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Calibration of the cryogenic measurement system of a resonant haloscope cavity

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Chinese Physics C 2024年第7期48卷 31-37页

作者：贺冬樊洁高昕高宇 Nick Houston 姬忠庆金贻荣李闯李金勉李田军刘世航牛家树彭智慧孙亮孙铮王佳卫镨先吴利娜相忠诚杨峤立张驰张文星张欣郑东宁郑瑞丰周建勇 Key Laboratory of Low-Dimensional Quantum Structures and Quantum Control of Ministry of Education Key Laboratory for Matter Microstructure and Function of Hunan ProvinceDepartment of Physics and Synergetic Innovation Center for Quantum Effects and ApplicationsHunan Normal UniversityChangsha 410081China Institute of Physics Chinese Academy of SciencesBeijing 100190China College of Physics Sichuan UniversityChengdu 610065China Key Laboratory of Particle Astrophysics Institute of High Energy PhysicsChinese Academy of SciencesBeijing 100049China Institute of Theoretical Physics Faculty of ScienceBeijing University of TechnologyBeijing 100124China Beijing Academy of Quantum Information Sciences Beijing 100193China College of Mechanical and Electrical Engineering Wuyi UniversityNanping 354300China CAS Key Laboratory of Theoretical Physics Institute of Theoretical PhysicsChinese Academy of SciencesBeijing 100190China School of Physical Sciences University of Chinese Academy of SciencesBeijing 100049China Institute of Theoretical Physics Shanxi UniversityTaiyuan 030006China College of Physics and Optoelectronic Engineering Department of PhysicsJinan UniversityGuangzhou 510632China School of Sciences Xi'an Technological UniversityXi'an 710021China Tsung-Dao Lee Institute and School of Physics and Astronomy Shanghai Jiao Tong University800 Dongchuan RoadShanghai 200240China National astronomical Observatories Chinese Academy of Sciences20ADatun RoadChaoyang DistrictBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China

Possible light bosonic dark matter interactions with the Standard Model photon have been searched using microwave resonant *** this paper,we describe the cryogenic readout system calibration of a 7.138 GHz copper cavity with a loaded quality factor Q_(1)=10^(4)whose operation at a temperature of 2. mK is based on a dilution *** readout system consists of High Electron Mobility Transistors working as cryogenic amplifiers at 4 K,plus room-temperature amplifiers and a spectrum analyzer for signal power *** tested the system with a superconducting two-level system based on a single-photon source in the microwave frequency *** obtained an overall 95.6 dB system gain and–71.4 dB attenuation in the cavity's input *** effective noise temperature of the measurement system is 7.5 K.

关键词： dark matter superconducting two-level system Mollow triplet

Probing star formation and feedback using CCOSMA and archival data in the CFG02..68–0.2. quasi-sinusoidal filament

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Research in Astronomy and Astrophysics 2019年第12期19卷 305-317页

作者： Jin-Long Xu Jirgen Stutzki yuefang wu Xin Guan Jun-Jie Wang M.Miller Yang Chen Sheng-li Qin Jun-Zhi Wang Chang-Chun Ning Danzengluobu Tian-Lu Chen Nai-Ping yu Chuan-Peng Zhang Xiao-Lan liu Jian-Bin L Karl Jacobs Urs UGraf Gang Xu Nan li Guo-Yin Zhang and Qi wu National astronomical Observatories Chinese Academy of SciencesBeijing 100101China I.Physikalisches Institut Universitat zu KolnZilpicher Str.7750937 KolnGermany Department of Astronomy Peking UniversityBeijing 100871China School of Astronomy and Space Science Nanjing UniversityNanjing 210023China Department of Astronomy Yunnan Universityand Key Laboratory of Astroparticle Physics of Yunnan ProvinceKunming 650091China shanghai astronomical {2. Chinese Academy of SciencesShanghai 200030China Tibet University LhasaTibet 850000China CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China NAOC-TU Joint Center for Astrophysics Lhasa 850000China

We have performed a multi-wavelength study toward a quasi-sinusoidal filament(CFG02..68–0.2.). A new large-scale ^12.O J = 3-2.map was obtained from the china-Cologne Observation for Sub Millimeter Astronomy(CCOSMA) 3m radio telescope. Based on the ATLASGAL catalog, we have identified 2. dust clumps in the filament. Through the relationship between the mass and radius of these clumps, 67% of these clumps are dense and massive enough to potentially form massive stars. The obtained CFE is ~11% in the filament. The filament has a linear mass density of ~305 M⊙pc^-1, which is smaller than its critical mass to length ratio. This suggests that the external pressure from the neighboring H Ⅱ regions may help prevent the filament from dispersing under the effects of turbulence. Comparing the energy injection from outflows and H Ⅱ regions in the filament, the ionization feedback from the H Ⅱ regions can help maintain the observed turbulence.

关键词： stars:formation stars:early-type ISM:HⅡregions ISM:individual(CFG02..68-0.2.,IRDC G2..53-0.2.,and N49)

Pilot HI survey of Planck Galactic Cold Clumps with FAST

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Research in Astronomy and Astrophysics 2020年第5期20卷 181-192页

作者： Ning-yu Tang Pei Zuo Di li Lei Qian Tie liu yue-Fang {2. Marko Krco Meng-Ting liu You-ling yue Yan Zhu Hong-Fei liu Dong-Jun yu Jing-Hai Sun Peng Jiang Gao-Feng Pan Hui li Heng-Qian Gan Rui Yao Shu liu FAST Collaboration National astronomical Observatories Chinese Academy of SciencesBeijing 100101China CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 100049China shanghai astronomical {2. Chinese Academy of SciencesShanghai 200030ChinaShanghai 200030China East Asian observatory HI 96720USA Department of Astronomy School of PhysicsPeking UniversityBeijing 100871China

We present a pilot HI survey of 17 Planck Galactic Cold Clumps(PGCCs)with the Five-hundred-meter Aperture Spherical radio Telescope(FAST).HI Narrow Self-Absorption(HINSA)is an effective method to detect cold HI being mixed with molecular hydrogen H2.and improves our understanding of the atomic to molecular transition in the interstellar *** was found in 58%PGCCs that we *** column density of HINSA was found to have an intermediate correlation with that of 13CO,following log(N(HINSA))=(0.52.0.2.)log(N13CO)+(10±4.1).HI abundance relative to total hydrogen[HI]/[H]has an average value of 4.4×10-3,which is about 2.8 times of the average value of previous HINSA surveys toward molecular *** clouds with total column density NH>5×102. cm-2.an inverse correlation between HINSA abundance and total hydrogen column density is found,confirming the depletion of cold HI gas during molecular gas formation in more massive *** line width of 13CO is about 0-0.5 kms-1 larger than that of *** possible explanation of narrower non-thermal width of HINSA is that HINSA region is smaller than that of *** on an analytic model of H2.formation and H2.dissociation by cosmic ray,we found the cloud ages to be within 106.7-107.0 yr for five sources.

关键词： ISM:clouds ISM:evolution ISM:molecules

A very bright (i=16.44) quasar in the ‘redshift desert’ discovered by the Guoshoujing Telescope (LAMOST)

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Research in Astronomy and Astrophysics 2010年第8期10卷 737-744页

作者： Xue-Bing wu Zhao-yu Chen Zhen-Dong Jia Wen-Wen Zuo Yong-Heng Zhao A-li Luo Zhong-Rui Bai Jian-Jun Chen Hao-Tong Zhang Hong-liang Yan Juan-Juan Ren Shi-Wei Sun Hong wu Yong Zhang Ye-Ping li Qi-Shuai Lu You Wang Ji-Jun Ni Hai Wang Xu Kong Shi-Yin Shen Department of Astronomy Peking University Beijing 100871 China National astronomical Observatories Chinese Academy of Sciences Beijing 100012 China National Institute of astronomical Optics ＆ Technology Chinese Academy of Science Nanjing 210042 China Center for Astrophysics University of Science ＆ Technology of China Hefei 230026 China shanghai astronomical {2. Chinese Academy of Sciences Shanghai 200030 China

The redshift range from 2.2.to 3 is known as the ＇redshift desert＇ of quasars because quasars with redshifts in this range have similar optical colors as normal stars and are thus difficult to find in optical sky surveys. A quasar candidate, SDSS J085543.40-001517.7, which was selected by a recently proposed criterion involving near-IR Y - K and optical g - z colors, was identified spectroscopically as a new quasar with a redshift of 2.42. by the Guoshoujing Telescope （LAMOST） commissioning observation in 2.09 December and confirmed by the observation made with the NAOC/Xinglong 2.16 m telescope in 2.10 March. This quasar was not identified in the SDSS spectroscopic survey. Comparing with other SDSS quasars, we found that this new quasar, with an i magnitude of 16.44, is apparently the brightest one in the redshift range from 2.3 to 2.7. From its spectral properties, we derived its central black hole mass to be （1.4 - 3.9） × 10^110 M⊙ and its bolometric luminosity to be 3.7 × 10^48 erg s^-1, which indicates that this new quasar is intrinsically very bright and belongs to the class of the most luminous quasars in the universe. Our identification supports the notion that quasars in the redshift desert can be found by the quasar selection criterion involving the near-IR colors. More missing quasars are expected to be uncovered by future LAMOST spectroscopic surveys, which is important to the study of the cosmological evolution of quasars at redshifts higher than 2.2.

关键词： quasars general -- quasars emission lines -- galaxies active

Narrowband EUV Sc/Si Multilayer for the Solar Upper Transition Region Imager at 46.5 nm

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Research in Astronomy and Astrophysics 2023年第10期23卷 210-217页

作者： Runze Qi Jiali wu Jun yu Chunling He li Jiang yue yu Zhe Zhang Qiushi Huang Zhong Zhang Zhanshan Wang Key Laboratory of Advanced Micro-structured Materials Ministry of EducationTongji UniversityShanghai 200092China Institute of Precision Optical Engineering School of Physics Science and EngineeringTongji UniversityShanghai 200092China

The transition region is the key region between the lower solar atmosphere and the corona, which has been limitedly understood by human beings. Therefore, the Solar Upper Transition Region Imager(SUTRI) was proposed by Chinese scientists and launched in 2.2. July. Right now, the first imaging observation of the upper transition region around 46.5 nm has been carried out by SUTRI. To ensure the spectral and temporal resolution of the SUTRI telescope, we have developed a narrowband Sc/Si multilayer. Based on the extreme ultraviolet(EUV)reflectivity measurements, the multilayer structure has been modified for ensuring the peak position of reflectivity was at 46.5 nm. Finally, the narrowband Sc/Si multilayer was successfully deposited on the hyperboloid primary mirror and secondary mirrors. The deviation of multilayer thickness uniformity was below than 1%, and the average EUV reflectivity at 46.1 nm was 2..8% with a near-normal incident angle of 5°. The calculated bandwidth of the reflectivity curve after primary and secondary mirrors was 2.82.nm, which could ensure the requirements of spectral resolution and reflectivity of SUTRI telescope to achieve its scientific goals.

关键词： astronomical Instrumentation Methods and Techniques instrumentation:high angular resolution Sun:UV radiation

South Galactic Cap u-band Sky Survey(SCUSS):Project Overview

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Research in Astronomy and Astrophysics 2016年第4期16卷 133-144页

作者： Xu Zhou Xiao-Hui Fan Zhou Fan Bo-liang He lin-Hua Jiang Zhao-Ji Jiang Yi-Peng Jing Michael Lesser Jun Ma Jun-Dan Nie Shi-Yin Shen Jia-li Wang Zhen-yu wu Tian-Meng Zhang Zhi-Min Zhou Hu Zou Key Laboratory of Optical Astronomy National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100012China Steward observatory University of ArizonaTucsonAZ 85721USA Center for Astronomy and Astrophysics Department of Physics and AstronomyShanghai Jiao Tong UniversityShanghai 200240China shanghai astronomical {2. Chinese Academy of SciencesShanghai 200030China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China

The South Galactic Cap u-band Sky Survey （SCUSS） was established in 2.09 in order to provide a photometric input catalog for target selection of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope （LAMOST） project. SCUSS is an international cooperative project between National astronomical Observatories, Chinese Academy of Sciences, and Steward observatory at the University of Arizona, using the 90 inch （2.3 m） Bok telescope on Kitt Peak. The telescope is equipped with a prime focus camera that is composed of a mosaic of four 4096 × 4096 CCDs and has a field of view of about 1 deg2. From 2.09 to {2.3, SCUSS performed a sky survey of an approximately 5000 deg2.field of the South Galactic Cap in u band, including the Galactic anticenter area and the SDSS-IV extended imaging area. The limiting magnitude of SCUSS is deeper than 2. mag （at a signal-to-noise ratio of 5）. In this paper, we briefly describe the goals of this project, method of observations and data reduction, and we also introduce current and potential scientific activities related to the SCUSS project.

关键词： observation: sky survey -- techniques: data reduction -- objects: stars and galaxies

The first data release(DR1) of the LAMOST regular survey

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Research in Astronomy and Astrophysics 2015年第8期15卷 1095-1124页

作者： A-li Luo Yong-Heng Zhao Gang Zhao li-Cai Deng Xiao-Wei liu Yi-Peng Jing Gang Wang Hao-Tong Zhang Jian-Rong Shi Xiang-Qun Cui Yao-Quan Chu Guo-Ping li Zhong-Rui Bai yue wu Yan Cai Shu-yun Cao Zi-Huang Cao Jeffrey L.Carlin Hai-yuan Chen Jian-Jun Chen Kun-Xin Chen li Chen Xue-Lei Chen Xiao-Yan Chen Ying Chen Norbert Christlieb Jia-Ru Chu Chen-Zhou Cui Yi-Qiao Dong Bing Du Dong-Wei Fan Lei Feng Jian-Ning Fu Peng Gao Xue-Fei Gong Bo-Zhong Gu Yan-Xin Guo Zhan-Wen Han Bo-liang He Jin-liang Hou Yong-Hui Hou Wen Hou Hong-Zhuan Hu Ning-Sheng Hu Zhong-Wen Hu Zhi-Ying Huo Lei Jia Fang-Hua Jiang Xiang Jiang Zhi-Bo Jiang Ge Jin Xiao Kong Xu Kong Ya-Juan Lei Ai-Hua li Chang-Hua li Guang-Wei li Hai-Ning li Jian li Qi li Shuang li Sha-Sha li Xin-Nan li Yan li Yin-Bi li Ye-Ping li yuan liang Chien-Cheng lin Chao liu Gen-Rong liu Guan-Qun liu Zhi-Gang liu Wen-Zhi Lu yu Luo Yin-Dun Mao Heidi Newberg Ji-Jun Ni Zhao-Xiang Qi Yong-Jun Qi Shi-Yin Shen Huo-Ming Shi Jing Song Yi-Han Song Ding-Qiang Su Hong-Jun Su Zheng-Hong Tang Qing-Sheng Tao yuan Tian Dan Wang Da-Qi Wang Feng-Fei Wang Guo-Min Wang Hai Wang Hong-Chi Wang Jian Wang Jia-Ning Wang Jian-ling Wang Jian-Ping Wang Jun-Xian Wang Lei Wang Meng-Xin Wang Shou-Guan Wang Shu-Qing Wang Xia Wang Ya-Nan Wang You Wang yue-Fei Wang You-Fen Wang Peng Wei Ming-Zhi Wei Hong wu Ke-Fei wu Xue-Bing wu yu-Zhong wu Xiao-Zheng Xing ling-Zhe Xu Xin-Qi Xu Yan Xu Tai-Sheng Yan De-Hua Yang Hai-Feng Yang Hui-Qin Yang Ming Yang Zheng-Qiu Yao Yong yu Hui yuan Hai-Bo yuan Hai-Long yuan Wei-Min yuan Chao Zhai En-Peng Zhang Hua-Wei Zhang Jian-Nan Zhang li-Pin Zhang Wei Zhang Yong Zhang Yan-Xia Zhang Zheng-Chao Zhang Ming Zhao Fang Zhou Xu Zhou Jie Zhu Yong-Tian Zhu Si-Cheng Zou Fang Zuo National astronomical Observatories Chinese Academy of Sciences Department of Astronomy Peking University shanghai astronomical {2. Chinese Academy of Sciences Nanjing Institute of astronomical Optics & Technology National Astronomical ObservatoriesChinese Academy of Sciences University of Science and Technology of china Department of Physics Applied Physics and AstronomyRensselaer Polytechnic InstituteTroyNY 12180USA Department of Physics and Astronomy Earlham CollegeRichmondIN 47374USA Universitt Heidelberg Zentrum für AstronomieLandessternwarteKnigstuhl 1269117 HeidelbergGermany Department of Astronomy Beijing Normal University yunnan Observatories Chinese Academy of Sciences Purple Mountain observatory Chinese Academy of Sciences

The Large sky Area Multi-Object Fiber Spectroscopic Telescope（LAMOST） general survey is a spectroscopic survey that will eventually cover approximately half of the celestial sphere and collect 10 million spectra of stars, galaxies and QSOs. Objects in both the pilot survey and the first year regular survey are included in the LAMOST DR1. The pilot survey started in October 2.11 and ended in June 2.12. and the data have been released to the public as the LAMOST Pilot Data Release in August 2.12. The regular survey started in September 2.12. and completed its first year of operation in June 2.13. The LAMOST DR1 includes a total of 12.2.plates containing 2.955 336 spectra, of which 1 790 879 spectra have observed signalto-noise ratio（SNR） ≥ 10. All data with SNR ≥ 2.are formally released as LAMOST DR1 under the LAMOST data policy. This data release contains a total of 2.2.4 696 spectra, of which 1 944 32. are stellar spectra, 12.082.are galaxy spectra and 5017 are quasars. The DR1 not only includes spectra, but also three stellar catalogs with measured parameters： late A,FGK-type stars with high quality spectra（1 061 918 entries）, A-type stars（100 073 entries）, and M-type stars（12. 52. entries）. This paper introduces the survey design, the observational and instrumental limitations, data reduction and analysis, and some caveats. A description of the FITS structure of spectral files and parameter catalogs is also provided.

关键词： techniques: spectroscopic survey—data release—catalog

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高时间稳定性的雪崩光电二极管单光子探测器

物理学报 2020年第7期69卷 68-73页

作者：张海燕汪琳莉吴琛怡王煜蓉杨雷潘海峰刘巧莉郭霞汤凯张忠萍吴光华东师范大学精密光谱科学与技术国家重点实验室上海200062 北京邮电大学电子工程学院北京100876 中国科学院上海天文台上海200030

雪崩光电二极管单光子探测器是一种具有超高灵敏度的光电探测器件,在远距离激光测距、激光成像和量子通信等领域有非常重要的应用.然而,由于雪崩光电二极管单光子探测器的雪崩点对工作温度高度敏感,因此在外场环境下工作时容易出现增益... 详细信息

雪崩光电二极管单光子探测器是一种具有超高灵敏度的光电探测器件,在远距离激光测距、激光成像和量子通信等领域有非常重要的应用.然而,由于雪崩光电二极管单光子探测器的雪崩点对工作温度高度敏感,因此在外场环境下工作时容易出现增益波动,继而导致单光子探测器输出信号的延时发生漂移,严重降低了探测器的时间稳定性.本文发展了一种稳定输出延时的方法,采用嵌入式系统控制雪崩光电二极管,使其处于恒定温度,并实时补偿由环境温度引起的延时漂移,实现了雪崩光电二极管单光子探测器的高时间稳定性探测.实验中,环境温度从16 ℃变化到36 ℃,雪崩光电二极管的工作温度稳定在15 ℃,经过延时补偿,雪崩光电二极管单光子探测器输出延时漂移小于±1 ps,时间稳定度达到0.15 ps@100 s.这项工作有望为全天候野外条件和空间极端条件下的高精度单光子探测应用提供有效的解决方法.

关键词：单光子探测雪崩光电二极管时间稳定度延时漂移

The Solar Upper Transition Region Imager(SUTRI)Onboard the SATech-01 Satellite

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Research in Astronomy and Astrophysics 2023年第6期23卷 153-171页

作者： Xianyong Bai Hui Tian yuanyong Deng Zhanshan Wang Jianfeng Yang Xiaofeng Zhang Yonghe Zhang Runze Qi Nange Wang Yang Gao Jun yu Chunling He Zhengxiang Shen Lun Shen Song Guo Zhenyong Hou Kaifan Ji Xingzi Bi Wei Duan Xiao Yang Jiaben lin Ziyao Hu Qian Song Zihao Yang Yajie Chen Weidong Qiao Wei Ge Fu li Lei Jin Jiawei He Xiaobo Chen Xiaocheng Zhu Junwang He Qi Shi liu liu Jinsong li Dongxiao Xu Rui liu Taijie li Zhenggong Feng Yamin Wang Chengcheng Fan Shuo liu Sifan Guo Zheng Sun yuchuan wu Haiyu li Qi Yang yuyang Ye Weichen Gu Jiali wu Zhe Zhang yue yu Zeyi Ye Pengfeng Sheng Yifan Wang Wenbin li Qiushi Huang Zhong Zhang National astronomical Observatories Chinese Academy of SciencesBeijing 100101China School of Astronomy and Space Science University of Chinese Academy of SciencesBeijing 101408China School of Earth and Space Sciences Peking UniversityBeijing 100871China Key Laboratory of Solar Activity and Space Weather National Space Science CenterChinese Academy of SciencesBeijing 100190China Tongji University Institute of Precision Optical EngineeringSchool of Physics Science and EngineeringKey Laboratory of Advanced Micro-Structured Materials MOEShanghaiChina Xi'an Institute of Optics and Precision Mechanics Chinese Academy of SciencesXi'an 710119China Innovation Academy for Microsatellites Chinese Academy of SciencesShanghai 201304China yunnan Observatories Chinese Academy of SciencesKunming650011China

The Solar Upper Transition Region Imager(SUTRI)onboard the Space Advanced Technology demonstration satellite(SATech-01),which was launched to a Sun-synchronous orbit at a height of~500 km in 2.2. July,aims to test the on-orbit performance of our newly developed Sc/Si multi-layer reflecting mirror and the 2.×2. EUV CMOS imaging camera and to take full-disk solar images at the Ne VII 46.5 nm spectral line with a filter width of~3 *** employs a Ritchey-Chrétien optical system with an aperture of 18 *** on-orbit observations show that SUTRI images have a field of view of~416×416 and a moderate spatial resolution of~8″without an image stabilization *** normal cadence of SUTRI images is 30 s and the solar observation time is about16 hr each day because the earth eclipse time accounts for about 1/3 of SATech-01's orbit ***15 GB data is acquired each day and made available online after *** images are valuable as the Ne VII 46.5 nm line is formed at a temperature regime of~0.5 MK in the solar atmosphere,which has rarely been sampled by existing solar *** observations will establish connections between structures in the lower solar atmosphere and corona,and advance our understanding of various types of solar activity such as flares,filament eruptions,coronal jets and coronal mass ejections.

关键词： Sun:transition region Sun:UV radiation Sun:activity space vehicles:instruments