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Chris Carilli (NRAO) AAS06 NRAO 50th

Chris Carilli (NRAO) AAS06 NRAO 50th. Chris Carilli (NRAO) Berlin June 29, 2005. CMB/WMAP – geometry of universe + seeds of cosmic structure from BB Relies on NRAO/CDL HEMT Amplifiers. 5.9 Gyr. HST/VLA+MERLIN Chapman +. T _univ = 13.6 Gyr. Realm of the Galaxies.

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Chris Carilli (NRAO) AAS06 NRAO 50th

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  1. Chris Carilli (NRAO) AAS06 NRAO 50th

  2. Chris Carilli (NRAO) Berlin June 29, 2005 CMB/WMAP – geometry of universe + seeds of cosmic structure from BB Relies on NRAO/CDL HEMT Amplifiers

  3. 5.9 Gyr HST/VLA+MERLIN Chapman + T_univ = 13.6 Gyr Realm of the Galaxies HST/CO Wilson et al

  4. SDSS J1148+5251 870 Myr (1/16 T_univ) Dark Ages First Light + Reionization Fan + Walter + VLA CO 3-2 Sloan Quasar 870 Myr 5kpc

  5. SDSS J1148+5251: Dust and molecular gas into cosmic reionization 870Myr VLA: CO 3-2 2.5kpc • 1e10 M_sun molecular gas = fuel for galaxy formation. • ‘Explosive’ galaxy and SMBH formation in merging system at 1/16 T_univ? • Very early formation of heavy elements • (within 0.5Gyr of BB) [C II] CO 6-5 1” IRAM

  6. ALMA Deep field: probing earliest ‘normal’ galaxies HST • Detect J1148 dust galaxies in seconds! • ALMA – weighted to distant, dusty galaxies • Image at kpc-resolution dust, cold gas, star formation in first galaxies T_univ > 4.5 Gyr < 4.5 Gyr ALMA

  7. Required: Panchromatic view of ‘First Light’ VLA CO 3-2 ALMA: cold gas and dust CO 3-2 z=6.4 EVLA: star formation/AGN JWST: stars, ionized gas

  8. END

  9. Panchromatic view of galaxy formation ALMA: cold gas and dust EVLA: star formation/AGN JWST: stars, ionized gas

  10. NRAO: Unveiling galaxy formation AAS 2006, C. Carilli (NRAO) IC342 T_univ = 13.6 Gyr 5.9 Gyr HST/CO Wilson et al HST/VLA+MERLIN

  11. The CMB From NRAO HEMTs OVRO/BIMA

  12. Millimeter VLBI – Imaging the Galactic center black hole (Falcke 2000) Kerr Schwarzschild Model: opt. thin synch 0.6 mm VLBI 16uas res 1.3 mm VLBI 33 uas res

  13. The details of early galaxy formation GBT/VLA: dense molecular gas – fuel for galaxy formation z=4.2 VLA CO 2-1 z=4.8 0.2” VLBA: sub-kpc imaging – distribution of star formation

  14. Panchromatic view of galaxy formation Arp 220 vs z cm: Star formation, AGN (sub)mm Dust, molecular gas Near-IR: Stars, ionized gas, AGN

  15. Epoch of “galaxy formation” (z=1.5 – 3) • Submm/radio surveys reveal massive, dusty starburst galaxies at high redshift, often unseen in deepest optical surveys (eg. HDF) • Comparable SFR at z>2 in these “submm galaxies” as optically selected galaxies = formation of large elliptical galaxies? • Combined radio/mm/(near)IR allows for accurate positions, and coarse redshifts • currently limited to extreme starbusts (1000 M_sun/yr)

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