Detectability of Satellite Planes in Mock Observations of Isolated L* Galaxies
Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天文与天体物理研究学院）；Leibniz-Institut für Astrophysik Potsdam（波茨坦阿斯特罗物理莱布尼茨研究所）；Institute of Physics, Laboratory of Astrophysics, Ecole Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院物理系天体物理实验室）；Clare Hall, University of Cambridge（剑桥大学克莱尔厅）
Ethan Crosby, Marcel S. Pawlowski, Oliver Müller, Helmut Jerjen
备注：
13 pages, 12 figures, accepted for publication in the MNRAS
The existence and prevalence of planar, co-rotating distributions of satellite galaxies around L* host galaxies in the local universe remains a subject of ongoing debate. Despite numerous observational efforts over the past decade, a statistically robust sample of "satellite planes" across the diversity of host galaxy environments is lacking. To guide future observing strategies, we construct a controlled suite of mock observations of on-sky positions and line-of-sight (LOS) velocities of isolated L* host galaxies and their satellite systems, based on samples drawn from the Illustris TNG100-1 cosmological simulation to build a statistical sample. In these mock systems, satellite planes are defined by three key parameters: the number of satellites ($N_{\mathrm{sat}}$), the fraction residing in a thin co-rotating plane ($f_{p}$), and the orientation angle relative to the observer ($θ_{\mathrm{rot}}$). We evaluate the sensitivity of three observational metrics, $N_{\mathrm{cor}}$ (number of co-rotating satellites), $b/a$ (projected flattening of the satellite distribution), and $v_\mathrm{los}$ (mean absolute LOS velocity), to the presence of such planes. Our results show that detection rates are strongly dependent on $θ_{\mathrm{rot}}$ and $N_{\mathrm{sat}}$. Satellite planes that are viewed nearly edge-on or face-on, are the most readily detected. In contrast, intermediate orientations and systems with fewer satellites yield low detection success rates. Generally, only satellite planes with $N_{\mathrm{sat}}>20$ have high chances of being detected. These findings provide a practical framework for prioritising observational targets and designing future surveys aimed at detecting and characterising satellite planes.
The detectability of bars at high redshift: a case study using Euclid-like mock observations of TNG50 simulated galaxies
Universidade Tecnológica Federal do Paraná（巴西联邦技术大学巴拉那）；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）；European Southern Observatory（欧洲南方天文台）；Aix Marseille Université, CNRS, CNES, LAM（艾克斯-马赛大学）；Universidade Federal do Rio de Janeiro, Observatório do Valongo（里约热内卢联邦大学瓦隆戈天文台）；Centro Brasileiro de Pesquisas Físicas（巴西物理研究中心）
On the Detectability and Measurement of Galactic Bars as a Function of Redshift
Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Department of Astronomy, School of Physics, Peking University（北京大学物理学院天文学系）；Department of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院天文学系）；Key Laboratory for Particle Astrophysics and Cosmology (MOE)/Shanghai Key Laboratory for Particle Physics and Cosmology（粒子天体物理与宇宙学教育部重点实验室/上海粒子物理与宇宙学重点实验室）；Department of Astronomy, University of Illinois Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校天文学系）
Mock Observatory: two thousand lightcone mock catalogues of luminous red galaxies from the Hyper Suprime-Cam Survey for the cosmological large-scale analysis
Observing the host galaxies of high-redshift quasars with JWST: predictions from the BlueTides simulation
高红移类星体发出的明亮辐射在静止坐标系的紫外/光学波段完全掩盖了它们的宿主星系，甚至哈勃太空望远镜（HST）也无法利用详细的点扩散函数（PSF）建模技术来探测这些波长的宿主星系。在这项研究中，我们产生模拟图像的样本z=7类星体提取的BlueTides模拟，并应用马尔可夫链蒙特卡洛为基础的PSF建模，以确定其宿主星系的可探测性与詹姆斯韦伯太空望远镜（JWST）。虽然没有统计学意义的检测与HST，我们预测，在相同的波长和曝光时间JWST近红外相机成像将检测到约50%的类星体宿主星系。我们研究了各种观测策略，发现长波长滤波器中的NIRCam宽带成像导致成功探测类星体宿主的比例最高，在5 ks的曝光时间内探测到>80%的明亮类星体宿主。在NIRCam宽波段滤波器中，需要约5 k s的曝光时间来探测大多数宿主星系，然而，即使用MIRI进行10 k s的曝光，也会导致<30%的宿主星系探测成功。我们发现星系的属性和它们的可探测性之间没有显着的趋势。PSF模型可以准确地恢复主机的大小，半径和空间分布的大规模的发射，占中央核心被污染的残余类星体通量。在解释使用PSF建模测量的主机属性时应小心。
Identifying signatures of inflow onto face-on galaxies using the Balmer decrement
Columbia University（哥伦比亚大学）；Tsinghua University（清华大学）；Rensselaer Polytechnic Institute（伦斯勒理工学院）；The University of Texas at Dallas（德克萨斯大学达拉斯分校）；York University（约克大学）
