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New evidence for lack of CMB power on large scales

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Science China(physics,Mechanics & Astronomy) 2010年第3期53卷 567-570页

作者： liu hao1.& li tipei1.2,{1., institute of high energy physics, chinese academy of sciences, beijing 1.0049, China 2 Department of physics & Center for astrophysics, Tsinghua University, beijing 1.0084, China 3 Department of Engineering physics & Center for astrophysics, Tsinghua University, beijing 1.0084, China 1. key {1. of {1. astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing 100049 China2. Department of Physics & Center for Astrophysics Tsinghua University Beijing 100084 China3. Department of Engineering Physics & Center for Astrophysics Tsinghua University Beijing 100084 China

A digitalized temperature map is recovered from the first light sky survey image published by the Planck team, from which an angular power spectrum of the cosmic microwave background (CMB) is derived. The amplitudes of the low multipoles (low-l) measured from the preliminary Planck power spectrum are significantly lower than those reported by the WMAP team. Possible systematical effects are far from enough to explain the observed low-l differences.

关键词： cosmology cosmic microwave background data analysis

Inconsistency between WMAP data and released map

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chinese Science Bulletin 2010年第10期55卷 907-909页

作者： liu hao1.& li tipei1.2,3 1.key laboratory of particle astrophysics,institute of high energy physics,chinese academy of sciences,beijing 1.0049,China 2 Department of physics & Center for {1.},Tsinghua University,beijing 100084,China 3 Department of Engineering physics & Center for {1.},Tsinghua University,beijing 100084,China key {1. of {1. astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing China Department of physics & Center for{1. Tsinghua University Beijing China Department of Engineering physics & Center for{1. Tsinghua University Beijing China

A remarkable inconsistency between the calibrated differential time-ordered data (TOD) of the Wilkinson Microwave Anisotropy Probe (WMAP) mission,which is the input for map-making,and the cosmic microwave background (CMB) temperature maps published by the WMAP team is revealed,indicating that there must exist a serious problem in the map making routine of the WMAP *** inconsistency is easy to be confirmed without the use of WMAP map-making *** view of the importance of this issue for cosmology study,we invite readers to check it by themselves.

关键词：威尔金森微波各向异性探测器 WMAP 地图制作宇宙微波背景有序数据制作软件 TOD CMB

西湖凹陷中央反转带花港组储层成岩演化南北差异及其影响因素分析

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地质论评 2024年第4期70卷 1353-1365页

作者：刘创新高红艳刘彬彬李文俊黄志龙屈童杨易卓夏瑜单理军中海石油(中国)有限公司上海分公司上海200335 油气资源与工程全国重点实验室北京102249 中国石油大学(北京)地球科学学院北京102249

东海盆地西湖凹陷花港组砂岩储层作为西湖凹陷的重要勘探目的层,储层非均质性研究至关重要,笔者等基于储层成岩作用和成岩演化分析,明确中央反转带南北差异,进一步分析其差异成因。研究结果表明,北部地区具有更强的压实作用和溶蚀作用,... 详细信息

东海盆地西湖凹陷花港组砂岩储层作为西湖凹陷的重要勘探目的层,储层非均质性研究至关重要,笔者等基于储层成岩作用和成岩演化分析,明确中央反转带南北差异,进一步分析其差异成因。研究结果表明,北部地区具有更强的压实作用和溶蚀作用,纵向上以3500 m和4000 m为界划分为酸性、酸碱过渡和碱性3个成岩带,经历两期硅质胶结和三期钙质胶结;而南部地区埋深浅、地温低,仅具有两期钙质胶结,纵向上以4000 m为界划分为酸性和碱性两个成岩带;由于北部地区具有更多的岩浆岩母源贡献使得储层抗压实能力较差,遭受压实更强,但烃源岩较强的生烃强度使得储层遭受溶蚀作用更强,因此北部地区花港组储层具有低孔高渗的特征。该研究对优质储层发育研究和甜点预测具有重要意义。

关键词：成岩演化影响因素花港组中央反转带西湖凹陷

Overview to the Hard X-ray Modulation Telescope (Insight-HXMT) Satellite

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Science China(physics,Mechanics & Astronomy) 2020年第4期63卷 2-19页

作者： Shuang-Nan Zhang tipei {1. FangJun Lu {1.Ming Song YuPeng X u CongZhan liu Yong Chen XueLei Cao QingCui Bu Zhi Chang Gang Chen {1. Chen TianXiang Chen YiBao Chen YuPeng Chen Wei Cui WeiWei Cui JingKang Deng YongWei Dong Yuan Yuan Du MinXue Fu GuanHua Gao He Gao Min Gao MingYu Ge YuDong Gu Ju Guan Can Gungor ChengCheng Guo DaWei Han Wei Hu Yue Huang Jia Huo ShuMei Jia LuHua Jiang WeiChun Jiang Jing Jin YongJie Jin Bing {1. ChengKui {1. Gang {1. MaoShun {1. Wei {1. Xian {1. XiaoBo {1. XuFang {1. YanGuo {1. ZiJian {1. ZhengWei {1. XiaoHua {1.ang JinYuan {1.ao GuoQing liu HongWei liu ShaoZhen liu XiaoJing liu Yuan liu YiNong liu Bo Lu XueFeng Lu Tao Luo Xiang Ma Bin Meng Yi Nang JianYin Nie Ge Ou JinLu Qu Na Sai RenCheng Shang GuoHong Shen {1.ang Sun Ying Tan {1.an Tao You{1. Tuo Chen Wang ChunQin Wang GuoFeng Wang HuanYu Wang Juan Wang WenShuai Wang YuSa Wang XiangYang Wen BaiYang Wu BoBing Wu Mei Wu GuangCheng Xiao Shao{1.n Xiong {1.n{1. Yan JiaWei Yang Sheng Yang YanJi Yang QiBin Yi Bin Yuan AiMei Zhang ChunLei Zhang ChengMo Zhang Fan Zhang HongMei Zhang Juan Zhang Qiang Zhang ShenYi Zhangs Shu Zhang Tong Zhang WanChang Zhang Wei Zhang WenZhao Zhang Yi Zhang YiFei Zhang YongJie Zhang Yue Zhang Zhao Zhang Zhi Zhang Zi{1.ang Zhang HaiSheng Zhao XiaoFan Zhao ShiJie Zheng JianFeng Zhou YuXuan Zhu Yue Zhu Ren{1.n Zhuang key {1. of {1. astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Beijing 100049China Department of Astronomy Tsinghua UniversityBeijing 100084China Department of physics Tsinghua UniversityBeijing 100084China Department of Astronomy Beijing Normal UniversityBeijing 100088China Department of Engineering physics Tsinghua UniversityBeijing 100084China National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China National Space Science Center Chinese Academy of SciencesBeijing 100190China

As China’s first X-ray astronomical satellite, the Hard X-ray Modulation Telescope (HXMT), which was dubbed as Insight-HXMT after the launch on June 1., 201., is a wide-band({1.50 ke V) slat-collimator-based X-ray astronomy satellite with the capability of all-sky monitoring in 0.2-3 Me V. It was designed to perform pointing, scanning and gamma-ray burst(GRB)observations and, based on the Direct Demodulation Method (DDM), the image of the scanned sky region can be *** we give an overview of the mission and its progresses, including payload, core sciences, ground calibration/facility, ground segment, data archive, software, in-orbit performance, calibration, background model, observations and some preliminary results.

关键词： X-and γ-ray telescopes and instrumentation neutron stars black holes X-ray binaries γ-ray bursts

The high {1. X-ray telescope (HE) onboard the Insight-HXMT astronomy satellite

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Science China(physics,Mechanics & Astronomy) 2020年第4期63卷 20-34页

作者： CongZhan liu YiFei Zhang XuFang {1. XueFeng Lu Zhi Chang ZhengWei {1. AiMei Zhang YongJie Jin HuiMing Yu Zhao Zhang MinXue Fu YiBao Chen JianFeng Ji YuPeng Xu JingKang Deng RenCheng Shang GuoQing liu FangJun Lu ShuangNan Zhang YongWei Dong tipei {1. Mei Wu YanGuo {1. HuanYu Wang BoBing Wu YongJie Zhang Zhi Zhang Shao{1.n Xiong Yuan liu Shu Zhang HongWei liu YiJung Yang Fan Zhang key {1. of {1. astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Department of Engineering physics Tsinghua UniversityBeijing 100084China Department of physics Tsinghua UniversityBeijing 100084China University of chinese academy of sciences Beijing 100049China

The Insight-Hard X-ray Modulation Telescope(Insight-HXMT) is a broadband X-ray and γ-ray(1.3000 ke V) astronomy satellite. One of its three main telescopes is the {1. energy X-ray telescope(HE). The main detector plane of HE comprises 1. Na I(Tl)/Cs I(Na) phoswich detectors, where Na I(Tl) is used as the primary detector to measure ~ 20-250 ke V photons incident from the field of view(FOV) defined by collimators, and Cs I(Na) is used as the active shielding detector to Na I(Tl) by pulse shape discrimination. Additionally, Cs I(Na) is used as an omnidirectional γ-ray monitor. The HE collimators have a diverse FOV,i.e. 1.1.×5.7°(1. units), 5.7°×5.7°(2 units), and blocked(1.unit). Therefore, the combined FOV of HE is approximately5.7°×5.7°. Each HE detector has a diameter of 1.0 mm resulting in a total geometrical area of approximately 51.0 cm2, and the energy resolution is ~1.% at 60 ke V. For each recorded X-ray event by HE, the timing accuracy is less than 1. μs and the deadtime is less than 1. μs. HE is used for observing spectra and temporal variability of X-ray sources in the 20-250 ke V band either by pointing observations for known sources or scanning observations to unveil new sources. Additionally, HE is used for monitoring the γ-ray burst in 0.2-3 Me V band. This paper not only presents the design and performance of HE instruments but also reports results of the on-ground calibration experiments.

关键词： X-ray telescope HXMT calibration scintillation detector

The Low energy X-ray telescope (LE) onboard the Insight-HXMT astronomy satel{1.te

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Science China(physics,Mechanics & Astronomy) 2020年第4期63卷 49-61页

作者： Yong Chen WeiWei Cui Wei li Juan Wang YuPeng Xu FangJun Lul YuSa Wang TianXiang Chen DaWei Han Wei Hu Yi Zhang Jia Huo YanJi Yang MaoShun li Bo Lu Ziliang Zhang tipei li ShuangNan Zhang Shaolin Xiong Shu Zhang RongFeng Xue XiaoFan Zhao Yue Zhu YuXuan Zhu HongWei liu YiJung Yang Fan Zhang key {1. of {1. astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China University of chinese academy of sciences Beijing 100049China Department of physics Tsinghua UniversityBeijing 100084China Department of Education Lu Liang UniversityLuliang 033000China Qian Xuesen laboratory of Space Technology China Academy of Space TechnologyBeijing 100094China College of physics Jilin UniversityChangchun 130023China

The Low energy X-ray telescope(LE) is one of the three main instruments of the Insight-Hard X-ray Modulation Telescope(Insight-HXMT). It is equipped with Swept Charge Device(SCD) sensor arrays with a total geometrical area of 384 cm^2 and an energy band from 0.7 to 1. ke V. In order to evaluate the particle induced X-ray background and the cosmic X-ray background simultaneously, LE adopts collimators to define four types of Field Of Views(FOVs), i.e., 1.6°×6°, 4°×6°, 50°-60°×2°-6 oand the blocked ones which block the X-ray by an aluminum cover. LE is constituted of three detector boxes(LEDs) and an electric control box(LEB) and achieves a good energy resolution of 1.0 e V@5.9 ke V, an excellent time resolution of 0.98 ms, as well as an extremely low pileup(1.@1.000 cts/s). Detailed performance tests and calibration on the ground have been performed,including energy-channel relation, energy response, detection efficiency and time response.

关键词： LE X-ray telescope SCD collimators

The Medium energy X-ray telescope (ME) onboard the Insight-HXMT astronomy satel{1.te

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Science China(physics,Mechanics & Astronomy) 2020年第4期63卷 35-48页

作者： XueLei Cao WeiChun Jiang Bin Meng WanChang Zhang Tao Luo Sheng Yang ChunLei Zhang YuDong Gu liang Sun XiaoJing {1. JiaWei Yang Xian li Ying Tan ShaoZhen {1. YuanYuan Du FangJun Lu YuPeng Xu Ju Guan ShuangNan Zhang HuanYu Wang tipei li ChengMo Zhang XiangYang Wen JinLu Qu liMing Song XiaoBo li MingYu Ge YuPeng Zhou Shaolin Xiong Shu Zhang YongJie Zhang Zehao Cheng Fei Zhang MaoShun li XiaoHua liang Min Gao EnBo Yang XiaoHang {1. HongWei {1. YiJung Yang Fan Zhang key {1. of {1. astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Department of Engineering physics Tsinghua UniversityBeijing 100084China beijing {1. {1. of Space Thermal Control Technology Beijing Institute of Spacecraft System EngineeringBeijing 100094China Department of Modern physics School of Physical SciencesUniversity of Science and Technology of ChinaHefei 230022China School of Physical sciences Guizhou UniversityGuivang 550025China School of Opto-Electronic Information Science and Technology Yantai UniversityYantai 264005China University of chinese academy of sciences Beijing 100049China

The Medium energy X-ray telescope(ME) is one of the three main telescopes on board the Insight hard X-ray modulation telescope(Insight-HXMT) astronomy satel{1.te. ME contains 1.28 pixels of Si-PIN detectors sensitive in 5-30 ke V with a total geometrical area of 952 cm^2. The app{1.cation specific integrated circuit(ASIC) chip, VA32TA6, is used to achieve low power consumption and low readout noise. The col{1.mators define three kinds of field of views(FOVs) for the telescope, 1.×4°, 4°×4°,and blocked ones. Combination of such FOVs can be used to estimate the in-orbit X-ray and {1. background *** energy resolution of ME is ~3 ke V at 1..8 ke V(FWHM) and the time resolution is 255 μs. In this paper, we introduce the design and performance of ME.

关键词： Si-PIN ASIC medium energy X-ray

Ta离子辐照对YBa_(2)Cu_(3)O_(7–δ)的微观结构和载流特性的影响

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科学通报 2021年第31期66卷 3965-3972页

作者：谷裕蔡传兵刘志勇刘杰刘丽黄荣铁上海大学物理系上海市高温超导重点实验室上海200444 上海上创超导科技有限公司上海201401 中国科学院近代物理研究所兰州730000 中国科学院大学核科学与技术学院北京100049

高温超导YBa_(2)Cu_(3)O_(7–δ)(YBCO)涂层导体也称为第二代高温超导带材(2G-HTS带材),在能源、交通等领域具有广泛的应用前景.然而,其在强磁场下临界电流密度较低的问题严重限制了其应用,因此提升其磁通钉扎和在场载流能力是YBCO涂层... 详细信息

高温超导YBa_(2)Cu_(3)O_(7–δ)(YBCO)涂层导体也称为第二代高温超导带材(2G-HTS带材),在能源、交通等领域具有广泛的应用前景.然而,其在强磁场下临界电流密度较低的问题严重限制了其应用,因此提升其磁通钉扎和在场载流能力是YBCO涂层导体的研究热点.本文利用1.9 GeV的Ta离子对YBCO带材进行辐照,研究了不同剂量的Ta离子辐照后YBCO带材的微观结构和载流特性变化.样品的场发射透射电子显微镜(field emission transmission electron microscope,FETEM)图像显示,辐照过程中高能^(1.1.Ta^(32+)离子在薄膜中形成了~1. nm尺寸的柱状缺陷,说明辐照后样品中产生了有效的钉扎中心.通过磁学测量系统(magnetic property measurement system,MPMS)对辐照样品的载流特性进行研究,发现当Ta离子剂量低于5.0×1.^(1.)ions/cm^(2)时,样品的临界转变温度T_(c,on)并无明显变化,但当剂量达到5.0×1.^(1.)ions/cm^(2)时,T_(c,on)减小了约0.6 K;当剂量高于1.0×1.^(8)ions/cm^(2)时,由零场冷磁化强度随温度变化情况可知,辐照样品的超导抗磁相明显多于无辐照样品.同时,较高辐照剂量如5.0×1.^(1.)ions/cm^(2)YBCO样品的J_(c)较高,不同磁场下的J_(c)均得到了明显提升,30 K、1.T时的提升因子达到了3.8(提升因子定义为不同温度、外场下的J_(c)与77 K自场下J_(c)的比值),为同温度同场下无辐照样品的3倍.将临界电流密度J_(c)与磁场强度H的关系采用J_(c)∝H–β进行拟合,发现高剂量样品的磁通匹配场H*和表征随磁场衰减参数β增大了.此外,约化钉扎力密度标度关系显示,在低场下,样品中的钉扎类型在低辐照剂量下主要是面钉扎,当辐照剂量达到5.0×1.^(1.)ions/cm^(2)时开始向点缺陷钉扎类型转变,高场下则是所有样品都更符合面钉扎类型.

关键词：高能Ta离子 YBa_(2)Cu_(3)O_(7-δ)高温超导涂层导体辐照钉扎缺陷载流特性

The 1.PW/0.1.Hz laser beamline in SULF facility

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high Power Laser Science and Engineering 2020年第1期8卷 23-29页

作者： Zongxin Zhang Fenxiang Wu Jiabing Hu Xiaojun Yang Jiayan Gui Penghua Ji Xingyan liu Cheng Wang Yanqi liu Xiaoming Lu Yi Xu Yuxin Leng Ruxin li Zhizhan Xu State key {1. of high Field Laser {1. Shanghai Institute of Optics and Fine MechanicsChinese Academy of SciencesShanghai 201800China University of chinese academy of sciences Beijing 100049China ShanghaiTech University Shanghai 201210China

In this paper,we report the recent progress on the 1.PW/0.1.Hz laser beamline of Shanghai Superintense Ultrafast Laser Facility(SULF).The SULF-1.PW laser beamline is based on the double chirped pulse amplification(CPA... 详细信息

In this paper,we report the recent progress on the 1 PW/0.1 Hz laser beamline of Shanghai Superintense Ultrafast Laser Facility(SULF).The SULF-1 PW laser beamline is based on the double chirped pulse amplification(CPA)scheme,which can generate laser pulses of 50.8 J at 0.1 Hz after the final amplifier;the shot-to-shot energy fluctuation of the amplified pulse is as low as 1.2%(std).After compression,the pulse duration of 29.6 fs is achieved,which can support a maximal peak power of 1 *** contrast ratio at-80 ps before main pulse is measured to be 2.5×10^-*** focused peak intensity is improved by optimizing the angular dispersion in the grating *** maximal focused peak intensity can reach 2.7×10^19W/cm2 even with an f/26.5 off-axis parabolic *** horizontal and vertical angular pointing fluctuations in 1 h are measured to be 1.89 and 2.45μrad,*** moderate repetition rate and the good stability are desirable characteristics for lasermatter *** SULF-1 PW laser beamline is now in the phase of commissioning,and preliminary experiments of {1. acceleration and secondary radiation under 300–400 TW/0.1 Hz laser condition have been *** progress on the experiments and the daily stable operation of the laser demonstrate the availability of the SULF-1 PW beamline.

关键词： laser amplifiers lasers titanium ultrafast lasers