All Figures

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7125fig1.eps}\end{figure}$ Figure 1: Temperature structure against Rosseland optical mean depth for the hydrostatic density structure produced from combining the subsonic TLUSTY velocity structure with the supersonic CMFGEN velocity structure, such that the velocity and velocity gradient are constant. The above example is for the B0.5 Ia star HD 185859 ( $T_{\rm eff}$ = 26 000 K, log g = 3.13).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{NEWFIGURE-7125fig2.eps}\end{figure}$ Figure 2: Overall CMFGEN fit to the optical spectrum of B0-B5 supergiants (4050-4250 Å). The solid black line is the observed spectrum and the red line denotes the CMFGEN model fit.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{7125fig3.eps}\end{figure}$ Figure 3: Overall CMFGEN fit to the optical spectrum of B0-B5 supergiants (4200-4450 Å). The solid black line is the observed spectrum and the red line denotes the CMFGEN model fit.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11cm,clip]{7125fig4.eps}\end{figure}$ Figure 4: Overall CMFGEN fit to the optical spectra of B0-B5 supergiants (4450-4650 Å). The solid black line is the observed spectrum and the red line denotes the CMFGEN model fit.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7125fig5.eps}\end{figure}$ Figure 5: The Galactic B supergiant $T_{\rm eff}$ scale as a function of spectral type. B Ia stars are indicated by an asterisk, whilst B Ib stars are marked by a plus sign.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7125fig6.eps}\end{figure}$ Figure 6: The Galactic B supergiant $T_{\rm eff}$ - log g scale.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7125fig7.eps}\end{figure}$ Figure 7: Example of a TLUSTY log g fit to H $\gamma$ profile of the B5 Ib/II star HD 164353. A value of log g = 2.75 is used here.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{7125fig8.eps}\end{figure}$ Figure 8: Position of the sample of Galactic B supergiants on the Hertzsprung-Russell diagram, along with other Galactic B supergiants Crowther et al. (2006), SMC B supergiants Trundle et al. (2004); Trundle & Lennon (2005) and Galactic O stars Repolust et al. (2004). Evolutionary tracks are taken from Maeder & Meynet (2001) and imply 15 $M_{\odot }$ < $M_{\rm evol}$ $\le$ 40 $M_{\odot }$ for the sample of 20 Galactic B supergiants presented in this work. Galactic B supergiants that are common to both our sample and that of Crowther et al. (2006) are joined by a dotted red line to illustrate the effect of different stellar parameters on a star's precise location on the HR diagram.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{7125fig9.eps}\end{figure}$ Figure 9: Comparison of evolutionary and spectroscopically-derived stellar masses for the sample of B supergiants. The dotted line indicates 1:1 correspondance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.55cm,clip]{NEWFIGURE-7125fig10.eps}\end{figure}$ Figure 10: Comparison of $\frac{M_{\rm evol}}{M_{\rm spec}}$ with luminosity (B5 Ib/II stars omitted). Values obtained for the 20 Galactic B supergiants (asterisks) are plotted with those derived for SMC B supergiants (diamonds) Trundle et al. (2004); Trundle & Lennon (2005). The dotted line indicates 1:1 correspondance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7125fg11.eps}\end{figure}$ Figure 11: Comparison of the relative strengths of the N and C lines in $\kappa$ Cas and HD 154090.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{7125fg12.eps}\end{figure}$ Figure 12: Examples of CMFGEN fits to H $\alpha$ profiles of $\kappa$ Cas, HD 190603, HD 14818, HD 190066, HD 193183 and HD 164353, along with the mass loss rate adopted for each star. The red, dotted line represents the CMFGEN model fit to each H $\alpha$ profile and the solid, black line indicates the observed H $\alpha$ profile.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7125fg13.eps}\end{figure}$ Figure 13: Comparison of CMFGEN derived mass loss rates with theoretical mass loss rates predicted by the Vink et al. (2000) mass loss prescription. The dotted line indicates 1:1 correspondance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.55cm,clip]{7125fg14.eps}\end{figure}$ Figure 14: Comparison of CMFGEN derived $\dot{M}$ with those of Kudritzki et al. (1999) for 8 stars common to both samples.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{7125fg15.eps}\end{figure}$ Figure 15: The wind-luminosity momentum relation for OBA stars. Note the dependence of the WLR on spectral type and metallicity. The theoretical WLR predicted by Vink et al. (2000) is calculated for our sample of Galactic B supergiants and is represented by the orange line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{7125fg16.eps}\end{figure}$ Figure 16: CMFGEN model fit to the IUE spectrum of HD 14818 (B2 Ia), focusing on the UV silicon $T_{\rm eff}$ diagnostics: Si II $\lambda$ 1265 and $\lambda$ 1309, Si III $\lambda$ 1294, $\lambda$ 1299 and $\lambda$ 1417. The ``best fit'' model derived from the optical has $T_{\rm eff}$ = 18 000 K, L = 2.5 $\times$ 10⁵ $L/L_{\odot }$ and $\dot{M}$ = 1.1 $\times$ 10^-6 $M_{\odot}~\rm {yr}^{-1}$ (dashed red line). Others models have $T_{\rm eff}$ = 17 500 K, L = 2.4 $\times$ 10⁵ $L/L_{\odot }$ , $\dot{M}$ = 1.2 $\times$ 10^-6 $M_{\odot}~\rm {yr}^{-1}$ (dotted green line) and $T_{\rm eff}$ = 18 500 K, L = 2.5 $\times$ 10⁵ $L/L_{\odot }$ , $\dot{M}$ = 1.8 $\times$ 10^-6 $M_{\odot}~\rm {yr}^{-1}$ (dot-dashed blue line).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{7125fg17.eps}\end{figure}$ Figure 17: CMFGEN fit to the IUE spectrum to the N V, C IV, Si IV, Al III and C II wind resonance lines of HD 190603 (B1.5 Ia+). Note that a good fit to H $\alpha$ does not guarantee the same mass loss rate will provide a good fit to the UV P Cygni profiles. Model parameters are $T_{\rm eff}$ = 19 500 K, $\log\ (L/\mbox{$L_{\odot}$ })$ = 5.41 and $\dot{M}$ = 2.4 $\times$ 10^-6 $M_{\odot }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{7125fg18.eps}\end{figure}$ Figure 18: CMFGEN fit to the IUE spectrum to the N V, C IV, Si IV, Al III and C II wind resonance lines of HD 14818 (B2 Ia). Even though the fit to H $\alpha$ is not perfect, a reasonable fit is made to the UV P Cygni profiles, particularly Si IV and Al III. Model parameters are $T_{\rm eff}$ = 18 000 K, $\log\ (L/\mbox{$L_{\odot}$ })$ = 5.40 and $\dot{M}$ = 1.0 $\times$ 10^-6 $M_{\odot }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{7125fg19.eps}\end{figure}$ Figure 19: CMFGEN fit to the IUE spectrum to the N V, C IV, Si IV, Al III and C II wind resonance lines of HD 53138 (B3 Ia). Although a good fit has been made to H $\alpha$ with the adopted mass loss rate, CMFGEN does not reproduce the observed UV P Cygni profiles well. Model parameters are $T_{\rm eff}$ = 16 500 K, $\log\ (L/\mbox{$L_{\odot}$ })$ = 5.30 and $\dot{M}$ = 4.5 $\times$ 10^-7 $M_{\odot }$ .
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7125fg20.eps}\end{figure}$ Figure 20: Comparison of UV wind resonance lines of HD 192660 for models with $\dot{M}$ = 5.0 $\times$ 10^-6 $M_{\odot }$ (red dashed line) and 2.6 $\times$ 10^-6 $M_{\odot }$ (blue dotted line) for HD 192660 (B0 Ib).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.85cm,clip]{7125fg21.eps}\end{figure}$ Figure 21: Comparison of UV wind resonance lines of HD 164353 for models with $\dot{M}$ = 6 $\times$ 10^-8 $M_{\odot}~\rm {yr}^{-1}$ (red dashed line) and =1.8 $\times$ 10^-7 $M_{\odot}~\rm {yr}^{-1}$ (blue dotted line) respectively.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7125fg22.eps}\end{figure}$ Figure 22: CMFGEN predicted ionisation structure at different $T_{\rm eff}$ , plotted against normalised veocity w. The ions are colour-coded as follows: N V = green, C IV = red, Si IV = dark blue, Si III = light blue, Al III = purple and C II = yellow. Si IV is predicted to be dominant for B0-B2 supergiants ( $30~000~{\rm K} \le$ $\mbox{$T_{\rm eff}$ }$ $\le$ 18 000 K), after which Si III, Al III and C II take over as the dominant ions in the wind for $T_{\rm eff}$ $\le$ 18 000 K.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg23.eps}\end{figure}$ Figure A.1: CMFGEN model fits (4050-4250 Å) to the optical spectra of 10 B Ia supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg24.eps}\end{figure}$ Figure A.2: CMFGEN model fits (4250-4450 Å) to the optical spectra of 10 B Ia supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg25.eps}\end{figure}$ Figure A.3: CMFGEN model fits (4450-4650 Å) to the optical spectra of 10 B Ia supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg26.eps}\end{figure}$ Figure A.4: CMFGEN model fits (4050-4250 Å) to the optical spectra of 10 B Ib supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg27.eps}\end{figure}$ Figure A.5: CMFGEN model fits (4250-4450 Å) to the optical spectra of 10 B Ib supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg28.eps}\end{figure}$ Figure A.6: CMFGEN model fits (4450-4650 Å) to the optical spectra of 10 B Ib supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{7125fg29.eps}\end{figure}$ Figure A.7: TLUSTY model fits to the H $\gamma$ profile of all 20 supergiants. Optical spectrum is represented by a solid, black line; TLUSTY model fit is shown as a dotted black line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{7125fg30.eps}\end{figure}$ Figure A.8: TLUSTY model fits to the H $\delta$ profile of all 20 supergiants. Optical spectrum is represented by a solid, black line; TLUSTY model fit is shown as a dotted black line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{7125fg31.eps}\end{figure}$ Figure A.9: CMFGEN model fit to the IUE spectra of 10 B0-B5 supergiants (1230-1480 Å). The solid red line represents the model fits whereas the solid black line is the IUE spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{7125fg32.eps}\end{figure}$ Figure A.10: CMFGEN model fit to the IUE spectra of 10 B0-B5 supergiants (1480-1680 Å). The solid red line represents the model fits whereas the solid black line is the IUE spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{7125fg33.eps}\end{figure}$ Figure A.11: CMFGEN model fit to the IUE spectra of 10 B0-B5 supergiants (1680-1880 Å). The solid red line represents the model fits whereas the solid black line is the IUE spectrum.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7125fig1.eps}\end{figure}$	Figure 1: Temperature structure against Rosseland optical mean depth for the hydrostatic density structure produced from combining the subsonic TLUSTY velocity structure with the supersonic CMFGEN velocity structure, such that the velocity and velocity gradient are constant. The above example is for the B0.5 Ia star HD 185859 ( $T_{\rm eff}$ = 26 000 K, log g = 3.13).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11cm,clip]{NEWFIGURE-7125fig2.eps}\end{figure}$	Figure 2: Overall CMFGEN fit to the optical spectrum of B0-B5 supergiants (4050-4250 Å). The solid black line is the observed spectrum and the red line denotes the CMFGEN model fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11cm,clip]{7125fig3.eps}\end{figure}$	Figure 3: Overall CMFGEN fit to the optical spectrum of B0-B5 supergiants (4200-4450 Å). The solid black line is the observed spectrum and the red line denotes the CMFGEN model fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11cm,clip]{7125fig4.eps}\end{figure}$	Figure 4: Overall CMFGEN fit to the optical spectra of B0-B5 supergiants (4450-4650 Å). The solid black line is the observed spectrum and the red line denotes the CMFGEN model fit.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{7125fig5.eps}\end{figure}$	Figure 5: The Galactic B supergiant $T_{\rm eff}$ scale as a function of spectral type. B Ia stars are indicated by an asterisk, whilst B Ib stars are marked by a plus sign.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{7125fig6.eps}\end{figure}$	Figure 6: The Galactic B supergiant $T_{\rm eff}$ - log g scale.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{7125fig7.eps}\end{figure}$	Figure 7: Example of a TLUSTY log g fit to H $\gamma$ profile of the B5 Ib/II star HD 164353. A value of log g = 2.75 is used here.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.25cm,clip]{7125fig9.eps}\end{figure}$	Figure 9: Comparison of evolutionary and spectroscopically-derived stellar masses for the sample of B supergiants. The dotted line indicates 1:1 correspondance.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.55cm,clip]{NEWFIGURE-7125fig10.eps}\end{figure}$	Figure 10: Comparison of $\frac{M_{\rm evol}}{M_{\rm spec}}$ with luminosity (B5 Ib/II stars omitted). Values obtained for the 20 Galactic B supergiants (asterisks) are plotted with those derived for SMC B supergiants (diamonds) Trundle et al. (2004); Trundle & Lennon (2005). The dotted line indicates 1:1 correspondance.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7125fg11.eps}\end{figure}$	Figure 11: Comparison of the relative strengths of the N and C lines in $\kappa$ Cas and HD 154090.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.5cm,clip]{7125fg12.eps}\end{figure}$	Figure 12: Examples of CMFGEN fits to H $\alpha$ profiles of $\kappa$ Cas, HD 190603, HD 14818, HD 190066, HD 193183 and HD 164353, along with the mass loss rate adopted for each star. The red, dotted line represents the CMFGEN model fit to each H $\alpha$ profile and the solid, black line indicates the observed H $\alpha$ profile.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{7125fg13.eps}\end{figure}$	Figure 13: Comparison of CMFGEN derived mass loss rates with theoretical mass loss rates predicted by the Vink et al. (2000) mass loss prescription. The dotted line indicates 1:1 correspondance.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.55cm,clip]{7125fg14.eps}\end{figure}$	Figure 14: Comparison of CMFGEN derived $\dot{M}$ with those of Kudritzki et al. (1999) for 8 stars common to both samples.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{7125fg15.eps}\end{figure}$	Figure 15: The wind-luminosity momentum relation for OBA stars. Note the dependence of the WLR on spectral type and metallicity. The theoretical WLR predicted by Vink et al. (2000) is calculated for our sample of Galactic B supergiants and is represented by the orange line.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{7125fg17.eps}\end{figure}$	Figure 17: CMFGEN fit to the IUE spectrum to the N V, C IV, Si IV, Al III and C II wind resonance lines of HD 190603 (B1.5 Ia+). Note that a good fit to H $\alpha$ does not guarantee the same mass loss rate will provide a good fit to the UV P Cygni profiles. Model parameters are $T_{\rm eff}$ = 19 500 K, $\log\ (L/\mbox{$L_{\odot}$ })$ = 5.41 and $\dot{M}$ = 2.4 $\times$ 10^-6 $M_{\odot }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=90,width=8.6cm,clip]{7125fg18.eps}\end{figure}$	Figure 18: CMFGEN fit to the IUE spectrum to the N V, C IV, Si IV, Al III and C II wind resonance lines of HD 14818 (B2 Ia). Even though the fit to H $\alpha$ is not perfect, a reasonable fit is made to the UV P Cygni profiles, particularly Si IV and Al III. Model parameters are $T_{\rm eff}$ = 18 000 K, $\log\ (L/\mbox{$L_{\odot}$ })$ = 5.40 and $\dot{M}$ = 1.0 $\times$ 10^-6 $M_{\odot }$ .
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{7125fg20.eps}\end{figure}$	Figure 20: Comparison of UV wind resonance lines of HD 192660 for models with $\dot{M}$ = 5.0 $\times$ 10^-6 $M_{\odot }$ (red dashed line) and 2.6 $\times$ 10^-6 $M_{\odot }$ (blue dotted line) for HD 192660 (B0 Ib).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.85cm,clip]{7125fg21.eps}\end{figure}$	Figure 21: Comparison of UV wind resonance lines of HD 164353 for models with $\dot{M}$ = 6 $\times$ 10^-8 $M_{\odot}~\rm {yr}^{-1}$ (red dashed line) and =1.8 $\times$ 10^-7 $M_{\odot}~\rm {yr}^{-1}$ (blue dotted line) respectively.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg23.eps}\end{figure}$	Figure A.1: CMFGEN model fits (4050-4250 Å) to the optical spectra of 10 B Ia supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg24.eps}\end{figure}$	Figure A.2: CMFGEN model fits (4250-4450 Å) to the optical spectra of 10 B Ia supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg25.eps}\end{figure}$	Figure A.3: CMFGEN model fits (4450-4650 Å) to the optical spectra of 10 B Ia supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg26.eps}\end{figure}$	Figure A.4: CMFGEN model fits (4050-4250 Å) to the optical spectra of 10 B Ib supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg27.eps}\end{figure}$	Figure A.5: CMFGEN model fits (4250-4450 Å) to the optical spectra of 10 B Ib supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9.3cm,clip]{7125fg28.eps}\end{figure}$	Figure A.6: CMFGEN model fits (4450-4650 Å) to the optical spectra of 10 B Ib supergiants, with the $T_{\rm eff}$ , luminosity and CNO diagnostic lines marked as shown. Optical spectrum is in black, CMFGEN model fit is shown in red.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{7125fg29.eps}\end{figure}$	Figure A.7: TLUSTY model fits to the H $\gamma$ profile of all 20 supergiants. Optical spectrum is represented by a solid, black line; TLUSTY model fit is shown as a dotted black line.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.8cm,clip]{7125fg30.eps}\end{figure}$	Figure A.8: TLUSTY model fits to the H $\delta$ profile of all 20 supergiants. Optical spectrum is represented by a solid, black line; TLUSTY model fit is shown as a dotted black line.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{7125fg31.eps}\end{figure}$	Figure A.9: CMFGEN model fit to the IUE spectra of 10 B0-B5 supergiants (1230-1480 Å). The solid red line represents the model fits whereas the solid black line is the IUE spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{7125fg32.eps}\end{figure}$	Figure A.10: CMFGEN model fit to the IUE spectra of 10 B0-B5 supergiants (1480-1680 Å). The solid red line represents the model fits whereas the solid black line is the IUE spectrum.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=11.3cm,clip]{7125fg33.eps}\end{figure}$	Figure A.11: CMFGEN model fit to the IUE spectra of 10 B0-B5 supergiants (1680-1880 Å). The solid red line represents the model fits whereas the solid black line is the IUE spectrum.
Open with DEXTER