The IRIS network is now fourteen years old, and has continuously been taking data since 1989. The data analysis, which produced some noticeable scientifical results, like the measurement of the ell = 1 rotationnal splitting or the measurement of the solar acoustic cut-off frequency, was mainly performed with the summer campaigns data of 1989 to 1992. P-mode frequency and width tables were recently published using the same subset of the IRIS data . We are now finishing the calibration and the timing of the whole set of IRIS data from 89 to 97, which will increase by a factor of 4 the amount of available data. The duty cycle of the IRIS network ranges from about 65% over 3 months of the summer campaigns to some 23% over one year in the worst case. To improve our duty cycle we developed several collaborations with other teams running similar instruments: (1) the Mark I instrument, ran at the IAC for many years, a potassium resonance single pixel device, also part of the BiSON network (Elsworth et al., 1988). (2) Alexandro Cacciani's MOF, ran at the JPL in Pasadena. Although this is a sodium resonance imaging instrument, it has been used in ``one pixel'' format for several summer seasons since 1989 (Cacciani et al., 1984). (3) the LOWL instrument is a Doppler imager also based on a Magneto-Optical Filter (MOF), operated at the Mauna Loa solar observatory since 1994 (Tomczyk et al., 1995). The merging of those 'alien' data has been carefully adressed at the calibration ands timing stages, and we can now present the advantages of such a-posteriori collaborations. We endeavour to set-up the corresponding database of 'one-pixel seismological data from ground-based intruments' in Nice and to open it to the scientific community of this meeting by the end of 1998. This database will soon have the potential to trace the spectral features of the solar signal over one 11-years cycle.