We have identified stellar and substellar members in the nearby star cluster Coma Berenices , using photometry , proper motions , and distances of a combination of 2MASS , UKIDSS , URAT1 , and Gaia /DR2 data . Those with Gaia /DR2 parallax measurements provide the most reliable sample to constrain the distance , averaging 86.7 pc with a dispersion 7.1 pc , and the age \sim 800 Myr , of the cluster . This age is older than the 400–600 Myr commonly adopted in the literature . Our analysis , complete within 5 \degr of the cluster radius , leads to identification of 192 candidates , among which , after field contamination is considered , about 148 are true members . The members have J \sim 3 mag to \sim 17.5 mag , corresponding to stellar masses 2.3–0.06 M _ { \sun } . The mass function of the cluster peaks around 0.3 M _ { \sun } and , in the sense of dN / dm = m ^ { - \alpha } , where N is the number of members and m is stellar mass , has a slope \alpha \approx 0.49 \pm 0.03 in the mass range 0.3–2.3 M _ { \sun } . This is much shallower than that of the field population in the solar neighborhood . The slope \alpha = -1.69 \pm 0.14 from 0.3 M _ { \sun } to 0.06 M _ { \sun } , the lowest mass in our sample . The cluster is mass segregated and has a shape elongated toward the Galactic plane . Our list contains nine substellar members , including three new discoveries of an M8 , an L1 and an L4 brown dwarfs , extending from the previously known coolest members of late-M types to even cooler types .