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A very reduced upper limit on the interstellar abundance of beryllium

We present the results of observations of the $λ3130.4$ Åinterstellar absorption line of Be II in the direction of zeta Per. The data were obtained at the Canada-France-Hawaii 3.6m Telescope using the Coudé f/4 Gecko spectrograph at a resolving power $\simeq 1.1 \times 10^5$, and a signal-to-noise ratio S/N $\simeq$ 2000. The Be II line is not detected, and we obtain an upper limit on the equivalent width $W_{3130.4}\leq30$ $μ$Å. This upper limit is 7 times below the lowest upper limit ever reported hitherto. The derived interstellar abundance is ($^9$Be/H) $\leq 7 \times 10^{-13}$, not corrected for the depletion of Be onto interstellar grains; it corresponds to an upper limit $δ_{Be} \leq -1.5$ dex on the depletion factor of Be. As such, it argues in favour of models of formation of dust grains in stellar atmospheres.