Broadband study and the discovery of pulsations from the Be/X-ray binary eRASSU J052914.9-662446 in the Large Magellanic Cloud
C. Maitra, D. Kaltenbrunner, F. Haberl, D. A. H. Buckley, I. M. Monageng, A. Udalski, S. Carpano, J. B. Coley, V. Doroshenko, L. Ducci, C. Malacaria, O. König, … 展开作者
C. Maitra, D. Kaltenbrunner, F. Haberl, D. A. H. Buckley, I. M. Monageng, A. Udalski, S. Carpano, J. B. Coley, V. Doroshenko, L. Ducci, C. Malacaria, O. König, A. Santangelo, G. Vasilopoulos, J. Wilms
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11 pages, 13 figures, 3 tables, accepted for publication in A&A
Context. The Magellanic Clouds are our nearest star-forming galaxies. While the population of high-mass X-ray binaries (HMXBs) in the Small Magellanic Cloud (SMC) is relatively well studied, our knowledge about the Large Magellanic Cloud (LMC) is far from complete given its large angular extent and insufficient coverage with X-ray observations. Aims. We conducted a search for new HMXBs in the LMC using data from eROSITA, the soft X-ray instrument on board the Spektrum-Roentgen-Gamma (SRG) satellite. Methods. After confirming the nature of eRASSU J052914.9-662446 as a hard X-ray source positionally coincident with an early type star, we followed it up with optical spectroscopic observations from South African Large Telescope (SALT) and a dedicated NuSTAR observation. Results. We study the broadband timing and spectral behaviour of the newly discovered HMXB eRASSU J052914.9-662446 through eROSITA, Swift and NuSTAR data in X-rays and the Optical Gravitational Lensing Experiment (OGLE) and SALT RSS data at optical wavelength. We report on detection of the spin period at 1412 s and suggest an orbital period of the system of ~151 days, and thereby establish eRASSU J052914.9-662446 as an accreting pulsar. Further, through optical spectroscopic observations and the existence of H alpha emission the source is identified as a Be X-ray binary pulsar in the LMC. We also investigate the variability of the source in the optical and X-ray regime over the last decades and provide estimates on the possible magnetic field strength of the neutron star.
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）
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）
X-ray, optical, and radio follow-up of five thermally emitting isolated neutron star candidates
Center for Lunar and Planetary Sciences, Institute of Geochemistry, Chinese Academy of Sciences（中国科学院地球化学研究所月球与行星科学中心）；College of Physics, Guizhou University（贵州大学物理学院）；Potsdam University, Institute for Physics and Astronomy（波茨坦大学物理与天文研究所）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Key Laboratory of Radio Astronomy and Technology, Chinese Academy of Sciences（中国科学院射电天文与技术重点实验室）
