Astronomy:Xuntian

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Short description: A planned Chinese space telescope
Xuntian (CSST)
China CSST Xuntian.jpg
Artist's impression of Xuntian space telescope
Mission typeAstronomy
OperatorCNSA
Mission duration10+ years (planned)
Spacecraft properties
Dry mass15,500 kilograms (34,200 lb)[1]
Start of mission
Launch date2025 (planned)
RocketLong March 5B (Y5)
Launch siteWenchang Satellite Launch Center
ContractorCASC
Orbital parameters
Reference systemLow Earth orbit
Main telescope
Diameter2 metres (6.6 ft)
Focal length28 m (92 ft)
Wavelengths255 ~ 1000 nm (Survey camera), 0.41~0.51 THz (590~730 μm) (Terahertz receiver)
Resolution0.15 arcsec
Tiangong program
← Mengtian module
 

Xuntian (Chinese: 巡天; pinyin: Xúntiān),[lower-alpha 1] also known as the Chinese Survey Space Telescope[4][5] (CSST) (Chinese: 巡天空间望远镜; pinyin: Xúntiān Kōngjiān Wàngyuǎnjìng) is a planned Chinese space telescope currently under development.[6] It will feature a 2-meter (6.6 foot) diameter primary mirror and is expected to have a field of view 300–350 times larger than the Hubble Space Telescope.[7] This will allow the telescope to image up to 40 percent of the sky using its 2.5 gigapixel camera over ten years.

Xuntian is scheduled for launch in 2025[8] on a Long March 5B rocket to co-orbit with the Tiangong space station in slightly different orbital phases, which will allow for periodic docking with the station.[9]

An artist's rendering of the 2 m-aperture Survey Space Telescope (also known as the China Space Station Telescope, CSST)

This state-of-the-art telescope, characterized by its off-axis design without any obstruction, sidesteps diffraction challenges associated with mirror support structures. As a result, its point spread function (PSF) remains unscathed, presenting a valuable asset for weak-lensing shear measurements. The CSST is equipped with five first-generation instruments, including a survey camera, a terahertz receiver, a multichannel imager, an integral field spectrograph, and a cool planet imaging coronagraph.[10]

Estimated distribution of the observation pointing centers of the survey for 1, 3, 5, 7, 9 and 10 years, respectively. The yellow circles in the bottom right figure are the selected deep fields. All maps use an Aitoff projection in equatorial coordinates, with origin α = δ = 0 at the center and α increasing from right to left. Mean densities are shown for the observation pointing centers in cells of about 0.84 square degrees.
Estimated distribution of the observation pointing centers of the CSST survey for 1, 3, 5, 7, 9 and 10 years.[11]

The primary mission of the CSST revolves around high-resolution large-area multiband imaging and slitless spectroscopy surveys, spanning the wavelength range of 255–1,000 nm. Precise cosmology serves as the principal scientific driver behind this ambitious endeavor, with a focus on observing regions at median-to-high Galactic and ecliptic latitudes. Over a period of 10 years, the survey camera is slated to cover approximately 17,500 square degrees of the sky in various bands, reaching point-source 5σ limiting magnitudes of about 26 (AB mag) in g and r bands.

The CSST's spectral resolution (R=λ/Δλ) for the slitless spectrograph averages no less than 200, attaining wide-band-equivalent limiting magnitudes in GV (400–620 nm) and GI (620–1,000 nm) bands at about 23 mag. Beyond its wide-area survey, the CSST will target specific deep fields, aiming for observations that surpass the depth of the broader survey by at least one magnitude. The collective strengths of its angular resolution, depth, wavelength range, and capacity for both imaging and spectroscopy, coupled with extensive sky coverage, render the CSST survey highly competitive.

Notably, the CSST's observations are poised to complement and enhance other contemporaneous large-scale projects, including the Vera Rubin Observatory, Euclid, and the Nancy Roman Space Telescope. Together, these initiatives promise to yield unprecedented datasets that hold the potential for groundbreaking discoveries spanning the realms from our solar system to cosmology and beyond.

Instruments

Survey camera

The survey camera is also known as the multi-color photometry and slitless spectroscopy survey module. The module is located at the main focal plane and divided into the multi-color photometry submodule of 7 bands (NUV, u, g, r, i, z, y) and the slitless spectroscopy submodule of 3 bands (GU, GV, GI). The multi-color photometry submodule includes 18 filters, covering 60% of the area of this module. The slitless spectroscopy submodule includes 12 gratings, covering the other 40% of the area.

Focal plane arrangement of the CSST survey camera
System throughput of CSST survey bands

Terahertz receiver

The terahertz receiver, also known as the high sensitivity terahertz detection module (HSTDM), enables terahertz (THz) astronomical observations from space. Conducting THz observations in space eliminates Earth's atmospheric absorption. HSTDM is a high-resolution spectrometer and the first space heterodyne receiver using niobium nitride (NbN)-based superconducting tunnel junction (Superconductor-Insulator-Superconductor (SIS)) mixer (the NbN SIS mixer).[12]

Multichannel imager

Left: The transmission curves for the nine MCI medium-band filters from NUV to NIR bands, including the F275W, F336W, F375M, F450M, F500M, F630M, F763M, F845M and F960M. Right: The transmission curves for the seven survey camera filters, including the NUV, u, g, r, i, z, and y bands. The dotted curves show the detector quantum efficiency, and the dashed lines and the solid lines are the intrinsic transmission and the total transmission by considering detector quantum efficiency, respectively.
Transmission curves of MCI and the survey camera[13]

The Multichannel imager (MCI) has three channels covering the same wavelength range as the survey camera from the NUV to NIR bands, and these channels can work simultaneously. Three sets of filters, i.e., narrow-, medium-, and wide-band filters, will be installed on the MCI to perform extreme-deep field surveys with a field of view of 7.5′×7.5′. The magnitude limit can be stacked to a depth of 29–30 AB mag in three channels. It will study the formation and evolution of high-z galaxies, properties of dark matter and dark energy, and also can be used to calibrate the photo-z measurements with its nine medium-band filters for the main surveys.[13]

Integral field spectrograph

The CSST-IFS (Integral Field Spectrograph) is one of the 5 instruments onboard the CSST. The key advantages of the CSST-IFS are the high spatial resolution of 0.2" and the full range optical wavelength coverage (0.35-1.0 μm). Considering the limitation of the 2-meter aperture of the CSST, the CSST-IFS is optimal for targeting compact and bright sources, which therefore will be irreplaceable for studying galactic central regions (AGN feedback) and star-forming regions. [14]

Cool planet imaging coronagraph

The cool planet imaging coronagraph (CPI-C) aims to realize high-contrast (< 10-8) direct imaging of exoplanets with an inner working angle (IWA) of 0.35′′ in the visible (0.6328 μm). It plans to follow up exoplanets discovered by radial velocity observations, study planet formation and evolution, and probe protoplanetary disks.[15] CPI-C works at 0.53-1.6 μm and is equipped with 7 broad passbands.

See also

Notes

  1. ↑ The name "Xuntian" comes from the Chinese translation of Astronomical survey (巡天调查, Xúntiān Diàochá). Xuntian can also literally translated as "surveying the sky"[2] or "survey to heavens".[3]

References

  1. ↑ Hu Zhan (2019-11-05). "An Update on the Chinese Space Station Telescope Project" (in en). National Astronomical Observatories. https://www.issibern.ch/teams/weakgravlense/wp-content/uploads/2019/11/H.-Zhan.pdf. Retrieved 2021-10-23. 
  2. ↑ "China Space Station Telescope "Almost Complete"". 2022-07-22. https://english.cas.cn/newsroom/news/202207/t20220722_308680.shtml. 
  3. ↑ "China's massive Xuntian Telescope set to beat NASA's Hubble Space Telescope". 2022-07-24. https://tech.hindustantimes.com/tech/news/chinas-massive-xuntian-telescope-set-to-beat-nasa-s-hubble-space-telescope-71658637590156.html. 
  4. ↑ "Flagship Chinese Space Telescope to Unravel Cosmic Mysteries". Chinese Academy of Sciences. 7 May 2022. https://english.cas.cn/newsroom/cas_media/202205/t20220507_305162.shtml. 
  5. ↑ Hu Zhan (2021-09-22). "The Chinese Survey Space Telescope" (in en). National Astronomical Observatories. http://ilariacaiazzo.com/wp-content/uploads/2021/09/HuZhanSlides.pdf. Retrieved 2021-09-22. 
  6. ↑ Gao, Ming; Zhao, Guangheng; Gu, Yidong (2015). "我国空间站的空间科学与应用任务" (in zh). Bulletin of Chinese Academy of Sciences (CAS) 30 (6): 721–732. doi:10.16418/j.issn.1000-3045.2015.06.002. http://www.bulletin.cas.cn/publish_article/2015/6/20150602.htm. Retrieved 2 May 2016. 
  7. ↑ "Outgunning NASA's Hubble, China Claims Its Xuntian Telescope with 350-Fold Bigger View Can Unravel 'Cosmic Mysteries'". 8 May 2022. https://eurasiantimes.com/china-claims-its-xuntian-telescope-with-350-fold-bigger/. 
  8. ↑ Qiu, Xiaoqing; Fan, Zhou; Song, Yihan; Gu, Hongrui; Jiang, Haijiao; Li, Jing (15 November 2023). "CSST Slitless Spectroscopy Ground Test Based on the 80 cm Telescope at the Xinglong Observatory". Astronomical Research and Technology 20: 564–575. doi:10.14005/j.cnki.issn1672-7673.20230911.001. http://html.rhhz.net/Jwk_twyjyjs/html/20230609.htm. 
  9. ↑ Jones, Andrew (20 April 2021). "China wants to launch its own Hubble-class telescope as part of space station". Space.com. https://www.space.com/china-hubble-class-telescope-for-space-station. 
  10. ↑ Zhan, Hu (2021-04-01). "The wide-field multiband imaging and slitless spectroscopy survey to be carried out by the Survey Space Telescope of China Manned Space Program" (in en). Chinese Science Bulletin 66 (11): 1290–1298. doi:10.1360/TB-2021-0016. ISSN 0023-074X. https://engine.scichina.com/doi/10.1360/TB-2021-0016. 
  11. ↑ Fu, Zhen-Sen; Qi, Zhao-Xiang; Liao, Shi-Long; Peng, Xi-Yan; Yu, Yong; Wu, Qi-Qi; Shao, Li; Xu, You-Hua (2023-06-02). "Simulation of CSST's astrometric capability". Frontiers in Astronomy and Space Sciences 10. doi:10.3389/fspas.2023.1146603. ISSN 2296-987X. Bibcode: 2023FrASS..1046603F. 
  12. ↑ 张坤, 姚明; ZHANG Kun, YAO Ming (2023-03-07). "高灵敏度太赫兹探测模块氮化铌超导SIS混频器空间环境适应性研究" (in zh). 红外与毫米波学报 42 (2): 188–192. doi:10.11972/j.issn.1001-9014.2023.02.006. ISSN 1001-9014. http://journal.sitp.ac.cn/hwyhmb/hwyhmbcn/article/abstract/2022256. 
  13. ↑ 13.0 13.1 Cao, Ye; Gong, Yan; Zheng, Zhen-Ya; Xu, Chun (2022-02-01). "Calibrating Photometric Redshift Measurements with the Multi-channel Imager (MCI) of the China Space Station Telescope (CSST)". Research in Astronomy and Astrophysics 22 (2): 025019. doi:10.1088/1674-4527/ac424e. ISSN 1674-4527. Bibcode: 2022RAA....22b5019C. https://iopscience.iop.org/article/10.1088/1674-4527/ac424e. 
  14. ↑ "Progress of the CSST-IFS". https://www.phy.cuhk.edu.hk/events/conf2023//abstract/Shiyin_Shen.html. 
  15. ↑ Gao, Ming; Zhao, Guangheng; Gu, Yidong (2022). "Recent Progress in Space Science and Applications of China’s Space Station in 2020–2022" (in en). 空间科学学报(Chin. J. Space Sci.) 42 (4): 503–510. doi:10.11728/cjss2022.04.yg29. ISSN 0254-6124. https://www.cjss.ac.cn/cn/article/doi/10.11728/cjss2022.04.yg29. 



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