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The stellar content of the intracluster light (ICL) provides unique insightinto the hierarchical assembly process of galaxy clusters.However, the ICL isdifficult to study due to its low surface brightness and large physical extent.We present optical spectra of three ICL regions in the Coma cluster, locatedbetween 100-180kpc from their nearest BCGs: NGC4889 and NGC4874. The meansurface brightness of the three ICL regions are {\mu}$_g$~25.3-26.2magarcsec$^{-2}$. IFU spectroscopy with 13.5 hr on-source integration time wereacquired as part of an ancillary program within the SDSS-IV MaNGA survey. Westacked the 127 individual fiber spectra in each IFU in order to achieve a1{\sigma} limiting surface brightness of 27.9mag arcsec$^{-2}$, correspondingto a mean S/N in the optical of 21.6,9.6,and 11.6\AA$^{-1}$. We apply stellarpopulation models to the stacked spectra, and measure the recession velocities,velocity dispersions ($\sigma$), stellar ages, and [Fe/H]. Our results showthat the $\sigma$ of ICL regions are very high, indicating the stars aretracing the gravitational potential of the cluster, instead of any individualgalaxy. The line-of-sight velocities of the three ICL regions are differentfrom each other by ~700km/s, while the velocity of each region is similar tothe closest BCG. This suggests that the ICL regions are associated with twodistinct subclusters centered on NGC4889 and NGC4874.The stellar populations ofthese regions are old and metal poor, with ages of 7-12Gyr, and [Fe/H] of -0.8to -0.6 dex. From the derived age and [Fe/H], the build-up of ICL in Coma islikely to be through the accretion of low mass galaxies or the tidal strippingof the outskirts of massive galaxies that have ended their star formation earlyon, instead of directly from major mergers of massive galaxies.

Spectroscopic Constraints on the Build-up of the Intracluster Light in the Coma Cluster