Non-parametric reconstruction of dark energy and cosmic expansion from the Pantheon compilation of type Ia supernovae

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英文篇名：Non-parametric reconstruction of dark energy and cosmic expansion from the Pantheon compilation of type Ia supernovae 作者：林海南 ; 李昕 ; 唐丽 英文作者：Hai-Nan Lin;Xin Li;Li Tang;Department of Physics, Chongqing University; 英文关键词：cosmology;;dark energy;;type Ia supernovae 中文刊名：KNWL 英文刊名：中国物理C 机构：Department of Physics, Chongqing University; 出版日期：2019-07-15 出版单位：Chinese Physics C 年：2019 期：v.43 基金：Supported by the National Natural Science Fund of China(11603005 and 11775038) 语种：英文; 页：KNWL201907014 页数：9 CN：07 ISSN：11-5641/O4 分类号：107-115

摘要

The equation of state(EoS) of dark energy plays an important role in the evolution of the universe and has attracted considerable interest in the recent years. With the progress in observational technique, a precise constraint on the EoS of dark energy can be obtained. In this study, we reconstruct the EoS of dark energy and cosmic expansion using Gaussian processes(GP) from the most up-to-date Pantheon compilation of type Ia supernovae(SNe Ia),which consists of 1048 finely calibrated SNe Ia. The reconstructed EoS of dark energy has a large uncertainty owing to its dependence on the second-order derivative of the construction. Adding the direct measurements of Hubble parameters H(z) as an additional constraint on the first-order derivative can partially reduce the uncertainty; however, it is still not sufficiently precise to distinguish between the evolving and the constant dark energy. Moreover, the results heavily rely on the prior of the Hubble constant H0. The H0 value inferred from SNe+ H(z) without prior is H0= 70.5 ± 0.5 km s~(-1) Mpc~(-1). Moreover, the matter density ?M has a non-negligible effect on the reconstruction of dark energy. Therefore, more accurate determinations on H_0 and ?_M are required to tightly constrain the EoS of dark energy.
        The equation of state(EoS) of dark energy plays an important role in the evolution of the universe and has attracted considerable interest in the recent years. With the progress in observational technique, a precise constraint on the EoS of dark energy can be obtained. In this study, we reconstruct the EoS of dark energy and cosmic expansion using Gaussian processes(GP) from the most up-to-date Pantheon compilation of type Ia supernovae(SNe Ia),which consists of 1048 finely calibrated SNe Ia. The reconstructed EoS of dark energy has a large uncertainty owing to its dependence on the second-order derivative of the construction. Adding the direct measurements of Hubble parameters H(z) as an additional constraint on the first-order derivative can partially reduce the uncertainty; however, it is still not sufficiently precise to distinguish between the evolving and the constant dark energy. Moreover, the results heavily rely on the prior of the Hubble constant H0. The H0 value inferred from SNe+ H(z) without prior is H0= 70.5 ± 0.5 km s~(-1) Mpc~(-1). Moreover, the matter density ?M has a non-negligible effect on the reconstruction of dark energy. Therefore, more accurate determinations on H_0 and ?_M are required to tightly constrain the EoS of dark energy.

引文

1S.Perlmutter,G.Aldering,G.Goldhaber et al,Astrophys.J.,517:565(1999)
    2A.G.Riess,A.V.Filippenko,P.Challis et al,Astron.J.,116:1009(1998)
    3M.Tegmark,M.Strauss,M.Blanton et al,Phys.Rev.D,69:103501(2004)
    4S.Nesseris and L.Perivolaropoulos,Phys.Rev.D,77:023504(2008)
    5P.A.R.Ade et al,[Planck Collaboration],Astron.Astrophys.A.,594:13(2016)
    6N.Aghanim et al,[Planck Collaboration],arXiv:1807.06209(2018)
    7 S.Weinberg,Rev.Mod.Phys.,61:1(1989)
    8I.Zlatev,L.M.Wang,and P.J.Steinhardt,Phys.Rev.Lett.,82:896(1999)
    9M.Chevallier and D.Polarski,Int.J.Mod.Phys.D,10:213(2001)
    10 E.V.Linder,Phys.Rev.Lett.,90:091301(2003)
    11W.Yang,S.Pan,and A.Paliathanasis,Mon.Not.Roy.Astron.Soc.,475:2605(2018)
    12 Y.Y.Xu and X.Zhang,Eur.Phys.J.C,76:88(2016)
    13R.R.Caldwell,R.Dave,and P.J.Steinhardt,Phys.Rev.Lett.,80:1582(1998)
    14 R.R.Caldwell,Phys.Lett.B,545:23(2002)
    15 A.Sen,Journal of High Energy Physics,2002:048(2002)
    16T.Holsclaw,U.Alam,and B.Sanso,Phys.Rev.Lett.,105:241302(2010)
    17 T.Holsclaw,U.Alam,and B.Sanso,Phys.Rev.D,82:103502(2010)
    18T.Holsclaw,U.Alam,and B.Sanso,Phys.Rev.D,84:083501(2011)
    19 M.Seikel,C.Clarkson,and M.Smith,JCAP,1206:036(2012)
    20 M.J.Zhang and J.Q.Xia,JCAP,1612:005(2016)
    21 M.J.Zhang and H.Li,Eur.Phys.J.C,78:460(2018)
    22 Z.Y.Yin and H.Wei,arXiv:1808.00377(2018)
    23A.Aghamousa,J.Hamann,and A.Shafieloo,JCAP,1709:031(2017)
    24J.E.Gonzalez,J.S.Alcaniz,and J.C.Carvalho,JCAP,1604:016(2016)
    25T.Yang,Z.K.Guo,and R.G.Cai,Phys.Rev.D,91:123533(2015)
    26R.G.Cai,Z.K.Guo,and T.Yang,Phys.Rev.D,93:043517(2016)
    27 D.M.Scolnic et al,Astrophys.J.,859:101(2018)
    28 A.G.Riess et al,Astrophys.J.,826:56(2016)
    29 S.Weinberg,(Cosmology,Oxford University Press)(2008)
    30 D.W.Hogg,astro-ph/9905116(1999)
    31J.Guy,P.Astier,and S.Nobili,Astron.Astrophys.,443:781(2005)
    32J.Guy,P.Astier,S.Baumont et al,Astron.Astrophys.,466:11(2007)
    33 R.Tripp,Astron.Astrophys.,331:815(1998)
    34 N.Suzuki et al,Astrophys.J.,746:85(2012)
    35M.Betoule et al,[SDSS Collaboration],Astron.Astrophys.,568:A22(2014)
    36 J.Magana,M.H.Amante,M.A.Garcia-Aspeitia,Mon.Not.Roy.Astron.Soc.,476:1036(2018)