Retrieving the data by figure number

Fig. 1 Number of O stars vs. time for an instantaneous burst converting 10^6 M_sun of gas into stars. Format: column 1 = time, column 2 = log(number of O stars)

Fig. 2 Number of O stars vs. time for a constant star formation rate of 1 M_sun per year. Format: column 1 = time, column 2 = log(number of O stars)

Fig. 3 Ratio of Wolf-Rayet over O stars vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(WR/O)

Fig. 4 Ratio of Wolf-Rayet over O stars vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(WR/O)

Fig. 5 Supernova rate vs. time for an instantaneous starburst. Format: column 1 = time, column 2 = log(SN rate [yr^(-1)])

Fig. 6 Supernova rate vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(SN rate [yr^(-1)])

Fig. 7 Absolute bolometric time for an instantaneous burst. Format: column 1 = time, column 2 = M_bol

Fig. 8 Absolute bolometric magnitude vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = M_bol

Fig. 9 Absolute B magnitude vs. time for an instantaneous burst. Format: column 1 = time, column 2 = M_B

Fig. 10 Absolute B magnitude vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = M_B

Fig. 11 Absolute V magnitude vs. time for an instantaneous burst. Format: column 1 = time, column 2 = M_V

Fig. 12 Absolute V magnitude vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = M_V

Fig. 13 (U-B) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (U-B)

Fig. 14 (U-B) vs time. for a continuous star-formation rate Format: column 1 = time, column 2 = (U-B)

Fig. 15 (B-V) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (B-V)

Fig. 16 (B-V) vs time. for a continuous star-formation rate Format: column 1 = time, column 2 = (B-V)

Fig. 17 (V-R) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (V-R)

Fig. 18 (V-R) vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = (V-R)

Fig. 19 (V-I) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (V-I)

Fig. 20 (V-I) vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = (V-I)

Fig. 21 (V-J) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (V-J)

Fig. 22 (V-J) vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = (V-J)

Fig. 23 (V-H) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (V-H)

Fig. 24 (V-H) vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = (V-H)

Fig. 25 (V-K) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (V-K)

Fig. 26 (V-K) vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = (V-K)

Fig. 27 (V-L) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (V-L)

Fig. 28 (V-L) vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = (V-L)

Fig. 29 (2100-V) vs. time for an instantaneous burst. Format: column 1 = time, column 2 = (2100-V)

Fig. 30 (2100-V) for a continuous star-formation rate. Format: column 1 = time, column 2 = (2100-V)

Fig. 31 Beta_1550, the slope of L_lambda between 1200 and 1900 Å, vs. time for an instantaneous burst. Format: column 1 = time, column 2 = beta_1550

Fig. 32 Beta_1550, the slope of L_lambda between 1200 and 1900 Å, vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = beta_1550

Fig. 33 Beta_2600, the slope of L_lambda between 2200 and 3000 Å, vs. time for an instantaneous burst. Format: column 1 = time, column 2 = beta_2600

Fig. 34 Beta_2600, the slope of L_lambda between 2200 and 3000 Å, vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = beta_2600

Fig. 35 Lyman discontinuity vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(F_nu(912^+)/F_nu(912^-))

Fig. 36 Lyman discontinuity vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(F_nu(912^+)/F_nu(912^-))

Fig. 37 Number of photons below 912 Å vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(N(H^0) [photons s^(-1)])

Fig. 38 Number of photons below 912 Å vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(N(H^0) [photons s^(-1)])

Fig. 39 Number of photons below 504 Å vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(N(He^0) [photons s^(-1)])

Fig. 40 Number of photons below 504 Å vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(N(He^0) [photons s^(-1)])

Fig. 41 Number of photons below 228 Å vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(N(He^+) [photons s^(-1)])

Fig. 42 Number of photons below 228 Å vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(N(He^+) [photons s^(-1)])

Fig. 43 Equivalent width of H-alpha vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(W(H-alpha) [Å])

Fig. 44 Equivalent width of H-alpha vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(W(H-alpha) [Å])

Fig. 45 Equivalent width of H-beta vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(W(H-beta) [Å])

Fig. 46 Equivalent width of H-beta vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(W(H-beta) [Å])

Fig. 47 Equivalent width of Paschen-beta vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(W(Pa-beta) [Å])

Fig. 48 Equivalent width of Paschen-beta vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(W(Pa-beta) [Å])

Fig. 49 Equivalent width of Brackett-gamma vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(W(Br-gamma) [Å])

Fig. 50 Equivalent width of Brackett-gamma vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(W(Br-gamma) [Å])

Fig. 51 Mass-deposition rate of stellar winds and supernovae vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(Mass-loss rate [M_sun yr^(-1)])

Fig. 52 Mass-deposition rate of stellar winds and supernovae vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(Mass-loss rate [M_sun yr^(-1)])

Fig. 53 Total mass returned by stellar winds and supernovae vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(Mass [M_sun])

Fig. 54 Total mass returned by stellar winds and supernovae vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(Mass [M_sun])

Fig. 55 Deposition rate of mechanical energy by stellar winds and supernovae vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(L_mech [erg s^(-1)])

Fig. 56 Deposition rate of mechanical energy by stellar winds and supernovae vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(L_mech [erg s^(-1)])

Fig. 57 Total mechanical energy released by stellar winds and supernovae vs. time for an instantaneous burst. Format: column 1 = time, column 2 = log(Energy [erg])

Fig. 58 Total mechanical energy released by stellar winds and supernovae vs. time for a continuous star-formation rate. Format: column 1 = time, column 2 = log(Energy [erg])

Fig. 59 Influence of the burst duration on M_bol. Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = M_bol.

tau=0	tau=1 Myr	tau=3 Myr
tau=10 Myr	tau=50 Myr

Fig. 60 Influence of the burst duration on N(H^0). Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = log(N(H^0) [photons s^(-1)]).

tau=0	tau=1 Myr	tau=3 Myr
tau=10 Myr	tau=50 Myr

Fig. 61 Influence of the burst duration energy deposition rate of winds and supernovae. Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = log(L_mech [erg s^(-1)]).

tau=0	tau=1 Myr	tau=3 Myr
tau=10 Myr	tau=50 Myr

Fig. 62 Comparison between the theoretical (U-B) with and without inclusion of the nebular continuum. Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = (U-B).

Burst, neb. cont.	Burst, no neb. cont.
Continuous, neb. cont.	Continuous, no neb. cont.

Fig. 63 Same as 62, but for (B-V) Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = (B-V).

Burst, neb. cont.	Burst, no neb. cont.
Continuous, neb. cont.	Continuous, no neb. cont.

Fig. 64 Same as 62, but for (V-K) Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = (V-K).

Burst, neb. cont.	Burst, no neb. cont.
Continuous, neb. cont.	Continuous, no neb. cont.

Fig. 65 Same as 62, but for the equivalent width of H-alpha. Z=Z_sun, alpha=2.35; M_up=100 M_sun. Format: column 1 = time, column 2 = log(W(H-alpha) [Å]).

Burst, neb. cont.	Burst, no neb. cont.
Continuous, neb. cont.	Continuous, no neb. cont.

Fig. 66 Ratio of the mechanical luminosity over the ionizing luminosity below 912 Å for an instantaneous burst. Format: column 1 = time, column 2 = log(L_mech/L_912^-))

Fig. 67 Ratio of the mechanical luminosity over the bolometric luminosity for an instantaneous burst. Format: column 1 = time, column 2 = log(L_mech/L)

Fig. 68 Ratio of the mechanical luminosity over the bolometric luminosity for a continuous star-formation rate. Format: column 1 = time, column 2 = log(L_mech/L)

Fig. 69 Ratio of the mechanical luminosity over the ionizing luminosity below 912 Å for a continuous star-formation rate Format: column 1 = time, column 2 = log(L_mech/L_912^-)

Fig. 70 Ratio of the ionizing luminosity below 912 Å over the bolometric luminosity for a continuous star-formation rate. Format: column 1 = time, column 2 = log(L_912^-/L)

Fig. 71 Ratio of the ionizing luminosity below 912 Å over the bolometric luminosity for an instantaneous burst. Format: column 1 = time, column 2 = log(L_912^-/L)