Sciences with the 2.5-meter Wide Field Survey Telescope (WFST)
The Wide Field Survey Telescope (WFST) is a dedicated photometric surveying facility being built jointly by the University of Science and Technology of China and the Purple Mountain Observatory. It is equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera...
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| creator | Collaboration, WFST Wang, Tinggui Liu, Guilin Cai, Zhenyi Geng, Jinjun Fang, Min He, Haoning Ji-an, Jiang Jiang, Ning Xu, Kong Li, Bin Li, Ye Luo, Wentao Pan, Zhizheng Wu, Xuefeng Yang, Ji Yu, Jiming Zheng, Xianzhong Zhu, Qingfeng Yi-Fu, Cai Chen, Yuanyuan Chen, Zhiwei Dai, Zigao Fan, Lulu Fan, Yizhong Fang, Wenjuan He, Zhicheng Hu, Lei Hu, Maokai Jin, Zhiping Jiang, Zhibo Li, Guoliang Li, Fan Li, Xuzhi Liang, Runduo Lin, Zheyu Liu, Qingzhong Liu, Wenhao Liu, Zhengyan Liu, Wei Liu, Yao Zheng, Lou Qu, Han Sheng, Zhenfeng Shi, Jianchun Shu, Yiping Su, Zhenbo Sun, Tianrui Wang, Hongchi Wang, Huiyuan Wang, Jian Wang, Junxian Wei, Daming Wei, Junjie Xue, Yongquan Yan, Jingzhi Yang, Chao Ye Yuan Yuan, Yefei Zhang, Hongxin Zhang, Miaomiao Zhao, Haibin Zhao, Wen |
| description | The Wide Field Survey Telescope (WFST) is a dedicated photometric surveying facility being built jointly by the University of Science and Technology of China and the Purple Mountain Observatory. It is equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera with 0.73 gigapixels on the primary focal plane for high-quality image capture over an FOV of 6.5-square-degree. It is anticipated that WFST will be set up at the Lenghu site in the summer of 2023 and begin to observe the northern sky in four optical bands (u, g, r, and i) with a range of cadences, from hourly/daily in the Deep High-Cadence Survey (DHS) program to semiweekly in the Wide-Field Survey (WFS) program, three months later. During a photometric night, a nominal 30 s exposure in the WFS program will reach a depth of 22.27, 23.32, 22.84, and 22.31 (AB magnitudes) in these four bands, respectively, allowing for the detection of a tremendous amount of transients in the low-z universe and a systematic investigation of the variability of Galactic and extragalactic objects. In the DHS program, intranight 90 s exposures as deep as 23 (u) and 24 mag (g), in combination with target of opportunity follow-ups, will provide a unique opportunity to explore energetic transients in demand for high sensitivities, including the electromagnetic counterparts of gravitational wave events, supernovae within a few hours of their explosions, tidal disruption events and fast, luminous optical transients even beyond a redshift of unity. In addition, the final 6-year co-added images, anticipated to reach g=25.8 mag in WFS or 1.5 mags deeper in DHS, will be of fundamental importance to general Galactic and extragalactic science. The highly uniform legacy surveys of WFST will serve as an indispensable complement to those of LSST that monitor the southern sky. |
| doi_str_mv | 10.48550/arxiv.2306.07590 |
| format | Article |
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It is equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera with 0.73 gigapixels on the primary focal plane for high-quality image capture over an FOV of 6.5-square-degree. It is anticipated that WFST will be set up at the Lenghu site in the summer of 2023 and begin to observe the northern sky in four optical bands (u, g, r, and i) with a range of cadences, from hourly/daily in the Deep High-Cadence Survey (DHS) program to semiweekly in the Wide-Field Survey (WFS) program, three months later. During a photometric night, a nominal 30 s exposure in the WFS program will reach a depth of 22.27, 23.32, 22.84, and 22.31 (AB magnitudes) in these four bands, respectively, allowing for the detection of a tremendous amount of transients in the low-z universe and a systematic investigation of the variability of Galactic and extragalactic objects. In the DHS program, intranight 90 s exposures as deep as 23 (u) and 24 mag (g), in combination with target of opportunity follow-ups, will provide a unique opportunity to explore energetic transients in demand for high sensitivities, including the electromagnetic counterparts of gravitational wave events, supernovae within a few hours of their explosions, tidal disruption events and fast, luminous optical transients even beyond a redshift of unity. In addition, the final 6-year co-added images, anticipated to reach g=25.8 mag in WFS or 1.5 mags deeper in DHS, will be of fundamental importance to general Galactic and extragalactic science. The highly uniform legacy surveys of WFST will serve as an indispensable complement to those of LSST that monitor the southern sky.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2306.07590</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>CCD cameras ; Explosions ; Gravitational waves ; Northern sky ; Photometry ; Physics - Astrophysics of Galaxies ; Physics - High Energy Astrophysical Phenomena ; Physics - Instrumentation and Methods for Astrophysics ; Physics - Solar and Stellar Astrophysics ; Primary mirrors ; Red shift ; Sky surveys (astronomy) ; Southern sky ; Supernovae ; Transients (astronomy)</subject><ispartof>arXiv.org, 2023-09</ispartof><rights>2023. This work is published under http://creativecommons.org/licenses/by/4.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><rights>http://creativecommons.org/licenses/by/4.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,780,881,27902</link.rule.ids><backlink>$$Uhttps://doi.org/10.1007/s11433-023-2197-5$$DView published paper (Access to full text may be restricted)$$Hfree_for_read</backlink><backlink>$$Uhttps://doi.org/10.48550/arXiv.2306.07590$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Collaboration, WFST</creatorcontrib><creatorcontrib>Wang, Tinggui</creatorcontrib><creatorcontrib>Liu, Guilin</creatorcontrib><creatorcontrib>Cai, Zhenyi</creatorcontrib><creatorcontrib>Geng, Jinjun</creatorcontrib><creatorcontrib>Fang, Min</creatorcontrib><creatorcontrib>He, Haoning</creatorcontrib><creatorcontrib>Ji-an, Jiang</creatorcontrib><creatorcontrib>Jiang, Ning</creatorcontrib><creatorcontrib>Xu, Kong</creatorcontrib><creatorcontrib>Li, Bin</creatorcontrib><creatorcontrib>Li, Ye</creatorcontrib><creatorcontrib>Luo, Wentao</creatorcontrib><creatorcontrib>Pan, Zhizheng</creatorcontrib><creatorcontrib>Wu, Xuefeng</creatorcontrib><creatorcontrib>Yang, Ji</creatorcontrib><creatorcontrib>Yu, Jiming</creatorcontrib><creatorcontrib>Zheng, Xianzhong</creatorcontrib><creatorcontrib>Zhu, Qingfeng</creatorcontrib><creatorcontrib>Yi-Fu, Cai</creatorcontrib><creatorcontrib>Chen, Yuanyuan</creatorcontrib><creatorcontrib>Chen, Zhiwei</creatorcontrib><creatorcontrib>Dai, Zigao</creatorcontrib><creatorcontrib>Fan, Lulu</creatorcontrib><creatorcontrib>Fan, Yizhong</creatorcontrib><creatorcontrib>Fang, Wenjuan</creatorcontrib><creatorcontrib>He, Zhicheng</creatorcontrib><creatorcontrib>Hu, Lei</creatorcontrib><creatorcontrib>Hu, Maokai</creatorcontrib><creatorcontrib>Jin, Zhiping</creatorcontrib><creatorcontrib>Jiang, Zhibo</creatorcontrib><creatorcontrib>Li, Guoliang</creatorcontrib><creatorcontrib>Li, Fan</creatorcontrib><creatorcontrib>Li, Xuzhi</creatorcontrib><creatorcontrib>Liang, Runduo</creatorcontrib><creatorcontrib>Lin, Zheyu</creatorcontrib><creatorcontrib>Liu, Qingzhong</creatorcontrib><creatorcontrib>Liu, Wenhao</creatorcontrib><creatorcontrib>Liu, Zhengyan</creatorcontrib><creatorcontrib>Liu, Wei</creatorcontrib><creatorcontrib>Liu, Yao</creatorcontrib><creatorcontrib>Zheng, Lou</creatorcontrib><creatorcontrib>Qu, Han</creatorcontrib><creatorcontrib>Sheng, Zhenfeng</creatorcontrib><creatorcontrib>Shi, Jianchun</creatorcontrib><creatorcontrib>Shu, Yiping</creatorcontrib><creatorcontrib>Su, Zhenbo</creatorcontrib><creatorcontrib>Sun, Tianrui</creatorcontrib><creatorcontrib>Wang, Hongchi</creatorcontrib><creatorcontrib>Wang, Huiyuan</creatorcontrib><creatorcontrib>Wang, Jian</creatorcontrib><creatorcontrib>Wang, Junxian</creatorcontrib><creatorcontrib>Wei, Daming</creatorcontrib><creatorcontrib>Wei, Junjie</creatorcontrib><creatorcontrib>Xue, Yongquan</creatorcontrib><creatorcontrib>Yan, Jingzhi</creatorcontrib><creatorcontrib>Yang, Chao</creatorcontrib><creatorcontrib>Ye Yuan</creatorcontrib><creatorcontrib>Yuan, Yefei</creatorcontrib><creatorcontrib>Zhang, Hongxin</creatorcontrib><creatorcontrib>Zhang, Miaomiao</creatorcontrib><creatorcontrib>Zhao, Haibin</creatorcontrib><creatorcontrib>Zhao, Wen</creatorcontrib><title>Sciences with the 2.5-meter Wide Field Survey Telescope (WFST)</title><title>arXiv.org</title><description>The Wide Field Survey Telescope (WFST) is a dedicated photometric surveying facility being built jointly by the University of Science and Technology of China and the Purple Mountain Observatory. It is equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera with 0.73 gigapixels on the primary focal plane for high-quality image capture over an FOV of 6.5-square-degree. It is anticipated that WFST will be set up at the Lenghu site in the summer of 2023 and begin to observe the northern sky in four optical bands (u, g, r, and i) with a range of cadences, from hourly/daily in the Deep High-Cadence Survey (DHS) program to semiweekly in the Wide-Field Survey (WFS) program, three months later. During a photometric night, a nominal 30 s exposure in the WFS program will reach a depth of 22.27, 23.32, 22.84, and 22.31 (AB magnitudes) in these four bands, respectively, allowing for the detection of a tremendous amount of transients in the low-z universe and a systematic investigation of the variability of Galactic and extragalactic objects. In the DHS program, intranight 90 s exposures as deep as 23 (u) and 24 mag (g), in combination with target of opportunity follow-ups, will provide a unique opportunity to explore energetic transients in demand for high sensitivities, including the electromagnetic counterparts of gravitational wave events, supernovae within a few hours of their explosions, tidal disruption events and fast, luminous optical transients even beyond a redshift of unity. In addition, the final 6-year co-added images, anticipated to reach g=25.8 mag in WFS or 1.5 mags deeper in DHS, will be of fundamental importance to general Galactic and extragalactic science. The highly uniform legacy surveys of WFST will serve as an indispensable complement to those of LSST that monitor the southern sky.</description><subject>CCD cameras</subject><subject>Explosions</subject><subject>Gravitational waves</subject><subject>Northern sky</subject><subject>Photometry</subject><subject>Physics - Astrophysics of Galaxies</subject><subject>Physics - High Energy Astrophysical Phenomena</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Physics - Solar and Stellar Astrophysics</subject><subject>Primary mirrors</subject><subject>Red shift</subject><subject>Sky surveys (astronomy)</subject><subject>Southern sky</subject><subject>Supernovae</subject><subject>Transients (astronomy)</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>BENPR</sourceid><sourceid>GOX</sourceid><recordid>eNotj8FLwzAYxYMgOOb-AE8GvOih9WvSpM1FkGFVGHhoYceSpl9YRrfWtJ3uv1_dPDze5fHe-xFyF0EYp0LAs_a_7hAyDjKERCi4IjPGeRSkMWM3ZNH3WwBgMmFC8Bl5yY3DvcGe_rhhQ4cNUhaKYIcDerp2NdLMYVPTfPQHPNICG-xN2yF9XGd58XRLrq1uelz8-5wU2Vux_AhWX--fy9dVoJWAgIvESonSJMrGVlprDKZMcLSTUKla6yqKteUVaBPpFJKKAVNcAmBdR5rPyf2l9gxXdt7ttD-Wf5DlGXJKPFwSnW-_R-yHctuOfj99Ktk0JWNIlOAn9LRS2g</recordid><startdate>20230914</startdate><enddate>20230914</enddate><creator>Collaboration, WFST</creator><creator>Wang, Tinggui</creator><creator>Liu, Guilin</creator><creator>Cai, Zhenyi</creator><creator>Geng, Jinjun</creator><creator>Fang, Min</creator><creator>He, Haoning</creator><creator>Ji-an, Jiang</creator><creator>Jiang, Ning</creator><creator>Xu, Kong</creator><creator>Li, Bin</creator><creator>Li, Ye</creator><creator>Luo, 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Hu, Maokai ; Jin, Zhiping ; Jiang, Zhibo ; Li, Guoliang ; Li, Fan ; Li, Xuzhi ; Liang, Runduo ; Lin, Zheyu ; Liu, Qingzhong ; Liu, Wenhao ; Liu, Zhengyan ; Liu, Wei ; Liu, Yao ; Zheng, Lou ; Qu, Han ; Sheng, Zhenfeng ; Shi, Jianchun ; Shu, Yiping ; Su, Zhenbo ; Sun, Tianrui ; Wang, Hongchi ; Wang, Huiyuan ; Wang, Jian ; Wang, Junxian ; Wei, Daming ; Wei, Junjie ; Xue, Yongquan ; Yan, Jingzhi ; Yang, Chao ; Ye Yuan ; Yuan, Yefei ; Zhang, Hongxin ; Zhang, Miaomiao ; Zhao, Haibin ; Zhao, Wen</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a950-357f66e6c79f4f6ffcce8253ef53ee99daab14af3b0ac1a807b20293600edd1a3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>CCD cameras</topic><topic>Explosions</topic><topic>Gravitational waves</topic><topic>Northern sky</topic><topic>Photometry</topic><topic>Physics - Astrophysics of Galaxies</topic><topic>Physics - High Energy Astrophysical 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Yefei</creatorcontrib><creatorcontrib>Zhang, Hongxin</creatorcontrib><creatorcontrib>Zhang, Miaomiao</creatorcontrib><creatorcontrib>Zhao, Haibin</creatorcontrib><creatorcontrib>Zhao, Wen</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni Edition)</collection><collection>ProQuest Central UK/Ireland</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central Korea</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>ProQuest Central (New)</collection><collection>ProQuest One Academic (New)</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Middle East (New)</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Applied & Life Sciences</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>Engineering Collection</collection><collection>arXiv.org</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Collaboration, WFST</au><au>Wang, Tinggui</au><au>Liu, Guilin</au><au>Cai, Zhenyi</au><au>Geng, Jinjun</au><au>Fang, Min</au><au>He, Haoning</au><au>Ji-an, Jiang</au><au>Jiang, Ning</au><au>Xu, Kong</au><au>Li, Bin</au><au>Li, Ye</au><au>Luo, Wentao</au><au>Pan, Zhizheng</au><au>Wu, Xuefeng</au><au>Yang, Ji</au><au>Yu, Jiming</au><au>Zheng, Xianzhong</au><au>Zhu, Qingfeng</au><au>Yi-Fu, Cai</au><au>Chen, Yuanyuan</au><au>Chen, Zhiwei</au><au>Dai, Zigao</au><au>Fan, Lulu</au><au>Fan, Yizhong</au><au>Fang, Wenjuan</au><au>He, Zhicheng</au><au>Hu, Lei</au><au>Hu, Maokai</au><au>Jin, Zhiping</au><au>Jiang, Zhibo</au><au>Li, Guoliang</au><au>Li, Fan</au><au>Li, Xuzhi</au><au>Liang, Runduo</au><au>Lin, Zheyu</au><au>Liu, Qingzhong</au><au>Liu, Wenhao</au><au>Liu, Zhengyan</au><au>Liu, Wei</au><au>Liu, Yao</au><au>Zheng, Lou</au><au>Qu, Han</au><au>Sheng, Zhenfeng</au><au>Shi, Jianchun</au><au>Shu, Yiping</au><au>Su, Zhenbo</au><au>Sun, Tianrui</au><au>Wang, Hongchi</au><au>Wang, Huiyuan</au><au>Wang, Jian</au><au>Wang, Junxian</au><au>Wei, Daming</au><au>Wei, Junjie</au><au>Xue, Yongquan</au><au>Yan, Jingzhi</au><au>Yang, Chao</au><au>Ye Yuan</au><au>Yuan, Yefei</au><au>Zhang, Hongxin</au><au>Zhang, Miaomiao</au><au>Zhao, Haibin</au><au>Zhao, Wen</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Sciences with the 2.5-meter Wide Field Survey Telescope (WFST)</atitle><jtitle>arXiv.org</jtitle><date>2023-09-14</date><risdate>2023</risdate><eissn>2331-8422</eissn><abstract>The Wide Field Survey Telescope (WFST) is a dedicated photometric surveying facility being built jointly by the University of Science and Technology of China and the Purple Mountain Observatory. It is equipped with a 2.5-meter diameter primary mirror, an active optics system, and a mosaic CCD camera with 0.73 gigapixels on the primary focal plane for high-quality image capture over an FOV of 6.5-square-degree. It is anticipated that WFST will be set up at the Lenghu site in the summer of 2023 and begin to observe the northern sky in four optical bands (u, g, r, and i) with a range of cadences, from hourly/daily in the Deep High-Cadence Survey (DHS) program to semiweekly in the Wide-Field Survey (WFS) program, three months later. During a photometric night, a nominal 30 s exposure in the WFS program will reach a depth of 22.27, 23.32, 22.84, and 22.31 (AB magnitudes) in these four bands, respectively, allowing for the detection of a tremendous amount of transients in the low-z universe and a systematic investigation of the variability of Galactic and extragalactic objects. In the DHS program, intranight 90 s exposures as deep as 23 (u) and 24 mag (g), in combination with target of opportunity follow-ups, will provide a unique opportunity to explore energetic transients in demand for high sensitivities, including the electromagnetic counterparts of gravitational wave events, supernovae within a few hours of their explosions, tidal disruption events and fast, luminous optical transients even beyond a redshift of unity. In addition, the final 6-year co-added images, anticipated to reach g=25.8 mag in WFS or 1.5 mags deeper in DHS, will be of fundamental importance to general Galactic and extragalactic science. The highly uniform legacy surveys of WFST will serve as an indispensable complement to those of LSST that monitor the southern sky.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2306.07590</doi><oa>free_for_read</oa></addata></record> |
| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2023-09 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_2306_07590 |
| source | arXiv.org; Free E- Journals |
| subjects | CCD cameras Explosions Gravitational waves Northern sky Photometry Physics - Astrophysics of Galaxies Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics Primary mirrors Red shift Sky surveys (astronomy) Southern sky Supernovae Transients (astronomy) |
| title | Sciences with the 2.5-meter Wide Field Survey Telescope (WFST) |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-02-21T20%3A35%3A40IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=Sciences%20with%20the%202.5-meter%20Wide%20Field%20Survey%20Telescope%20(WFST)&rft.jtitle=arXiv.org&rft.au=Collaboration,%20WFST&rft.date=2023-09-14&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.2306.07590&rft_dat=%3Cproquest_arxiv%3E2825640795%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2825640795&rft_id=info:pmid/&rfr_iscdi=true |