1. Sébastien Muller (ASIAA, Taiwan) M. Guélin (IRAM) M. Dumke (ESO) R. Lucas (IRAM) Probing isotopic ratios at z=0.89 Molecular line absorptions in front of the quasar PKS 1830-211 IAU Colloquium 199 Probing galaxies through quasar absorption lines, ShangHai, China, 2005 March 14-19

2. Absorption systems - Lyman  forest  gas filaments in extragalactic medium 10 12 - 10 19 cm -2 - Damped Lyman  & HI 21 cm absorption  outer parts of spiral galaxies 10 19 - 10 21 cm -2 - Molecular absorption  central parts of galaxies 10 20 - 10 24 cm -2

3. Background quasars & molecular absorption Need a background continuum source …  mm flux of quasars weaker than in the radio cm (SNR depending on the background continuum source) And an absorption system !  Dense gas, closer to the center of the intervening galaxy (small impact parameter)  Highly probable association with gravitational lensing

4. Molecular absorption systems in the mm Z abs N H 2 (cm -2 ) Cen A0.0022. 10 20 Host galaxy 3C2930.04> 6. 10 20 Host galaxy PKS 1413+1350.255. 10 20 Host galaxy B3 1504+3770.671.2 10 21 Host galaxy B 0218+3570.684. 10 23 Background QSR PKS 1830-2110.894. 10 22 Background QSR

5. HST WFPC2 I band image NE SW MERLIN 6cm 2–4 kpc Intervening galaxy : z=0.89 Typical spiral Photometry from HST (Winn et al 2002) I = 22 V > 24.7 SW position I > 24.9 V > 26.3 1st case of QSR lensed by a face-on spiral Mass within 3 kpc: (Wiklind & Combes 1998) 6 – 9 10 10 M  1’’ PKS 1830-211 Patnaik et al 1994

6. Plateau de Bure Interferometer observations Observations :  Summer time between 1999 – 2002 % Compact configuration % Self calibration HCO + (1-2)94.6GHz H 13 CO + (1-2)92.0GHz HC 18 O + (1-2)90.3GHz HC 17 O + (1-2)92.3GHz HCN(1-2)94.0GHz H 13 CN(1-2)91.6GHz HC 15 N(1-2)91.3GHz HNC(1-2)96.2GHz HN 13 C(1-2)92.4GHz H 15 NC(1-2)94.2GHz CS(3-4)103.9GHz C 34 S(3-4)102.2GHz 12 C/ 13 C 14 N/ 15 N 16 O/ 18 O 18 O/ 17 O 32 S/ 34 S

7. Main isotopomers  2 components NE and SW  SW : complete absorption for HCO +  non symetric profiles  = sum of velocity components with widths similar to MW clouds (~10 km/s)

8. I abs = I O (1-exp-  )

9. Let’s compare the isotopic ratios in:  One beam pencil in a galaxy at z = 0.89 6.4 Gyr ago  Solar System 4.5 Gyr ago  Local ISM (Lucas & Liszt 1998) now !  Galactic Center  IRC +10216 (Cernicharo et al 2000) archetype of AGB star  LMC (Chin 1999) low metallicity galaxy  NGC 4945 (Wanf et al 2004) nucleus of a nearby SB galaxy Is there a clear chemical evolution ???

10. 12 C : produced directly from He in massive stars (primary) 13 C : produced from 12 C and 16 O in H burning (secondary) Problems : selected photodissociation, chemical fractionation, optically thin lines for 12 C

11. 14 N : secondary, enhanced in CNO cycle at equilibrium 15 N : secondary, destroyed in CNO, produced in explosive H or He burning 14 N / 15 N : increases with metallicity (gradient in the MW)

12. 16 O : primary, produced in massive stars 18 O : secondary, produced in He burning from 14 N

13. 18 O / 17 O : constant value through the disk of the MW 17 O : secondary, produced in low mass stars

14. Sulfur : product of explosive O burning in MASSIVE stars Ratio 32 S / 34 S ???

15. Isotopic ratios in the z=0.89 galaxy are :  Different from SS, local ISM, GC  Very different from IRC+10216 !  Closer to SBs no time for the low and intermediate mass stars to release the processed materials Nearby SB : because of time scale, outputs from massive stars dominate  Different from LMC (O) (metallicity ?) Summary

16. Isotopic ratios = signature of the chemical evolution and nuclear processing (???) Molecular absorption measurements Galaxy at z = 0.89 : look back time of 6.4 Gyr But only one beam pencil STATISTICS and chemical evolution : MORE SOURCES !!! Need to observe more absorption systems at different z ! ALMA Conclusion

17. Background source Absorption And even 2 lensed images !

18. PKS 1830 Solar System Local ISM IRC +10216 Nuclei of nearby SB NGC 4945 LMC 12 C / 13 C32  10 8940 - 70455062 14 N / 15 N140 -50+130 270240> 4400100114 16 O / 18 O67  24 4906001300200> 2000 18 O / 17 O13  3 5.53.50.762 32 S / 34 S10  1 20192213.518 Chin 1999 Wang et al 2004 Lucas & Liszt 1998 Cernicharo et al 2000