Refined Mass and Geometric Measurements of the High-Mass PSR J0740+6620
Emmanuel Fonseca, H. Thankful Cromartie, Timothy T. Pennucci, Paul S. Ray, Aida Yu. Kirichenko, Scott M. Ransom, Paul B. Demorest, Ingrid H. Stairs, Zaven Arzou… 展开作者
Emmanuel Fonseca, H. Thankful Cromartie, Timothy T. Pennucci, Paul S. Ray, Aida Yu. Kirichenko, Scott M. Ransom, Paul B. Demorest, Ingrid H. Stairs, Zaven Arzoumanian, Lucas Guillemot, Aditya Parthasarathy, Matthew Kerr, Ismael Cognard, Paul T. Baker, Harsha Blumer, Paul R. Brook, Megan DeCesar, Timothy Dolch, F. Adam Dong, Elizabeth C. Ferrara, William Fiore, Nathaniel Garver-Daniels, Deborah C. Good, Ross Jennings, Megan L. Jones, Victoria M. Kaspi, Michael T. Lam, Duncan R. Lorimer, Jing Luo, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Arun Naidu, Cherry Ng, David J. Nice, Nihan Pol, Henri A. Radovan, Brent Shapiro-Albert, Chia Min Tan, Shriharsh P. Tendulkar, Joseph K. Swiggum, Haley M. Wahl, Weiwei Zhu
备注：
Final version after minor corrections during referee process. Published in the Astrophysical Journal Letters on 1 July 2021
We report results from continued timing observations of PSR J0740+6620, a high-mass, 2.8-ms radio pulsar in orbit with a likely ultra-cool white dwarf companion. Our data set consists of combined pulse arrival-time measurements made with the 100-m Green Bank Telescope and the Canadian Hydrogen Intensity Mapping Experiment telescope. We explore the significance of timing-based phenomena arising from general-relativistic dynamics and variations in pulse dispersion. When using various statistical methods, we find that combining $\sim 1.5$ years of additional, high-cadence timing data with previous measurements confirms and improves upon previous estimates of relativistic effects within the PSR J0740+6620 system, with the pulsar mass $m_{\rm p} = 2.08^{+0.07}_{-0.07}$ M$_\odot$ (68.3\% credibility) determined by the relativistic Shapiro time delay. For the first time, we measure secular variation in the orbital period and argue that this effect arises from apparent acceleration due to significant transverse motion. After incorporating contributions from Galactic differential rotation and off-plane acceleration in the Galactic potential, we obtain a model-dependent distance of $d = 1.14^{+0.17}_{-0.15}$ kpc (68.3\% credibility). This improved distance confirms the ultra-cool nature of the white dwarf companion determined from recent optical observations. We discuss the prospects for future observations with next-generation facilities, which will likely improve the precision on $m_{\rm p}$ for J0740+6620 by an order of magnitude within the next few years.
The Tail of PSR J0002+6216 and the Supernova Remnant CTB 1
我们已经进行了VLA成像和费米定时分析的115毫秒的伽玛射线和射电脉冲星PSR J0002+6216。我们发现，脉冲星位于一个狭窄的准直彗星般的7弧分的非热无线电发射的尾巴，我们确定为弓形激波脉冲星风星云的顶点。星云的尾部指向超新星遗迹CTB 1（G116.9+0.2）的几何中心，距离为28弧分，位置角为$θ_μ=113^\circ$。我们测量的自行与2.9 $σ$的意义从费米定时分析$μ$ =115 $\pm$ 33 mas yr $^{-1}$和$θ_μ=121^\circ\pm{13}^\circ$，对应于一个大的横向脉冲星速度为1100 km s $^{-1}$在2 kpc的距离。这个自行的大小和方向都是正确的，支持PSR J0002+6216诞生于产生CTB 1的同一颗超新星的说法。我们探讨了脉冲星诞生期，不对称超新星爆炸，和机制脉冲星出生踢速度的影响。
Improved proper motion and gravity tests with PSR J1913+1102
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Aalborg University（奥尔堡大学）；Henan Academy of Sciences（河南省科学院）；Beijing Normal University（北京师范大学）；University of East Anglia（东英吉利大学）；University of Manchester（曼彻斯特大学）
Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854
Department of Applied Mathematics, University of Cape Town（开普敦大学应用数学系）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Department of Physics and Astronomy, West Virginia University（西弗吉尼亚大学物理与天文学系）；Center for Gravitational Waves and Cosmology, West Virginia University（西弗吉尼亚大学引力波与宇宙学中心）；Jodrell Bank Center for Astrophysics, University of Manchester（曼彻斯特大学乔德雷尔银行天体物理学中心）；Centre for Astrophysics and Supercomputing, Swinburne University of Technology（斯威本科技大学天体物理学与超级计算中心）；South African Radio Astronomy Observatory（南非射电天文观测台）；INAF – Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；SKA Observatory（平方公里阵列射电望远镜观测台）
A Unified Multi-Band Secular Framework for the Hierarchical Triple PSR J0435+3233 System
Tata Institute of Fundamental Research（塔塔基础研究所）；Indian Institute of Science Education and Research Thiruvananthapuram（特鲁凡得琅印度科学教育与研究学院）；University of Turku（图尔库大学）；Tsinghua University（清华大学）；Chinese Academy of Sciences（中国科学院）
Multipolar Magnetic-Field Inference for PSR J0740+6620 with Neural-Network-Accelerated NICER Pulse-Profile Modeling
Los Alamos National Laboratory（洛斯阿拉莫斯国家实验室）；Florida State University（佛罗里达州立大学）；NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心）；Hamburger Sternwarte, Universität Hamburg（汉堡天文台，汉堡大学）；Max Planck Institute for Astrophysics（马克斯·普朗克天体物理学研究所）
