HADAR实验对活动星系核伽马射线辐射观测的预期研究

钱祥利; 孙惠英; 陈天禄; 单增罗布; 冯有亮; 高启; 苟全补; 郭义庆; 胡红波; 康明铭; 厉海金; 刘成; 刘茂元; 刘伟; 乔冰强; 王旭; 王振; 辛广广; 姚玉华; 袁强; 张毅

doi:10.7498/aps.72.20221976

摘要

HADAR (High Altitude Detection of Astronomical Radiation)是一个基于大气切伦科夫成像技术的地面望远镜阵列, 其采用大口径折射式水透镜系统来收集大气切伦科夫光, 以实现对10 GeV—10 TeV能量段的伽马射线和宇宙线的探测. HADAR具有低阈能和大视场的优势, 因此可以对天区进行连续扫描和观测, 在观测活动星系核(Active Galactic Nuclei, AGN)等银河系外伽马射线源方面具有明显优势. 本文研究了HADAR实验对AGN的探测能力. 基于费米望远镜(Fermi Large Area Telescope, Fermi-LAT)的AGN源能谱信息, 将观测能量外推至甚高能能段, 同时加入河外背景光的吸收效应, 以计算HADAR对AGN源观测的统计显著性. 研究结果显示, HADAR运行一年时间, 预计将有31个Fermi-LAT AGN源以高于5倍显著性被观测到, 其中大部分为蝎虎状天体类型.

关键词:

Abstract

The High Altitude Detection of Astronomical Radiation (HADAR) experiment is a refracting terrestrial telescope array based on the atmospheric Cherenkov imaging technique. It is a hybrid array consisting of four water-lens telescopes and a surrounding scintillation detector array for observing Cherenkov light induced by 10 GeV–10 TeV cosmic rays and gamma rays in the atmosphere. The water-lens telescope mainly consists of a hemispherical lens with a diameter of 5 m acting as a Cherenkov light collector, a cylindrical metal tank with a 4 m radius and 7 m height, and an imaging system at the bottom of the tank. The sky region covered by HADAR is much larger than the current generation of Imaging Atmospheric Cherenkov Telescopes, and even the CTA. The field-of-view (FOV) of HADAR can reach up to 60 degrees. The HADAR experiment possesses the advantages of a large field-of-view and low energy threshold, so it can continuously scan wide portions of the sky and easily observe extragalactic gamma-ray sources. The majority of the extragalactic gamma-ray sources detected at very high energy (VHE) energies are active galactic nuclei (AGNs). In this study, we present the potential of using the HADAR experiment for detecting AGN. Based on the AGN catalog sources of the Fermi Large Area Telescope (Fermi-LAT), the observed energy is extrapolated to the VHE range. The VHE gamma rays propagating over cosmological distances can interact with the low-energy of the extragalactic background light (EBL) and produce electron-positron pairs. Therefore, we consider the absorption effects of different EBL models when calculating the expected gamma ray spectra of the AGN sample. We select the sample with redshift measurements and locations inside the FOV of HADAR from 4LAC catalog. In total, there are 375 BL Lacertae objects (BL Lacs) and 289 flat-spectrum radio quasars (FSRQs) satisfying the selection conditions. The integral gamma ray spectra are derived and compared with the sensitivity curve of HADAR, the number of sources with fluxes above the sensitivity of HADAR is counted. Further, we calculate the statistical significance of HADAR for AGN source observation based on the equi-zenith angle sky scanning analysis method. The simulation results reveal that a total of 31 sources of Fermi-LAT AGN can be detected by HADAR with a significance greater than five standard deviations over a one-year survey period, most of which are BL Lacs.

Keywords:

作者及机构信息

1.
山东管理学院智能工程学院, 济南　250357

2.
西藏大学宇宙线教育部重点实验室, 拉萨　850000

3.
中国科学院高能物理研究所粒子天体物理中心, 北京　100049

4.
中国科学院大学, 北京　100049

5.
四川大学物理学院, 成都　610064

6.
上海交通大学李政道研究所, 上海　200240

7.
苏州空天信息研究院, 苏州　215000

8.
重庆大学物理学院, 重庆　401331

9.
中国科学院紫金山天文台暗物质与空间天文重点实验室, 南京　210023

通信作者: 陈天禄, chentl@ihep.ac.cn ; 郭义庆, guoyq@ihep.ac.cn ;

基金项目: 国家自然科学基金(批准号: 12263005, 11873005, 11705103, 12005120, 12147218, U1831208, U1632104, 11875264, U2031110)和西藏大学宇宙线教育部重点实验室开放基金(批准号: KLCR-202201)资助的课题

Authors and contacts

1.
School of Intelligent Engineering, Shandong Management University, Jinan 250357, China

2.
Key Laboratory of Cosmic Rays, Ministry of Education, Tibet University, 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, 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.
Suzhou Aerospace Information Research Institute, Suzhou 215000, China

8.
College of Physics, Chongqing University, Chongqing 401331, China

9.
Key Laboratory of Dark Matter and Space Astronomy, Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210023, China

Corresponding author: Chen Tian-Lu, chentl@ihep.ac.cn ; Guo Yi-Qing, guoyq@ihep.ac.cn ;

Funds: Project supported by the National Natural Science Foundation of China (Grant Nos. 12263005, 11873005, 11705103, 12005120, 12147218, U1831208, U1632104, 11875264, U2031110) and the Key Laboratory for Cosmic Ray of the Education Ministry of China, Tibet University (Grant No. KLCR-202201)

文章全文 : translate this paragraph

参考文献

[1]	Aharonian F, Akhperjanian A G, Bazer-Bachi A R 2007 Astrophys. J. 664 L71 Google Scholar
[2]	Albert J, Aliu E, Anderhub H 2007 Astrophys. J. 669 862 Google Scholar
[3]	Sikora M, Begelman M C, Rees M J 1994 Astrophys. J. 421 153 Google Scholar
[4]	Marscher A P 2016 Galaxies. 4 37 Google Scholar
[5]	Aharonian F 2000 New. Astron. 5 377 Google Scholar
[6]	Mücke A, Protheroe R J, Engel R, Rachen J P, Stanev T 2003 Astropart. Phys. 18 593 Google Scholar
[7]	Fossati G, Maraschi L, Celotti A, Comastri A, Ghisellini G 1998 Mon. Not. R. Astron. Soc. 299 433 Google Scholar
[8]	Ghisellini G, Righi C, Costamante L, Tavecchio F 2017 Mon. Not. R. Astron. Soc. 469 255 Google Scholar
[9]	Padovani P, Giommi P 1995 Mon. Not. R. Astron. Soc. 277 1477 Google Scholar
[10]	Ajello M, Arimoto M, Axelsson M 2019 Astrophys. J. 878 52 Google Scholar
[11]	Hinton J A 2004 New. Astron. Rev. 48 331 Google Scholar
[12]	Aleksić J, Ansoldi S, Antonelli L A 2016 Astropart. Phys. 72 61 Google Scholar
[13]	Weekes T C, Badran H, Biller S D 2002 Astropart. Phys. 17 221 Google Scholar
[14]	Abeysekara A U, Alfaro R, Alvarez C 2013 Astropart. Phys. 50 26 Google Scholar
[15]	Sciascio G D 2016 Nucl. Part. Phys. P. 279 166 Google Scholar
[16]	CTA Consortium 2018 Science with the Cherenkov Telescope Array (Singapore: World Scientific) pp11–26
[17]	Punch M, Akerlof C W, Cawley M F 1992 Nature 358 477 Google Scholar
[18]	Quinn J, Akerlof C W, Biller S 1996 Astrophys. J. 456 L83 Google Scholar
[19]	Albert J, Aliu E, Anderhub H 2008 Science 320 1752 Google Scholar
[20]	Aliu E, Archambault S, Arlen T 2012 Astrophys. J. 750 94 Google Scholar
[21]	Abramowski A, Acero F, Aharonian F 2012 Astron. Astrophys. 538 A103 Google Scholar
[22]	Abramowski A, Acero F, Aharonian F 2013 Mon. Not. R. Astron. Soc. 434 1889 Google Scholar
[23]	Abdo A A, Ackermann M, Ajello M 2011 Astrophys. J. 736 131 Google Scholar
[24]	Ahnen M L, Ansoldi S, Antonelli L A 2017 Astron. Astrophys. 603 A31 Google Scholar
[25]	Abdalla H, Adam R, Aharonian F 2021 Astron. Astrophys. 648 A23 Google Scholar
[26]	Arlen T, Aune T, Beilicke M 2012 Astrophys. J. 762 92 Google Scholar
[27]	Abdo A A, Ackermann M, Ajello M 2011 Astrophys. J. 727 129 Google Scholar
[28]	Bartoli B, Bernardini P, Bi X J 2012 Astrophys. J. 758 2 Google Scholar
[29]	Albert J, Aliu E, Anderhub H 2007 Astrophys. J. 667 358 Google Scholar
[30]	Gilmore R C, Madau P, Primack J R, Somerville R S, Haardt F 2009 Mon. Not. R. Astron. Soc. 399 1694 Google Scholar
[31]	Inoue S, Salvaterra R, Choudhury T R, Ferrara A, Ciardi B, Schneider R 2010 Mon. Not. R. Astron. Soc. 404 1938 Google Scholar
[32]	Takahashi K, Inoue S, Ichiki K, Nakamura T 2011 Mon. Not. R. Astron. Soc. 410 2741 Google Scholar
[33]	Wang Z, Guo Y Q, Cai H 2018 Exp. Astron. 45 363 Google Scholar
[34]	Xin G G, Yao Y H, Qian X L 2021 Astrophys. J. 923 112 Google Scholar
[35]	Holler M, Balzer A, Chalmé-Calvet R, de Naurois M, and Zaborov D 2015 Proceedings of the 34th International Cosmic Ray Conference, Hague, Netherlands, 30 July–6 August 2015 34 980
[36]	Aleksić J, Ansoldi S, Antonelli L A 2016 Astropart. Phys. 72 76 Google Scholar
[37]	Ma X H, Bi Y J, Cao Z 2022 Chinese Phys. C 46 030001 Google Scholar
[38]	DeYoung T 2012 Nucl. Instrum. Meth. A 692 72 Google Scholar
[39]	Zhao Y, Yuan Q, Bi X J, Zhu F R, Jia H Y 2016 Int. J. Mod. Phys. D 25 1650006 Google Scholar
[40]	Cai H, Zhang Y, Liu C 2017 J. Instrum. 12 09023 Google Scholar
[41]	Chen T L, Liu C, Gao Q 2019 Nucl. Instrum. Meth. A 927 46 Google Scholar
[42]	Ajello M, Angioni R, Axelsson M 2020 Astrophys. J. 892 105 Google Scholar
[43]	Stecker F W, De Jager O C, Salamon M H 1992 Astrophys. J. 390 L49 Google Scholar
[44]	Franceschini A, Rodighiero G, Vaccari M 2008 Astron. Astrophys. 487 837 Google Scholar
[45]	Finke J D, Razzaque S, Dermer C D 2010 Astrophys. J. 712 238 Google Scholar
[46]	Domínguez A, Primack J R, Rosario D J 2011 Mon. Not. R. Astron. Soc. 410 2556 Google Scholar
[47]	Gilmore R C, Somerville R S, Primack J R, Domínguez A 2012 Mon. Not. R. Astron. Soc. 422 3189 Google Scholar
[48]	Helgason K, Kashlinsky A 2012 Astrophys. J. Lett. 758 L13 Google Scholar
[49]	Inoue Y, Inoue S, Kobayashi M A R, Makiya R, Niino Y, Totani T 2013 Astrophys. J. 768 197 Google Scholar
[50]	Stecker F W, Scully S T, Malkan M A 2016 Astrophys. J. 827 6 Google Scholar
[51]	Abdollahi S, Acero F, Ackermann M 2020 Astrophys. J. Suppl. S. 247 33 Google Scholar
[52]	Amenomori M, Ayabe S, Chen D 2005 Astrophys. J. 633 1005 Google Scholar
[53]	Gaisser T K, Stanev T, Tilav S 2013 Front. Phys. 8 748 Google Scholar

施引文献

图 1 HADAR阵列示意图　(a)阵列分布图; (b)单个水透镜详细结构图^[34]

Fig. 1. Schematic of HADAR: (a) Layout of the HADAR experiment; (b) detailed design of a water-lens telescope^[34]

下载: 全尺寸图片幻灯片

图 2 HADAR实验的角分辨, 入射事例的天顶角分别为10°, 20°和30°^[34]

Fig. 2. Performance of HADAR angular resolution. The incident zenith angles are 10°, 20° and 30°^[34]

下载: 全尺寸图片幻灯片

图 3 HADAR实验的有效面积　(a)不同天顶角伽马事例入射时的有效面积及与其他实验的比较; (b)实验的有效孔径

Fig. 3. Performance of HADAR effective area: (a) Effective areas for incident γ-ray events at different zenith angles and comparison with other IACT and EAS experiments; (b) acceptance for HADAR and other experiments

下载: 全尺寸图片幻灯片

图 4 HADAR及其他伽马射线实验的灵敏度曲线对比图

Fig. 4. Comparisons of the sensitivity of HADAR with other γ-ray instruments

下载: 全尺寸图片幻灯片

图 5 筛选出的664个AGN源的能谱指数分布图(左)与红移分布图(右)

Fig. 5. Distribution of photon index (left) and redshift (right) for 664 selected AGN sources

下载: 全尺寸图片幻灯片

图 6 预期的经过5种不同EBL模型吸收之后的AGN源的伽马射线能谱图及与HADAR灵敏度曲线的比较. 其中蓝色实线为BL Lacs, 红色虚线为FSRQs, 黑色粗线为HADAR的灵敏度曲线

Fig. 6. Expected γ-ray spectra of the AGN sample after EBL absorption. Different panels are for the five different EBL models as labeled. The blue solid lines represent BL Lacs and red dashed lines represent FSRQs. The sensitivity of HADAR is shown with the thick black line

下载: 全尺寸图片幻灯片

图 7 赤道坐标系(J2000 坐标)下HADAR对河外源的观测显著性预期, 显著性显示范围为–3—15

Fig. 7. Expected significance of extragalactic sources in the equatorial coordinates (J2000 epoch) in the HADAR FOV. The visualization range is limited between –3 and 15

下载: 全尺寸图片幻灯片

表 1 HADAR实验一年观测时间对河外源观测的显著性估计, 列表从左到右依次为: Fermi源名称, 相关联的源, 赤经, 赤纬, 红移, 归一化的流强, $ E_0 $, 谱指数α, 谱指数β, 一年内的有效观测时间, 预期显著性

Table 1. Expected significance of extragalactic sources with HADAR between 30 GeV and 10 TeV using a 1 yr observation time. Columns from left to right are as follows: Fermi source name, associations, R.A., Dec., redshift, normalization flux, $ E_0 $, spectral index α, spectral index β, effective livetime, expected significance by HADAR

Fermi Source	Assoc.	R.A./(°)	Dec./(°)	z	$N_0/(\rm TeV^{-1}{\cdot}cm^{-2}{\cdot}s^{-1})$	$ E_0 $/GeV	α	β	Livetime/hrs	S/σ
4FGL J0112.1+2245	S2 0109+22	18.03	22.75	0.265	1.399× 10^–5	0.76	1.99	0.057	277.8	8.9
4FGL J0222.6+4302	3C66A	35.67	43.04	0.444	1.008×10^–5	1.21	1.88	0.045	264.2	21.5
4FGL J0319.8+1845	1E 0317.0+1835	49.97	18.75	0.190	1.618×10^–8	5.98	1.67	0.0	257.8	5.1
4FGL J0650.7+2503	1ES 0647+250	102.70	25.05	0.203	6.587×10^–7	2.06	1.66	0.035	286.0	25.3
4FGL J0738.1+1742	PKS 0735+17	114.54	17.71	0.424	2.640×10^–6	1.54	1.97	0.065	251.3	7.4
4FGL J0809.8+5218	1ES 0806+524	122.46	52.31	0.138	2.222×10^–6	1.30	1.80	0.041	193.9	15.1
4FGL J0915.9+2933	Ton 0396	138.99	29.55	0.190	1.068×10^–6	1.35	1.74	0.083	294.7	7.8
4FGL J1015.0+4926	1H 1013+498	153.77	49.43	0.212	7.019×10^–6	1.01	1.76	0.041	220.0	29.9
4FGL J1058.6+5627	TXS 1055+567	164.67	56.46	0.143	2.525×10^–6	1.06	1.87	0.040	149.4	6.3
4FGL J1104.4+3812	Mkn 421	166.12	38.21	0.030	1.842×10^–5	1.29	1.72	0.023	284.9	529.6
4FGL J1117.0+2013	RBS 0958	169.27	20.23	0.139	4.167×10^–7	1.84	1.95	0.0	266.1	5.7
4FGL J1150.6+4154	RBS 1040	177.66	41.91	0.320	5.965×10^–7	1.73	1.65	0.091	270.0	6.6
4FGL J1217.9+3007	B2 1215+30	184.48	30.12	0.130	7.113×10^–6	1.07	1.88	0.040	295.1	31.6
4FGL J1221.3+3010	PG 1218+304	185.34	30.17	0.184	1.742×10^–7	4.44	1.71	0.0	295.2	31.3
4FGL J1221.5+2814	W Comae	185.38	28.24	0.102	3.516×10^–6	1.06	2.16	0.0	293.1	6.6
4FGL J1224.4+2436	MS 1221.8+2452	186.12	24.61	0.219	2.417×10^–7	2.36	1.89	0.0	284.6	5.5
4FGL J1224.9+2122	4C +21.35	186.23	21.38	0.434	2.187×10^–4	0.39	2.27	0.045	271.8	5.4
4FGL J1230.2+2517	ON 246	187.56	25.30	0.135	6.100×10^–6	0.82	1.99	0.061	286.7	6.0
4FGL J1231.7+2847	B2 1229+29	187.93	28.79	0.236	7.991×10^–7	1.58	1.99	0.0	293.9	5.1
4FGL J1427.0+2348	PKS 1424+240	216.76	23.80	0.604	6.508×10^–6	1.23	1.70	0.060	281.8	23.8
4FGL J1428.5+4240	H 1426+428	217.13	42.68	0.129	2.772×10^–8	5.02	1.66	0.0	266.1	9.7
4FGL J1555.7+1111	PG 1553+113	238.93	11.19	0.360	3.325×10^–6	1.85	1.54	0.070	199.5	58.9
4FGL J1653.8+3945	Mkn 501	253.47	39.76	0.033	4.439×10^–6	1.48	1.71	0.018	279.5	258.4
4FGL J1725.0+1152	1H 1720+117	261.27	11.87	0.180	7.214×10^–7	2.22	1.76	0.056	205.9	13.9
4FGL J1728.3+5013	I Zw 187	262.08	50.23	0.055	1.950×10^–7	3.01	1.78	0.0	213.2	24.1
4FGL J1838.8+4802	GB6J1838+4802	279.71	48.04	0.300	3.198×10^–7	2.55	1.85	0.0	231.3	6.1
4FGL J2116.2+3339	B2 2114+33	319.06	33.66	0.350	1.068×10^–6	1.71	1.74	0.102	294.4	7.2
4FGL J2202.7+4216	BL Lac	330.69	42.28	0.069	4.498×10^–5	0.75	2.18	0.060	268.2	15.0
4FGL J2250.0+3825	B3 2247+381	342.51	38.42	0.119	2.881×10^–8	5.33	1.72	0.060	284.2	9.9
4FGL J2253.9+1609	3C 454.3	343.50	16.15	0.859	6.408×10^–4	0.52	2.39	0.0	240.7	14.7
4FGL J2323.8+4210	1ES 2321+419	350.97	42.18	0.059	2.926×10^–7	2.47	1.90	0.0	268.7	13.4

下载: 导出CSV

[1]	Aharonian F, Akhperjanian A G, Bazer-Bachi A R 2007 Astrophys. J. 664 L71 Google Scholar
[2]	Albert J, Aliu E, Anderhub H 2007 Astrophys. J. 669 862 Google Scholar
[3]	Sikora M, Begelman M C, Rees M J 1994 Astrophys. J. 421 153 Google Scholar
[4]	Marscher A P 2016 Galaxies. 4 37 Google Scholar
[5]	Aharonian F 2000 New. Astron. 5 377 Google Scholar
[6]	Mücke A, Protheroe R J, Engel R, Rachen J P, Stanev T 2003 Astropart. Phys. 18 593 Google Scholar
[7]	Fossati G, Maraschi L, Celotti A, Comastri A, Ghisellini G 1998 Mon. Not. R. Astron. Soc. 299 433 Google Scholar
[8]	Ghisellini G, Righi C, Costamante L, Tavecchio F 2017 Mon. Not. R. Astron. Soc. 469 255 Google Scholar
[9]	Padovani P, Giommi P 1995 Mon. Not. R. Astron. Soc. 277 1477 Google Scholar
[10]	Ajello M, Arimoto M, Axelsson M 2019 Astrophys. J. 878 52 Google Scholar
[11]	Hinton J A 2004 New. Astron. Rev. 48 331 Google Scholar
[12]	Aleksić J, Ansoldi S, Antonelli L A 2016 Astropart. Phys. 72 61 Google Scholar
[13]	Weekes T C, Badran H, Biller S D 2002 Astropart. Phys. 17 221 Google Scholar
[14]	Abeysekara A U, Alfaro R, Alvarez C 2013 Astropart. Phys. 50 26 Google Scholar
[15]	Sciascio G D 2016 Nucl. Part. Phys. P. 279 166 Google Scholar
[16]	CTA Consortium 2018 Science with the Cherenkov Telescope Array (Singapore: World Scientific) pp11–26
[17]	Punch M, Akerlof C W, Cawley M F 1992 Nature 358 477 Google Scholar
[18]	Quinn J, Akerlof C W, Biller S 1996 Astrophys. J. 456 L83 Google Scholar
[19]	Albert J, Aliu E, Anderhub H 2008 Science 320 1752 Google Scholar
[20]	Aliu E, Archambault S, Arlen T 2012 Astrophys. J. 750 94 Google Scholar
[21]	Abramowski A, Acero F, Aharonian F 2012 Astron. Astrophys. 538 A103 Google Scholar
[22]	Abramowski A, Acero F, Aharonian F 2013 Mon. Not. R. Astron. Soc. 434 1889 Google Scholar
[23]	Abdo A A, Ackermann M, Ajello M 2011 Astrophys. J. 736 131 Google Scholar
[24]	Ahnen M L, Ansoldi S, Antonelli L A 2017 Astron. Astrophys. 603 A31 Google Scholar
[25]	Abdalla H, Adam R, Aharonian F 2021 Astron. Astrophys. 648 A23 Google Scholar
[26]	Arlen T, Aune T, Beilicke M 2012 Astrophys. J. 762 92 Google Scholar
[27]	Abdo A A, Ackermann M, Ajello M 2011 Astrophys. J. 727 129 Google Scholar
[28]	Bartoli B, Bernardini P, Bi X J 2012 Astrophys. J. 758 2 Google Scholar
[29]	Albert J, Aliu E, Anderhub H 2007 Astrophys. J. 667 358 Google Scholar
[30]	Gilmore R C, Madau P, Primack J R, Somerville R S, Haardt F 2009 Mon. Not. R. Astron. Soc. 399 1694 Google Scholar
[31]	Inoue S, Salvaterra R, Choudhury T R, Ferrara A, Ciardi B, Schneider R 2010 Mon. Not. R. Astron. Soc. 404 1938 Google Scholar
[32]	Takahashi K, Inoue S, Ichiki K, Nakamura T 2011 Mon. Not. R. Astron. Soc. 410 2741 Google Scholar
[33]	Wang Z, Guo Y Q, Cai H 2018 Exp. Astron. 45 363 Google Scholar
[34]	Xin G G, Yao Y H, Qian X L 2021 Astrophys. J. 923 112 Google Scholar
[35]	Holler M, Balzer A, Chalmé-Calvet R, de Naurois M, and Zaborov D 2015 Proceedings of the 34th International Cosmic Ray Conference, Hague, Netherlands, 30 July–6 August 2015 34 980
[36]	Aleksić J, Ansoldi S, Antonelli L A 2016 Astropart. Phys. 72 76 Google Scholar
[37]	Ma X H, Bi Y J, Cao Z 2022 Chinese Phys. C 46 030001 Google Scholar
[38]	DeYoung T 2012 Nucl. Instrum. Meth. A 692 72 Google Scholar
[39]	Zhao Y, Yuan Q, Bi X J, Zhu F R, Jia H Y 2016 Int. J. Mod. Phys. D 25 1650006 Google Scholar
[40]	Cai H, Zhang Y, Liu C 2017 J. Instrum. 12 09023 Google Scholar
[41]	Chen T L, Liu C, Gao Q 2019 Nucl. Instrum. Meth. A 927 46 Google Scholar
[42]	Ajello M, Angioni R, Axelsson M 2020 Astrophys. J. 892 105 Google Scholar
[43]	Stecker F W, De Jager O C, Salamon M H 1992 Astrophys. J. 390 L49 Google Scholar
[44]	Franceschini A, Rodighiero G, Vaccari M 2008 Astron. Astrophys. 487 837 Google Scholar
[45]	Finke J D, Razzaque S, Dermer C D 2010 Astrophys. J. 712 238 Google Scholar
[46]	Domínguez A, Primack J R, Rosario D J 2011 Mon. Not. R. Astron. Soc. 410 2556 Google Scholar
[47]	Gilmore R C, Somerville R S, Primack J R, Domínguez A 2012 Mon. Not. R. Astron. Soc. 422 3189 Google Scholar
[48]	Helgason K, Kashlinsky A 2012 Astrophys. J. Lett. 758 L13 Google Scholar
[49]	Inoue Y, Inoue S, Kobayashi M A R, Makiya R, Niino Y, Totani T 2013 Astrophys. J. 768 197 Google Scholar
[50]	Stecker F W, Scully S T, Malkan M A 2016 Astrophys. J. 827 6 Google Scholar
[51]	Abdollahi S, Acero F, Ackermann M 2020 Astrophys. J. Suppl. S. 247 33 Google Scholar
[52]	Amenomori M, Ayabe S, Chen D 2005 Astrophys. J. 633 1005 Google Scholar
[53]	Gaisser T K, Stanev T, Tilav S 2013 Front. Phys. 8 748 Google Scholar

[1]	孙惠英, 钱祥利, 陈天禄, 单增罗布, 冯有亮, 高启, 苟全补, 郭义庆, 胡红波, 康明铭, 厉海金, 刘成, 刘茂元, 刘伟, 乔冰强, 王旭, 王振, 辛广广, 姚玉华, 袁强, 张毅. HADAR实验对Fermi-LAT伽马射线源观测的预期研究. 物理学报, 2023, 72(19): 199501. doi: 10.7498/aps.72.20230977
[2]	黎丽, 赵志国, 古华光. 兴奋性和抑制性自反馈压制靠近Hopf分岔的神经电活动比较. 物理学报, 2022, 71(5): 050504. doi: 10.7498/aps.71.20211829
[3]	丁学利, 贾冰, 李玉叶. 利用相位响应曲线解释抑制性反馈增强神经电活动. 物理学报, 2019, 68(18): 180502. doi: 10.7498/aps.68.20190197
[4]	董磊, 卢振武, 刘欣悦, 李正炜. 三种降采样成像策略的性能优化以及与传统傅里叶望远镜的比较. 物理学报, 2019, 68(7): 074203. doi: 10.7498/aps.68.20181801
[5]	朱玥, 张子良, 杨彦佶, 薛荣峰, 崔苇苇, 陆波, 王娟, 陈田祥, 王于仨, 李炜, 韩大炜, 霍嘉, 胡渭, 李茂顺, 张艺, 祝宇轩, 刘苗, 赵晓帆, 陈勇. 硬X射线调制望远镜低能探测器量子效率标定. 物理学报, 2017, 66(11): 112901. doi: 10.7498/aps.66.112901
[6]	方志明, 崔荣一, 金璟璇. 基于生物视觉特征和视觉心理学的视频显著性检测算法. 物理学报, 2017, 66(10): 109501. doi: 10.7498/aps.66.109501
[7]	颜召军, 陈欣扬, 郑立新, 丁媛媛, 朱能鸿. 基于色散干涉图像的拼接望远镜共相零位标定方法研究. 物理学报, 2016, 65(19): 199501. doi: 10.7498/aps.65.199501
[8]	于树海, 董磊, 刘欣悦, 凌剑勇. 傅里叶望远镜重构图像虚像分析. 物理学报, 2015, 64(18): 184205. doi: 10.7498/aps.64.184205
[9]	颜召军, 陈欣扬, 杨朋千, 周丹, 郑立新, 朱能鸿. 基于光栅色散干涉条纹的菲佐光干涉望远镜共相检测方法研究. 物理学报, 2015, 64(14): 149501. doi: 10.7498/aps.64.149501
[10]	廖宏宇, 马晓燠, 郭友明, 饶长辉, 魏凯. 基于AR模型搜索迭代算法的望远镜跟踪误差分析. 物理学报, 2014, 63(17): 179501. doi: 10.7498/aps.63.179501
[11]	金左轮, 韩静, 张毅, 柏连发. 基于纹理显著性的微光图像目标检测. 物理学报, 2014, 63(6): 069501. doi: 10.7498/aps.63.069501
[12]	王萍, 潘跃. 基于显著性特征的大冰雹识别模型. 物理学报, 2013, 62(6): 069202. doi: 10.7498/aps.62.069202
[13]	董富通, 王菲鹿, 仲佳勇, 赵刚. Fe离子M壳层不可分辨跃迁系不透明度研究. 物理学报, 2012, 61(16): 163201. doi: 10.7498/aps.61.163201
[14]	赵保银, 吕百达. 使用离焦望远镜系统合成轴上平顶光束的一种新方法. 物理学报, 2008, 57(5): 2919-2924. doi: 10.7498/aps.57.2919
[15]	王斌, 唐昌建, 刘濮鲲. 离子通道中相对论电子注的切连科夫辐射. 物理学报, 2006, 55(11): 5953-5958. doi: 10.7498/aps.55.5953
[16]	韩英魁, 王清月, 张志刚, 张伟力, 柴路, 袁晓东, 黄小军. 飞秒啁啾脉冲放大系统中折叠反射式望远镜对脉冲波前的影响. 物理学报, 2005, 54(4): 1613-1618. doi: 10.7498/aps.54.1613
[17]	徐光, 钱列加, 王韬, 朱鹤元, 范滇元. 用于超短脉冲扩展的时间望远镜. 物理学报, 2004, 53(1): 93-98. doi: 10.7498/aps.53.93
[18]	吴坚强, 刘盛纲, 莫元龙. 未磁化等离子体介质切连科夫脉塞的线性理论. 物理学报, 1997, 46(2): 324-331. doi: 10.7498/aps.46.324
[19]	张毅波. 切伦科夫自由电子激光中自发辐射与受激辐射的关系. 物理学报, 1987, 36(10): 1344-1348. doi: 10.7498/aps.36.1344
[20]	《解放军报》. 毛泽东思想是我们革命事业的望远镜和显微镜. 物理学报, 1966, 22(8): 855-858. doi: 10.7498/aps.22.855

计量

文章访问数: 5236
PDF下载量: 154
被引次数: 0

姓名
邮箱
手机号码
标题
留言内容
验证码

搜索

留言板