As an efficient method to detect blending of general gravitational microlensing events, it is proposed to measure the shift of source star image centroid caused by microlensing. The conventional method to detect blending by this method is measuring the difference between the positions of the source star image point spread function measured on the images taken before and during the event (the PSF centroid shift, ${delta}{ heta}$c,PSF). In this paper, we investigate the difference between the centroid positions measured on the reference and the subtracted images obtained by using the difference image analysis method (DIA centroid shift, ${delta}{ heta}$c.DIA), and evaluate its relative usefulness in detecting blending over the conventional method based on ${delta}{ heta}$c,PSF measurements. From this investigation, we find that the DIA centroid shift of an event is always larger than the PSF centroid shift. We also find that while ${delta}{ heta}$c,PSF becomes smaller as the event amplification decreases, ${delta}{ heta}$c.DIA remains constant regardless of the amplification. In addition, while ${delta}{ heta}$c,DIA linearly increases with the increasing value of the blended light fraction, ${delta}{ heta}$c,PSF peaks at a certain value of the blended light fraction and then eventually decreases as the fraction further increases. Therefore, measurements of ${delta}{ heta}$c,DIA instead of ${delta}{ heta}$c,PSF will be an even more efficient method to detect the blending effect of especially of highly blended events, for which the uncertainties in the determined time scales are high, as well as of low amplification events, for which the current method is highly inefficient.