Most field stars will have encountered the highest stellar density and hence the largest number of interactions in their birth environment . Yet the stellar dynamics during this crucial phase are poorly understood . Here we analyze the radial velocities measured for 152 out of 380 observed stars in the 2-6 Myr old star cluster IC 348 as part of the SDSS-III APOGEE . The radial velocity distribution of these stars is fitted with one or two Gaussians , convolved with the measurement uncertainties including binary orbital motions . Including a second Gaussian improves the fit ; the high-velocity outliers that are best fit by this second component may either ( 1 ) be contaminants from the nearby Perseus OB2 association , ( 2 ) be a halo of ejected or dispersing stars from IC 348 , or ( 3 ) reflect that IC 348 has not relaxed to a Gaussian velocity distribution . We measure a velocity dispersion for IC 348 of 0.72 \pm 0.07 km s ^ { -1 } ( or 0.64 \pm 0.08 km s ^ { -1 } if two Gaussians are fitted ) , which implies a supervirial state , unless the gas contributes more to the gravitational potential than expected . No evidence is found for a dependence of this velocity dispersion on distance from the cluster center or stellar mass . We also find that stars with lower extinction ( in the front of the cloud ) tend to be redshifted compared with stars with somewhat higher extinction ( towards the back of the cloud ) . This data suggests that the stars in IC 348 are converging along the line of sight . We show that this correlation between radial velocity and extinction is unlikely to be spuriously caused by the small cluster rotation of 0.024 \pm 0.013 km s ^ { -1 } arcmin ^ { -1 } or by correlations between the radial velocities of neighboring stars . This signature , if confirmed , will be the first detection of line-of-sight convergence in a star cluster . Possible scenarios for reconciling this convergence with IC 348 ’ s observed supervirial state include : a ) the cluster is fluctuating around a new virial equilibrium after a recent disruption due to gas expulsion or a merger event , or b ) the population we identify as IC 348 results from the chance alignment of two sub-clusters converging along the line of sight . Additional measurements of tangential and radial velocities in IC 348 will be important for clarifying the dynamics of this region , and informing models of the formation and evolution of star clusters . The radial velocities analyzed in this paper have been made available online .