Purple Mountain Observatory, May 2010 Radio observations of the formation of the first galaxies and supermassive Black Holes Chris Carilli (NRAO) Purple Mountain Observatory, May 2010 Concepts and tools in radio astronomy: dust, cool gas, and star formation Quasar host galaxies at z=6: coeval formation of massive galaxies and SMBH within 1 Gyr of the Big Bang Bright (and near!) future: Atacama Large Millimeter Array and the Expanded Very Large Array Collaborators: R.Wang, D. Riechers, Walter, Fan, Bertoldi, Menten, Cox, Strauss, Neri ESO

Millimeter through centimeter astronomy: unveiling the cold, obscured universe Submm = dust optical mid-IR CO Galactic GN20 SMG z=4.0 optical studies provide a limited view of star and galaxy formation cm/mm reveal the dust-obscured, earliest, most active phases of star and galaxy formation HST/CO/SUBMM

Cosmic ‘Background’ Radiation 30 nW m-2 sr-1 17 nW m-2 sr-1 Over half the light in the Universe is absorbed and reemitted in the FIR Franceschini 2000

Radio – FIR: obscuration-free estimate of massive star formation Radio: SFR = 10-21 L1.4 W/Hz FIR: SFR = 3x10-10 LFIR (Lo)

Magic of (sub)mm: distance independent method of studying objects in universe from z=0.8 to 10 LFIR ~ 4e12 x S250(mJy) Lo SFR ~ 1e3 x S250 Mo/yr FIR = 1.6e12 L_sun 1000 Mo/yr obs = 250 GHz

Spectral lines cm submm z=0.2 z=4 Atomic fine structure lines Molecular rotational lines

Molecular gas CO = total gas masses = fuel for star formation M(H2) = α L’(CO(1-0)) Velocities => dynamical masses Gas excitation => ISM physics (densities, temperatures) Dense gas tracers (eg. HCN) => gas directly associated with star formation Astrochemistry/biology Wilson et al. CO image of ‘Antennae’ merging galaxies

Fine Structure lines [CII] 158um (2P3/2 - 2P1/2) Principal ISM gas coolant: efficiency of photo-electric heating by dust grains. Traces star formation and the CNM COBE: [CII] most luminous cm to FIR line in the Galaxy ~ 1% Lgal Herschel: revolutionary look at FSL in nearby Universe – AGN/star formation diagnostics [CII] CO [OI] 63um [CII] [OIII]/[CII] [OIII] 88um [CII] Cormier et al.

Powerful suite of existing cm/mm facilites MAMBO at 30m Powerful suite of existing cm/mm facilites First glimpses into early galaxy formation 30’ field at 250 GHz rms < 0.3 mJy Very Large Array 30’ field at 1.4 GHz rms< 10uJy, 1” res High res imaging at 20 to 50 GHz rms < 0.1 mJy, res < 0.2” Plateau de Bure Interferometer High res imaging at 90 to 230 GHz rms < 0.1mJy, res < 0.5”

Massive galaxy and SMBH formation at z~6: gas, dust, star formation in quasar hosts SDSS Apache Point NM Why quasars? Rapidly increasing samples: z>4: > 1000 known z>5: > 100 z>6: 20 Spectroscopic redshifts Extreme (massive) systems MB < -26 => Lbol > 1014 Lo MBH > 109 Mo (Eddington / MgII) 1148+5251 z=6.42

First galaxies and SMBH: z>6 => tuniv < 1 Gyr Gunn Peterson trough => pushing into cosmic reionization = first galaxies, black holes 1148+5251 z=6.42

QSO host galaxies – MBH -- Mbulge relation Nearby galaxies Haaring & Rix All low z spheroidal galaxies have SMBH: MBH=0.002 Mbulge ‘Causal connection between SMBH and spheroidal galaxy formation’ Luminous high z quasars have massive host galaxies (1012 Mo)

Cosmic Downsizing Massive galaxies form most of their stars rapidly at high z ~(e-folding time)-1 Currently active star formation tH-1 Red and dead => Require active star formation at early times Zheng+ Massive old galaxies at high z Stellar population synthesis in nearby ellipticals

Dust in high z quasar host galaxies: 250 GHz surveys HyLIRG Wang sample 33 z>5.7 quasars 30% of z>2 quasars have S250 > 2mJy LFIR ~ 0.3 to 1.3 x1013 Lo (~ 1000xMilky Way) Mdust ~ 1.5 to 5.5 x108 Mo

Dust formation at tuniv<1Gyr? AGB Winds ≥ 1.4e9yr High mass star formation? (Dwek, Anderson, Cherchneff, Shull, Nozawa) ‘Smoking quasars’: dust formed in BLR winds (Elvis) Extinction toward z=6.2 QSO and z~6 GRBs => different mean grain properties (Perley, Stratta) Larger, silicate + amorphous carbon dust grains formed in core collapse SNe vs. eg. graphite SMC, z<4 quasars Galactic z~6 quasar, GRBs Stratta et al.

Dust heating? Radio to near-IR SED low z SED TD ~ 1000K TD = 47 K FIR excess = 47K dust SED consistent with star forming galaxy: SFR ~ 400 to 2000 Mo yr-1 Star formation? AGN Radio-FIR correlation

Fuel for star formation Fuel for star formation? Molecular gas: 8 CO detections at z ~ 6 with PdBI, VLA M(H2) ~ 0.7 to 3 x1010 (α/0.8) Mo Δv = 200 to 800 km/s 1mJy

CO excitation: Dense, warm gas, thermally excited to 6-5 230GHz 691GHz starburst nucleus Milky Way LVG model => Tk > 50K, nH2 = 2x104 cm-3 Galactic Molecular Clouds (50pc): nH2~ 102 to 103 cm-3 GMC star forming cores (≤1pc): nH2~ 104 cm-3 18

LFIR vs L’(CO): ‘integrated Kennicutt-Schmidt star formation law’ Further circumstantial evidence for star formation Gas consumption time (Mgas/SFR) decreases with SFR FIR ~ 1010 Lo/yr => tc~108yr FIR ~ 1013 Lo/yr => tc~107yr => Need gas re-supply to build giant elliptical SFR 1e3 Mo/yr Index=1.5 MW 1e11 Mo Mgas

1148+52 z=6.42: VLA imaging at 0.15” resolution CO3-2 VLA IRAM 0.3” 1” ~ 6kpc + ‘molecular galaxy’ size ~ 6 kpc Double peaked ~ 2kpc separation, each ~ 1kpc TB ~ 35 K ~ starburst nuclei

Gas dynamics => ‘weighing’ the first galaxies z=6.42 -150 km/s 7kpc +150 km/s CO only method for deriving dynamical masses at these distances Dynamical mass (r < 3kpc) ~ 0.4 to 2 x1011 Mo M(H2)/Mdyn ≥ 0.1 to 0.5 => gas/baryons dominate inner few kpc

Break-down of MBH -- Mbulge relation at very high z z>4 QSO CO z<0.2 QSO CO Low z galaxies Riechers + <MBH/Mbulge> = 15 higher at z>4 => Black holes form first?

[CII] 158um search in z > 6.2 quasars For z>6 => redshifts to 250GHz => Bure! 1” [CII] [NII] L[CII] = 4x109 Lo (L[NII] < 0.1L[CII] ) S250GHz = 5.5mJy S[CII] = 12mJy S[CII] = 3mJy S250GHz < 1mJy => don’t pre-select on dust

1148+5251 z=6.42:‘Maximal star forming disk’ PdBI 250GHz 0.25”res [CII] size ~ 1.5 kpc => SFR/area ~ 1000 Mo yr-1 kpc-2 Maximal starburst (Thompson, Quataert, Murray 2005) Self-gravitating gas disk Vertical disk support by radiation pressure on dust grains ‘Eddington limited’ SFR/area ~ 1000 Mo yr-1 kpc-2 eg. Arp 220 on 100pc scale, Orion SF cloud cores < 1pc

Malhotra, Maiolino, Bertoldi, Knudsen, Iono, Wagg… [CII] [CII]/FIR decreases with LFIR = lower gas heating efficiency due to charged dust grains => luminous starbursts are still hard to detect in [CII] Opacity in FIR may also play role (Papadopoulos) Malhotra, Maiolino, Bertoldi, Knudsen, Iono, Wagg…

Malhotra, Maiolino, Bertoldi, Knudsen, Iono, Wagg… [CII] z >4 HyLIRG at z> 4: large scatter, but no worse than low z ULIRG Normal star forming galaxies are not much harder to detect Malhotra, Maiolino, Bertoldi, Knudsen, Iono, Wagg…

Summary cm/mm observations of 33 quasars at z~6: only direct probe of the host galaxies J1425+3254 CO at z = 5.9 J1048 z=6.23 CO w. PdBI, VLA 11 in mm continuum => Mdust ~ 108 Mo: Dust formation in SNe? 10 at 1.4 GHz continuum: Radio to FIR SED => SFR ~ 1000 Mo/yr 8 in CO => Mgas ~ 1010 Mo: Fuel for star formation in galaxies High excitation ~ starburst nuclei Follow star formation law (LFIR vs L’CO): tc ~ 107 yr 3 in [CII] => maximal star forming disk: 1000 Mo yr-1 kpc-2 Confirm decrease in RNZ with increasing z

Building a giant elliptical galaxy + SMBH at tuniv< 1Gyr 10 Multi-scale simulation isolating most massive halo in 3 Gpc3 Stellar mass ~ 1e12 Mo forms in series (7) of major, gas rich mergers from z~14, with SFR  1e3 Mo/yr SMBH of ~ 2e9 Mo forms via Eddington-limited accretion + mergers Evolves into giant elliptical galaxy in massive cluster (3e15 Mo) by z=0 6.5 Li, Hernquist et al. Li, Hernquist+ Rapid enrichment of metals, dust in ISM Rare, extreme mass objects: ~ 100 SDSS z~6 QSOs on entire sky Goal: push to normal galaxies at z > 6

What is Atacama Large Milllimeter Array? North American, European, Japanese, and Chilean collaboration to build & operate a large millimeter/submm array at high altitude site (5000m) in northern Chile => order of magnitude, or more, improvement in all areas of (sub)mm astronomy, including resolution, sensitivity, and frequency coverage.

ALMA Specs High sensitivity array = 54x12m Wide field imaging array = 12x7m antennas Frequencies = 80 GHz to 720 GHz Resolution = 20mas res at 700 GHz Sensitivity = 13uJy in 1hr at 230GHz

What is EVLA? First steps to the SKA-high By building on the existing infrastructure, multiply ten-fold the VLA’s observational capabilities, including: 10x continuum sensitivity (1uJy) Full frequency coverage (1 to 50 GHz) 80x Bandwidth (8GHz) 40mas resolution at 40GHz Overall: ALMA+EVLA provide > order magnitude improvement from 1GHz to 1 THz!

Pushing to normal galaxies: spectral lines 100 Mo yr-1 at z=5 cm telescopes: star formation, low order molecular transitions -- total gas mass, dense gas tracers (sub)mm: dust, high order molecular lines, fine structure lines -- ISM physics, dynamics

ALMA and first galaxies: [CII] and Dust 100Mo/yr 10Mo/yr

Wide bandwidth spectroscopy J1148+52 at z=6.4 in 24hrs with ALMA If one placed CO 6-5 in the LSB, one would get the 211-202 line of H2O and the 7-6 line of 13CO, in addition to several H2CO lines, in the USB. ALMA: Detect multiple lines, molecules per 8GHz band EVLA 30 to 38 GHz = CO2-1 at z=5.0 to 6.7 => large cosmic volume searches (1 beam = 104 cMpc3)

EVLA Status Antenna retrofits 70% complete (100% at ν ≥ 18GHz). Early science in March 2010 using new correlator (2GHz) Full receiver complement completed 2012 with 8GHz bandwidth

EVLA Early Science Results: GN20 molecule-rich proto-cluster at z=4 4.051 4.052 0.7mJy CO2-1 46GHz 0.4mJy 1000 km/s

GN20 z=4.0 +250 km/s -250 km/s

ALMA Status Antennas, receivers, correlator in production: best submm receivers and antennas ever! Site construction well under way: Observation Support Facility, Array Operations Site, 3 Antenna interferometry at high site! Early science call Q1 2011 embargoed first light image

END

(sub)mm Dust, FSL, mol. gas Near-IR: Stars, ionized gas, AGN Pushing to normal galaxies: continuum A Panchromatic view of 1st galaxy formation 100 Mo yr-1 at z=5 cm: Star formation, AGN (sub)mm Dust, FSL, mol. gas Near-IR: Stars, ionized gas, AGN

Comparison to low z quasar hosts z=6 quasars IRAS selected Stacked mm non-detections PG quasars Hao et al. 2005

Molecular gas mass: X factor M(H2) = X L’(CO(1-0)) Milky way: X = 4.6 MO/(K km/s pc^2) (virialized GMCs) ULIRGs: X = 0.8 MO/(K km/s pc^2) (CO rotation curves) Optically thin limit: X ~ 0.2 Downes + Solomon