logo

More info
  • ReceivedDec 6, 2018
  • AcceptedDec 27, 2018
  • PublishedMar 19, 2019

Abstract

There is no abstract available for this article.


Acknowledgment

This work was supported by the National Key R&D Program of China (Grant No. 2017YFA0402600), the State Key Development Program for Basic Research (Grant No. 2015CB857100), and the Open Project Program of the Key Laboratory of FAST, NAOC, Chinese Academy of Sciences. Lei Qian was supported in part by the Youth Innovation Promotion Association of CAS (Id. 2018075). ZhiChen Pan was supported by the National Natural Science Foundation of China (Grant No. 11703047) and the CAS “Light of West China" Program. YouLing Yue was supported by the CAS “Light of West China” Program. WeiWei Zhu was supported by the Chinese Academy of Sciences Pioneer Hundred Talents Program, the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDB23000000), and the National Natural Science Foundation of China (Grant Nos. 11690024, 11743002, and 11873067). The Parkes radio telescope is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO.


References

[1] P. Jiang, Y.L. Yue, H.Q. Gan, R. Yao, H. Li, G.F. Pan, J.H. Sun, D.J. Yu, H.F. Liu, N.Y. Tang, L. Qian, J.G. Lu, J. Yan, B. Peng, S.X. Zhang, Q.M. Wang, Q. Li, D. Li (FAST Project), Sci. China-Phys. Mech. Astron. 2019(5), in press. Google Scholar

[2] Nan R., Li D., Jin C., Wang Q., Zhu L., Zhu W., Zhang H., Yue Y., Qian L.. Int. J. Mod. Phys. D, 2011, 20: 989 CrossRef ADS arXiv Google Scholar

[3] Clifton T. R., Lyne A. G., Jones A. W., McKenna J., Ashworth M.. Mon. Not. R. Astron. Soc., 1992, 254: 177 CrossRef ADS Google Scholar

[4] Manchester R. N., Lyne A. G., Camilo F., Bell J. F., Kaspi V. M., D'Amico N., McKay N. P. F., Crawford F., Stairs I. H., Possenti A., Kramer M., Sheppard D. C.. Mon. Not. R. Astron. Soc., 2001, 328: 17 CrossRef ADS Google Scholar

[5] Yunes N., Siemens X.. Y. Nicolás. Google Scholar

[6] Deng X. P., Hobbs G., You X. P., Li M. T., Keith M. J., Shannon R. M., Coles W., Manchester R. N., Zheng J. H., Yu X. Z., Gao D., Wu X., Chen D.. Adv. Space Res., 2013, 52: 1602 CrossRef ADS arXiv Google Scholar

[7] D. Li, P. Wang, L. Qian, M. Krv co, P. Jiang, Y.L. Yue, C.J. Jin, Y. Zhu, Z.C. Pan, R.D. Nan, A. Dunning, IEEE Microwave Magazine 19, 112 (2018). Google Scholar

[8] Hotan A. W., van Straten W., Manchester R. N.. Publ. Astron. Soc. Aust, 2004, 21: 302 CrossRef ADS Google Scholar

[9] S. Ransom, New search techniques for binary pulsars, PhD Thesis, Harvard University, Cambridge, Massachusetts (2001). Google Scholar

[10] Faulkner A. J., Stairs I. H., Kramer M., Lyne A. G., Hobbs G., Possenti A., Lorimer D. R., Manchester R. N., McLaughlin M. A., D'Amico N., Camilo F., Burgay M.. Mon. Not. R. Astron. Soc., 2004, 355: 147 CrossRef ADS Google Scholar

[11] Zhu W. W., Berndsen A., Madsen E. C., Tan M., Stairs I. H., Brazier A., Lazarus P., Lynch R., Scholz P., Stovall K., Ransom S. M., Banaszak S., Biwer C. M., Cohen S., Dartez L. P., Flanigan J., Lunsford G., Martinez J. G., Mata A., Rohr M., Walker A., Allen B., Bhat N. D. R., Bogdanov S., Camilo F., Chatterjee S., Cordes J. M., Crawford F., Deneva J. S., Desvignes G., Ferdman R. D., Freire P. C. C., Hessels J. W. T., Jenet F. A., Kaplan D. L., Kaspi V. M., Knispel B., Lee K. J., van Leeuwen J., Lyne A. G., McLaughlin M. A., Siemens X., Spitler L. G., Venkataraman A.. Astrophys. J., 2014, 781: 117 CrossRef ADS arXiv Google Scholar

  • Figure 1

    (Color online) The folded pulse profile (top left), intensity (gray-scale) of the pulse as a function of pulse phase and integration time (bottom left), intensity as a function of pulse phase and observing frequency (top middle), a measure of the signal-to-noise of the pulse profile as a function of dispersion measure (bottom middle) of PSR J1900-0134 (note that as this is the discovery plot we indicate the pulsar's original name of PSR J1859-01). The right-hand plots show small-scale searches to identify the pulse period and the period derivative that leads to the folded pulse profile with the highest signal-to-noise ratio.

  • Table 1   FAST specifications
    Specifications Value
    Declination range $-$14.4$^\circ$-65.6$^\circ$
    System temperature $T_{\rm~sys}$ (without the 60-70
    contribution from sky $T_{\rm~sky}$) (K)
    Frequency range (ultra-wide band receiver) (MHz) 270-1620
    Number of polarization 2
    Sampling time ($\mu$s) 200
  • Table 2   Parameters of PSR J1900-0134 from the timing observation of the Parkes telescope
    Properties Value
    Right ascension, RA (J2000) 19:00:26.02(7)
    Declination, Dec (J2000) $-$01:34:38(2)
    Spin period, $P$ (s) 1.8323313839(15)
    Spin period derivative, $\dot{P}$ $3.040(8)\times10^{-14}$
    Timing epoch (MJD) 58007
    Dispersion measure, DM ($\text{pc}\,\text{cm}^{-3}$) 179(2)
    Data span (MJD) 58008-58395
    Number of TOAs 103
    RMS residual ($\mu$s) 4246

Copyright 2020 Science China Press Co., Ltd. 《中国科学》杂志社有限责任公司 版权所有

京ICP备18024590号-1       京公网安备11010102003388号