X-Ray Characterization of the Pulsar PSR J1849-0001 and Its Wind Nebula G32.64+0.53 Associated with TeV Sources Detected by HESS, HAWC, Tibet ASγ, and LHAASO

被引：4
作者：
Kim, Chanho [1 ]
Park, Jaegeun [1 ]
Woo, Jooyun [2 ]
Silverman, Sarah [2 ]
An, Hongjun [1 ]
Bamba, Aya [3 ,4 ,5 ]
Mori, Kaya [2 ]
Reynolds, Stephen P. [6 ]
Safi-Harb, Samar [7 ]
机构：
[1] Chungbuk Natl Univ, Dept Astron & Space Sci, Cheongju 28644, South Korea
[2] Columbia Astrophys Lab, 550 West 120th St, New York, NY 10027 USA
[3] Univ Tokyo, Grad Sch Sci, Dept Phys, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan
[4] Univ Tokyo, Sch Sci, Res Ctr Early Universe, 7-3-1 Hongo,Bunkyo Ku, Tokyo 1130033, Japan
[5] Univ Tokyo, Trans Scale Quantum Sci Inst, Tokyo 1130033, Japan
[6] NC State Univ, Phys Dept, Raleigh, NC 27695 USA
[7] Univ Manitoba, Dept Phys & Astron, Winnipeg, MB R3T 2N2, Canada
来源：
ASTROPHYSICAL JOURNAL | 2024年 / 960卷 / 01期
基金：
日本学术振兴会; 新加坡国家研究基金会;
关键词：
CRAB-NEBULA; PARTICLE-ACCELERATION; NUSTAR; SPECTROSCOPY; CONSTRAINTS; TELESCOPE; EVOLUTION; EMISSION; SPECTRA; CATALOG;
D O I：
10.3847/1538-4357/ad0ecd
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We report on the X-ray emission properties of the pulsar PSR J1849-0001 and its wind nebula (PWN), as measured by Chandra, XMM-Newton, NICER, Swift, and NuSTAR. In the X-ray data, we detected the 38 ms pulsations of the pulsar up to similar to 60 keV with high significance. Additionally, we found that the pulsar's on-pulse spectral energy distribution displays significant curvature, peaking at approximate to 60 keV. Comparing the phase-averaged and on-pulse spectra of the pulsar, we found that the pulsar's off-pulse emission exhibits a spectral shape that is very similar to its on-pulse emission. This characterization of the off-pulse emission enabled us to measure the >10 keV spectrum of the faint and extended PWN using NuSTAR's off-pulse data. We measured both the X-ray spectrum and the radial profiles of the PWN's brightness and photon index, and we combined these X-ray measurements with published TeV results. We then employed a multizone emission scenario to model the broadband data. The results of the modeling suggest that the magnetic field within the PWN is relatively low (approximate to 7 mu G) and that electrons are accelerated to energies greater than or similar to 400 TeV within this PWN. The electrons responsible for the TeV emission outside the X-ray PWN may propagate to similar to 30 pc from the pulsar in similar to 10 kyr.
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页数：12
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