We present a model for the Galactic supernova remnant (SNR) VRO 42.05.01, suggesting that its intriguing morphology can be explained by a progenitor model of a supersonically moving, mass losing star. The mass outflows of the progenitor star were in the form of an asymmetric stellar wind focused on the equatorial plane of the star. The systemic motion of the parent star in combination with its asymmetric outflows excavated an extended wind bubble that revealed a similar structure to this of VRO 42.05.01. Currently the SNR is interacting with the wind bubble and it is dominantly shaped by it. Employing 2D hydrodynamic simulations we model VRO 42.05.01 under the framework of this model and we reproduce its overall morphological properties. We discuss the variations of our progenitor model in light of the current observational uncertainties.

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We present preliminary analysis for PKS 2254+074 and S5 1803+784 from a multiband optical photometric monitoring programme of BL Lacertae objects carried out during 3 nights observing runs in 2001. The observations resulted in almost evenly sampled light curves 6-9 h long. We found inter-day variations with average amplitudes of 7-10 % and 2-6% respectively.

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