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Reduction of Tat-interacting Protein 30 Expression Could be a Prognostic Marker in Bladder Urothelial Cancer

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Chinese Medical Journal 2018年第2期131卷 188-193页

作者： ye-ping li Jian-Fang Zhu Ka-TeHuang Rong-Rong Wang Bing Cai Hui Xie Hong-De Chen Department of Urology The First Affiliated Hospital of Wenzhou Medical University Wenzhou Zhejiang 325000 China Department of Vascular Surgery The Second Hospital of Shaoxing City Shaoxing Zhejiang 312000 China Department of Pathology The First Affiliated Hospital of Wenzhou Medical University Wenzhou Zhejiang 325000 China

Background： Tat-interacting protein 30 （TIP30） has been reported to be a tumor suppressor, with reduced or absent expression in various tumors. However, its role in bladder urothelial cancer （BUC） has not been investigated. Therefore, herein, we investigated the expression of T1P30 protein in BUC and normal bladder mucosa and the clinical significance of TIP30 expression in the prognosis of BUC. Methods： We reviewed data from 79 cases of BUC and 15 adjacent tissue samples from 79 patients treated at our institution between 2004 and 2007. TIP30 expression was examined by immunohistochemistry. The relationship between TIP30 expression and tumor stage, histological grade, and survival was analyzed. Differences between groups were evaluated using the t-test or matched-pairs test, and differences in the survival rates were analyzed with the log-rank test. Results： TIP30 protein expression was significantly reduced in BUC tissue （t = -6.91, P 〈 0.05） compared with normal tissue samples, and in invasive bladder cancer （t = 10.89, P 〈 0.05） compared with superficial bladder cancer. TIP30 protein expression differed significantly among different differentiated groups classified either according to the World Health Organization （2004, F = 17.48, P 〈 0.01） or World Health Organization （1973, F = 10.68, P 〈 0.01）. TIP30 protein expression was significantly reduced in high-grade papillary urothelial carcinoma compared with papillary urothelial neoplasm of low malignant potential （P 〈 0.05） and low-grade papillary urothelial carcinoma （P 〈 0.05）. Meanwhile, TIP30 protein expression was significantly reduced in Grade 111 BUC, compared with Grade I （P 〈 0.05） and Grade 11 （P 〈 0.05）. Patients with low T1P30 expression showed a higher incidence of disease progression than those with high TIP30 expression （t - 2.63, P 〈 0.05）. Kaplan-Meier survival analysis showed a strong positive relationship between TIP30 expression and overall survival （OS）（x^2 = 17.29, P 〈 0.05）. Conclusions： TIP30 expression was associated with clinical tum

关键词： Bladder Urothelial Cancer Overall Survival Time Tat-interacting Protein 30

Focal surface attitude detection for LAMOST

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Research in Astronomy and Astrophysics 2020年第11期20卷 263-272页

作者： Tian-Zhu Hu Yong Zhang Xiang-Qun Cui ye-ping li Xiu-Shan Pan Ying Fu National Astronomical Observatories/Nanjing Institute of Astronomical Optics&Technology Chinese Academy of ScienceNanjing 210042China CAS Key Laboratory of Astronomical Optics&Technology Nanjing Institute of Astronomical Optics&TechnologyNanjing 210042China University of Chinese Academy of Sciences Beijing 100049China

With telescope apertures becoming larger and larger,the deployment of large-field telescopes is becoming increasingly popular.However,optical path calibration is necessary to ensure the image quality of large-field and large-diameter telescopes.In particular,focal plane attitude calibration is an essential optical path calibration technique that has a direct impact on image quality.In this paper,a focal plane attitude detection method using eight acquisition cameras is proposed based on the calibration requirements of the wide-field telescope,LAMOST(Large Sky Area Multi-Object Fiber Spectroscopic Telescope).Comparison of simulation and experimental results shows that the detection accuracy of the proposed method can reach 30 arcsec.With additional testing and verification,this method could be used to facilitate regular focal plane attitude calibration for LAMOST as well as other large-field telescopes.

关键词： methods data analysis techniques high angular resolution techniques image processing

Preliminary study of a dispersed fringe type sensing system

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Research in Astronomy and Astrophysics 2009年第8期9卷 945-952页

作者： Yong Zhang Gen-Rong liu Yue-Fei Wang ye-ping li Ya-Jun Zhang liang Zhan-g National Astronomical Observatories / Nanjing Institute of Astronomical Optics ＆ Technology Chinese Academy of Sciences Nanjing 210042 China Key Laboratory of Astronomical Optics ＆ Technology Nanjing Institute of Astronomical Optics ＆ Technology Chinese Academy of Sciences Nanjing 210042 China Graduate University of Chinese Academy of Sciences Beijing 100049 China

Telescopes with large aspherical primary mirrors collect more light and are therefore sought after by astronomers. Instead of using a single large one-piece mirror, smaller segments can be assembled into a useable telescopic primary. Because the segments must fit together to create the effect of a single mirror, segmented optics present unique challenges to the fabrication and testing that are absent in monolithic optics. A dispersed fringe sensor （DFS） using a broadband point source is an efficient method for cophasing and is also highly automated and robust. Unlike the widely adopted Shack- Hartmann Wavefront sensor and curvature wavefront sensor with edge sensors for calibration of relative pistons, DFS can estimate the piston between segments by only using the spectrum formed by the transmissive grating＇s dispersion, and therefore can replace the edge sensors, which are difficult to calibrate. We introduce the theory of the DFS and Dispersed Hartmann Sensor （DHS） for further utilization of the coarse phasing method of DFS. According to the theory, we bring out the preliminary system design of the cophasing experimental system based on DFS and DHS which is now established in our institute. Finally, a summary is reached.

关键词： instrumentation active optics -- techniques image processing -- tech- niques spectroscopic -- telescope cophasing sensor

An experimental indoor phasing system based on active optics using dispersed Hartmann sensing technology in the visible waveband

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Research in Astronomy and Astrophysics 2011年第9期11卷 1111-1122页

作者： Yong Zhang Gen-Rong liu Yue-Fei Wang ye-ping li Ya-Jun Zhang liang Zhang Yi-Zhong Zeng Jie Zhang National Astronomical Observatories / Nanjing Institute of Astronomical Optics ＆ Technology Chinese Academy of Sciences Nanjing 210042 China Key Laboratory of Astronomical Optics ＆ Technology Nanjing Institute of Astronomical Optics ＆ Technology Chinese Academy of Sciences Nanjing 210042 China Graduate University of Chinese Academy of Sciences Beijing 100049 China

A telescope with a larger primary mirror can collect much more light and resolve objects much better than one with a smaller mirror, and so the larger version is always pursued by astronomers and astronomical technicians. Instead of using a monolithic primary mirror, more and more large telescopes, which are currently being planned or in construction, have adopted a segmented primary mirror design. Therefore, how to sense and phase such a primary mirror is a key issue for the future of extremely large optical/infrared telescopes. The Dispersed Fringe Sensor （DFS）, or Dispersed Hartmann Sensor （DHS）, is a non-contact method using broadband point light sources and it can estimate the piston by the two-directional spectrum formed by the transmissive grating＇s dispersion and lenslet array. Thus it can implement the combination of co-focusing by Shack-Hartmann technology and phasing by dispersed fringe sensing technologies such as the template-mapping method and the Hartmann method. We introduce the successful design, construction and alignment of our dis- persed Hartmann sensor together with its design principles and simulations. We also conduct many successful real phasing tests and phasing corrections in the visible waveband using our existing indoor segmented mirror optics platform. Finally, some conclusions are reached based on the test and correction of experimental results.

关键词： astronomical instrumentation -- methods and techniques -- instrumen- tation： active optics -- adaptive optics

Double casing warhead with sandwiched charge:The axial distribution of fragments velocities

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Defence Technology（防务技术） 2024年第4期34卷 201-216页

作者： ping ye Yongxiang Dong Qitian Sun Peizhuo Shi Wang Yao Yongnan li Yujing li Mingze li State Key Laboratory of Explosion Science and Technology Beijing Institute of TechnologyBeijing 100081China

The double casing warhead with sandwiched charge is a novel fragmentation warhead that can produce two groups of fragments with different velocity,and the previous work has presented a calculation formula to determine the maximum fragment velocity.The current work builds on the published formula to further develop a formula for calculating the axial distribution characteristics of the fragment velocity.For this type of warhead,the simulation of the dispersion characteristics of the detonation products at different positions shows that the detonation products at the ends have a much larger axial velocity than those in the middle,and the detonation products have a greater axial dispersion velocity when they are closer to the central axis.The loading process and the fragment velocity vary with the axial position for both casing layers,and the total velocity of the fragments is the vector sum of the radial velocity and the axial velocity.At the same axial position,the acceleration time of the inner casing is greater than that of the outer casing.For the same casing,the fragments generated at the ends have a longer acceleration time than the fragments from the middle.The proposed formula is validated with the X-ray radiography results of the four warheads previously tested experimentally and the 3D smoothedparticle hydrodynamics numerical simulation results of several series of new warheads with different configurations.The formula can accurately and reliably calculate the fragment velocity when the lengthto-diameter ratio of the charge is greater than 1.5 and the thickness of the casing is less than 20%its inner radius.This work thus provides a key reference for the theoretical analysis and the design of warheads with multiple casings.

关键词： Double casing warhead Sandwiched charge Fragment velocity Rarefaction wave Gurney formula Explosive loading

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基于时间最短的生鲜农产品配送路径规划系统

信息技术 2024年第4期48卷 100-105,114页

作者：吴卓葵江卓阳张文峰曾涛叶丽萍仲恺农业工程学院自动化学院广州510225 广东省农产品冷链运输与物流工程技术研究中心广州510225

合适的配送路径可缩短生鲜农产品的配送时间,有利于保证生鲜农产品的新鲜度和减少损耗。为了为生鲜农产品配送提供便利的路径规划服务,提出一种基于时间最短的生鲜农产品配送路径规划系统。系统以配送时间最短为路径规划目标,对分散的... 详细信息

合适的配送路径可缩短生鲜农产品的配送时间,有利于保证生鲜农产品的新鲜度和减少损耗。为了为生鲜农产品配送提供便利的路径规划服务,提出一种基于时间最短的生鲜农产品配送路径规划系统。系统以配送时间最短为路径规划目标,对分散的多个配送点的配送顺序进行最优排序。系统设计采用基于Node.js的Web开发方式和前后端分离的架构,实现生鲜农产品配送路径规划、配送方案实施和管理、生鲜农产品管理等功能。测试与应用结果表明,设计的系统可有效缩短生鲜农产品的配送时间,提高配送效率和降低配送成本。

关键词：路径规划时间最短生鲜农产品配送时间配送效率

Eight new quasars discovered by the Guoshoujing Telescope (LAMOST) in one extragalactic field

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Research in Astronomy and Astrophysics 2010年第8期10卷 745-752页

作者： Xue-Bing Wu Zhen-Dong Jia Zhao-Yu Chen 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 Sciences Nanjing 210042 China Center for Astrophysics University of Science ＆ Technology of China Hefei 230026 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China

We report the discovery of eight new quasars in one extragalactic field （a five-degree field centered at RA=08^h58^m08.2^s, Dec=01°32′29.7″） with the Guoshoujing Telescope （LAMOST） commissioning observations made on 2009 December 18. These quasars, with i magnitudes from 16.44 to 19.34 and redshifts from 0.898 to 2.773, were not identified in the SDSS spectroscopic survey, though six of them with redshifts less than 2.5 were selected as quasar targets in SDSS. Except for one source without near-IR Y-band data, seven of these eight new quasars satisfy a newly proposed quasar selection criterion involving both near-IR and optical colors. Two of them were found in the ＇redshift desert＇ for quasars （z from 2.2 to 3）, indicating that the new criterion is efficient for uncovering missing quasars with similar optical colors to stars. Although LAMOST encountered some problems during the commissioning observations, we were still able to identify 38 other known SDSS quasars in this field, with i magnitudes from 16.24 to 19.10 and redshifts from 0.297 to 4.512. Our identifications imply that a substantial fraction of quasars may be miss- ing in previous quasar surveys. The implication of our results to the future LAMOST quasar survey is discussed.

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

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 Observatory 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 2.427 by the Guoshoujing Telescope （LAMOST） commissioning observation in 2009 December and confirmed by the observation made with the NAOC/Xinglong 2.16 m telescope in 2010 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

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST)

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Research in Astronomy and Astrophysics 2012年第9期12卷 1197-1242页

作者： Xiang-Qun Cui Yong-Heng Zhao Yao-Quan Chu Guo-ping li Qi li li-ping Zhang Hong-Jun Su Zheng-Qiu Yao Ya-Nan Wang Xiao-Zheng Xing Xin-Nan li Yong-Tian Zhu Gang Wang Bo-Zhong Gu A-li Luo Xin-Qi Xu Zhen-Chao Zhang Gen-Rong liu Hao-Tong Zhang De-Hua Yang Shu-Yun Cao Hai-Yuan Chen Jian-Jun Chen Kun-Xin Chen Ying Chen Jia-Ru Chu Lei Feng Xue-Fei Gong Yong-Hui Hou Hong-Zhuan Hu Ning-Sheng Hu Zhong-Wen Hu Lei Jia Fang-Hua Jiang Xiang Jiang Zi-Bo Jiang Ge Jin Ai-Hua li Yan li ye-ping li Guan-Qunliu Zhi-Gang liu Huo-Ming Shi Zheng-Hong Tang Qing-Sheng Tao Xiang-Yan Yuan Chao Zhai Jing Zhang Yan-Xia Zhang Yong Zhang Ming Zhao Fang Zhou Guo-Hua Zhou Jie Zhu Si-Cheng Zou National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China yzhao @ *** Nanjing Institute of Astronomical Optics and Technology National Astronomical ObservatoriesChinese Academy of Sciences Nanjing 210042 China University of Science and Tecfinologyof China Hefei 230026 China Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai 200030 China Institute of Architecture Design and Research Chinese Academy of Sciences Beijing 100190China

The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, also called the Guo Shou Jing Telescope) is a special reflecting Schmidt telescope. LAMOST’s special design allows both a large aperture (effective aperture of 3.6 m–4.9 m) and a wide field of view (FOV) (5°). It has an innovative active reflecting Schmidt configuration which continuously changes the mirror’s surface that adjusts during the observation process and combines thin deformable mirror active optics with segmented active optics. Its primary mirror (6.67m×6.05 m) and active Schmidt mirror (5.74m×4.40 m) are both segmented, and composed of 37 and 24 hexagonal sub-mirrors respectively. By using a parallel controllable fiber positioning technique, the focal surface of 1.75 m in diameter can accommodate 4000 optical fibers. Also, LAMOST has 16 spectrographs with 32 CCD cameras. LAMOST will be the telescope with the highest rate of spectral acquisition. As a national large scientific project, the LAMOST project was formally proposed in 1996, and approved by the Chinese government in 1997. The construction started in 2001, was completed in 2008 and passed the official acceptance in June 2009. The LAMOST pilot survey was started in October 2011 and the spectroscopic survey will launch in September 2012. Up to now, LAMOST has released more than 480 000 spectra of objects. LAMOST will make an important contribution to the study of the large-scale structure of the Universe, structure and evolution of the Galaxy, and cross-identification of multiwaveband properties in celestial objects.

关键词： techniques: wide field telescope - active optics - multi fiber - spectroscopy survey - data reduction