Circumstellar disks: what can we learn from ALMA? March ARC meeting, CSL

ARC meeting - March ALMA site - January 2011 Now

ARC meeting - March In 2013

ARC meeting - March

4 What is ALMA? ALMA will be the worlds largest interferometer for millimetre and sub-millimetre wavelengths It is in full construction in the Atacama desert Collaboration between ESO, NRAO, and NAOJ Three sites in Chile

ARC meeting - March

7 ALMA specifications 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 ( 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

9 Status February 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 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 First results

ARC meeting - March First results

ARC meeting - March 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 Early science

ARC meeting - March Early science

ARC meeting - March Circumstellar disks Imaging protoplanetary disks 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 Circumstellar disks 1 AU

ARC meeting - March Young Stellar Objects

ARC meeting - March Imaging proto-planets

ARC meeting - March Imaging proto-planets DAngelo et al. 2002

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 ARC meeting - March 2011 Early ScienceHerschel

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 ARC meeting - March 2011 Early ScienceHerschel Connection?

ARC meeting - March Debris disks Dust trapped in resonances by migrating planets in disk

ARC meeting - March Debris disks Content of residual gas in debris disks Deep spectroscopy Comet collisions should evaporate H 2 O, CO Method to study exo-comet composition

ARC meeting - March ALMA is coming !

ARC meeting - March What is ALMA?

ARC meeting - March Early science

ARC meeting - March Early science Limitations to be kept in mind: Limited number of antennas (Resolution not better than existing interferometers) Limited sensitivity as compared to full ALMA (Sensitivity ~10x better than existing interferometers) Imaging requires Earth rotation synthesis Limited angular resolution No multi resolution available Limited time available for science observations ALMA ES capabilities and constraints are best suited for limited scope Projects (as opposed to large scale surveys) Typical project for ES should be few hrs (4-10) and deliver result!

ARC meeting - March

1 Picture was taken before ALMA construction started

ARC meeting - March Circumstellar disks