Nather, RE; Winget, DE; Clemens, JC; et al.

Hubble deep field: Observations, data reduction,and galaxy photometry

Williams, RE; Blacker, B; Dickinson, M; et al.

The UKIRT Infrared Deep Sky Survey (UKIDSS)

Lawrence, A.; Warren, S. J.; Almaini, O; et al.

Herschel Space Observatory: An ESA facility for far-infrared and submillimetre astronomy

Pilbratt, G. L; Riedinger, J. R.; Passvogel, T;

FAST工程建設(shè)進(jìn)展

南仁東1,2，張海燕1,2，張瑩1，楊麗1，蔡文靜1，劉娜1，謝嘉彤1，張蜀新1

新一代大射電望遠(yuǎn)鏡機(jī)電光一體化設(shè)計研究

段寶巖，蘇玉鑫，仇原鷹，等

國家重大科技基礎(chǔ)設(shè)施：天文望遠(yuǎn)鏡

·編者按·

重大科技基礎(chǔ)設(shè)施是為探索未知世界、發(fā)現(xiàn)自然規(guī)律、實現(xiàn)技術(shù)變革、提供極限研究手段的大型復(fù)雜科學(xué)研究系統(tǒng)，是突破科學(xué)前沿、解決經(jīng)濟(jì)社會發(fā)展和國家安全重大科技問題的物質(zhì)技術(shù)基礎(chǔ)。它的發(fā)展?fàn)顩r是國家科技水平和綜合實力的重要標(biāo)志之一。

2013年2月，國務(wù)院印發(fā)的《國家重大科技基礎(chǔ)設(shè)施建設(shè)中長期規(guī)劃（2012—2030年）》指出，在空間和天文科學(xué)領(lǐng)域，要以揭示宇宙奧秘和解釋物質(zhì)運動規(guī)律為目標(biāo)，面向宇宙天體起源及演化、太陽活動及對地球的影響、空間環(huán)境與物質(zhì)作用等方向，按宇宙、星系、太陽系等不同空間尺度布局設(shè)施建設(shè)，提升我國天文觀測研究能力、空間天氣和災(zāi)害應(yīng)對能力以及空間科學(xué)實驗基礎(chǔ)能力。建成大口徑射電望遠(yuǎn)鏡，為宇宙大尺度結(jié)構(gòu)及物理規(guī)律研究提供支撐。

500米口徑球面射電望遠(yuǎn)鏡（FAST）工程是國家“十一五”重大科技基礎(chǔ)設(shè)施建設(shè)項目，被稱為“中國天眼”。該項目是利用貴州天然喀斯特洼地作為望遠(yuǎn)鏡臺址，建造世界第一大單口徑射電望遠(yuǎn)鏡——

500米口徑球冠狀主動反射面射電望遠(yuǎn)鏡，以實現(xiàn)大天區(qū)面積、高精度的天文觀測。FAST突破了射電望遠(yuǎn)鏡的百米極限，開創(chuàng)了建造巨型射電望遠(yuǎn)鏡的新模式。它擁有30個足球場大的接收面積，將是國際上最大的單口徑望遠(yuǎn)鏡。與號稱“地面最大的機(jī)器”的德國波恩100米望遠(yuǎn)鏡相比，靈敏度提高約10倍；與排在阿波羅登月之前、被評為人類20世紀(jì)10大工程之首的美國Arecibo 300米望遠(yuǎn)鏡相比，其綜合性能提高約10倍。FAST工程于2011年3月25日開工建設(shè)，2016年9月完工。

具有我國自主知識產(chǎn)權(quán)的FAST，它的研制和建設(shè)，體現(xiàn)了我國自主創(chuàng)新能力，還將推動我國在天線制造技術(shù)、微波電子技術(shù)、并聯(lián)機(jī)器人、大尺度結(jié)構(gòu)工程、公里范圍高精度動態(tài)測量等眾多高科技領(lǐng)域的發(fā)展。

本專題得到專家杜彪教授（中國電子科技集團(tuán)公司第五十四研究所；國家射電天文技術(shù)聯(lián)合實驗室）、黃穎教授（廣西柳工集團(tuán)歐維姆技術(shù)中心錨固技術(shù)研究所）的大力支持。

·熱點數(shù)據(jù)排行·

截至2017年9月23日，中國知網(wǎng)（CNKI）和Web of Science（WoS）的數(shù)據(jù)報告顯示，以“重大科技基礎(chǔ)設(shè)施（Major National Science and Technology Infrastructure Project）”“天文望遠(yuǎn)鏡（Astronomical Telescope）”“射電望遠(yuǎn)鏡（Radio Telescope）”“FAST（Five-hundred-meter Aperture Spherical radio Telescope）”為詞條可以檢索到的期刊文獻(xiàn)分別為762條與15801條，本專題將相關(guān)數(shù)據(jù)按照：研究機(jī)構(gòu)發(fā)文數(shù)、作者發(fā)文數(shù)、期刊發(fā)文數(shù)、被引用頻次進(jìn)行排行，結(jié)果如下。

研究機(jī)構(gòu)發(fā)文數(shù)量排名（CNKI）

研究機(jī)構(gòu)發(fā)文數(shù)量排名（WoS）

研究機(jī)構(gòu)發(fā)文數(shù)量排名（CNKI）（續(xù)表）

研究機(jī)構(gòu)發(fā)文數(shù)量排名（WoS）（續(xù)表）

作者發(fā)文數(shù)量排名（CNKI）

作者發(fā)文數(shù)量排名（WoS）

期刊發(fā)文數(shù)量排名（CNKI）

期刊發(fā)文數(shù)量排名（WoS）

根據(jù)中國知網(wǎng)（CNKI）數(shù)據(jù)報告，以“重大科技基礎(chǔ)設(shè)施（Major National Science and Technology Infrastructure Project）”“天文望遠(yuǎn)鏡（Astronomical Telescope）”“射電望遠(yuǎn)鏡（Radio Telescope）”“FAST（Five-hundred-meter Aperture Spherical radio Telescope）”為詞條可以檢索到的高被引論文排行結(jié)果如下。

國內(nèi)數(shù)據(jù)庫高被引論文排行

國內(nèi)數(shù)據(jù)庫高被引論文排行（續(xù)表）

根據(jù)中國知網(wǎng)（CNKI）數(shù)據(jù)報告，以“重大科技基礎(chǔ)設(shè)施（Major National Science and Technology Infrastructure Project）”“天文望遠(yuǎn)鏡（Astronomical Telescope）”“射電望遠(yuǎn)鏡（Radio Telescope）”“FAST（Five-hundred-meter Aperture Spherical radio Telescope）”為詞條可以檢索到的高被引論文排行結(jié)果如下。

國外數(shù)據(jù)庫高被引論文排行

·經(jīng)典文獻(xiàn)推薦·

基于Web of Science檢索結(jié)果，利用Histcite軟件選取LCS（Local Citation Score，本地引用次數(shù)）TOP50文獻(xiàn)作為節(jié)點進(jìn)行分析，得到本領(lǐng)域推薦的經(jīng)典文獻(xiàn)如下。

本領(lǐng)域經(jīng)典文獻(xiàn)

The whole earth telescope: A new astronomical instrument

Nather, RE; Winget, DE; Clemens, JC; et al.

Hubble deep field: Observations, data reduction,and galaxy photometry

Williams, RE; Blacker, B; Dickinson, M; et al.

The UKIRT Infrared Deep Sky Survey (UKIDSS)

Lawrence, A.; Warren, S. J.; Almaini, O; et al.

來源出版物：Monthly Notices of the Royal Astronomical Society, 2007, 379(4): 1599-1617

Herschel Space Observatory: An ESA facility for far-infrared and submillimetre astronomy

Pilbratt, G. L; Riedinger, J. R.; Passvogel, T;

Abstract:Herschel was launched on 14 May 2009, and is now an operational ESA space observatory offering unprecedented observational capabilities in the far-infrared and submillimetre spectral range 55-671 μm. Herschel carries a 3.5 m diameter passively cooled Cassegrain telescope, which is the largest of its kind and utilises a novel silicon carbide technology. The science payload comprises three instruments: two direct detection cameras/medium resolution spectrometers, PACS and SPIRE, and a very high-resolution heterodyne spectrometer, HIFI, whose focal plane units are housed inside a superfluid helium cryostat. Herschel is an observatory facility operated in partnership among ESA, the instrument consortia, and NASA. The mission lifetime is determined by the cryostat hold time. Nominally approximately 20000 h will be available for astronomy, 32% is guaranteed time and the remainder is open to the worldwide general astronomical community through a standard competitive proposal procedure.

Key words:space vehicles; space vehicle; instruments;infrared; general; submillimetre; general

來源出版物：Astronomy & Astrophysics, 2010, 518(3):383-416

·推薦綜述·

FAST工程建設(shè)進(jìn)展

南仁東1,2，張海燕1,2，張瑩1，楊麗1，蔡文靜1，劉娜1，謝嘉彤1，張蜀新1

1 引言

1993年，國際無線電科聯(lián)（URSI）京都大會上，包括中國在內(nèi)的10國射電天文學(xué)家聯(lián)合發(fā)起了新一代射電“大望遠(yuǎn)鏡”（Large Telescope，簡稱LT）的倡議，1999年易名為平方公里陣列（Square Kilometer Array，SKA），即接收面積為1 km2的巨型射電望遠(yuǎn)鏡，它的靈敏度將比目前世界上最大的射電望遠(yuǎn)鏡高2個數(shù)量級。這個將由多國合作建設(shè)的望遠(yuǎn)鏡陣列，總投資約10億美元，計劃建設(shè)10年，期望能在2020年后建成，至少運行50年，因此又被稱為“21世紀(jì)的國際射電望遠(yuǎn)鏡”。

1995年底，以北京天文臺（現(xiàn)國家天文臺）為主，聯(lián)合國內(nèi)20余家大學(xué)和研究所成立了LT中國推進(jìn)委員會，提出了利用中國貴州喀斯特（KARST）洼地，建造球反射面即Arecibo型天線陣的KARST工程概念。此天線陣由30余面口徑約300 m的球面天線組成，它將分布于方圓數(shù)百公里的范圍內(nèi)，具有1′至100μαs的多級分辨率，將從本質(zhì)上改善展源的射電天文成像能力。中國科學(xué)家為進(jìn)一步推進(jìn)KARST概念，提出獨立研制一臺新型的KARST單元：500 m口徑主動球反射面望遠(yuǎn)鏡，即FAST。

2 工程簡介

2.1 FAST科學(xué)目標(biāo)

FAST具有極其重大的科學(xué)意義。它以接收面積為突破方向，可觀測的天體數(shù)目將大幅度增加，可為科學(xué)家提供更多、更好的觀測統(tǒng)計樣本，更可靠地檢驗現(xiàn)代物理學(xué)、天文學(xué)的理論和模型；它將搜尋到更多的奇異天體，其中蘊涵著大量新發(fā)現(xiàn)的機(jī)會。它的研究涵蓋廣泛的天文學(xué)內(nèi)容，從宇宙初始混濁、暗物質(zhì)暗能量與大尺度結(jié)構(gòu)、星系與銀河系的演化、恒星類天體，到太陽系行星與鄰近空間事件等的觀測研究。FAST擬回答的科學(xué)問題不僅是天文的，也是面對人類與自然的，它潛在的科學(xué)產(chǎn)出也許我們今天還難以預(yù)測。FAST主要的科學(xué)目標(biāo)包括：1）巡視宇宙中的中性氫，研究宇宙大尺度物理學(xué)，以探索宇宙起源和演化；2）觀測脈沖星，研究極端狀態(tài)下的物質(zhì)結(jié)構(gòu)與物理規(guī)律；3）主導(dǎo)國際低頻甚長基線干涉測量網(wǎng)，獲得天體超精細(xì)結(jié)構(gòu)；4）探測星際分子；5）搜索可能的星際通訊信號。

FAST在國家重大需求方面也有重要應(yīng)用價值。它可將我國空間測控能力由月球延伸至太陽系外緣，將深空通訊數(shù)據(jù)下行速率提高幾十倍。脈沖星到達(dá)時間測量精度由目前的120 ns提高至30 ns，成為國際上最精確的脈沖星計時陣，為自主導(dǎo)航這一前瞻性研究制作脈沖星鐘；進(jìn)行高分辨率微波巡視，以1 Hz的分辨率診斷識別微弱的空間訊號。

FAST可作為國家重大科學(xué)工程“東半球空間環(huán)境地基綜合檢測子午鏈（子午工程）”的非相干散射雷達(dá)接收系統(tǒng)，提高分辨率和觀測效率；跟蹤探測日冕物質(zhì)拋射事件，服務(wù)于空間天氣預(yù)報。

2.2 FAST創(chuàng)新與突破

FAST與國際上已有的巨型單口徑射電望遠(yuǎn)鏡相比，有3項主要特色：用貴州省境內(nèi)喀斯特地貌中的天然洼坑作為臺址；洼坑內(nèi)鋪設(shè)數(shù)千塊單元，構(gòu)成500 m球冠狀主動反射面，球冠反射面在射電源方向形成300 m口徑瞬時拋物面，使望遠(yuǎn)鏡接收機(jī)能與傳統(tǒng)拋物面天線一樣處在焦點上；采用輕型索拖動機(jī)構(gòu)和并聯(lián)機(jī)器人，實現(xiàn)接收機(jī)的高精度定位。

攜全新設(shè)計思路加得天獨厚的臺址優(yōu)勢，F(xiàn)AST突破了射電望遠(yuǎn)鏡的百米極限，開創(chuàng)了建造巨型射電望遠(yuǎn)鏡的新模式。它將擁有30個足球場大的接收面積，成為國際上最大的單口徑望遠(yuǎn)鏡，在10～20年內(nèi)處于國際領(lǐng)先地位。

2.3 FAST工程目標(biāo)與內(nèi)容

FAST工程在貴州喀斯特洼地內(nèi)鋪設(shè)口徑為500 m的球冠形主動反射面，通過主動控制在觀測方向形成300 m口徑瞬時拋物面；采用光機(jī)電一體化的索支撐輕型饋源平臺，加之饋源艙內(nèi)的二次調(diào)整裝置，在饋源與反射面之間無剛性連接的情況下，實現(xiàn)高精度的指向跟蹤；在饋源艙內(nèi)配置覆蓋頻率70 MHz～3 GHz的多波段、多波束饋源和接收機(jī)系統(tǒng)；針對科學(xué)目標(biāo)發(fā)展不同用途的終端設(shè)備；建造一流的天文觀測站。

為實現(xiàn)上述建設(shè)目標(biāo)，我們需要完成以下6項主要建設(shè)內(nèi)容：1）臺址勘察與開挖：查清臺址工程地質(zhì)和水文地質(zhì)條件，開挖清理洼地，使其滿足望遠(yuǎn)鏡建設(shè)的需要。2）主動反射面：建設(shè)上萬根鋼索和數(shù)千個反射單元組成的球冠型索膜結(jié)構(gòu)，口徑約500 m，球冠張角110°～120°，拋物面變形的均方差為5 mm。3）饋源支撐系統(tǒng)：建設(shè)公里尺度的鋼索支撐體系，在饋源艙內(nèi)安裝并聯(lián)機(jī)器人用于二級調(diào)整，最終調(diào)整定位精度為10 mm。4）測量與控制：建設(shè)洼地基準(zhǔn)網(wǎng)和基準(zhǔn)站、激光全站儀和近景測量系統(tǒng)，百米距離測量精度2 mm，采用現(xiàn)場總線技術(shù)實現(xiàn)數(shù)千點自動控制。5）接收機(jī)與終端：研制高性能的多波束饋源接收機(jī)，頻率覆蓋70 MHz～3 GHz。研制饋源、低噪聲致冷放大器、寬頻帶數(shù)字中頻傳輸設(shè)備、高穩(wěn)定度的時鐘和高精度的頻率標(biāo)準(zhǔn)設(shè)備等。配置多用途數(shù)字天文終端設(shè)備。6）觀測基地建設(shè)：建立望遠(yuǎn)鏡觀測室、終端設(shè)備室、數(shù)據(jù)處理中心、各關(guān)鍵技術(shù)實驗室、辦公樓和綜合服務(wù)體系等。

3 FAST工程進(jìn)展

自2011年3月FAST開工報告批復(fù)以后，F(xiàn)AST項目正式進(jìn)入工程實施階段，主體工程介紹如下。

3.1 臺址開挖與邊坡治理

在前期多年艱苦選址工作基礎(chǔ)上，從300余個候選洼地中選出了位于貴州省黔南苗族布依族自治州平塘縣克度鎮(zhèn)金科村大窩凼作為FAST臺址。

臺址勘察與開挖系統(tǒng)完成了地形圖測繪、臺址勘察、施工圖設(shè)計、臺址開挖及臺址監(jiān)測系統(tǒng)建設(shè)等主要工程任務(wù)。2010年3月完成了臺址詳勘，隨后對臺址巖土工程進(jìn)行了專項勘察。得到兩項勘察報告后，2011年3月臺址開挖工作正式啟動，2012年12月，F(xiàn)AST臺址開挖與邊坡治理工程通過驗收。

3.2 主動反射面系統(tǒng)

主動反射面系統(tǒng)主要由約500 m直徑的圈梁，6670根鋼索構(gòu)成的主索網(wǎng)，4300塊邊長約11 m的三角形反射面單元，2225根下拉索、地錨及促動器構(gòu)成。

圈梁是FAST索網(wǎng)的支撐結(jié)構(gòu)，由承臺基礎(chǔ)、格構(gòu)柱及環(huán)梁構(gòu)成，形成直徑為500 m的圓周。2014年9月11日，圈梁制造和安裝工程完工并通過驗收。

FAST索網(wǎng)是世界上跨度最大、精度最高的索網(wǎng)結(jié)構(gòu)，也是世界上第1個采用變位工作方式的索網(wǎng)體系。索網(wǎng)結(jié)構(gòu)是FAST主動反射面的主要支撐結(jié)構(gòu)，是反射面主動變位工作的關(guān)鍵點。索網(wǎng)制造與安裝工程也是500 m口徑球面射電望遠(yuǎn)鏡工程的主要技術(shù)難點之一。索網(wǎng)工程于2014年7月17日正式開始，于2015年2月4日順利完成合攏。

FAST圈梁及索網(wǎng)工程獲“中國鋼結(jié)構(gòu)協(xié)會科學(xué)技術(shù)獎”特等獎，意味著FAST工程己經(jīng)在上述關(guān)鍵技術(shù)難點方面實現(xiàn)實質(zhì)性突破，也為我國相關(guān)產(chǎn)業(yè)技術(shù)水平的提升做出重要貢獻(xiàn)。

FAST反射面單元主要由面板單元、背架、調(diào)整裝置、連接機(jī)構(gòu)等組成，有187個種類，考慮到反射面單元為空間結(jié)構(gòu)不能鏡像，實際種類為342種。2015年8月2日，第1塊拼裝檢測合格的反射面單元在FAST工程現(xiàn)場成功吊裝，F(xiàn)AST工程建設(shè)進(jìn)入最后沖刺階段，2016年7月3日最后一片反射面板吊裝完成，標(biāo)志著FAST工程主體工程的順利完工。

反射面液壓促動器在上位控制系統(tǒng)的控制下，通過液壓促動器活塞桿的伸縮實現(xiàn)精確定位、協(xié)同運動，通過調(diào)整下拉索下端的位置，從而間接同步調(diào)整索網(wǎng)節(jié)點位置，實時實現(xiàn)滿足擬合精度的300 m口徑瞬時拋物面，實現(xiàn)天文觀測的跟蹤，換源等運動要求。2015年7月完成了全部促動器的制造、現(xiàn)場安裝和調(diào)試工作。

3.3 饋源支撐系統(tǒng)

饋源支撐系統(tǒng)主要由6座百米高的支撐塔、6套公里尺度的柔性鋼索體系及驅(qū)動裝置、1個重約30噸的饋源艙和1座直徑約20 m的艙?？科脚_構(gòu)成。

最先進(jìn)入施工的6基饋源支撐塔是FAST饋源支撐系統(tǒng)的主體承載結(jié)構(gòu)，是鋼索承載和驅(qū)動的依托支架，并為塔頂導(dǎo)向滑輪提供足夠剛性的支撐平臺，保證驅(qū)動鋼索能夠牽引饋源艙在預(yù)定軌跡上運動。饋源塔制造與安裝工程于2014年3月15日正式開始現(xiàn)場安裝工作，2014年11月30日通過竣工驗收。

索驅(qū)動作為世界上在建的最大繩牽引并聯(lián)機(jī)構(gòu)，是FAST工程的三大自主創(chuàng)新技術(shù)之一它由驅(qū)動機(jī)構(gòu)、導(dǎo)向機(jī)構(gòu)、纜索裝置、控制系統(tǒng)、設(shè)備基礎(chǔ)及其他附屬設(shè)施組成。2015年2月10日，F(xiàn)AST望遠(yuǎn)鏡索驅(qū)動第1根支撐索安裝成功。2015年11月完成六索驅(qū)動機(jī)構(gòu)的安裝工作，進(jìn)入六索聯(lián)調(diào)階段。

饋源艙是饋源支撐系統(tǒng)的核心部件，主要包括星形框架、AB軸機(jī)構(gòu)、Stewart平臺、多波束接收機(jī)轉(zhuǎn)向裝置、艙罩和其他附屬設(shè)備/設(shè)施等。2014年10月，饋源艙的代艙開始在大窩凼現(xiàn)場進(jìn)行安裝，隨后配合索驅(qū)動的調(diào)試試驗。2015年3月，代艙完成預(yù)驗收。代艙作為饋源艙的代替艙，主要用于FAST的前期調(diào)試和試驗。2015年11月21日上午11時，F(xiàn)AST望遠(yuǎn)鏡饋源支撐系統(tǒng)首次升艙成功，這標(biāo)志著FAST工程饋源支撐系統(tǒng)正式進(jìn)入六索帶載聯(lián)調(diào)階段。

3.4 測量與控制系統(tǒng)

測量與控制系統(tǒng)主要包括基礎(chǔ)測量、主動反射面測控、饋源位姿測控及望遠(yuǎn)鏡總控4個部分。要求對FAST進(jìn)行精確、快速、遠(yuǎn)距離的非接觸測量和對主反射面進(jìn)行實時控制。

測量基墩是FAST工程測量與控制系統(tǒng)的主體建筑。通過在大窩凼洼地內(nèi)建造24個伸出反射面的基墩，為高精度測量儀器提供穩(wěn)定可靠的安裝平臺，完成對反射面節(jié)點位置和饋源艙位姿測量，為反射面和饋源支撐控制提供測量數(shù)據(jù)。該工程于2013年5月開始建造，2014年10月16日竣工驗收。

望遠(yuǎn)鏡總控系統(tǒng)聯(lián)系、協(xié)調(diào)和控制各子系統(tǒng)操作，并監(jiān)測各部件運行狀態(tài)，排除故障，收集記錄運行數(shù)據(jù)，以及提供統(tǒng)一的時間標(biāo)準(zhǔn)。饋源支撐整體控制系統(tǒng)的主要功能有饋源支撐測量數(shù)據(jù)處理、天文軌跡規(guī)劃、饋源支撐整體控制和系統(tǒng)校時。主動反射面控制系統(tǒng)主要目標(biāo)是根據(jù)天文軌跡規(guī)劃和測量數(shù)據(jù)，通過調(diào)整促動器的伸長量控制反射面節(jié)點位置，形成位置和面型準(zhǔn)確的拋物面?？刂葡到y(tǒng)接收總控系統(tǒng)發(fā)來的天文觀測指令及時鐘信息，并綜合反射面測量和健康監(jiān)測系統(tǒng)的數(shù)據(jù)實現(xiàn)對2225個促動器進(jìn)行控制。目前，各分部工作全部完成，正在進(jìn)行系統(tǒng)聯(lián)調(diào)。

3.5 接收機(jī)與終端系統(tǒng)

接收機(jī)與終端系統(tǒng)包括頻率覆蓋70 MHz～3 GHz的7套接收機(jī)及終端，時間頻率標(biāo)準(zhǔn)、數(shù)據(jù)傳輸、處理、存儲和接收機(jī)監(jiān)視及診斷系統(tǒng)。

2012年，完成了中頻信號光纖傳輸系統(tǒng)技術(shù)方案，并開展了射頻直接傳輸方案研究。2013年，開展了中頻信號傳輸實驗。

在低頻寬帶接收機(jī)方面，通過與美國加州理工學(xué)院電子工程系多次討論，初步確定采用Caltech低頻寬帶接收機(jī)用于FAST工程低頻寬帶接收機(jī)建設(shè)。覆蓋頻率范圍為0.27～1.62 GHz。它是FAST早期科學(xué)觀測的主要接收機(jī)，將用于中性氫、脈沖星等觀測。2014年6月19日，國家天文臺和美國加州理工學(xué)院簽訂研制合同。2016年9月，低頻寬帶接收機(jī)己安裝在饋源艙下平臺，正在進(jìn)行調(diào)試和試觀測。

3.6 觀測基地建設(shè)系統(tǒng)

觀測基地建設(shè)是FAST望遠(yuǎn)鏡建設(shè)、運行和維護(hù)的基礎(chǔ)保障，主要包括兩個部分：觀測基地基本建設(shè)和公用及配套設(shè)施。

FAST工程臺址進(jìn)場道路全長約7 km，2010年3月開始施工，2011年7月全線通車，完成進(jìn)場道路一期施工。FAST工程觀測基地于2011年完成了1︰200地形圖測繪，2012年8月啟動設(shè)計，2015年10月順利開工建設(shè)，2016年9月完成主體建筑施工工程。

4 FAST工程展望

FAST工程于2016年9月25日竣工。在FAST建設(shè)期間，為給FAST運行作科學(xué)上的準(zhǔn)備，F(xiàn)AST工程成立了科學(xué)部，培養(yǎng)射電天文人才并進(jìn)行早期科學(xué)目標(biāo)研究，以期在FAST建成后能由中國科學(xué)家主導(dǎo)取得重大成果。

具有中國獨立自主知識產(chǎn)權(quán)的FAST建成后，其靈敏度、天區(qū)覆蓋面和測量精度將大大超越世界上己建成的其他射電望遠(yuǎn)鏡，與美國Arceibo望遠(yuǎn)鏡相比，綜合靈敏度提升10倍，屆時將成為世界上口徑最大、最具威力的單口徑射電望遠(yuǎn)鏡。FAST涵蓋的天文學(xué)內(nèi)容豐富，從宇宙初始混濁、星系演化、恒星乃至太陽、行星與鄰近空間事件等的觀測研究，都有非常強的競爭力，其中脈沖星探測、中性氫和奇異暗弱天體成像等課題蘊藏著巨大的發(fā)現(xiàn)機(jī)遇。作為一個多學(xué)科研究平臺，擬回答的問題不僅是天文的，也是面對人類與自然的。它還將在日地環(huán)境研究、深空探測和國家安全等方面發(fā)揮重要作用。FAST工程建設(shè)將推動中國眾多高科技領(lǐng)域的發(fā)展。

【作者單位：1. 中國科學(xué)院國家天文臺；2. 中國科學(xué)院射電天文重點實驗室】

（摘自《天文學(xué)報》2016年第6期）

·高被引論文摘要·

被引頻次：64

新一代大射電望遠(yuǎn)鏡機(jī)電光一體化設(shè)計研究

段寶巖，蘇玉鑫，仇原鷹，等

針對美國Arecibo大射電望遠(yuǎn)鏡（口徑305 m）設(shè)計方案的不足與對新一代大射電望遠(yuǎn)鏡的要求，提出了全新的機(jī)電光一體化設(shè)計方案。對懸索饋源系統(tǒng)的非線性隨機(jī)響應(yīng)與二次穩(wěn)定平臺的運動精度做了理論分析與計算機(jī)仿真研究，結(jié)果表明該方案能夠滿足跟蹤精度的要求。

大射電望遠(yuǎn)鏡；機(jī)電光一體化；懸索與饋源系統(tǒng)結(jié)構(gòu)；非線性力學(xué)分析；Stewart平臺；饋源跟蹤精度

來源出版物：中國機(jī)械工程, 1999, 10(9): 1002-1004

被引頻次：55

具有主動主反射面的巨型球面射電望遠(yuǎn)鏡

邱育海

摘要：提出一種新穎的大球面射電望遠(yuǎn)鏡的設(shè)計方案．以往球面射電望遠(yuǎn)鏡的設(shè)計方案是利用各種復(fù)雜饋源系統(tǒng)，如Arecibo三反射面系統(tǒng)來克服球差，而我們擬實時地改變被饋源照明的部分球反射面的形狀以最大限度地擬合旋轉(zhuǎn)拋物面，從而用傳統(tǒng)的拋物面饋源照明來實現(xiàn)寬帶與偏振觀測。此設(shè)計有天空覆蓋范圍大及可實現(xiàn)獨立多瓣觀測等優(yōu)點。文中還對500 m口徑的球面射電望遠(yuǎn)鏡（曲率半徑300 m）以及300 m可用口徑的具體實例提出了實施方案。

關(guān)鍵詞：球面射電望遠(yuǎn)鏡；旋轉(zhuǎn)拋物面天線；主動主反射面

來源出版物：天體物理學(xué)報, 1998, 18(2): 222-228

被引頻次：53

中國科學(xué)院光電技術(shù)研究所的自適應(yīng)光學(xué)研究進(jìn)展

姜文漢，張雨東，饒長輝，等

摘要：中國科學(xué)院光電技術(shù)研究所的自適應(yīng)光學(xué)研究始于1979年。1980年建立自適應(yīng)光學(xué)研究室，在突破了波前校正器（包括變形反射鏡和高速傾斜反射鏡）、波前傳感器、波前處理機(jī)和波前控制等關(guān)鍵技術(shù)的基礎(chǔ)上，研制了一系列自適應(yīng)光學(xué)系統(tǒng)，用于天文望遠(yuǎn)鏡、慣性約束聚變和人眼視覺研究等。

關(guān)鍵詞：自適應(yīng)光學(xué)；天文望遠(yuǎn)鏡；慣性約束聚變；視網(wǎng)膜成像；變形反射鏡；波前傳感器

來源出版物：光學(xué)學(xué)報, 2011, 31(9): 0900106

被引頻次：47

六自由度Stewart平臺運動精度分析

蘇玉鑫，段寶巖

摘要：利用Stewart型平臺之間的位置向量關(guān)系，推導(dǎo)出Stewart型平臺運動精度模型，并將其應(yīng)用到所設(shè)計的大射電望遠(yuǎn)鏡精調(diào)穩(wěn)定平臺運動精度分析，詳細(xì)給出了其運動精度分析結(jié)果，證明所設(shè)計的精調(diào)穩(wěn)定平臺完全可以滿足饋源軌跡跟蹤精度的要求。

關(guān)鍵詞：Stewart型平臺；大射電望遠(yuǎn)鏡；運動精度模型；精度分析

來源出版物：西安電子科技大學(xué)學(xué)報, 2007, (5): 9-23

被引頻次：46

用于LAMOST的并行可控式光纖定位系統(tǒng)

邢曉正，胡紅專，杜華生，等

摘要：給出了一種可用于大天區(qū)面積多目標(biāo)光纖光譜天文望遠(yuǎn)鏡（LAMOST）的光纖定位系統(tǒng)。它可以在數(shù)分鐘之內(nèi)將4000根光纖重新定位，并具有可實時補償溫度和其它因素引起的各種誤差，制造費用和運行費用低等一系列優(yōu)點。本技術(shù)也可以用于其他焦面較大的光譜望遠(yuǎn)鏡。

關(guān)鍵詞：光纖定位；光譜；望遠(yuǎn)鏡

來源出版物：中國科學(xué)技術(shù)大學(xué)學(xué)報, 1997, 27(4): 492-495

被引頻次：44

FAST反射面支承結(jié)構(gòu)整體索網(wǎng)方案研究

錢宏亮，范峰，沈世釗，等

摘要：采用整體索網(wǎng)作為大射電望遠(yuǎn)鏡（FAST）反射面的支承結(jié)構(gòu)，通過對四邊形、凱威特型和短程線型三種整體索網(wǎng)方案的研究、對比，認(rèn)為短程線型網(wǎng)格是一種合理的較優(yōu)方案；分別對提出的剛性、半剛性和柔性三種子結(jié)構(gòu)方案進(jìn)行分析研究，論證該剛性方案的可行性，初步論證半剛性方案的可行性，同時對柔性方案提出改進(jìn)建議。

關(guān)鍵詞：大射電望遠(yuǎn)鏡；整體索網(wǎng)；子結(jié)構(gòu)

來源出版物：土木工程學(xué)報, 2005, 38(12): 18-23

被引頻次：43

冗余度大型射電望遠(yuǎn)鏡廣義Stewart平臺

仇原鷹，魏強，段寶巖，等

摘要：鑒于新一代大型射電望遠(yuǎn)鏡的懸索艙體系統(tǒng)與Stewart平臺機(jī)構(gòu)在工作原理上的相似性，將懸索艙體系統(tǒng)視為廣義Stewart平臺。為了消除系統(tǒng)的力奇異性，通過增加冗余懸索，構(gòu)造了冗余度大型射電望遠(yuǎn)鏡廣義Stewart平臺。利用作用于艙體的懸索張力與載荷之間的Jacobian變換矩陣的行列式與條件數(shù)，描述了系統(tǒng)工作空間內(nèi)力奇異性的特點，以及冗余驅(qū)動力消除系統(tǒng)力奇異性的顯著效果。

關(guān)鍵詞：力奇異性；力冗余性；大型射電望遠(yuǎn)鏡；Stewart平臺

來源出版物：機(jī)械工程學(xué)報, 2001, 37(12): 7-15

被引頻次：40

大型射電望遠(yuǎn)鏡饋源定位3 T索牽引并聯(lián)機(jī)構(gòu)分析與設(shè)計

姚蕊，唐曉強，李鐵民，等

摘要：在新一代大型射電望遠(yuǎn)鏡的機(jī)構(gòu)設(shè)計中，由于饋源質(zhì)量的大幅降低，在饋源定位的設(shè)計中，提出采用四繩索牽引并聯(lián)機(jī)構(gòu)，牽引饋源艙實現(xiàn)三個方向的平動運動，達(dá)到加大饋源工作空間的目的。為了研究非線性繩索控制機(jī)構(gòu)中的尺度優(yōu)化設(shè)計問題，在已知饋源艙位置的情況下，為解決由于繩索自重導(dǎo)致的懸鏈線問題，通過將懸鏈線簡化成拋物線的方法，解決懸鏈線帶來的高度非線性靜力平衡方程組的求解問題，得到簡化的靜力學(xué)平衡方程。通過建立的簡化靜力學(xué)平衡方程，求解出四繩索牽引并聯(lián)系統(tǒng)的工作空間與設(shè)計參數(shù)間的關(guān)系，并使用一種以力優(yōu)化為目標(biāo)的優(yōu)化算法得到工作空間中四繩索靜力平衡下的精確索拉力和伸長量。通過綜合考慮滿足條件的參數(shù)，最終給出滿足設(shè)計要求的機(jī)構(gòu)優(yōu)化尺度參數(shù)。

關(guān)鍵詞：大型射電望遠(yuǎn)鏡；索牽引并聯(lián)機(jī)構(gòu)；工作空間；懸鏈線；

來源出版物：機(jī)械工程學(xué)報, 2007, 43(11): 105-109

被引頻次：35

巨型射電望遠(yuǎn)鏡（FAST）反射面支承結(jié)構(gòu)日照溫度場效應(yīng)分析

金曉飛，范峰，沈世釗

摘要：研究分析500 m口徑球冠狀巨型射電望遠(yuǎn)鏡（Five-hundred-meter Aperture Spherical radio Telescope，簡稱FAST）反射面支承結(jié)構(gòu)的日照溫度場效應(yīng)。借助ANSYS熱分析模塊，建立FAST反射面結(jié)構(gòu)和實測周邊地形的整體參數(shù)化有限元模型，計算最不利氣候之一即夏季晴天無云天氣各時刻的空氣對流換熱、太陽輻射、周圍環(huán)境的長波輻射換熱以及陰影遮擋等各種邊界條件，在較為合理的結(jié)構(gòu)初始溫度場下，進(jìn)行連續(xù)多天的時程分析，直至結(jié)構(gòu)的任一點溫度收斂于24 h前的結(jié)果，并據(jù)此結(jié)果計算反射面結(jié)構(gòu)溫度變形和溫度應(yīng)力，給出日照下反射面形狀擬合精度隨時間的變化規(guī)律、結(jié)構(gòu)應(yīng)力的變化范圍和分布規(guī)律。結(jié)果表明在日照下結(jié)構(gòu)的溫度場較不均勻，局部溫差最高達(dá)到了11℃，較大地影響了反射面形狀精度，為將來結(jié)構(gòu)的設(shè)計、施工、監(jiān)測以及控制提供了參考信息。

關(guān)鍵詞：FAST；日照溫度場；時程分析；溫度變形；溫度應(yīng)力

來源出版物：土木工程學(xué)報, 2008, 41(11): 71-77

被引頻次：31

射電望遠(yuǎn)鏡的發(fā)展和前景

吳盛殷，南仁東

摘要：在近代科學(xué)技術(shù)發(fā)展的基礎(chǔ)上誕生和成長起來的射電天文學(xué)已經(jīng)走過了66年的歷程，作為射電天文學(xué)主要探測工具的射電望遠(yuǎn)鏡有了長足的進(jìn)步，面臨21世紀(jì)人類社會和自然科學(xué)技術(shù)包括天文學(xué)發(fā)展的挑戰(zhàn)，射電望遠(yuǎn)鏡及射電天文學(xué)將邁出新的步伐。從射電天文學(xué)和射電望遠(yuǎn)鏡發(fā)展的關(guān)系、射電望遠(yuǎn)鏡幾個主要發(fā)展方向和目前水平、自90年代以來逐步勾畫而明確起來的未來發(fā)展方向等方面闡明了射電望遠(yuǎn)鏡的發(fā)展和前景，以作為我國發(fā)展新一代射電望遠(yuǎn)鏡的參考。

關(guān)鍵詞：射電天文學(xué)—儀器；射電望遠(yuǎn)鏡

來源出版物：天文學(xué)進(jìn)展, 1998, 16(3): 169-176

被引頻次：1664

Herschel space observatory area facility for far-infrared and submillimetre astronomy

Pilbratt, G. L; Riedinger, J. R; Passvogel, T; et al.

Abstract:Herschel was launched on 14 May 2009, and is now an operational ESA space observatory offering unprecedented observational capability in the far-infrared and submillimetre spectral range 55-671 μm. Herschel carries a 3.5 m diameter passively cooled Cassegrain telescope, which is the largest of its kind and utilizes a novel silicon carbide technology. The science payload comprises three instruments: two direct detection cameras/medium resolution spectrometers, PACS and SPIRE, and a very high-resolution heterodyne spectrometer, HIFI, whose focal plane units are housed inside a superfluid helium cryostat. Herschel is an observatory facility operated in partnership among ESA, the instrument consortia, and NASA. The mission lifetime is determined by the cryostat hold time. Nominally approximately 20000 h will be available for astronomy, 32% is guaranteed time and the remainder is open to the worldwide general astronomical community through a standard competitive proposal procedure.

Key words:space vehicles; space vehicles: instruments;infrared: general; submillimetre; general

來源出版物：Astronomy & Astrophysics, 2010, 518(3):383-416

被引頻次：717

SCUBA: A common-user submillimetre camera operating on the James Clerk Maxwell Telescope

Holland, WS; Robson, EI; Gear, WK; et al.

Abstract:SCUBA, the Submillimetre Common-User Bolometer Array, built by the Royal Observatory Edinburgh for the James Clerk Maxwell Telescope, is the most versatile and powerful of a new generation of submillimetre cameras, It combines a sensitive dualwaveband imaging array with a three-band photometer, and is sky-background-limited by the emission from the Mauna Kea atmosphere at all observing wavelengths from 350 μm to 2 mm. The increased sensitivity and array size mean that SCUBA maps close to 10000 times faster than its single-pixel predecessor (UKT14). SCUBA is a facility instrument, open to the world community of users, and is provided with a high level of user support. We give an overview of the instrument, describe the observing modes,user interface and performance figures on the telescope,and present a sample of the exciting new results that have revolutionized submillimetre astronomy.

關(guān)鍵詞：instrumentation; detectors; telescopes; dust,extinction; radio continuum; galaxies; radio continuum;ISM; radio continuum; stars

來源出版物：Monthly Notices of the Royal Astronomical Society, 1999, 303(4): 659-672

被引頻次：603

Fermi large area telescope first source catalog

Abdo, A A.; Ackermann, M; Ajello, M; et al.

Abstract:We present a catalog of high-energy gamma-ray sources detected by the Large Area Telescope (LAT), the primary science instrument on the Fermi Gamma-ray Space Telescope (Fermi), during the first 11 months of the science phase of the mission, which began on 2008 August 4. The First Fermi-LAT catalog (1FGL) contains 1451 sources detected and characterized in the 100 MeV to 100 GeV range. Source detection was based on the average flux over the 11 month period, and the threshold likelihood Test Statistic is 25, corresponding to a significance of just over 4 sigma. The 1FGL catalog includes source location regions, defined in terms of elliptical fits to the 95%confidence regions and power-law spectral fits as well as flux measurements in five energy bands for each source. In addition, monthly light curves are provided. Using a protocol defined before launch we have tested for several populations of gamma-ray sources among the sources in the catalog. For individual LAT-detected sources we provide firm identifications or plausible associations with sources in other astronomical catalogs. Identifications are based on correlated variability with counterparts at other wavelengths, or on spin or orbital periodicity. For the catalogs and association criteria that we have selected, 630 of the sources are unassociated. Care was taken to characterize the sensitivity of the results to the model of interstellar diffuse gamma-ray emission used to model the bright foreground, with the result that 161 sources at low Galactic latitudes and toward bright local interstellar clouds are flagged as having properties that are strongly dependent on the model or as potentially being due to incorrectly modeled structure in the Galactic diffuse emission.

Key words:catalogs; gamma rays: general

來源出版物：Astrophysical Journal Supplement Series,2010, 188(2): 405-436

被引頻次：496

The Nuclear Spectroscopic Telescope Array(NuSTAR) high-energy X-ray mission

Harrison, Fiona A; Craig, William W;Christensen, Finn E; et al.

Abstract:The Nuclear Spectroscopic Telescope Array(NuSTAR) mission, launched on 2012 June 13, is the first focusing high-energy X-ray telescope in orbit. NuSTAR operates in the band from 3 to 79 keV, extending the sensitivity of focusing far beyond the similar to 10 keV high-energy cutoff achieved by all previous X-ray satellites. The inherently low background associated with concentrating the X-ray light enables NuSTAR to probe the hard X-ray sky with a more than 100-fold improvement in sensitivity over the collimated or coded mask instruments that have operated in this bandpass. Using its unprecedented combination of sensitivity and spatial and spectral resolution, NuSTAR will pursue five primary scientific objectives: (1) probe obscured active galactic nucleus (AGN) activity out to the peak epoch of galaxy assembly in the universe (at z less than or similar to 2) by surveying selected regions of the sky; (2) study the population of hard X-ray-emitting compact objects in the Galaxy by mapping the central regions of the Milky Way;(3) study the non-thermal radiation in young supernova remnants, both the hard X-ray continuum and the emission from the radioactive element Ti-44; (4) observe blazars contemporaneously with ground-based radio, optical, and TeV telescopes, as well as with Fermi and Swift, to constrain the structure of AGN jets; and (5) observe line and continuum emission from core-collapse supernovae in the Local Group, and from nearby Type Ia events, to constrain explosion models. During its baseline two-year mission, NuSTAR will also undertake a broad program of targeted observations. The observatory consists of two co-aligned grazing-incidence X-ray telescopes pointed at celestial targets by a three-axis stabilized spacecraft.Deployed into a 600 km, near-circular, 6 degrees inclination orbit, the observatory has now completed commissioning, and is performing consistent with pre-launch expectations. NuSTAR is now executing its primary science mission, and with an expected orbit lifetime of 10 yr, we anticipate proposing a guest investigator program, to begin in late 2014.

Key words:space vehicles; instruments; X-rays; general

來源出版物：Astrophysical Journal, 2013, 770(2): UNSP 103

被引頻次：400

The James Webb Space Telescope

Gardner, Jonathan P; Mather, John C; Clampin, Mark;et al.

Abstract:The James Webb Space Telescope (JWST) is a large (6.6 m), cold (＜50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth-Sun Lagrange point. The observatory will have four instruments: A near-IR camera,a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 ＜λ＜ 5.0 μm,while the mid-IR instrument will do both imaging and spectroscopy from 5.0 ＜λ＜ 29 μm. The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe.The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars,metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems.Within these themes and objectives, we have derived representative astronomical observations. To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor.The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities.

Key words:galaxies; formation; infrared; general; planetary systems; space vehicles; instruments; stars; formation

來源出版物：Space Science Reviews, 2006, 123(4): 485-606

被引頻次：394

Fermi large area telescope third source catalog

Acero, F.; Ackermann, M; Ajello, M; et al.

Abstract:We present the third Fermi Large Area Telescope (LAT) source catalog (3FGL) of sources in the 100 MeV-300 GeV range. Based on the first 4 yr of science data from the Fermi Gamma-ray Space Telescope mission,it is the deepest yet in this energy range. Relative to the Second Fermi LAT catalog, the 3FGL catalog incorporates twice as much data, as well as a number of analysis improvements, including improved calibrations at the event reconstruction level, an updated model for Galactic diffuse γ-ray emission, a refined procedure for source detection,and improved methods for associating LAT sources with potential counterparts at other wavelengths. The 3FGL catalog includes 3033 sources above 4 sigma significance,with source location regions, spectral properties, and monthly light curves for each. Of these, 78 are flagged as potentially being due to imperfections in the model for Galactic diffuse emission. Twenty-five sources are modeled explicitly as spatially extended, and overall 238 sources are considered as identified based on angular extent or correlated variability (periodic or otherwise)observed at other wavelengths. For 1010 sources we have not found plausible counterparts at other wavelengths.More than 1100 of the identified or associated sources are active galaxies of the blazar class; several other classes of non-blazar active galaxies are also represented in the 3FGL. Pulsars represent the largest Galactic source class.From source counts of Galactic sources we estimate that the contribution of unresolved sources to the Galactic diffuse emission is similar to 3% at 1 GeV.

Key words:catalogs; gamma-rays: general

來源出版物：Astrophysical Journal Supplement Series,2015, 218(2): 23

被引頻次：220

The Giant Meter-wave Radio Telescope

Swarup, G; Ananthakrishnan, S Ananthakrishnan, S;Kapahi, Vk; et al.

Abstract:The Giant Metre-wave Radio Telescope, an aperture-synthesis array consisting of 30 fully steerable parabolic dishes of 45 m diameter each, is being set up about 80 km north of Pune as a national facility for frontline research in radio astronomy in the frequency range 38 MHz to 1420 MHz. The new and novel design of a low-solidity dish for metre-wave operation, in which a thin wire mesh (varying in size from 10 mm × 10 mm to 20 mm×20 mm and made of 0.55 mm diameter stainless-steel wire), which constitutes the reflecting surface, is stretched over a parabolic surface formed by rope trusses, has made it possible to build a large collecting area (total effective area of about 30000 m2, over three times that of the Very Large Array in the USA) at modest cost. It will be a major new instrument designed to fill the existing world-wide gap in powerful radio telescopes operating at metre wavelengths, where there are many exciting and challenging astrophysical problems and phenomena to be investigated. Two of the primary scientific objectives of the telescope are to detect the highly redshifted ‘21-cm’ line of neutral hydrogen from protoclusters or protogalaxies in the early epochs of the Universe before galaxy formation and to detect and study a large number of millisecond pulsars in an attempt to detect the primordial background of gravitational radiation.

來源出版物：Current Science, 1991, 60(2): 95-105

被引頻次：217

First-order performance evaluation of adaptiveoptics systems for atmospheric-turbulence compensation in extended-field-of-view astronomical telescopes

Ellerbroek, BL

Abstract:An approach is presented for evaluating the performance achieved by a closed-loop adaptive-optics system that is employed with an astronomical telescope.This method applies to systems incorporating one or several guide stars, a wave-front reconstruction algorithm that is equivalent to a matrix multiply, and one or several deformable mirrors that are optically conjugate to different ranges. System performance is evaluated in terms of residual mean-square phase distortion and the associated optical transfer function. This evaluation accounts for the effects of the atmospheric turbulenceC2n(h) and wind profiles, the wave-front sensor and deformable-mirror fitting error, the sensor noise, the control-system bandwidth, and the net anisoplanatism for a given constellation of natural and/or laser guide stars. Optimal wave-front reconstruction algorithms are derived that minimize the telescope’s fieldof-view-averaged residual mean-square phase distortion.Numerical results are presented for adaptive-optics configurations incorporating a single guide star and a single deformable mirror, multiple guide stars and a single deformable mirror, or multiple guide stars and two deformable mirrors.

來源出版物：Journal of the Optical Society of America A-Optics Image Science and Vision, 1994, 11(2): 783-805

被引頻次：113

The five-hundred-meter aperture spherical radio telescope (FAST) project

Nan, Rendong; Li, Di; Jin, Chengjin; et al.

Abstract:Five-hundred-meter Aperture Spherical radio Telescope (FAST) is a Chinese mega-science project to build the largest single dish radio telescope in the world. Its innovative engineering concept and design pave a new road to realize a huge single dish in the most effective way.FAST also represents Chinese contribution in the international efforts to build the square kilometer array(SKA). Being the most sensitive single dish radio telescope, FAST will enable astronomers to jump-start many science goals, such as surveying the neutral hydrogen in the Milky Way and other galaxies, detecting faint pulsars, looking for the first shining stars, hearing the possible signals from other civilizations, etc. The idea of sitting a large spherical dish in a karst depression is rooted in Arecibo telescope. FAST is an Arecibo-type antenna with three outstanding aspects: The karst depression used as the site, which is large to host the 500-meter telescope and deep to allow a zenith angle of 40 degrees; the active main reflector correcting for spherical aberration on the ground to achieve a full polarization and a wide band without involving complex feed systems; and the lightweight feed cabin driven by cables and servomechanism plus a parallel robot as a secondary adjustable system to move with high precision. The feasibility studies for FAST have been carried out for 14 years, supported by Chinese and world astronomical communities. Funding for FAST has been approved by the National Development and Reform Commission in July of 2007 with a capital budget similar to 700 million RMB. The project time is 5.5 years from the commencement of work in March of 2011 and the first light is expected to be in 2016. This review intends to introduce the project of FAST with emphasis on the recent progress since 2006. In this paper, the subsystems of FAST are described in modest details followed by discussions of the fundamental science goals and examples of early science projects.

Key words:radio telescope; active main reflector; HI 21 cm line; pulsar

來源出版物：International Journal of Modern Physics D,2011, 20(6): 989-1024

·推薦論文摘要·

961單元變形鏡研制及性能測試

林旭東，劉欣悅，王建立，等

摘要：為了滿足天文望遠(yuǎn)鏡自適應(yīng)光學(xué)系統(tǒng)的需要，研制了一個961單元的變形鏡及其控制系統(tǒng)。利用Zygo激光干涉儀對變形鏡的性能進(jìn)行測試，包括單個促動器的響應(yīng)測試、相鄰促動器間推拉測試、耦合測試；對于變形鏡的校正能力，分別進(jìn)行了Waffle模式測試、Zernike多項式擬合和展平測試。測試表明，961單元變形鏡在單個促動器作用下的最大面形校正量為±2.5 μm；相鄰促動器間推拉變形量為4 μ m；相鄰促動器間的耦合為23%；相對于之前的137單元變形鏡，其對Zernike多項式的擬合能力有較大地提高；展平后的面形優(yōu)于λ/70（λ =632.8 nm）。測試結(jié)果達(dá)到了天文望遠(yuǎn)鏡自適應(yīng)光學(xué)系統(tǒng)對變形鏡的性能指標(biāo)要求。

關(guān)鍵詞：自適應(yīng)光學(xué)；變形鏡；性能測試；校正能力

來源出版物：光學(xué)學(xué)報, 2013, 33(6): 0601001

FAST索網(wǎng)高應(yīng)力幅變位疲勞問題的優(yōu)化分析

孔旭，姜鵬，王啟明

摘要：五百米口徑射電望遠(yuǎn)鏡（FAST）采用柔性索網(wǎng)作為主要支承結(jié)構(gòu)，根據(jù)擬定的變位策略要求，通過促動器連接下拉索控制索網(wǎng)變位實現(xiàn)巡天觀測。由于變位觀測過程中索網(wǎng)將長期承受高達(dá)約500 MPa的疲勞載荷，約為目前相關(guān)標(biāo)準(zhǔn)規(guī)定值的兩倍多，故索網(wǎng)結(jié)構(gòu)將是該望遠(yuǎn)鏡中的關(guān)鍵易損部位。為此，該文以索網(wǎng)結(jié)構(gòu)后期運行、監(jiān)測及維護(hù)為背景，通過量綱分析方法明確影響索網(wǎng)變位應(yīng)力幅值的主導(dǎo)因素，基于大型有限元軟件ANSYS建立索網(wǎng)模型進(jìn)行連續(xù)變位仿真分析，探索合理的變位策略以降低索網(wǎng)變位過程中的應(yīng)力變化幅值，提高索網(wǎng)運行的可靠性。

關(guān)鍵詞：FAST工程；索網(wǎng)結(jié)構(gòu)；疲勞；量綱分析；ANSYS；有限元

來源出版物：工程力學(xué), 2013, 30(S1): 33-38

射電望遠(yuǎn)鏡相控陣饋源技術(shù)

伍洋，杜彪，金乘進(jìn)，等

摘要：相位陣饋源是作為多波束饋源使用的小型二維相控陣天線，用以產(chǎn)生多個緊密交疊的波束，擴(kuò)大射電望遠(yuǎn)鏡的視場，提高巡天效率。文章分析了焦面場匹配與天線效率之間的聯(lián)系，在單波束和多波束應(yīng)用方面對相控陣饋源與傳統(tǒng)的波導(dǎo)饋源進(jìn)行了細(xì)致的比較，并介紹了相控陣饋源饋電的射電望遠(yuǎn)鏡信噪比模型。作為一種新的饋源技術(shù)，相控陣饋源展現(xiàn)出更大的靈活性和更為優(yōu)異的性能。

關(guān)鍵詞：射電望遠(yuǎn)鏡；饋源；焦面場；多波束

來源出版物：電波科學(xué)學(xué)報, 2013, 28(2): 348-353

FAST的進(jìn)展——科學(xué)、技術(shù)與設(shè)備

南仁東，李會賢

摘要：隨著射電天文學(xué)的發(fā)展，高靈敏度的大口徑射電望遠(yuǎn)鏡成為射電觀測的重要設(shè)備。我國正在建設(shè)中的500 m口徑球面射電望遠(yuǎn)鏡（FAST）將成為世界上最大、最靈敏的單口徑射電望遠(yuǎn)鏡，它有望在中性氫巡視、脈沖星搜索、國際VLBI網(wǎng)聯(lián)測及地外生命搜尋等重要前沿領(lǐng)域取得突破。本文介紹了FAST工程概念的提出及望遠(yuǎn)鏡概況，列出了FAST的主要科學(xué)目標(biāo)及早期科學(xué)準(zhǔn)備，重點敘述了FAST工程在科學(xué)、技術(shù)與設(shè)備方面的最新進(jìn)展，并對FAST工程的發(fā)展做出了展望。

關(guān)鍵詞：射電天文；單口徑射電望遠(yuǎn)鏡；FAST

來源出版物：中國科學(xué)：物理學(xué) 力學(xué) 天文學(xué), 2014,44(10): 1063-1074

200單元硅基單壓電變形鏡的設(shè)計與測試

馬劍強，劉瑩，陳俊杰，等

摘要：針對天文望遠(yuǎn)鏡對變形鏡的需求，設(shè)計了200單元級硅基單壓電變形鏡并對其進(jìn)行了性能測試。首先，通過有限元方法對單壓電變形鏡進(jìn)行結(jié)構(gòu)建模，分析比較了電極排列形式和邊界支撐方式對變形鏡性能的影響。然后，制備了3款200單元變形鏡樣機(jī)（環(huán)形簡支、環(huán)形固支、六邊形簡支）。最后，利用干涉儀測量了變形鏡的影響函數(shù)，并通過激光多普勒測振儀測量其頻響特性。仿真與實驗結(jié)果表明：致動器在50 V電壓下變形量可達(dá)1 μm，固支條件下諧振頻率在1 kHz左右，對前100項Zernike像差具有良好的校正能力。該變形鏡在低成本天文自適應(yīng)光學(xué)系統(tǒng)中具有應(yīng)用潛力。

關(guān)鍵詞：壓電變形鏡；硅基變形鏡；自適應(yīng)光學(xué)；天文望遠(yuǎn)鏡

來源出版物：光學(xué)精密工程, 2014, 22(8): 2047-2053

FAST索網(wǎng)疲勞評估及高疲勞性能鋼索研制

姜鵬，朱萬旭，劉飛，等

摘要：500 m口徑射電望遠(yuǎn)鏡（FAST）采用柔性索網(wǎng)作為主要支承結(jié)構(gòu)，變位觀測過程中索網(wǎng)將長期承受高達(dá)500 MPa的疲勞載荷，約為目前相關(guān)標(biāo)準(zhǔn)規(guī)范規(guī)定值的兩倍。索網(wǎng)結(jié)構(gòu)將是該望遠(yuǎn)鏡系統(tǒng)的關(guān)鍵易損部件，故該文主要開展如下工作：1）根據(jù)望遠(yuǎn)鏡的科學(xué)目標(biāo)，估算未來30年望遠(yuǎn)鏡的觀測軌跡，評估望遠(yuǎn)鏡運行觀測對索網(wǎng)結(jié)構(gòu)疲勞性能的要求；2）結(jié)合環(huán)氧涂層技術(shù)和改進(jìn)擠壓錨固工藝研制高疲勞性能鋼索結(jié)構(gòu)，并通過實驗驗證該種鋼索結(jié)構(gòu)可以滿足該望遠(yuǎn)鏡對索網(wǎng)結(jié)構(gòu)的技術(shù)要求。

關(guān)鍵詞：FAST工程；索網(wǎng)結(jié)構(gòu)；疲勞性能；有限元分析；射電望遠(yuǎn)鏡

來源出版物：工程力學(xué), 2015, 32(9): 243-249

500 m口徑球面射電望遠(yuǎn)鏡瞬時拋物面擬合精度的預(yù)估與改善

薛建興，王啟明，古學(xué)東，等

摘要：依據(jù)500 m口徑球面射電望遠(yuǎn)鏡（FAST）主動反射面工作原理及相關(guān)結(jié)構(gòu)尺寸，基于反射面單元動態(tài)面形精度分析研究了FAST瞬時拋物面的擬合精度。首先，以反射面單元為研究對象，自節(jié)點開始推導(dǎo)考慮了機(jī)構(gòu)運動的反射面單元動態(tài)面形精度計算方法。然后，提取不同區(qū)域19塊反射面單元的各自9種初始面形工況，給出了分析算例。最后，基于單元動態(tài)精度特性，提出瞬時拋物面機(jī)械本體擬合精度及考慮饋源照明函數(shù)的半光程差擬合精度預(yù)估方法，并給出2種改善措施，即擴(kuò)大可控區(qū)至300 m拋物面外一層節(jié)點靶標(biāo)，及拋物面周圈節(jié)點靶標(biāo)向球心、中心反向各自偏移4 mm。結(jié)果表明：反射面單元初始面形應(yīng)優(yōu)選面形精度RMS為2 mm的波浪式面板。改進(jìn)控制策略后機(jī)械本體擬合精度提高至RMS為3.938 mm，優(yōu)于RMS為5 mm的設(shè)計指標(biāo)，此時半光程差擬合精度RMS為0.629 mm。該項研究對確定反射面單元初始面形及調(diào)節(jié)瞬時拋物面擬合精度很有意義。

關(guān)鍵詞：500 m口徑球面射電望遠(yuǎn)鏡；反射面單元；初始面形；動態(tài)面形；面形精度；瞬時拋物面；擬合精度

來源出版物：光學(xué)精密工程, 2015, 23(7): 51-59

大型射電望遠(yuǎn)鏡電磁環(huán)境頻譜監(jiān)測

李建斌，彭勃，劉東亮

摘要：射電天文的發(fā)展需要更寬的觀測頻率，但是隨著通訊的不斷發(fā)展，射頻無線電干擾（Radio Frequency Interference, RFI）對射電觀測的影響日益加重，射電望遠(yuǎn)鏡需要選擇電磁環(huán)境優(yōu)良的站址并進(jìn)行保護(hù)。文中描述了目前國內(nèi)在建和預(yù)研階段的望遠(yuǎn)鏡的電磁環(huán)境的測試過程，闡述了數(shù)據(jù)分析和處理方法。通過對我國射電望遠(yuǎn)鏡臺址選擇和保護(hù)進(jìn)行的電磁環(huán)境測試，優(yōu)選出適合建立大型射電望遠(yuǎn)鏡的臺址。

關(guān)鍵詞：射電望遠(yuǎn)鏡；電磁環(huán)境；頻譜監(jiān)測；選址

來源出版物：電波科學(xué)學(xué)報, 2015, 30(2): 378-382

平方公里陣中國驗證天線光學(xué)設(shè)計

杜彪，伍洋，周建寨

摘要：平方公里陣SKA（Square Kilometre Array）將是世界上最大的綜合孔徑射電望遠(yuǎn)鏡，致力于回答宇宙起源等基本問題。目前SKA項目已進(jìn)入建設(shè)準(zhǔn)備階段，包括中國在內(nèi)的許多國家正在進(jìn)行先導(dǎo)天線、相控陣饋源、超寬帶單波束饋源等關(guān)鍵技術(shù)的試驗研究。其中，中國驗證天線DVA-C（Dish Verification Antenna-China）是我國針對SKA中頻反射面天線陣列提出的技術(shù)方案。文章詳細(xì)介紹了DVA-C的微波光學(xué)與饋源的設(shè)計思路、方法和研究成果，以及預(yù)期達(dá)到的指標(biāo)。由于DVA-C以軸向波束性能最優(yōu)作為設(shè)計原則，對使用相控陣饋源的多波束觀測造成了一定影響，故文中對此也進(jìn)行了仿真和分析，并提出了應(yīng)對的方案。

關(guān)鍵詞：平方公里陣；射電望遠(yuǎn)鏡；反射面天線；微波光學(xué)；饋源

來源出版物：中國科學(xué)：信息科學(xué), 2015, 30(2): 378-382

LAMOST銀河系大規(guī)模光譜巡天計劃的進(jìn)展和展望

劉曉為

摘要：大天區(qū)面積多目標(biāo)光纖光譜天文望遠(yuǎn)鏡（LAMOST，又稱郭守敬望遠(yuǎn)鏡）是一臺新型準(zhǔn)中星儀式反射施密特望遠(yuǎn)鏡。其有效口徑4 m，視場20平方度，配備了16臺攝譜儀和4000根光纖，可同時獲取至多4000個天體的光譜。光譜覆蓋為370～910 nm，分辨率為1800。為期5年的LAMOST銀河系大規(guī)模恒星光譜巡天計劃已于2012年秋啟動，計劃獲取超過700萬條恒星光譜，截至2014年6月已獲得超過300萬條光譜。文章簡要回顧了銀河系研究的重要性和現(xiàn)狀，介紹了LAMOST銀河系光譜巡天計劃的科學(xué)意義和目標(biāo)，數(shù)據(jù)采集、處理和分析進(jìn)展以及已獲得的初步科研成果，并對LAMOST銀河系光譜巡天計劃的未來進(jìn)行了展望。

關(guān)鍵詞：銀河系；光譜巡天

來源出版物：物理, 2015, 44(4): 213-227

FAST工程建設(shè)進(jìn)展

南仁東，張海燕，張瑩，等

摘要：“十一五”國家重大科技基礎(chǔ)設(shè)施建設(shè)項目—500 m口徑球面射電望遠(yuǎn)鏡（FAST）工程，是利用貴州天然喀斯特洼地作為望遠(yuǎn)鏡臺址，建造世界第一大單口徑射電望遠(yuǎn)鏡——500 m口徑主動反射球面射電望遠(yuǎn)鏡，以實現(xiàn)大天區(qū)面積、高精度的天文觀測。FAST工程由中國科學(xué)院和貴州省人民政府聯(lián)合共建，于2016年9月25日竣工。

關(guān)鍵詞：射電天文；射電望遠(yuǎn)鏡；FAST工程

來源出版物：天文學(xué)報, 2016, 57(6): 623-630

天文望遠(yuǎn)鏡反射鏡面的飛秒激光清潔

勞召欣，李家文，胡衍雷，等

摘要：金屬鏡面反射鏡是反射式天文望遠(yuǎn)鏡中成像系統(tǒng)的核心部件，反射鏡定期清洗是天文望遠(yuǎn)鏡維護(hù)中的一項重要工作。目前采用的干冰人工清洗方法工序繁雜，成本較高，還需要定期使用清潔劑和清潔布擦拭的方法去除難以清洗的污染物，容易損傷鏡面。針對以上缺點，本文利用放大級飛秒脈沖激光器，對天文望遠(yuǎn)鏡中反射表面上黏附的微米級灰塵顆粒進(jìn)行了清潔研究。首先研究了飛秒激光與反射鋁鏡的作用規(guī)律，通過調(diào)節(jié)激光能量密度，對清洗后的鋁鏡表面形貌進(jìn)行觀測，得出實驗用鋁鏡的飛秒激光損傷閾值為60 mJ/cm2。通過改變激光能量等掃描參數(shù)，對清潔前后的鋁鏡鏡面附著物進(jìn)行分析，得到最優(yōu)的清潔參數(shù)。結(jié)果表明，當(dāng)激光能量密度為30～55 mJ/cm2時，飛秒激光對微米級灰塵顆粒有良好的清潔效果。在可見光范圍內(nèi)，清潔后的反射鏡鏡面反射率獲得了明顯的提升。最后，通過對灰塵顆粒及鋁鏡基底的能譜分析，對飛秒激光的清潔機(jī)理進(jìn)行了討論，在灰塵顆粒的激光清潔中熱膨脹因素占據(jù)主導(dǎo)作用。飛秒激光清潔在天文望遠(yuǎn)鏡的清潔領(lǐng)域有著良好的應(yīng)用前景。

關(guān)鍵詞：飛秒激光；天文望遠(yuǎn)鏡；激光清潔；金屬反射鏡

來源出版物：科學(xué)通報, 2016, 61(6): 622-629

下一代天文望遠(yuǎn)鏡及巡天任務(wù)（上）

黃晨，王建軍，薛莉，等

摘要：對國際上已完成的光學(xué)/紅外天文望遠(yuǎn)鏡進(jìn)行了回顧和總結(jié)，詳細(xì)論述了正在研制建設(shè)的下一代天文望遠(yuǎn)鏡，要包括科學(xué)目的、光學(xué)結(jié)構(gòu)、搭載儀器、性能參數(shù)等。分析了下一代天文望遠(yuǎn)鏡的技術(shù)特點、發(fā)展趨勢。借鑒國外在計劃制定、工程應(yīng)用等方面的經(jīng)驗，結(jié)合中國實際提出幾點思考和建議。

關(guān)鍵詞：天文望遠(yuǎn)鏡；光學(xué)結(jié)構(gòu)；紅外相機(jī)；巡天觀測；天體物理

來源出版物：紅外與激光工程, 2016, 45(2): 0217006

下一代天文望遠(yuǎn)鏡及巡天任務(wù)（下）

黃晨，王建軍，薛莉，等

摘要：對國際上已完成的光學(xué)/紅外天文望遠(yuǎn)鏡進(jìn)行了回顧和總結(jié)，詳細(xì)論述分析了正在研制建設(shè)的下一代天文望遠(yuǎn)鏡，主要包括科學(xué)目的、光學(xué)結(jié)構(gòu)、搭載儀器、性能參數(shù)等。重點對下一代天文望遠(yuǎn)鏡的光學(xué)設(shè)計/口徑、站址/軌道進(jìn)行了總結(jié)歸納，其在地基/天基協(xié)作觀測、器件模塊化通用化、觀測結(jié)果大數(shù)據(jù)分享等方面展示了自身的技術(shù)特點和發(fā)展趨勢。借鑒國外經(jīng)驗，結(jié)合我國實際情況可形成自身優(yōu)勢特色領(lǐng)域。同時在長期規(guī)劃制定、開放民間資本等方面提出幾點思考和建議。

關(guān)鍵詞：天文望遠(yuǎn)鏡；光學(xué)結(jié)構(gòu)；紅外相機(jī)；巡天觀測；天體物理

來源出版物：紅外與激光工程, 2016, 45(3): 0313001

大口徑反射面天線技術(shù)綜述

杜彪，伍洋，張一凡

摘要：大口徑反射面天線是射電天文觀測和深空探測的關(guān)鍵設(shè)備之一。介紹了國內(nèi)外大口徑反射面天線的發(fā)展現(xiàn)狀，描述了幾個代表性大口徑天線的主要指標(biāo)和技術(shù)特點，重點論述大口徑反射面天線的微波光學(xué)設(shè)計、饋源網(wǎng)絡(luò)、頻段切換、結(jié)構(gòu)型式選擇與保型設(shè)計、高精度面板設(shè)計與制造、主動反射面和伺服控制等關(guān)鍵技術(shù)及實現(xiàn)方法，最后給出了其技術(shù)發(fā)展方向。

關(guān)鍵詞：射電望遠(yuǎn)鏡；反射面天線；饋源網(wǎng)絡(luò)；保型設(shè)計

來源出版物：無線電通信技術(shù), 2016, 42(1): 1-8

500 m口徑球面射電望遠(yuǎn)鏡反射面液壓促動器關(guān)鍵性能分析

王啟明，高原，薛建興，等

摘要：針對國家重大科技基礎(chǔ)設(shè)施項目500 m口徑球面射電望遠(yuǎn)鏡（Five-hundred-meter Aperture Spherical radio Telescope, FAST）液壓促動器進(jìn)行分析研究。提出利用齒輪泵泄漏特性及液控單向閥開啟特性實現(xiàn)流量閉環(huán)的建模方法可使數(shù)學(xué)模型更準(zhǔn)確。設(shè)計樣機(jī)試驗并研發(fā)試驗設(shè)備以獲取齒輪泵流量壓力系數(shù)Kq及液控單向閥開啟特性Kf兩參數(shù)。利用Matlab/Simulink軟件搭建系統(tǒng)模型分析了促動器在開環(huán)外伸及閉環(huán)跟蹤兩模式下的運動特性，并通過試驗對系統(tǒng)模型進(jìn)行對比驗證。結(jié)果表明：建立的模型能夠描述液壓促動器的工作原理，參數(shù)Kq及Kf與試驗結(jié)果一致性較好。開環(huán)時促動器的速度隨輸入脈沖頻率增加而增大，閉環(huán)時促動器在變載荷下可實現(xiàn)穩(wěn)定跟蹤。仿真與試驗最大跟蹤誤差分別為0.15 mm和0.2 mm，滿足設(shè)計精度要求。該系統(tǒng)模型為FAST液壓促動器奠定理論基礎(chǔ)，同時可為伸縮回路差異較大的液壓系統(tǒng)提供參考。

關(guān)鍵詞：FAST工程；液壓促動器；理論建模；參數(shù)識別；仿真分析；試驗驗證

來源出版物：機(jī)械工程學(xué)報, 2017, 53(2): 183-191

500 m口徑球面射電望遠(yuǎn)鏡反射面主體支承結(jié)構(gòu)設(shè)計

朱忠義，劉飛，張琳，等

摘要：500 m口徑球面射電望遠(yuǎn)鏡（FAST）是國家重大科技基礎(chǔ)設(shè)施項目，由主動反射面系統(tǒng)、饋源支撐系統(tǒng)、測量與控制系統(tǒng)、接收機(jī)與終端系統(tǒng)四大部分構(gòu)成，其中主動反射面包括主體支承結(jié)構(gòu)、促動器、背架結(jié)構(gòu)和反射面板四部分。FAST反射面主體支承結(jié)構(gòu)由格構(gòu)柱、圈梁和索網(wǎng)組成，是迄今為止世界上最大的空間結(jié)構(gòu)，具有主動變位和高精度的特點，且地處地形、地貌復(fù)雜的山區(qū)，設(shè)計、建造難度較大。本文從結(jié)構(gòu)體系、索網(wǎng)性能、節(jié)點、參數(shù)敏感性等方面對主體支承結(jié)構(gòu)設(shè)計的關(guān)鍵問題進(jìn)行了介紹。

關(guān)鍵詞：500 m口徑球面射電望遠(yuǎn)鏡；主體支承結(jié)構(gòu)；結(jié)構(gòu)體系；格構(gòu)柱；圈梁；索網(wǎng)

來源出版物：空間結(jié)構(gòu), 2017, 23(2): 3-8

FAST radio burst discovered in the Arecibo pulsar Alfa survey

Spitler, L. G; Cordes, J. M.; Hessels, J. W. T; et al.

Abstract:Recent work has exploited pulsar survey data to identify temporally isolated, millisecond-duration radio bursts with large dispersion measures (DMs). These bursts have been interpreted as arising from a population of extragalactic sources, in which case they would provide unprecedented opportunities for probing the intergalactic medium; they may also be linked to new source classes.Until now, however, all so-called fast radio bursts (FRBs)have been detected with the Parkes radio telescope and its 13-beam receiver, casting some concern about the astrophysical nature of these signals. Here we present FRB 121102, the first FRB discovery from a geographic location other than Parkes. FRB 121102 was found in the Galactic anti-center region in the 1.4 GHz Pulsar Arecibo L-band Feed Array (ALFA) survey with the Arecibo Observatory with aDM=557.4±2.0 pc cm-3, pulse width of 3.0±0.5 ms, and no evidence of interstellar scattering. The observed delay of the signal arrival time with frequency agrees precisely with the expectation of dispersion through an ionized medium. Despite its low Galactic latitude (b=-0°.2), the burst has three times the maximum Galactic DM expected along this particular line of sight, suggesting an extragalactic origin. A peculiar aspect of the signal is an inverted spectrum; we interpret this as a consequence of being detected in a sidelobe of the ALFA receiver. FRB 121102’s brightness, duration, and the inferred event rate are all consistent with the properties of the previously detected Parkes bursts.

來源出版物：Astrophysical Journal, 2014, 790(2): 101

Prospects for detecting the 326.5 MHz redshifted 21 cm HI signal with the Ooty Radio Telescope (ORT)

Ali, Sk. Saiyad; Bharadwaj, Somnath

Abstract:Observations of the redshifted 21 cm HI fluctuations promise to be an important probe of the postreionization era (z≤6). In this paper we calculate the expected signal and foregrounds for the upgraded Ooty Radio Telescope (ORT) which operates at frequencyνo=326.5 MHz which corresponds to redshiftz=3.35.Assuming that the visibilities contain only the HI signal and system noise, we show that a 3 sigma detection of the HI signal (similar to 1 mK) is possible at angular scales 11'to 3° with a parts per thousand 1000 h of observation.Foreground removal is one of the major challenges for a statistical detection of the redshifted 21 cm HI signal. We assess the contribution of different foregrounds and find that the 326.5 MHz sky is dominated by the extragalactic point sources at the angular scales of our interest. The expected total foregrounds are 104-105times higher than the HI signal.

Keywords:cosmology; large scale structure of universe;intergalactic medium; diffuse radiation

來源出版物：Journal of Astrophysics and Astronomy,2014, 35(2): 157-182

Pulsar-black hole binaries: Prospects for new gravity tests with future radio telescopes

Liu, K.; Eatough, R. P.; Wex, N; et al.

Abstract:The anticipated discovery of a pulsar in orbit with a black hole is expected to provide a unique laboratory for black hole physics and gravity. In this context, the next generation of radio telescopes, like the Five-hundred-meter Aperture Spherical radio Telescope(FAST) and the Square Kilometre Array (SKA), with their unprecedented sensitivity, will play a key role. In this paper, we investigate the capability of future radio telescopes to probe the space-time of a black hole and test gravity theories by timing a pulsar orbiting a stellar-mass black hole (SBH). Based on mock data simulations, we show that a few years of timing observations of a sufficiently compact pulsar-SBH (PSR-SBH) system with future radio telescopes would allow precise measurements of the black hole mass and spin. A measurement precision of 1 per cent can be expected for the spin. Measuring the quadrupole moment of the black hole, needed to test general relativity's (GR's) no-hair theorem, requires extreme system configurations with compact orbits and a large SBH mass. Additionally, we show that a PSR-SBH system can lead to greatly improved constraints on alternative gravity theories even if they predict black holes (practically) identical to GR’s. This is demonstrated for a specific class of scalar-tensor theories. Finally, we investigate the requirements for searching for PSR-SBH systems. It is shown that the high sensitivity of the next generation of radio telescopes is key for discovering compact PSR-SBH systems, as it will allow for sufficiently short survey integration times.

來源出版物：Monthly Notices of the Royal Astronomical Society, 2014, 445(3): 3115-3132

A novel Hybrid Phased Array Antenna for Satellite Communication on-the-Move in Ku-band

G Han; B Du; W Wu; B Yang

Abstract:This paper introduces a novel waveguide hybrid phased array (HPA) for mobile satellite communications operating in Ku-band. The array is low profile and low cost, adopting an electrical scan in elevation and mechanical scan in azimuth to track satellites. High directivity and wide bandwidth impedance is provided by a dual linear polarized waveguide radiating element that covers both Rx and Txfrequencies within the band. The vertical and horizontal polarizations are excited by direct feeding and slot coupled aperture feeding, respectively.The array structure of 32×12 elements is split into inclined and interlaced 12 subarrays 225 mm in height. The feed networks and duplexers are designed in unconventional waveguide sizes. In the system, there are 12 independent receiving (Rx) and transmitting (Tx) modules with phased shifter components, which realize beam and polarization tracking. The system is designed to track satellites by scanning 15°-75° (relative to the ground plane) electrically in the elevation and 0°-360° mechanically in the azimuth.The array has been successfully developed and measured.The maximal gain loss in scanning range is about 4.0 dB.

來源出版物：IEEE Transactions on Antennas &Propagation, 2015, 63(4): 1375-1383

Gravitational redshift test with the space radio telescope “Radio Astron”

Biriukov, A. V.; Kauts, V. L.; Kulagin, V. V; et al.

Abstract:The space radio telescope “RadioAstron” is equipped with a high performance hydrogen maser frequency standard and thus provides a unique opportunity for a gravitational redshift test. We consider various modes of operation of the on-board scientific equipment and their impact on accuracy of the anticipated experiment. We find that the accuracy of the test is limited by similar to 10-2for the hardware configuration routinely used in radio astronomical observations, which is a consequence of using ballistic data to remove the no relativistic Doppler frequency shift from the analyzed signal. On the other hand, the so-called “Semi-coherent” mode of the on-board hardware provides for combining the space and ground maser signals in such a way that the resulting signal carries information about the useful effect but is free from the no relativistic Doppler and troposphere frequency shifts. The proposed compensation scheme, which is different from the one used in the Gravity Probe an experiment, allows for testing the gravitational redshift effect with similar to 10-6accuracy.

來源出版物：Astronomy Reports, 2014, 58(11): 783-795

Identifying the source of perytons at the Parkes radio telescope

Petroff, E.; Keane, E. F; Barr, E. D; et al.

Abstract:‘Perytons’ are millisecond-duration transients of terrestrial origin, whose frequency-swept emission mimics the dispersion of an astrophysical pulse that has propagated through tenuous cold plasma. In fact, their similarity to FRB 010724 had previously cast a shadow over the interpretation of ‘Fast Radio Bursts’ (FRBs), which otherwise appear to be of extragalactic origin. Until now,the physical origin of the dispersion-mimicking perytons had remained a mystery. We have identified strong out-of-band emission at 2.3-2.5 GHz associated with several peryton events. Subsequent tests revealed that a peryton can be generated at 1.4 GHz when a microwave oven door is opened prematurely and the telescope is at an appropriate relative angle. Radio emission escaping from microwave ovens during the magnetron shut-down phase neatly explains all of the observed properties of the peryton signals. Now that the peryton source has been identified,we furthermore demonstrate that the microwave ovens on site could not have caused FRB 010724. This and other distinct observational differences show that FRBs are excellent candidates for genuine extragalactic transients.

來源出版物：Monthly Notices of the Royal Astronomical Society, 2015, 451(4): 3933-3940

A lunar radio experiment with the Parkes radio telescope for the LUNASKA project

Bray, J. D; Ekers, R. D.; Roberts, P; et al.

Abstract:We describe an experiment using the Parkes radio telescope in the 1.2-1.5 GHz frequency range as part of the LUNASKA project, to search for nanosecond-scale pulses from particle cascades in the Moon, which may be triggered by ultra-high-energy astroparticles. Through the combination of a highly sensitive multi-beam radio receiver, a purpose-built backend and sophisticated signal-processing techniques, we achieve sensitivity to radio pulses with threshold electric field strength of 0.0053 IAV/m/MHz, lower than previous experiments by a factor of three. We observe no pulses in excess of this threshold in observations with an effective duration of 127 h. The techniques we employ, including compensating for the phase, dispersion and spectrum of the expected pulse, are relevant for future lunar radio experiments.

Key words:ultra-high-energy neutrinos; ultra-high-energy cosmic rays; lunar radio experiment; radio instrumentation

來源出版物：Astroparticle Physics, 2015, 65: 22-39

A real-time coherent dedispersion pipeline for the giant metrewave radio telescope

De, Kishalay; Gupta, Yashwant

Abstract:A fully real-time coherent dedispersion system has been developed for the pulsar back-end at the Giant Metrewave Radio Telescope (GMRT). The dedispersion pipeline uses the single phased array voltage beam produced by the existing GMRT software back-end (GSB)to produce coherently dedispersed intensity output in real time, for the currently operational bandwidths of 16 MHz and 32 MHz. Provision has also been made to coherently dedisperse voltage beam data from observations recorded on disk. We discuss the design and implementation of the real-time coherent dedispersion system, describing the steps carried out to optimise the performance of the pipeline. Presently functioning on an Intel Xeon X5550 CPU equipped with a NVIDIA Tesla C2075 GPU, the pipeline allows dispersion free, high time resolution data to be obtained in real-time. We illustrate the significant improvements over the existing incoherent dedispersion system at the GMRT, and present some preliminary results obtained from studies of pulsars using this system,demonstrating its potential as a useful tool for low frequency pulsar observations. We describe the salient features of our implementation, comparing it with other recently developed real-time coherent dedispersion systems. This implementation of a real-time coherent dedispersion pipeline for a large, low frequency array instrument like the GMRT, will enable long-term observing programs using coherent dedispersion to be carried out routinely at the observatory. We also outline the possible improvements for such a pipeline, including prospects for the upgraded GMRT which will have bandwidths about ten times larger than at present.

Keywords:coherent dedispersion; pulsars; parallel processing; graphics processing unit

來源出版物：Experimental Astronomy, 2016, 41(2): 67-93

The Five-hundred-meter Aperture Spherical radio Telescope project

Li, Di; Pan, Zhichen

Abstract:The Five-hundred-meter Aperture Spherical Radio Telescope (FAST) is a Chinese megascience project funded by the National Development and Reform Commission (NDRC) of the People's Republic of China.The National Astronomical Observatories of China(NAOC) is in charge of its construction and subsequent operation. Upon its expected completion in September 2016, FAST will surpass the 305 m Arecibo Telescope and the 100 m Green Bank Telescope in terms of absolute sensitiveity in the 70 MHz to 3 GHz bands. In this paper,we report on the project, its current status, the key science goals, and plans for early science.

Key words:telescope; active surface; large single dish;atomic hydrogen

來源出版物：Radio Science, 2016, 51(7): 1060-1064

Evaluation of solar temperature field under different wind speeds for Shanghai 65 m radio telescope

Qian, Hongliang; Chen, Deshen; Fan, Feng; et al.

Abstract:The Shanghai 65 m radio telescope is currently the largest full range rotatable radio telescope in Asia.Gravity, wind and temperature are the three main factors which may have a bad effect on the reflector’s surface precision. To study the effect of the thermal deformation caused by daily non-uniform temperature fields on the surface precision of the main reflector, both the temperature field and its effect were studied in detail for two typical days (January 15th and July 15th). The method to simulate temperature fields was studied initially,considering heat conduction, solar radiation, shadowing,air convection, sky radiation and ground radiation. Then,an integral parametric thermal finite element model (FEM)of the telescope was established using the ANSYS thermal analysis module. Finally, the effect of non-uniform temperature fields on the surface precision of the main reflector was estimated in terms of the Root Mean Square(RMS) deformation based on temperature transient analysis. The proposed methods and conclusions drawn can provide valuable information for thermal design, thermal monitoring and thermal control of the Shanghai 65 m radio telescope and other similar giant antenna structures.

Keywords:non-uniform temperature field; solar illuminetion; radio telescope; surface precision

來源出版物：International Journal of Steel Structures,2016, 16(2): 383-393

Antenna pattern measurement of the large-size radio telescope by correlation techniques and GNSS

Zhuang, Wang; Da, Huang; Wang, Meng-Nan; et al.

Abstract:It is a challenge to measure the antenna pattern of a large-sized radio telescope with a high resolution because it hardly rotates. This letter presents a simple and efficient method to measure the large-sized radio antenna pattern based on correlation techniques and the Global Navigation Satellite System (GNSS). We estimate the normalized pattern function of the electric field by utilizing correlation properties of the navigation signal in the auxiliary antenna and the radio antenna. The method avoids obtaining a large number of accurate pseudo-code information. Compared to the traditional methods based on the energy detection, the proposed method extends the measurement range and improves the measurement accuracy of the antenna pattern. At the same time, the method also has a better performance in anti-variation of channel and anti-interference.

Keywords:antenna pattern measurement; auxiliary antenna; correlation technique; GNSS

來源出版物：IEEE Antennas and Wireless Propagation Letters, 2017, 15: 1136-1139

Square Kilometre Array: The radio telescope of the XXI century

Grainge, K.; Alachkar, B; Amy, Shaun; et al.

Abstract:The Square Kilometre Array (SKA) will be the world’s largest and most sensitive radio telescope. It will address fundamental unanswered questions about our Universe including how the first stars and galaxies formed after the Big Bang, how dark energy is accelerating the expansion of the Universe, the role of magnetism in the cosmos, the nature of gravity, and the search for life beyond Earth. This project envisages the construction of 13315 m antennas in South Africa and 131072 log-periodic antennas in Australia, together with the associated infrastructure in the two desert sites. In addition, the SKA is an exemplar Big Data project, with data rates of over 10 Tbps being transported from the telescope to HPC/HTC facilities.

來源出版物：Astronomy Reports, 2017, 61(4): 288-296

Non-uniform temperature field measurement and simulation of a radio telescope’s main reflector under solar radiation

Chen, Deshen; Qian, Hongliang; Wang, Huajie; et al.

Abstract:To improve the ability of deep-space exploration,many astronomers around the world are actively engaged in the construction of large-aperture and high-precision radio telescopes. The temperature effect is one of three main factors affecting the reflector accuracy of radio telescopes.To study the daily nonuniform temperature field of the main reflector, experimental studies are first carried out with a 3 m aperture radio telescope model. According to the test results for 16 working conditions, the distribution rule and time-varying regularity of the daily temperature field are summarized initially. Next, theoretical methods for the temperature field of the main reflector are studied considering multiple environmental parameters and self-shadows. Finally, the validity of the theoretical methods is evaluated with test results. The experimental study demonstrates that the non-uniform temperature distribution of the main reflector truly exists and should not be overlooked, and that the theoretical methods for the reflector temperature field proposed in this paper are effective. The research methods and conclusions can provide valuable references for thermal design, monitoring and control of similar high-precision radio telescopes.

Keywords:radio telescope; temperature distribution;shadow distribution; solar radiation; thermal analysis

來源出版物：Applied Thermal Engineering, 2017, 111:1330-1341

The very large array: Design and performance of a modern synthesis radio telescope

Napier. PJ; Thompson. AR; Ekers. RD; et al.

Since its development in the 1960’s, the technique of obtaining high-resolution radio images of astronomical objects using Fourier synthesis has advanced sufficiently so that today such images often provide better angular resolution than is obtainable with the largest optical telescopes. A synthesis array measures the Fourier transform of the observed brightness distribution by cross-correlating the signals from antennas separated by distances up to tens of kilometers. The antennas must be equipped with low-noise receiving systems and connected together by phase-stable transmission links. Widebandwidth digital correlators are used to perform the cross correlation. The data-reduction algorithms and computing system play a critical role in determining the quality of the images produced by the array. The Very Large Array(VLA) synthesis telescope, recently constructed in New Mexico, consists of twenty-seven 25-m-diameter antennas arranged in a Y-shaped array. Each arm of the Y is approximately 21 km long and the antetmas can be moved to various positions on the arms by a rail-mounted transporter. The antennas are equipped with cryogenically cooled receiving systems and are interconnected by low-loss, TE01-mode, large-diameter waveguide. The crosscorrelation products for each of the 351 pair combinations of antennas are measured for 4 IF signals by a 50-MHz bandwidth digital correlator. In this paper we discuss the design of synthesis arrays in general, and describe the design and performance of the VLA in particular, under the seven headings: array geometry design, sensitivity considerations,phase stability requirements, signal transmission system,delay and correlator system, control system, and data-reduction requirments. In each section, we review the underlying instrumental requirements and provide details of how the VLA was designed to meet them. Recently developed data-reduction algorithms provide effective ways of correcting synthesis images for the effects of missing Fourier components and instrumental and atmospheric amplitude and phase errors. The power of these algorithms is demonstrated using actual VLA images.

來源出版物：Proceedings of the IEEE, 1983, 71(11): 1295-1320

Abstract:A new multimirror ground-based telescope for time-series photometry of rapid variable stars, designed to minimize or eliminate gaps in the brightness record caused by the rotation of the earth, is described. A sequence of existing telescopes distributed in longitude, coordinated from a single control center, is used to measure designated target stars so long as they are in darkness. Data are returned by electronic mail to the control center, where they are analyzed in real time. This instrument is the first to provide data of continuity and quality that permit true high-resolution power spectroscopy of pulsating white dwarf stars.

來源出版物：Astrophysical Journal, 1990, 361(1): 309-317

Abstract:The Hubble Deep Field (HDF) is a Director’s Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground-based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.

來源出版物：Astronomical Journal, 1996, 112(4): 1335-1386

Abstract:We describe the goals, design, implementation,and initial progress of the UKIRT Infrared Deep Sky Survey (UKIDSS), a seven-year sky survey which began in 2005 May. UKIDSS is being carried out using the UKIRT Wide Field Camera (WFCAM), which has the largest etendue of any infrared astronomical instrument to date. It is a portfolio of five survey components covering various combinations of the filter set ZYJHK and H-2. The Large Area Survey, the Galactic Clusters Survey, and the Galactic Plane Survey cover approximately 7000 square degrees to a depth ofKsimilar to 18; the Deep Extragalactic Survey covers 35 square degrees toKsimilar to 21, and the Ultra Deep Survey covers 0.77 square degrees toKsimilar to 23.Summed together UKIDSS is 12 times larger in effective volume than the 2MASS survey. The prime aim of UKIDSS is to provide a long-term astronomical legacy data base; the design is, however, driven by a series of specific goals for example, to find the nearest and faintest substellar objects, to discover Population II brown dwarfs,if they exist, to determine the substellar mass function, to break thez=7 quasar barrier; to determine the epoch of re-ionization, to measure the growth of structure fromz=3 to the present day, to determine the epoch of spheroid formation, and to map the Milky Way through the dust,to several kpc. The survey data are being uniformly processed. Images and catalogues are being made available through a fully queryable user interface-the WFCAM Science Archive. The data are being released in stages. The data are immediately public to astronomers in all ESO member states, and available to the world after 18 months.Before the formal survey began, UKIRT and the UKIDSS consortia collaborated in obtaining and analysing a series of small science verification (SV) projects to complete the commissioning of the camera. We show some results from these SV projects in order to demonstrate the likely power of the eventual complete survey. Finally, using the data from the First Data Release, we assess how well UKIDSS is meeting its design targets so far.

surveys; infrared; general

責(zé)任編輯：衛(wèi)夏雯