Chris Carilli (NRAO) AAS06 NRAO 50th.

Slides:

Advertisements

Similar presentations

F. Walter, M. Aravena, F. Bertoldi, C. Carilli, P. Cox, E. da Cunha, E. Daddi, D. Downes, M. Dickinson, R. Ellis, R. Maiolino, K. Menten, R. Neri, D. Riechers,

Advertisements

JWST Science 4-chart version follows. End of the dark ages: first light and reionization What are the first galaxies? When did reionization occur? –Once.

The Highest-Redshift Quasars and the End of Cosmic Dark Ages Xiaohui Fan Collaborators: Strauss,Schneider,Richards, Hennawi,Gunn,Becker,White,Rix,Pentericci,

ESO Recent Results on Reionization Chris Carilli (NRAO) Dakota/Berkeley,August 2011 CO intensity mapping during reionization: signal in 3 easy steps Recent.

Molecular Gas, Dense Molecular Gas and the Star Formation Rate in Galaxies (near and far) P. Solomon Molecular Gas Mass as traced by CO emission and the.

Molecular gas in the z~6 quasar host galaxies Ran Wang National Radio Astronomy Observatory Steward Observatory, University of Atrizona Collaborators:

The Dark Age… before the stars, beyond the galaxies…

Star formation at high redshift (2 < z < 7) Methods for deriving star formation rates UV continuum = ionizing photons (dust obscuration?) Ly  = ionizing.

Dusty star formation at high redshift Chris Willott, HIA/NRC 1. Introductory cosmology 2. Obscured galaxy formation: the view with current facilities,

Molecular absorption in Cen A on VLBI scales Huib Jan van Langevelde, JIVE Ylva Pihlström, NRAO Tony Beasley, CARMA.

ESO Galaxy Formation: The Radio Decade (Dense Gas History of the Universe) Chris Carilli (NRAO) Santa Fe, March 2011 Power of radio astronomy: dust, cool.

130 cMpc ~ 1 o z~ = 7.3 Lidz et al ‘Inverse’ views of evolution of large scale structure during reionization Neutral intergalactic medium via HI.

130 cMpc ~ 1 o z = 7.3 Lidz et al ‘Inverse’ views of evolution of large scale structure during reionization Neutral intergalactic medium via HI 21cm.

ALMA DOES GALAXIES! A User’s Perspective on Early Science Jean Turner UCLA.

The Science Case for Band 1 James Di Francesco Herzberg Institute of Astrophysics Victoria, BC, Canada.

Radio observations of massive galaxy and black hole formation in the early Universe Chris Carilli (NRAO) MPIA, Heidelberg, Aug 7, 2009  Introductory remarks.

Studying the gas, dust, and star formation in the first galaxies at cm and mm wavelengths Chris Carilli, KIAA-PKU reionization workshop, July 2008  QSO.

1 National Radio Astronomy Observatory – Town Hall AAS 211 th Meeting – Austin, Texas Science Synergies with NRAO Telescopes Chris Carill NRAO.

SMA [CII] 158um 334GHz, 20hrs BRI z=4.7 Quasar-SMG pair Both HyLIRG Both detected in CO Iono ea 2007 Omont ea ”4” HST 814 Hu ea 96.

Renaissance: Formation of the first light sources in the Universe after the Dark Ages Justin Vandenbroucke, UC Berkeley Physics 290H, February 12, 2008.

Seeing Stars with Radio Eyes Christopher G. De Pree RARE CATS Green Bank, WV June 2002.

The Environs of Massive Black Holes and Their Relativistic Jets Greg Taylor NRAO Albuquerque AAS, 2002 June 5.

Molecular Gas (Excitation) at High Redshift Fabian Walter Max Planck Institute for Astronomy Heidelberg Fabian Walter Max Planck Institute for Astronomy.

New tales of molecular gas in galaxies: (not so) near and far Jeff Wagg Max-Planck/NRAO Fellow NRAO – Socorro NRAO postdoc symposium Socorro April 29,

Galaxies with Active Nuclei Chapter 14:. Active Galaxies Galaxies with extremely violent energy release in their nuclei (pl. of nucleus).  “active galactic.

Cosmos Survey PI Scoville HST 590 orbits I-band 2 deg. 2 !

ALMA: Imaging the cold Universe Great observatories May 2006 C. Carilli (NRAO) National Research Council Canada.

Radio astronomical probes of the 1 st galaxies Chris Carilli, Aspen, February 2008  Current State-of-the-Art: gas, dust, star formation in QSO host galaxies.

C.Carilli, AUI Board October 2006 ISAC-run three year process: Quantified ‘experiments’ for future large area cm telescopes 50 chapters, 90 authors, 25%

ESO Radio observations of the formation of the first galaxies and supermassive black holes Chris Carilli (NRAO) Keck Institute, August 2010 Current State-of-Art:

Big Bang f(HI) ~ 0 f(HI) ~ 1 f(HI) ~ History of Baryons (mostly hydrogen) Redshift Recombination Reionization z = 1000 (0.4Myr) z = 0 (13.6Gyr) z.

The Evolution of Galaxies: From the Local Group to the Epoch of Reionization Fabian Walter National Radio Astronomy Observatory.

Warm Dust in the Most Distant Quasars Ran Wang Department of Astronomy, Peking University, China.

The M BH -  star relation at the highest redshifts Fabian Walter (MPIA)

What is EVLA? Giant steps to the SKA-high ParameterVLAEVLAFactor Point Source Sensitivity (1- , 12 hr.)10  Jy1  Jy 10 Maximum BW in each polarization0.1.

ESO Radio observations of the formation of the first galaxies and supermassive Black Holes Chris Carilli (NRAO) Notre Dame Astrophysics March 30, 2010.

ESO The other side of galaxy formation: radio line and continuum ‘Great Surveys’ Santa Fe November 2008 Chris Carilli NRAO.

High Redshift Galaxies/Galaxy Surveys ALMA Community Day April 18, 2011 Neal A. Miller University of Maryland.

Radio observations of massive galaxy and black hole formation in the early Universe Chris Carilli (NRAO) MPE, Garching, July 16, 2009  Introductory remarks.

Galaxy Evolution and WFMOS

Dust, cool gas, and star formation in z>6 SMBH host galaxies

Purple Mountain Observatory, May 2010

Evidence for a Population of high redshift Submm Galaxies

ALMA does Circumstellar Disks

ALMA studies of the first galaxies

Radio multiobject spectrograph C

Probing the Faint Radio Population

Dense Gas History of the Universe ‘Missing half of galaxy formation’

First galaxies: cm/mm observations Carilli (NRAO)

Xiaohui Fan University of Arizona June 21, 2004

Current and Future Science with NRAO Instruments

SKA KSP: probing cosmic reionization and the first galaxies

1st galaxies: cm/mm observations – fuel for galaxy formation

ALMA: Imaging the cold Universe

Giant Clouds and Star Clusters in the Antennae

1.4 GHz Source Counts (Hopkins 2000)

What is EVLA? Build on existing infrastructure, replace all electronics (correlator, Rx, IF, M/C) => multiply ten-fold the VLA’s observational capabilities.

The Most Distant Quasars

ALMA and Cosmology The high-redshift Universe Advantages of mm/submm

Extragalactic Science

Radio observations of dust and cool gas in the first galaxies

ALMA: Imaging the cold Universe

Dense gas history of the Universe  Tracing the fuel for galaxy formation over cosmic time SF Law SFR Millennium Simulations, Obreschkow & Rawlings 2009;

Evolution of radio telescopes (Braun 1996)

Radio Observations of Nearby HST BL Lacs

Black Holes in the Deepest Extragalactic X-ray Surveys

Galaxies With Active Nuclei

Observing Molecules in the EoR

Galaxies With Active Nuclei

ALMA: Resolving (optically) obscured galaxy formation

Presentation transcript:

Chris Carilli (NRAO) AAS06 NRAO 50th

CMB/WMAP – geometry of universe + seeds of cosmic structure from BB 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 T_univ = 13.6 Gyr Realm of the Galaxies HST/VLA+MERLIN Chapman + T_univ = 13.6 Gyr Realm of the Galaxies HST/CO Wilson et al

First Light + Reionization 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

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] Undetected in 38 hrs on JCMT by Bolatto et al. 04 [C II] was detected in over 12 hrs with the 30m to peak intensity 12 (4) mJy; with ALMA it will be 5 sigma in a minute. But J1148 has L=2 x 10^13. With 16 antennas, of course, we could get this in ten minutes. CO 6-5 1” IRAM

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

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

END

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

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

The CMB From NRAO HEMTs OVRO/BIMA

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

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

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

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)