S. Hu

Sichuan University

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Lili Yang

Sun Yat-sen University

W. X. Wu

Nanjing University of Science and Technology

H. K. Lv

Chinese Academy of Sciences

Yu. V. Stenkin

Institute for Nuclear Research

L. Shao

Hebei Normal University

M. Qi

Chinese Academy of Sciences

H. Y. Jia

Southwest Jiaotong University

Z. Y. Pei

Guangzhou University

J. R. Mao

Yunnan Observatories

F. Shi

Chinese Academy of Sciences

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Chinese Academy of Sciences

433

Institute of High Energy Physics

322

University of Chinese Academy of Sciences

195

Southwest Jiaotong University

166

University of Science and Technology of China

112

Tibet University

112

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104

Gansu Great Wall Electrical and Electronics Engineering Research Institute

Purple Mountain Observatory

National Natural Science Foundation of China

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mBin1b transgenic mice show enhanced resistance to epididymal infection by bacteria challenge

Genes and Immunity (2012)

Zhaoliang Fei S. Hu Liang Xiao Jingfeng Zhou Haiqing Diao

10.1038/gene.2012.13

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Citations (27)

Construction and on-site performance of the LHAASO WFCTA camera

The European Physical Journal C (2021)

F. Aharonian Q. An Axikegu Lixin Bai Y. X. Bai

The focal plane camera is the core component of the Wide Field-of-view Cherenkov/fluorescence Telescope Array (WFCTA) of the Large High-Altitude Air Shower Observatory (LHAASO). Because of the capability of working under moonlight without aging, silicon photomultipliers (SiPM) have been proven to be not only an alternative but also an improvement to conventional photomultiplier tubes (PMT) in this application. Eighteen SiPM-based cameras with square light funnels have been built for WFCTA. The telescopes have collected more than 100 million cosmic ray events and preliminary results indicate that these cameras are capable of working under moonlight. The characteristics of the light funnels and SiPMs pose challenges (e.g. dynamic range, dark count rate, assembly techniques). In this paper, we present the design features, manufacturing techniques and performances of these cameras. Finally, the test facilities, the test methods and results of SiPMs in the cameras are reported here.

Silicon Photomultiplier

Moonlight

10.1140/epjc/s10052-021-09414-z

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Citations (9)

Prospects for a multi-TeV gamma-ray sky survey with the LHAASO water Cherenkov detector array *

Chinese Physics C (2020)

F. Aharonian В. В. Алексеенко Q. An Axikegu Lixin Bai

The Water Cherenkov Detector Array (WCDA) is a major component of the Large High Altitude Air Shower Array Observatory (LHAASO), a new generation cosmic-ray experiment with unprecedented sensitivity, currently under construction. The WCDA is aimed at the study of TeV $\gamma$-rays. In order to evaluate the prospects of searching for TeV $\gamma$-ray sources with the WCDA, we present in this paper a projection for the one-year sensitivity of the WCDA to TeV $\gamma$-ray sources from TeVCat (footnote: http://tevcat.uchicago.edu) using an all-sky approach. Out of 128 TeVCat sources observable to the WCDA up to a zenith angle of $45^\circ$, we estimate that 42 would be detectable for one year of observations at a median energy of 1 TeV. Most of them are Galactic sources, and the extragalactic sources are Active Galactic Nuclei (AGN).

Zenith

Air shower

Cherenkov detector

Cherenkov Telescope Array

10.1088/1674-1137/44/6/065001

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Citations (13)

The optical properties of Bi3.25La0.75Ti3O12 thin films with different thickness prepared by chemical solution deposition

Materials Research Bulletin (2004)

S. Hu

Chemical bath deposition

Fused quartz

Deposition

10.1016/s0025-5408(04)00108-4

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Design and Testing of the Front-End Electronics of WCDA in LHAASO

IEEE Transactions on Nuclear Science (2021)

F. Aharonian Q. An Axikegu Lixin Bai Y. Bai

Water Cherenkov detector array (WCDA) is one of the key parts of the Large High Altitude Air Shower Observatory (LHAASO), the construction of which was completed by the end of 2020. The WCDA covers a 78 000-m ² area and there exist 3120 large size photomultiplier tubes (PMTs) in three ponds: 8-in PMTs are used in WCDA pond No. 1 and 20-in PMTs are used in ponds No. 2 and No. 3. The front-end electronics (FEE) system based on multigain measurement technique is designed to achieve both high-precision time and charge measurements over a large dynamic range from single photon electron (S.P.E.) to 4000 P.E. (for water pond No. 1)/1800 P.E. (for water ponds No. 2 and No. 3). To achieve a high-quality clock distribution and phase alignment as well as mixed transmission of data, clock, and commands in one fiber over a long distance, an enhanced white rabbit (WR) technique is used. Testing of all the 350 FEE modules for the WCDA is presented in this article. Test results indicate that the charge resolution is better than 20% at S.P.E. and 1% at 1800/4000 P.E. and the time resolution is better than 300 ps root mean square (rms), which successfully meets the application requirement. All the FEE modules have been fabricated and installed for the LHAASO WCDA from 2018 to 2020, and the initial commissioning operation indicates that the FEEs function well.

Cherenkov detector

Photon Counting

10.1109/tns.2021.3092739

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Citations (1)

Calibration of the air shower energy scale of the water and air Cherenkov techniques in the LHAASO experiment

Physical review. D/Physical review. D. (2021)

F. Aharonian Q. An Axikegu Lixin Bai Yucen Bai

The Wide Field-of-View Cherenkov Telescope Array (WFCTA) and the Water Cherenkov Detector Arrays (WCDA) of LHAASO are designed to work in combination for measuring the energy spectra of various cosmic ray species over a very wide energy range from a few TeV to 10 PeV. The energy calibration of WCDA can be achieved with a proven technique of measuring the westward shift of the Moon shadow of galactic cosmic rays due to the geomagnetic field. This deflection angle $\Delta$ is inversely proportional to the energy of the cosmic rays. The precise measurements of the shifts by WCDA allows us to calibrate its energy scale for energies as high as 35 TeV. The energy scale measured by WCDA can be used to cross calibrate the energy reconstructed by WFCTA, which spans the whole energy range up to 10 PeV. In this work, we will demonstrate the feasibility of the method using the data collected from April 2019 to January 2020 by the WFCTA array and WCDA-1 detector, the first of the three water Cherenkov ponds, already commissioned at LHAASO site.

Air shower

Cherenkov detector

Cherenkov Telescope Array

10.1103/physrevd.104.062007

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Citations (13)

Cable Fault Detection and Location System Based on Low Background Noise Distributed Acoustic Sensing

Yuping Huang Changwei Ma Jue Zhang Ruipeng Liu Wenjiao Chen

Distributed Acoustic Sensing

10.1109/sgee64306.2024.10865841

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Doped-type coplanar junctions in the Bi/sub 2/Sr/sub 2/Ca/sub 1/Cu/sub 2/O/sub 8+δ/ system

IEEE Transactions on Applied Superconductivity (1997)

A.C. Meltzow S. Hu J. Hollkott J. Auge Bernd Spangenberg

We report on a vertical Josephson junction in the Bi/sub 2/Sr/sub 2/Ca/sub 1/Cu/sub 2/O/sub 8+/spl delta// (BSCCO) system, based on a bilayer structure. A highly resistive bottom layer of Bi/sub 2/Sr/sub 2/(Ca/sub 1-z/Gd/sub z/)Cu/sub 2/O/sub 8+/spl delta// is deposited by DC-sputtering and covered by an undoped BSCCO layer with a T/sub c/ of typically 90 K. Junctions are formed by trenches patterned through the top layer into the resistive bottom layer. We found that the critical current I/sub c/ of the junctions is determined by the width of the grooves. Josephson coupling is demonstrated by Shapiro-like steps in the I-V curve up to a width of 0.8 /spl mu/m.

Resistive touchscreen

10.1109/77.621880

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Citations (12)

Ash and burn control in ITER-type tokamak

S. Hu V. Varadarajan George H. Miley

Summary Form only given, as follows. Ash control in the long-pulse tokamaks such as the ITER is addressed from the point of view of sawtooth pumping and fishbone excitation. An analytic model for predicting the influence of sawtooth and edge pumping on the helium contamination has been developed. One of its uses is to compute the ash density level for a given fusion power versus helium pumping fraction. The change of ash concentration due to sawtooth disruptions is also evaluated. The results show that the helium contamination can be changed drastically if pumping is strong enough. The results also show that adding sawteeth to help remove the ash from the center of the plasma becomes useful when the temperature profiles are parabolic or flatter. The controlled excitation of fishbone oscillations can directly help to control the ash accumulation by ejecting the alphas as they slow down to low energies. Estimates of the fishbone instability threshold rule out low frequency fishbones.< >

Sawtooth wave

KSTAR

Fusion power

10.1109/plasma.1989.166022

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Performance of LHAASO-WCDA and observation of the Crab Nebula as a standard candle *

Chinese Physics C (2021)

F. Aharonian Q. An 克古 Axikegu Lixin Bai Y. X. Bai

Abstract The first Water Cherenkov detector of the LHAASO experiment (WCDA-1) has been operating since April 2019. The data for the first year have been analyzed to test its performance by observing the Crab Nebula as a standard candle. The WCDA-1 achieves a sensitivity of 65 mCU per year, with a statistical threshold of 5 . To accomplish this, a 97.7% cosmic-ray background rejection rate around 1 TeV and 99.8% around 6 TeV with an approximate photon acceptance of 50% is achieved after applying an algorithm to separate gamma-induced showers. The angular resolution is measured using the Crab Nebula as a point source to be approximately 0.45° at 1 TeV and better than 0.2° above 6 TeV, with a pointing accuracy better than 0.05°. These values all match the design specifications. The energy resolution is found to be 33% for gamma rays around 6 TeV. The spectral energy distribution of the Crab Nebula in the range from 500 GeV to 15.8 TeV is measured and found to be in agreement with the results from other TeV gamma ray observatories.

Crab Nebula

Cosmic distance ladder

Cherenkov detector

10.1088/1674-1137/ac041b

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Citations (44)