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HIGH RESOLUTION OBSERVATIONS OF IONIZED AND MOLECULAR GAS IN REGIONS OF HIGH MASS STAR FORMATION

HIGH RESOLUTION OBSERVATIONS OF IONIZED AND MOLECULAR GAS IN REGIONS OF HIGH MASS STAR FORMATION. Igor Zinchenko Institute of Applied Physics, Russian Academy of Sciences. Participants. Stan Kurtz – Centro de Radioastronomía y Astrofísica de la UNAM, Mexico

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HIGH RESOLUTION OBSERVATIONS OF IONIZED AND MOLECULAR GAS IN REGIONS OF HIGH MASS STAR FORMATION

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  1. HIGH RESOLUTION OBSERVATIONS OF IONIZED AND MOLECULAR GAS IN REGIONS OF HIGH MASS STAR FORMATION Igor Zinchenko Institute of Applied Physics,Russian Academy of Sciences

  2. Participants • Stan Kurtz – Centro de Radioastronomía y Astrofísica de la UNAM, Mexico • Sheng-Yuan Liu, Yu-Nung Su – Academia Sinica Institute of Astronomy and Astrophysics, Taiwan • Rui-Qing Mao – Purple Mountain Observatory CAS, China • Devendra Ojha – Tata Institute of Fundamental Research, India

  3. Objectives • Detailed studies of the structure and physical properties of high mass star forming regions on various scales. • Investigation of star formation triggering by expansion of H II regions. • Studies of chemical variations in high mass star forming regions on various scales.

  4. Observations

  5. A part of theS 255N spectrum measured at SMA

  6. Examples of the SMA maps S255IR S255N

  7. Large scale structure: S255

  8. Large scale structure : S76 MSX 8 μm + GB6 CO J=1-0(observed at PMO-14m)

  9. 13CO(1-0) (color) and MSX 8 µm contours

  10. CO, 13CO and C18O summary spectra

  11. CO and 13CO spectra in the central “hole” The envelope should be clumpy and turbulent

  12. VLA 3 cm (green) and HCO+(4-3) (blue) contours overlaid on the Spitzer 3.6 and 8 μm images

  13. 1.2 mm (IRAM-30m) contours (log scale) overlaid on the Spitzer 8 μm image

  14. NMA observations An example of sequential high mass star formation?

  15. Physical parameters of the clumps

  16. Multi-line observations of selected objects: S255 1.2 mm

  17. SMA images of S255IR in various lines

  18. CH3CN spectrum towards S255 IR mm1 and the best fit

  19. S255IR: 1.1 mm continuum (color), 20 cm continuum (green contours) and CO line wings (blue and red contours).

  20. The position-velocity diagram for the CO outflow

  21. S255N: 1.1 mm continuum (color), 20 cm continuum (green contours), 1.3 cm continuum (blue contours) and NH3 (1,1) emission (yellow contours).

  22. How common is triggering?

  23. S187: another example?

  24. Conclusions • Star formation in envelopes of H II regions is a common phenomenon and is probably triggered by expansion of these envelopes. • Observations of different CO isotopes indicate that the envelopes are clumpy and turbulent. • In the regions of active star formation clumps at various stages of this process are observed. Physical properties and chemical content of these clumps can differ significantly. • Highly collimated bipolar outflows and disks in regions of high mass star formation imply the star formation process similar to that for low mass stars.

  25. Thank you for your attention!

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