Complex organic molecules in hot corinos Sandrine Bottinelli Laboratoire d’AstrOphysique de Grenoble (France) / Institute for Astronomy (Hawaii) Cecilia Ceccarelli (LAOG), Jonathan Williams (IfA) and Roberto Neri (IRAM) Outline: I – Background II – 30m observations of NGC1333- IRAS4A III – PdB observations of IRAS16293 IV – Conclusions
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Complex organic molecules in hot corinos Sandrine Bottinelli Laboratoire d’AstrOphysique de Grenoble (France) / Institute for Astronomy (Hawaii) Cecilia.
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Complex organic molecules in hot corinos
Sandrine BottinelliLaboratoire d’AstrOphysique de Grenoble (France) /
Institute for Astronomy (Hawaii)
Cecilia Ceccarelli (LAOG), Jonathan Williams (IfA)
and Roberto Neri (IRAM)
Outline: I – BackgroundII – 30m observations of NGC1333-IRAS4A
III – PdB observations of IRAS16293IV – Conclusions
Hot core: first stage in the evolution of massive protostars
~300 GHz, beam ~ 1.9" 0.9" (Chandler et al. 2005, ApJ in press).
Continuum emission
SpectraIRAS16293
202,19-192,18
A E
201,19-191,18
A ECN 2-1
6 4,0-5 4,0
6 0,0-5 0,0
6 1,0-5 1,0
6 2,0-5 2,0
6 3,0-5 3,0
2 scenariosIRAS16293
MA ~ 1M
MB < MA
Vsin i = 1.2 km/s
830 AU
2
• VLSR (A) = 3.9 km/s and VLSR (B) = 2.7 km/s.
1
• VLSR (A,B) = 3.9 km/s.
• MA ~ MB, B more compact.
• Lines optically thick towards B.
Chemical modeling
• Coupling between chemistry, dynamics and radiative transfer is computationally intensive, but many efforts to tackle different aspects: – chemical evolution in protostellar envelopes (e.g. Rodgers &
Charnley 2003; Doty et al. (2004); – laboratory studies (e.g. Horn et al. 2004); – molecular line profiles (e.g. Lee et al. 2004);– chemical clocks (e.g. Wakelam et al. 2004, previous talk);– grain surface reactions (e.g. Weaver & Blake this afternoon).
• Problem = difficult to reconcile theory and observations for gas-phase formation of complex molecules (e.g. for HCOOCH3 - Horn et al. 2004).
Conclusions
• Hot corinos exist and have been imaged.• IRAS16293 not alone (however still don’t
know how common hot corinos are).• Open questions:
– What are the formation mechanisms of these molecules?
– Evolution, link with comets?
to answer, continue the effort through combining modeling and observations.