update

docs/source/Mnu.rst

@@ -4,3 +4,10 @@
 Massive neutrinos
 *****************
 
+Quijote include N-body simulations that model massive neutrinos. In these simulations, neutrinos as modelled as a separate cold and pressureless fluid represented by neutrino particles. The main difference between these particles and those of dark matter is that neutrino particles have thermal velocities that are draw in the initial conditions from the underlying Fermi-Dirac distribution.
+
+The initial conditions of these simulations are generated using the Zel'dovich approximation taking into account the scale-dependent growth factor and growth rate induced by neutrinos. For details on this we refer the reader `1605.05283 <https://arxiv.org/abs/1605.05283>`_.
+
+Currently, the simulations including massive neutrinos are ``Mnu_p``, ``Mnu_pp``, ``Mnu_ppp`` (designed to compute derivatives for Fisher matrix calculations), and the ``nwLH`` latin-hypercube (designed for machine learning applications). See :ref:`types` for further details.
+
+These simulations are designed to explore and quantify the impact of massive neutrinos on the different elements of the cosmic web.

docs/source/lcdm.rst

@@ -5,3 +5,12 @@ LCDM
 ****
 
 
+Quijote contains standard N-body simulations varying the five vanilla :math:`\Lambda{\rm CDM}` parameters: :math:`\Omega_{\rm m}`, :math:`\Omega_{\rm b}`, :math:`h`, :math:`n_s`, :math:`\sigma_8`. In these simulations :math:`w=-1`, :math:`M_\nu=0~{\rm eV}`, :math:`\Omega_K=0` and the initial conditions are generated with 2LPT.
+
+These simulations include ``Om_p``, ``Om_m``, ``Ob_p``, ``Ob_m``, ``h_p``, ``h_m``, ``ns_p``, ``ns_m``, ``s8_p``, ``s8_m``, ``Ob2_p``, ``Ob2_m``, ``fidcial``, ``fiducial_HR``, ``fiducial_LR``, ``fiducial_ZA``, and the three standard latin-hypercubes.
+
+.. Note::
+
+   The initial conditions of the ``fiducial_ZA`` simulations have been generated with the Zel'dovich approximation and not 2LPT. This is because these simulations are designed to be used with other Zel'dovich generated ICs simulation such as ``Mnu_p``, ``Mnu_pp``, and ``Mnu_ppp``.
+
+These simulations are designed to explore and quantify the impact of vanilla cosmological parameters of the spatial distribution of matter, halos, and galaxies.

docs/source/su.rst

@@ -3,3 +3,11 @@
 *****************
 Separate Universe
 *****************
+
+In standard N-body simulations, the mean matter matter density in the box is :math:`\Omega_{\rm m}\rho_{\rm crit}(1+z)^3`, where :math:`\rho_{\rm crit}(z)` is the critical density at redshift 0. In other words, the mean matter overdensity (with respect to the global one), :math:`\delta_b`, is zero. However, in the real Universe, regions of finite volume will exhibit fluctuations around :math:`\delta_b=0` due to perturbation on scales larger than the considered regions. Separate Universe simulations will follow the evolution of dark matter particles under the influence of an overdensity different to zero; or equivalently under the impact of a fluctuation that is larger than the size of the box. These simulations will thus have one extra parameter, :math:`\delta_b` that represents the mean overdensity over the entire box.
+
+The way to incorporate the global overdensity is to change the cosmology of it, introducing curvature. Thus, in these simulations :math:`\Omega_K \neq 1`. Currently, the only Quijote simulations with :math:`\delta_b\neq 0` are ``DC_p`` and ``DC_m`` that are designed to compute partial derivatives to quantify supersample covariance effects. See section 2.3 of the `Quijote paper <https://arxiv.org/abs/1909.05273>`_.
+
+These simulation are designed to explore and quatify the impact of super-sample covariance on cosmological ohservables. Many thanks to Yin Li for setting up the initial conditions and cosmology of these simulations.
+
+

docs/source/w.rst

@@ -3,3 +3,9 @@
 ***********
 Dark energy
 ***********
+
+Quijote contains simulations where the dark energy equation of state is :math:`w=\neq -1`. These are standard N-body simulations run with a different Hubble function, :math:`H(z)`, that contains the changes introduced in the evolution of the background by the dark energy equation of state. 
+
+The initial conditions of these simulations are generated using the Zel'dovich approximation and the inital matter power spectrum and :math:`H(z)` function is computed using `reps <https://github.com/matteozennaro/reps>`_. The simulations ``w_p`` and ``w_m`` (designed to compute partial derivatives for Fisher matrix calculations) together with the ``nwLH`` latin-hypercube are examples of simulations where :math:`w \neq -1`.
+
+These simulations are designed to explore and quantify the impact of the dark energy equation of state on the large-scale structure of the Universe.