Figure 2: Hydrogen isotope signatures for different objects in the Solar System.
The grey bar indicates the range of δD values predicted for the lunar interior based on the previous studies of water and its H-isotopic composition in lunar samples2,3,6,7,8. (a) The H-isotopic compositions of comets, where the data for comets 1P/Halley60, Hyakutake61, Hale-Bopp62, C/2002 T7 (ref. 63), C/2009 P1 (ref. 64), 8P/Tuttle65, and 153P/Ikeya-Zhang66, 45P/Honda-Mrkos-Pajdusakova57, 103P/Hartley 2 (ref. 56) and 67P/Churyumov-Gerasimenko58. (b) The average H-isotopic composition of apatite grains from eucrites47, and the range in values for interplanetary dust particles (IDPs)67,68. (c) The bulk H-isotope data for bulk Tagish Lake (TL) and other carbonaceous and ordinary chondrites (CC and OC, respectively)11,55, carbonaceous and ordinary chondrite hydroxyl and organic matter54. (d) Hydrogen isotope data for Enceladus69 and the jovian planets70,71,72. (e) The H-isotopic compositions of martian apatite73,74,75, martian melt inclusions46,74, martian meteorite groundmass46, martian atmosphere76 and martian crust and mantle46,73,74,75. (f) Data for lunar apatite5,6,7,8,33,41,77, lunar picritic glasses2,3 and lunar olivine-hosted melt-inclusions in picritic glass beads2. (g) The range in H-isotopic compositions of H2O on Earth12,13,78. (h) The H-isotopic composition of Proto-solar and interstellar medium42. For carbonaceous chondrites, CI-, CM-, CV-, CO- and CR- refer to the different groups, named according to one prominent meteorite of the group, respectively Ivuna, Mighei, Vigorano, Ornans and Renazzo. OC stands for ordinary chondrites. Error bars indicate measured analytical uncertainties, please see original references for more information (Encleadus, Jovian planets, and comets error bars, 1 s.d., and Eucrite data, 2 s.d.).
