Prospective study on observations of γ-ray sources in the Galaxy using the HADAR experiment

doi:10.1007/s11467-022-1206-x

Frontiers of Physics

2022, Vol. 17

Issue (6): 64602 https://doi.org/10.1007/s11467-022-1206-x

本期目录

Prospective study on observations of γ-ray sources in the Galaxy using the HADAR experiment

Xiangli Qian^1,², Huiying Sun¹, Tianlu Chen²(

), Danzengluobu², Youliang Feng², Qi Gao², Quanbu Gou³, Yiqing Guo^3,⁴, Hongbo Hu^3,⁴, Mingming Kang⁵, Haijin Li², Cheng Liu³, Maoyuan Liu², Wei Liu³, Bingqiang Qiao³, Xu Wang¹, Zhen Wang⁶, Guangguang Xin⁷, Yuhua Yao⁵, Qiang Yuan⁸, Yi Zhang⁸

¹. School of Intelligent Engineering, Shandong Management University, Jinan 250357, China
². The Key Laboratory of Cosmic Rays (Tibet University), Ministry of Education, Lhasa 850000, China
³. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
⁴. University of Chinese Academy of Sciences, 19 A Yuquan Road, Shijingshan District, Beijing 100049, China
⁵. College of Physics, Sichuan University, Chengdu 610064, China
⁶. Tsung-Dao Lee Institute, Shanghai Jiao Tong University, Shanghai 200240, China
⁷. School of Physics and Technology, Wuhan University, Wuhan 430072, China
⁸. Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, China

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Abstract：

The High Altitude Detection of Astronomical Radiation (HADAR) experiment is a refracting terrestrial telescope array based on the atmospheric Cherenkov imaging technique. It focuses the Cherenkov light emitted by extensive air showers through a large aperture water-lens system for observing very-high-energy γ-rays and cosmic rays. With the advantages of a large field-of-view (FOV) and low energy threshold, the HADAR experiment operates in a large-scale sky scanning mode to observe galactic sources. This study presents the prospects of using the HADAR experiment for the sky survey of TeV γ-ray sources from TeVCat and provids a one-year survey of statistical significance. Results from the simulation show that a total of 23 galactic point sources, including five supernova remnant sources and superbubbles, four pulsar wind nebula sources, and 14 unidentified sources, were detected in the HADAR FOV with a significance greater than 5 standard deviations (σ). The statistical significance for the Crab Nebula during one year of operation reached 346.0 σ and the one-year integral sensitivity of HADAR above 1 TeV was ~1.3%–2.4% of the flux from the Crab Nebula.

Key words： HADAR Galactic sources significance gamma rays

收稿日期: 2022-05-26 出版日期: 2022-10-11

Corresponding Author(s): Tianlu Chen,Yiqing Guo

引用本文:

. [J]. Frontiers of Physics, 2022, 17(6): 64602.
Xiangli Qian, Huiying Sun, Tianlu Chen, Danzengluobu, Youliang Feng, Qi Gao, Quanbu Gou, Yiqing Guo, Hongbo Hu, Mingming Kang, Haijin Li, Cheng Liu, Maoyuan Liu, Wei Liu, Bingqiang Qiao, Xu Wang, Zhen Wang, Guangguang Xin, Yuhua Yao, Qiang Yuan, Yi Zhang. Prospective study on observations of γ-ray sources in the Galaxy using the HADAR experiment. Front. Phys. , 2022, 17(6): 64602.

链接本文:

https://academic.hep.com.cn/fop/CN/10.1007/s11467-022-1206-x
https://academic.hep.com.cn/fop/CN/Y2022/V17/I6/64602

Fig.1

Tab.1

Fig.2

Fig.3

Source	R.A. (°)	Dec. (°)	$J 0$ (TeV⁻¹·cm⁻²·s⁻¹)	$E 0$ (TeV)	$Γ$	Extension (°)	Livetime (hrs)	S( $σ$ )	Ref.

W 49B	287.78	9.16	$3.15 × 10 − 13$	1	3.14	–	195.0	8.6	[7]
HESS J1912+101	288.20	10.15	$3.66 × 10 − 14$	7	2.64	0.7	203.3	20.6	[14]
W 51	290.73	14.19	$2.61 × 10 − 14$	7	2.51	0.9	230.4	8.2	[14]
ARGO J2031+4157	307.80	42.50	$3.50 × 10 − 9$	0.1	2.16	2.0	277.7	23.6	[32]
Cassiopeia A	350.81	58.81	$1.10 × 10 − 11$	0.433	2.40	–	98.7	5.7	[33]

Tab.2

Source	R.A. (°)	Dec. (°)	$J 0$ (TeV⁻¹·cm⁻²·s⁻¹)	$E 0$ (TeV)	$Γ$	Extension (°)	Livetime (hrs)	S( $σ$ )	Ref.

Crab	83.63	22.01	$1.85 × 10 − 13$	7	2.58	−	241.8	346.0	[14]
Geminga	98.12	17.37	$4.87 × 10 − 14$	7	2.23	2.0	230.2	13.7	[14]
TeV J1930+188	292.63	18.87	$1.96 × 10 − 14$	7	2.18	−	255.0	10.5	[34]
2HWC J1953+294	298.26	29.48	$8.30 × 10 − 15$	7	2.78	−	288.6	31.4	[14]

Tab.3

Source	R.A. (°)	Dec. (°)	$J 0$ (TeV⁻¹·cm⁻²·s⁻¹)	$E 0$ (TeV)	$Γ$	Extension (°)	Livetime (hrs)	S( $σ$ )	Ref.

MAGIC J0223+403	35.80	43.01	$1.70 × 10 − 11$	0.3	3.10	–	252.5	13.5	[35]
2HWC J1829+070	277.34	7.03	$8.10 × 10 − 15$	7	2.69	–	173.8	14.4	[14]
2HWC J1852+ $013 ∗$	283.01	1.38	$1.82 × 10 − 14$	7	2.90	–	73.6	36.9	[14]
MAGIC J1857.6+0297	284.40	2.97	$6.10 × 10 − 12$	1	2.39	0.1	112.2	25.5	[36]
2HWC J1902+ $048 ∗$	285.51	4.86	$8.30 × 10 − 15$	7	3.22	–	145.7	82.1	[14]
2HWC J1907+ $084 ∗$	286.79	8.50	$7.30 × 10 − 15$	7	3.25	–	189.4	102.5	[14]
MGRO J1908+06	286.98	6.27	$8.51 × 10 − 14$	7	2.33	0.8	164.6	12.4	[14]
2HWC J1914+ $117 ∗$	288.68	11.72	$8.50 × 10 − 15$	7	2.83	–	215.3	29.1	[14]
2HWC J1921+131	290.30	13.13	$7.90 × 10 − 15$	7	2.75	–	223.8	21.5	[14]
2HWC J1928+177	292.15	17.78	$1.07 × 10 − 14$	7	2.60	–	249.9	19.8	[37]
2HWC J1938+238	294.74	23.81	$7.40 × 10 − 15$	7	2.96	–	274.7	51.9	[14]
2HWC J1955+285	298.83	28.59	$5.70 × 10 − 15$	7	2.40	–	286.7	7.3	[14]
2HWC J2006+341	301.55	34.18	$9.60 × 10 − 15$	7	2.64	–	292.0	42.7	[14]
VER J2019+407	305.02	40.76	$1.50 × 10 − 12$	1	2.37	0.23	284.3	14.9	[38]

Tab.4

Fig.4

Fig.5

Tab.5

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