The Infrared Space Observatory (ISO) has detected water vapor in the stratospheres of the giant planets and Titan and CO2 on Jupiter, Saturn and Neptune (Feuchtgruber et al. 1997, 1999, Lellouch et al. 1997). The presence of the atmospheric cold trap implies an external origin for H2O (interplanetary dust (IDP), sputtering from the satellites and /or rings, large meteoritic impacts). In the case of Jupiter, the sources of water could either be IDP or the SL9 comet impacts (Moses et al. 2000, Lellouch et al. 2002). The H2O submillimetric line at 557 GHz on Jupiter was detected by the SWAS satellite in 1999 and 2001 (Bergin et al. 2000, Lellouch et al. 2002) and by the Odin space telescope in 2002 with a high signal to noise ratio. The vertical profile and the column density previously derived from the SWAS observations (Bergin et al. 2000) were different from the one obtained from ISO measurements (Lellouch et al. 2002). SWAS measurements favored an IDP source, whereas ISO observations favored a SL9 source. We have re-analyzed SWAS data with the same approach we had for Odin data (Cavalié et al. 2006). Both origins for water supply have been modeled with our time-dependant photochemical model (Ollivier et al. 2000, adapted for Jupiter). The origin of water vapor in the stratosphere of Jupiter as suggested by our results will be discussed. References : Feuchtgruber et al. (1997), Nature, 389, 159-162. Feuchtgruber et al. (1999), The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP, 427, 133. Lellouch et al. (1997), BAAS, 29, 992. Moses et al. (2000), Icarus, 145, 166-202. Lellouch et al. (2002), Icarus, 159, 112-131. Bergin et al. (2000), ApJ, 539, L147-L150. Ollivier et al. (2000), Plan. Space Sci., 48, 699-716. Cavalié et al. (2006), BAAS, 38, 497-498.< Leer menos