import numpy as np
from scipy.interpolate import interp1d
from ..pyutils import _check_array_params
from ..background import growth_factor
from .. import ccllib as lib


def translate_IA_norm(cosmo, z, a1=1.0, a1delta=None, a2=None,
                      Om_m2_for_c2=False, Om_m_fid=0.3):
    """
    Function to convert from a_ia values to c_ia values,
    using the standard convention of Blazek 2019 or the variant used
    by the Dark Energy Survey analysis.

    Args:
        cosmo (:class:`~pyccl.core.Cosmology`): cosmology object.
        z (float or array_like): z value(s) where amplitude is evaluated
        a1 (float or array_like): IA a1 at input z values. Defaults to 1.0
        a1delta (float or array_like): IA a1delta at input z values.
            Defaults to None.
        a2 (float or array_like): IA a2 at input z values.
            Defaults to None.
        Om_m2_for_c2 (bool): True to use the Blazek 2019 convention of
            Om_m^2 scaling. Defaults to False
        Om_m_fid (float): Value for Blazek 2019 scaling. Defaults to 0.3.

    Returns:
        c1 (float or array_like): IA c1 at input z values
        c1delta (float or array_like): IA c1delta at input z values
        c2 (float or array_like): IA c2 at input z values
    """

    def check_input_array(a, name):
        if a is None:
            return

        if np.ndim(a) > 1:
            raise ValueError(name +
                             " should be a scalar or 1D")

        if np.ndim(a) == 1:
            if len(a) != len(z):
                raise ValueError("Both z and " + name +
                                 " should have the same size")

    if np.ndim(z) > 1:
        raise ValueError("z should be a scalar or 1D")
    check_input_array(a1, 'a1')
    check_input_array(a2, 'a2')
    check_input_array(a1delta, 'a1delta')

    Om_m = cosmo['Omega_m']
    rho_crit = lib.cvar.constants.RHO_CRITICAL
    c1 = c1delta = c2 = None
    gz = growth_factor(cosmo, 1./(1+z))

    if a1 is not None:
        c1 = -1*a1*5e-14*rho_crit*Om_m/gz

    if a1delta is not None:
        c1delta = -1*a1delta*5e-14*rho_crit*Om_m/gz

    if a2 is not None:
        if Om_m2_for_c2:  # Blazek2019 convention
            c2 = a2*5*5e-14*rho_crit*Om_m**2/(Om_m_fid*gz**2)
        else:  # DES convention
            c2 = a2*5*5e-14*rho_crit*Om_m/(gz**2)

    return c1, c1delta, c2


class PTTracer(object):
    """PTTracers contain the information necessary to describe the
    perturbative, non-linear inhomogeneities associated with
    different physical quantities.

    In essence their main function is to store a set of redshift-
    dependent functions (e.g. perturbation theory biases) needed
    in a perturbation theory framework to provide N-point
    correlations.
    """
    def __init__(self):
        self.biases = {}
        self.type = None
        pass

    def get_bias(self, bias_name, z):
        """Get the value of one of the bias functions at a given
        redshift.

        Args:
            bias_name (str): name of the bias function to return.
            z (float or array_like): redshift.

        Returns:
            float or array_like: bias value at the input redshifts.
        """
        if bias_name not in self.biases:
            raise KeyError("Bias %s not included in this tracer" % bias_name)
        return self.biases[bias_name](z)

    def _get_bias_function(self, b):
        # If None, assume it's zero
        if b is None:
            b = 0

        # If it's a scalar, then assume it's a constant function
        if np.ndim(b) == 0:
            def _const(z):
                if np.ndim(z) == 0:
                    return b
                else:
                    return b * np.ones_like(z)

            return _const
        else:  # Otherwise interpolate
            z, b = _check_array_params(b)
            return interp1d(z, b, bounds_error=False,
                            fill_value=b[-1])


class PTMatterTracer(PTTracer):
    """:class:`PTTracer` representing matter fluctuations.
    """
    def __init__(self):
        self.biases = {}
        self.type = 'M'


class PTNumberCountsTracer(PTTracer):
    """:class:`PTTracer` representing number count fluctuations.
    This is described by 1st and 2nd-order biases and
    a tidal field bias. These are provided as floating
    point numbers or tuples of (reshift,bias) arrays.
    If a number is provided, a constant bias is assumed.
    If `None`, a bias of zero is assumed.

    Args:
        b1 (float or tuple of arrays): a single number or a
            tuple of arrays (z, b(z)) giving the first-order
            bias.
        b2 (float or tuple of arrays): as above for the
            second-order bias.
        bs (float or tuple of arrays): as above for the
            tidal bias.
        b3nl (float or tuple of arrays): as above for the
            third-order bias.
        bk2 (float or tuple of arrays): as above for the
            non-local bias.
    """
    def __init__(self, b1, b2=None, bs=None, b3nl=None, bk2=None):
        self.biases = {}
        self.type = 'NC'

        # Initialize b1
        self.biases['b1'] = self._get_bias_function(b1)
        # Initialize b2
        self.biases['b2'] = self._get_bias_function(b2)
        # Initialize bs
        self.biases['bs'] = self._get_bias_function(bs)
        # Initialize b3nl
        self.biases['b3nl'] = self._get_bias_function(b3nl)
        # Initialize bk2
        self.biases['bk2'] = self._get_bias_function(bk2)

    @property
    def b1(self):
        """Internal first-order bias function.
        """
        return self.biases['b1']

    @property
    def b2(self):
        """Internal second-order bias function.
        """
        return self.biases['b2']

    @property
    def bs(self):
        """Internal tidal bias function.
        """
        return self.biases['bs']

    @property
    def b3nl(self):
        """Internal third-order bias function.
        """
        return self.biases['b3nl']

    @property
    def bk2(self):
        """Internal non-local bias function.
        """
        return self.biases['bk2']


class PTIntrinsicAlignmentTracer(PTTracer):
    """:class:`PTTracer` representing intrinsic alignments.
    This is described by 1st and 2nd-order alignment biases
    and an overdensity bias. These are provided as floating
    point numbers or tuples of (reshift,bias) arrays.
    If a number is provided, a constant bias is assumed.
    If `None`, a bias of zero is assumed.

    Args:
        c1 (float or tuple of arrays): a single number or a
            tuple of arrays (z, c1(z)) giving the first-order
            alignment bias.
        c2 (float or tuple of arrays): as above for the
            second-order alignment bias.
        cdelta (float or tuple of arrays): as above for the
            overdensity bias.
    """
    def __init__(self, c1, c2=None, cdelta=None):

        self.biases = {}
        self.type = 'IA'

        # Initialize c1
        self.biases['c1'] = self._get_bias_function(c1)
        # Initialize c2
        self.biases['c2'] = self._get_bias_function(c2)
        # Initialize cdelta
        self.biases['cdelta'] = self._get_bias_function(cdelta)

    @property
    def c1(self):
        """Internal first-order bias function.
        """
        return self.biases['c1']

    @property
    def c2(self):
        """Internal second-order bias function.
        """
        return self.biases['c2']

    @property
    def cdelta(self):
        """Internal overdensity bias function.
        """
        return self.biases['cdelta']

import numpy as np
from scipy.interpolate import interp1d
from ..pyutils import _check_array_params
from ..background import growth_factor
from .. import ccllib as lib


def translate_IA_norm(cosmo, z, a1=1.0, a1delta=None, a2=None,
                      Om_m2_for_c2=False, Om_m_fid=0.3):
    """
    Function to convert from a_ia values to c_ia values,
    using the standard convention of Blazek 2019 or the variant used
    by the Dark Energy Survey analysis.

    Args:
        cosmo (:class:`~pyccl.core.Cosmology`): cosmology object.
        z (float or array_like): z value(s) where amplitude is evaluated
        a1 (float or array_like): IA a1 at input z values. Defaults to 1.0
        a1delta (float or array_like): IA a1delta at input z values.
            Defaults to None.
        a2 (float or array_like): IA a2 at input z values.
            Defaults to None.
        Om_m2_for_c2 (bool): True to use the Blazek 2019 convention of
            Om_m^2 scaling. Defaults to False
        Om_m_fid (float): Value for Blazek 2019 scaling. Defaults to 0.3.

    Returns:
        c1 (float or array_like): IA c1 at input z values
        c1delta (float or array_like): IA c1delta at input z values
        c2 (float or array_like): IA c2 at input z values
    """

    def check_input_array(a, name):
        if a is None:
            return

        if np.ndim(a) > 1:
            raise ValueError(name +
                             " should be a scalar or 1D")

        if np.ndim(a) == 1:
            if len(a) != len(z):
                raise ValueError("Both z and " + name +
                                 " should have the same size")

    if np.ndim(z) > 1:
        raise ValueError("z should be a scalar or 1D")
    check_input_array(a1, 'a1')
    check_input_array(a2, 'a2')
    check_input_array(a1delta, 'a1delta')

    Om_m = cosmo['Omega_m']
    rho_crit = lib.cvar.constants.RHO_CRITICAL
    c1 = c1delta = c2 = None
    gz = growth_factor(cosmo, 1./(1+z))

    if a1 is not None:
        c1 = -1*a1*5e-14*rho_crit*Om_m/gz

    if a1delta is not None:
        c1delta = -1*a1delta*5e-14*rho_crit*Om_m/gz

    if a2 is not None:
        if Om_m2_for_c2:  # Blazek2019 convention
            c2 = a2*5*5e-14*rho_crit*Om_m**2/(Om_m_fid*gz**2)
        else:  # DES convention
            c2 = a2*5*5e-14*rho_crit*Om_m/(gz**2)

    return c1, c1delta, c2


class PTTracer(object):
    """PTTracers contain the information necessary to describe the
    perturbative, non-linear inhomogeneities associated with
    different physical quantities.

    In essence their main function is to store a set of redshift-
    dependent functions (e.g. perturbation theory biases) needed
    in a perturbation theory framework to provide N-point
    correlations.
    """
    def __init__(self):
        self.biases = {}
        self.type = None
        pass

    def get_bias(self, bias_name, z):
        """Get the value of one of the bias functions at a given
        redshift.

        Args:
            bias_name (str): name of the bias function to return.
            z (float or array_like): redshift.

        Returns:
            float or array_like: bias value at the input redshifts.
        """
        if bias_name not in self.biases:
            raise KeyError("Bias %s not included in this tracer" % bias_name)
        return self.biases[bias_name](z)

    def _get_bias_function(self, b):
        # If None, assume it's zero
        if b is None:
            b = 0

        # If it's a scalar, then assume it's a constant function
        if np.ndim(b) == 0:
            def _const(z):
                if np.ndim(z) == 0:
                    return b
                else:
                    return b * np.ones_like(z)

            return _const
        else:  # Otherwise interpolate
            z, b = _check_array_params(b)
            return interp1d(z, b, bounds_error=False,
                            fill_value=b[-1])


class PTMatterTracer(PTTracer):
    """:class:`PTTracer` representing matter fluctuations.
    """
    def __init__(self):
        self.biases = {}
        self.type = 'M'


class PTNumberCountsTracer(PTTracer):
    """:class:`PTTracer` representing number count fluctuations.
    This is described by 1st and 2nd-order biases and
    a tidal field bias. These are provided as floating
    point numbers or tuples of (reshift,bias) arrays.
    If a number is provided, a constant bias is assumed.
    If `None`, a bias of zero is assumed.

    Args:
        b1 (float or tuple of arrays): a single number or a
            tuple of arrays (z, b(z)) giving the first-order
            bias.
        b2 (float or tuple of arrays): as above for the
            second-order bias.
        bs (float or tuple of arrays): as above for the
            tidal bias.
        b3nl (float or tuple of arrays): as above for the
            third-order bias.
        bk2 (float or tuple of arrays): as above for the
            non-local bias.
    """
    def __init__(self, b1, b2=None, bs=None, b3nl=None, bk2=None):
        self.biases = {}
        self.type = 'NC'

        # Initialize b1
        self.biases['b1'] = self._get_bias_function(b1)
        # Initialize b2
        self.biases['b2'] = self._get_bias_function(b2)
        # Initialize bs
        self.biases['bs'] = self._get_bias_function(bs)
        # Initialize b3nl
        self.biases['b3nl'] = self._get_bias_function(b3nl)
        # Initialize bk2
        self.biases['bk2'] = self._get_bias_function(bk2)

    @property
    def b1(self):
        """Internal first-order bias function.
        """
        return self.biases['b1']

    @property
    def b2(self):
        """Internal second-order bias function.
        """
        return self.biases['b2']

    @property
    def bs(self):
        """Internal tidal bias function.
        """
        return self.biases['bs']

    @property
    def b3nl(self):
        """Internal third-order bias function.
        """
        return self.biases['b3nl']

    @property
    def bk2(self):
        """Internal non-local bias function.
        """
        return self.biases['bk2']


class PTIntrinsicAlignmentTracer(PTTracer):
    """:class:`PTTracer` representing intrinsic alignments.
    This is described by 1st and 2nd-order alignment biases
    and an overdensity bias. These are provided as floating
    point numbers or tuples of (reshift,bias) arrays.
    If a number is provided, a constant bias is assumed.
    If `None`, a bias of zero is assumed.

    Args:
        c1 (float or tuple of arrays): a single number or a
            tuple of arrays (z, c1(z)) giving the first-order
            alignment bias.
        c2 (float or tuple of arrays): as above for the
            second-order alignment bias.
        cdelta (float or tuple of arrays): as above for the
            overdensity bias.
    """
    def __init__(self, c1, c2=None, cdelta=None):

        self.biases = {}
        self.type = 'IA'

        # Initialize c1
        self.biases['c1'] = self._get_bias_function(c1)
        # Initialize c2
        self.biases['c2'] = self._get_bias_function(c2)
        # Initialize cdelta
        self.biases['cdelta'] = self._get_bias_function(cdelta)

    @property
    def c1(self):
        """Internal first-order bias function.
        """
        return self.biases['c1']

    @property
    def c2(self):
        """Internal second-order bias function.
        """
        return self.biases['c2']

    @property
    def cdelta(self):
        """Internal overdensity bias function.
        """
        return self.biases['cdelta']

Function to convert from a_ia values to c_ia values,     using the standard convention of Blazek 2019 or the variant used     by the Dark Energy Survey analysis.      Args:         cosmo (:class:`~pyccl.core.Cosmology`): cosmology object.         z (float or array_like): z value(s) where amplitude is evaluated         a1 (float or array_like): IA a1 at input z values. Defaults to 1.0         a1delta (float or array_like): IA a1delta at input z values.             Defaults to None.         a2 (float or array_like): IA a2 at input z values.             Defaults to None.         Om_m2_for_c2 (bool): True to use the Blazek 2019 convention of             Om_m^2 scaling. Defaults to False         Om_m_fid (float): Value for Blazek 2019 scaling. Defaults to 0.3.      Returns:         c1 (float or array_like): IA c1 at input z values         c1delta (float or array_like): IA c1delta at input z values         c2 (float or array_like): IA c2 at input z values # Blazek2019 convention # DES convention PTTracers contain the information necessary to describe the     perturbative, non-linear inhomogeneities associated with     different physical quantities.      In essence their main function is to store a set of redshift-     dependent functions (e.g. perturbation theory biases) needed     in a perturbation theory framework to provide N-point     correlations. Get the value of one of the bias functions at a given         redshift.          Args:             bias_name (str): name of the bias function to return.             z (float or array_like): redshift.          Returns:             float or array_like: bias value at the input redshifts. # If None, assume it's zero # If it's a scalar, then assume it's a constant function # Otherwise interpolate :class:`PTTracer` representing matter fluctuations. :class:`PTTracer` representing number count fluctuations.     This is described by 1st and 2nd-order biases and     a tidal field bias. These are provided as floating     point numbers or tuples of (reshift,bias) arrays.     If a number is provided, a constant bias is assumed.     If `None`, a bias of zero is assumed.      Args:         b1 (float or tuple of arrays): a single number or a             tuple of arrays (z, b(z)) giving the first-order             bias.         b2 (float or tuple of arrays): as above for the             second-order bias.         bs (float or tuple of arrays): as above for the             tidal bias.         b3nl (float or tuple of arrays): as above for the             third-order bias.         bk2 (float or tuple of arrays): as above for the             non-local bias. # Initialize b1 # Initialize b2 # Initialize bs # Initialize b3nl # Initialize bk2 Internal first-order bias function. Internal second-order bias function. Internal tidal bias function. Internal third-order bias function. Internal non-local bias function. :class:`PTTracer` representing intrinsic alignments.     This is described by 1st and 2nd-order alignment biases     and an overdensity bias. These are provided as floating     point numbers or tuples of (reshift,bias) arrays.     If a number is provided, a constant bias is assumed.     If `None`, a bias of zero is assumed.      Args:         c1 (float or tuple of arrays): a single number or a             tuple of arrays (z, c1(z)) giving the first-order             alignment bias.         c2 (float or tuple of arrays): as above for the             second-order alignment bias.         cdelta (float or tuple of arrays): as above for the             overdensity bias. # Initialize c1 # Initialize c2 # Initialize cdelta Internal first-order bias function. Internal second-order bias function. Internal overdensity bias function.