1. Odin’s Hunt for Molecules cooperation between Canada, Finland, France and Sweden

2. Some Odin Quick - Facts : * 1.1 m telescope (beam size: 2’ / 9’ at mm / submm) * 4 x cryo-cooled, tuneable submm mixers (486-504 & 541-581 GHz) * Cryo-cooled HEMT receiver at 119 GHz for sensitive O2 searches * Broad-band AOS (BW = 1040 MHz) * 2 x Hybrid autocorrelators (BW= 100-800 MHz) ”Simultaneous observations using any combination of three receivers”

3. Odin projects not to be discussed by me: Hunting for O 2 - Pagani Hunt of Comets - Biver The Atmosphere of Mars - Lellouch and also … by Signore & by Maoli …

4. Spectral scan searches for Primordial Molecules - ”Hunting structure formation during the dark ages”

5. Ammonia and water in IRC+10216 Hasegawa et al. 2005, submitted to ApJ Confirms SWAS -H 2 O (60 hours vs 600hours) Ammonia and water abundances are very high in this C-rich source : 1x10 -6 and 2x10 -6 Suggested SWAS scenario is ”Evaporation of Comets”, but cannot explain ammonia level (in case of solar-type comets)

6. Water in W Hya Justtanont et al. 2005 (A&A 439, 627) Water abundance is very high: (2-3)x10 -3 ”Another extra-solar cometary system may have been detected”

7. Ammonia in Sgr B2 & Orion KL

8. Water in Sgr B2 18 O/ 17 O ratio = 2.9, after correction for optical depth H 2 O absorption is very optically thick; H 2 O emission, too…

9. Water & HCO + (J=1-0) towards W49N

10. Infall / Outflow / Absorption towards the G34.3-0.2 hot core

11. Orion KL spectral scan In total: 487- 492 and 541-576 GHz Shown here: 547- 562 GHz Observing time: 50 hours / GHz

12. Orion KL spectral scan 550.5-553.5 GHz

13. Water emission regions in Orion KL HDO (2 0 2 - 1 11 ) E u = 66 K para-H 2 O ( 6 2 4 - 7 1 7 ) E u = 868 K - Hot Core ortho-H 2 O (1 10 - 1 01 ) E u = 27 K (61 K) -H 2 18 O -H 2 17 O

14. Water and CO(5-4) at 40” resolution ”Deconvolution of mapping cubes”

15. Shocked H 2 in Orion KL

16. Water & CO in the Orion Bar

17. Orion KL 13 CO(5-4) at 40” resolution ”Deconvolution of mapping cubes”

18. Ammonia et al. in Orion KL - H 2 S (3 31 -3 22 ), E u =166 K Blend with SO 2 -NH 3 (1 0 -0 0 ), E u = 29 K - 15 NH 3 (1 0 -0 0 ), E u = 29 K -CH3CN (J=30-29, K=4) E u =500 K

19. Herschel vs Odin * Small source Odin signals will be > 10 times stronger * Herschel’s SIS noise level will be > 10 times lower that of Odin’s Scottky mixers * Counted in required integration time this means > 10000 : 1 & Great hope !!!

20. Some Odin References : Odin Special Issue of A&A Letters (A&A 402, L21-L81) Hjalmarson et al. 2005, Advances in Space Research Wilson et al. 2005, A&A 433, L5 (O2 search in SMC) Justtanont et al. 2005, A&A 439, 627 (W Hya) Hasegawa et al. 2005, ApJ, submitted (IRC+10216) Talks at the recent Asilomar IAU Symposium* by René Liseau and by Hans Olofsson 2005 Posters at the recent Asilomar IAU Symposium* by Persson et al., Encrenaz et al, Wirström et al & Ristorcelli et al. 2005 * http://asilomar.caltech.edu/