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Three New Spiral Galaxies with Active Nuclei Producing Double Radio Lobes

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Research in Astronomy and Astrophysics 2023年第3期23卷 46-53页

作者： x.y.gao Z.S.yuan J.L.Han Z.L.Wen S.S.Shan National Astronomical Observatories Chinese Academy of SciencesBejing 10011China CAS Key Laboratory of FAST National Astronomical ObservatoriesChinese Academy of SciencesBeijing 100101China School of Astronomy University of Chinese Academy of SciencesBeijing 100049China

Double radio lobes are generally believed to be produced by active nuclei of elliptical ***,several double-lobed radio sources have been solidly found to be associated with spiral *** cross-matching~9×105 spiral galaxies selected from the Sloan Digital Sky Survey DR8 data with the full 1.4 GHz radio source catalogs of NRAO VLA Sky Survey and Faint Images of the Radio Sky at Twenty-centimeters,we identify three new spiral galaxies:J0326-0623,J1110+0321 and J1134+3046 that produce double radio lobes,and five doublelobed spirals previously *** combining the newly discovered and all the other known cases in literature,we confirm the relation that more massive spiral galaxies could produce more powerful radio *** find that most of these spiral galaxies are located in a galaxy group or a poor cluster,in which the environment is denser than in the field,and about half of them are the central brightest galaxies in their parent *** therefore suggest that the environment is one of the key factors for a spiral to produce double radio lobes.

关键词： galaxies galaxy massive

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高分辨MR血管壁成像在鉴别动脉粥样硬化相关烟雾状血管病与烟雾病中的诊断效能

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国际医学放射学杂志 2023年第6期 752-753页

作者： S.T.Liu M.M.Lu x.y.gao C.M.Wen B.B.Sun y.Liu 周新哲

摘要目的评价高分辨MR血管壁成像（HRMR-VWI）在烟雾病（MMD）与动脉粥样硬化相关烟雾状血管病（ASMMV）鉴别中的诊断效能，并探讨精准鉴别诊断的方法。方法

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Mott transition controlled by lattice-orbital coupling in double layer ruthenates

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Mott transition controlled by lattice-orbital coupling in do...

The FAST Galactic Plane Pulsar Snapshot survey:*** design and pulsar discoveries

中国晶体学会第六届学术年会暨会员代表大会——多晶（粉晶）衍射分会

作者： J.Peng M.Q.Gu x.M.Gu G.T.Zhou x.y.gao J.y.Liu W.F.xu G.Q.Liu x.Ke L.Zhang H.Han Z.Qu D.W.Fu H.L.Cai F.M.Zhang Z.Q.Mao x.S.Wu Collaborative Innovation Center of Advanced Microstrucutres Lab of Solid State Microstructures School of Physics Nanjing University Department of Physics and Engineering Physics Tulane University Ningbo Institute of Material Technology and Engineering Chinese Academy of Sciences Michigan State University High Magnetic Field Laboratory Chinese Academy of Sciences Ordered Matter Science Research Center Southeast University

We have investigated unusual phase transitions triggered by chemical doping in *** experiments show a few percent doping of Mn(>4%)can switch the quasi-two-dimensional metallic state with the antiferromagnetic order(AFM-b)comprised of ferromagnetic(FM)bilayers of CaRuO to a Mott insulating state with the nearest-neighbor antiferromagnetic order(G-AFM),

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Research in Astronomy and Astrophysics 2021年第5期21卷 5-42页

作者： J.L.Han Chen Wang P.F.Wang Tao Wang D.J.Zhou Jing-Hai Sun yi yan Wei-Qi Su Wei-Cong Jing xue Chen x.y.gao Li-Gang Hou Jun xu K.J.Lee Na Wang Peng Jiang Ren-xin xu Jun yan Heng-Qian Gan xin Guan Wen-Jun Huang Jin-Chen Jiang Hui Li yun-Peng Men Chun Sun Bo-Jun Wang H.G.Wang Shuang-Qiang Wang Jin-Tao xie Heng xu Rui yao xiao-Peng you D.J.yu Jian-Ping yuan Rai yuen Chun-Feng Zhang yan Zhu National Astronomical Observatories Chinese Academy of SciencesBeijing 100101China CAS Key Laboratory of FAST NAOCChinese Academy of SciencesBeijing 100101China School of Astronomy University of Chinese Academy of SciencesBeijing 100049China Kavli Institute for Astronomy and Astrophysics Peking UniversityBeijing 100871China Department of Astronomy Peking UniversityBeijing 100871China xinjiang Astronomical Observatory Chinese Academy of SciencesUrumqi 830011China Key Laboratory of Radio Astronomy Chinese Academy of SciencesNanjing 210008China Department of Astronomy Guangzhou UniversityGuangzhou 510006China School of Physical Science and Technology Southwest UniversityChongqing 400715China

Discovery of pulsars is one of the main goals for large radio *** Five-hundredmeter Aperture Spherical radio Telescope(FAST),that incorporates an L-band 19-beam receiver with a system temperature of about 20 K,is the most sensitive radio telescope utilized for discovering *** designed the snapshot observation mode for a FAST key science project,the Galactic Plane Pulsar Snapshot(GPPS)survey,in which every four nearby pointings can observe a cover of a sky patch of 0.1575 square degrees through beam-switching of the L-band 19-beam *** integration time for each pointing is 300 seconds so that the GPPS observations for a cover can be made in 21 *** goal of the GPPS survey is to discover pulsars within the Galactic latitude of±10∘from the Galactic plane,and the highest priority is given to the inner Galaxy within±5∘.Up to now,the GPPS survey has discovered 201 pulsars,including currently the faintest pulsars which cannot be detected by other telescopes,pulsars with extremely high dispersion measures(DMs)which challenge the currently widely used models for the Galactic electron density distribution,pulsars coincident with supernova remnants,40 millisecond pulsars,16 binary pulsars,some nulling and mode-changing pulsars and rotating radio transients(RRATs).The follow-up observations for confirmation of new pulsars have polarization-signals recorded for polarization profiles of the ***-detection of previously known pulsars in the survey data also leads to significant improvements in parameters for 64 *** GPPS survey discoveries are published and will be updated at http://***/GPPS/.

关键词： pulsars:general

The FAST Galactic Plane Pulsar Snapshot survey:Ⅰ. Project design and pulsar discoveries

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Research in Astronomy and Astrophysics 2021年第5期21卷 6-43页

作者： J.L.Han Chen Wang P.F.Wang Tao Wang D.J.Zhou Jing-Hai Sun yi yan Wei-Qi Su Wei-Cong Jing xue Chen x.y.gao Li-Gang Hou Jun xu K.J.Lee Na Wang Peng Jiang Ren-xin xu Jun yan Heng-Qian Gan xin Guan Wen-Jun Huang Jin-Chen Jiang Hui Li yun-Peng Men Chun Sun Bo-Jun Wang H.G.Wang Shuang-Qiang Wang Jin-Tao xie Heng xu Rui yao xiao-Peng you D.J.yu Jian-Ping yuan Rai yuen Chun-Feng Zhang yan Zhu National Astronomical Observatories Chinese Academy of Sciences CAS Key Laboratory of FAST NAOC Chinese Academy of Sciences School of Astronomy University of Chinese Academy of Sciences Kavli Institute for Astronomy and Astrophysics Peking University xinjiang Astronomical Observatory Chinese Academy of Sciences Key Laboratory of Radio Astronomy Chinese Academy of Sciences Department of Astronomy Peking University Department of Astronomy Guangzhou University School of Physical Science and Technology Southwest University

Discovery of pulsars is one of the main goals for large radio *** Five-hundred-meter Aperture Spherical radio Telescope (FAST),that incorporates an L-band 19-beam receiver with a system temperature of about 20 K,is the most sensitive radio telescope utilized for discovering *** designed the snapshot observation mode for a FAST key science project,the Galactic Plane Pulsar Snapshot (GPPS) survey,in which every four nearby pointings can observe a cover of a sky patch of 0.1575square degrees through beam-switching of the L-band 19-beam *** integration time for each pointing is 300 seconds so that the GPPS observations for a cover can be made in 21 *** goal of the GPPS survey is to discover pulsars within the Galactic latitude of ±10° from the Galactic plane,and the highest priority is given to the inner Galaxy within ±5°.Up to now,the GPPS survey has discovered 201 pulsars,including currently the faintest pulsars which cannot be detected by other telescopes,pulsars with extremely high dispersion measures (DMs) which challenge the currently widely used models for the Galactic electron density distribution,pulsars coincident with supernova remnants,40 millisecond pulsars,16 binary pulsars,some nulling and mode-changing pulsars and rotating radio transients (RRATs).The follow-up observations for confirmation of new pulsars have polarization-signals recorded for polarization profiles of the ***-detection of previously known pulsars in the survey data also leads to significant improvements in parameters for 64 *** GPPS survey discoveries are published and will be updated at http://***/GPPS/.

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ARF4 acting upstream of LBD16 promotes adventitious root formation in peach

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Horticultural Plant Journal 2025年第1期11卷 145-161页

作者： Jingjing Liu Lingling gao Ruoxi Zhang Anqi gao Zamith Kerubo Oginga Beibei Zheng yuepeng Han CAS Key Laboratory of Plant Germplasm Enhancement and Specialty Agriculture Wuhan Botanical GardenThe Innovative Academy of Seed Design of Chinese Academy of SciencesWuhanHubei 430074China Hubei Hongshan Laboratory WuhanHubei 430070China University of Chinese Academy of Sciences Beijing 100049China

Although class A auxin response factors(ARFs)are known to regulate adventitious root(AR)development through the canonical SCFTIR1-Aux/IAA-ARF signaling pathway,the regulatory role of class B ARFs in AR development remains largely ***,this research focused on the role of class B ARF transcription factors in peach(Prunus persica‘Shengli')adventitious root ***,we report the role of a class B ARF gene Pp ARF4 in adventitious root formation in *** transcriptome and q RT-PCR analyses showed that the transcription of Pp ARF4 was significantly up-regulated in auxin-treated stem explants.y2H assay showed that Pp ARF4 had no interaction with Pp IAAs(AUxIN/INDOLE ACETIC ACIDs).Pp ARF4 could bind the promoters of lateral root development gene Pp LBD16 and auxin transport gene Pp PIN1 to activate their *** overexpression of Pp ARF4 and Pp LBD16 in Arabidopsis promoted AR ***,Pp ARF4 could act as a negative regulator of flavone synthesis and thus prevent the explants from *** results not only provide novel insights into the functions of ARFs in regulating plant growth and development,but will also be useful for fulfilling asexual propagation by stem cuttings in peach.

关键词： Prunus persica Adventitious root Auxin Pp ARF4 Pp LBD16

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Deep view of composite SNR CTA1 with LHAASO in γ-rays up to 300 TeV

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Science China(Physics,Mechanics & Astronomy) 2025年

作者： Zhen Cao F.Aharonian Axikegu y.x.Bai y.W.Bao D.Bastieri x.J.Bi y.J.Bi W.Bian A.V.Bukevich Q.Cao W.y.Cao Zhe Cao J.Chang J.F.Chang A.M.Chen E.S.Chen H.x.Chen Liang Chen Lin Chen Long Chen M.J.Chen M.L.Chen Q.H.Chen S.Chen S.H.Chen S.Z.Chen T.L.Chen y.Chen N.Cheng y.D.Cheng M.C.Chu M.y.Cui S.W.Cui x.H.Cui y.D.Cui B.Z.Dai H.L.Dai Z.G.Dai Danzengluobu x.Q.Dong K.K.Duan J.H.Fan y.Z.Fan J.Fang J.H.Fang K.Fang C.F.Feng H.Feng L.Feng S.H.Feng x.T.Feng y.Feng y.L.Feng S.Gabici B.gao C.D.gao Q.gao W.gao W.K.gao M.M.Ge T.T.Ge L.S.Geng G.Giacinti G.H.Gong Q.B.Gou M.H.Gu F.L.Guo J.Guo x.L.Guo y.Q.Guo y.y.Guo y.A.Han O.A.Hannuksela M.Hasan H.H.He H.N.He J.y.He y.He y.K.Hor B.W.Hou C.Hou x.Hou H.B.Hu Q.Hu S.C.Hu C.Huang D.H.Huang T.Q.Huang W.J.Huang x.T.Huang x.y.Huang y.Huang y.y.Huang x.L.Ji H.y.Jia K.Jia H.B.Jiang K.Jiang x.W.Jiang Z.J.Jiang M.Jin M.M.Kang I.Karpikov D.Khangulyan D.Kuleshov K.Kurinov B.B.Li C.M.Li Cheng Li Cong Li D.Li F.Li H.B.Li H.C.Li Jian Li Jie Li K.Li S.D.Li W.L.Li W.L.Li x.R.Li xin Li y.Z.Li Zhe Li Zhuo Li E.W.Liang y.F.Liang S.J.Lin B.Liu C.Liu D.Liu D.B.Liu H.Liu H.D.Liu J.Liu J.L.Liu M.y.Liu R.y.Liu S.M.Liu W.Liu y.Liu y.N.Liu Q.Luo y.Luo H.K.Lv B.Q.Ma L.L.Ma x.H.Ma J.R.Mao Z.Min W.Mitthumsiri H.J.Mu y.C.Nan A.Neronov K.C.y.Ng L.J.Ou P.Pattarakijwanich Z.y.Pei J.C.Qi M.y.Qi B.Q.Qiao J.J.Qin A.Raza D.Ruffolo A.Sáiz M.Saeed D.Semikoz L.Shao O.Shchegolev x.D.Sheng F.W.Shu H.C.Song yu.V.Stenkin V.Stepanov y.Su D.x.Sun Q.N.Sun x.N.Sun Z.B.Sun J.Takata P.H.T.Tam Q.W.Tang R.Tang Z.B.Tang W.W.Tian L.H.Wan C.Wang C.B.Wang G.W.Wang H.G.Wang H.H.Wang J.C.Wang Kai Wang Kai Wang L.P.Wang L.y.Wang P.H.Wang R.Wang W.Wang x.G.Wang x.y.Wang y.Wang y.D.Wang y.J.Wang Z.H.Wang Z.x.Wang Zhen Wang Zheng Wang D.M.Wei J.J.Wei y.J.Wei T.Wen C.y.Wu H.R.Wu Q.W.Wu S.Wu x.F.Wu y.S.Wu S.Q.xi J.xia G.M.xiang D.x.xiao G.xiao y.L.xin y.xing D.R.xiong Z.xiong D.L.xu R.F.xu R.x.xu W.L.xu L.xue D.H.yan J.Z.yan T.yan C.W.yang C.y.yang F.yang F.F.yang L.L.yang M.J.yang R.Z.yang W.x.yang y.H.yao Z.G.yao L.Q.yin N.yin x.H.you Z.y.you y.H Southwest Jiaotong University School of Astronomy and Space Science Nanjing University Center for Astrophysics Guangzhou University Tsung-Dao Lee Institute & School of Physics and Astronomy Shanghai Jiao Tong University Institute for Nuclear Research of Russian Academy of Sciences Hebei Normal University University of Science and Technology of China LHAASO Collaboration State Key Laboratory of Particle Detection and Electronics Key Laboratory of Dark Matter and Space Astronomy & Key Laboratory of Radio Astronomy Purple Mountain Observatory Chinese Academy of Sciences Research Center for Astronomical Computing Zhejiang Laboratory Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Chinese Academy of Sciences School of Physics and Astronomy Key Laboratory of Particle Astrophysics & Experimental Physics Division & Computing Center yunnan University Key Laboratory of Cosmic Rays (Tibet University) Ministry of Education Department of Physics The Chinese University of Hong Kong Key Laboratory of Radio Astronomy and Technology National Astronomical Observatories Chinese Academy of Sciences School of Physics and Astronomy (Zhuhai) & School of Physics (Guangzhou) & Sino-French Institute of Nuclear Engineering and Technology (Zhuhai) Sun yat-sen University Institute of High Energy Physics Institute of Frontier and Interdisciplinary Science Shandong University APC Université Paris Cité CNRS/IN2P3 CEA/IRFU Observatoire de Paris Department of Engineering Physics & Department of Astronomy Tsinghua University School of Physics and Microelectronics Chinese Academy of Sciences Zhengzhou University yunnan Observatories Chinese Academy of Sciences China Center of Advanced Science and Technology College of Physics Sichuan University School of Physics Peking University Guangxi Key Laboratory for Relativistic Astrophysics School of Physical Science and Technology University of Chinese Academy of Sciences Guangxi University Department of Physics Faculty of Science Mahidol University Moscow Institute

The ultra-high-energy（UHE） gamma-ray source 1LHAASO J0007+7303u is positionally associated with the composite SNR CTA1 that is located at high Galactic Latitude b ≈ 10.5°. This provides a rare opportunity to spatially resolve the component of the pulsar wind nebula（PWN） and supernova remnant（SNR） at UHE. This paper conducted a dedicated data analysis of 1LHAASO J0007+7303u using the data collected from December 2019 to July 2023. This source is well detected with significances of 21σ and 17σ at 8-100 TeV and >100 TeV, respectively. The corresponding extensions are determined to be 0.23°±0.03°and 0.17°±0.03°. The emission is proposed to originate from the relativistic electrons accelerated within the PWN of PSR J0007+7303. The energy spectrum is well described by a power-law with an exponential cutoff function dN/dE =（42.4 ± 4.1）(E/（20 TeV）)-2.31±0.11exp(-E/（110±25 TeV）) TeV-1cm-2s-1in the energy range from 8 to 300 TeV, implying a steady-state parent electron spectrum dNe/dEe∝(Ee/（100 TeV）)-3.13±0.16exp[(-Ee/（373±70 TeV）)2] at energies above ≈ 50 TeV. The cutoff energy of the electron spectrum is roughly equal to the expected current maximum energy of particles accelerated at the PWN terminal shock. Combining the x-ray and gamma-ray emission, the current space-averaged magnetic field can be limited to≈ 4.5 μG. To satisfy the multi-wavelength spectrum and the γ-ray extensions, the transport of relativistic particles within the PWN is likely dominated by the advection process under the free-expansion phase assumption.

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LHAASO detection of very-high-energy γ-ray emission surrounding PSR J0248+6021

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Science China(Physics,Mechanics & Astronomy) 2025年

We report the detection of an extended very-high-energy(VHE) γ-ray source coincident with the location of middle-aged(62.4 kyr) pulsar PSR J0248+6021, by using the LHAASO-WCDA data of live 796 d and LHAASO-KM2A data of live 1216d. A significant excess of γ-ray induced showers is observed both by WCDA in energy bands of 1-25 Te V and KM2A in energy bands of >25 TeV with 7.3σ and 13.5σ, respectively. The best-fit position derived through WCDA data is R.A. = 42.06°± 0.12°and Dec. = 60.24°± 0.13°with an extension of 0.69°±0.15°and that of the KM2A data is R.A.= 42.29°± 0.13°and Dec. =60.38°± 0.07°with an extension of 0.37°±0.07°. No clear extended multiwavelength counterpart of this LHAASO source has been found from the radio band to the GeV band. The most plausible explanation of the VHE γ-ray emission is the inverse Compton process of highly relativistic electrons and positrons injected by the pulsar. These electrons/positrons are hypothesized to be either confined within the pulsar wind nebula or to have already escaped into the interstellar medium, forming a pulsar halo.

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Observation of the γ-ray emission from W43 with LHAASO

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Science China(Physics,Mechanics & Astronomy) 2025年

In this paper, we report the detection of the very-high-energy (VHE, 100 Ge V100 TeV) γ-ray emissions from the direction of the young star-forming region W43, observed by the Large High Altitude Air Shower Observation (LHAASO). The extended γ-ray source was detected with a significance of～16σby KM2A and～17σby WCDA, respectively. The angular extension of this γ-ray source is about 0.5 degrees, corresponding to a physical size of about 50pc. We discuss the origin of the γ-ray emission and possible cosmic ray acceleration in the W43 region using multi-wavelength data. Our findings suggest that W43 is likely another young star cluster capable of accelerating cosmic rays (CRs) to at least several hundred TeV.

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