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Compact Bright Radio-loud AGNs. III. A Large VLBA Survey at 43 GHz

文献类型：期刊论文

作者Cheng, X-P1,2,3; An, T.1,4; Frey, S.5,6; Hong, X-Y1,2,4; He, X.1; Kellermann, K., I7; Lister, M. L.8; Lao, B-Q1; Li, X-F1,2; Mohan, P.1
刊名ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
出版日期2020-04-01
卷号247期号:2页码:27
ISSN号0067-0049
关键词Very long baseline interferometry Active galaxies Surveys Radio loud quasars Jets
DOI10.3847/1538-4365/ab791f
英文摘要We present the results from the 43 GHz Very Long Baseline Array (VLBA) observations of 124 compact radio-loud active galactic nuclei (AGNs) that were conducted between 2014 November and 2016 May. The typical dimensions of the restoring beam in each image are about 0.5 mas x 0.2 mas. The highest resolution of 0.2 mas corresponds to a physical size of 0.02 pc for the lowest redshift source in the sample. The 43 GHz very long baseline interferometry (VLBI) images of 97 AGNs are presented for the first time. We study the source compactness on milliarcsecond and submilliarcsecond scales, and suggest that 95 sources in our sample are suitable for future space VLBI observations. By analyzing our data supplemented with other VLBA AGN surveys from the literature, we find that the core brightness temperature increases with increasing frequency below a break frequency similar to 7 GHz, and decreases between similar to 7 and 240 GHz but increases again above 240 GHz in the rest frame of the sources. This indicates that the synchrotron opacity changes from optically thick to thin. We also find a strong statistical correlation between radio and gamma-ray flux densities. Our correlation is tighter than those in the literature derived from lower-frequency VLBI data, suggesting that the gamma-ray emission is produced more cospatially with the 43 GHz VLBA core emission. This correlation can also be extrapolated to the unbeamed AGN population, implying that a universal gamma-ray production mechanism might be at work for all types of AGNs.
WOS关键词ACTIVE GALACTIC NUCLEI ; CELESTIAL REFERENCE FRAME ; BASE-LINE INTERFEROMETRY ; PEAKED SPECTRUM SOURCES ; COMPLETE SAMPLE ; CALIBRATOR SURVEY ; VLA OBSERVATIONS ; SPACE ; JETS ; TEMPERATURE
资助项目SKA pre-research funding - National Key R&D Programme of China[2018YFA0404602] ; SKA pre-research funding - National Key R&D Programme of China[2018YFA0404603] ; Chinese Academy of Sciences (CAS)[114231KYSB20170003] ; Hungarian National Research, Development and Innovation Office[2018-2.1.14-TET-CN-2018-00001] ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT[2019H1D3A1A01102564] ; Shanghai Astronomical Observatory through an MoU ; NRAO[BA111] ; NASA-Fermi grants[NNX15AU76G] ; NASA-Fermi grants[NNX12A087G] ; NASA[NNX08AW31G] ; NASA[NNX11A043G] ; NASA[NNX14AQ89G] ; NSF[AST-0808050] ; NSF[AST-1109911]
WOS研究方向Astronomy & Astrophysics
语种英语
出版者IOP PUBLISHING LTD
WOS记录号WOS:000523420200001
资助机构SKA pre-research funding - National Key R&D Programme of China ; SKA pre-research funding - National Key R&D Programme of China ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; Hungarian National Research, Development and Innovation Office ; Hungarian National Research, Development and Innovation Office ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Shanghai Astronomical Observatory through an MoU ; Shanghai Astronomical Observatory through an MoU ; NRAO ; NRAO ; NASA-Fermi grants ; NASA-Fermi grants ; NASA ; NASA ; NSF ; NSF ; SKA pre-research funding - National Key R&D Programme of China ; SKA pre-research funding - National Key R&D Programme of China ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; Hungarian National Research, Development and Innovation Office ; Hungarian National Research, Development and Innovation Office ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Shanghai Astronomical Observatory through an MoU ; Shanghai Astronomical Observatory through an MoU ; NRAO ; NRAO ; NASA-Fermi grants ; NASA-Fermi grants ; NASA ; NASA ; NSF ; NSF ; SKA pre-research funding - National Key R&D Programme of China ; SKA pre-research funding - National Key R&D Programme of China ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; Hungarian National Research, Development and Innovation Office ; Hungarian National Research, Development and Innovation Office ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Shanghai Astronomical Observatory through an MoU ; Shanghai Astronomical Observatory through an MoU ; NRAO ; NRAO ; NASA-Fermi grants ; NASA-Fermi grants ; NASA ; NASA ; NSF ; NSF ; SKA pre-research funding - National Key R&D Programme of China ; SKA pre-research funding - National Key R&D Programme of China ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; Hungarian National Research, Development and Innovation Office ; Hungarian National Research, Development and Innovation Office ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Korea Research Fellowship Program through the National Research Foundation of Korea (NRF) - Ministry of Science and ICT ; Shanghai Astronomical Observatory through an MoU ; Shanghai Astronomical Observatory through an MoU ; NRAO ; NRAO ; NASA-Fermi grants ; NASA-Fermi grants ; NASA ; NASA ; NSF ; NSF
源URL[http://ir.bao.ac.cn/handle/114a11/55420]  
专题中国科学院国家天文台
通讯作者An, T.
作者单位1.Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China
2.Univ Chinese Acad Sci, 19A Yuquanlu, Beijing 100049, Peoples R China
3.Korea Astron & Space Sci Inst, 776 Daedeok Daero, Daejeon 34055, South Korea
4.Chinese Acad Sci, Key Lab Radio Astron, Nanjing 210008, Peoples R China
5.Res Ctr Astron & Earth Sci, Konkoly Observ, Konkoly Thege Miklos Ut 15-17, H-1121 Budapest, Hungary
6.Eotvos Lorand Univ, Inst Phys, Pazmany Peter Setany 1-A, H-1117 Budapest, Hungary
7.Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA
8.Purdue Univ, Dept Phys, 525 Northwestern Ave, W Lafayette, IN 47907 USA
9.Chalmers Univ Technol, Dept Earth & Space Sci, Onsala Space Observ, SE-43992 Onsala, Sweden
推荐引用方式
GB/T 7714		 Cheng, X-P,An, T.,Frey, S.,et al. Compact Bright Radio-loud AGNs. III. A Large VLBA Survey at 43 GHz[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2020,247(2):27.
APA Cheng, X-P.,An, T..,Frey, S..,Hong, X-Y.,He, X..,...&Zhao, W..(2020).Compact Bright Radio-loud AGNs. III. A Large VLBA Survey at 43 GHz.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,247(2),27.
MLA Cheng, X-P,et al."Compact Bright Radio-loud AGNs. III. A Large VLBA Survey at 43 GHz".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 247.2(2020):27.

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