6.7 Conclusion

The fits shown on Figure 6.7 are highly correlated, but the gradient is significantly different from a one-to-one plot possibly indicating that the method used to derive the magnitude is not accurate. A cautionary note must also, once again, be sounded by the errors on these fits. It is evident that the procedure derived by Fabregat and Torrejon (1998) is valid, but the large observational errors obtained in gaining the data may be unavoidable due to the dominant photospheric contiuum flux in this region (see Figure 6.2). Therefore it is expedient to try and derive a method that will produce smaller errors and thus make the relationship between the Strömgren photometry and optical emission lines more reliable. In Chapter 7 a new method of separating the circumstellar excess, interstellar reddening and intrinsic colour of Be stars is presented. This method is then used, in Chapter 8, with the Strömgren data presented in this chapter to try and improve the results.