large scale co emission in the orion nebula

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)

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. 12CO and 13CO: 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

Observations IRAM 30M radiotelescope (Granada, Spain) Size 1ox0.8o (63 submaps), centered at IRc2/KL :=05h35m14.5s, =-05o22’29.3’’ HERA 3x3 multibeam receiver

12CO (2-1) @ 230.5 GHz 13CO (2-1) @ 220.4 GHz

Angular resolution ~ 11’’(0.02 pc @ 414 pc) Velocity resolution ~ 0.4 km/s

Postdoc Symposium, April 11 2011

Postdoc Symposium, April 11 2011

12CO (2-1)

Postdoc Symposium, April 11 2011

13CO (2-1)

Postdoc Symposium, April 11 2011

12CO (2-1)

12CO emission @ -5 to 8 km/s

Postdoc Symposium, April 11 2011

Postdoc Symposium, April 11 2011

12CO emission @ -5 to 8 km/s

Postdoc Symposium, April 11 2011

IRAC 3.6 m

12CO emission @ -5 to 8 km/s

12CO emission @ -5 to 8 km/s

Postdoc Symposium, April 11 2011

Postdoc Symposium, April 11 2011

12CO emission @ -5 to 8 km/s

IRAC 3.6 m

Postdoc Symposium, April 11 2011

Orion Waves

Berné, Marcelino & Cernicharo (Nature, 466, 947)

Expansion of the HII regionprovoked 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

12CO emission @ 8 to 12 km/s

Postdoc Symposium, April 11 2011

12CO emission @ 12 to 25 km/s

Postdoc Symposium, April 11 2011

Postdoc Symposium, April 11 2011

12CO emission @ 12 to 25 km/s

SCUBA 850 m

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

12CO (2-1) emission

Postdoc Symposium, April 11 2011