tokens: The x -axis in the line profiles gives the lambda channels and the y -axis is the intensity in arbitrary units. Both [S ii ] lines at 6717 Å and 6731 Å are detected. The decomposition of each profile is indicated by the thin lines. The resulting profile is shown as hollow circles and with numbers. The dotted line represents the sum of all fitted components. We assume the brightest component of the line to be the main velocity component of the SNR. It is marked with a 0 in Fig. 6 . For each emission line, we can also identify two extreme velocity components. We shall refer to these as V min and V max . These are marked with a 2 and a 4, respectively. Table 3 reports the velocity components of the [S ii ] λ6717 Å line. Column 1 is the region ID. Columns 2, 3 and 4 indicate the main and extreme velocity components ( V min and V max ) corrected for the local standard of rest (LSR). Column 5 gives the difference in velocity between the extreme velocity components. Column 6 lists the distance of each region in arcmin to the geometrical centre of the SNR. Column 7 lists the [S ii ]/H α line ratio and finally column 8 indicates the associated filament to which each region belongs. As one can see from Fig. 6 and Table 3 , the radial velocity profiles are, in general, composite, implying large motions as expected in a SNR. They show at least three velocity components. The brightest one corresponds to the systemic motion of the SNR, while two faint velocity components are seen at extreme velocities. The several velocity components found in the velocity profiles of the filaments are probably due to the SNR shock expansion, as well as to contamination due to the interaction of the SNR gas with dense interstellar clouds that could be associated with the H ii regions located to the north and south-west of the remnant. Note the existence in the SNR velocity profiles of a velocity component also identified with those of regions located in the Perseus arm, as we will discuss below. The velocities of the main component vary from −34 to −89 km s −1 . Taking the average of all the velocities of the main components in Table 3 , we obtain a LSR velocity of −59 ± 17 km s −1 as a first estimate of the systemic velocity of the SNR. The averages for the extreme velocity components, in all the boxes where velocity profiles were extracted, are V min ∼ −122 km s −1 and V max ∼ +152 km s −1 . Another way of obtaining the systemic velocity is to average the extreme velocity components ( V min and V max ). Doing this, we obtained a systemic velocity V LSR = −50 ± 6 km s −1 . For some regions, we find an additional velocity component averaging 1 km s −1 . This latter velocity component agrees with the component found by Roberts ( 1972 ) in the theoretical H i profile of the TASS model at 12° pitch angle ( V LSR = 0 km s −1 ) in the direction of SNR CTB 109. Roberts ( 1972 ) attributed this component to gas located very close to the Sun in the Orion spur. Fig. 7 shows a
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