...1,2,[*]
Address for correspondence: Krasin str. 19, ap. 81, Moscow 123056, Russia. 
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... pulsar[*]
Note that this estimate is about ten times smaller than what follows from the usual dipole formula (Weisskopf et al. 1983). 
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... SNR[*]
Note that these structures could be significantly offset from the geometrical centre of a middle-aged SNR due to the proper motion of the SN progenitor star (Gvaramadze 1999b, 2000a,b). 
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...$4)\times 10^4$ years[*]
No proper motion for PSR B1509-58 has yet been detected (Kaspi et al. 1994; Gaensler et al. 1999), though the recent finding of the candidate optical counterpart of this pulsar (Caraveo et al. 1994, see also Mignami et al. 1998 and Sect. 4) allows one to hope that it will be detected in due course. For the distance to the pulsar of 5d5 kpc (e.g. Gaensler et al. 1999), a velocity of $150\, {\rm km} \, {\rm s}^{-1}$corresponds to a proper motion of $\simeq$ $6 \, {\rm mas}\,{\rm yr}^{-1}$; this is much smaller than the upper limits on the pulsar's proper motion given by Kaspi et al. (1994) and Gaensler et al. (1999). 
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... parameters[*]
Note that shocks in the range ( $v_{\rm s} \geq 40\, {\rm km}\,{\rm s}^{-1}$, where $v_{\rm s}$ is the shock velocity ($\simeq$$v_{\ast}$), $10^6 \, {\rm cm}^{-3} \leq n_{\rm cl} \leq 10^8 \, {\rm cm}^{-3}$) produce strong 22GHz ${\rm H}_2 {\rm O}$ masers (see Fig. 3 of Hollenbach 1997). The possible detection of ${\rm H}_2 {\rm O}$ masers towards PSR B1509-58 will lend strong support to the suggestions of this paper. 
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Copyright ESO 2001