Harvard-Smithsonian CfA

1. Cosmic Compact Objects & Harvard-Smithsonian CfA Future Submm-FIR Space Astronomy Jun-Hui Zhao

2. Spectra

3. Spectra

4. Spectra

5. 1156-296 Helical Jet Images NGV 4258 Micro-quasar HH111 • Dust Obscuring (Av ~ 100 mag) • Self Absorption (Radio and mm) • Sub-mm/FIR Spectral Lines Star-planet SS 433 M 87 NGC 4261 NGC 326

6. Rotational Transitions High critical density (1e10 cm^-3) Coolant lines

7. Top 5 Telescopes Telescopes, Angular Resolution & Sensitivity Galileo Home-made Spyglass Palomar 5m Very Large Array Chandra HST

8. Telescopes, Angular Resolution & Sensitivity Hat creek mm Array (BIMA) IRAM (PdB, Pico) GBT, NRAO

9. Telescopes, Angular Resolution & Sensitivity CSO SMA Kosma-3m ALMA JCMT

11. Telescopes, Angular Resolution & Sensitivity Space Submm: SWAS (NASA) Odin (Sweden/Canada) Calibration – No Earth Atmosphere Effect (Attenuation, Turbulence) Science - Star Formation and Molecular Cooling The Chemical Evolution of ISM

12. Telescopes, Angular Resolution & Sensitivity

13. Science • STARs • Star Formation ISM, Molecular Clouds, Dust Fragmentation Proto-stars Accretion and Molecular outflow • Stellar evolution KH contraction, Hayashi track, Nuclear ignition M.S. stars AGB, Red giants/super giants, SNe White Dwarf, Neutron Stars, BHs

14. Science • Galactic Nuclear Region Supermassive BH, physics and formation Astrophysical Process in Extreme Environs (Turbulence, B-field, Tidal Forces) How are stars (high mass) formed? How do stars evolve? How Supermassive BH accretes stars? (growing BH?) Properties of Circum-nuclear Medium (Metallicity , Chemistry, Dust?) • First Generation Star Formation & Galaxy Formation in The Early Universe

15. The Galactic Center The Galactic Center

16. Radio

17. Sub-mm

18. IR

19. X-Ray

20. Arches Cluster Quintuplet Cluster Pistal Star and nebula 10^7 Lo, 150 Mo Sgr A Complex & HII Clusters

21. Chandra 100hr X-ray Flare 2.6 Million Mo Black Hole Mass 10^-7 Mo/yr 10^-8.7 Ledd Keck 8-micron VLA 1.3 cm (0.1 arcsec)

22. 240 d 100 d Optically thick up to 340 GHz VLBA, 6,3.5,2,1.3,0.7 cm 40 Rs Frequency (GHz)

23. High Mass Star Formation in Extreme Astrophysical Environments • How do Molecular Clouds Collapse Proto-stars Mj ~ 1e5 Mo, Lj ~ 20 pc, similar to cosmological conditions at decoupling. Periodic Nucleus Explosions Shock Waves to trigger. • Flat IMF High Mass Stars only? Intermediate/low mass star formation sites? Dust obscuring? • Chemistry and Dust Properties (grain size) in the Very High Mass Star formation sites Molecular Lines Masers Excitation mechanisms Radiation coolants (H20, CO, OI, CI, CII etc)

24. Stellar Evoltuion in Extreme Astrophysical Environments • Tidal Disruption Star –explosions, Stellar Debris Squeezar – spin-up, L-flares Missing red giants in central 2” Tidally Striping envelope from red giants/super giants Fate of the remnants – structure Rings? Dynamic role to the accretion disk?

25. The Struction of Immediate Environs of SMBH • ADAF, CDAF, Jet-ADAF accretion-radiation processes • Orbital Resonance • Observation High Angular resolution Sub-mm VBLI • Structure of Accretion Disk and Surroundings of SMBH

26. Future Submm/FIR Space Astronomy • SAFIR (Single Aperture Far-IR Observatory) Filling the gap between ALMA and JWST Understand the structure of the universe from its earliest beginning to its ultimate fate.

27. Future Submm/FIR Space Astronomy • Space Interferometer • SPECS (Sub-mm Probe of the Evolution of Cosmic Structure) 1km BL, FIR/sub-mm imaging & spectral space interferometer Mather etal 1999 • SPIRIT (Space IR Interferometric Telescope) Leisawitz 2000

28. Future Submm/FIR Space Astronomy Sub-mm/FIR Space VLBI Space Interferometer + Ground Interferometers Understand the fine structure of the cosmic objects Can China plays a role in this game? How? 1st step: Ground mm/Sub-mm VBLI facility as a test bed. Establish International Collaboration (Japan, S. Korea, Europe, USA etc)