scalpy package

Submodules

scalpy.fluids module

class scalpy.fluids.GCG(Om0, As, alpha, h=0.7, Ob0=0.045, Or0=5e-05, ns=0.96, sigma_8=0.8)

Bases: scalpy.fluids.LCDM

A Class to calculate cosmological observables for a model with CDM and dark energy for which equation of state is parametrized as that by GCG $p= -A/rho^{alpha}$: w(z) = -As/(As+(1-As)*(1+z)**(3*(1+alpha))) where ‘z’ is the redshift and As,alpha are model parameters.

parameters are: Om0 : present day density parameter for total matter (baryonic + dark) As and alpha: parameters involved in eqn. of state for GCG (ref()) Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 MPc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 MPc scale

hubble_normalized_z(z)
class scalpy.fluids.LCDM(Om0, h=0.7, Ob0=0.045, Or0=0, ns=0.96, sigma_8=0.8)

Bases: object

A Class to calculate cosmological observables for concordance LCDM model. Equation of state, w = -1

parameters are: Om0 : present day density parameter for total matter (baryonic + dark) Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 MPc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 MPc scale

A0bbks()
A0wh()
DPk_bbks(k, z)

Dimensionless Matter Power Spectra Pk as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be BBKS Ref: Bardeen et. al., Astrophys. J., 304, 15 (1986)

DPk_wh(k, z)

Dimensionless Matter Power Spectra Pk as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be Eisenstein & Hu Ref: Eisenstein and Hu, Astrophys. J., 496, 605 (1998)

D_H()

Hubble distance in units of MPc (David Hogg arxiv: astro-ph/9905116v4)

D_p(a)
D_plus_a(a)
D_plus_z(z)

Normalized solution for the growing mode as a function of redshift

Omega_m_a(a)

Density parameter for matter Omega_m as a function of scale factor ‘a’

Omega_m_z(z)

Density parameter for matter Omega_m as a function of redshift ‘z’

Pk_bbks(k, z)

Matter Power Spectra Pk in units if h^{-3}Mpc^{3} as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be BBKS Ref: Bardeen et. al., Astrophys. J., 304, 15 (1986)

Pk_wh(k, z)

Matter Power Spectra Pk in units if h^{-3}Mpc^{3} as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be Eisenstein & Hu Ref: Eisenstein and Hu, Astrophys. J., 496, 605 (1998)

Wf(k)

Window function

acoustic_length()

It calculates acoustis length scale at decoupling redshift

angular_diameter_distance_z(z)

Angular diameter distance as function of redshift z in units of MPc

cmb_shift_parameter()

CMB Shift parameter at decoupling redshift (see Shafer and Huterer, arxiv:1312.1688v2) Output:

R (shift parameter)
comoving_distance_z(z1)

Line of sight comoving distance as a function of redshift z as described in David Hogg paper in units of MPc

deriv(y, a)
fsigma8z(z)

fsigma_{8} as a function of redshift

growth_rate_a(a)
growth_rate_z(z)

Growth Rate f = D log(Dplus)/ D Log(a) as a function of redshift

hubble_normalized_a(a)

Calculates normalized Hubble parameter h(a) = H(a)/H0 where:

H(a) is the Hubble parameter at redshift z H0 is the current value of Hubble parameter
Input:
a: scale factor of the Universe
Output:
h(a): normalized hubble parameter
hubble_normalized_z(z)

Calculates normalized Hubble parameter h(z) = H(z)/H0 where:

H(z) is the Hubble parameter at redshift z H0 is the current value of Hubble parameter
Input:
z: redshift
Output:
h(z): normalized hubble parameter
hubble_prime_normalized_a(a)

Derivative of dimensionless hubble parameter w.r.t. a

integrand_bbks(k)
integrand_wh(k)
inverse_hubble_normalized_z(z)

Inverse of the normalized hubble parameter: 1/h(z) where h(z) = H(z)/H0 Input:

z: redshift
Output:
1/h(z): inverse of normalized hubble parameter
lookback_time_z(z)

Lookback time as a function of redshift z in units of billion years

luminosity_distance_z(z)

Luminosity distance in as function of redshift z in units of MPc

sol1()
sound_horizon(z)

Gives the sound horizon at redshift z

t_H()

Hubble time in units of Billion years

time_delay_distance(zd, zs)

Time delay distance used in strong lensing cosmography (See Suyu et. al., Astrophys. J. 766, 70, 2013; arxiv:1208.6010) zs = redshift at which the source is placed zd = redshift at which the deflector (or lens) is present

z_decoupling()

Gives the redshit of the decoupling era

z_drag_epoch()

Gives the redshit of baryon drag epoch Eisenstein and Hu; arxiv:astro-ph/9709112

class scalpy.fluids.w0waCDM(Om0, w0, wa, h=0.7, Ob0=0.045, Or0=5e-05, ns=0.96, sigma_8=0.8)

Bases: scalpy.fluids.LCDM

A Class to calculate cosmological observables for a model with CDM and dark energy for which equation of state w is parametrized as: w(a) = w0 + wa*(1-a) where ‘a’ is the scale factor and w0,wa are constants in Taylor expansion of variable equation of state w(a)

parameters are: Om0 : present day density parameter for total matter (baryonic + dark) w0 and wa: coefficients of Taylor expansion of equation of state w(a) near a=1 Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 MPc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 MPc scale

hubble_normalized_z(z)
class scalpy.fluids.w0waCDMzi(Om0, w0, wa, zi, h=0.7, Ob0=0.045, Or0=5e-05, ns=0.96, sigma_8=0.8)

Bases: scalpy.fluids.LCDM

A Class to calculate cosmological observables for a model with CDM and dark energy for which equation of state w is parametrized as: w(a) = w0 + wa*(1-a) where ‘a’ is the scale factor and w0,wa are constants in Taylor expansion of variable equation of state w(a)

parameters are: Om0 : present day density parameter for total matter (baryonic + dark) w0 and wa: coefficients of Taylor expansion of equation of state w(a) near a=1 Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 MPc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 MPc scale

hubble_normalized_z(z)
class scalpy.fluids.wCDM(Om0, w, h=0.7, Ob0=0.045, Or0=5e-05, ns=0.96, sigma_8=0.8)

Bases: scalpy.fluids.LCDM

A Class to calculate cosmological observables for a model with CDM and dark energy for which equation of state w is constant but not equal to -1. See hubble_normalized_z function for details.

parameters are: Om0 : present day density parameter for total matter (baryonic + dark) Ob0 : present day density parameter for baryons (or visible matter) w : equation of state for “dark energy” ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 MPc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 MPc scale

hubble_normalized_z(z)

scalpy.scalar module

class scalpy.scalar.galileonexp(Ophi_i, epsilon_i, li, Orad_i, h=0.7, Ob0=0.045, ns=0.96, sigma_8=0.8)

Bases: scalpy.scalar.galileonpow

A Class to calculate cosmological observables for Galileon field with exponential potential.

parameters are: Ophi_i : initial value (at a = 0.001) of density parameter for Galileon field epsilon_i : initial value (at a = 0.001) for epsilon (see readme.rst) li : initial value (at a = 0.001) for the slope of potential (-V’(phi)/V(phi)) Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 Mpc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 Mpc scale

gal(x, efold)
class scalpy.scalar.galileonpow(Ophi_i, epsilon_i, li, n, Orad_i, h=0.7, Ob0=0.045, ns=0.96, sigma_8=0.8)

Bases: scalpy.scalar.scalarpow

A Class to calculate cosmological observables for Galileon field with exponential potential.

parameters are: Ophi_i : initial value (at a = 0.001) of density parameter for Galileon field epsilon_i : initial value (at a = 0.001) for epsilon (see readme.rst) li : initial value (at a = 0.001) for the slope of potential (-V’(phi)/V(phi)) Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 Mpc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 Mpc scale

Omega_m_n(N)

Density parameter for matter component as a function of log(a) Input:

N: log(a)
Output:
Omega_m_n(z): density parameter for matter component as a function of e-folding

Examples: 1) Calculating Omega_m with scalar field with power law potential V=phi^n: n=1 at log(a) = -2

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_m_n(-2)
  1. Calculating present day density parameter Omega_m with scalar field for exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_m_n(0)
Omega_phi_n(N)

Density parameter for scalar field as a function of log(a) where ‘a’ is the scale factor of the Universe. Input:

N: log(a)
Output:
Omega_phi(N): density parameter for scalar field as a function of e-folding

Examples: 1) Calculating Omega_phi for scalar field with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_phi_n(-2)
  1. Calculating present day density parameter scalar field with exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_phi_n(0)
Omega_r_n(N)

Density parameter for radiation as a function of log(a) Input:

N: log(a)
Output:
Omega_r_n(z): density parameter for radiation component as a function of e-folding

Examples: 1) Calculating Omega_r for radiation component with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_r_n(-2)
  1. Calculating present day density parameter of radiation component with scalar field

and exponential potential

> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_r_n(0)

comoving_distance_n(N)

Line of sight comoving distance as a function of log(a) as described in David Hogg paper in units of Mpc

equation_of_state_n(N)

Equation of state as a function of log(a)

gal(x, efold)
hubble_normalized_n(N)

Dimensionless Hubble constant as a function of N = log(a)

sol()
class scalpy.scalar.scalarexp(Ophi_i, li, Orad_i, h=0.7, Ob0=0.045, ns=0.96, sigma_8=0.8)

Bases: scalpy.scalar.scalarpow

A Class to calculate cosmological observables for quintessence field with exponential potential.

parameters are: Ophi_i : initial value (at a = 0.001) of density parameter for scalar field li : initial value (at a = 0.001) for the slope of potential (-V’(phi)/V(phi)) Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 Mpc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 Mpc scale

f(x, efold)
class scalpy.scalar.scalarpow(Ophi_i, li, n, Orad_i, h=0.7, Ob0=0.045, ns=0.96, sigma_8=0.8)

Bases: object

A Class to calculate cosmological observables for quintessence field with power law potential.

parameters are: Ophi_i : initial value (at a = 0.001) of density parameter for scalar field li : initial value (at a = 0.001) for the slope of potential (-V’(phi)/V(phi)) n : order of power law potential V(phi)=phi**n Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 Mpc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 Mpc scale

A0bbks()
A0wh()
DPk_bbks(k, z)

Dimensionless Matter Power Spectra Pk as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be BBKS Ref: Bardeen et. al., Astrophys. J., 304, 15 (1986)

DPk_wh(k, z)

Dimensionless Matter Power Spectra Pk as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be Eisenstein & Hu (ref(Eisenstein and Hu, Astrophys. J., 496, 605 (1998)))

D_H()

Hubble distance in units of Mpc (David Hogg, arxiv: astro-ph/9905116v4)

D_p(N)
D_plus_n(N)

Normalized solution for the growing mode as a function of efolding

D_plus_z(z)

Normalized solution for the growing mode as a function of redshift

Omega_m_a(a)
Omega_m_n(N)

Density parameter for matter component as a function of log(a) Input:

N: log(a)
Output:
Omega_m_n(z): density parameter for matter component as a function of e-folding

Examples: 1) Calculating Omega_m with scalar field with power law potential V=phi^n: n=1 at log(a) = -2

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_m_n(-2)
  1. Calculating present day density parameter Omega_m with scalar field for exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_m_n(0)
Omega_m_z(z)

Density parameter for matter component as a function of redshift z Input:

z: redshift
Output:
Omega_m_z(z): density parameter for matter component as a function of redshift

Examples: 1) Calculating Omega_m with scalar field with power law potential V=phi^n: n=1 at z=2

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_m_z(2)
  1. Calculating present day density parameter Omega_m with scalar field for exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_m_z(0)
Omega_phi_n(N)

Density parameter for scalar field as a function of log(a) where ‘a’ is the scale factor of the Universe. Input:

N: log(a)
Output:
Omega_phi(N): density parameter for scalar field as a function of e-folding

Examples: 1) Calculating Omega_phi for scalar field with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_phi_n(-2)
  1. Calculating present day density parameter scalar field with exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_phi_n(0)
Omega_phi_z(z)

Density parameter for scalar field as a function of redshift z Input:

z: redshift
Output:
Omega_phi_z(z): density parameter for scalar field as a function of redshift

Examples: 1) Calculating Omega_phi for scalar field with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_phi_z(2)
  1. Calculating present day density parameter scalar field with exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_phi_z(0)
Omega_r_n(N)

Density parameter for radiation as a function of log(a) Input:

N: log(a)
Output:
Omega_r_n(z): density parameter for radiation component as a function of e-folding

Examples: 1) Calculating Omega_r for radiation component with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_r_n(-2)
  1. Calculating present day density parameter of radiation component with scalar field

and exponential potential

> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_r_n(0)

Omega_r_z(z)

Density parameter for radiation as a function of redshift z Input:

z: redshift
Output:
Omega_r_z(z): density parameter for radiation component as a function of redshift

Examples: 1) Calculating Omega_r for scalar field with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).Omega_r_z(2)
  1. Calculating present day density parameter Omega_r with scalar field for exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).Omega_r_z(0)
Pk_bbks(k, z)

Matter Power Spectra Pk in units if h^{-3}Mpc^{3} as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be BBKS Ref: Bardeen et. al., Astrophys. J., 304, 15 (1986)

Pk_wh(k, z)

Matter Power Spectra Pk in units if h^{-3} Mpc^{3} as a function of k in units of [h Mpc^{-1}] and z; Transfer function is taken to be Eisenstein & Hu (ref(Eisenstein and Hu, Astrophys. J., 496, 605 (1998)))

Wf(k)
acoustic_length()

It calculates acoustis length scale at decoupling redshift

angular_diameter_distance_z(z)

Angular diameter distance as function of redshift z in units of Mpc

cmb_shift_parameter()

CMB Shift parameter

comoving_distance_n(N)

Line of sight comoving distance as a function of log(a) as described in David Hogg paper in units of Mpc

comoving_distance_z(z)

Line of sight comoving distance as a function of redshift z as described in David Hogg paper in units of Mpc

deriv(y1, N)
equation_of_state_n(N)

Equation of state as a function of log(a) Input:

N: log(a)
Output:
w(N): equation of state for scalar field component as a function of e-folding N= log(a)

Examples: 1) Calculating w(N) with power law potential V=phi^n with n=1 at e-folding = -2

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).equation_of_state_n(-2)
  1. Calculating present day equation of state of scalar field with exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).equation_of_state_n(0)
equation_of_state_z(z)

Equation of state as a function of z Input:

z: redshift
Output:
w(z): equation of state for scalar field component as a function of redshift

Examples: 1) Calculating w(z) with power law potential V=phi^n with n=1 at redshift z = 2

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).equation_of_state_z(2)
  1. Calculating present day equation of state of scalar field with exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).equation_of_state_z(0)
f(x, efold)
fsigma8z(z)

fsigma_{8} as a function of redshift

growth_rate_n(N)
growth_rate_z(z)

Growth Rate f = D log(Dplus)/ D Log(a) as a function of redshift

hubble_normalized_a(a)
hubble_normalized_n(N)

Dimensionless Hubble constant as a function of N = log(a)

hubble_normalized_z(z)

Dimensionless Hubble parameter as a function of redshift z

hubble_prime_normalized(N)

Derivative of dimensionless hubble constant w.r.t. log(a)

integrand_bbks(k)
integrand_wh(k)
inverse_hubble_normalized_z(z)

Inverse of the normalized hubble parameter: 1/h(z) where h(z) = H(z)/H0 Input:

z: redshift
Output:
1/h(z): inverse of normalized hubble parameter
lookback_time_n(N)

Lookback time as a function of log(a) in units of billion years

lookback_time_z(z)

Lookback time as a function of redshift z in units of billion years

luminosity_distance_z(z)

Luminosity distance in as function of redshift z in units of Mpc

n1 = array([-7.00397414, -6.99696315, -6.98995217, -6.98294118, -6.9759302 , -6.96891921, -6.96190823, -6.95489724, -6.94788626, -6.94087527, -6.93386429, -6.9268533 , -6.91984232, -6.91283133, -6.90582035, -6.89880936, -6.89179837, -6.88478739, -6.8777764 , -6.87076542, -6.86375443, -6.85674345, -6.84973246, -6.84272148, -6.83571049, -6.82869951, -6.82168852, -6.81467754, -6.80766655, -6.80065557, -6.79364458, -6.7866336 , -6.77962261, -6.77261163, -6.76560064, -6.75858966, -6.75157867, -6.74456769, -6.7375567 , -6.73054572, -6.72353473, -6.71652375, -6.70951276, -6.70250178, -6.69549079, -6.68847981, -6.68146882, -6.67445784, -6.66744685, -6.66043587, -6.65342488, -6.6464139 , -6.63940291, -6.63239193, -6.62538094, -6.61836996, -6.61135897, -6.60434798, -6.597337 , -6.59032601, -6.58331503, -6.57630404, -6.56929306, -6.56228207, -6.55527109, -6.5482601 , -6.54124912, -6.53423813, -6.52722715, -6.52021616, -6.51320518, -6.50619419, -6.49918321, -6.49217222, -6.48516124, -6.47815025, -6.47113927, -6.46412828, -6.4571173 , -6.45010631, -6.44309533, -6.43608434, -6.42907336, -6.42206237, -6.41505139, -6.4080404 , -6.40102942, -6.39401843, -6.38700745, -6.37999646, -6.37298548, -6.36597449, -6.35896351, -6.35195252, -6.34494154, -6.33793055, -6.33091957, -6.32390858, -6.31689759, -6.30988661, -6.30287562, -6.29586464, -6.28885365, -6.28184267, -6.27483168, -6.2678207 , -6.26080971, -6.25379873, -6.24678774, -6.23977676, -6.23276577, -6.22575479, -6.2187438 , -6.21173282, -6.20472183, -6.19771085, -6.19069986, -6.18368888, -6.17667789, -6.16966691, -6.16265592, -6.15564494, -6.14863395, -6.14162297, -6.13461198, -6.127601 , -6.12059001, -6.11357903, -6.10656804, -6.09955706, -6.09254607, -6.08553509, -6.0785241 , -6.07151312, -6.06450213, -6.05749115, -6.05048016, -6.04346918, -6.03645819, -6.0294472 , -6.02243622, -6.01542523, -6.00841425, -6.00140326, -5.99439228, -5.98738129, -5.98037031, -5.97335932, -5.96634834, -5.95933735, -5.95232637, -5.94531538, -5.9383044 , -5.93129341, -5.92428243, -5.91727144, -5.91026046, -5.90324947, -5.89623849, -5.8892275 , -5.88221652, -5.87520553, -5.86819455, -5.86118356, -5.85417258, -5.84716159, -5.84015061, -5.83313962, -5.82612864, -5.81911765, -5.81210667, -5.80509568, -5.7980847 , -5.79107371, -5.78406273, -5.77705174, -5.77004076, -5.76302977, -5.75601879, -5.7490078 , -5.74199681, -5.73498583, -5.72797484, -5.72096386, -5.71395287, -5.70694189, -5.6999309 , -5.69291992, -5.68590893, -5.67889795, -5.67188696, -5.66487598, -5.65786499, -5.65085401, -5.64384302, -5.63683204, -5.62982105, -5.62281007, -5.61579908, -5.6087881 , -5.60177711, -5.59476613, -5.58775514, -5.58074416, -5.57373317, -5.56672219, -5.5597112 , -5.55270022, -5.54568923, -5.53867825, -5.53166726, -5.52465628, -5.51764529, -5.51063431, -5.50362332, -5.49661234, -5.48960135, -5.48259037, -5.47557938, -5.4685684 , -5.46155741, -5.45454642, -5.44753544, -5.44052445, -5.43351347, -5.42650248, -5.4194915 , -5.41248051, -5.40546953, -5.39845854, 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sol()
sol1()
sound_horizon(z)

Sound horizon as a function of redshift ‘z’

sound_horizon1(z)
t_H()

Hubble time in units of Billion years

time_delay_distance(zd, zs)

Time delay distance used in strong lensing cosmography (See Suyu et. al., Astrophys. J. 766, 70, 2013; arxiv:1208.6010) Input:

zd = redshift at which the deflector (or lens) is present zs = redshift at which the source is placed
Output:
Time_delay_distance
z_decoupling()

redshift of decoupling or reionization Input:

None
Output:
z_decoupling

Example: 1) Calculating z_decoupling with power law potential V=phi^n with n=1

> import scalpy.scalar as s1 > s1.scalarpow(2.,0.2,1.,0.1).z_decoupling()
  1. Calculating z_decoupling in scalar field model with exponential potential
> import scalpy.scalar as s1 > s1.scalarexp(2.,0.2,0.1).z_decoupling()
z_drag_epoch()

Gives the redshit of baryon drag epoch Eisenstein and Hu; arxiv:astro-ph/9709112 Input:

None
Output:
z_drag_epoch
class scalpy.scalar.tachyonexp(Ophi_i, li, Orad_i, h=0.7, Ob0=0.045, ns=0.96, sigma_8=0.8)

Bases: scalpy.scalar.tachyonpow

A Class to calculate cosmological observables for tachyon field with power law potential.

parameters are: Ophi_i : initial value (at a = 0.001) of density parameter for tachyon field li : initial value (at a = 0.001) for the slope of potential (-V’(phi)/V(phi)) Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 Mpc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 Mpc scale

f(x, efold)
class scalpy.scalar.tachyonpow(Ophi_i, li, n, Orad_i, h=0.7, Ob0=0.045, ns=0.96, sigma_8=0.8)

Bases: scalpy.scalar.scalarpow

A Class to calculate cosmological observables for tachyon field with power law potential.

parameters are: Ophi_i : initial value (at a = 0.001) of density parameter for tachyon field li : initial value (at a = 0.001) for the slope of potential (-V’(phi)/V(phi)) n : order of power law potential V(phi)=phi**n Ob0 : present day density parameter for baryons (or visible matter) ns : spectral index for primordial power spectrum h : dimensionless parameter related to Hubble constant H0 = 100*h km s^-1 Mpc^-1 sigma_8 : r.m.s. mass fluctuation on 8h^-1 Mpc scale

f(x, efold)

scalpy.transfer_func module

scalpy.transfer_func.C1(x, k, om0, h)
scalpy.transfer_func.G(x)
scalpy.transfer_func.Rd(om0, ob0, h)
scalpy.transfer_func.Req(om0, ob0, h)
scalpy.transfer_func.T0(k, x, y, om0, ob0, h)
scalpy.transfer_func.Tb(k, x1, y1, om0, ob0, h)
scalpy.transfer_func.Tbbks(k, om0, ob0, h)
scalpy.transfer_func.Tc(k, x, y, om0, ob0, h)
scalpy.transfer_func.Twh(k, om0, ob0, h)
scalpy.transfer_func.a1(om0, h)
scalpy.transfer_func.a2(om0, h)
scalpy.transfer_func.alphab(om0, ob0, h)
scalpy.transfer_func.alphac(om0, ob0, h)
scalpy.transfer_func.b1(om0, h)
scalpy.transfer_func.b2(om0, h)
scalpy.transfer_func.bb1(om0, h)
scalpy.transfer_func.bb2(om0, h)
scalpy.transfer_func.betab(om0, ob0, h)
scalpy.transfer_func.betac(om0, ob0, h)
scalpy.transfer_func.betanode(om0, h)
scalpy.transfer_func.f(k, om0, ob0, h)
scalpy.transfer_func.gm(om0, ob0, h)
scalpy.transfer_func.keq(om0, h)
scalpy.transfer_func.ksilk(om0, ob0, h)
scalpy.transfer_func.q(k, om0, h)
scalpy.transfer_func.q1(k, om0, ob0, h)
scalpy.transfer_func.s(om0, ob0, h)
scalpy.transfer_func.s1(k, om0, ob0, h)
scalpy.transfer_func.zd(om0, ob0, h)
scalpy.transfer_func.zeq(om0, h)

Module contents