All Figures

Figure 1: Typical hydrodynamical structure: density as a function of Rosseland optical depth for a model with  = 40 000 K,  = 3.50 and  =   /yr. The red dashed line is the initial TLUSTY structure on which a velocity law is connected to give the final CMFGEN input structure (black solid line). The dotted line shows the CMFGEN velocity structure as a function of Rosseland optical depth. The TLUSTY and CMFGEN structures are similar in the very inner atmosphere and start to depart from each other around which corresponds to a velocity of a few km s-1.

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In the text

Figure 2: Lower panel: gravity as a function of spectral type. Symbols corresponds to results derived from spectroscopic analysis of observed Galactic stars (sources: Repolust et al. 2004; Herrero et al. 2002; and Martins et al. 2005). Triangles are dwarfs, squares are giants and circles are supergiants. Lines are the least square fits of the observational data (solid: dwarfs; dashed: giants; dot-dashed: supergiants). Upper panel: difference between the calibration of Vacca et al. (1996) and the present ones.

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In the text

	Figure 3: Lower panel: "theoretical'' effective temperature scale for dwarfs (solid line), giants (dashed line) and supergiants (dot-dashed line) as derived from our model grid. Upper panel: difference between the scales of Vacca et al. (1996) and the present results.
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In the text

Figure 4: Effective temperature scale for dwarfs as derived from our model grid ("theoretical'' scale, solid line) compared to "observational'' results based on non-LTE line blanketed models including winds (Herrero et al. 2002; Repolust et al. 2004; and Martins et al. 2005). The dashed line is the result of linear regression to the data points. The typical error bars for the observational results are 0.5 unit for spectral types and are taken from detailed spectroscopic analysis for . The upper panel shows the difference between the relation of Vacca et al. (1996) and our scales (solid line: relation from model grid; dashed line: relation from spectroscopic analysis).

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In the text

	Figure 5: Same as Fig. 4 for giants.
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In the text

	Figure 6: Same as Fig. 4 for supergiants.
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In the text

	Figure 7: Comparison between H and He line profiles of the same model (A2, see Paper I) computed with the ISA-Wind photospheric structure (dashed line) and the TLUSTY structure (solid line). See text for discussion.
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In the text

	Figure 8: Same as Fig. 2 for absolute magnitudes. The standard deviation from the mean relation is 0.4 mag for dwarfs, 0.26 mag for giants and 0.45 mag for supergiants.
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In the text

	Figure 9: Bolometric correction as a function of effective temperature from our set of CMFGEN models. The solid line is the linear regression (Eq. (4)) and the dotted line is the relation of Vacca et al. (1996) and is shifted by 0.1 mag compared to our relation.
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In the text

	Figure 10: Bolometric correction as a function of spectral type from our set of CMFGEN models (solid lines) and from Vacca et al. (1996, dotted lines). BCs are usually reduced by 0.2 to 0.5 mag for a given spectral type, the reduction being the largest for early supergiants.
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In the text

	Figure 11: Same as Fig. 10 but with the bolometric corrections derived using the "theoretical'' (bold lines) and "observational'' (thin lines) scales. The upper panel shows the differences between "theoretical'' and "observational'' BCs.
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In the text

Figure 12: HR diagram showing the typical position of dwarfs (triangles), giants (squares) and supergiants (circles) from the present "theoretical'' calibration of and . Isochrones for 0, 1, 3 and 5 Myr are shown together with evolutionary tracks for different masses (taken from Meynet et al. 1994). The crosses and dotted lines are the positions of dwarfs, giants and supergiants following the Vacca et al. (1996) calibrations.

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In the text

	Figure 13: Ionising fluxes as a function of spectral type for dwarfs (triangles), giants (squares) and supergiants (circles) derived using the theoretical scale.
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In the text

	Figure 14: Lyman continuum photon fluxes derived using the theoretical (bold lines) and observational (thin lines) scales. Solid lines are for dwarfs, dashed lines for giants and dot-dashed lines for supergiants. The upper panel shows the difference between theoretical and observational results.
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In the text

	Figure 15: Same as Fig. 14 but for He  I ionising fluxes.
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In the text

	Figure 16: Comparison between CMFGEN, TLUSTY and WM-BASIC ionising fluxes for dwarfs. TLUSTY models are from Lanz & Hubeny (2002) and WM-BASIC models from Smith et al. (2002). Note that the latter have been estimated from the original SEDs and not from the SEDs re-binned for the inclusion in Starburst99. The CMFGEN fluxes are taken from Tables 1 to 6.
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In the text

	Figure 17: Same as Fig. 16 for supergiants.
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In the text

	Figure 18: Comparison between the present ionising fluxes of dwarfs and the results of Vacca et al. (1996) and Schaerer & de Koter (1997, CoStar models).
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In the text

	Figure 19: Same as Fig. 18 for giants.
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In the text

	Figure 20: Same as Fig. 18 for supergiants.
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In the text