The high energy cosmic-radiation detection (HERD) facility onboard China's Space Station

Zhang, S. N.; Adriani, O.; Albergo, S.; Ambrosi, G.; An, Qi; Bao, Tianwei; Battiston, R.; Bi, X. J.; Cao, Z.; Chai, Jun; Chang, Jin; Chen, G. M.; Chen, Y.; Cui, Xiaohong; Dai, Z. G.; D’Alessandro, R.; Dong, Yongwei; Fan, YaMing; Feng, C.; Feng, Hua; Feng, Zhaopeng; Gao, Xilong; Gargano, F.; Giglietto, N.; Gou, Q. B.; Guo, Y. Q.; Hu, Bi-Ying; Hu, Haibing; He, H. H.; Huang, G. S.; Huang, J.; Huang, Yuhua; Li, H.; Li, L.; Li, Y. G.; Li, Z.; Liang, En‐Wei; Liu, H.; Liu, J. B.; Liu, J. T.; Liu, S. B.; Liu, S. M.; Liu, X.; Lü, J. G.; Mazziotta, M. N.; Mori, N.; Orsi, S.; Pearce, Mark; Pohl, M.; Zheng, Qing; Ryde, F.; Shi, Hongyuan; Спиллантини, П.; Su, Meng; Sun, Jianchao; Sun, XL; Tang, Zhicheng; Walter, R.; Wang, J. C.; Wang, J. M.; Wang, L.; Wang, R. J.; Wang, X. L.; Wang, X. Y.; Wang, Z. G.; Wei, D. M.; Wu, B. B.; Wu, J.; Wu, X.; Xia, Jingkai; Xiao, H. L.; Xu, Hu-Shan; Xu, Menglin; Xu, Z.; Yan, Huan; Yin, Peng-Fei; Yu, Y.; Yuan, Qiang; Zha, M.; Zhang, L.; Zhang, L. Y.; Zhang, Y.; Zhang, Y. J.; Zhang, Y. L.; Zhao, Zhongxiang

doi:10.1117/12.2055280

Cited by 58 publications

(41 citation statements)

References 24 publications

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“…An improvement of roughly one order of magnitude for the Fermi-LAT bounds will be possible depending on new dwarf spheroidal galaxy discovery [39]. Finally, future more powerful instruments, such as GAMMA-400 [40,41], HERD (High Energy cosmic Radiation Detection) [42,43] or CTA (Cherenkov Telescope Array) [44][45][46] may set even stronger limits at different mass scales.…”

Section: Indirect Detectionmentioning

confidence: 99%

Classification of dark pion multiplets as dark matter candidates and collider phenomenology

Beauchesne

Cortona

2020

J. High Energ. Phys.

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New confining sectors can contain a set of pseudo-Goldstone mesons that exhibit a complicated structure in terms of stability and relative masses. Stable ones can act as dark matter candidates, while their interactions with the unstable ones determine their relic abundances. The overall structure, by specifying which channels are kinematically forbidden or not, affects the cosmology, constraints and collider phenomenology. In this paper, we present a classification of these pseudo-Goldstone meson structures. We find that the structures can be classified into three categories, corresponding to strong, suppressed and essentially non-existent constraints from indirect detection. Limits on decay lengths of the unstable mesons and dark jet properties are presented for several benchmark models.

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Section: Indirect Detectionmentioning

confidence: 99%

Classification of dark pion multiplets as dark matter candidates and collider phenomenology

Beauchesne

Cortona

2020

J. High Energ. Phys.

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“…Motivated by this observation, we explore the parameter space of CoyDM by challenging the model with: (i) the observed DM relic abundance, (ii) the constraints imposed by observations of dwarf spheroidal satellites [34], (iii) the bounds resulting from γ-ray line searches in the GC region [35] and (iv) the broad photon excess detected at the GC in an energy window of 1 ÷ 5 GeV [14][15][16][17][18][19][20][21][22][23][24] 1 . In the context of γ-ray line searches, we also evaluate the reach of forthcoming experiments such as DAMPE [38][39][40][41], HERD [42] and GAMMA-400 [43], showing the region of parameter space that these could probe. With our analysis we show that the γ-ray line searches based on the Fermi LAT data significantly bound the properties of CoyDM, although the current constraints are not able to probe the region of the parameter space associated to the detected GC excess.…”

Section: [I] Introductionmentioning

confidence: 99%

Gamma-ray line constraints on coy dark matter

2017

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Coy dark matter is an effective scheme in which a fermionic dark matter candidate interacts with the Standard Model fermions via a pseudoscalar mediator. This simple setup avoids the strong constraints posed by direct detection experiments in a natural way and explains, on top of the observed dark matter relic abundance, the spatially extended γ-ray excess recently detected at the Galactic Center. In this Letter we study the phenomenology of coy dark matter accounting for a novel signature of the model: the diphoton annihilation signal induced by the Standard Model fermions at the loop level. By challenging the model with the observations of spheroidal dwarf satellite galaxies and the results of γ-ray line searches obtained by the Fermi LAT experiment, we assess its compatibility with the measured dark matter relic abundance and the Galactic Center excesses. We show that despite the γ-ray line constraint rules out a significant fraction of the considered parameter space, the region connected to the observed Galactic Center excess remains currently viable. Nevertheless, we find that nextgeneration experiments such as DAMPE, HERD and GAMMA-400 have the potential to probe exhaustively this elusive scenario. [I] IntroductionThe matter content of our Universe is dominated by a component which, differently from ordinary matter, interacts at most very weakly with the photons of the Standard Model (SM) -the dark matter (DM). It is usually assumed that DM consists of stable and weaklyinteracting massive particles (WIMPs), which are thermal relics of dynamics once active in the hot early Universe. The reason behind the success of this picture is that particles with masses and annihilation cross sections set by the electroweak scale yield, in a natural way, DM relic densities of the order of the observed one. The basis of this remarkable coincidence lies in the freeze-out mechanism (for a review: [1, 2]), a natural consequence of the interplay between particle physics and an expanding Universe. For its simplicity and the appealing connection to frameworks like supersymmetry, the WIMP model became the paradigm of DM and shaped the dedicated long term experimental program. Direct detection experiments as XENON100 [3], PANDA [4] and LUX [5] investigate the possible elastic scattering of DM on SM particles mediated by the postulated weak-scale interactions. Similarly, indirect detection investigations scrutinise potential traces of DM annihilations proceeding in the Galaxy or on cosmological scales via the same interactions. Finally, the direct production of DM particles in weak-scale phenomena is studied at collider experiments such as the LHC at CERN [6,7].To date, in spite of the intense experimental effort, the nature and the properties of DM remain still a puzzle. Furthermore, the negative results of dedicated experiments accumulated so far have started to shake the belief of the community in the WIMP paradigm. In fact, the non-detection of supersymmetric partners of SM particles at collider experiments has impair...

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“…The whole calorimeter consists of 100 × 100 × 100 cubes corresponding to 5 λ I deep (Larger dimensions of the calorimeter than those of HERD are used in this simulation to study the longitudinal development of hadronic showers), thus the shower maximum produced by 1 PeV proton can be contained within the calorimeter for those early showered events. The data are derived from Monte Carlo simulation using Fluka 2011 with DPMJET3 [6] from Monte Carlo simulation show that a dynamical range of 2 × 10 6 is required for HCC [1]: A minimum detectable signal down to 30 MeV is required for calibration using MIP; meanwhile, the maximum energy deposition induced by PeV proton shower is up to 60 TeV (energy density is about 8 TeV/cm 3 , Fig. 1).…”

Section: Figmentioning

confidence: 99%

“…The main scientific objectives of HERD are indirect dark matter search, precise CR spectrum and composition measurements up to the knee energy and high energy γ -ray monitoring and survey [1]. To achieve these scientific objectives, a 3-D imaging and five-side active calorimeter is designed to perform high energy resolution and high statistics measurements of the CR nuclei, electrons and positrons, and γ -rays in space.…”

Section: Introductionmentioning

confidence: 99%

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Study of linearity of LYSO crystal for the high energy cosmic radiation detection (HERD) facility

Zheng

Wang

et al. 2017

Radiat Detect Technol Methods

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The high energy cosmic-radiation detection (HERD) facility is a space mission designed for detecting cosmic ray (CR) electrons, γ -rays up to tens of TeV and CR nuclei from proton to iron up to several PeV. The main instrument of HERD is a 3-D imaging calorimeter (CALO) composed of nearly ten thousand lutetium yttrium orthosilicate (LYSO, with cerium doping) crystal cubes. A large dynamic range of single HERD CALO Cell (HCC) is necessary to achieve HERD's PeV observation objectives, which means that the response of HCC should maintain a good linearity from minimum ionizing particle (MIP) calibration to PeV shower maximum. In order to study the linearity of HCC over such a large energy range, a beam test has been implemented at the E2 and E3 beam lines of BEPC. High intensity pulsed electron beam provided by E2 line is used for producing high energy density within HCC; π + /proton provided by E3 line are used for HCC calibration. The results show that no saturation effect occurs and the linearity of HCC is better than 10% from 30 MeV (1 MIP) to 1.1 × 10 3 TeV (energy density is 93 TeV/cm 3 ), which can meet the requirement mentioned above.

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The high energy cosmic-radiation detection (HERD) facility onboard China's Space Station

Cited by 58 publications

References 24 publications

Classification of dark pion multiplets as dark matter candidates and collider phenomenology

Classification of dark pion multiplets as dark matter candidates and collider phenomenology

Gamma-ray line constraints on coy dark matter

Study of linearity of LYSO crystal for the high energy cosmic radiation detection (HERD) facility

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