N–Ne–Ar data for 14 grouped (IIAB-IIG, IID) and 14 ungrouped iron meteorites

This dataset accompanies the paper “Tracing early disk substructures and accretionary relationships through nitrogen isotopes in iron meteorites” by Evelyn Füri, Fridolin Spitzer, Julie Gamblin, Christoph Burkhardt, Béatrice Luais, Julien Boulliung, Laurent Zimmermann, submitted to Geochimica et Cosmochimica Acta.

Table 1 lists the iron meteorites analyzed in this study together with their Ni and Ge contents. These values were obtained from Astromat Synthesis (https://astromat.org) on June 5 2025, using the following parameters: Sample = Meteorite name; Chemical variables = Trace Element: (Ge, Ni).

Supplementary Table S1 reports the abundances and isotopic compositions of neon, argon, and nitrogen extracted by stepped laser heating from 14 grouped (IIAB-IIG, IID) and 14 ungrouped iron meteorites. Abbreviations: n.d. = not determined (accidentally pumped); b.d. = below detection (blank contribution ≥ 30 %).

Supplementary Table S2 summarizes the isotopic data (δ15N, Δ17O, ε50Ti, ε54Cr, µ54Fe, µ60Ni, µ64Ni, ε94Mo, Δ95Mo, ε100Ru) used for hierarchical clustering of outer-disk meteorite samples and their resulting cluster membership (see Fig. 6 of the paper). δ¹⁵N values are group averages or individual meteorite values; uncertainties are not reported as the values are not internally consistent.
Notes:
Wiley is officially classified as an IIC iron, but its Mo and W isotopic compositions are distinct from IIC irons (Worsham et al., EPSL, 2019).
Sombrerete is officially classified as an IAB iron (NC), but its isotopic characteristics assign it to the CC reservoir.
The NWA 6704 grouplet represents the mean of NWA 6704 and NWA 6926.
Data sources:
N in Ryugu samples (Nakamura et al., 2022; Naraoka et al., 2023; Oba et al., 2023; Gamblin et al., 2024) N in Bennu samples: Lauretta et al. (MAPS, 2024), Barnes et al. (Nat. Astron., 2025), Marty et al. (MAPS, 2025), Glavin et al. (Nat. Astron., 2025)
N in chondrites (Injerd and Kaplan, 1974; Kung and Clayton, 1978; Thiemens and Clayton, 1981; Robert and Epstein, 1982; Grady et al., 1983, 2002; Lewis et al., 1983; Kerridge, 1985; Sephton et al., 2003; Pearson et al., 2006; Alexander et al., 2012, 2013, 2018; Füri et al., 2013; Marrocchi et al., 2021; Hashizume et al., 2024; Patzek et al., 2025; Laize-Générat et al. 2024), Marrocchi et al., in revision))
N in iron meteorites (this study; Pepin and Becker, 1982; Prombo and Clayton, 1993; Grewal et al., Nat. Astron. 2021)
Ni (Spitzer et al., Sci. Adv. 2024, EPSL 2025)
Fe (Hopp et al., Sci. Adv. 2022; Anand et al., GCA 2024; Spitzer et al., EPSL 2025; Rego et al., 2025; Zhu et al., 2025)
Mo (Spitzer et al., GCA 2025)
Ru, Ti, Cr (Tissot et al., Space Sci. Rev. 2025)
O (Spitzer et al., EPSL 2025)