**Cosmological Parameters:** params_lcdmw5.txt

**MPGRAFIC Input File:** mpgrafic_input_lcdmw5.dat

**Matter Power Spectrum:** pk_lcdmw5.dat

**RAMSES Input File:** ramses_input_lcdmw5.dat

*File Description:*

**param_xxxxx.txt**

#### h : reduced Hubble constant, H_{0} / (100 km/s/Mpc)

Ω_{m}: matter density

Ω_{b}: baryon density (used to compute initial power spectrum)

Ω_{r}: radiation density

#### n_{s}: spectral index

σ_{8}: linear rms of density fluctuations at z=0 smoothed in sphere of 8 Mpc/h radius

#### w: constant equation of state (for wcdm models)

α: slope of the scalar potential (for quintessence models)

**mpgrafic_input_xxxxx.dat**

#### a, dlna/dτ_{s}/(H0/100), D_{+}, dlnD_{+}/dlna

#### where a is the scale factor in the range 0.0001 < a < 1, τ_{s} is the superconformal time (= integral of dt/a^{2}), D_{+} is the linear growth factor (normalized to 1 at z=0)

**pk_xxxxx.dat**

#### k, P(k)

#### where k is the wavenumber in units Mpc^{-1} h and P(k) the linear matter power spectrum at z = 0 in units (Mpc/h)^{3}

**ramses_input_xxxxx.dat**

#### a, H/H_{0}, τ_{s}*H_{0}, t_{lookback}*H_{0}, t_{proper}*H_{0}

#### where a is the scale factor, H is the Hubble rate defined as H = 1/a * da/dτ_{s} with τ_{s} being the superconformal time (= integral of dt/a^{2}), t_{lookback} is the look-back time and t_{proper} is the proper time (= integral of dt/a)