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CCAT and Star formation

CCAT and Star formation. Derek Ward-Thompson Cardiff University CCAT meeting 13/09/06. Where we are. The greatest advance SCUBA has given to star formation studies is wide-field sub-mm astronomy. SCUBA-2 will give us an even greater lead in this area. JCMT will close in 2012.

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CCAT and Star formation

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  1. CCAT and Star formation Derek Ward-Thompson Cardiff University CCAT meeting 13/09/06

  2. Where we are • The greatest advance SCUBA has given to star formation studies is wide-field sub-mm astronomy. • SCUBA-2 will give us an even greater lead in this area. • JCMT will close in 2012. • Where do we go after that?

  3. Orion with SCUBA-1

  4. Orion core mass function Nutter & W-T 2006 MN submitted

  5. SCUBA-2 mapping area

  6. Oph-Sco with SCUBA-2

  7. Statistics give us: • Core mass functions • Statistical lifetimes of pre-stellar and protostellar stages • This then leads to accretion rates • Which allows us to choose between various star formation model scenarios

  8. SEDs of protostars & prestellar cores

  9. SEDs of L1544 & L1498 Ward-Thompson et al (2002) MNRAS 329, 257

  10. Why study 200 microns? • Peak of 15K black-body • Cold dust is brightest there • Optimal wavelength to study: Proto-stars Pre-stellar cores Embedded clusters

  11. THz sky transmission

  12. Weather statistics

  13. Tau relation (Thumper) Ward-Thompson et al 2005 MNRAS 364, 843

  14. Previous measurements (Chile) tau(1500) = (105+/-32) * tau(220) (Matsushita et al 1999, PASJ, 51, 603)

  15. Previous measurements (South pole) Tau(1500) = (100 +/- 20) * tau(225) The TREND team ( Gerecht et al, 2003, 14th THz ISS; Chamberlin et al 2002, SPIE, 4855-83)

  16. First Thumper data - map of Jupiter Ward-Thompson et al 2005 MNRAS 364, 843

  17. CCAT: • Would continue the UK’s interest in wide-field sub-mm astronomy through the next decade • Would allow us to build on our JCMT SCUBA-1 & 2 expertise • Would give us 2-4 arcsec resolution over very wide fields - rather than the current 14 arcsec • Would give us access to wavelengths where prestellar cores and protostars emit most of their energy

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