[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"detail-sidebar-cat-0-en-105":3,"doc-seo-270180-105":59,"doc-detail-270180-en":123},{"code":4,"msg":5,"data":6},0,"success",[7,13,18,23,28,33,38,43,48,51,55],{"id":8,"doc_module":4,"doc_module_name":9,"category_name":10,"show_sort_weight":11,"slug":12},1,"Document","Story & Novel",90,"story-novel",{"id":14,"doc_module":4,"doc_module_name":9,"category_name":15,"show_sort_weight":16,"slug":17},2,"Literature",80,"literature",{"id":19,"doc_module":4,"doc_module_name":9,"category_name":20,"show_sort_weight":21,"slug":22},4,"Exam",70,"exam",{"id":24,"doc_module":4,"doc_module_name":9,"category_name":25,"show_sort_weight":26,"slug":27},5,"Comic",60,"comic",{"id":29,"doc_module":4,"doc_module_name":9,"category_name":30,"show_sort_weight":31,"slug":32},6,"Technology",50,"technology",{"id":34,"doc_module":4,"doc_module_name":9,"category_name":35,"show_sort_weight":36,"slug":37},7,"Healthcare",40,"healthcare",{"id":39,"doc_module":4,"doc_module_name":9,"category_name":40,"show_sort_weight":41,"slug":42},8,"Research & Report",30,"research-report",{"id":44,"doc_module":4,"doc_module_name":9,"category_name":45,"show_sort_weight":46,"slug":47},9,"Religion & Spirituality",20,"religion-spirituality",{"id":46,"doc_module":4,"doc_module_name":9,"category_name":49,"show_sort_weight":46,"slug":50},"World Cup","world-cup",{"id":52,"doc_module":4,"doc_module_name":9,"category_name":53,"show_sort_weight":52,"slug":54},10,"Lifestyle","lifestyle",{"id":56,"doc_module":4,"doc_module_name":9,"category_name":57,"show_sort_weight":24,"slug":58},19,"General","general",{"code":4,"msg":60,"data":61},"ok",{"site_id":62,"language":63,"slug":64,"title":65,"keywords":66,"description":67,"schema_data":68,"social_meta":116,"head_meta":118,"extra_data":120,"updated_unix":122},105,"en","discovery-of-a-star-sensitive-to-the-spin-of-sgr-a","Discovery of a Star Sensitive to the Spin of Sgr A*","","Residing in the center of the Milky Way, Sgr A* is the closest massive black hole, enabling measurements of individual stellar orbits with periods as short as 12 years. These orbits act as test particles to probe the gravitational potential around the central 4:3×10^6 M⊙ black hole and reveal relativistic effects such as gravitational redshift, transverse Doppler effect, and prograde precession. Here, a faint main-sequence star, S301, is reported, with an 8.7-year orbit and peak velocity reaching 8% of c, making its motion directly sensitive to Sgr A* spin and suggestive of Hills-mechanism capture.",{"@graph":69,"@context":115},[70,84,106],{"@type":71,"itemListElement":72},"BreadcrumbList",[73,77,79,82],{"item":74,"name":75,"@type":76,"position":8},"https://docshare.wps.com","Home","ListItem",{"item":78,"name":9,"@type":76,"position":14},"https://docshare.wps.com/document/",{"item":80,"name":40,"@type":76,"position":81},"https://docshare.wps.com/document/research-report/",3,{"item":83,"name":65,"@type":76,"position":19},"https://docshare.wps.com/document/discovery-of-a-star-sensitive-to-the-spin-of-sgr-a/270180/",{"url":83,"name":65,"@type":85,"image":86,"author":91,"headline":65,"publisher":94,"fileFormat":97,"inLanguage":63,"description":67,"dateModified":98,"datePublished":99,"encodingFormat":97,"isAccessibleForFree":100,"interactionStatistic":101},"DigitalDocument",{"url":87,"@type":88,"width":89,"height":90},"https://docshare.wps.com/thumbnails/discovery-of-a-star-sensitive-to-the-spin-of-sgr-a/270180.png","ImageObject",300,407,{"name":92,"@type":93},"Theodore","Person",{"url":74,"name":95,"@type":96},"DocShare","Organization","application/pdf","2026-10-28","2026-09-15",true,{"@type":102,"interactionType":103,"userInteractionCount":105},"InteractionCounter",{"@type":104},"ViewAction",11,{"@type":107,"mainEntity":108},"FAQPage",[109],{"name":110,"@type":111,"acceptedAnswer":112},"What is S301 and why is it relevant to measuring Sgr A* spin?","Question",{"text":113,"@type":114},"S301 is a faint main-sequence star with an 8.7-year orbital period and a small pericenter distance. Its peak velocity and measurable trajectory make its motion directly sensitive to the spin of Sgr A*.","Answer","https://schema.org",{"og:url":83,"og:type":117,"og:title":65,"og:site_name":95,"og:description":67},"article",{"robots":119,"canonical":83},"index,follow",{"doc_id":121,"site_id":62},270180,1790508682,{"code":4,"msg":5,"data":124},{"doc_id":121,"user_id":125,"nickname":92,"user_avatar":126,"doc_module":4,"category_id":39,"category_name":40,"doc_title":65,"doc_description":67,"doc_content":127,"file_id":128,"file_url":129,"file_type":130,"file_size":131,"view_count":105,"is_deleted":4,"is_public":8,"is_downloadable":8,"audit_status":8,"page_count":132,"language":133,"language_code":63,"site_id":62,"html_lang":63,"table_of_contents":134,"faqs":135,"seo_title":136,"seo_description":67,"update_tm":137,"read_time":138,"preview_page_count":4},7971461740886,"https://ap-avatar.wpscdn.com/davatar_3d24733baf745e90a7e4bdd5f77d97b2","Discovery of a star sensitive to the spin of Sgr A*  \nK. Abd El Dayem2 , R. Abuter7 , N. Aimar 10; 13 , P. Amaro-Seoane21; 1 , A. Berdeu7;2 , J.-P. Berger4 , G. Bourdarot 1 , W. Brandner5 ,  \nA. Burkert26; 1 , D. Calderon24 , C. Correia 10; 13 , J. Cuadra22;23 , R. Davies 1 , D. Defr􀀒ere9 , L. Delit2 , A. Drescher4; 1 , F. Eisenhauer 1; 12 , L. Esteras Otal7 , M. Fabricius 1 , H. Feuchtgruber 1 , N.M. F􀁿orster Schreiber 1 , A. Foschi2 , P. Garcia 10; 13 , R. Garcia Lopez 15 , A. Generozov 18 , R. Genzel 1; 11 , S. Gillessen 1 , F. Gont􀀓e7 , X. Haubois25 , S.F. H􀁿onig8 , M. Houll􀀓e4 , S. Joharle 1 , A. Kaufer25 , J. Kammerer7 , P. Kervella2 , J. Kolb7 , L. Kreidberg5 , R. Laugier9 , S. Lacour2 , O. Lai3 , J.-B. Le Bouquin4 , J. Leftley8 , B. Lopez3 , D. Lutz 1 , F. Mang 1; 12; ∗, A. M􀀓erand7 , F. Millour3 , M. Montarg􀀒es2 , N. Moruj~ao 10; 13 , H. Nowacki3 , M. Nowak2 , S. Oberti7 , J. Osorno2;􀀃 , T. Ott 1 , T. Paumard2 , C. Paladini25 , H.B. Perets 19 , K. Perraut4 , G. Perrin2 , R. Petrov3 , P.O. Petrucci4 , T. Piran20 , N. Pourr􀀓e4 , S. Rabien 1 , D.C. Ribeiro 1 , S. Robbe-Dubois3 , M. Sadun Bordoni 1 , J. S􀀓anchez Berm􀀓udez 16 , D. Santos 1 , R. Sari20 , J. Sauter5 , S. Scheithauer5 , J. Scigliuto3 , J. Shangguan 1 , T.T. Shimizu 1 , F. Soulez 17 , J. Stadler26 , C. Straubmeier6 , E. Sturm 1 , M. Subroweit6 , C. Sykes8 , L.J. Tacconi 1 ,  \nP. Th􀀓evenet2 , I. Urso2 , F. Vincent2 , J. Woillez7 , G. Zins25 (GRAVITY+ Collaboration)  \n1 Max Planck Institute for Extraterrestrial Physics, Giessenbachstra􀀙e 1, 85748 Garching, Germany  \n2 LIRA, Observatoire de Paris, Universit􀀓e PSL, CNRS, Sorbonne Universit􀀓e, Universit􀀓e de Paris, 5 place Jules Janssen, 92195 Meudon, France  \n∗ Corresponding authors: F. Mang ([fmang@mpe.mpg.de](fmang@mpe.mpg.de)), J. Osorno ([juan.osorno@obspm.fr](juan.osorno@obspm.fr)), S. Gillessen ([ste@mpe.mpg.de](ste@mpe.mpg.de))  \n1  \n3 Universit􀀓e C^ote d'Azur, Observatoire de la C^ote d'Azur, CNRS, Laboratoire Lagrange, France  \n4 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France  \n5 Max Planck Institute for Astronomy, K􀁿onigstuhl 17, 69117 Heidelberg, Germany  \n6 1st Institute of Physics, University of Cologne, Z􀁿ulpicher Stra􀀙e 77, 50937 Cologne, Germany  \n7 European Southern Observatory, Karl-Schwarzschild-Stra􀀙e 2, 85748 Garching, Germany  \n8 School of Physics & Astronomy, University of Southampton, Southampton, SO17 1BJ, United Kingdom  \n9 Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001, Leuven, Belgium  \n10 Faculdade de Engenharia, Universidade do Porto, rua Dr. Roberto Frias, 4200-465 Porto, Portugal  \n11 Departments of Physics & Astronomy, Le Conte Hall, University of California,  \nBerkeley, CA 94720, USA  \n12 Department of Physics, Technical University of Munich, 85748 Garching, Germany  \n13 CENTRA - Centro de Astrof􀀓􀀐sica e Gravita􀀘c~ao, IST, Universidade de Lisboa, 1049-001 Lisboa, Portugal  \n14 Max Planck Institute for Radio Astronomy, auf dem H􀁿ugel 69, 53121 Bonn, Germany  \n15 School of Physics, University College Dublin, Bel􀀌eld, Dublin 4, Ireland  \n16 Instituto de Astronom􀀓􀀐a, National Autonomous University of Mexico, Mexico City, Mexico  \n17 Univ. Lyon, Univ. Lyon 1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230, Saint Genis-Laval, France  \n18 Astronomy Dept. and Oden Institute, University of Texas at Austin, Austin, TX 78712, USA  \n19 Physics department, Technion - Israel Institute of Technology, Technion city, Haifa 3200002, Israel  \n20 Racah Institute of Physics, The Hebrew University, Jerusalem 91904, Israel  \n21 Universitat Polit􀀒ecnica de Val􀀒encia, C/Vera s/n, Val􀀒encia, 46022, Spain  \n22 Universidad Adolfo Iba~nez, Av. Padre Hurtado 750, Vi~na del Mar, Chile  \n23 Millennium Nucleus on Transversal Research and Technology to Explore Supermassive Black Holes (TITANS), Chile  \n24 Max Planck Institute for Astrophysics, Karl-Schwarzschild-Stra􀀙e 1, 85748 Garching, Germany  \n25 European Southern Observatory, Casilla 19001, Santiago 19, ","cbCaipUGYpTMUIQ8","https://ap.wps.com/l/cbCaipUGYpTMUIQ8","pdf",1313760,34,"English","# Abstract\n## Keywords\n# Introduction","[{\"question\":\"What is S301 and why is it relevant to measuring Sgr A* spin?\",\"answer\":\"S301 is a faint main-sequence star with an 8.7-year orbital period and a small pericenter distance. Its peak velocity and measurable trajectory make its motion directly sensitive to the spin of Sgr A*.\"}]","Discovery of a Star Sensitive to the Spin of Sgr A* | PDF",1789455044,86]