Abstract Here we put forward some arguments in favour of the existence of slow bars. More then a half of spiral galaxies have in their central regions a bar — a structure in the form of triaxial ellipsoid. Historically two models of the bar were developed — those of the so called “slow” and “fast” bars. In both cases the bar is in some resonance with the galactic disc region near the bar ends — it is the corotation resonance for a fast bar and the inner Lindblad resonance for a slow bar. For the same angular velocity the fast bar would be larger then the slow bar. Alternatively, for the same size the fast bar would have much higher angular velocity, that being the reason for the terminology used. Up till now, the direct measurement of angular velocity of a bar has been an open problem. This is why all arguments on the nature of bar observed in some particular galaxy are inevitably indirect. Despite the fact that the model of slow bars was developed slightly earlier, the main part of attention was focused on the fast bars. Presently many researchers believe in the existence of the fast bars in real galaxies, while discussions on the existence of the slow bars continue so far. In this Letter we demonstrate that the bar detected in the grand design spiral galaxy NGC 157 is the slow bar.