Abstract Old and recent puzzles of GRBs and SGRs find a solution with a model based on the fast blazing of very collimated thin gamma Jets. Damped oscillating afterglows in GRB 030329 find a natural explanation assuming a very thin Jet - &frac;{ΔΩ}{Ω}≤ 10-8 - whose persistent activity and different angle of view maybe combined at once with the Supernovæ power and the apparent huge GRBs output: ˙{E}GRBs ≃ ˙{E}SN&frac;{Ω}{ΔΩ}. This leads to a better understanding of the remarkable GRB-Supernovæ connection discovered in the GRB 980425/SN 1998bw and in the most recent GRB 030329/SN 2003dh events. The same thin beaming offer an understanding of the apparent SGR-Pulsar power connection: ˙{E}SGRs ≃ ˙{E}Xpuls&frac;{Ω}{ΔΩ}. A thin collimated precessing Gamma Jet model for both GRBs and SGRs, at their different scaled luminosity ( 1038-1044 erg s-1), explains the existence of few identical energy spectra and time evolution of these sources leading to a unified model. Their similarity with the huge precessing Jets in AGN, QSRs and Radio-Galaxies inspires this smaller scale SGR-GRB model. The spinning-precessing Jet explains the rare (≈ 6\%) mysterious X-Ray precursors in GRBs and SGRs events. Any large Gamma Jet off-axis beaming to the observer might lead to the X-Flash events without any GRB signals, as the most recent XRF 030723. Its possible re-brightening would confirm the evidence of the variable pointing of the jet in or off line towards the observer. Indeed a multi-precessing Jet at peak activity in all bands may explain the puzzling X or optical re-brightening bumps found in the GRB 021004, GRB 030329 and the SGR 1900+ 14 on 27 August 1998 and once again on the 18 April 2001. Rarest micro-quasars neutron star in our galaxy as SS433, and Herbig Haro objects and Cir-X-1 describe these thin precessing Jet imprints in the spectacular shapes of their relic nebulae.

Keywords gamma-rays burst, SGR

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