1. Introduction

IJAA

International Journal of Astronomy and Astrophysics

2161-4717

Scientific Research Publishing

10.4236/ijaa.2019.93017

IJAA-94843

Articles

Physics&Mathematics

The Distance Modulus in Dark Energy and Cardassian Cosmologies via the Hypergeometric Function

Lorenzo

Zaninetti

₁^*

Physics Department, via P. Giuria 1, Turin, Italy

08072019

090323124611, June 20191, September 2019 4, September 2019

2014

This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/

The presence of the dark energy allows both the acceleration and the expansion of the universe. In the case of a constant equation of state for dark energy we derived an analytical solution for the Hubble radius in terms of the hypergeometric function. An approximate Taylor expansion of order seven is derived for both the constant and the variable equation of state for dark energy. In the case of the Cardassian cosmology, we also derived an analytical solution for the Hubble radius in terms of the hypergeometric function. The astronomical samples of the distance modulus for Supernova (SN) of type Ia allows the derivation of the involved cosmological in the case of constant equation of state, variable equation of state and Cardassian cosmology.

Cosmology Observational Cosmology Distances Redshifts Radial Velocities Spatial Distribution of Galaxies Magnitudes and Colors Luminosities

1. Introduction

The name dark energy started to be used by [1] in order to explain both the expansion and both the acceleration of the universe. In a few years the dark energy was widely used as a cosmological model to be tested. Many review papers have been written; we select among others a general review by [2] and a theoretical review by [3] . The term wCDM has been introduced to classify the case of constant equation of state and we will use in the following wzCDM to classify the variable equation of state. The Cardassian cosmology started with [4] and was introduced in order to model both the expansion and the acceleration of the universe, the name from a humanoid race in Star Trek. As an example [5] derived the cosmological parameters for the original Cardassian expansion and the modified polytropic Cardassian expansion. The cosmological theories can be tested on the samples of Supernova (SN) of type Ia. The first sample to be used to derive the cosmological parameters contained 7 SNs, see [6] , the second one contained 34 SNs, see [7] and the third one contained 42 SNs, see [8] . The above historical samples allowed to derive the cosmological parameters for the expanding and accelerating universe. At the moment of writing the astronomical research is focused on value of the distance modulus versus the redshift: the Union 2.1 compilation contains 580 SNs, see [9] , and the joint light-curve analysis (JLA) contains 740 SNs, see [10] . The above observations can be done up to a limited value in redshift z ≈ 1.7 , we, therefore, speak of evaluation of the distance modulus at low redshift. This limited range can be extended up z ≈ 8 , the high redshift region, analyzing the Gamma-Ray Burst (GRB) and, as an example, [11] has derived the distance modulus for 59 calibrated high-redshift GRBs, the so-called “Hymnium” GRBs sample. This paper reviews in Section 2.1. The ΛCDM cosmology evaluates the basic integral of wCDM cosmology in Section 3, introduces a Taylor expansion for the basic integral of wzCDM cosmology in Section 4 and analyzes the Cardassian model in Section 5. The parameters which characterize the three cosmologies are derived via the Levenberg-Marquardt method in Section 6.

2. Preliminaries

This section reviews the ΛCDM cosmology and the adopted statistics.

2.1. The Standard Cosmology

In ΛCDM cosmology the Hubble distance D H is defined as

D H ≡ c H 0 . (1)

The first parameter is Ω M

Ω M = 8 π G ρ 0 3 H 0 2 , (2)

where G is the Newtonian gravitational constant, H 0 is the Hubble constant and ρ 0 is the mass density at the present time. The second parameter is Ω Λ

Ω Λ ≡ Λ c 2 3 H 0 2 , (3)

where Λ is the cosmological constant, see [12] . These two parameters are connected with the curvature Ω K by

Ω M + Ω Λ + Ω K = 1. (4)

The comoving distance, D C , is

D C = D H ∫ 0 z d z ′ E ( z ′ ) (5)

where E ( z ) is the “Hubble function”

E ( z ) = Ω M ( 1 + z ) 3 + Ω K ( 1 + z ) 2 + Ω Λ . (6)

In the case of Ω K , we have the flat case.

2.2. The Statistics

The adopted statistical parameters are the percent error, δ , between theoretical value and approximated value, the merit function χ 2 evaluated as

χ 2 = ∑ i = 1 N [ y i , t h e o − y i , o b s σ i ] 2 (7)

where y i , o b s and σ i represent the observed value and its error at position i and y i , t h e o the theoretical value at position i, the reduced merit function χ r e d 2 , the Akaike information criterion (AIC), the number of degrees of freedom N F = n − k where n is the number of bins and k is the number of parameters and the goodness of the fit as expressed by the probability Q.

3. Constant Equation of State

In dark matter cosmology, wCDM, the Hubble radius is

d H ( z ; Ω M , w , Ω D E ) = 1 ( 1 + z ) 3 Ω M + Ω D E ( 1 + z ) 3 + 3 w , (8)

where w parametrizes the dark energy and is constant, see Equation (3.4) in [13] or Equation (18) in [14] for the luminosity distance.

In flat cosmology

Ω M + Ω D E = 1, (9)

and the Hubble radius becomes

d H ( z ; Ω M , w ) = 1 ( 1 + z ) 3 Ω M + ( 1 − Ω M ) ( 1 + z ) 3 + 3 w . (10)

The indefinite integral in the variable z of the above Hubble radius, I z , is

I z ( z ; Ω M , w ) = ∫ d H ( z ; Ω M , w ) d z . (11)

3.1. The Analytical Solution

In order to solve the indefinite integral we perform a change of variable 1 + z = t 1 / 3

I z ( t ; Ω M , w ) = 1 3 ∫ 1 − t ( ( − 1 + Ω M ) t w − Ω M ) t 2 / 3 d t . (12)

The indefinite integral is

I z ( t ; Ω M , w ) = − 2 F 2 1 ( 1 2 , − 1 6 w − 1 ; 1 − 1 6 w − 1 ; − t w − ( 1 − Ω M ) Ω M ) Ω M t 6 , (13)

where F 2 1 ( a , b ; c ; z ) is the regularized hypergeometric function, see Appendix B. This dependence of the above integral upon the hypergeometric function has been recognized but not developed by [15] .

We now return to the variable z, the redshift, and the indefinite integral becomes

I z ( z ; Ω M , w ) = − 2 F 2 1 ( 1 2 , − 1 6 w − 1 ; 1 − 1 6 w − 1 ; − ( − z 3 + 3 z 2 + 3 z + 1 ) w ( 1 − Ω M ) − Ω M ) Ω M z 3 + 3 z 2 + 3 z + 1 6 . (14)

We denote by F ( z ; Ω M , w ) the definite integral

F ( z ; Ω M , w ) = I z ( z = z ; Ω M , w ) − I z ( z = 0 ; Ω M , w ) . (15)

3.2. The Taylor Expansion

We evaluate the integrand of the integral (11) with a first series expansion, T I about z = 0 , denoted by I and a second series expansion, T I I , about z = 1 , denoted by I I . The order of expansion for the two series is 7. The integration of T I in z is denoted by I z I ,7 and gives

I z I ,7 ( z ; Ω M , w ) = ∑ i = 1 i = 7 c I , i z i (16)

and the coefficients, c I , i , are reported in Appendix A. The integral, I z I I ,7 of the second Taylor expansion about z = 1 , T I I is complicated and we limit ourselves to order 2, I z I I ,2 , see Appendix A. The two definite integrals, F I ,7 ( z ; Ω M , w ) and F I I ,7 ( z ; Ω M , w ) are

F I ,7 ( z ; Ω M , w ) = I z I ,7 ( z = z ; Ω M , w ) − I z I ,7 ( z = 0 ; Ω M , w ) , (17)

and

F I I ,7 ( z ; Ω M , w ) = I z I I ,7 ( z = z ; Ω M , w ) − I z I I ,7 ( z = 0 ; Ω M , w ) . (18)

The percent error, δ , between the analytical integral F and the two approximations, F I ,7 and F I I ,7 is evaluated as

δ I = | 1 − F I , 7 F | × 100 (19)

δ I I = | 1 − F I I , 7 F | × 100. (20)

On inserting the astrophysical parameters as reported in Table 1 we have δ I = δ I I at z ≈ 0.58 , see Figure 1.

The above value in z will, therefore, be the boundary between region I and region II for the Taylor approximation of the definite integral

F 7 ( z ; Ω M , w ) = { F I I ,7 ( z ; Ω M , w ) , 0.58 ≤ z ≤ 1.4 F I ,7 ( z ; Ω M , w ) , 0 < z < 0.58 (21)

Table 1 Numerical values from the Union 2.1 compilation of χ 2 , χ r e d 2 and Q, where k stands for the number of parameters

Cosmology	SNs	k	parameters	χ 2	χ r e d 2	Q
ΛCDM	580	3	H 0 = 69.81 ; Ω M = 0.239 ; Ω Λ = 0.651	562.61	0.975	0.658
wCDM Hypergeometric solution	580	3	H 0 = ( 70.02 ± 0.35 ) ; Ω M = ( 0.277 ± 0.025 ) ; w = ( − 1.003 ± 0.05 )	562.21	0.974	0.662
wCDM Taylor approximation	580	3	H 0 = ( 70.02 ± 0.47 ) ; Ω M = ( 0.282 ± 0.07 ) ; w = ( − 1.01 ± 0.2 )	562.21	0.974	0.662
wzCDM Taylor approximation	580	4	H 0 = ( 70.08 ± 0.31 ) ; Ω M = ( 0.284 ± 0.01 ) ; w 0 = ( − 1.03 ± 0.031 ) ; w 1 = ( 0.1 ± 0.018 ) ;	562.21	0.976	0.651
Cardassian	58k0	3	H 0 = ( 70.15 ± 0.38 ) ; Ω M = ( 0.305 ± 0.019 ) ; n = ( − 0.081 ± 0.01 )	562.35	0.974	0.661

4. Variable Equation of State

The dark energy as function of the redshift is assumed to be

w ( z ) = w 0 + w 1 z 1 + z , (22)

where w 0 and w 1 are two parameters to be fixed by the fit. The Hubble radius in wzCDM cosmology is

d H ( z ; Ω M , w 0 , w 1 ) = 1 ( 1 + z ) 3 Ω M + ( 1 − Ω M ) ( 1 + z ) 3 w 0 + 3 w 1 + 3 e − 3 w 1 z 1 + z (23)

which is the same as Equation (20) in [14] . The above integral does not yet have an analytical expression and we evaluate the integrand with a first series expansion about z = 0 and a second series expansion about z = 1 . Also here the order of the two series expansion is 7. The integration in z is denoted by I w z I ,7 and gives

I w z I ,7 ( z ; Ω M , w 0 , w 1 ) = ∑ i = 1 i = 7 c I , i z i (24)

and the first five coefficients, c I , i , are reported in Appendix C. The integral, I w z I I ,7 of the second Taylor expansion about z = 1 is complicated and we limit ourselves to order 2, I w z I I ,2 , see Appendix C. The two definite integrals, F w z I ,7 ( z ; Ω M , w 0 , w 1 ) and F w z I I ,7 ( z ; Ω M , w 0 , w 1 ) are

F w z I ,7 ( z ; Ω M , w 0 , w 1 ) = I w z I ,7 ( z = z ; Ω M , w 0 , w 1 ) − I w z I ,7 ( z = 0 ; Ω M , w 0 , w 1 ) , (25)

and

F w z I I ,7 ( z ; Ω M , w 0 , w 1 ) = I w z I I ,7 ( z = z ; Ω M , w 0 , w 1 ) − I w z I I ,7 ( z = 0 ; Ω M , w 0 , w 1 ) . (26)

Finally the definite integral, F w z , is

F w z 7 ( z ; Ω M , w 0 , w 1 ) = { F w z I I ,7 ( z ; Ω M , w 0 , w 1 ) , 0.58 ≤ z ≤ 1.4 F w z I ,7 ( z ; Ω M , w 0 , w 1 ) , 0 < z < 0.58 (27)

The above definite integral can also be evaluated in a numerical way,

F w z n u m ( z ; Ω M , w 0 , w 1 ) .

5. Cardassian Cosmology

In flat Cardassian cosmology the Hubble radius is

d H ( z ; Ω M , w , n ) = 1 ( 1 + z ) 3 Ω M + ( 1 − Ω M ) ( 1 + z ) 3 n , (28)

where n is a variable parameter, n = 0 means ΛCDM cosmology, see Equation (17) in [14] . The indefinite integral in the variable z of the above Hubble radius, I z , is

I z ( z ; Ω M , n ) = ∫ d H ( z ; Ω M , n ) d z . (29)

Also here in order to solve the indefinite integral we perform a change of variable 1 + z = t 1 / 3

I z ( t ; Ω M , n ) = 1 3 ∫ 1 − t n Ω M + Ω M t + t n t 2 / 3 d t . (30)

The indefinite integral is

I z ( t ; Ω M , n ) = − 2 F 2 1 ( 1 / 2 , − ( 6 n − 6 ) − 1 ; 6 n − 7 6 n − 6 ; t n − 1 ( Ω M − 1 ) Ω M ) Ω M t 6 , (31)

where F 2 1 ( a , b ; c ; z ) is the regularized hypergeometric function. We now return to the original variable z as function of z which is

I z ( z ; Ω M , n ) = − 2 F 2 1 ( 1 / 2 , − ( 6 n − 6 ) − 1 ; 6 n − 7 6 n − 6 ; ( ( 1 + z ) 3 ) n − 1 ( Ω M − 1 ) Ω M ) Ω M ( 1 + z ) 3 6 . (32)

We denote by F c ( z ; Ω M , n ) the definite integral

F c ( z ; Ω M , n ) = I z ( z = z ; Ω M , n ) − I z ( z = 0 ; Ω M , n ) . (33)

6. The Distance Modulus

The luminosity distance, d L , for wCDM cosmology in the case of the analytical solution is

d L ( z ; c , H 0 , Ω M , w ) = c H 0 ( 1 + z ) F ( z ; Ω M , w ) , (34)

where F ( z ; Ω M , w ) is given by Equation (15) and in the case of the Taylor approximation is

d L,7 ( z ; c , H 0 , Ω M , w ) = c H 0 ( 1 + z ) F 7 ( z ; Ω M , w ) , (35)

where F 7 ( z ; Ω M , w ) is given by Equation (21). The distance modulus in the case of the analytical solution for wCDM is

( m − M ) = 25 + 5 log 10 ( d L ( z ; c , H 0 , Ω M , w ) ) , (36)

and in the case of the Taylor approximation

( m − M ) 7 = 25 + 5 log 10 ( d L,7 ( z ; c , H 0 , Ω M , w ) ) . (37)

In the case of variable equation of state, wzCDM, the numerical luminosity distance is

d L , n u m ( z ; c , H 0 , Ω M , w 0 , w 1 ) = c H 0 ( 1 + z ) F w z n u m ( z ; Ω M , w 0 , w 1 ) , (38)

where F w z n u m ( z ; Ω M , w 0 , w 1 ) is the definite numerical integral and the Taylor approximation for the luminosity distance is

d L,7 ( z ; c , H 0 , Ω M , w 0 , w 1 ) = c H 0 ( 1 + z ) F w z 7 ( z ; Ω M , w 0 , w 1 ) , (39)

where F w z 7 ( z ; Ω M , w 0 , w 1 ) is given by Equation (27). In wzCDM, the numerical distance modulus is

( m − M ) n u m = 25 + 5 log 10 ( d L, n u m ( z ; c , H 0 , Ω M , w 0 , w 1 ) ) , (40)

and the Taylor approximated distance modulus is

( m − M ) 7 = 25 + 5 log 10 ( d L,7 ( z ; c , H 0 , Ω M , w 0 , w 1 ) ) . (41)

In the case of Cardassian cosmology the luminosity distance is

d L ( z ; c , H 0 , Ω M , n ) = c H 0 ( 1 + z ) F c ( z ; Ω M , n ) , (42)

where F c ( z ; Ω M , n ) is given by Equation (33) and the distance modulus is

( m − M ) = 25 + 5 log 10 ( d L ( z ; c , H 0 , Ω M , n ) ) . (43)

The cosmological parameters unknown are three, H 0 , Ω M and w, in the case of wCDM and four, H 0 , Ω M , w 0 and w 1 , in the case of wzCDM. In flat Cardassian cosmology the number of parameters is three, H 0 , Ω M and n. In the presence of a given sample for the distance modulus, we can map the chi-square as given by Formula (7), see Figure 2 in the case of wCDM with hypergeometric solution. The above cosmological parameters are obtained by a fit of the astronomical data for the distance modulus of SNs via the Levenberg-Marquardt method (subroutine MRQMIN in [16] ) which minimizes the chi-square as given by Formula (7). Table 1 presents the above cosmological parameters for the Union 2.1 compilation of SNs and Figure 3 reports the best fit. As a practical example of the utility of the cosmological parameters determination, we report the distance modulus in an explicit form for the Union 2.1 compilation in wCDM.

( m − M ) = 5 + 5 1 ln ( 10 ) × ln ( 4281.52 ( 1 + z ) × ( − 3.8 F 2 1 ( 0.1661, 1 2 ; 1.1661 ; − 2.6101 ( z 3 + 3 z 2 + 3 z + 1 ) − 1.003 ) z 3 + 3 z 2 + 3 z + 1 6 + 3.4146 ) ) (44)

when 0 < z < 1.4 ,

And in flat Cardassian cosmology

( m − M ) = 1 ln ( 10 ) 25 ln ( 10 ) + 5 ln ( − 4273.59 ( 1 + z ) ( 3.62142 ( z 3 + 3 z 2 + 3 z + 1 ) − 0.16666 × F 2 1 ( 0.15417, 1 / 2 ; 1.1541 ; − 2.2786 ( z 3 + 3 z 2 + 3 z + 1 ) − 1.081 ) − 3.304 ) ) (45)

when 0 < z < 1.4 .

Table 2 reports the cosmological parameters for the JLA compilation and Figure 4 the connected fit.

The presence of the “Hymnium” GRBs sample allows to calibrate the distance modulus in the high redshift region (see Table 3 and Figure 5).

The extension of the Hubble diagram to the GRBs, as an example, has been implemented in [11] [17] [18] [19] [20] .

Table 2 Numerical values for the JLA compilation of χ 2 , χ r e d 2 and Q, where k stands for the number of parameters

Cosmology	SNs	k	parameters	χ 2	χ r e d 2	Q
ΛCDM	740	3	H 0 = 69.39 ; Ω M = 0.18 ; Ω Λ = 0.537	625.74	0.849	0.99
wCDM Hypergeometric solution	740	3	H 0 = ( 69.71 ± 0.5 ) ; Ω M = ( 0.293 ± 0.021 ) ; w = ( − 0.996 ± 0.08 )	627.908	0.851	0.998
wCDM Taylor approximation	740	4	H 0 = ( 69.99 ± 0.29 ) ; Ω M = ( 0.133 ± 0.13 ) ; w = ( − 0.709 ± 0.18 )	625.69	0.848	0.998
wzCDM Taylor approximation	740	4	H 0 = ( 69.99 ± 0.29 ) ; Ω M = ( 0.3 ± 0.009 ) ; w 0 = ( − 1.05 ± 0.027 ) ; w 1 = ( 0.097 ± 0.01 ) ;	628.76	0.854	0.998
Cardassian	740	3	H 0 = ( 70.036 ± 0.44 ) ; Ω M = ( 0.301 ± 0.019 ) ; n = ( − 0.055 ± 0.0045 )	628.73	0.863	0.999

Table 3 Numerical values from the Union 2.1 compilation + the “Hymnium” GRBs sample of χ 2 , χ r e d 2 and Q, where k stands for the number of parameters

Cosmology	SNs	k	parameters	χ 2	χ r e d 2	Q
ΛCDM	639	3	H 0 = 69.80 ; Ω M = 0.239 ; Ω Λ = 0.651	586.08	0.921	0.922
wCDM Hypergeometric solution	639	3	H 0 = ( 70.12 ± 0.4 ) ; Ω M = ( 0.294 ± 0.024 ) ; w = ( − 1.04 ± 0.04 )	585.42	0.92	0.924
wzCDM numerical integration	639	4	H 0 = ( 70 ± 0.32 ) ; Ω M = ( 0.3 ± 0.011 ) ; w 0 = ( − 1.05 ± 0.033 ) ; w 1 = ( 0.1 ± 0.01 ) ;	585.59	0.922	0.92
Cardassian	639	3	H 0 = ( 70.10 ± 0.42 ) ; Ω M = ( 0.299 ± 0.019 ) ; n = ( − 0.063 ± 0.0095 )	585.43	0.92	0.924

7. Conclusions

Constant equation of state

In the case of wCDM cosmology, we found a new analytical expression for the Hubble distance in terms of the hypergeometric function, see Equation (13). As a consequence an analytical expression for the luminosity distance and the distance modulus is derived. Two approximate Taylor expansions for the Hubble distance about z = 0 and z = 1 of order 7 are also derived. The derivation of the value of w, Ω M and H 0 , here considered as a parameter to be found, is given for the Union 2.1 compilation, the JLA compilation and the Union 2.1 compilation plus the “Hymnium” GRBs sample, see Tables 1-3. As an example, in the case of the Union 2.1 compilation, we have derived H 0 = ( 70.02 ± 0.35 ) , Ω M = ( 0.277 ± 0.025 ) and w = ( − 1.003 ± 0.05 ) .

Variable equation of state

In the case of wzCDM cosmology the Hubble distance, Equation (23) is evaluated numerically and with a Taylor expansion of order 7, see Equation (24). The four parameters w 0 , w 1 , Ω M and H 0 are reported in Tables 1-3. As an example, in the case of the Union 2.1 compilation, we have found H 0 = ( 70.08 ± 0.31 ) , Ω M = ( 0.284 ± 0.01 ) , w 0 = ( − 1.03 ± 0.031 ) , and w 1 = ( 0.1 ± 0.018 ) .

High redshift

The inclusion of the “Hymnium” GRBs sample allows to extend the calibration of the distance modulus up to z = 8 (see Table 3). As an example, the Union 2.1 compilation + the “Hymnium” GRBs sample gives H 0 = ( 70 ± 0.32 ) , Ω M = ( 0.3 ± 0.011 ) , w 0 = ( − 1.05 ± 0.033 ) , and w 1 = ( 0.1 ± 0.01 ) .

Cardassian cosmology

A new solution for the Hubble radius for Cardassian cosmology is presented in terms of the hypergeometric function, see Equation (reficardz). As an example, in the case of the Union 2.1 compilation, we have derived H 0 = ( 70.15 ± 0.38 ) , Ω M = ( 0.305 ± 0.019 ) and n = ( − 0.081 ± 0.01 ) .

Conflicts of Interest

The author declares no conflicts of interest regarding the publication of this paper.

Cite this paper

Zaninetti, L. (2019) The Distance Modulus in Dark Energy and Cardassian Cosmologies via the Hypergeometric Function. International Journal of Astronomy and Astrophysics, 9, 231-246. https://doi.org/10.4236/ijaa.2019.93017

AppendixA. Taylor Expansion When W Is Constant

The coefficients of the Taylor expansion of I z I ,7 ( z ; Ω M , w ) about z = 0

c I ,1 = 1, (A.1)

c I ,2 = 3 / 4 w Ω M − 3 / 4 w − 3 / 4 , (A.2)

c I ,3 = − 3 / 2 Ω M w 2 − w Ω M + 3 / 8 w 2 + w + 5 / 8 + 9 Ω M 2 w 2 8 , (A.3)

c I ,4 = − 71 w 64 − 9 w 3 64 − 35 64 − 45 w 2 64 + 45 Ω M w 2 16 − 135 Ω M 2 w 2 64 − 243 Ω M 2 w 3 64 + 117 Ω M w 3 64 + 135 Ω M 3 w 3 64 + 71 w Ω M 64 , (A.4)

c I ,5 = 93 w 80 + 63 128 + 27 w 3 80 + 27 w 4 640 + 309 w 2 320 − 309 Ω M w 2 80 + 927 Ω M 2 w 2 320 + 729 Ω M 2 w 3 80 − 351 Ω M w 3 80 − 81 Ω M 3 w 3 16 + 2349 Ω M 2 w 4 320 − 27 Ω M w 4 16 − 81 Ω M 3 w 4 8 + 567 Ω M 4 w 4 128 − 93 w Ω M 80 , (A.5)

c I ,6 = − 3043 w 2560 − 231 512 − 27 w 5 2560 − 141 w 3 256 − 63 w 4 512 − 14175 Ω M 4 w 5 512 + 5103 Ω M 5 w 5 512 − 301 w 2 256 + 301 Ω M w 2 64 − 903 Ω M 2 w 2 256 − 3807 Ω M 2 w 3 256 + 1833 Ω M w 3 256 + 2115 Ω M 3 w 3 256 − 5481 Ω M 2 w 4 256 + 315 Ω M w 4 64 + 945 Ω M 3 w 4 32 − 6615 Ω M 4 w 4 512 − 2673 Ω M 2 w 5 256 + 3267 Ω M w 5 2560 + 6885 Ω M 3 w 5 256 + 3043 w Ω M 2560 , (A.6)

c I ,7 = 2689 w 2240 + 81 w 6 35840 + 81 w 5 2240 + 171 w 3 224 + 1665 w 4 7168 + 48259 w 2 35840 + 429 1024 + 95985 Ω M 4 w 6 1024 − 19683 Ω M 5 w 6 256 + 24057 Ω M 6 w 6 1024 + 61479 Ω M 2 w 6 5120 − 1053 Ω M w 6 1280 − 23085 Ω M 3 w 6 448 + 6075 Ω M 4 w 5 64 − 2187 Ω M 5 w 5 64 + 8019 Ω M 2 w 5 224 − 9801 Ω M w 5 2240 − 20655 Ω M 3 w 5 224 + 144855 Ω M 2 w 4 3584

− 8325 Ω M w 4 896 − 24975 Ω M 3 w 4 448 + 24975 Ω M 4 w 4 1024 + 4617 Ω M 2 w 3 224 − 2223 Ω M w 3 224 − 2565 Ω M 3 w 3 224 − 48259 Ω M w 2 8960 + 144777 Ω M 2 w 2 35840 − 2689 w Ω M 2240 . (A.7)

The integral of the Taylor expansion of order 2 about z = 1 is

I z I I ,2 = N D , (A.8)

where

N = ( 3 × 8 w Ω M w z − 6 × 8 w w Ω M + 3 × 8 w Ω M z − 3 w z 8 w − 14 × 8 w Ω M + 6 w 8 w − 3 z 8 w − 3 Ω M z + 14 × 8 w + 14 Ω M ) z (A.9)

and

D = ( − 2 3 + 3 w Ω M + 2 3 + 3 w + 8 Ω M ) 3 / 2 . (A.10)

B. The Hypergeometric Function

The regularized hypergeometric function, F 2 1 ( a , b ; c ; z ) , as defined by the Gauss series, is

F 2 1 ( a , b ; c ; z ) = ∑ s = 0 ∞ ( a ) s ( b ) s ( c ) s s ! z s = 1 + a b c z + a ( a + 1 ) b ( b + 1 ) c ( c + 1 ) 2 ! z 2 + ⋯ = Γ ( c ) Γ ( a ) Γ ( b ) ∑ s = 0 ∞ Γ ( a + s ) Γ ( b + s ) Γ ( c + s ) s ! z s (B.1)

where z = x + i y , ( a ) s is the Pochhammer symbol

( a ) s = a ( a + 1 ) ⋯ ( a + s − 1 ) , (B.2)

Γ ( z ) is the Gamma function defined as

Γ ( z ) = ∫ 0 ∞ e − t t z − 1 d t , (B.3)

z is a complex variable defined on the disk | z | < 1 that should not be confused with the redshift, see [21] [22] [23] [24] [25] . The following relationship

F 2 1 ( a , b ; c ; x ) = ( 1 − x ) − a F 2 1 ( a , c − b ; c ; x x − 1 ) (B.4)

connect the the hypergeometric function with x in (−1, 1) to one with x in ( − ∞ , 1 2 ) , see more details in [26] .

C. Taylor Expansion When W Is Variable

The coefficients of the Taylor expansion of I w z I ,7 ( z ; Ω M , w 0 , w 1 ) about z = 0

c I ,1 = 1, (C.1)

c I ,2 = 3 4 w 0 Ω M − 3 4 w 0 − 3 4 , (C.2)

c I ,3 = 5 / 8 + w 0 − 1 / 4 w 1 + 1 / 4 w 1 Ω M − w 0 Ω M + 3 / 8 w 0 2 − 3 / 2 Ω M w 0 2 + 9 Ω M 2 w 0 2 8 , (C.3)

c I ,4 = − 35 64 − 71 w 0 64 + 17 w 1 32 − 17 w 1 Ω M 32 + 71 w 0 Ω M 64 − 45 w 0 2 64 + 9 w 0 w 1 32 + 45 Ω M w 0 2 16 − 135 Ω M 2 w 0 2 64 − 243 Ω M 2 w 0 3 64 + 117 Ω M w 0 3 64 + 135 Ω M 3 w 0 3 64 − 9 w 0 3 64 − 9 Ω M w 0 w 1 8 + 27 Ω M 2 w 0 w 1 32 , (C.4)

c I ,5 = 27 w 0 3 80 + 63 128 − 9 w 1 2 Ω M 40 + 2349 Ω M 2 w 0 4 320 − 27 Ω M w 0 4 16 + 27 w 1 2 Ω M 2 160 − 81 Ω M 3 w 0 4 8 + 567 Ω M 4 w 0 3 128 − 27 w 0 2 w 1 160 + 309 w 0 2 320 − 3 4 w 0 w 1 + 729 Ω M 2 w 0 3 80 − 351 Ω M w 0 3 80 − 81 Ω M 3 w 0 3 16 + 93 w 0 80 − 129 w 1 160 + 9 w 1 2 160 + 27 w 0 4 640 + 351 Ω M w 0 2 w 1 160 + 129 w 1 Ω M 160 − 309 Ω M w 0 2 80 + 927 Ω M 2 w 0 2 320 − 93 w 0 Ω M 80 + 81 Ω M 3 w 0 2 w 1 32 − 729 Ω M 2 w 0 2 w 1 160 − 9 4 Ω M 2 w 0 w 1 + 3 Ω M w 0 w 1 . (C.5)

The integral of the Taylor expansion of order 2 about z = 1 in the case wzLCDM cosmology

I w z I I ,2 = N w z D w z , (C.6)

where

N w z = e 3 4 w 1 ( 6 × 2 1 / 2 + 3 w 0 + 3 w 1 Ω M z w 0 + 3 × 2 1 / 2 + 3 w 0 + 3 w 1 Ω M z w 1 − 6 e 3 / 2 w 1 Ω M 2 z + 6 × 2 1 / 2 + 3 w 0 + 3 w 1 Ω M z − 12 × 2 1 / 2 + 3 w 0 + 3 w 1 w 0 Ω M − 6 × 2 1 / 2 + 3 w 0 + 3 w 1 Ω M w 1 − 6 × 2 1 / 2 + 3 w 0 + 3 w 1 z w 0 − 3 × 2 1 / 2 + 3 w 0 + 3 w 1 z w 1 + 28 e 3 / 2 w 1 Ω M 2 − 28 × 2 1 / 2 + 3 w 0 + 3 w 1 Ω M − 6 × 2 1 / 2 + 3 w 0 + 3 w 1 z + 12 × 2 1 / 2 + 3 w 0 + 3 w 1 w 0 + 6 × 2 1 / 2 + 3 w 0 + 3 w 1 w 1 + 28 × 2 1 / 2 + 3 w 0 + 3 w 1 ) z (C.7)

and

D w z = 64 ( − Ω M 2 3 w 0 + 3 w 1 + 2 3 w 0 + 3 w 1 + Ω M e 3 / 2 w 1 ) 3 / 2 . (C.8)

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