HR-e)ddlmZddlmZddlmZddlmZddl m Z ddl m Z m Z dd gZd d giZGd de ZGd d e eZdS))expN) Parameter)aszarr)scalar_inv_efuncs)FLRW FlatFLRWMixinw0wzCDM Flatw0wzCDM*scipyceZdZdZeddZeddZdddejzddej zd fd d d fd Z d Z d Z xZ S)r a FLRW cosmology with a variable dark energy equation of state and curvature. The equation for the dark energy equation of state uses the simple form: :math:`w(z) = w_0 + w_z z`. This form is not recommended for z > 1. Parameters ---------- H0 : float or scalar quantity-like ['frequency'] Hubble constant at z = 0. If a float, must be in [km/sec/Mpc]. Om0 : float Omega matter: density of non-relativistic matter in units of the critical density at z=0. Ode0 : float Omega dark energy: density of dark energy in units of the critical density at z=0. w0 : float, optional Dark energy equation of state at z=0. This is pressure/density for dark energy in units where c=1. wz : float, optional Derivative of the dark energy equation of state with respect to z. A cosmological constant has w0=-1.0 and wz=0.0. Tcmb0 : float or scalar quantity-like ['temperature'], optional Temperature of the CMB z=0. If a float, must be in [K]. Default: 0 [K]. Setting this to zero will turn off both photons and neutrinos (even massive ones). Neff : float, optional Effective number of Neutrino species. Default 3.04. m_nu : quantity-like ['energy', 'mass'] or array-like, optional Mass of each neutrino species in [eV] (mass-energy equivalency enabled). If this is a scalar Quantity, then all neutrino species are assumed to have that mass. Otherwise, the mass of each species. The actual number of neutrino species (and hence the number of elements of m_nu if it is not scalar) must be the floor of Neff. Typically this means you should provide three neutrino masses unless you are considering something like a sterile neutrino. Ob0 : float or None, optional Omega baryons: density of baryonic matter in units of the critical density at z=0. If this is set to None (the default), any computation that requires its value will raise an exception. name : str or None (optional, keyword-only) Name for this cosmological object. meta : mapping or None (optional, keyword-only) Metadata for the cosmology, e.g., a reference. Examples -------- >>> from astropy.cosmology import w0wzCDM >>> cosmo = w0wzCDM(H0=70, Om0=0.3, Ode0=0.7, w0=-0.9, wz=0.2) The comoving distance in Mpc at redshift z: >>> z = 0.5 >>> dc = cosmo.comoving_distance(z) z%Dark energy equation of state at z=0.float)doc fvalidatez9Derivative of the dark energy equation of state w.r.t. z.RQ@Nnamemetac  >t||||||| | |  ||_||_|jjdkr8t j|_|j |j |j |j |j f|_dS|jsFt j|_|j |j |j |j|jz|j |j f|_dSt j|_|j |j |j |j|j|j|j|j |j f |_dS)N) H0Om0Ode0Tcmb0Neffm_nuOb0rrr)super__init__w0wz_Tcmb0valuerw0wzcdm_inv_efunc_norel_inv_efunc_scalar_Om0_Ode0_Ok0_w0_wz_inv_efunc_scalar_args _massivenuw0wzcdm_inv_efunc_nomnu_Ogamma0_Onu0w0wzcdm_inv_efunc _neff_per_nu _nmasslessnu _nu_y_list) selfrrrr"r#rrrrrr __class__s >lib/python3.11/site-packages/astropy/cosmology/flrw/w0wzcdm.pyr!zw0wzCDM.__init__\s/    ;  ! !%6%ND "    +D ' ' ' %6%ND "     * +D ' ' '&7%HD "    !! +D ' ' 'c@|j|jt|zzS)aReturns dark energy equation of state at redshift ``z``. Parameters ---------- z : Quantity-like ['redshift'], array-like, or `~numbers.Number` Input redshift. Returns ------- w : ndarray or float The dark energy equation of state. Returns `float` if the input is scalar. Notes ----- The dark energy equation of state is defined as :math:`w(z) = P(z)/\rho(z)`, where :math:`P(z)` is the pressure at redshift z and :math:`\rho(z)` is the density at redshift z, both in units where c=1. Here this is given by :math:`w(z) = w_0 + w_z z`. )r+r,rr6zs r8wz w0wzCDM.ws*x$(VAYY...r9ct|}|dzdd|jz|jz zztd|jz|zzS)aVEvaluates the redshift dependence of the dark energy density. Parameters ---------- z : Quantity-like ['redshift'], array-like, or `~numbers.Number` Input redshift. Returns ------- I : ndarray or float The scaling of the energy density of dark energy with redshift. Returns `float` if the input is scalar. References ---------- .. [1] Linder, E. (2003). Exploring the Expansion History of the Universe. Physics Review Letters, 90(9), 091301. Notes ----- The scaling factor, I, is defined by :math:`\rho(z) = \rho_0 I`, and in this case is given by ([1]_) .. math:: I = \left(1 + z\right)^{3 \left(1 + w_0 - w_z\right)} \exp \left(3 w_z z\right) g?g@)rr+r,rr;s r8de_density_scalezw0wzCDM.de_density_scalesS: 1IICSC$(NTX$=>?# $(NQ C C   r9)__name__ __module__ __qualname____doc__rr"r#uKeVr!r=r? __classcell__r7s@r8r r sBBH >' R R RB  G   B  ACi  14Z > >>>>>>>@///.        r9cXeZdZdZdddejzddejzdfdddfd ZxZS)r a FLRW cosmology with a variable dark energy equation of state and no curvature. The equation for the dark energy equation of state uses the simple form: :math:`w(z) = w_0 + w_z z`. This form is not recommended for z > 1. Parameters ---------- H0 : float or scalar quantity-like ['frequency'] Hubble constant at z = 0. If a float, must be in [km/sec/Mpc]. Om0 : float Omega matter: density of non-relativistic matter in units of the critical density at z=0. w0 : float, optional Dark energy equation of state at z=0. This is pressure/density for dark energy in units where c=1. wz : float, optional Derivative of the dark energy equation of state with respect to z. A cosmological constant has w0=-1.0 and wz=0.0. Tcmb0 : float or scalar quantity-like ['temperature'], optional Temperature of the CMB z=0. If a float, must be in [K]. Default: 0 [K]. Setting this to zero will turn off both photons and neutrinos (even massive ones). Neff : float, optional Effective number of Neutrino species. Default 3.04. m_nu : quantity-like ['energy', 'mass'] or array-like, optional Mass of each neutrino species in [eV] (mass-energy equivalency enabled). If this is a scalar Quantity, then all neutrino species are assumed to have that mass. Otherwise, the mass of each species. The actual number of neutrino species (and hence the number of elements of m_nu if it is not scalar) must be the floor of Neff. Typically this means you should provide three neutrino masses unless you are considering something like a sterile neutrino. Ob0 : float or None, optional Omega baryons: density of baryonic matter in units of the critical density at z=0. If this is set to None (the default), any computation that requires its value will raise an exception. name : str or None (optional, keyword-only) Name for this cosmological object. meta : mapping or None (optional, keyword-only) Metadata for the cosmology, e.g., a reference. Examples -------- >>> from astropy.cosmology import Flatw0wzCDM >>> cosmo = Flatw0wzCDM(H0=70, Om0=0.3, w0=-0.9, wz=0.2) The comoving distance in Mpc at redshift z: >>> cosmo.comoving_distance(0.5) rrrNrc  t||d||||||| |  |jjdkr2tj|_|j|j|j |j f|_ dS|j s@tj |_|j|j|j|jz|j |j f|_ dStj|_|j|j|j|j|j|j|j |j f|_ dS)Nr) rrrr"r#rrrrrrr)r r!r$r%rfw0wzcdm_inv_efunc_norelr'r(r)r+r,r-r.fw0wzcdm_inv_efunc_nomnur0r1fw0wzcdm_inv_efuncr3r4r5) r6rrr"r#rrrrrrr7s r8r!zFlatw0wzCDM.__init__s   ;  ! !%6%OD "+/9dj$(DH*UD ' ' ' %6%OD "    * +D ' ' '&7%ID "   !! +D ' ' 'r9) r@rArBrCrDrErFr!rGrHs@r8r r sz>>H  ACi  14Z 5 55555555555r9)numpyr astropy.unitsunitsrDastropy.cosmology.parameterrastropy.cosmology.utilsrrbaserr __all____doctest_requires__r r r9r8rXs111111******%%%%%%%% m $gY'B B B B B dB B B Jvvvvv-vvvvvr9