Circumstellar disks: what can we learn from ALMA?

1. Circumstellar disks: what can we learn from ALMA? March 2011 - ARC meeting, CSL

2. 1 Now ALMA site - January 2011 ARC meeting - March 2011

3. 2 In 2013 ARC meeting - March 2011

4. 1 ARC meeting - March 2011

5. 4 What is ALMA? • ALMA will be the world’s largest interferometer for millimetre and sub-millimetrewavelengths • It is in full construction in the Atacama desert • Collaboration between ESO, NRAO, and NAOJ • Three sites in Chile ARC meeting - March 2011

6. 1 ARC meeting - March 2011

7. 7 ALMA specifications • 54 12-m antennas,12 7-m antennas, at 5000 m site • 192 antenna stations • Array configurations between 150 m and ~15-18 km • Angular resolution ~40 mas at 100 GHz (5 mas at 900 GHz) • 10 bands in range 31 to 950 GHz (350-7000 µm) • Dual polarization • ALMA vs Herschel (3.5 m) • Wavelengths: 350 – 7000 µm vs 70 – 550 µm • Angular resol: 1‘ – 0.01“ vs 6“– 35“ • Lifetime : 30 years vs 3.5 years ARC meeting - March 2011

8. 8 ARC meeting - March 2011

9. 9 Status February 2011 • 8 antennas on site 5000m site and working as interfer. • Fringes observed in 4 bands • Phase closure achieved • ~30 antennas delivered to site in total ARC meeting - March 2011

10. 10 Main science goals • Detect and map CO and [C II] in a Milky Way galaxy at z=3 in less than 24 hours of observation • Map dust emission and gas kinematics in proto-planetary disks • Massive stars (wind acceleration, photosphere,…) Provide high fidelity imaging in the (sub)millimeter at 0.01 arcsec resolution ARC meeting - March 2011

11. 11 First results ARC meeting - March 2011

12. 12 First results ARC meeting - March 2011

13. 13 Early science • When? • Call in early April, deadline 8 weeks after • Observations: Fall 2011 • What? • 16 antennas, 2 compact configurations • Bands 3, 6, 7 and 9 (3mm, 1mm, 0.85mm, 0.45mm) • Baselines up to 250m (maybe 500m) • At most 30% of the available time for the first call • Only service mode • Typical project for ES should be few hrs (4-10) and deliver result! ARC meeting - March 2011

14. 7 Early science ARC meeting - March 2011

15. 7 Early science ARC meeting - March 2011

16. 16 Circumstellar disks • Imaging protoplanetarydisks • Accretion, rotation and outflow • Molecular gas content, chemistry and removal mechanisms • How gaps are created by planets • Imaging debris disks • Dust evolution, radial dependence of grain properties • Following planets with dust rings • Probe the growth of dust in disks and constrain planet formation theories ARC meeting - March 2011

17. 17 Circumstellar disks 1 AU ARC meeting - March 2011

18. 19 Imaging proto-planets ARC meeting - March 2011

19. 20 Imaging proto-planets D’Angelo et al. 2002 ARC meeting - March 2011

20. 21 Debris disks • Optically thin dust in thermal equilibrium with the star : • traces mass of debris or infer mass of comets • shows scale of planetary system Early Science Herschel ARC meeting - March 2011

21. 21 Debris disks • Optically thin dust in thermal equilibrium with the star : • traces mass of debris or infer mass of comets • shows scale of planetary system Early Science Herschel Connection? ARC meeting - March 2011

22. 22 Debris disks • Dust trapped in resonances by migrating planets in disk ARC meeting - March 2011

23. 23 Debris disks • Content of residual gas in debris disks • Deep spectroscopy • Comet collisions should evaporate H2O, CO • Method to study exo-comet composition ARC meeting - March 2011

24. 1 ALMA is coming! ARC meeting - March 2011