We revisit the predictions for the merger rate of massive black hole binaries detectable by the Laser Interferometer Space Antenna (LISA) and their background signal for pulsar-timing arrays. We focus on the effect of the delays between the merger of galaxies and the final coalescence of black hole binaries, and on supernova feedback on the black hole growth. By utilizing a semi-analytic galaxy formation model, not only do we account for the driving the evolution of binaries at separations $\lesssim 1$ pc (gas-driven migration, stellar hardening and triple/quadruple massive black hole systems), but we also improve on previous studies by accounting for the time spent by black hole pairs from kpc down to pc separation. We also include the effect of supernova feedback, which may eject gas from the nuclear region of low-mass galaxies, thus hampering the growth of black holes via accretion and suppressing their orbital migration in circumbinary disks. Despite including these novel physical effects, we predict that the LISA detection rate should still be $\gtrsim 2 \mbox{yr}^{-1}$, irrespective of the model for the black hole seeds at high redshifts. Scenarios where black holes form from $\sim100 M_\odot$ seeds are more significantly impacted by supernova feedback. We also find that for detectable events, the merging black holes typically have mass ratios between $\sim 0.1$ and $1$. Predictions for the stochastic background in the band of pulsar-timing array experiments are instead rather robust, and show only a mild dependence on the model.
Wandering intermediate-mass black holes and off-nuclear tidal disruption events from early star clusters
Carnegie Mellon University（卡内基梅隆大学）；Massachusetts Institute of Technology（麻省理工学院）；Philipps Universität Marburg（马尔堡菲利普斯大学）；Rutgers, The State University of New Jersey（罗格斯大学）；Flatiron Institute（平顿研究所）；The University of Tokyo（东京大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI)（宇宙物理与数学研究 Kavli 研究所）
Distance Determination of Southern Galactic Plane Supernova Remnants with the Mopra CO Survey and DECaPS 3D Dust Map
School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究院）；Institute of Astronomy and Physics, Inner Mongolia University（内蒙古大学天文与物理学院）；Departamento de Fisica y Astronomia, Facultad de Ciencias Exactas, Universidad Andres Bello（安德烈斯贝略大学精确科学学院物理与天文学系）；Center for Astrophysics, Guangzhou University（广州大学天体物理中心）
A Study Revealing Physical Attributes of Supernova Remnant in G321.3-3.9
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；School of Physics and Electronic Science, Guizhou Normal University（贵州师范大学物理与电子科学学院）；School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）
The Extinction Distance of Supernova Remnants in Combination with the CO Line Measurements
School of Physics and Astronomy, Beijing Normal University（北京师范大学物理与天文学院）；Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University（北京师范大学前沿天文与天体物理研究所）；Center for Astrophysics, Guangzhou University（广州大学天体物理中心）；Departamento de Fisica y Astronomia, Facultad de Ciencias Exactas, Universidad Andres Bello（安第斯贝尔托大学精确科学学院物理与天文系）
A high resolution HI study towards the supernova remnant Puppis A and its environments
我们观察超新星遗迹（SNR）船尾座A在21厘米线与澳大利亚望远镜紧凑阵列的目的是确定系统的速度，因此，相应的运动学距离。对于紧凑的，在现场的背景源，我们得到的吸收光谱，通过应用两种方法：（a）减去轮廓上和关闭源连续发射，和（b）过滤傅立叶平面中的短空间频率，以消除大规模的发射。船尾座A外壳东部最亮的特征之一被发现是背景源，可能是河外星系。除去这个和以前已知的不相关的源的贡献，船尾座A的系统速度被限制在8和12 km s $^{-1}$之间，这使得这个源的距离为1.3 $\pm$ 0.3 kpc。从包括单碟和干涉数据的组合图像中，我们分析了星际氢的分布。我们认为，如果距离为$\lesssim$ 1.2 kpc，那么在$v \sim $ +8 km s $^{-1}$处的椭球环可能是船尾座A的祖先吹出的气泡的遗迹。与以前的出版物（$v =$ +16 km s $^{-1}$和$d = $ 2.2 kpc）相比，新的系统速度和距离的主要结果是在东方没有一个致密的相互作用云来解释形态，以及壳层尺寸和中子星速度的减小，现在与统计值更好地吻合。
Unveiling the Milky Way with a Gaia DR3 census of OB-type stars within 2 kpc. I. Tracing local Galactic structure, massive star-forming regions and core-collapse supernova progenitors
Observatoire de Paris, Université PSL, Sorbonne Université, Université Paris Cité, CY Cergy Paris Université, CNRS（巴黎天文台，巴黎文理研究大学，索邦大学，巴黎西岱大学，CY塞吉-蓬图瓦兹大学，法国国家科学研究中心）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；INAF – Osservatorio Astrofisico di Torino（意大利国家天体物理研究所都灵天文台）；University of Vienna（维也纳大学）；Keele University（基尔大学）；Instituto de Astrofísica de Canarias（加那利天体物理学研究所）；Universidad de La Laguna（拉古纳大学）；European Southern Observatory（欧洲南方天文台）
SN 2025adpq: A Type Ia supernova in a collisional ring formed during a major galaxy merger
Carnegie Mellon University（卡内基梅隆大学）；University of Pennsylvania（宾夕法尼亚大学）；Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；Swinburne University of Technology（斯威本科技大学）；Ludwig-Maximilians-Universität München（慕尼黑路德维希-马克西米利安大学）
