Context : HIP 96515 A is a double-lined spectroscopic binary included in the SACY catalog as a potential young star , and classified as an eclipsing binary in the ASAS catalog . It has a visual companion ( CCDM 19371-5134 B , HIP 96515 B ) at 8 \aas@@fstack { \prime \prime } 6 . If bound to the primary , the optical and infrared colors of this wide companion are consistent with those of a white dwarf . Aims : The aim of this work is to characterize the system HIP 96515 A & B by studying each of its components . Methods : We have analyzed spectroscopic and photometric observations of HIP 96515 A and its visual companion , HIP 96515 B . To confirm the system as a common proper motion pair , we have analyzed the astrometry of the components using high-angular resolution infrared observations obtained within a time span of two years and archival astrometry . Results : The high-resolution optical spectrum of HIP 96515 A has been used to derive a mass ratio , M _ { 2 } / M _ { 1 } , close to 0.9 , with the components showing spectral types of M1 and M2 . The optical light-curve of HIP 96515 A shows periodic variations with P _ { orb } =2.3456 days , confirming that HIP 96515 A is an eclipsing binary , with preliminary parameters of i = 89 \aas@@fstack { \circ } 0 \pm 0 \aas@@fstack { \circ } 2 , and M _ { 1 } =0.59 \pm 0.03 M _ { \odot } and M _ { 2 } =0.54 \pm 0.03 M _ { \odot } , for the primary and secondary , respectively , at an estimated distance of 42 \pm 3 pc . This is a new eclipsing binary with component masses below 0.6 M _ { \odot } . Multi-epoch observations of HIP 96515 A & B show that the system is a common proper motion pair . The optical spectrum of HIP 96515 B is consistent with a pure helium atmosphere ( DB ) white dwarf . The comparison with evolutionary cooling sequence models provides T _ { \mathrm { eff,WD } } =19,126 \pm 195 K , \log g _ { \mathrm { WD } } =8.08 , M _ { \mathrm { WD } } / \mathrm { M } _ { \odot } =0.6 , and a distance of \sim 46 pc . The estimated WD cooling age is \sim 100 Myr and the total age of the object ( including the main-sequence phase ) is \sim 400 Myr . Finally , if HIP 96515 A & B are coeval , and assuming a common age of \sim 400 Myr , the comparison of the masses of the eclipsing binary members with evolutionary tracks shows that they are underestimated by \sim 15 % and 10 % , for the primary and secondary , respectively . Conclusions :