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The composition of a forming planet is set by the material it accretes fromits parent protoplanetary disk. Therefore, it is crucial to map the chemicalmake-up of the gas in disks to understand the chemical environment of planetformation. This paper presents molecular line observations taken with theAtacama Large Millimeter/submillimeter Array of the planet-hosting disk aroundthe young star HD 169142. We detect N2H+, CH3OH, [CI], DCN, CS, C34S, 13CS,H2CS, H2CO, HC3N and c-C3H2 in this system for the first time. Combining thesedata with the recent detection of SO and previously published DCO+ data, weestimate the location of H2O and CO snowlines and investigate radial variationsin the gas phase C/O ratio. We find that the HD 169142 disk has a relativelylow N2H+ flux compared to the disks around Herbig stars HD 163296 and MWC 480indicating less CO freeze-out and place the CO snowline beyond the millimetredisk at ~150 au. The detection of CH3OH from the inner disk is consistent withthe H2O snowline being located at the edge of the central dust cavity at ~20au. The radially varying CS/SO ratio across the proposed H2O snowline locationis consistent with this interpretation. Additionally, the detection of CH3OH insuch a warm disk adds to the growing evidence supporting the inheritance ofcomplex ices in disks from the earlier, colder stages of star formation.Finally, we propose that the giant HD 169142 b located at 37 au is formingbetween the CO2 and H2O snowlines where the local elemental make of the gas isexpected to have C/O=1.0.

Tracing snowlines and C/O ratio in a planet-hosting disk: ALMA molecular line observations towards the HD169142 disk