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The possible existence of intermediate mass binary black holes (IMBBHs) inglobular clusters (GCs) offers a unique geometry in which to detect space-timeoscillations. For certain pulsar-IMBBH configurations possible within a GC, theusual far-field plane wave approximation for the IMBBH metric perturbationseverely underestimates the magnitude of the induced pulsar pulsetime-of-arrival (TOA) fluctuations. In this letter, the expected TOAfluctuations induced by an IMBBH lying close to the line-of-sight between apulsar and the Earth are calculated for the first time. For an IMBBH consistingof 10 Msolar and 10^3 Msolar components, a 10 year orbital period, and located0.1 lyr from the Earth-Pulsar line of sight, the induced pulsar timing residualamplitude will be of order 5 to 500 ns.Comment: Accepted into ApJ Letters. This is a slightly augmented version  containing one extra figur

Pulsar Timing and the Detection of Black Hole Binary Systems in Globular Clusters