Odin’s Hunt for Moleculescooperation between Canada, Finland, France and Sweden

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”

Odin projects not to be discussed by me:

• Hunting for O2 - Pagani

• Hunt of Comets - Biver

• The Atmosphere of Mars - Lellouch

• and also … by Signore & by Maoli …

Spectral scan searches for Primordial Molecules -

”Hunting structure formation during the dark ages”

Ammonia and water in IRC+10216• Hasegawa et al. 2005,

submitted to ApJ

• Confirms SWAS -H2O (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)

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”

Ammonia in Sgr B2 & Orion KL

Water in Sgr B2

• 18O/17O ratio = 2.9, after correction for optical depth

• H2O absorption is

very optically thick;

H2O emission, too…

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

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

Orion KL spectral scan

In total:

487- 492 and

541-576 GHz

Shown here:

547- 562 GHz

Observing time:

50 hours / GHz

Orion KL spectral scan 550.5-553.5 GHz

Water emission regions in Orion KL• HDO (20 2 - 111)

Eu = 66 K

• para-H2O ( 62 4 - 71 7)

Eu = 868 K - Hot Core

• ortho-H2O (110 - 101)

Eu = 27 K (61 K)

- H218O

- H217O

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

Shocked H2 in Orion KL

Water & CO in the Orion Bar

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

Ammonia et al. in Orion KL

- H2S (331-322), Eu=166 K

Blend with SO2

- NH3 (10-00), Eu= 29 K

- 15NH3 (10-00), Eu= 29 K

- CH3CN (J=30-29, K=4)

Eu=500 K

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 !!!

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/