The potential role of magnetic fields and cosmic ray propagation for feedback processes in the early Universe can be probed by studies of local starburst counterparts with an equivalent star-formation rate. Archival data from the WSRT was reduced and a new calibration technique introduced to reach the high dynamic ranges needed for the complex source morphology of M82. This data was combined with archival VLA data, yielding total power maps at 3cm, 6cm, 22cm and 92cm. The data shows a confinement of the emission at wavelengths of 3/6cm to the core region and a largely extended halo reaching up to 4kpc away from the galaxy midplane at wavelengths of 22/92cm up to a sensitivity limit of 90muJy and 1.8mJy respectively. The results are used to calculate the magnetic field strength in the core region to 98muG and to 24muG in the halo regions. From the observation of free-free losses the filling factor of the ionised medium could be estimated to 2%. We find that the radio emission from the core region is dominated by very dense HII-regions and supernova remnants, while the surrounding medium is filled with hot X-ray and neutral gas. Cosmic rays radiating at frequencies higher than 1.4 GHz are suffering from high synchrotron and inverse Compton losses in the core region and are not able to reach the halo. Even the cosmic rays radiating at longer wavelengths are only able to build up the observed kpc sized halo, when several starbursting periods are assumed where the photon field density varies by an order of magnitude. These findings together with the strong correlation between Halpha, PAH+, and our radio continuum data suggests a magnetic field which is frozen into the ionised medium and driven out of the galaxy kinematically.
The Rapid ASKAP Continuum Survey VII: Spectra and Polarisation In Cutouts of Extragalactic Sources (SPICE-RACS) Second Data Release -- Unveiling the Magnetised Sky
SKA Observatory, SKA-Low Science Operations Centre（SKA 天文台，SKA-Low 科学运营中心）；ATNF, CSIRO Space & Astronomy（CSIRO 空间与天文学部 ATNF）；CSIRO Information Management & Technology（CSIRO 信息管理与技术部）；Departamento de Física de la Tierra y Astrofísica & IPARCOS-UCM, Universidad Complutense de Madrid（马德里康普顿斯大学地球物理与天体物理学系及 IPARCOS-UCM）；Research School of Astronomy & Astrophysics, The Australian National University（澳大利亚国立大学天文学与天体物理学研究学院）；Dunlap Institute for Astronomy and Astrophysics, University of Toronto（多伦多大学邓普勒天文学与天体物理学研究所）
MEDUSA I. Tracing magnetic field structures in tidal arms of the dwarf-dwarf merger NGC 1487
Ruhr Astroparticle and Plasma Physics Center (RAPP Center)（鲁尔高能粒子与等离子体物理中心）；CSIRO Space and Astronomy（澳大利亚联邦科学与工业研究组织空间与天文部门）；Thüringer Landessternwarte（图林根州立天文台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Ruhr University Bochum, Faculty for Physics & Astronomy, Theoretical Physics IV: Plasma Astroparticle Physics（波鸿鲁尔大学物理与天文学学院理论物理学第四系：等离子体高能天体物理学）；SKA Observatory, SKA-Low Science Operations Centre（平方公里阵列射电望远镜天文台，SKA低频科学运行中心）；INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；Astronomical Observatory of the Jagiellonian University（雅盖隆大学天文台）
Misaligned or chaotic? A strong break of axial symmetry in the local LRD J1025 revealed with VLT/FORS2 spectropolarimetry
Kavli Institute for Cosmology, University of Cambridge（卡弗里宇宙学研究所，剑桥大学）；Cavendish Laboratory, University of Cambridge（卡文迪许实验室，剑桥大学）；Kapteyn Astronomical Institute, University of Groningen（卡普坦天文研究所，格罗宁根大学）
我们目前1至10 GHz的无线电连续通量密度，光谱指数，偏振和旋转测量（RM）的最年轻的已知银河系超新星遗迹（SNR）G1.9+0.3的图像，使用澳大利亚望远镜紧凑阵列（ATCA）的观测。我们在1984年至2017年期间进行了一项跨越8个时期的扩张研究，得出的结果与之前的G1.9+0.3扩张研究一致。我们发现一个平均的无线电连续扩展率（$0.78 \pm 0.09$）百分之一年$^{-1}$（或$\sim8900$公里秒$^{-1}$在一个假设的距离为8.5千秒差距），虽然扩展率在整个SNR周长变化。在2016年至2017年的最近时期，我们观察到北部地区的扩张速度快于预期。我们找到了$-0.81\pm0.02$（76 MHz $-$ 10 GHz）的G1.9+0.3的全局频谱指数。然而，朝向北部地区，观测到无线电频谱显著变陡（$\sim -$ 1）。对于G1.9+0.3的两个所谓的（东和西）“耳”，我们发现400-600 rad m $^{2}$和100-200 rad m $^{2}$的RM值分别非常不同。射电连续辐射的分极化达到（19 $\pm$ 2）~ %，与其它稍老的SNR（如Cas~A）一致。
Cosmic-ray electron propagation in NGC 3044 from radio continuum observations
Yunnan University（云南大学）；SKA Observatory, SKA-Low Science Operations Centre（SKA天文台，SKA低频科学运营中心）；CSIRO Space and Astronomy（CSIRO空间与天文学）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；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）；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）；Queen’s University（女王大学）；Instituto de Astrofísica de Andalucía (IAA-CSIC)（安达卢西亚天体物理研究所）
