Table A.1.
Selected meteorites used in this study reported with their spectral reference (in the last column).
| Meteorite names | Meteorite types | H content ± H error (wt.%) | ESPAT | NOPL | λ continuum | Spectral reference |
|---|---|---|---|---|---|---|
| (Reference) | (normalized unit) | (normalized unit) | (μm) | |||
| ALH83100 | CM1/2 | 1.353 ± 0.009 (a) | 0.644 | 0.477 | 2.64–3.34 | Garenne et al. (2016) |
| ALH83100 | CM1/2 | 1.353 ± 0.009 (a) | 0.559 | 0.416 | 2.64–3.33 | Potin et al. (2019) |
| ALH84029 | CM1/2 | 1.260 ± 0.009 (a) | 0.694 | 0.488 | 2.64–3.32 | Garenne et al. (2016) |
| ALH84033 | Heated CM | 0.610 ± 0.018 (a) | 0.160 | 0.205 | 2.66–3.34 | Garenne et al. (2016) |
| ALH84044 | CM1/2 | 1.240 ± 0.008 (a) | 0.427 | 0.394 | 2.66–3.32 | Garenne et al. (2016) |
| Allende | CV3 | 0.09 ± 0.000 (a) | 0.120 | 0.143 | 2.66–3.30 | Takir et al. (2019) |
| Banten | CM2 | 0.910 ± 0.01 (a) | 0.045 | 0.064 | 2.68–3.34 | Takir et al. (2019) |
| Cold Bokkeveld | CM2 | 1.220 ± 0.004 (a) | 0.302 | 0.264 | 2.63–3.30 | Takir et al. (2013) |
| DOM03183 | Heated CM | 0.950 ± 0.001 (a) | 0.196 | 0.212 | 2.62–3.32 | Garenne et al. (2016) |
| DOM08003 | CM2 | 1.359 ± 0.006 (a) | 0.538 | 0.403 | 2.62–3.32 | Potin et al. (2019) |
| EET83355 | Heated CM | 0.410 ± 0.001 (a) | 0.110 | 0.144 | 2.64–3.32 | Garenne et al. (2016) |
| EET96029 | Heated CM | 0.728 ± 0.012 (a) | 0.197 | 0.239 | 2.66–3.34 | Garenne et al. (2016) |
| EET96029 | Heated CM | 0.728 ± 0.012 (a) | 0.099 | 0.106 | 2.63–3.34 | Potin et al. (2019) |
| Essebi | CM2? | 0.770 ± 0.005 (a) | 0.254 | 0.243 | 2.66–3.31 | Takir et al. (2019) |
| GRA06100 | Heated CR | 0.13 ± 0.003 (a) | 0.085 | 0.124 | 2.66–3.32 | Garenne et al. (2016) |
| Ivuna | CI1 | 1.330 ± 0.094 (a) | 0.551 | 0.394 | 2.60–3.25 | Takir et al. (2013) |
| LAP02277 | Heated CM | 1.112 ± 0.009 (a) | 0.393 | 0.317 | 2.66–3.10 | Takir et al. (2013) |
| LAP02333 | CM2 | 1.020 ± 0.005 (a) | 0.186 | 0.220 | 2.66–3.32 | Garenne et al. (2016) |
| LAP02336 | CM2 | 0.950 ± 0.005 (a) | 0.226 | 0.251 | 2.64–3.34 | Garenne et al. (2016) |
| LEW87022 | CM2 | 1.090 ± 0.014 (a) | 0.293 | 0.295 | 2.64–3.32 | Garenne et al. (2016) |
| LEW90500 | CM2 | 0.990 ± 0.005 (a) | 0.403 | 0.361 | 2.62–3.34 | Garenne et al. (2016) |
| MAC88100 | Heated CM | 0.894 ± 0.010 (a) | 0.321 | 0.281 | 2.64–3.34 | Potin et al. (2019) |
| MET01070 | CM1 | 1.274 ± 0.000 (a) | 0.535 | 0.405 | 2.64–3.32 | Garenne et al. (2016) |
| MET01070 | CM1 | 1.274 ± 0.000 (a) | 0.333 | 0.280 | 2.64–3.34 | Potin et al. (2019) |
| Mighei | CM2 | 0.994 ± 0.003 (a) | 0.220 | 0.240 | 2.66–3.33 | G. Poggiali, (priv. comm.) |
| MIL07700 | Heated CM | 0.570 ± 0.016 (a) | 0.236 | 0.251 | 2.64–3.33 | Garenne et al. (2016) |
| MIL07700 | Heated CM | 0.570 ± 0.016 (a) | 0.091 | 0.096 | 2.65–3.33 | Potin et al. (2019) |
| MIL07700 | Heated CM | 0.570 ± 0.016 (a) | 0.011 | 0.013 | 2.71–3.10 | Takir et al. (2013) |
| Murchison | CM2 | 0.956 ± 0.002 (a) | 0.117 | 0.130 | 2.65–3.32 | Potin et al. (2019) |
| Murchison | CM2 | 0.956 ± 0.002 (a) | 0.357 | 0.287 | 2.62–3.34 | Takir et al. (2019) |
| Orgueil BM | CI1 | 1.366 ± 0.015 (a) | 0.547 | 0.399 | 2.66–3.33 | Potin et al. (2019) |
| Orgueil Smith. | CI1 | 1.346 ± 0.019 (a) | 0.547 | 0.399 | 2.66–3.33 | Potin et al. (2019) |
| Orgueil BM | CI1 | 1.366 ± 0.015 (a) | 0.532 | 0.395 | 2.64–3.33 | Takir et al. (2019) |
| Orgueil Smith. | CI1 | 1.346 ± 0.019 (a) | 0.532 | 0.395 | 2.64–3.33 | Takir et al. (2019) |
| QUE97990 | CM2 | 0.959 ± 0.000 (a) | 0.066 | 0.077 | 2.67–3.33 | Potin et al. (2019) |
| QUE97990 | CM2 | 0.959 ± 0.000 (a) | 0.148 | 0.159 | 2.60–3.34 | Takir et al. (2013) |
| QUE99038 | CV | 0.06 ± 0.001 (a) | 0.006 | 0.009 | 2.71–3.14 | Takir et al. (2013) |
| RBT04133 | CR | 0.26 ± 0.001 (a) | 0.106 | 0.151 | 2.64–3.32 | Garenne et al. (2016) |
| TL4 | C2 | 0.72 ± 0.000 (c) | 0.098 | 0.101 | 2.65–3.31 | Potin et al. (2019) |
| TL5b | C2 | 0.72 ± 0.003 (a) | 0.229 | 0.199 | 2.60–3.30 | Takir et al. (2019) |
| TL11 | C2 | 0.642 ± 0.004 (a) | 0.229 | 0.199 | 2.60–3.30 | Takir et al. (2019) |
| WIS91600 | Heated CM | 0.878 ± 0.000 (b) | 0.239 | 0.248 | 2.64–3.30 | Garenne et al. (2016) |
| WIS91600 | Heated CM | 0.878 ± 0.000 (b) | 0.066 | 0.070 | 2.65–3.30 | Potin et al. (2019) |
Notes. The H content is from (a) Alexander et al. (2012, 2013), (b) Garenne et al. (2016), and (c): Gilmour et al. (2019). Their ESPAT and NOPL values, both calculated at the wavelength center of 2.72 μm, are reported, as are the used continuum anchor point wavelengths (λ). As for grain size information, the spectra from Takir et al. 2013, 2019 were taken from a meteorite sample ground into 100 μm powder, with no grain size distribution determined due to meteorite sample scarcity. The meteorite reflectance spectra from Potin et al. (2019) and Garenne et al. (2016) were measured on manually ground, non-sieved samples to retain a large grain size distribution. Finally, the Mighei spectrum was measured at INAF-Astrophysical Observatory of Arcetri in Firenze (Italy) on a powder sample with grain size < 500 μm (Poggiali, priv. comm.).
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