Here we present two sets of tables. The first includes the tables of the autocorrelation functions for dipolar emission (one photon) and for two-photon absorption obtained in the simulations. The second are the tables of the emission and polarization profiles calculated from the autocorrelation functions obtained in the simulations.

For each case considered in the simulation we present four files: 1) The autocorrelation function of the dipolar emission processes in the transition from level n=2 to level n=1. 2) The autocorrelation function of the two photon absorption process in the transition from the n=1 to the n=2 level. 3) Stark broadened spectral profiles of the Lyman alpha dipolar emission with fine structure. 4) Stark broadened profiles that could be obtained in a two-photon polarization spectroscopy experiment for the same transition, along with fine structure.

As the simulation processes include ion dynamics effects, each one of these files has the results that correspond to five different values of the reduced mass $\mu$ of the emitter-perturber pair. More precisely, each file includes the results corresponding to $\mu$ = 0.5, 0.8, 0.9, 1.0 and 2.0 (measured in units of proton mass).

The tables are ordered according to the parameter $\rho$ that characterizes the simulations. For the same value of $\rho$ the tables are organized in increasing values of the electron density.

The autocorrelation function files have, then, eleven columns, the first one corresponding to the time step (in seconds), followed by five pairs of columns corresponding to the five values of $\mu$ . Each pair is formed by the $C_{\rm R}(t)$ and $C_{\rm I}(t)$ parts of the autocorrelation function. The name of the files are rXXnYYYY.c1p or rXXnYYYY.c2p, where XX and YYYY correspond, respectively, to $100\times\rho$ and to $100\times\log{(N_{\rm e})}$ , $\rho$ and $N_{\rm e}$ being the values of the parameter $\rho$ and of the electron density for which the calculation was made. The c1p and c2p mean, respectively, correlation function for one photon emission and correlation function for two-photon absorption. An example of a correlation function file is given in Table 1.

**Table 3:** Temperature of the plasma - in K - of the simulation conditions considered
log $N_{\rm e}$	$\rho$
${\rm m}^{-3}$	0.10	0.15	0.20	0.25	0.30	0.40	0.50	0.60	0.70
19.67	29041	12907	7260	4647	-	-	-	-	-
20.00	37508	16670	9377	6001	4168	-	-	-	-
20.33	48444	21531	12111	7751	5383	-	-	-	-
20.67	62568	27808	15642	10011	6952	3910	-	-	-
21.00	80809	35915	20202	12929	8979	5051	3232	2245	-
21.33	104369	46386	26092	16699	11597	6523	4175	2899	-
21.67	-	59910	33699	21568	14978	8425	5392	3744	-
22.00	-	77377	43525	27856	19344	10881	6964	4836	3553
22.33	-	-	56214	35977	24984	14054	8994	6246	4589
22.67	-	-	-	46466	32268	18151	11617	8067	5927
23.00	-	-	-	60013	41676	23443	15003	10419	7655

The profile files have six columns, where the first one is the displacement in wavelength measured in meters from the wavelength that corresponds to the transition from the center of the fine structure sublevels of the level n=2 to the level n=1. The other five columns show the areanormalized profiles obtained for the five values of $\mu$ . The tabulated profiles give only the central part of the transition (to more or less $\frac{1}{10}$ of the peak intensity), because the plasma model employed in the simulation does not allow calculations far away from the center of the line. The name of the profiles files are rXXnYYYY.d1p or rXXnYYYY.p2p, where XX and YYYY have the same meaning as before, and the d1p and p2p mean, respectively, one photon dipolar emission profile and two-photon polarization profile. An example of a profile file is given in Table 2.

Table 3 summarizes the cases considered in the simulations and indicates the equilibrium temperature of the plasma for each value of $\rho$ and $N_{\rm e}$ .

The values of $C_{\rm R}(t)$ and $C_{\rm I}(t)$ given in the tables are those obtained directly from the computer simulations. However, the profiles given in the tables have been calculated from a smoothed autocorrelation function. These smooth functions have been obtained fitting their last channels to functions like

In addition, this fit avoids the appearance of a ${\rm sinc}(\Delta\omega)$ convolved in the Fourier transform.

3 Results. Calculated lines