Edinburgh, Royal Observatory, Edinburgh（爱丁堡大学皇家天文台天文学研究所）；The Inter-University Institute for Data Intensive Astronomy (IDIA), Department of Astronomy, University of Cape Town（开普敦大学天文学系数据密集型天文学跨大学研究所）
发现红移 z = 0.032 处 15 Mpc 的旋转星系丝状结构，揭示星系角动量与宇宙网结构的关系及早期演化特征。
Zippers and Twisters: Planes of Satellite Galaxies Emerge from Whirling and Shocking Gas Streams in the Cosmic Web
Johns Hopkins University（约翰斯·霍普金斯大学）；NYC College of Technology, City University of New York（纽约市立大学学院技术学院）；Graduate Center, City University of New York（纽约市立大学研究生中心）；Institut d’Astrophsyique de Paris, UMR 7095, CNRS, UPMC Univ.（巴黎天体物理研究所）；Kyung Hee University（庆熙大学）；LSST-DA Catalyst Fellowship, LSST Discovery Alliance（LSST-DA催化剂奖学金，LSST发现联盟）；Centre for Astrophysics Research, University of Hertfordshire（赫特福德大学天体物理学研究中心）
Star-forming galaxies in the cosmic web in the last 11 Gyr
Observatoire Astronomique de Strasbourg, UMR 7550, CNRS, Université de Strasbourg（斯特拉斯堡天文台）；Institute for Astronomy, University of Edinburgh（爱丁堡大学天体物理研究所）；Department of Physics and Astronomy, University of the Western Cape（西开普大学物理与天文学系）
pop-cosmos: Galaxy size evolution across structural and star-formation classifications in COSMOS-Web
Institute of Astronomy, University of Cambridge（剑桥大学天体物理学研究所）；Cavendish Laboratory, Department of Physics, University of Cambridge（剑桥大学物理学院卡文迪许实验室）；The Oskar Klein Centre, Department of Physics, Stockholm University（斯德哥尔摩大学物理学院奥斯卡·克莱因中心）；Astrophysics Group, Imperial College London（伦敦帝国理工学院天体物理学组）；Department of Mathematics, Imperial College London（伦敦帝国理工学院数学系）；Research Computing Services, University of Cambridge（剑桥大学研究计算服务）
