New CCD photometry of seven successive years from 2010 is presented for the HW Vir-type eclipsing binary 2M 1533+3759 . Using the VI light curves together with the radial-velocity data given by For et al . ( 2010 ) , we determined the absolute parameters of each component to be M _ { 1 } = 0.442 \pm 0.012 M _ { \odot } , M _ { 2 } = 0.124 \pm 0.005 M _ { \odot } , R _ { 1 } = 0.172 \pm 0.002 R _ { \odot } , R _ { 2 } = 0.157 \pm 0.002 R _ { \odot } , L _ { 1 } = 19.4 \pm 1.4 L _ { \odot } , and L _ { 2 } = 0.002 \pm 0.002 L _ { \odot } . These indicate that 2M 1533+3759 is a detached system consisting of a normal sdB primary and an M7 dwarf companion . Detailed analyses of 377 minimum epochs , including our 111 timings , showed that the orbital period of the system remains constant during the past 12 yrs . Inspecting both types of minima , we found a delay of 3.9 \pm 1.0 s in the arrival times of the secondary eclipses relative to the primary eclipse times . This delay is in satisfactory agreement with the predicted Rømer delay of 2.7 \pm 1.4 s and the result is the second measurement in sdB+M eclipsing binaries . The time shift of the secondary eclipse can be explained by some combination of the Rømer delay and a non-zero eccentricity . Then , the binary star would have a very small eccentricity of e \cos { \omega } \simeq 0.0001 .