1. Peering into the Birthplaces of Solar Systems Atacama Large Millimeter/submillimeter Array Expanded Very Large Array Robert C. Byrd Green Bank Telescope Very Large Baseline Array Early ALMA and EVLA Observations of Circumstellar Disks David J. Wilner Harvard-Smithsonian Center for Astrophysics K. Teramura UH IfA

2. From Disks to Planets Astro2010: How do circumstellar disks evolve and form planetary systems? McCaughren & O’Dell 1995 Marois et al. 2008, 2010 Silhouette Disks in Orion Nebula around ~1 Myr-old stars Planets Orbting HR8799 AAAS, February 20122

3. Relevance of Radio Astronomy avoid high dust opacities mass tracer many spectral lines diagnostics, kinematics sensitive to cold material including mid-plane contrast with star planet-forming region high sensitivity and angular resolution ALMA and EVLA! ALMA EVLA AAAS, February 20123

4. Next Generation Radio Telescopes 66 moveable 12m/7m antennas 5000 m site in northern Chile  = 300  m to 3 mm global collaboration (NA, EU, EA) to fund >$1B construction 27 moveable 25 m antennas 2000 m site in New Mexico  = 7 mm to 4 m modern electronics and signal processing, c. 1980 infrastructure Atacama Large Millimeter Array Expanded Very Large Array AAAS, February 20124 10-100x better sensitivity, spectral capabilities, resolution

5. Some Early Disk Observations ALMA Science Verification: TW Hya Protoplanetary Disk test system validity, data released to community disks@EVLA key project: Grain Growth and Structure PI Claire Chandler (NRAO) and 17 co-I’s worldwide ALMA Early Science: Fomalhaut Debris Disk PI Aaron Boley (U. Florida) and 5 co-I’s These results already showcase the extraordinary science potential of the new radio telescopes. Many more amazing observations are underway. AAAS, February 20125

6. HST, Weinberger et al. 2002 TW Hya Background closest gas-rich ~few Myr-old disk (160 ly) – isolated, viewed nearly face-on – southern sky – many studies with Submillimeter Array Andrews et al. 2011 Qi et al. 2004 Doppler shift AAAS, February 20126

7. TW Hya CO J=3-2 from ALMA Keplerian model/data comparison – can you tell the difference? AAAS, February 20127 incredible data (from a small fraction of ALMA)!

8. TW Hya DCN J=3-2 from ALMA imaging a deuterated, nitrogen-bearing, triatomic molecule (!) Earth’s oceans are enriched in deuterium deuteration is associated with low temps: H 3 + + HD  H 2 D + + H 2 +  E water delivery from cold, outer Solar System? (by comets) Hartogh et al. 2011 AAAS, February 20128

9. TW Hya DCN J=3-2 from ALMA SMA DCO + : D/H enhancement at large disk radii – supports in situ deuteration at low T in outer disk water delivered from cold, outer Solar System? evidence for multiple pathways to deuterium enhancement in disks DCN distribution is different! Oberg et al. 2012 Qi et al. 2008 AAAS, February 20129

10. radio spectral signatures From Dust to Planets planet-disk interactions 1  m 1mm 1m 1km 1000km <1km Planetesimal formationPlanet formation Collisional agglomoration Gravity- assisted growth Gas capture ??? (collective effects) Debris Collisons AAAS, February 201210

11. Spectral Signatures of Grain Growth mm/cm dust emissivity  ~ -   is diagnostic of maximum grain size  AAAS, February 201211 see Draine 2006 Rodmann et al. 2006 ISM grains “pebbles” 2  0 previous VLA results

12. Disks@EVLA Key Project (PI Chandler) grain growth and substructure in protoplanetary disks: last observable link in chain from ISM to planets 1.photometry of 60+ disks at 7/9/13/50 mm – spectral indices reveal large grains – reduction and modeling underway 2.imaging of subsets, to 50 mas = few AU – surface densities, disk-planet interactions – observations ongoing – expect resolved mm/cm colors K. Teramura UH IfA AAAS, February 201212

13. (Preliminary) EVLA Taurus Disk Images spectral indices = 9 mm (30.5 and 37.5 GHz) θ ~ 0.7 arcsec = 100 AU Chandler et al, in prep AAAS, February 201213

14. P. Armitage: jila.coloarado.edu/~pja TW Hya: Planet-Disk Interaction giant planet opens disk gap and creates cavity 4 AU radius cavity (barely) detected with VLA Hughes et al. 2007 AAAS, February 201214

15. TW Hya: Planet-Disk Interaction should be easy to detect with EVLA and ALMA at the limits of ALMA Wolf & D’Angelo 2005 AAAS, February 201215

16. Fomalhaut Background ~200 Myr-old nearby star (25 ly) with dusty debris directly imaged orbiting planet possible circumplanetary disk? Kalas et al. (2008) AAAS, February 201216

17. Kalas et al. (2009) PI Boley: measure thermal dust emission from known circumstellar material and potentially circumplanetary dust near Fomalhaut b using the compact (3 hrs) and extended early science antenna configurations Fomalhaut with ALMA at 870  m AAAS, February 201217 20 arcseconds ~ 150 AU Boley et al. in prep. ALMA Cycle 0 Reference Image rms noise 70  Jy 1.5” x 1.2”

18. Underway in ALMA Cycle 0… young disks: Orion, brown dwarfs, binaries, chemistry, gas/dust structure, dynamics PIs: Mann, Akeson, Ricci, Qi, Lin, Carpenter, Salyk, Chapillon, Walsh old disks: debris, birth rings, Herschel cold disks PIs: Rodriguez, Jordan, Carpenter, Boley, Wilner, Woitke in-between disks: gas-poor/dust-rich, gas-rich/dust-poor, gas in cavities, dust in cavities, unusually small/large disks PIs: Dutrey, Andrews, Chapillon, Casassus, van Dishoek, Perez, Schreiber, Kospal disks and planets: interactions PIs: Jordan, Huelamo, Boley AAAS, February 201218

19. A new “Radio Era” for Disk Studies large samples of planet-forming disks now within reach major unknown is distribution/evolution of cold dust and gas at Solar System scales: key observables for ALMA and EVLA amazing prospects expect surprises! at the limits of ALMA AAAS, February 201219

20. AAAS, February 201220