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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(9) : 095101 DOI: 10.1088/1674-1137/42/9/095101

Local probes strongly favor ∧CDM against power-law and Rh=ct universe

  • 1.

      Department of Physics, Chongqing University, Chongqing 401331, China

  • 2.

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

  • 3.

     University of Chinese Academy of Sciences, Beijing 100049, China

  • We constrain three cosmological models-the concordance cold dark matter plus cosmological constant (∧CDM) model, the power-law (PL) model, and the Rh=ct model-using the available local probes, which include the JLA compilation of type-Ia supernovae (SNe Ia), the direct measurement of the Hubble constant (H(z)), and the baryon acoustic oscillations (BAO). For the ∧CDM model, we consider two different cases, i.e. zero and non-zero spatial curvature. We find that by using the JLA alone, the ∧CDM and PL models are indistinguishable, but the Rh=ct model is strongly disfavored. If we combine JLA+H(z), the ∧CDM model is strongly favored over the other two models. The combination of all three datasets supports ∧CDM as the best model. We also use the low-redshift (z<0.2) data to constrain the deceleration parameter using the cosmography method, and find that only the ∧CDM model is consistent with cosmography. However, there is no strong evidence to distinguish between flat and non-flat ∧CDM models by using the local data alone.
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  • References

    [1] S. Perlmutter, G. Aldering, G. Goldhaber et al, Astrophys. J., 517:565 (1999)
    [2] A. G. Riess, A. V. Filippenko, P. Challis et al, Astron. J., 116:1009 (1998)
    [3] C. L. Bennett et al (WMAP Collaboration), Astrophys. J., 192:S16 (2011)
    [4] C. L. Bennett et al (WMAP Collaboration), Astrophys. J., 208:S20 (2013)
    [5] P. A. R. Ade et al (Planck Collaboration), Astron. Astrophys., 571:A16 (2014)
    [6] P. A. R. Ade et al (Planck Collaboration), Astron. Astrophys., 594:A13 (2016)
    [7] S. Weinberg, Rev. Mod. Phys., 61:1 (1989)
    [8] I. Zlatev, L. M. Wang, and P. J. Steinhardt, Phys. Rev. Lett., 82:896 (1999)
    [9] A. G. Riess et al, Astrophys. J., 826:56 (2016)
    [10] F. Melia, The Edge of Infinity:Supermassive Black Holes in the Universe (Cambridge University Press 2003)
    [11] F. Melia, Mon. Not. Roy. Astron. Soc., 382:1917 (2007)
    [12] F. Melia, Astrophys. J., 764:72 (2013)
    [13] J. J. Wei, X. F. Wu, and F. Melia, Astron. J., 149:165 (2015)
    [14] F. Melia, T. M. McClintock, Astron. J., 150:119 (2015)
    [15] J. J. Wei, X. F. Wu, F. Melia, Mon. Not. Roy. Astron. Soc., 463:1144 (2016)
    [16] F. Melia, Mon. Not. Roy. Astron. Soc., 464:1966 (2017)
    [17] M. Bilicki, M. Seikel, Mon. Not. Roy. Astron. Soc., 425:1664 (2012)
    [18] D. L. Shafer, Phys. Rev. D, 91:103516 (2015)
    [19] B. S. Haridasu, V. V. Luković:R. D'Agostino, and N. Vittorio, Astron. Astrophys., 600:L1 (2017)
    [20] A. D. Dolgov, Phys. Rev. D, 55:5881 (1997)
    [21] A. Dolgov, V. Halenka, I. Tkachev, and J. Cosmol. Astropart. Phys., 1410:047 (2014)
    [22] G. Sethi, A. Dev, and D. Jain, Phys. Lett. B, 624:135 (2005)
    [23] Z. H. Zhu, M. Hu, J. S. Alcaniz, and Y. X. Liu, Astron. Astrophys., 483:15 (2008)
    [24] I. Tutusaus, B. Lamine, A. Blanchard et al, Phys. Rev. D, 94:103511 (2016)
    [25] J. T. Nielsen, A. Guffanti, and S. Sarkar, Sci. Rep., 6:35596 (2016)
    [26] I. Tutusaus, B. Lamine, A. Dupays, and A. Blanchard, Astron. Astrophys., 602:A73 (2017)
    [27] D. W. Hogg, astro-ph/9905116
    [28] F. Melia, A. Shevchuk, Mon. Not. Roy. Astron. Soc., 419:2579 (2012)
    [29] P. K. S. Dunsby, O. Luongo, Int. J. Geom. Meth. Mod. Phys., 13:1630002 (2016)
    [30] M. Kowalski et al, Astrophys. J., 686:749 (2008)
    [31] R. Amanullah et al, Astrophys. J., 716:712 (2010)
    [32] N. Suzuki et al, Astrophys. J., 746:85 (2012)
    [33] M. Betoule et al (SDSS Collaboration), Astron. Astrophys., 568:A22 (2014)
    [34] R. Tripp, Astron. Astrophys., 331:815 (1998)
    [35] J. Guy, P. Astier, S. Nobili, N. Regnault, and R. Pain, Astron. Astrophys., 443:781 (2005)
    [36] R. Jimenez, A. Loeb, Astrophys. J., 573:37 (2002)
    [37] D. Stern, R. Jimenez, L. Verde, M. Kamionkowski, S. A. Stanford, and J. Cosmol. Astropart. Phys., 1002:008 (2010)
    [38] M. Moresco et al, J. Cosmol. Astropart. Phys., 1208:006 (2012)
    [39] E. Gaztanaga, A. Cabre, and L. Hui, Mon. Not. Roy. Astron. Soc., 399:1663 (2009)
    [40] C. Blake et al, Mon. Not. Roy. Astron. Soc., 425:405 (2012)
    [41] M. Moresco et al, JCAP, 1605:014 (2016)
    [42] D. J. Eisenstein, W. Hu, Astrophys. J., 496:605 (1998)
    [43] C. Cheng, Q. G. Huang, Sci. China Phys. Mech. Astron., 58:599801 (2015)
    [44] F. Beutler, C. Blake, M. Colless et al, Mon. Not. R. Astron. Soc., 416:3017 (2011)
    [45] L. Anderson et al, Mon. Not. R. Astron. Soc., 441:24 (2014)
    [46] T. Delubac et al (BOSS Collaboration), Astron. Astrophys., 574:A59 (2015)
    [47] E. A. Kazin et al, Mon. Not. Roy. Astron. Soc., 441:3524 (2014)
    [48] H. Akaike, IEEE Trans. Automatic Control, 19:716 (1974)
    [49] G. Schwarz, Ann. Statist., 6:461 (1978)
    [50] H. Jeffreys, The theory of probability (Oxford University Press, Oxford U.K.) (1998)
    [51] A. R. Liddle, Mon. Not. R. Astron. Soc., 377:L74 (2007)
    [52] D. Foreman-Mackey, D. W. Hogg, D. Lang, and J. Goodman, Publ. Astron. Soc. Pac., 125:306 (2013)
    [53] A. G. Riess et al, arXiv:1710.00844 (2017)
    [54] B. P. Abbott, et al (LIGO Scientific and Virgo Collaborations), Phys. Rev. Lett., 119:161101 (2017)
    [55] A. Goldstein et al, Astrophys. J., 848:L14 (2017)
    [56] B. P. Abbott, et al (LIGO Scientific and Virgo and Fermi-GBM and INTEGRAL Collaborations), Astrophys. J., 848:L13 (2017)
    [57] D. A. Coulter et al, Science, 358:1556 (2017)
    [58] B. P. Abbott et al, Nature, 551:85 (2017)

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Hai-Nan Lin, Xin Li and Yu Sang. Local probes strongly favor ∧CDM against power-law and Rh=ct universe[J]. Chinese Physics C, 2018, 42(9): 095101. doi: 10.1088/1674-1137/42/9/095101
Hai-Nan Lin, Xin Li and Yu Sang. Local probes strongly favor ∧CDM against power-law and Rh=ct universe[J]. Chinese Physics C, 2018, 42(9): 095101.  doi: 10.1088/1674-1137/42/9/095101 shu
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Received: 2018-04-08
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    Supported by National Natural Science Fund of China (11603005, 11775038, 11647307, 11675182, 11690022)

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Local probes strongly favor ∧CDM against power-law and Rh=ct universe

    Corresponding author: Hai-Nan Lin,
    Corresponding author: Xin Li,
    Corresponding author: Yu Sang,
  • 1.  Department of Physics, Chongqing University, Chongqing 401331, China
  • 2. Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
  • 3. University of Chinese Academy of Sciences, Beijing 100049, China
  • Received Date: 2018-04-08
  • Available Online: 2018-09-05
Fund Project:  Supported by National Natural Science Fund of China (11603005, 11775038, 11647307, 11675182, 11690022)

Abstract: We constrain three cosmological models-the concordance cold dark matter plus cosmological constant (∧CDM) model, the power-law (PL) model, and the Rh=ct model-using the available local probes, which include the JLA compilation of type-Ia supernovae (SNe Ia), the direct measurement of the Hubble constant (H(z)), and the baryon acoustic oscillations (BAO). For the ∧CDM model, we consider two different cases, i.e. zero and non-zero spatial curvature. We find that by using the JLA alone, the ∧CDM and PL models are indistinguishable, but the Rh=ct model is strongly disfavored. If we combine JLA+H(z), the ∧CDM model is strongly favored over the other two models. The combination of all three datasets supports ∧CDM as the best model. We also use the low-redshift (z<0.2) data to constrain the deceleration parameter using the cosmography method, and find that only the ∧CDM model is consistent with cosmography. However, there is no strong evidence to distinguish between flat and non-flat ∧CDM models by using the local data alone.

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