脉冲星B0329+54的S/X双频CVN观测
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摘要
利用CVN(Chinese VLBI Network)对脉冲星B0329+54进行了首次S/X双频观测,观测采用相位参考模式,频段为S/X双频16通道观测,数据采集终端是CDAS(Chinese Data Acquirement System),单通道带宽16 MHz.使用上海VLBI(very long baseline interferometry)中心的Di FX(Distributed FX)相关处理机对数据进行相关处理.利用Di FX特有的Pulsar Binning模式,以提高数据信噪比.对观测数据处理后得到了S/X两波段的高分辨率图像和位置信息,与前人VLBI结果对比显示观测结果较为符合.
A VLBI(very long baseline interferometry) observation of pulsar B0329+54was carried out with CVN(Chinese VLBI Network) in February 2015. It is the first time for CVN to observe the pulsar B0329+54 in S/X dual frequency bands. The observation was performed in phase referencing mode. The observation data, including16 channels and 16 MHz bandwidth of each channel, were collected by CDAS(Chinese Data Acquirement System). The correlation was made by the Di FX(Distributed FX)correlator at Shanghai Astronomical Observatory. The pulsar binning mode in Di FX was used to increase the signal to noise ratio of the pulsar fringes. We obtained the accurate position of pulsar B0329+54 through the VLBI image. Our results are in good agreement with the previous VLBI results.
A VLBI(very long baseline interferometry) observation of pulsar B0329+54was carried out with CVN(Chinese VLBI Network) in February 2015. It is the first time for CVN to observe the pulsar B0329+54 in S/X dual frequency bands. The observation was performed in phase referencing mode. The observation data, including16 channels and 16 MHz bandwidth of each channel, were collected by CDAS(Chinese Data Acquirement System). The correlation was made by the Di FX(Distributed FX)correlator at Shanghai Astronomical Observatory. The pulsar binning mode in Di FX was used to increase the signal to noise ratio of the pulsar fringes. We obtained the accurate position of pulsar B0329+54 through the VLBI image. Our results are in good agreement with the previous VLBI results.
引文
[1]Baade W,Zwicky W.PNSA,1934,20:254
[2]Hewish A,Bell S J,Pilkington J D H,et al.Nature,1968,217:709
[3]Gold T.Nature,1968,218:731
[4]Pacini F.Nature,1968,219:145
[5]Taylor J H.Proceedings of the IEEE,1991,7:1054
[6]陈浩,吴鑫基.天文学进展,1985,4:158
[7]杨树启,陈鼎,蔡宏兵,等.天文学报,2012,53:411
[8]Yang S Q,Chen D,Cai H B,et al.Ch A&A,2013,37:195
[9]Manchester R N.Science,2004,304:542
[10]Lorimer D R,Yates J A,Lyne A G,et al.MNRAS,1995,273:411
[11]Lorimer D R,Kramer M.Hadnbook of Pulsar Astronomy.Cambridge:Cambridge University Press,2005:13
[12]Rickett B J.ARA&A,1990,28:561
[13]Han J L.Tuerbulence,Dynamos,Accretion Disks,Pulsars and Collective Plasma Processes.New York:Springer,2008:99
[14]钱志瀚,李金岭.甚长基线干涉测量技术在深空探测中的应用.北京:中国科学技术出版社,2012:34
[15]Fritz G,Henry R C,Meekins J F,et al.Science,1969,164:709
[16]Deller A T,Tingay S J,Bailes M,et al.PASP,2007,119:318
[17]Brisken W F,Benson J,Goss W M.Ap J,2002,571:906
[18]Chatterjee S,Cordes J M,Vlemmings W H T,et al.Ap J,2004,604:339
[19]Hobbs G B,Edwards R T,Manchester R N.MNRAS,2006,369:655
[20]Hobbs G B,Edwards R T,Manchester R N.MNRAS,2006,372:1549
[21]Guo L,Zheng X W,Zhang B,et al.Science China Physics,Mechanics and Astronomy,2010,53:1559
[22]Wayth R B,Brisken W F,Deller A T,et al.Ap J,2011,735:97
[2]Hewish A,Bell S J,Pilkington J D H,et al.Nature,1968,217:709
[3]Gold T.Nature,1968,218:731
[4]Pacini F.Nature,1968,219:145
[5]Taylor J H.Proceedings of the IEEE,1991,7:1054
[6]陈浩,吴鑫基.天文学进展,1985,4:158
[7]杨树启,陈鼎,蔡宏兵,等.天文学报,2012,53:411
[8]Yang S Q,Chen D,Cai H B,et al.Ch A&A,2013,37:195
[9]Manchester R N.Science,2004,304:542
[10]Lorimer D R,Yates J A,Lyne A G,et al.MNRAS,1995,273:411
[11]Lorimer D R,Kramer M.Hadnbook of Pulsar Astronomy.Cambridge:Cambridge University Press,2005:13
[12]Rickett B J.ARA&A,1990,28:561
[13]Han J L.Tuerbulence,Dynamos,Accretion Disks,Pulsars and Collective Plasma Processes.New York:Springer,2008:99
[14]钱志瀚,李金岭.甚长基线干涉测量技术在深空探测中的应用.北京:中国科学技术出版社,2012:34
[15]Fritz G,Henry R C,Meekins J F,et al.Science,1969,164:709
[16]Deller A T,Tingay S J,Bailes M,et al.PASP,2007,119:318
[17]Brisken W F,Benson J,Goss W M.Ap J,2002,571:906
[18]Chatterjee S,Cordes J M,Vlemmings W H T,et al.Ap J,2004,604:339
[19]Hobbs G B,Edwards R T,Manchester R N.MNRAS,2006,369:655
[20]Hobbs G B,Edwards R T,Manchester R N.MNRAS,2006,372:1549
[21]Guo L,Zheng X W,Zhang B,et al.Science China Physics,Mechanics and Astronomy,2010,53:1559
[22]Wayth R B,Brisken W F,Deller A T,et al.Ap J,2011,735:97