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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2018, Vol. 42> Issue(11) : 115103 DOI: 10.1088/1674-1137/42/11/115103

Searching for a possible dipole anisotropy in acceleration scale with 147 rotationally supported galaxies

  • 1.

     Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China

  • 2.

     School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China

  • 3.

      Department of Physics, Chongqing University, Chongqing 401331, China

  • We report a possible dipole anisotropy in acceleration scale g† with 147 rotationally supported galaxies in the local Universe. It is found that a monopole and dipole correction for the radial acceleration relation can better describe the SPARC data set. The monopole term is negligible but the dipole magnitude is significant. It is also found that the dipole correction is mostly induced by anisotropy in the acceleration scale. The magnitude of the ĝ†-dipole reaches 0.25±0.04, and its direction is aligned to (l,b)=(171.30°±7.18°, -15.41°±4.87°), which is very close to the maximum anisotropy direction from the hemisphere comparison method. Furthermore, a robust check shows that the dipole anisotropy could not be reproduced by an isotropic mock data set. However, it is still premature to claim that the Universe is anisotropic, due to the small data samples and uncertainty in the current observations.
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  • References

    [1] S. Weinberg, Cosmology, (Oxford, UK:Oxford University Press, 2008)
    [2] C. L. Bennett et al (WMAP), Astrophys. J. Suppl., 208:20 (2013)
    [3] G. Hinshaw et al (WMAP), Astrophys. J. Suppl., 208:19 (2013)
    [4] P. A. R. Ade et al (Planck), Astron. Astrophys., 571:A16 (2014)
    [5] P. A. R. Ade et al (Planck), Astron. Astrophys., 594:A13 (2016)
    [6] D. Hutsemekers, R. Cabanac, H. Lamy, and D. Sluse, Astron. Astrophys., 441:915 (2005)
    [7] A. Kashlinsky, F. Atrio-Barandela, H. Ebeling, A. Edge, and D. Kocevski, Astrophys. J., 712:L81 (2010)
    [8] H. A. Feldman, R. Watkins, and M. J. Hudson, Mon. Not. Roy. Astron. Soc., 407:2328 (2010)
    [9] J. K. Webb, J. A. King, M. T. Murphy, V. V. Flambaum, R. F. Carswell, and M. B. Bainbridge, Phys. Rev. Lett., 107:191101 (2011)
    [10] J. A. King, J. K. Webb, M. T. Murphy, V. V. Flambaum, R. F. Carswell, M. B. Bainbridge, M. R. Wilczynska, and F. E. Koch, Mon. Not. Roy. Astron. Soc., 422:3370 (2012)
    [11] A. Mariano and L. Perivolaropoulos, Phys. Rev. D, 86:083517 (2012)
    [12] Z. Chang, X. Li, H.-N. Lin, and S. Wang, Eur. Phys. J. C, 74:2821 (2014)
    [13] Z. Chang and H.-N. Lin, Mon. Not. Roy. Astron. Soc., 446:2952 (2015)
    [14] H.-N. Lin, X. Li, and Z. Chang, Mon. Not. Roy. Astron. Soc., 460:617 (2016)
    [15] V. C. Rubin, W. K. Ford, Jr., and N. Thonnard, Astrophys. J., 225:L107 (1978)
    [16] A. Bosma, Astron. J., 86:1825 (1981)
    [17] A. Tan et al (PandaX-Ⅱ), Phys. Rev. Lett., 117:121303 (2016)
    [18] E. Aprile et al (XENON100), Phys. Rev. D, 94:122001 (2016)
    [19] M. Milgrom, Astrophys. J., 270:365 (1983)
    [20] M. Milgrom, New Astron. Rev., 46:741 (2002)
    [21] M. Milgrom, Mon. Not. Roy. Astron. Soc., 437:2531 (2014)
    [22] K. G. Begeman, A. H. Broeils, and R. H. Sanders, Mon. Not. Roy. Astron. Soc., 249:523 (1991)
    [23] R. A. Swaters, R. H. Sanders, and S. S. McGaugh, Astrophys. J., 718:380 (2010)
    [24] Z. Chang, M.-H. Li, X. Li, H.-N. Lin, and S. Wang, Eur. Phys. J. C, 73:2447 (2013)
    [25] M. Milgrom, in Proceedings, 2nd International Heidelberg Conference on Dark matter in astrophysics and particle physics (DARK 1998):Heidelberg, Germany, July 20-25, 1998 (1998) p. 443-457
    [26] Y. Zhou, Z.-C. Zhao, and Z. Chang, Astrophys. J., 847:86 (2017)
    [27] F. Lelli, S. S. McGaugh, and J. M. Schombert, Astron. J., 152:157 (2016)
    [28] S. S. McGaugh, F. Lelli, and J. M. Schombert, Phys. Rev. Lett., 117:201101 (2016)
    [29] A. Begum and J. N. Chengalur, Astron. Astrophys., 424:509 (2005)
    [30] W. J. G. de Blok, S. S. McGaugh, and J. M. van der Hulst, Mon. Not. Roy. Astron. Soc., 283:18 (1996)
    [31] M. Milgrom, (2016), arXiv:1609.06642
    [32] P. T. Boggs, R. H. Byrd, and R. B. Schnabel, SIAM Journal on Scientific and Statistical Computing, 8:1052 (1987)
    [33] H. Akaike, IEEE Transactions on Automatic Control, 19:716 (1974)
    [34] G. Schwarz, Annals of Statistics, 6:461 (1978)
    [35] A. R. Liddle, Mon. Not. Roy. Astron. Soc., 377:L74 (2007)
    [36] F. Arevalo, A. Cid, and J. Moya, Eur. Phys. J. C, 77:565 (2017)
    [37] H.-N. Lin, X. Li, and Y. Sang, (2017), arXiv:1711.05025
    [38] D. Foreman-Mackey, D. W. Hogg, D. Lang, and J. Goodman, Publications of the Astronomical Society of the Pacific, 125:306 (2013)
    [39] W. Zhao, P.-X. Wu, and Y. Zhang, Int. J. Mod. Phys. D, 22:1350060 (2013)
    [40] Z. Chang, S. Wang, and X. Li, Eur. Phys. J. C, 72:1838 (2012)
    [41] Z. Chang, M.-H. Li, and S. Wang, Phys. Lett. B, 723:257 (2013)
    [42] X. Li, H.-N. Lin, S. Wang, and Z. Chang, Eur. Phys. J. C, 75:181 (2015)
    [43] J. M. Schombert and S. McGaugh, PASA, 31:e011 (2014)
    [44] P.-F. Li, F. Lelli, S. McGaugh, and J. Schormbert, Astron. Astrophys., 615:A3 (2018)

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Zhe Chang, Hai-Nan Lin, Zhi-Chao Zhao and Yong Zhou. Searching for a possible dipole anisotropy in acceleration scale with 147 rotationally supported galaxies[J]. Chinese Physics C, 2018, 42(11): 115103. doi: 10.1088/1674-1137/42/11/115103
Zhe Chang, Hai-Nan Lin, Zhi-Chao Zhao and Yong Zhou. Searching for a possible dipole anisotropy in acceleration scale with 147 rotationally supported galaxies[J]. Chinese Physics C, 2018, 42(11): 115103.  doi: 10.1088/1674-1137/42/11/115103 shu
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Received: 2018-07-27
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    Supported by National Natural Science Foundation of China (11675182, 11690022, 11603005)

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Searching for a possible dipole anisotropy in acceleration scale with 147 rotationally supported galaxies

  • 1. Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
  • 2. School of Physical Sciences, University of Chinese Academy of Sciences, Beijing 100049, China
  • 3.  Department of Physics, Chongqing University, Chongqing 401331, China
  • Received Date: 2018-07-27
  • Available Online: 2018-11-05
Fund Project:  Supported by National Natural Science Foundation of China (11675182, 11690022, 11603005)

Abstract: We report a possible dipole anisotropy in acceleration scale g† with 147 rotationally supported galaxies in the local Universe. It is found that a monopole and dipole correction for the radial acceleration relation can better describe the SPARC data set. The monopole term is negligible but the dipole magnitude is significant. It is also found that the dipole correction is mostly induced by anisotropy in the acceleration scale. The magnitude of the ĝ†-dipole reaches 0.25±0.04, and its direction is aligned to (l,b)=(171.30°±7.18°, -15.41°±4.87°), which is very close to the maximum anisotropy direction from the hemisphere comparison method. Furthermore, a robust check shows that the dipole anisotropy could not be reproduced by an isotropic mock data set. However, it is still premature to claim that the Universe is anisotropic, due to the small data samples and uncertainty in the current observations.

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