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The putative center in NGC1052

文献类型：期刊论文

作者Baczko, Anne-Kathrin155,156; Kadler, Matthias154; Ros, Eduardo155; Fromm, Christian M.153,154,155; Wielgus, Maciek155; Perucho, Manel151,152; Krichbaum, Thomas P.155; Baloković, Mislav150; Blackburn, Lindy148,149; Chan, Chi-kwan1,146,147
刊名ASTRONOMY & ASTROPHYSICS
出版日期2024-12-17
卷号692
ISSN号0004-6361
DOI10.1051/0004-6361/202450898
产权排序第109完成单位
文献子类Article
英文摘要Context. Many active galaxies harbor powerful relativistic jets, however, the detailed mechanisms of their formation and acceleration remain poorly understood. Aims. To investigate the area of jet acceleration and collimation with the highest available angular resolution, we study the innermost region of the bipolar jet in the nearby low-ionization nuclear emission-line region (LINER) galaxy NGC1052. Methods. We combined observations of NGC1052 taken with VLBA, GMVA, and EHT over one week in the spring of 2017. Our study is focused on the size and continuum spectrum of the innermost region containing the central engine and the footpoints of both jets. We employed a synchrotron-self absorption model to fit the continuum radio spectrum and we combined the size measurements from close to the central engine out to similar to 1 pc to study the jet collimation. Results. For the first time, NGC1052 was detected with the EHT, providing a size of the central region in-between both jet bases of 43 mu as perpendicular to the jet axes, corresponding to just around 250 R-S (Schwarzschild radii). This size estimate supports previous studies of the jets expansion profile which suggest two breaks of the profile at around 3 x 10(3) R-S and 1 similar to 10(4) R-S distances to the core. Furthermore, we estimated the magnetic field to be 1.25 Gauss at a distance of 22 mu as from the central engine by fitting a synchrotron-self absorption spectrum to the innermost emission feature, which shows a spectral turn-over at similar to 130 GHz. Assuming a purely poloidal magnetic field, this implies an upper limit on the magnetic field strength at the event horizon of 2:6 x 10(4) Gauss, which is consistent with previous measurements. Conclusions. The complex, low-brightness, double-sided jet structure in NGC1052 makes it a challenge to detect the source at millimeter (mm) wavelengths. However, our first EHT observations have demonstrated that detection is possible up to at least 230 GHz. This study o ffers a glimpse through the dense surrounding torus and into the innermost central region, where the jets are formed. This has enabled us to finally resolve this region and provide improved constraints on its expansion and magnetic field strength.
学科主题天文学 ; 天体物理学 ; 高能天体物理学 ; 星系与宇宙学
URL标识查看原文
出版地17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE
WOS关键词ACTIVE GALACTIC NUCLEI ; LOW-LUMINOSITY AGN ; NGC 1052 ; H2O MASER ; JET ; RADIO ; ACCRETION ; TORUS ; NGC-1052 ; FLOWS
资助项目international Gemini Observatory; NSF NOIRLab; U.S. National Science Foundation; United States of America; National Research Foundation of Korea(NRF) - Korea government(MSIT)[RS-2024-00449206]; NASA through the NASA Hubble Fellowship[HST-HF2-51552.001A]; Space Telescope Science Institute; NASA[NAS5-26555]
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:001410383100001
出版者EDP SCIENCES S A
资助机构international Gemini Observatory ; NSF NOIRLab ; U.S. National Science Foundation ; United States of America ; National Research Foundation of Korea(NRF) - Korea government(MSIT)[RS-2024-00449206] ; NASA through the NASA Hubble Fellowship[HST-HF2-51552.001A] ; Space Telescope Science Institute ; NASA[NAS5-26555]
版本出版稿
源URL[http://ir.ynao.ac.cn/handle/114a53/28172]  
专题星系类星体研究组
云南天文台_中国科学院天体结构与演化重点实验室
作者单位1.Data Science Institute, University of Arizona, 1230 N. Cherry Ave., Tucson, AZ 85721, USA;
2.Department of Physics and Astronomy, Michigan State University, 567 Wilson Rd, East Lansing, MI 48824, USA
3.Astronomy Department, University of Science and Technology of China, Hefei 230026, PR China;
4.Center for Astronomy and Astrophysics and Department of Physics, Fudan University, Shanghai 200438, PR China;
5.Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK;
6.School of Physics, Huazhong University of Science and Technology, Wuhan, Hubei 430074, PR China;
7.School of Natural Sciences, Institute for Advanced Study, 1 Einstein Drive, Princeton, NJ 08540, USA;
8.Radboud Excellence Fellow of Radboud University, Nijmegen, The Netherlands;
9.Tuorla Observatory, Department of Physics and Astronomy, University of Turku, FI-20014 TURUN YLIOPISTO, Finland;
10.Physics Department, Brandeis University, 415 South Street, Waltham, MA 02453, USA;
推荐引用方式
GB/T 7714		 Baczko, Anne-Kathrin,Kadler, Matthias,Ros, Eduardo,et al. The putative center in NGC1052[J]. ASTRONOMY & ASTROPHYSICS,2024,692.
APA Baczko, Anne-Kathrin.,Kadler, Matthias.,Ros, Eduardo.,Fromm, Christian M..,Wielgus, Maciek.,...&Zhao, Guang-Yao.(2024).The putative center in NGC1052.ASTRONOMY & ASTROPHYSICS,692.
MLA Baczko, Anne-Kathrin,et al."The putative center in NGC1052".ASTRONOMY & ASTROPHYSICS 692(2024).

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来源：云南天文台

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