First studies of the diffuse X-ray emission in the Large Magellanic Cloud with eROSITA
Manami Sasaki, Jonathan Knies, Frank Haberl, Chandreyee Maitra, Jürgen Kerp, Andrei M. Bykov, Konrad Dennerl, Miroslav D. Filipović, Michael Freyberg, Bärbel S.… 展开作者
Manami Sasaki, Jonathan Knies, Frank Haberl, Chandreyee Maitra, Jürgen Kerp, Andrei M. Bykov, Konrad Dennerl, Miroslav D. Filipović, Michael Freyberg, Bärbel S. Koribalski, Sean Points, Lister Staveley-Smith
备注：
Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission
In the first months after the launch in July 2019, eROSITA onboard Spektr-RG (SRG) performed long-exposure observations in the regions around SN 1987A and SNR N132D in the Large Magellanic Cloud (LMC). We analyse the distribution and the spectrum of the diffuse X-ray emission in the observed fields to determine the physical properties of the hot phase of the interstellar medium (ISM). The eROSITA data are complemented by newly derived column density maps for the Milky Way and the LMC, 888 MHz radio continuum map from the Australian Square Kilometer Array Pathfinder (ASKAP), and optical images of the Magellanic Cloud Emission Line Survey (MCELS). We detect significant emission from thermal plasma with kT=0.2 keV in all the regions. There is also an additional higher-temperature emission component from a plasma with kT = 0.7 keV. In addition, non-thermal X-ray emission is significantly detected in the superbubble 30 Dor C. The absorbing column density NH in the LMC derived from the analysis of the X-ray spectra taken with eROSITA is consistent with the NH obtained from the emission of the cold medium over the entire area. Neon abundance is enhanced in the regions in and around 30 Dor and SN 1987A, indicating that the ISM has been chemically enriched by the young stellar population. Emission from the stellar cluster RMC 136 and the Wolf-Rayet stars RMC 139 and RMC 140 is best modelled with a high-temperature (kT>1 keV) non-equilibrium ionisation plasma emission and a non-thermal component with a photon index of Γ =1.3. In addition, the optical SNR candidate J0529-7004 is also detected with eROSITA and we thus confirm the source as an SNR.
Searching for dark matter X-ray lines from the Large Magellanic Cloud with eROSITA
Istituto Nazionale di Fisica Nucleare, Sezione di Torino（意大利国家核物理研究所都灵分部）；CERN（欧洲核子研究组织）；Dipartimento di Fisica, “Sapienza” Università di Roma & Sezione INFN Roma1（罗马大学物理系及INFN罗马一分部）；Weizmann Institute of Science（魏茨曼科学研究所）；Louisiana State University（路易斯安那州立大学）；Dipartimento di Fisica, Università di Torino（都灵大学物理系）
A comprehensive catalogue of high-mass X-ray binaries in the Large Magellanic Cloud detected during the first eROSITA all-sky survey
Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；Inter-University Centre for Astronomy and Astrophysics (IUCAA)（大学间天文学与天体物理学中心）；Anton Pannekoek Institute for Astronomy, University of Amsterdam（阿姆斯特丹大学安东·潘内库克天体物理研究所）；Department of Astronomy, The University of Michigan（密歇根大学天文学系）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、CEA、CNRS、AIM）；Southern African Astronomical Observatory（南非天文台）；Department of Astronomy, University of Cape Town（开普敦大学天文学系）；Leibniz Institut für Astrophysik Potsdam（波茨坦莱布尼茨天体物理研究所）
Broadband study of the Be/X-ray binary pulsar eRASSU J012422.9-724248 in the Magellanic Bridge, near the Eastern Wing of the Small Magellanic Cloud
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Max-Planck-Institut für extraterrestrische Physik（马克斯·普朗克地外物理研究所）；Inter-University Centre for Astronomy and Astrophysics (IUCAA)（大学间天文学与天体物理学中心）；Institut für Astronomie und Astrophysik, Universität Tübingen（蒂宾根大学天文与天体物理研究所）；Astronomical Observatory, University of Warsaw（华沙大学天文台）；Department of Physics, National and Kapodistrian University of Athens（雅典国立卡波迪斯特里亚斯大学物理系）；Institute of Accelerating Systems & Applications（加速系统与应用研究所）
Identification of a Large-Scale Diffuse Gamma-Ray Structure in the Southern Galactic Hemisphere
School of Astronomy and Space Science, University of Science and Technology of China（中国科学技术大学天文与空间科学学院）；Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台暗物质与空间天文重点实验室）
Bayesian Multi-wavelength Imaging of the LMC SN1987A with SRG/eROSITA
Max Planck Institute for Astrophysics（马克斯·普朗克天体物理研究所）；Ludwig-Maximilians-Universität München（慕尼黑路德维希-马克西米利安大学）；Kavli Institute for Particle Astrophysics & Cosmology, Stanford University（斯坦福大学卡弗里粒子天体物理学与宇宙学研究所）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理学研究所）；Excellence Cluster ORIGINS（ORIGINS卓越集群）
X-ray panorama of the SS433/W50 complex by SRG/eROSITA
Space Research Institute (IKI)（空间研究所）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）；Universitäts-Sternwarte, Fakultät für Physik, Ludwig-Maximilians-Universität München（慕尼黑大学物理学院大学天文台）
Thermal or Non-thermal? Diffuse emission in the infall region of stacked galaxy groups
Ludwig-Maximilians-Universität（路德维希-马克西米利安大学）；INAF, Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所，天文与空间科学观测站）；University of Geneva（日内瓦大学）；California Institute of Technology（加州理工学院）；Princeton University（普林斯顿大学）；Max Planck Institute for Extraterrestrial Physics（马普地外物理研究所）
Differential Sensitivity of the KM3NeT/ARCA detector to a diffuse neutrino flux and to point-like source emission: exploring the case of the Starburst Galaxies
eRASSU J043115.8-711730 :the first pulsating symbiotic super-soft X-ray source in the Magellanic Bridge
Inter-University Centre for Astronomy Astrophysics（大学间天文与天体物理中心）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；School of Physics Astronomy University of Southampton（南安普顿大学物理与天文学学院）；Department of Physics University of the Free State（自由州大学物理系）；Astronomical Observatory of the University of Warsaw（华沙大学天文台）；South African Astronomical Observatory（南非天文台）；Department of Astronomy University of Cape Town（开普敦大学天文学系）；Southern African Large Telescope（南部非洲大型望远镜）；Dr. Karl Remeis-Sternwarte, Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg（弗里德里希-亚历山大·埃尔朗根-纽伦堡大学卡尔·雷米斯天文台、埃尔朗根天体粒子物理中心）
A Swift X-ray view of the SMS4 sample - III: Deeper insight into previously undetected sources
INAF-Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；ASI Space Science Data Center (SSDC)（意大利航天局空间科学数据中心）；Harvard-Smithsonian Center for Astrophysics（哈佛-史密森尼天体物理中心）
The diffusion coefficient in the Large Magellanic Cloud
University of Alberta（阿尔伯塔大学）；Istituto Nazionale di Fisica Nucleare, Sezione di Napoli（意大利国家核物理研究所，那不勒斯分部）；INFN Sezione di Pisa（意大利国家核物理研究所，比萨分部）；University of Torino（意大利国家核物理研究所，都灵分部）
