Table 1 Deoxysugar derivatives identified in the ice photolysis residues (regular and 13C-labeled)

From: Deoxyribose and deoxysugar derivatives from photoprocessed astrophysical ice analogues and comparison to meteorites

Compoundsa

Formulas

Rt (min)b

Abundances in residuesc (pmol)

Detected in meteorites?

Deoxysugars

 2-Deoxyribose

C5H10O4

61.2, 61.4

217–3855

Undeterminedk

 2-Deoxyxylosed

C5H10O4

57.0, 57.3

373–3636e

Undeterminedk

Deoxysugar alcohols

 1,2-Propanediolf

C3H8O2

9.9

≥8–375

Yesl,m

 1,3-Propanediolf,g

C3H8O2

36.9

≥19–27

No

 2-Methyl-1,3-propanediolg,h

C4H10O2

38.7

≤1038–3354h

No

 2-(Hydroxymethyl)-1,3-propanediol

C4H10O3

30.9

n.d.

Yesl

 1,2,3-Butanetriol

C4H10O3

14.5

6–39

No

 1,2,4-Butanetriol

C4H10O3

32.2

35–50

Yesl

Deoxysugar acids

 3,4-Dihydroxybutyric acidi,j

C4H8O4

16.5

Yesn

Sugars

 Ribose

C5H10O5

64.7, 65.0

237–2467

No

  1. n.d., Not detected
  2. aCompounds were detected using the (+)-2-butanol/TFAA derivatization method, unless otherwise stated
  3. bRetention times (Rt) correspond to average values in the GC-MS chromatograms of the residues, or to standard chromatograms if compounds were not detected in the residues. Chiral compounds whose enantiomers are separated have two retention times
  4. cAbundances for chiral compounds correspond to the sum for both enantiomers
  5. dTentatively identified by comparison of its mass spectrum with that of the 2-deoxyribose standard (see Fig. 1 and Supplementary Fig. 3)
  6. eAbundances estimated based on the GC-MS detector response for the 2-deoxyribose standard
  7. fVolatile compounds that may have been partially lost during the warm-up phase and/or the sample preparation. Abundances given thus correspond to lower limits
  8. gDetected in samples derivatized with the MTBSTFA method
  9. hElutes with another unidentified compound with similar mass fragments, so abundances given are upper limits
  10. iTentatively identified by comparison with the NIST mass spectrometry library in samples derivatized with the BSTFA method
  11. jMay be present in its dimer form
  12. kThe presence of these compounds in meteorites is uncertain, and further analyses are required
  13. lDetected in Murchison (Fig. 4)
  14. mDetected in GRA 06100 (Fig. 4)
  15. nDetected in Murchison and Murray4