1. Large Scale CO Emission in the Orion Nebula Núria Marcelino (NRAO-CV) Olivier Berné (Leiden Obs, The Netherlands) José Cernicharo (CSIC/INTA, Spain) HST CO (2-1)

2. Motivations  The closest (brightest) massive star forming region  Prototypical source: observed at almost all wavelengths  Star formation features: hot cores, HII regions, protostars, circumstellar disks, outflows, HH objects, PDRs, etc.  12 CO and 13 CO: spatial distribution, kinematics, and column densities of molecular gas  Previous large scale CO maps have poor spectral and/or angular resolution Postdoc Symposium, April 11 2011

3. Observations  IRAM 30M radiotelescope (Granada, Spain)  Size 1 o x0.8 o (63 submaps), centered at IRc2/KL : =05 h 35 m 14.5 s, =-05 o 22’29.3’’  HERA 3x3 multibeam receiver — 12 CO (2-1) @ 230.5 GHz — 13 CO (2-1) @ 220.4 GHz  Angular resolution ~ 11’’ (0.02 pc @ 414 pc)  Velocity resolution ~ 0.4 km/s Postdoc Symposium, April 11 2011

4. 12 CO (2-1)

5. Postdoc Symposium, April 11 2011 13 CO (2-1)

6. Postdoc Symposium, April 11 2011 12 CO (2-1)

7. 12 CO emission @ -5 to 8 km/s Postdoc Symposium, April 11 2011

8. 12 CO emission @ -5 to 8 km/s

9. Postdoc Symposium, April 11 2011 IRAC 3.6 m 12 CO emission @ -5 to 8 km/s

10. Postdoc Symposium, April 11 2011

11. 12 CO emission @ -5 to 8 km/s IRAC 3.6 m

12. Postdoc Symposium, April 11 2011

13. Orion Waves Berné, Marcelino & Cernicharo (Nature, 466, 947)  Expansion of the HII region provoked Kelvin-Helmholtz instabilities and cloud fragmentation  Intense and ionizing stellar irradiation caused the acceleration of the clumps  First observational evidence of KH instabilities, result of hydrodynamical feedback of massive stars on their parental cloud Postdoc Symposium, April 11 2011

14. 12 CO emission @ 8 to 12 km/s Postdoc Symposium, April 11 2011

15. 12 CO emission @ 12 to 25 km/s Postdoc Symposium, April 11 2011

16. 12 CO emission @ 12 to 25 km/s SCUBA 850 m

17. Conclusions  Very complex dynamics and velocity structure  Clumps, filaments, cavities, pillars/cometary globules, outflows, etc.  Interaction between massive star winds, HII regions, and molecular ambient cloud: energy transport, turbulence, formation of filaments, triggered star formation, etc.  High angular and spectral resolutions are essential to study in detail these processes Postdoc Symposium, April 11 2011

18. 12 CO (2-1) emission Postdoc Symposium, April 11 2011