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A scenario for the origin of the system PSR B1757-24/supernova remnant (SNR)G5.4-1.2 is proposed. It is suggested that both objects are the remnants of asupernova (SN) that exploded within a pre-existing bubble blown-up by a runawaymassive star (the SN progenitor) during the final (Wolf-Rayet) phase of itsevolution. This suggestion implies that (a) the SN blast centre wassignificantly offset from the geometric centre of the wind-blown bubble (i.e.from the centre of the future SNR), (b) the bubble was surrounded by a massivewind-driven shell, and (c) the SN blast wave was drastically decelerated by theinteraction with the shell. Therefore, one can understand how the relativelyyoung and low-velocity pulsar PSR B1757-24 was able to escape from theassociated SNR G5.4-1.2 and why the inferred vector of pulsar transversevelocity does not point away from the geometric centre of the SNR. A possibleorigin of the radio source G5.27-0.9 (located between PSR B1757-24 and the SNRG5.4-1.2) is proposed. It is suggested that G5.27-0.9 is a lobe of a low Machnumber (\simeq 1.7) jet of gas outflowing from the interior of G5.4-1.2 throughthe hole bored in the SNR's shell by the escaping pulsar. It is also suggestedthat the non-thermal emission of the comet-shaped pulsar wind nebula originatesin the vicinity of the termination shock and in the cylindric region ofsubsonically moving shocked pulsar wind. The role of magnetized wind-drivenshells (swept-up during the Wolf-Rayet phase from the ambient interstellarmedium with the regular magnetic field) in formation of elongated axisymmetricSNRs is discussed.Comment: 7 pages, accepted for publication in A&

On the origin of the system PSR B 1757$\mathsf{-}$24/SNR G 5.4$\mathsf{-}$1.2