Astrophysics

nnero.astrophysics.dmhalo_dmuv(hz: float | ndarray, m_uv: float | ndarray, alpha_star: float | ndarray, t_star: float | ndarray, f_star10: float | ndarray, omega_b: float | ndarray, omega_m: float | ndarray, *, mh: ndarray | None = None, mask: ndarray | None = None)

nnero.astrophysics.f_duty(mh: float | ndarray, m_turn: float | ndarray)

nnero.astrophysics.m_halo(hz: float | ndarray, m_uv: float | ndarray, alpha_star: float | ndarray, t_star: float | ndarray, f_star10: float | ndarray, omega_b: float | ndarray, omega_m: float | ndarray) → tuple[ndarray, ndarray]

Halo mass in term of the UV magnitude for a given astrophysical model

Parameters:

• hz (float, np.ndarray) – Shape (q, r). Hubble factor given in s^{-1}

• m_uv (float, np.ndarry (s,) or (r, s)) – UV magnitude.

• omega_b (float, np.ndaray (q,)) – Reduced abundance of baryons

Return type:

numpy.ndarray with shape (q, r, s)

nnero.astrophysics.phi_uv(z: float | ndarray, hz: float | ndarray, m_uv: float | ndarray, k: ndarray, pk: ndarray, alpha_star: float | ndarray, t_star: float | ndarray, f_star10: float | ndarray, m_turn: float | ndarray, omega_b: float | ndarray, omega_m: float | ndarray, h: float | ndarray, sheth_a: float = 0.322, sheth_q: float = 1.0, sheth_p: float = 0.3, *, window: str = 'sharpk', c: float = 2.5, mh: ndarray | None = None, mask: ndarray | None = None, dndmh: ndarray | None = None)

UV flux in Mpc^{-3}

Parameters:

• m_uv (float, np.ndarry (s,))

• omega_b (float, np.ndaray (q,))

Return type:

result of shape (q, r, s)