Study of the Diffuse Gamma-Ray Emission From the Galactic Plane With Argo-Ybj

Bartoli, B.; Bernardini, P.; Bi, X. J.; Branchini, P.; Budano, A.; Camarri, P.; Cao, Z.; Cardarelli, R.; Catalanotti, S.; Chen, Songzhan; Chen, T. L.; Creti, P.; Cui, S. W.; Dai, B. Z.; D’Amone, A.; Danzengluobu,; Mitri, I. De; Piazzoli, B. D’Ettorre; Girolamo, T. Di; Sciascio, G. Di; Feng, C.; Feng, Z.; Feng, Z. Y.; Gou, Q. B.; Guo, Y. Q.; He, H. H.; Hu, Haibing; Hu, Hongbo; Iacovacci, M.; Iuppa, R.; Jia, H. Y.; Labaciren,; Li, H. J.; Liguori, G.; Liu, C.; Liu, J.; Liu, M. Y.; Lü, H.; L., L.; H., X.; Mancarella, G.; Mari, Stefano Maria; Marsella, G.; Martello, D.; Mastroianni, S.; Montini, P.; Ning, C. C.; Panareo, M.; Perrone, L.; Pistilli, P.; Ruggieri, F.; Salvini, P.; Santonico, R.; Shen, P. R.; Sheng, X. D.; Shi, Fang; Surdo, A.; Tan, Y. H.; Vallania, P.; Vernetto, S.; Vigorito, C.; Wang, H.; Wu, C. Y.; Wu, H. R.; Xue, L.; Yang, Q. Y.; Yang, X. C.; Yao, Z. G.; Yuan, A. F.; Zha, M.; Zhang, H. M.; Zhang, L.; Zhang, X. Y.; Zhang, Y.; Zhao, J. W.; Zhaxiciren,; Zhaxisangzhu,; Zhou, X. X.; Zhu, F. R.; Zhu, Q. Q.; Zizzi, G.

doi:10.1088/0004-637x/806/1/20

Cited by 95 publications

(88 citation statements)

References 84 publications

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“…This phenomenon was detected by Fermi at GeV region and ARGO-YBJ/Milagro at TeV region. The newest results by ARGO-YBJ experiment are consistent with the predictions of the Fermi model for the diffuse Galactic emission [30]. We provide the expectation of LHAASO on diffuse γ-rays in the Galactic region 25 • < l < 100 • , |b| <5 • (Figure 4(a)) and in Cygnus region (Figure 4 (b)).…”

Section: Pos(icrc2015)974supporting

confidence: 84%

Expectation on Observation of Gamma-ray Astronomy with the LHAASO Project

Liu¹,

Cui²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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for the LHAASO CollaborationThe Large High Altitude Air Shower Observatory (LHAASO) project is a new generation EAS array, which will be built in Daocheng, Sichuan province, China at 4400m above sea level. With a wide field-of-view and high duty cycle, LHAASO will survey a large sky region in the declination band from -20 • to 80 • with a sensitivity of 10 mili-Crab per year at a much wider energy range from 100 GeV to 1 PeV. Besides increasing the number of VHE gamma-ray sources, it will also provide accurate spectrum measurement for the known γ-ray sources, especially for extended sources and transient phenomena. These are very important for us to look sight into γ-ray emission mechanism and particle acceleration within the sources. In this paper, we will investigate, basing on detector simulation, the ability of LHAASO on the measurement of spectra of SNRs, Cygnus region, diffuse galactic γ-rays and AGN flares.

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Section: Pos(icrc2015)974supporting

confidence: 84%

Expectation on Observation of Gamma-ray Astronomy with the LHAASO Project

Liu¹,

Cui²

2016

Proceedings of the 34th International Cosmic Ray Conference — PoS(ICRC2015)

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“…The different lines indicate the energy spectra expected from the Fermi-DGE (with index -2.6, which also rules their extensions) in the different sky regions investigated by the detectors (details are given in [9]). Left: region 40…”

Section: Diffuse γ-Rays From the Galactic Planementioning

confidence: 99%

“…The events collected by ARGO-YBJ have been analysed to determine the diffuse γ-ray emission in the Galactic plane at longitudes 25 • < l < 100 • and latitudes |b| < 5 • [9]. This analysis was carried out in the energy range connecting the region explored by Fermi/LAT with that investigated by Milagro.…”

Section: Diffuse γ-Rays From the Galactic Planementioning

confidence: 99%

Recent results inγ-ray astronomy with the ARGO-YBJ detector

Girolamo

2017

EPJ Web Conf.

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Abstract. The ARGO-YBJ air shower detector has been in stable data taking for five years at the YangBaJing Cosmic Ray Laboratory (Tibet, P.R. China, 4300m a.s.l.) with a duty cycle > 86% and an energy threshold of a few hundreds of GeV. With the scaler mode technique, the minimum threshold of 1 GeV can be reached. In this paper recent results in γ-ray astronomy will be presented, including those from 4.5 years of observations of the blazar Mrk 421 in common with the Fermi satellite. The detectorThe ARGO-YBJ experiment is located at Yangbajing (Tibet, P.R. China, 4300 m a.s.l.) and consists of a single layer of Resistive Plate Counters (RPCs) on a total area of about 110 × 100 m 2 . The detector has a modular structure, the basic module being a cluster (5.7 × 7.6 m 2 ), made of 12 RPCs. Each RPC is read by 80 strips (6.75×61.8 cm 2 ) which are the space pixels, logically organized in 10 independent pads (55.6 × 61.8 cm 2 ) which are individually acquired and represent the time pixels of the detector [1]. The detector carpet is connected to two different DAQ systems, which work independently: in shower mode, for each event the location and timing of each detected particle is recorded, allowing the reconstruction of the lateral distribution and of the arrival direction; in scaler mode, the counting rate of each cluster is measured every 0.5 s, with little information on the space distribution and arrival direction of the detected particles. The trigger of the shower mode was N pad ≥ 20 in a time window of 420 ns, with a rate of 3.5 kHz. In the scaler mode, for each cluster four scalers recorded the rate of counts ≥ 1, ≥ 2, ≥ 3 and ≥ 4 in a time window of 150 ns. The corresponding measured rates are, respectively, ∼40 kHz, ∼2 kHz, ∼300 Hz and ∼120 Hz [2]. The experiment has been taking data with its full layout from November 2007 to February 2013. The detector pointing accuracy, angular resolution and absolute energy calibration have been determined studying the deficit in the cosmic ray flux due to the Moon [3]. Sky surveyThe ARGO-YBJ detector surveyed the northern hemisphere, in the declination band from -10 • to 70 • , at energies above 0.3 TeV. With an integrated sensitivity down to 0.24 Crab unit (depending on the declination) after five years of data taking, six sources were detected with a statistical significance S>5 standard deviations (s.d.), and five excesses are reported as potential (S>4 s.d.) γ-ray emitters. The list of excess regions, with their corresponding significances and TeV associations, is in table 1 [4]. In the rest of this section, a selection of results concerning the detected sources will be presented. a

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“…These experiments either measure an intersection of the air shower by particle detectors using water Cherenkov detectors (like Milagro [1] and HAWC [2]) or carpets of particle detectors (like ARGO-YBJ [3]), or work calorimetricly using the atmosphere, as in the case of imaging atmospheric Cherenkov telescopes (IACTs). All in common have large effective areas necessary for the detection of very-high-energy (VHE) γ-rays with their low fluxes and steeply falling spectra.…”

Section: Introductionmentioning

confidence: 99%

“…As a consequence, at TeV energies the sky is no longer dominated by the diffuse emission as observed at MeV energies but rather by the γ-ray sources, and the diffuse γ-ray emission is reduced to a very faint signal. Observations of diffuse γ-ray emission in the VHE regime exist by Milagro [1] at a median energy of 15 TeV, and by ARGO-YBJ [3]. While these experiments can provide the large field of view (and additionally the superior duty cycle) favouring a measurement of large-scale emission, they are limited in their γ-hadron separation possibilities and in their angular resolution, which is a key feature for the discrimination between γ-ray sources and diffuse emission signatures.…”

Section: Introductionmentioning

confidence: 99%

Diffuse Galactic Gamma-ray Emission with H.E.S.S.

Egberts¹

2016

Proceedings of XI Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF15)

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While imaging atmospheric Cherenkov telescopes have been very successful in the discovery and detailed measurement of γ-ray sources, observation of large-scale diffuse emission has been complicated by their small field of view. With the H.E.S.S. Galactic plane survey exists for the first time a deep-exposure data set of large spatial extension, covering the central part of the Milky Way. In the analysis of these data, a signal of large-scale γ-ray emission along the Galactic plane is detected in regions off significantly detected γ-ray sources. This is the first time that large-scale γ-ray emission is observed by imaging atmospheric Cherenkov telescopes. Due to the imperfect γ-hadron separation and the applied background subtraction, the analysis is only sensitive to signals of extensions in Galactic latitude that are small compared to the H.E.S.S. field of view. Emission with larger scale height can be recovered only partly. Contributions to the observed signal originate probably from unresolved γ-ray sources and a truly diffuse emission of hadronic interactions with π 0 decay and inverse Compton scattering. Calculations show that the minimum γ-ray emission from π 0 -decay represents already a significant fraction of the total signal. While unresolved sources provide the smallest scale height and are recoverable to a large extend, the hadronic emission via π 0 decay follows the broader gas distribution and looses around a third of its signal. The inverse Compton component depends at TeV γ-ray energies on the short lifetime and propagation distances of the emitting electrons and renders predictions difficult. At lower energies a smooth emission with large scale height results in a signal loss of ∼ 95%. XI Multifrequency Behaviour of High Energy Cosmic Sources Workshop

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Study of the Diffuse Gamma-Ray Emission From the Galactic Plane With Argo-Ybj

Cited by 95 publications

References 84 publications

Expectation on Observation of Gamma-ray Astronomy with the LHAASO Project

Expectation on Observation of Gamma-ray Astronomy with the LHAASO Project

Recent results inγ-ray astronomy with the ARGO-YBJ detector

Diffuse Galactic Gamma-ray Emission with H.E.S.S.

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