pyccl.halos.pk_4pt module
- pyccl.halos.pk_4pt.halomod_trispectrum_1h(cosmo, hmc, k, a, prof, *, prof2=None, prof3=None, prof4=None, prof12_2pt=None, prof34_2pt=None)[source]
Computes the halo model 1-halo trispectrum for four different quantities defined by their respective halo profiles. The 1-halo trispectrum for four profiles \(u_{1,2}\), \(v_{1,2}\) is calculated as:
\[T_{u_1,u_2;v_1,v_2}(k_u,k_v,a) = I^0_{2,2}(k_u,k_v,a|u_{1,2},v_{1,2})\]where \(I^0_{2,2}\) is defined in the documentation of
I_0_22()
.Note
This approximation assumes that the 4-point profile cumulant is the same as the product of two 2-point cumulants. We may relax this assumption in future versions of CCL.
- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.k (
float
or array) – comoving wavenumber in \({\rm Mpc}^{-1}\).a (
float
or array) – scale factor.prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above).prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above). IfNone
,prof
will be used asprof2
.prof12_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment ofprof
andprof2
. IfNone
, the default second moment will be used, corresponding to the products of the means of both profiles.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. IfNone
,prof
will be used asprof3
.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. IfNone
,prof2
will be used asprof4
.prof34_2pt (
Profile2pt
) – same asprof12_2pt
forprof3
andprof4
.
- Returns:
1-halo trispectrum evaluated at each combination of
k
anda
. The shape of the output will be(N_a, N_k, N_k)
whereN_k
andN_a
are the sizes ofk
anda
respectively. The ordering is such thatoutput[ia, ik2, ik1] = T(k[ik1], k[ik2], a[ia])
Ifk
ora
are scalars, the corresponding dimension will be squeezed out on output.- Return type:
(
float
or array)
- pyccl.halos.pk_4pt.halomod_Tk3D_1h(cosmo, hmc, prof, *, prof2=None, prof3=None, prof4=None, prof12_2pt=None, prof34_2pt=None, lk_arr=None, a_arr=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False)[source]
Returns a
Tk3D
object containing the 1-halo trispectrum for four quantities defined by their respective halo profiles. Seehalomod_trispectrum_1h()
for more details about the actual calculation.- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile. IfNone
,prof
will be used asprof2
.prof3 (
HaloProfile
) – halo profile. IfNone
,prof
will be used asprof3
.prof4 (
HaloProfile
) – halo profile. IfNone
,prof2
will be used asprof4
.prof12_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment ofprof
andprof2
. IfNone
, the default second moment will be used, corresponding to the products of the means of both profiles.prof34_2pt (
Profile2pt
) – same asprof12_2pt
forprof3
andprof4
.a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If
None
, the internal values used bycosmo
will be used.lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of \({\rm Mpc}^{-1}\)) at which the trispectrum should be calculated for interpolation. If
None
, the internal values used bycosmo
will be used.extrap_order_lok (
int
) – extrapolation order to be used on k-values below the minimum of the splines. SeeTk3D
.extrap_order_hik (
int
) – extrapolation order to be used on k-values above the maximum of the splines. SeeTk3D
.use_log (
bool
) – ifTrue
, the trispectrum will be interpolated in log-space (unless negative or zero values are found).
- Returns:
1-halo trispectrum.
- Return type:
- pyccl.halos.pk_4pt.halomod_trispectrum_3h(cosmo, hmc, k, a, prof, *, prof2=None, prof3=None, prof4=None, prof13_2pt=None, prof14_2pt=None, prof24_2pt=None, prof32_2pt=None, p_of_k_a=None)[source]
Computes the isotropized halo model 3-halo trispectrum for four profiles \(u_{1,2}\), \(v_{1,2}\) as
\[\bar{T}^{3h}(k_1, k_2, a) = \int \frac{d\varphi_1}{2\pi} \int \frac{d\varphi_2}{2\pi} T^{2h}_{22}({\bf k_1},-{\bf k_1},{\bf k_2},-{\bf k_2}),\]with
\[T^{3h}{u_1,u_2;v_1,v_2}(k_u,k_v,a) = B^{PT}({f k_{u_1}}, {f k_{u_2}}, {f k_{v_1}} + {f k_{v_2}}) \, I^1_1(k_{u_1} | u) I^1_1(k_{u_2} | u) I^1_2(k_{v_1}, k_{v_2}|v}) \, + 5 perm\]where \(I^1_1\) and \(I^1_2\) are defined in the documentation of \(~HMCalculator.I_1_1\) and \(~HMCalculator.I_1_2\), respectively; and \(B^{PT}\) can be found in Eq. 30 of arXiv:1302.6994.
- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.k (float or array_like) – comoving wavenumber in Mpc^-1.
a (float or array_like) – scale factor.
prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above. If None, prof will be used as prof2.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. If None, prof will be used as prof3.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. If None, prof2 will be used as prof4.prof13_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment of prof and prof3. If None, the default second moment will be used, corresponding to the products of the means of both profiles.prof14_2pt (
Profile2pt
) – same as prof14_2pt for prof and prof4.prof24_2pt (
Profile2pt
) – same as prof14_2pt for prof2 and prof4.prof32_2pt (
Profile2pt
) – same as prof14_2pt for prof3 and prof2.p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. If None, the power spectrum stored within cosmo will be used.
- Returns:
integral values evaluated at each combination of k and a. The shape of the output will be (N_a, N_k, N_k) where N_k and N_a are the sizes of k and a respectively. The ordering is such that output[ia, ik2, ik1] = T(k[ik1], k[ik2], a[ia]) If k or a are scalars, the corresponding dimension will be squeezed out on output.
- Return type:
float or array_like
- pyccl.halos.pk_4pt.halomod_trispectrum_4h(cosmo, hmc, k, a, prof, prof2=None, prof3=None, prof4=None, p_of_k_a=None)[source]
Computes the isotropized halo model 4-halo trispectrum for four profiles \(u_{1,2}\), \(v_{1,2}\) as
\[\bar{T}^{4h}(k_1, k_2, a) = \int \frac{d\varphi_1}{2\pi} \int \frac{d\varphi_2}{2\pi} T^{4h}({\bf k_1},-{\bf k_1},{\bf k_2},-{\bf k_2}),\]with
\[T^{4h}{u_1,u_2;v_1,v_2}(k_u,k_v,a) = T^{PT}({f k_{u_1}}, {f k_{u_2}}, {f k_{v_1}}, {f k_{v_2}}) \, I^1_1(k_{u_1} | u) I^1_1(k_{u_2} | u) I^1_1(k_{v_1} | v) \, I^1_1(k_{v_2} | v) \,\]where \(I^1_1\) is defined in the documentation of \(~HMCalculator.I_1_1\) and \(P^{PT}\) can be found in Eq. 30 of arXiv:1302.6994.
- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.k (float or array_like) – comoving wavenumber in Mpc^-1.
a (float or array_like) – scale factor.
prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above. If None, prof will be used as prof2.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. If None, prof will be used as prof3.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. If None, prof2 will be used as prof4.p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. If None, the power spectrum stored within cosmo will be used.
- Returns:
integral values evaluated at each combination of k and a. The shape of the output will be (N_a, N_k, N_k) where N_k and N_a are the sizes of k and a respectively. The ordering is such that output[ia, ik2, ik1] = T(k[ik1], k[ik2], a[ia]) If k or a are scalars, the corresponding dimension will be squeezed out on output.
- Return type:
float or array_like
- pyccl.halos.pk_4pt.halomod_Tk3D_2h(cosmo, hmc, prof, prof2=None, prof3=None, prof4=None, prof12_2pt=None, prof13_2pt=None, prof14_2pt=None, prof24_2pt=None, prof32_2pt=None, prof34_2pt=None, p_of_k_a=None, lk_arr=None, a_arr=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False)[source]
Returns a
Tk3D
object containing the 2-halo trispectrum for four quantities defined by their respective halo profiles. Seehalomod_trispectrum_1h()
for more details about the actual calculation.- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above. If None, prof will be used as prof2.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. If None, prof will be used as prof3.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. If None, prof2 will be used as prof4.prof12_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment of prof and prof2. If None, the default second moment will be used, corresponding to the products of the means of both profiles.prof13_2pt (
Profile2pt
) – same as prof12_2pt for prof and prof3.prof14_2pt (
Profile2pt
) – same as prof14_2pt for prof and prof4.prof24_2pt (
Profile2pt
) – same as prof14_2pt for prof2 and prof4.prof32_2pt (
Profile2pt
) – same as prof14_2pt for prof3 and prof2.prof34_2pt (
Profile2pt
) – same as prof34_2pt for prof3 and prof4.p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. If None, the power spectrum stored within cosmo will be used.a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of Mpc^-1) at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
extrap_order_lok (int) – extrapolation order to be used on k-values below the minimum of the splines. See
Tk3D
.extrap_order_hik (int) – extrapolation order to be used on k-values above the maximum of the splines. See
Tk3D
.use_log (bool) – if True, the trispectrum will be interpolated in log-space (unless negative or zero values are found).
- Returns:
2-halo trispectrum.
- Return type:
- pyccl.halos.pk_4pt.halomod_Tk3D_3h(cosmo, hmc, prof, prof2=None, prof3=None, prof4=None, prof13_2pt=None, prof14_2pt=None, prof24_2pt=None, prof32_2pt=None, lk_arr=None, a_arr=None, p_of_k_a=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False)[source]
Returns a
Tk3D
object containing the 3-halo trispectrum for four quantities defined by their respective halo profiles. Seehalomod_trispectrum_3h()
for more details about the actual calculation.- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above. If None, prof will be used as prof2.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. If None, prof will be used as prof3.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. If None, prof2 will be used as prof4.prof13_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment of prof and prof3. If None, the default second moment will be used, corresponding to the products of the means of both profiles.prof14_2pt (
Profile2pt
) – same as prof14_2pt for prof and prof4.prof24_2pt (
Profile2pt
) – same as prof14_2pt for prof2 and prof4.prof32_2pt (
Profile2pt
) – same as prof14_2pt for prof3 and prof2.lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of Mpc^-1) at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. If None, the power spectrum stored within cosmo will be used.extrap_order_lok (int) – extrapolation order to be used on k-values below the minimum of the splines. See
Tk3D
.extrap_order_hik (int) – extrapolation order to be used on k-values above the maximum of the splines. See
Tk3D
.use_log (bool) – if True, the trispectrum will be interpolated in log-space (unless negative or zero values are found).
- Returns:
3-halo trispectrum.
- Return type:
- pyccl.halos.pk_4pt.halomod_Tk3D_4h(cosmo, hmc, prof, prof2=None, prof3=None, prof4=None, lk_arr=None, a_arr=None, p_of_k_a=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False)[source]
Returns a
Tk3D
object containing the 3-halo trispectrum for four quantities defined by their respective halo profiles. Seehalomod_trispectrum_4h()
for more details about the actual calculation.- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above. If None, prof will be used as prof2.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. If None, prof will be used as prof3.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. If None, prof2 will be used as prof4.lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of Mpc^-1) at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. If None, the power spectrum stored within cosmo will be used.extrap_order_lok (int) – extrapolation order to be used on k-values below the minimum of the splines. See
Tk3D
.extrap_order_hik (int) – extrapolation order to be used on k-values above the maximum of the splines. See
Tk3D
.use_log (bool) – if True, the trispectrum will be interpolated in log-space (unless negative or zero values are found).
- Returns:
4-halo trispectrum.
- Return type:
- pyccl.halos.pk_4pt.halomod_Tk3D_SSC_linear_bias(cosmo, hmc, *, prof, bias1=1, bias2=1, bias3=1, bias4=1, is_number_counts1=False, is_number_counts2=False, is_number_counts3=False, is_number_counts4=False, p_of_k_a=None, lk_arr=None, a_arr=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False, extrap_pk=False)[source]
Returns a
Tk3D
object containing the super-sample covariance trispectrum, given by the tensor product of the power spectrum responses associated with the two pairs of quantities being correlated. Each response is calculated as:\[\frac{\partial P_{u,v}(k)}{\partial\delta_L} = b_u b_v \left( \left(\frac{68}{21}-\frac{d\log k^3P_L(k)}{d\log k}\right) P_L(k)+I^1_2(k|u,v)\right) - (b_{u} + b_{v}) P_{u,v}(k)\]where the \(I^1_2\) is defined in the documentation
I_1_2()
and \(b_{u}\) and \(b_{v}\) are the linear halo biases for quantities \(u\) and \(v\), respectively. The second term is only included if the corresponding profiles do not represent number counts.- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – a halo profile representing the matter overdensity.bias1 (
float
or array) – linear galaxy bias for quantity 1. If an array, it has to have the shape ofa_arr
.bias2 (
float
or array) – linear galaxy bias for quantity 2.bias3 (
float
or array) – linear galaxy bias for quantity 3.bias4 (
float
or array) – linear galaxy bias for quantity 4.is_number_counts1 (
bool
) – IfTrue
, quantity 1 will be considered number counts and the clustering counter terms computed.is_number_counts2 (
bool
) – asis_number_counts1
but for quantity 2.is_number_counts3 (
bool
) – asis_number_counts1
but for quantity 3.is_number_counts4 (
bool
) – asis_number_counts1
but for quantity 4.p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. IfNone
, the power spectrum stored withincosmo
will be used.a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If
None
, the internal values used bycosmo
will be used.lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of \({\rm Mpc}^{-1}\)) at which the trispectrum should be calculated for interpolation. If
None
, the internal values used bycosmo
will be used.extrap_order_lok (
int
) – extrapolation order to be used on k-values below the minimum of the splines. SeeTk3D
.extrap_order_hik (
int
) – extrapolation order to be used on k-values above the maximum of the splines. SeeTk3D
.use_log (
bool
) – ifTrue
, the trispectrum will be interpolated in log-space (unless negative or zero values are found).extrap_pk (
bool
) – Whether to extrapolatep_of_k_a
in casea
is out of its support. IfFalse
, and the queried values are out of bounds, an error is raised. The default isFalse
.
- Returns:
SSC effective trispectrum.
- Return type:
- pyccl.halos.pk_4pt.halomod_Tk3D_SSC(cosmo, hmc, prof, *, prof2=None, prof3=None, prof4=None, prof12_2pt=None, prof34_2pt=None, p_of_k_a=None, lk_arr=None, a_arr=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False, extrap_pk=False)[source]
Returns a
Tk3D
object containing the super-sample covariance trispectrum, given by the tensor product of the power spectrum responses associated with the two pairs of quantities being correlated. Each response is calculated as:\[\frac{\partial P_{u,v}(k)}{\partial\delta_L} = \left(\frac{68}{21}-\frac{d\log k^3P_L(k)}{d\log k}\right) P_L(k)I^1_1(k,|u)I^1_1(k,|v)+I^1_2(k|u,v) - (b_{u} + b_{v}) P_{u,v}(k)\]where the \(I^a_b\) are defined in the documentation of
I_1_1()
andI_1_2()
and \(b_{u}\) and \(b_{v}\) are the linear halo biases for quantities \(u\) and \(v\), respectively (zero if the profiles are not number counts).- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – halo profile.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above). IfNone
,prof
will be used asprof2
.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above). IfNone
,prof
will be used asprof3
.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above). IfNone
,prof2
will be used asprof4
.prof12_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment ofprof
andprof2
. IfNone
, the default second moment will be used, corresponding to the products of the means of both profiles.prof34_2pt (
Profile2pt
) – same asprof12_2pt
forprof3
andprof4
. IfNone
,prof12_2pt
will be used.p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. IfNone
, the power spectrum stored withincosmo
will be used.a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If
None
, the internal values used bycosmo
will be used.lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of \({\rm Mpc}^{-1}\)) at which the trispectrum should be calculated for interpolation. If
None
, the internal values used bycosmo
will be used.extrap_order_lok (
int
) – extrapolation order to be used on k-values below the minimum of the splines. SeeTk3D
.extrap_order_hik (
int
) – extrapolation order to be used on k-values above the maximum of the splines. SeeTk3D
.use_log (
bool
) – ifTrue
, the trispectrum will be interpolated in log-space (unless negative or zero values are found).extrap_pk (
bool
) – Whether to extrapolatep_of_k_a
in casea
is out of its support. IfFalse
, and the queried values are out of bounds, an error is raised. The default isFalse
.
- Returns:
SSC effective trispectrum.
- Return type:
- pyccl.halos.pk_4pt.halomod_Tk3D_cNG(cosmo, hmc, prof, prof2=None, prof3=None, prof4=None, prof12_2pt=None, prof13_2pt=None, prof14_2pt=None, prof24_2pt=None, prof32_2pt=None, prof34_2pt=None, p_of_k_a=None, lk_arr=None, a_arr=None, extrap_order_lok=1, extrap_order_hik=1, use_log=False)[source]
Returns a
Tk3D
object containing the non-Gaussian covariance trispectrum for four quantities defined by their respective halo profiles. This is the sum of the trispectrum terms 1h + 2h + 3h + 4h.- Parameters:
cosmo (
Cosmology
) – a Cosmology object.hmc (
HMCalculator
) – a halo model calculator.prof (
HaloProfile
) – halo profile (corresponding to \(u_1\) above.prof2 (
HaloProfile
) – halo profile (corresponding to \(u_2\) above. If None, prof will be used as prof2.prof3 (
HaloProfile
) – halo profile (corresponding to \(v_1\) above. If None, prof will be used as prof3.prof4 (
HaloProfile
) – halo profile (corresponding to \(v_2\) above. If None, prof2 will be used as prof4.prof12_2pt (
Profile2pt
) – a profile covariance object returning the the two-point moment of prof and prof2. If None, the default second moment will be used, corresponding to the products of the means of both profiles.prof13_2pt (
Profile2pt
) – same as prof12_2pt for prof and prof3.prof14_2pt (
Profile2pt
) – same as prof12_2pt for prof and prof4.prof24_2pt (
Profile2pt
) – same as prof12_2pt for prof2 and prof4.prof32_2pt (
Profile2pt
) – same as prof12_2pt for prof3 and prof2.prof34_2pt (
Profile2pt
) – same as prof12_2pt for prof3 and prof4.p_of_k_a (
Pk2D
) – a Pk2D object to be used as the linear matter power spectrum. If None, the power spectrum stored within cosmo will be used.a_arr (array) – an array holding values of the scale factor at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
lk_arr (array) – an array holding values of the natural logarithm of the wavenumber (in units of Mpc^-1) at which the trispectrum should be calculated for interpolation. If None, the internal values used by cosmo will be used.
extrap_order_lok (int) – extrapolation order to be used on k-values below the minimum of the splines. See
Tk3D
.extrap_order_hik (int) – extrapolation order to be used on k-values above the maximum of the splines. See
Tk3D
.use_log (bool) – if True, the trispectrum will be interpolated in log-space (unless negative or zero values are found).
- Returns:
2-halo trispectrum.
- Return type: