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Isotopic fractionation is an important tool to investigate the chemicalhistory of our Solar System (SS). In particular, the isotopic fraction ofnitrogen (14N/15N) is lower in comets and other pristine SS bodies with respectto the value measured for the protosolar nebula, suggesting a local chemicalenrichment of 15N during the SS formation. Therefore, interferometric studiesof nitrogen fractionation in SS precursors are imperative for us to obtainclues about our astrochemical origins. In this work, we investigated thevariation of the 14N/15N ratio in one of the closest analogues of theenvironment in which the SS was born: the protocluster OMC-2 FIR4. We presentthe first comparison at high angular resolution between HCN and N2H+ usinginterferometric data. We analysed observations of the HCN isotopologues H13CNand HC15N in the OMC-2 FIR4 protocluster, specifically the transitions H13CN(1-0) and HC15N (1-0), from NOEMA within the context of the IRAM Seeds Of LifeIn Space Large Program. We combined our results with analysis of archival dataobtained with ALMA of N2H+ and its 15N isotopologues. Our results show a smallregional variation in the ratio for HCN from ~250 to 500. The ratios in thecentral regions of FIR4, where the candidate protostars are located, arelargely consistent (~300). They also show little variation from the part of theprotocluster known to harbour a high cosmic-ray ionisation rate, to the portionwith lower rate. We also found a small variation in the ratio of N2H+ acrossdifferent regions from ~200 to ~400. These results suggest that local changesin the physical parameters occurring on small linear scales probed by ourobservations do not seem to affect the 14N/15N ratio in either HCN or N2H+ andhence that this is independent of the molecule used. Moreover, the high levelof irradiation due to cosmic rays does not affect the N-fractionation either.

Seeds of Life in Space (SOLIS). XIII. Nitrogen fractionation towards the protocluster OMC-2 FIR4