The Educational Adaptive-optics Solar Telescope at the Shanghai Astronomy Museum

The Educational Adaptive-optics Solar Telescope(EAST)at the Shanghai Astronomy Museum has been running routine astronomical observations since 2021.It is a 65-cm-aperture Gregorian solar telescope for scientific education,outreach,and research.The telescope system is designed in an“open”format so that the solar tower architecture can be integrated with it,and visitors can watch the observations live from inside the tower.Equipped with adaptive optics,a high-resolution imaging system,and an integral field unit spectro-imaging system,this telescope can obtain high-resolution solar images in the TiO and Hαbands,and perform spectral image reconstruction using 400 optical fibers at selected wavelengths.It can be used not only in public education and scientific outreach but also in solar physics research.

The Science of Radio Astronomy: An Investigation of Crab Nebula

The science of radio astronomy focuses on the observation and study of celestial objects by reading their radio waves. The 5 meter radio-telescope is able to observe different radio sources using a C-band LNB. This research was essentially focused on Crab Nebula, also known as Taurus A. The study led to interesting observations, which were validated numerically using various scientific computing software. The radio waves emitted by Taurus A are readable by the RTL-SDR, a software defined radio receiver. This device is capable of reading radio frequencies in the range of 0.5 MHZ to 1700 MHZ.

A High-Temperature Superconducting Wideband Bandpass Filter at the L Band for Radio Astronomy

In order to ensure the normal operation of radio astronomy observations,an extremely sensitive receiver system needs to be equipped in front of the large radio telescope.An 8-pole wideband high-temperature superconducting(HTS)filter using a Coplanar Spiral Resonator Structure with a passband of 1160~1670 MHz is developed to suppress strong radio interference.The filter is fabricated on a 36 mm×14 mm YBCO HTS film,which is deposited on a 0.5 mm thick MgO substrate.The minimum insertion loss measured in the liquid nitrogen temperature region is 0.03 dB,and the first parasitic passband appears at 2600 MHz.The measured results are in good agreement with the simulations.The filter can be used in radio telescope receivers for the observation of neutral hydrogen and pulsars,as well as in high-sensitivity satellite navigation instruments.

Space Astronomy in China: 2002-2004

More and more proposals, or potential projects have been proposed in recent two years. We try to briefly outline these new proposals, although most of them are in fact only in their conception studies. The progress of previously mentioned projects, like Space Solar Telescope (SST), the Hard X-ray Modulation Telescope (HXMT), as well as newly initiated LUnar Resource Explorer (LUREX), will be introduced elsewhere.

Space Astronomy in China During 2004 - 2006

For the past two years, some real progress has been made in Chinese Space Astronomy, though we have not launched any missions exclusively belonging to the scope of Astronomy. In order to program the next five years' national plan (2006-2010), the Chinese Space Agency organized a series of authorized evaluations for the future missions. Among more than ten astronomical mission proposals, several were selected to give the green light to continue for their Phase A studies. We try to briefly outline these proposals.

China’s Space Astronomy and Solar Physics in 2011—2012

In the first part of this paper,we describe briefly the mid and long-term plan of Chinese space astronomy,its preliminary study program,the current status of satellite missions undertaken, and the current status of astronomy experiments in China's manned space flight program.In the second part,the recent research progress made in the fields of solar physics is summarized briefly, including solar vector magnetic field,solar flares,CME and filaments,solar radio and nonthermal processes,EUV waves,MHD waves and coronal waves,solar model and helioseismology,solar wind and behavior of solar cycle.

Journey through the birth, growth and maturity of X-ray astronomy

In this biographical account, I recall my scientific journey that began in 1961 when I joined as a Physics Trainee in the BARC Training School and after one year course was admitted in TIFR as a Research Associate. During 1962–1967, I worked on determination of the He^3 /He^4 ratio in cosmic rays using a gas Cerenkov counter and also used a scintillation + solid Cerenkov detector to measure flux of protons and helium nuclei in primary cosmic rays. I also developed a large area scintillation-Cerenkov detector with a spark chamber between them for measuring charge composition of primary cosmic rays. I joined the X-ray astronomy programme in 1967 initiated by Prof. B. V. Sreekantan and played a leading role in developing a balloon borne hard X-ray instrument for studying time variability and energy spectra of cosmic X-ray sources. We carried out a series of balloon experiments and studied temporal intensity variation and energy spectra of X-ray objects like Sco X-1, Cyg X-1, etc. Results on rapid intensity changes and spectra appeared in a series of publications based on which I obtained a Ph.D. degree in 1972. Immediately afterwards, I joined Prof. Gordon Garmire at Caltech as a Research Fellow (a post-doctoral position) to work with him on the low energy component of HEAO A-2 experiment. The instrument was developed and successfully realised. Working on this satellite experiment was a thrilling experience which exposed me to the technical complexities of space instruments. The HEAO-1 satellite was launched in 1978. During 1978–1979, Guenter Riegler and I, working at JPL, reported detection of intense soft X-rays from several classes of extragalactic and Galactic objects like new BL Lacs, a new AM Her binary, coronal X-rays from active stars, etc. After returning to TIFR, I developed a rocket experiment with K. P. Singh to map the spatial and spectral distribution of the Soft Diffuse X-ray Background. At the same time, I also designed 15 cm deep Xenon filled Proportional Counters (XPCs) of ~ 2500 cm^2 area for balloon experiments which were done during 1983–1990 and produced new results on several X-ray binaries. During this period I also developed a proportional counter (PC) based satellite instrument and submitted a proposal jointly with the astronomy group at the Indian Space Research Organization (ISRO) for an Indian X-ray Astronomy Experiment (IXAE). After success of the Polar Satellite Launch Vehicle (PSLV), the IXAE instrument was included on the top deck of the IRS-P3 satellite that was launched in March 1996. Despite the severe limitation of a polar orbit, the IXAE observed a good number of X-ray binaries and produced interesting results, with the most notable being quasi-regular bursts from a new transient, GRS 1915+105, which turned out to be an enigmatic black hole source. Following success of the IXAE, a proposal for an ambitious multiwavelength astronomy satellite, named ASTROSAT, with broad spectral coverage in the optical, NUV, FUV, soft X-ray and hard X-ray by a suite of instruments, was submitted to ISRO and finally approved by the Govt. of India in 2004. Over the next 10 years, the development and fabrication of the five ASTROSAT instruments were accomplished and a PSLV launch on Sept. 28, 2015 placed ASTROSAT in a 650 km circular orbit with 6 degree inclination. The ASTROSAT instruments have been performing well for ~4 years and have observed more than 500 cosmic sources. Results from ASTROSAT have appeared in a large number of journal publications. Successful realization and performance of ASTROSAT marks culmination of my research career. I formally retired as a Senior Professor from TIFR on 2006 April 30 on attaining the age of superannuation. However by agreement with TIFR, ISRO designated me ‘ISRO Chair Professor’, which was later renamed as ISRO Satish Dhawan Professor, and asked me to continue to lead ASTROSAT as PI. At the end of my tenure as ISRO Professor on 2011 April 30, I relinquished the PI position. I am at present affiliated with the MU-DAE Centre of Excellence for Basic Sciences, Mumbai University Campus at Mumbai as an Emeritus Professor.

Characterization of silicon microstrip sensors for space astronomy

Silicon microstrip detectors are widely used in experiments for space astronomy.Before the detector is assembled,extensive characterization of the silicon microstrip sensors is indispensable and challenging.This work electrically evaluates a series of sensor parameters,including the depletion voltage,bias resistance,metal strip resistance,total leakage current,strip leakage current,coupling capacitance,and interstrip capacitance.Two methods are used to accurately measure the strip leakage current,and the test results match each other well.In measuring the coupling capacitance,we extract the correct value based on a SPICE model and two-port network analysis.In addition,the expression of the measured bias resistance is deduced based on the SPICE model.

Reminiscence of my Sixty-five year Voyage in Astronomy

I returned to China from the United Kingdom in 1953, then worked in Purple Mountain Observatory. It was the early days of new China. The elder generation of astronomers was undertaking an effort of ＂repairing broken and filling defect＂ during those post-war years, and started planning and lay- ing the foundation of modern astronomy. Under their leadership, I started a journey of astronomy whose main task was construction. The journey has been full of twists and turns. As a result of the ＂Great Leap Forward＂ in 1958 and the 1966 launch of the decade-long ＂Cultural Revolution＂ period, the situation of construction in astronomy was similar to that in other sciences, suffering bad effects. Not until the ＂Reform and Opening up＂ period after those events was construction able to continue, and various disciplines and international connections began to open. A ＂passage＂ had gradually developed. In this new circumstance, I kept pursuing the pioneers to explore a forward direction. Looking back today, this journey has been three periods of a four generation relay. This article is divided into three sections that describe my research work in these times that I recall： （1） Looking back at the beginning of the return and tracing the footprints of the founders. （2） Recalling my radio astronomy tour. （3） Retrospection and expectation of LAMOST.

Terahertz atmospheric windows for high angular resolution terahertz astronomy from Dome A

Atmospheric transmission from Dome A, Antarctica, presents new possibilities in the field of terahertz astronomy, where space telescopes have been the only observational tools until now. Using atmospheric transmission measurements from Dome A with a Fourier transform spectrometer, transmission spectra and long-term stabilities have been analyzed at 1.461 THz, 3.393 THz, 5.786 THz and 7.1 THz, which show that important atmospheric windows for terahertz astronomy open for a reasonable length of time in the winter season. With large aperture terahertz telescopes and interferometers at Dome A, high angular resolution terahertz observations are foreseen of atomic fine-structure lines from ionized gas and a water ice feature from protoplanetary disks.

IMAGING IN HIGH ENERGY ASTRONOMY

Space research is usually costly, and this restricts participation of developing countries. With traditional techniques one must construct high resolution instrument,more and more complicated and expensive, to obtain high resolution results from space observations. It is a difficult task to make observations with both high sensitivity and high resolution. Applying advanced inversion technique, one can subtract more information from old data in public domain,and, furthermore, conduct high sensitive and high-resolution experiments with low-cost low-resolution instruments. So developing and applying data analysis technique is of great importance for developing countries to do basic space science.In this paper we summarize efforts of Chinese scientists in recent years along this direction on imaging in space high energy astronomy.

Space Astronomy

This chapter reports the recent progress on the space astronomy missions of China,including the following missions:currently operating in orbit,e.g.,DAMPE,Insight-HXMT,GECAM,Polar Light,GRID and Lobster-eye X-ray Satellite;approved and under development for launch in the next a couple of years,e.g.,SVOM and EP;planned experiments to be onboard China’s Space Station in the next several years,e.g.,CSST,HERD,POLAR-2,DIXE and Ly RIC;candidate missions that have passed the first round of review of Strategy Priority Program on space science(Ⅲ)of the Chinese Academy of Sciences,e.g.,eXTP,DAMPE-2,Earth 2.0,DSL and CHES.

Progress Report on Insight-HXMT:China's First X-ray Astronomy Satellite

Insight-HXIUT is China's hrst X-ray astronomy satellite.It was launched on 15 June 2017 and is currently in service smoothly.Insight-HXMT has been used to scan the Galactic plane repeatedly,making pointing observations to neutron stars and black holes,and monitor the whole sky continuously in the MeV band.Insight-HXMT is also very flexible in making ToO observations,with the response time from about 3 hours to within a day.So far more than 50 refereed publications have been made with data from its observations;many more publications have used the data or results of Insight-HXMT one way or another.The scientific impacts of Insight-HXMT have been growing rapidly since launch.We expect Insight-HXMT to continue to operate for several more years.

Chinese Journal of Astronomy and Astrophysics

An international bimonthly journal,founded in 2001 as a continuation of Acta Astrophysica Sinica(founded in 1981,ISSN 0253-2379).The Chinese Journal of Astronomy and Astrophysics (ISSN 1009-9271)is published for the Chinese Astronomical Society and the National Astronomical Observatories of Chinese Academy of Sciences by the Science Press in Beijing.

The messier objects as a tool in teaching astronomy

The French astronomer Charles Messier (1730- 1817) compiled a catalogue [1] of astronomical objects which reached109 innumber after additions by later astronomers were added. The catalogue contains galaxies, emission nebulae, a supernova remnant, a double star, globular clusters, open clusters, an asterism, a star cloud, and planetary nebulae. While the objective of Messier in compiling the catalogue was to guide comet hunters not to be confused by his objects which he thought looked like comets [2], the Messier Catalogue as it later became known became a standard guide to astronomers for a study of the sky’s “greatest hits” or the best samples of objects which can be observed and studied. This paper explores the value of the Messier Catalogue in the teaching of Astronomy and Earth Science. The range of objects is wide and contains some of the best examples of their type. The teaching method I propose is the actual observations of the objects through a telescope, with the corresponding explanation. Some principles which will be covered through this process are stellar evolution from the birth and death of stars, galaxy types, formation of galaxies, galactic interactions, life in the Universe, cosmology, and our place in the Universe.

Protection of Radio Astronomy Frequency in China

General situation of the protection of radio astronomy frequency in China is introduced in this paper. The organization that is responsible for the management of radio frequencies in China, then the environment of international cooperation are briefly described in the first two section. The situation of the protection of radio astronomy frequency we met, and what we have done and ever achieved so far are followed to show a geneneral scene of radio environment for radio astronomy in China.

Zhang Sixun and the Prosperous Astronomy in the Song Dynasty

Chinese astronomy reached its pinnacle in the Song Dynasty(960-1279)as culture continued to prosper to a new height.The invention of the“Taiping Armillary Sphere”by Zhang Sixun,who was from Bazhong in the Shu area(today’s Sichuan province),marked a milestone in the astronomical development in China.This article delves into the driving forces behind Zhang Sixun’s outstanding contributions to astronomy from the perspectives of the important role of astronomy in the politics of the Song Dynasty,the great attention the imperial court paid to astronomy,and the influence of the Shu culture,which centers on the belief“Tian Shu Zai Shu”(the rule of the universe is best observed in Shu).

X-ray Astronomy and Einstein Probe

The Einstein Probe(EP) is an international mission initiated and led by the Chinese Academy of Sciences(CAS) to observe high-energy transients, a type of astronomical objects whose temporal dynamics helps us understand the evolution of the universe and some fundamental questions in basic physics. Expected to fly at the end of 2022, it will close a long-existing gap in X-ray astronomy. Dr. JIN Chichuan, a researcher of the EP team has the story.

National center for Antarctic astronomy inaugurated

The founding of the Chinese Center for Antarctic Astronomy was announced on 24 December, 2006, in Nanjing. As a non-corporate body, the Center is a