The MAGPI Survey: the subtle role of environment and not-so-subtle impact of generations of stars on galaxy dynamics
Caroline Foster, Sabine Bellstedt, Francesco DEugenio, Adriano Poci, Ryan Bagge, Katherine Harborne, Thomas Venville, J. Trevor Mendel, Claudia Del P. Lagos, Em… 展开作者
Caroline Foster, Sabine Bellstedt, Francesco DEugenio, Adriano Poci, Ryan Bagge, Katherine Harborne, Thomas Venville, J. Trevor Mendel, Claudia Del P. Lagos, Emily Wisnioski, Tania M. Barone, Andrew J. Battisti, Stefania Barsanti, Sarah Brough, Scott M. Croom, Caro Derkenne, Lucas C. Kimmig, Anilkumar Mailvaganam, Rhea-Silvia Remus, Gauri Sharma, Sarah M. Sweet, Sabine Thater, Lucas M. Valenzuela, Jesse van de Sande, Sam P. Vaughan, Bodo Ziegler
备注：
17 pages, 13 figures, 3 tables, accepted for publication in PASA
星系的恒星年龄与质量被认为是星系动力学状态的主要决定因素，而环境似乎不起作用或仅起非常微小的作用。我们利用MAGPI巡天中处于中等红移（z~0.3）的77个星系样本，研究环境对星系动力学的微妙影响。我们结合统计技术（简单相关、偏相关和主成分分析）来分离环境对星系动力学的贡献，同时明确考虑了恒星年龄、恒星形成历史和恒星质量等已知因素。我们考虑的动力学参数包括：视线速度分布的高阶运动学（由Gauss-Hermite系数$h_3$和$h_4$参数化）、使用kinemetry导出的运动学不对称性$V_{\ m asym}$以及观测自旋参数代理$λ_{R_e}$。其中，平均$h_4$是唯一被发现与以群动力学质量参数化的环境存在显著相关的参数。即使在考虑了年龄和恒星质量趋势之后，这种相关性依然存在。最后，我们证实自旋参数$λ_{R_e}$的变化与年龄呈最强（反）相关，这与局部研究的结果一致，并表明这种依赖关系在z~0.3时已确立。
英文摘要：
The stellar age and mass of galaxies have been suggested as the primary determinants for the dynamical state of galaxies, with environment seemingly playing no or only a very minor role. We use a sample of 77 galaxies at intermediate redshift (z~0.3) in the Middle-Ages Galaxies Properties with Integral field spectroscopy (MAGPI) Survey to study the subtle impact of environment on galaxy dynamics. We use a combination of statistical techniques (simple and partial correlations and principal component analysis) to isolate the contribution of environment on galaxy dynamics, while explicitly accounting for known factors such as stellar age, star formation histories and stellar masses. We consider these dynamical parameters: high-order kinematics of the line-of-sight velocity distribution (parametrised by the Gauss-Hermite coefficients $h_3$ and $h_4$), kinematic asymmetries $V_{\rm asym}$ derived using kinemetry and the observational spin parameter proxy $λ_{R_e}$. Of these, the mean $h_4$ is the only parameter found to have a significant correlation with environment as parametrised by group dynamical mass. This correlation exists even after accounting for age and stellar mass trends. Finally, we confirm that variations in the spin parameter $λ_{R_e}$ are most strongly (anti-)correlated with age as seen in local studies, and show that this dependence is well-established by z~0.3.
The MAGPI Survey: forward modelled gas-phase metallicity gradients in galaxies at $z\sim 0.3$
Sydney Institute for Astronomy (SIfA), School of Physics, The University of Sydney（悉尼大学物理学院天体物理学研究所）；Australian Astronomical Optics, Macquarie University（麦考瑞大学澳大利亚光学天文台）；ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D)（ARC三维全天空天体物理学卓越中心）；Astrophysics and Space Technologies Research Centre, Macquarie University（麦考瑞大学天体物理学与空间技术研发中心）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文学与天体物理学研究学院）；International Centre for Radio Astronomy (ICRAR), M468, The University of Western Australia（西澳大利亚国际射电天文中心）；School of Physics, University of New South Wales（新南威尔士大学物理学院）；Institute for Computational Cosmology, Durham University（杜伦大学计算宇宙学研究所）；Centre for Extragalactic Astronomy, Durham University（杜伦大学河外天文研究中心）；Department of Physics, Durham University（杜伦大学物理系）；Department of Astrophysics, University of Vienna（维也纳大学天体物理系）；School of Mathematical and Physical Sciences, Macquarie University（麦考瑞大学数学与物理科学学院）；Sub-Department of Astrophysics, University of Oxford（牛津大学天体物理学子部门）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München（慕尼黑大学物理学院大学天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；School of Mathematics and Physics, University of Queensland（昆士兰大学数学与物理学院）
The MAGPI Survey: Evidence for Non-Universal Resolved Dust Attenuation Relations Beyond the Local Universe
Macquarie University（麦考瑞大学）；University of Groningen（格罗宁根大学）；Indiana University（印第安纳大学）；National Astronomical Observatory of Japan（日本国立天文台）；Durham University（杜伦大学）；The University of Western Australia（西澳大学）；Australian National University（澳大利亚国立大学）；The University of Sydney（悉尼大学）
研究 MAGPI 巡天星系中尘埃消光与恒星形成率面密度的关系，通过与 MaNGA 本地关系比较，发现中等红移处两者关系非通用，本地校准关系无法完全描述，强调解释星系属性时需考虑星系群体和红移的消光校准。
The MAGPI survey: Stellar population radial trends and mass assembly in star-forming galaxies at z~0.3
University of Vienna（维也纳大学）；Universidade do Porto（波尔图大学）；Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto（波尔图大学空间与天体物理研究所）；University of Strasbourg（斯特拉斯堡大学）；SISSA- International School for Advanced Studies（国际高等研究院）；UWC- University of the Western Cape（西开普大学）；IFPU- Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INFN-Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Durham University（杜伦大学）
The MAGPI Survey: Emission Line Products Data Release and the Role of Spectroscopic Aperture Covering Fraction on the Balmer Decrement-Stellar Mass Relation
Deep Extragalactic VIsible Legacy Survey (DEVILS): Morphologically-selected galaxy merger fractions and their direct comparison to close-pair samples
The University of Western Australia（西澳大利亚大学）；Monash University（莫纳什大学）；Instituto Astrofisica de Canarias（加那利天体物理研究所）；Institute of Space Sciences (ICE, CSIC)（空间科学研究所）
CASCO: Cosmological and AStrophysical parameters from Cosmological simulations and Observations IV. Testing warm dark matter cosmologies with galaxy scaling relations: A joint simulation-observation study using DREAMS simulations
INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Dipartimento di Fisica “E. Pancini”, Università degli studi di Napoli Federico II（那不勒斯费德里科二世大学E. Pancini物理系）；INFN, Sez. di Napoli（意大利国家核物理研究院那不勒斯分部）；The NSF-Simons AI Institute for Cosmic Origins, University of Texas at Austin（德克萨斯大学奥斯汀分校NSF-Simons宇宙起源AI研究所）；Departments of Statistics and Data Sciences, University of Texas at Austin（德克萨斯大学奥斯汀分校统计与数据科学系）；Department of Astronomy, University of Virginia（弗吉尼亚大学天文系）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；Virginia Institute for Theoretical Astronomy, University of Virginia（弗吉尼亚理论天文研究所）；Department of Astrophysical Sciences, Princeton University（普林斯顿大学天体物理学科学系）
When galaxies cross cold fronts: wind tunnel simulations of ram pressure stripping
Universidade Tecnológica Federal do Paraná（帕拉纳联邦技术大学）；Observatório Nacional（国家天文台）；Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo（圣保罗大学天文、地球物理与大气科学研究所）
Galaxy And Mass Assembly (GAMA): The absence of stellar mass segregation in galaxy groups and consistent predictions from GALFORM and EAGLE simulations
Towards Accurate Modelling of Galaxy Clustering on Small Scales: Testing the Standard $Λ\mathrm{CDM}$ + Halo Model
用晕模型解释星系的小尺度成团现象可以阐明星系与暗物质晕之间的联系。不幸的是，建模通常不够准确，无法在统计上排除模型。因此，很难使用小尺度编码的信息来测试宇宙学模型或探测星系-晕连接的微妙特征。在本文中，我们试图推动晕模型的"准确"的制度，完全数值模拟为基础的方法和统计和系统误差的仔细治疗。通过我们的前向建模方法，我们可以将聚类统计纳入传统的两点统计之外。我们使用这种建模方法来测试标准的$Λ\mathrm{CDM}$+晕模型对SDSS DR 7星系的聚类。具体地说，我们使用投影关联函数，群多重性函数和星系数密度作为约束条件。我们发现，虽然模型分别拟合每个统计量，但它很难同时拟合它们。添加组统计量会导致对模型进行更严格的测试，并对模型参数进行更严格的约束。我们探讨了不同的晕定义和宇宙学模型的影响，发现改变宇宙学有显着的差异。我们尝试的最成功的模型（普朗克宇宙学与Mvir晕）匹配的低光度星系的集群，但表现出2.3 $σ$张力与发光星系的集群，从而提供了证据，"标准"晕模型需要扩展。这项工作打开了大门，增加有趣的自由光环模型，并包括额外的聚类统计作为约束。
