The possible detection of C 24 , a planar graphene, recently reported in several planetary nebulae by García-Hernández et al. (2011 inspires us to explore whether and how much graphene could exist in the interstellar medium (ISM) and how it would reveal its presence through its ultraviolet (UV) extinction and infrared (IR) emission. In principle, interstellar graphene could arise from the photochemical processing of polycyclic aromatic hydrocarbon (PAH) molecules which are abundant in the ISM through a complete loss of their hydrogen atoms, and/or from graphite which is thought to be a major dust species in the ISM through fragmentation caused by grain-grain collisional shattering. Both quantum-chemical computations and laboratory experiments have shown that the exciton-dominated electronic transitions in graphene cause a strong absorption band near 2755Å. We calculate the UV absorption of graphene and place an upper limit of ∼ 5 ppm of C/H (i.e., ∼ 1.9% of the total interstellar C) on the interstellar graphene abundance. We also model the stochastic heating of graphene C 24 in the ISM, excited by single starlight photons of the interstellar radiation field and calculate its IR emission spectra. We also derive the abundance of graphene in the ISM to be < 5 ppm of C/H by comparing the model emission spectra with that observed in the ISM.

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