Odin

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Odins Hunt for Moleculescooperation between
Canada, Finland, France and Sweden
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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

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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

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Spectral scan searches for Primordial Molecules
-Hunting structure formation during the dark
ages
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Ammonia and water in IRC10216

• 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)

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Water in W Hya

• Justtanont et al. 2005
• (AA 439, 627)
• Water abundance is very high (2-3)x10-3
• Another extra-solar cometary system may have
  been detected

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Ammonia in Sgr B2 Orion KL
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Water in Sgr B2

• 18O/17O ratio 2.9, after correction for optical
  depth
• H2O absorption is
• very optically thick
• H2O emission, too

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Water HCO(J1-0) towards W49N
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Infall / Outflow / Absorption towards the
G34.3-0.2 hot core
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Orion KL spectral scan

• In total
• 487- 492 and
• 541-576 GHz
• Shown here
• 547- 562 GHz
• Observing time
• 50 hours / GHz

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Orion KL spectral scan 550.5-553.5 GHz
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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

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Water and CO(5-4) at 40 resolutionDeconvolution
of mapping cubes
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Shocked H2 in Orion KL
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Water CO in the Orion Bar
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Orion KL 13CO(5-4) at 40 resolution
Deconvolution of mapping cubes
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Ammonia et al. in Orion KL

• - H2S (331-322), Eu166 K
• Blend with SO2
• NH3 (10-00), Eu 29 K
• 15NH3 (10-00), Eu 29 K
• CH3CN (J30-29, K4)
• Eu500 K

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Herschel vs Odin

• Small source Odin signals will be
• gt 10 times stronger
• Herschels SIS noise level will be
• gt 10 times lower
• that of Odins
  Scottky mixers
• Counted in required integration time this
  means
• gt 10000 1 Great hope !!!

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Some Odin References

• Odin Special Issue of AA Letters (AA 402,
  L21-L81)
• Hjalmarson et al. 2005, Advances in Space
  Research
• Wilson et al. 2005, AA 433, L5 (O2 search in
  SMC)
• Justtanont et al. 2005, AA 439, 627 (W Hya)
• Hasegawa et al. 2005, ApJ, submitted (IRC10216)
• 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/