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Context: The earliest stages of high-mass star formation are still poorlycharacterized. It is also unknown whether the initial conditions vary withenvironment. Aims: We want to investigate the youngest massive gas clumps inthe environment of extremely active star formation. Methods: We selected theIRDC18454 complex associated with the W43 Galactic mini-starburst, and observedit in the continuum emission between 70mu and 1.2mm, and in spectral lineemission of N2H+ and 13CO with single-dish instruments and an interferometer.Results: The multi-wavelength continuum study allows us to identify clumps thatare infrared dark even at 70mu and hence the best candidates to be genuinehigh-mass starless gas clumps. The spectral energy distributions revealelevated temperatures and luminosities compared to more quiescent environments.Furthermore, we identify a temperature gradient from the W43 mini-starbursttoward the starless clumps. We discuss whether the radiation impact of thenearby mini-starburst changes the fragmentation properties of the gas clumpsand by that maybe favors more high-mass star formation in such an environment.The spectral line data reveal two different velocity components of the gas at100 and 50km/s. While chance projection is a possibility to explain thesecomponents, the projected associations of the emission sources as well as theprominent location at the Galactic bar -- spiral arm interface also allow thepossibility that these two components may be spatially associated and eveninteracting. Conclusions: High-mass starless gas clumps can exist in the closeenvironment of very active star formation without being destroyed. The impactof the active star formation sites may even allow for more high-mass stars toform in these 2nd generation gas clumps.

The onset of high-mass star formation in the direct vicinity of the galactic mini-starburst W43