Xinjiang Astronomical Observatory

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The main administration in Ürümqi

The Xinjiang Astronomical Observatory ( Chinese 中国科学院 新疆 天文台 , English XinJiang Astronomical Observatory , XAO ) in Urumqi , Science 1 Street 150, is an astronomical research facility of the Chinese Academy of Sciences , established in 1957 as the "Urumqi Satellite Observation Station of the Chinese Academy of Sciences “(中国科学院 乌鲁木齐 人造卫星 观测 站) was founded. Wang Na (王娜, * 1965) has been the director of the observatory since February 2005.

history

On October 4, 1957, the Soviet Union launched the first artificial Earth satellite, Sputnik 1 . Eleven days later, on October 15, Deputy Prime Minister Nie Rongzhen and Mikhail Georgievich Pervukhin , Deputy Chairman of the Council of Ministers of the USSR , signed the “Agreement between the Chinese Government and the Government of the Soviet Union on the Manufacture of Novel Arms and Military Equipment and Construction a comprehensive nuclear industry in China ”. On the basis of this agreement, the "Satellite Observation Network of the Chinese Academy of Sciences" (中国 人造卫星 观测 网络, Pinyin Zhōnggúo Rénzào Wèixīng Guāncè Wǎngluò ) was set up in China from November 1957 , initially with 12 optical observation stations, one of them Ürümqi. From October 1958 lecturers from the Faculty of Physics of the Agricultural Institute of the People's Liberation Army (新疆 八一 农学院, Pinyin Xīnjiāng Bā Yī Nóng Xuéyuàn ), at that time the only university in Xinjiang , who observed the trajectories of the Soviet satellites - the first Chinese satellite did not take off into space until April 24, 1970 - and forwarded the data to the higher-level agencies.

After the break with the Soviet Union in 1960, of course, the orbital data of the satellites were no longer reported to Baikonur , and actual astronomical observations began. This was intensified under the aegis of Yang Rupu (杨汝 朴), who was head or party secretary of the Ürümqi satellite observation station from February 1980 to July 1987. In September 1982 a binocular solar telescope with a lens diameter of 18 cm was installed for the observation of the chromosphere and the photosphere . In August 1983, a radio telescope with a dish diameter of 2 m followed, which was used to continuously observe the electromagnetic radiation of the sun in the 3.2 cm band. This was the first radio telescope in Xinjiang.

On October 26, 1987, the new realities were also formally taken into account and the former satellite observation station was renamed "Urumqi Astronomical Station of the Chinese Academy of Sciences" (中国科学院 乌鲁木齐 天文 站). On April 21, 2001, the Yunnan Astronomical Observatory , the Research Institute of Astronomical Optics and Technology, Nanjing , the Changchun Satellite Observation Station, and the Ürumqi Astronomical Station were formed into the National Astronomical Observatories of the Chinese Academy of Sciences , located in Beijing (the Astronomical Observatory Shanghai and the Purple Mountain Observatory were also part of the new organization for practical purposes, but retained their status as separate legal entities).

On 22 November 1993, the Astronomical Station had in the past 75 km south of Urumqi Municipal put a radio telescope with a 25-meter parabolic antenna in operation Gangou (甘沟乡) (see below). In 2010, reference point stations for the navigation satellites used by the Chinese Tectonic Observation Network (中国 大陆 构造 环境 监测 网络) were set up in Bayanbulak and Ulastai, on the south side of the Tian Shan. So the area of ​​the facility extended far beyond Urumqi. The station (站) was upgraded to an observatory (台) in January 2011 and was given its current name Xinjiang Astronomical Observatory (新疆 天文台, Pinyin Xīnjiāng Tiānwéntái ). On August 27, 2011, the new door plate was unveiled in a festive ceremony.

Branch offices

Nanshan

The Nanshan radio telescope

The construction of the Nanshan base (南山 基地, lit. "base in the southern mountains", international code N87 ) began on August 30, 1991 with the ceremonial laying of the foundation stone for the 25-m radio telescope. The name of the facility is derived from its location in the foothills of the Tian Shan, 75 km south of Ürümqi, and has nothing to do with the Nan Shan Mountains on the border between Qinghai and Gansu . The radio telescope, located at an altitude of 2080 m above sea level and designed from the start as part of the Chinese VLBI network , was put into operation on November 22, 1993. The telescope in the Cassegrain Beam Waveguide design currently works on the wavelengths 18 cm, 13 cm, 6 cm, 3.6 cm and 1.3 cm, i.e. the frequency bands L, C, X, K , and can be accurate to 15 arc seconds be aligned. The telescope is in use almost all year round, in 2010 for example on 349 days, 6453 hours of which are pure observation time; that year, 813 hours were spent on system maintenance.

The Nanshan Telescope, known internationally as the “Nanshan Radio Telescope” or “NSRT”, has been part of the People's Republic of China's lunar program since 2005, i.e. since the first tests on the ground, and has been part of the 2007 Chang'e-1 mission the radio observatories in Miyun near Beijing, Kunming and Shanghai established a VLBI network for orbital observation of the lunar probes. In 2013/14, the telescope was then under the direction of Aili Yusup, chief engineer of the Nanshan base and planning manager for the lunar exploration activities of the Ürümqi observatory, in preparation for the Chang'e-4 mission as well as for future return missions (the 3rd phase of the lunar program) expanded to a diameter of 26 m and installed a dual frequency receiver for the S and X bands.

In 2009 the base had already been expanded to an area of ​​21 hectares, with a dormitory, canteen, electricity and water supply. In addition to the 26 m radio telescope, traditionally often referred to as the 25 m telescope to this day, the facility, which was renamed the “Nanshan Observation Station” (南山 观测 站) in 2015, has a high-precision optoelectronic 40 cm telescope, an 80 -cm telescope and some optical telescopes with 30 cm lens diameter, which are used to observe space debris. In 2005 , a 1.2 m telescope for quantum communication was installed for the Scientific Quantum Experiment Satellite (量子 科学 实验 卫星, Pinyin Liàngzǐ Kēxué Shíyàn Wèixīng ), abbreviated to QUESS because of the English name Quantum Experiments at Space Scale international September 2017 a tap-proof video conference was held with the Institute for Quantum Optics and Quantum Information in Vienna .

There are also three ground stations for navigation satellites on the Nanshan site:

  • Reference point station for the navigation satellites used by the Chinese Tectonic Observation Network

Kashgar

A map of the plate drift created with navigation satellite data

The Kashgar satellite ground station of the Xinjiang Astronomical Observatory (喀什 卫星 地面站, Pinyin Kāshí Wèixīng Dìmiànzhàn ), not to be confused with the one built in the late 1960s, the then "Department of Satellite Geodesy" in Weinan (now subordinate to the Xi'an satellite control center ) Kashgar (喀什 地面 观测 站) or the reconnaissance satellite ground station Kashgar (中国 遥感 卫星 地面站 喀什 站), which went into operation on January 28, 2008 , is a ground station specially designed for the navigation satellites of the Chinese Regional Positioning System (中国 区域 定位 系统, Pinyin Zhōnggúo Qūyù Dìngwèi Xìtǒng ), internationally abbreviated to CAPS after the English name “Chinese Area Positioning System”, as well as the satellites of the Beidou satellite navigation system .

Located in the Ostliche Muztagh Strasse, about 1 km east of the Baltic Sea, 5 scientists and engineers as well as 4 administrative employees are responsible for the recording and dissemination of data necessary for research in the fields of geodesy , geodynamics and especially plate tectonics , as well as for forecasts used to change the duration of the revolution of the earth . A larger parabolic antenna is available for this on the east side of the building and 8 smaller parabolic antennas on the south side.

Bayanbulak

In October 2006, the Chinese Office for Seismology , the Chinese Academy of Sciences, the then Office for Topography and Cartography at the General Staff (today Office for Satellite-Based Navigation of the Joint General Staff at the Central Military Commission ), the State Office for Land Surveying, Cartography and Geoinformation, the Chinese Weather Service and the Ministry of Education established the Chinese Tectonic Observation Network. In December 2007 we started to build a total of 260 reference stations for navigation satellites, one of them in 2010, the GNSS -Bezugspunktstation Bayanbulak of the Astronomical Observatory Xinjiang (巴音布鲁克GNSS基准站, Pinyin Bayin Bùlǔkè GNSS Jīzhǔnzhàn ) in the district of Hejing the Mongolian Autonomous Prefecture Bayingolin on the south side of the Tian Shan. The data collected by Bayanbulak and the other reference point stations serve not only for basic research on plate tectonics, geodynamics, etc., but above all for earthquake prediction and the assessment of the extent of earthquake damage.

Ulastai

The first antenna groups of the 21CMA system in December 2004

The Ulastai observation station (乌拉斯 台 观测 站, Pinyin Wūlāsītái Guāncèzhàn ) is also in Hejing County, 440 km east of Bayanbulak in the area of ​​the village of Ulastai Chaghan (乌拉斯 台 查 汗 村) in the municipality of Algu (阿拉 沟乡) . On a plateau 2650 m above sea level, far from civilization (194 km from the county seat), d. H. with little interference from radio and television signals, a radio interferometer consisting of 81 groups with 127 logarithmic-periodic antennas each (i.e. a total of 10,287 antennas) was built here from 2004 to July 2006 , which are arranged in two L-shaped perpendicular to each other, precisely in north- South and east-west facing arms of 4 km and 3 km in length are arranged. With these fixed, non-swiveling antennas, a sky area of ​​10 ° × 10 ° around the north celestial pole is observed around the clock in the frequency range 50 MHz to 200 MHz with a resolution of 24 kHz to avoid the 21 cm background radiation of the hydrogen line from the stars, Record supernovas and black holes from the reionization era of the universe. Actually, a wavelength of 21 cm corresponds to a frequency of 1420 MHz, but since the signals have been strongly redshifted due to the expansion of the universe in the last 12 billion years , one looks now in Ulastai at 50–200 MHz. Because of the English name “Primeval Structure Telescope”, the system is abbreviated internationally with PaST, often also referred to as “21 centimeter array” or 21CMA. It is operated as a kind of prototype for the planned square kilometer array in Australia and South Africa.

Since the infrastructure and personnel were already available with the 21CMA system, and of course also because of the low civilizational interference radiation above 20 MHz, the "Tian Shan Radio Experiment for Neutrino Detection", TREND for short, was set up there from 2008, a joint project the Chinese Academy of Sciences with the French Center national de la recherche scientifique . In the first phase of this experiment, the air showers generated by cosmic rays were to be detected by means of an antenna system on the basis of the radio radiation emitted. In spring 2010 15 logarithmic-periodic antennas and 3 scintillation counters were installed more or less along the 21CMA axes in Ulastai. In the summer and autumn of that year the system was expanded 250 m to the east to a total of 50 antennas; Regular measuring operations with the expanded system have been running since March 2011.

In the long term, a "Giant Radio Array for Neutrino Detection", GRAND for short, with around 100,000 antennas, spread over 200,000 km², is to be built according to this principle. As a preliminary stage, the GRANDproto system with 35 three-armed spiral antennas and 24 scintillation counters was built in Ulastai in 2017, also called "GRANDproto35" because of the number of antennas. The next stage is a plant that will extend over an area of ​​300 km². GRANDproto, like TREND and 21CMA, is headed by Wu Xiangping (武向平, * 1961) from the Cosmology Research Group at the National Astronomical Observatories of the Chinese Academy of Sciences ; the Xinjiang observatory provides 3 engineers and 2 technicians who look after the systems on site.

500 m east of the data acquisition center of the Ulastai observation station, the Ulastai GNSS reference point station (乌拉斯 台 GNSS 基准 站, Pinyin Wūlāsītái GNSS Jīzhǔnzhàn ) was set up for the Chinese Tectonic Observation Network in 2010, at the same time as the Bayanbulak reference point station. Located on gravel, sand and clay sediments from the Holocene and Young Pleistocene , 1 km south of a tectonic fault , it, like its sister station in Bayanbulak, serves not only for basic research on plate tectonics, geodynamics, etc., but above all for earthquake forecasting. Both reference point stations are subordinate to Zhang Ali (张 阿丽) from the research laboratory for applied astronomy (应用 天文 研究室) at the main administration of the observatory in Ürümqi.

Qitai

In March 2010, a symposium on the construction took place in Ürümqi with the participation of Zhan Wenlong (詹文龙, * 1955), Vice President of the Academy of Sciences, Yang Gang (杨刚, * 1953), Vice Chairman of the Standing Committee of the Xinjiang Government, and other cadres of a large-diameter radio telescope in Xinjiang. The decision was made for a location in a valley on the northern slope of the Tian Shan, now known as the “Astronomy Valley” (天文 谷, Pinyin Tiānwén Gǔ ), in the area of ​​the large community of Banjiegou (半截 沟镇) in Qitai County , 202 km to the east the then Nanshan base. The Astronomy Valley measures about 1.5 km from east to west and 2 km from north to south and is located at an altitude of 1730-1830 m above sea level. On August 27, 2011, the day the Xinjiang Observatory received its new door plate, the first of many workshops on the fully pivoting radio telescope with a diameter of 110 m was held in Urumqi, and on July 15, 2012, in the presence of the first groundbreaking ceremony in the Astronomy Valley took place with many prominent figures from science and politics.

While the construction machines were laying access roads and building foundations in Qitai, the “Program 973” for the promotion of basic research (973 计划, Pinyin 973 Jìhuà , for “started at the 3rd meeting of the science and technology management group in the year 1997 "), d. H. With funding from the Department of Science and Education at the Ministry of Finance of the People's Republic of China (财政部 科教 司), a preparatory project was initiated to find out about the technology required for the parabolic antenna, internationally abbreviated as QTT because of the English name "Qitai Telescope" to get clear. As part of this project, symposia are still held today, for example on November 11-14. July 2018 in Ürümqi with the participation of representatives of MT Mechatronics from Mainz , which was involved in the construction of the 100-m radio telescope Effelsberg from 1968 to 1971 and has been involved in the Qitai project since February 2012, most recently on 17-20. December 2018 in Guangzhou . The preparatory project should be completed in the course of 2019. In November 2018, engineers began to be recruited for the broadband receiver (150 MHz – 115 GHz) and data processing for the actual antenna.

Research areas

The employed 36 professors, 11 engineers and 4 laboratory directors of the observatory (as of April 2019) work with their master and doctoral students - the Xinjiang observatory is a campus of the University of the Chinese Academy of Sciences - and numerous other scientists, including Otmar Lochner and Christian Henkel from the Max Planck Institute for Radio Astronomy , currently in four areas:

The research group Pulsars (脉冲 星 研究 团队) headed by Wang Na is currently using the 25 m radio telescope in Nanshan to observe 300 pulsars, including around a dozen millisecond pulsars , which can serve as potential timers for a pulsar-based standard time. In addition, one deals with the observation of so-called " RRATs ", short for "Rotating Radio Transients", ie pulsars with occasional intermittent pulses, and magnetars , as well as the search for new radio pulsars . Since observing four pulsars in January 1996 - the first pulsar observation in China - the research group has published more than 100 publications on topics such as magnetic field and radiation bursts from magnetars, rotation model and thermal evolution of neutron stars, and much more.

The Orion A molecular cloud

The research group Formation and Evolution of Stars (恒星 形成 与 演化 研究 团组) under the direction of Jarken Esimbek, deputy director of the observatory since March 2014, is currently mainly concerned with giant molecular clouds , their structure and physical properties. Star formation in the Milky Way and neighboring galaxies takes place almost exclusively in giant molecular clouds; The scientists around Jarken Esimbek are particularly interested in the initial conditions for the formation of massive stars , so-called H-II regions , i.e. gas clouds with a large amount of ionized atomic hydrogen, and the triggers for star formation. In addition, a targeted search for natural water measles is currently taking place in areas where massive stars are formed. In 2013, the spectrometer installed on the 25 m radio telescope in Nanshan was used to observe the ammonia absorption line in giant molecular clouds, initially in the Taurus molecular cloud, and more recently in the Orion A molecular cloud in order to gain a better insight to get into the structure of these clouds.

The research group Galaxies and Cosmology (星系 宇宙 学 研究 团组) under the direction of Liu Xiang (刘祥) is currently investigating active galaxy nuclei, both with the 25 m radio telescope in Nanshan as a single telescope and as part of the international VLBI Networks such as the European VLBI Network. The scientists led by Liu Xiang are primarily interested in the changes in the radiation emitted by these galaxy nuclei over the course of a day and from year to year, for which they developed their own software for analyzing the data. They were able to confirm that the strong and rapid changes are mainly caused by interstellar scintillation , i.e. the deflection of radiation in the interstellar medium , analogous to the twinkling of stars in the visible sky.

The Microwave Receivers (微波 接收机 团组) group headed by Chen Maozheng (陈 卯 蒸) is responsible for the maintenance, improvement and new development of receivers. Together with the Max Planck Institute for Radio Astronomy, a cooled double polarization receiver for the 6 cm or C band was developed and built in Bonn and then installed in the Nanshan telescope, where it is now part of the Galaxies and Cosmology research group Observation of the radiation from active galaxy nuclei, which varies within a day, is used. In addition, a cooled double-polarization receiver for the 1.3 cm or K-band was produced on site in Ürümqi, which, installed in the Nanshan telescope, was used by the star formation and evolution research group for the systematic search for ammonia absorption lines used in the galactic plane . The latest project by the engineers working with Chen Maozheng is the development of a broadband receiver (150 MHz – 115 GHz) for the 100 m radio telescope currently under construction in Qitai.

Individual evidence

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Coordinates: 43 ° 51 ′ 56 ″  N , 87 ° 34 ′ 19 ″  E