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We present the results of high-resolution spectroscopic observations carried out over three years aimed at estimating the short-period (P orb < 100 days) binary frequency of a sample of T Tauri stars in Oph-Sco, Cha, Lup, CrA star forming regions (SFRs), already observed with high angular resolution techniques by Ghez et al. (1993) and by Ghez et al. (1997) to detect wider components. When combining all four SFRs, the short-period binary frequency is indistinguishable from that found bydoi:10.1051/0004-6361:20031242 fatcat:eep75nrm55ex3ft3i2xnq56ro4