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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 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.

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Authors and contacts

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)

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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

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Vol. 72, Issue 4 - 2023-02-20

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