By using accelerator mass spectrometry, we measured 10 Be (T 1/2 =1.5Ma) concentrations in nine Ivory Coast (IVC) tektites, in six soil samples collected near the Bosumtwi impact crater, the likely source region, and in a depth profile taken through a 23g moldavite. In the core of the moldavite sample we also measured an upper limit on the 36 Cl (T 1/2 =0.3My) concentration. The average 10 Be concentration in IVC tektites of (22±11)×10 6 atom/g exceeds reasonable limits for a meteoritic component or cosmic-ray production in situ after tektite formation. The 10 Be must be meteoric, which implies that IVC tektites formed from soils or sediments. Corrected to the time of formation (ToF) 1.07Ma ago and for a small in situ component, the average 10 Be concentration of (35±7)×10 6 atom/g (1−σ mean) is considerably lower than those of contemporary Bosumtwi soils, ∼250×10 6 atom/g, or of Australasian tektites at their ToF, 0.8Ma B.P. near Lake Bosumtwi today the soil column is only ∼1m thick. If the landscape was similar 1.07Ma ago, then the total thickness of the tektite formation zone probably did not exceed 10m. With increasing depth below the surface of the moldavite, the 10 Be concentrations decrease rapidly owing to the presence of a surface component, probably of recent origin. The main interior mass of the sample contains ∼0.8×10 6 atom 10 Be/g and fewer than 0.1×10 6 atom 36 Cl/g, little of which can be meteoritic. Although not definitive, consideration of several possible cosmic-ray exposure histories suggests that about half the interior 10 Be has a meteoric origin, which if corrected to the time of formation yields a concentration compatible with those measured in typical contemporary soils. The observations are consistent with the formation of three of the four main tektite groups from surface soils or sediments.