The TRAPUM Small Magellanic Cloud pulsar survey with MeerKAT -- II. Nine new radio timing solutions and glitches from young pulsars
E. Carli, D. Antonopoulou, M. Burgay, M. J. Keith, L. Levin, Y. Liu, B. W. Stappers, J. D. Turner, E. D. Barr, R. P. Breton, S. Buchner, M. Kramer, P. V. Padman… 展开作者
E. Carli, D. Antonopoulou, M. Burgay, M. J. Keith, L. Levin, Y. Liu, B. W. Stappers, J. D. Turner, E. D. Barr, R. P. Breton, S. Buchner, M. Kramer, P. V. Padmanabh, A. Possenti, V. Venkatraman Krishnan, C. Venter, W. Becker, C. Maitra, F. Haberl, T. Thongmeearkom
备注：
20 pages, 13 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society
We report new radio timing solutions from a three-year observing campaign conducted with the MeerKAT and Murriyang telescopes for nine Small Magellanic Cloud pulsars, increasing the number of characterised rotation-powered extragalactic pulsars by 40 per cent. We can infer from our determined parameters that the pulsars are seemingly all isolated, that six are ordinary pulsars, and that three of the recent MeerKAT discoveries have a young characteristic age of under 100 kyr and have undergone a spin-up glitch. Two of the sources, PSRs J0040$-$7337 and J0048$-$7317, are energetic young pulsars with spin-down luminosities of the order of 10$^{36}$ erg s$^{-1}$. They both experienced a large glitch, with a change in frequency of about 30 $μ$Hz, and a frequency derivative change of order $-10^{-14}$ Hz s$^{-1}$. These glitches, the inferred glitch rate, and the properties of these pulsars (including potentially high inter-glitch braking indices) suggest these neutron stars might be Vela-like repeating glitchers and should be closely monitored in the future. The position and energetics of PSR J0048$-$7317 confirm it is powering a new Pulsar Wind Nebula (PWN) detected as a radio continuum source; and similarly the association of PSR J0040$-$7337 with the PWN of Supernova Remnant (SNR) DEM S5 (for which we present a new Chandra image) is strengthened. Finally, PSR J0040$-$7335 is also contained within the same SNR but is a chance superposition. It has also been seen to glitch with a change of frequency of $10^{-2}$ $μ$Hz. This work more than doubles the characterised population of SMC radio pulsars.
The TRAPUM Large Magellanic Cloud pulsar survey with MeerKAT II: 12 new discoveries and timing solutions for 7 pulsars
The University of Cape Town（开普敦大学）；University of Cape Town（开普敦大学）；The University of Manchester（曼彻斯特大学）；North-West University（西北大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；South African Radio Astronomy Observatory (SARAO)（南非射电天文台）；INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；LAPTh, CNRS, USMB（拉格朗日天体物理实验室，法国国家科学研究中心，尚贝里大学）；Swinburne University of Technology（斯威本科技大学）；OzGrav: The ARC Center of Excellence for Gravitational Wave Discovery（澳引力波发现卓越中心）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；Universität Bielefeld（比勒费尔德大学）；National Astronomical Research Institute of Thailand（泰国国家天文研究所）；National Institute for Theoretical and Computational Sciences, South Africa（南非理论与计算科学研究所）
Pulsar Discoveries from the TRAPUM UHF Survey of Fermi-LAT Sources
The University of Manchester（曼彻斯特大学）；National Astronomical Research Institute of Thailand（泰国国家天文研究所）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）
The pulsar population of Omega Centauri: New TRAPUM searches, timing, and cluster dynamics with MeerKAT and Parkes
INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Australia Telescope National Facility, CSIRO（CSIRO澳大利亚望远镜国家设施）；School of Science, Western Sydney University（西悉尼大学理学院）；Space Science Division, Naval Research Laboratory（海军研究实验室空间科学部）；South African Radio Astronomy Observatory（南非射电天文观测站）
TRAPUM search for pulsars in supernova remnants and pulsar wind nebulae - II. Survey analysis and population study
The University of Manchester（曼彻斯特大学）；Max Planck Institute for Radio Astronomy（马克斯·普朗克射电天文研究所）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所-卡利亚里天文台）；Royal Holloway, University of London（伦敦大学皇家霍洛威学院）；Institute of Space Sciences (ICE-CSIC)（空间科学研究所（西班牙高等科学研究委员会））；National Astronomical Research Institute of Thailand（泰国国家天文研究所）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理学研究所（阿尔伯特·爱因斯坦研究所））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；Trinity College Dublin（都柏林三一学院）；Universität Bielefeld（比勒费尔德大学）
Optical Study of TRAPUM Pulsars and Modelling of the Redbacks: PSR J1036$-$4353 and PSR J1803$-$6707
The University of Manchester（曼彻斯特大学）；National Astronomical Research Institute of Thailand（泰国国家天文研究所）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Leibniz University Hannover（汉诺威莱布尼茨大学）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所-卡利亚里天文台）；Michigan State University（密歇根州立大学）；University of Illinois at Urbana-Champaign（伊利诺伊大学厄巴纳-香槟分校）；University College Cork（科克大学学院）；Heidelberg University（海德堡大学）；University of Sheffield（谢菲尔德大学）
本文报道了用MeerKAT望远镜在球状星团M28中发现的两颗黑寡妇毫秒双星。PSR J1824 $-$ 2452 M（M28 M）是一颗4.78毫秒的脉冲星，在$5.82\,$小时轨道上运行; PSR J1824 $-$ 2452 N（M28 N）是一颗3.35毫秒的脉冲星，在$4.76\,$小时轨道上运行。这两颗双星都有$119.30\,$ pc $\,$ cm $^{-3}$附近的色散测量值，并且有低质量的伴星（$\sim$ $0.01-0.03\,$ M $_\odot$），它们不会引起强烈的射电食或轨道变化。包括这些系统在内，M28中目前已知有五个黑寡妇卫星。脉冲星搜索是MeerKAT球状星团普查初始阶段的一部分（在TRAPUM大型调查项目中）。这些微弱的发现证明了MeerKAT的调查灵敏度比以前的搜索的优势，我们希望在这个集群的继续搜索中找到更多的恒星。
Jodrell Bank Centre for Astrophysics, Department of Physics and Astronomy, The University of Manchester（曼彻斯特大学物理与天文学系约维尔银行天体物理学中心）；LPC2E, OSUC, Univ Orleans, CNRS, CNES, Observatoire de Paris（奥尔良大学地球环境与气候实验室（LPC2E））；ORN, Observatoire de Paris, Université PSL, Univ Orléans, CNRS（巴黎天文台南锡观测站）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超算中心）；OzGrav: The ARC Centre of Excellence for Gravitational Wave Discovery（澳大利亚引力波发现卓越研究中心（OzGrav））；Department of Physics and Astronomy, Vanderbilt University（范德堡大学物理与天文学系）；Dipartimento di Fisica “G. Occhialini”, Università degli Studi di Milano-Bicocca（米兰比可卡大学G.奥恰利尼物理学系）；INFN, Sezione di Milano-Bicocca（意大利国家核物理研究所米兰比可卡分部）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；CSIRO Astronomy and Space Science（澳大利亚联邦科学与工业研究组织天文与空间科学部）；Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）
Radio and Gamma-Ray Timing of a Newly Discovered Millisecond Pulsar
University of Wisconsin-Milwaukee（密尔沃基威斯康星大学）；Max Planck Institute for Gravitational Physics (Albert Einstein Institute)（马克斯·普朗克引力物理研究所（爱因斯坦研究所））；Leibniz Universität Hannover（汉诺威莱布尼茨大学）；University of North Carolina at Chapel Hill（北卡罗来纳大学教堂山分校）
