Observation of Gamma Rays up to 320 TeV from the Middle-aged TeV Pulsar Wind Nebula HESS J1849−000
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Published:2023-09-01
Issue:2
Volume:954
Page:200
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ISSN:0004-637X
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Container-title:The Astrophysical Journal
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language:
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Short-container-title:ApJ
Author:
Amenomori M., Asano S., Bao Y. W., Bi X. J., Chen D., Chen T. L., Chen W. Y., Chen Xu, Chen Y., Cirennima , Cui S. W., Danzengluobu , Ding L. K., Fang J. H., Fang K.ORCID, Feng C. F., Feng Zhaoyang, Feng Z. Y., Gao QiORCID, Gomi A., Gou Q. B., Guo Y. Q.ORCID, Guo Y. Y., Hayashi Y., He H. H., He Z. T., Hibino K., Hotta N., Hu Haibing, Hu H. B., Hu K. Y., Huang J., Jia H. Y., Jiang L., Jiang P., Jin H. B., Kasahara K., Katayose Y., Kato C., Kato S.ORCID, Kawahara I., Kawashima T., Kawata K.ORCID, Kozai M., Kurashige D., Labaciren , Le G. M., Li A. F., Li H. J., Li W. J., Li Y., Lin Y. H., Liu B., Liu C., Liu J. S., Liu L. Y., Liu M. Y., Liu W., Lu H., Meng X. R., Meng Y., Munakata K., Nagaya K., Nakamura Y., Nakazawa Y., Nanjo H., Ning C. C., Nishizawa M., Noguchi R., Ohnishi M., Okukawa S., Ozawa S., Qian X., Qian X. L., Qu X. B., Saito T., Sakakibara Y., Sakata M., Sako T.ORCID, Sako T. K., Sasaki T., Shao J., Shibata M., Shiomi A., Sugimoto H., Takano W., Takita M., Tan Y. H., Tateyama N., Torii S., Tsuchiya H., Udo S., Wang H., Wang S. F., Wang Y. P., Wangdui , Wu H. R., Wu Q., Xu J. L., Xue L., Yang Z., Yao Y. Q., Yin J., Yokoe Y., Yu Y. L., Yuan A. F., Zhai L. M., Zhang H. M., Zhang J. L., Zhang X., Zhang X. Y., Zhang Y., Zhang Yi, Zhang Ying, Zhao S. P., Zhaxisangzhu , Zhou X. X., Zou Y. H.
Abstract
Abstract
Gamma rays from HESS J1849−000, a middle-aged TeV pulsar wind nebula (PWN), are observed by the Tibet air shower array and the muon detector array. The detection significance of gamma rays reaches 4.0σ and 4.4σ levels above 25 TeV and 100 TeV, respectively, in units of the Gaussian standard deviation σ. The energy spectrum measured between 40 TeV < E < 320 TeV for the first time is described with a simple power-law function of
dN
/
dE
=
(
2.86
±
1.44
)
×
10
−
16
(
E
/
40
TeV
)
−
2.24
±
0.41
TeV
−
1
cm
−
2
s
−
1
. The gamma-ray energy spectrum from the sub-TeV (E < 1 TeV) to sub-PeV (100 TeV < E < 1 PeV) ranges, including the results of previous studies, can be modeled with the leptonic scenario, i.e., inverse Compton scattering by high-energy electrons accelerated by the PWN of PSR J1849−0001. On the other hand, the gamma-ray energy spectrum can also be modeled with the hadronic scenario in which gamma rays are generated from the decay of neutral pions produced by collisions between accelerated cosmic-ray protons and the ambient molecular cloud found in the gamma-ray-emitting region. The cutoff energy of cosmic-ray protons E
p,cut is estimated as
log
10
(
E
p
,
cut
/
TeV
)
=
3.73
−
0.66
+
2.98
, suggesting that protons are accelerated up to the PeV energy range. Our study thus proposes that HESS J1849−000 should be further investigated as a new candidate as a Galactic PeV cosmic-ray accelerator, or “PeVatron.”
Funder
MOST ∣ National Key Research and Development Program of China MOST ∣ National Natural Science Foundation of China Grant-in-Aid for Scientific Research Grant-in-Aid for Scientific Research on Priority Areas Grant-in-Aid for international Scientific Research Grant-in-Aid for General Scientific Research Grant-in-Aid for Overseas Scientific Research Grant-in-Aid for Young Scientists JST SPRING
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
5 articles.
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