{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,9,24]],"date-time":"2026-09-24T20:19:46Z","timestamp":1790281186267,"version":"4.1.0"},"reference-count":33,"publisher":"American Association for the Advancement of Science (AAAS)","issue":"5329","content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Science"],"published-print":{"date-parts":[[1997,8,22]]},"abstract":"<jats:p>Intramolecular carbon, hydrogen, and sulfur isotope ratios were measured on a homologous series of organic sulfonic acids discovered in the Murchison meteorite. Mass-independent sulfur isotope fractionations were observed along with high deuterium\/hydrogen ratios. The deuterium enrichments indicate formation of the hydrocarbon portion of these compounds in a low-temperature environment that is consistent with that of interstellar clouds. Sulfur-33 enrichments observed in methanesulfonic acid could have resulted from gas-phase ultraviolet irradiation of a precursor, carbon disulfide. The source of the sulfonic acid precursors may have been the reactive interstellar molecule carbon monosulfide.<\/jats:p>","DOI":"10.1126\/science.277.5329.1072","type":"journal-article","created":{"date-parts":[[2002,7,27]],"date-time":"2002-07-27T09:44:47Z","timestamp":1027763087000},"page":"1072-1074","source":"Crossref","is-referenced-by-count":83,"title":["Sulfur and Hydrogen Isotope Anomalies in Meteorite Sulfonic Acids"],"prefix":"10.1126","volume":"277","author":[{"given":"George W.","family":"Cooper","sequence":"first","affiliation":[{"name":"G. W. Cooper, SETI Institute and NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"S. Chang, NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"M. H. Thiemens and T. L. Jackson, Department of Chemistry and Biochemistry, University of California, San Diego, La Jolla, CA 92093\u20130356, USA."}],"role":[{"vocabulary":"crossref","role":"author"}]},{"given":"Mark H.","family":"Thiemens","sequence":"additional","affiliation":[{"name":"G. W. Cooper, SETI Institute and NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"S. Chang, NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"M. H. Thiemens and T. L. Jackson, Department of Chemistry and Biochemistry, University of California, San Diego, La Jolla, CA 92093\u20130356, USA."}],"role":[{"vocabulary":"crossref","role":"author"}]},{"given":"Teresa L.","family":"Jackson","sequence":"additional","affiliation":[{"name":"G. W. Cooper, SETI Institute and NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"S. Chang, NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"M. H. Thiemens and T. L. Jackson, Department of Chemistry and Biochemistry, University of California, San Diego, La Jolla, CA 92093\u20130356, USA."}],"role":[{"vocabulary":"crossref","role":"author"}]},{"given":"Sherwood","family":"Chang","sequence":"additional","affiliation":[{"name":"G. W. Cooper, SETI Institute and NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"S. Chang, NASA Ames Research Center, MS 239-4, Moffett Field, CA 94035, USA."},{"name":"M. H. Thiemens and T. L. Jackson, Department of Chemistry and Biochemistry, University of California, San Diego, La Jolla, CA 92093\u20130356, USA."}],"role":[{"vocabulary":"crossref","role":"author"}]}],"member":"221","reference":[{"key":"e_1_3_1_2_2","unstructured":"J. R. Cronin and S. Chang in Chemistry of Life's Origins J. M. Greenberg V. Pirronello C. Mendoza-Gomez Eds. (Kluwer Dordrecht Netherlands 1993) pp. 209\u2013258."},{"key":"e_1_3_1_3_2","unstructured":"E. F. Van Dishoeck G. A. Blake B. T. Draine J. I. Lunine in Protostars and Planets III E. H. Levy and J. I. Lunine Eds. (Univ. of Arizona Tucson AZ 1993) pp. 163\u2013241."},{"key":"e_1_3_1_4_2","doi-asserted-by":"crossref","first-page":"1543","DOI":"10.1016\/0016-7037(80)90118-0","volume":"44","author":"Bunch T. E.","year":"1980","unstructured":"Bunch T. E., Chang S., Geochim. Cosmochim. Acta 44, 1543 (1980).","journal-title":"Geochim. Cosmochim. Acta"},{"key":"e_1_3_1_5_2","first-page":"4109","volume":"56","author":"Cooper G. W.","year":"1992","unstructured":"Cooper G. W., Onwo W. M., Cronin J. R., ibid. 56, 4109 (1992).","journal-title":"ibid."},{"key":"e_1_3_1_6_2","unstructured":"Also see (6). The stable isotopes of S have masses of 32 (95.02%) 33 (0.75%) 34 (4.21%) and 36 (0.02%) atomic mass units (amu). The deviation of the ratio of S isotopes in a sample from the standard (S in the Canyon Diablo iron meteorite) is given in parts per thousand or per mil which is defined as \u03b4 x S = {[( x S\/ 32 S) sample \/( x S\/ 32 S) standard ] \u2212 1} \u00d7 1000 where x = 33 34 or 36. If plotted on a three-isotope graph normal mass-dependent fractionations should lie on the line \u03b4 33 S = 0.5 \u03b4 34 S because the difference between 33 S and 32 S is 1 amu and the difference between 34 S and 32 S is 2 amu which gives 0.5 as the slope. Similarly \u03b4 36 S = 1.97 \u03b4 34 S. Therefore any mass-independent isotopic anomaly in 33 S and 36 S is given by (in per mil) 33 \u0394 = \u03b4 33 S \u2212 0.5 \u03b4 34 S and 36 \u0394 = \u03b4 36 S \u2212 1.97 \u03b4 34 S respectively. All known terrestrial S lies on normal mass-dependent fractionation lines. The calculation of \u03b4 values for C and H is similar to that of S that is \u03b4H = {[( H\/L ) sample \/( H\/L ) standard ]\u22121} \u00d7 1000 where H and L are the heavy and light isotopes respectively of each element."},{"key":"e_1_3_1_7_2","doi-asserted-by":"publisher","DOI":"10.1016\/0016-7037(91)90381-E"},{"key":"e_1_3_1_8_2","first-page":"1405","author":"Thiemens M. H.","year":"1995","unstructured":"Thiemens M. H., Jackson T., Lunar Planet. Sci. XXVI, 1405 (1995).","journal-title":"Lunar Planet. Sci."},{"key":"e_1_3_1_9_2","first-page":"540","volume":"29","author":"Thiemens M. H.","year":"1994","unstructured":"Thiemens M. H., et al., Meteoritics 29, 540 (1994).","journal-title":"Meteoritics"},{"key":"e_1_3_1_10_2","doi-asserted-by":"publisher","DOI":"10.1016\/0016-7037(95)00018-6"},{"key":"e_1_3_1_11_2","unstructured":"The fraction containing the sulfonics and phosphonics (9) was then injected into a Dionex (Sunnyvale CA) ion chromatograph (IC) equipped with two 9 mm by 250 mm Dionex AS4-A columns and eluted with a carbonate buffer 1.8 mM Na 2 CO 3 + 1.7 mM NaHCO 3 (4 ml\/min) to collect sulfonics and phosphonics as separate groups. At this step nPSA separates sufficiently from the other sulfonics for collection. To collect the remaining sulfonics individually we then reinjected the sulfonics into the IC which was equipped with a 10 m by 100 mm Phenomenex (Torrance CA) star-ion anion exchange column and eluted them with a 5.4 mM Na 2 CO 3 + 5.1 mM NaHCO 3 buffer. We separated ESA from a small amount of co-eluting sulfate by reinjecting the two compounds and eluting them with a 3.2 mM Na 2 CO 3 + 3.1 NaHCO 3 mM buffer. Baseline separation between MSA and ESA\/sulfate was \u223c2 min; between ESA\/sulfate and iPSA it was \u223c9 min and between ESA and sulfate it was \u223c1 min. After removal of the carbonate buffer with HCl each compound was then placed in a quartz tube and dried by rotary evaporation (maximum temperature \u223c 50\u00b0C). Copper oxide was then placed in each tube and high vacuum with mild warming (<100\u00b0C) was used for complete drying. The samples were then sealed and combusted to sulfate CO 2 and H 2 O at 800\u00b0C. The CO 2 and H 2 O were collected with a procedure similar to that of Epstein et al. (13). The H 2 O was converted to H by the method of Coleman and Moore (27) with a zinc catalyze from J. M. Hayes of Indiana University. The CO 2 and H were then analyzed with 6-60-Nuclide and 3-60-HD-Nuclide mass spectrometers. The sulfate was extracted from each tube with hydrochloric acid and prepared for S isotopic analysis as in (6)."},{"key":"e_1_3_1_12_2","doi-asserted-by":"crossref","first-page":"3159","DOI":"10.1016\/0016-7037(93)90300-L","volume":"57","author":"Gao X.","year":"1993","unstructured":"Gao X., Thiemens M. H., Geochim. Cosmochim. Acta 57, 3159 (1993).","journal-title":"Geochim. Cosmochim. Acta"},{"key":"e_1_3_1_13_2","doi-asserted-by":"crossref","first-page":"252","DOI":"10.1038\/307252a0","volume":"307","author":"Yuen G.","year":"1984","unstructured":"Yuen G., Blair N., Des Marais D. J., Chang S., Nature 307, 252 (1984).","journal-title":"Nature"},{"key":"e_1_3_1_14_2","first-page":"477","volume":"326","author":"Epstein S.","year":"1987","unstructured":"Epstein S., Krishnamurthy R. V., Cronin J. R., Pizzarello S., Yuen G. U., ibid. 326, 477 (1987).","journal-title":"ibid."},{"key":"e_1_3_1_15_2","doi-asserted-by":"publisher","DOI":"10.1126\/science.273.5276.774"},{"key":"e_1_3_1_16_2","doi-asserted-by":"publisher","DOI":"10.1029\/93GL01080"},{"key":"e_1_3_1_17_2","doi-asserted-by":"publisher","DOI":"10.1063\/1.450373"},{"key":"e_1_3_1_18_2","unstructured":"X. Xu and M. H. Thiemens unpublished data."},{"key":"e_1_3_1_19_2","doi-asserted-by":"crossref","first-page":"391","DOI":"10.1021\/cr00084a003","volume":"88","author":"Moltzen E.","year":"1988","unstructured":"Moltzen E., Klabunde K. J., Senning A., Chem. Rev. 88, 391 (1988);","journal-title":"Chem. Rev."},{"key":"e_1_3_1_19_3","unstructured":". In most of the literature this solid phase is referred to as a \u201cCS polymer \u201d and we will use the terms polymer and polymerization for convenience. In the laboratory this polymerization is highly exothermic. The heat of formation (\u0394H f ) values in the range of \u221250 kcal\/mol of CS have been estimated for the formation of CS polymers."},{"key":"e_1_3_1_20_2","doi-asserted-by":"crossref","unstructured":"K. J. Klabunde E. Moltzen K. Voska Phosphorus Sulfur Silica Relat. Elem. 43 47 (1989).","DOI":"10.1080\/10426508908040278"},{"key":"e_1_3_1_21_2","doi-asserted-by":"crossref","first-page":"6452","DOI":"10.1021\/ja00042a024","volume":"114","author":"Bohn R. B.","year":"1992","unstructured":"Bohn R. B., Hannachi Y., Andrews L., J. Am. Chem. Soc. 114, 6452 (1992).","journal-title":"J. Am. Chem. Soc."},{"key":"e_1_3_1_22_2","unstructured":"C. M. White thesis University of North Dakota Grand Forks (1974)."},{"key":"e_1_3_1_23_2","first-page":"4196","volume":"158","author":"Hogg M. A. P.","year":"1958","unstructured":"Hogg M. A. P., Spice J. E., J. Chem. Soc. 158, 4196 (1958).","journal-title":"J. Chem. Soc."},{"key":"e_1_3_1_24_2","doi-asserted-by":"crossref","first-page":"1886","DOI":"10.1139\/v65-249","volume":"43","author":"De Sorgo M.","year":"1965","unstructured":"De Sorgo M., Yarwood A. J., Strausz O. P., Gunning H. E., Can. J. Chem. 43, 1886 (1965).","journal-title":"Can. J. Chem."},{"key":"e_1_3_1_25_2","unstructured":"Some reported CS reaction products are CS 2 C 2 S C 2 S 2 C 3 S C 3 S 2 CO CO 2 OCS S S 2 SO and SO 2 . On the basis of infrared observations of low-temperature (solid phase) CS reactions Steudel (28) suggested a reaction sequence where molecules of increasing carbon number are formed leading to a polymer: x CS \u2192 CS 2 CCS C 3 S 2 C y S z \u2192 polymer. Of the above molecules C x S 2 and S 2 (if searched for) have not been reported to occur in the interstellar medium. In addition to CS 2 (see text) OCS and S x are also observed in carbonaceous meteorites (25 26)."},{"key":"e_1_3_1_26_2","doi-asserted-by":"crossref","first-page":"239","DOI":"10.1016\/S0016-7037(68)80006-7","volume":"32","author":"Hayes J. M.","year":"1968","unstructured":"Hayes J. M., Biemann K., Geochim. Cosmochim. Acta 32, 239 (1968);","journal-title":"Geochim. Cosmochim. Acta"},{"key":"e_1_3_1_26_3","unstructured":". In the experiments core samples of the meteorites were placed directly in the inlet of the mass spectrometer. For the identification of ions C 2 S C 3 S and C 3 SO a sample was heated only between 25\u00b0 and 100\u00b0C for a total of 5 min. The authors give reasons as to why this temperature and time range is not severe enough to produce S compounds by decomposition of S and organics. In the case of C 3 S 2 heating was between 160\u00b0 and 200\u00b0C for 5 min. No theory of how such reactive compounds could have survived in the meteorite for billions of years was offered. However if the compounds were indigenous and of the same structure as the CS condensation products (and the identified interstellar molecules) they would seem to require a special carrier in the meteorite matrix perhaps a carbon phase such as one produced from polymerization of CS or other reactive molecules (or both)."},{"key":"e_1_3_1_27_2","first-page":"189","volume":"36","author":"Studier M. H.","year":"1972","unstructured":"Studier M. H., Hayatsu R., Anders E., ibid. 36, 189 (1972).","journal-title":"ibid."},{"key":"e_1_3_1_28_2","doi-asserted-by":"crossref","first-page":"1594","DOI":"10.1021\/ac50033a056","volume":"50","author":"Coleman M. L.","year":"1978","unstructured":"Coleman M. L., Moore M. P., Anal. Chem. 50, 1594 (1978).","journal-title":"Anal. Chem."},{"key":"e_1_3_1_29_2","doi-asserted-by":"crossref","unstructured":"R. Steudel Z. Naturforsch. Teil B. 218 1106 (1966).","DOI":"10.1515\/znb-1966-1123"},{"key":"e_1_3_1_30_2","first-page":"500","volume":"30","author":"Cooper G. W.","year":"1995","unstructured":"Cooper G. W., Thiemens M. H., Jackson T. L., Chang S., Meteoritics 30, 500 (1995).","journal-title":"Meteoritics"},{"key":"e_1_3_1_31_2","first-page":"281","author":"Cooper G. W.","year":"1995","unstructured":"Cooper G. W., Chang S., Lunar Planet. Sci. XXVI, 281 (1995).","journal-title":"Lunar Planet. Sci."},{"key":"e_1_3_1_32_2","unstructured":"We thank C. Moore (Arizona State University Center for Meteorite Studies) for the sample of the Murchison meteorite; A. Tharpe for carbon isotope measurements; K. Klabunde and S. Charnley for helpful conversation; and V. Morris N. Lerner D. Des Marais K. Zahnle and L. Allamandola for comments on the manuscript. Supported by NASA grant NAGW 3551 and the Exobiology and Cosmochemistry Programs of NASA."}],"container-title":["Science"],"original-title":[],"language":"en","link":[{"URL":"https:\/\/www.science.org\/doi\/pdf\/10.1126\/science.277.5329.1072","content-type":"unspecified","content-version":"vor","intended-application":"similarity-checking"}],"deposited":{"date-parts":[[2024,1,13]],"date-time":"2024-01-13T03:23:12Z","timestamp":1705116192000},"score":1,"resource":{"primary":{"URL":"https:\/\/www.science.org\/doi\/10.1126\/science.277.5329.1072"}},"subtitle":[],"short-title":[],"issued":{"date-parts":[[1997,8,22]]},"references-count":33,"journal-issue":{"issue":"5329","published-print":{"date-parts":[[1997,8,22]]}},"alternative-id":["10.1126\/science.277.5329.1072"],"URL":"https:\/\/doi.org\/10.1126\/science.277.5329.1072","relation":{},"ISSN":["0036-8075","1095-9203"],"issn-type":[{"value":"0036-8075","type":"print"},{"value":"1095-9203","type":"electronic"}],"subject":[],"published":{"date-parts":[[1997,8,22]]}}}