Star formation at high redshift (2 < z < 7) Methods for deriving star formation rates UV continuum = ionizing photons (dust obscuration?) Ly = ionizing photons (dust obscuration?) Far IR = bolometric (covering factor?) Radio continuum (synchrotron) = empirical (radio – FIR correlation?) Radio free-free/RRLs = ionizing photons (sensitivity, spectral confusion?) All relate mostly to massive stars (> 5 M _sun ) => total SFR depends on extrapolation of IMF, and temporal behavior
Cosmic (proper) time
Radio-FIR correlation: tightest correlation in extragalactic astronomy Separating FF – Synch is difficult Synch. Free-free Thermal dust M82
SKA in context z=8 EVLA
Cosmic ‘background’: ½ starlight reprocessed by dust
Evolution of space density of luminous QSOs (Fan et al. 2003) Madau-Lilly plot: evolution of cosmic star formation rate density
Galaxy populations at high redshift (2 < z < 7) Radio galaxies: only z > 0.5 galaxies before 90’s UV dropouts/Ly-break: broadband colors Ly : narrow band imaging Submm: (sub)mm bolometer camera imaging QSO Hosts: HST, (sub)mm QSO absorption lines: metalicity evolution, parent galaxies z=0.3 to 2: EROs, faint blue, Butcher-Oemler, Jy radio sources, ISO GRB hosts Pop III stars: early reionization by 100 M _sun stars in minihalos at z = 20?
z = kpc High z radio galaxies (L _1.4 > 1e28 W/Hz) 10kpc z= z= z=
K-z relation: HzRGs = Giant Ellipticals z>8 radio galaxies?
Alignment effect: Jet-induced star formation? Clumpy morphologies => forming ellipticals? z=2.2
Alignement effect: Radio-Xray Radio-Ly halo 18kpc
Clustering on Mpc scales around HzRGs ( z=2.2) => protoclusters?
Dusty radio galaxies at high z? Overdensity of submm galaxies?
UV dropouts/Ly break (Ly
Star formation rates in Ly break galaxies Extinction uncorrected corrected
Correlation between extinction and SFR => L _UV is independent of SFR
Ly break galaxies = highly biased (ie. clustered) galaxy formation
Ly break galaxies with Ly halos
SUBMM galaxies: dust obscured galaxy formation HDF - optical HDF – 850 m
Dust obscured star formation dominates at z>2? Submm galaxies: L _FIR = 1e12 to 1e13 L _sun => SFR = 100 to 1000 M _sun /yr M _dust = 1e8-9 M _sun
Magic of submm 350 GHz 250 GHz
Brightest mm source in HDF: K = 23.5
Radio photometric redshifts: two colors, or ‘drop- outs’
Redshift distribution
Next step: photometric redshifts
CO emission => M(H _2 ) = 1e10-11 M _sun
Submm galaxies
QSO host galaxies Most low z spheroidal galaxies have SMBH M _BH = M _bulge => ‘Causal connection between SMBH and spheroidal galaxy formationn’ (Gebhardt et al. 2002)?
30% of luminous QSOs have S _250 > 2 mJy L_FIR > 7e12 M _sun Dust heating: starburst or AGN? z=6.4 S _250 =5.5mJy
Radio-to-IR SED = M82
CO(1-0) w. VLA: L _FIR = 3e13 L _sun M(H _2 ) = 1e11 M _sun
A Molecular Einstein Ring: VLA 45 GHz observations of CO2-1 emission from the gravitationally lensed QSO at z=4.12 (Carilli et al. 2003) Keck RbandVLA CO2-1 2”
Using the gravitational lens to probe sub-kpc scales in : A starburst disk surrounding a SMBH => coeval SMBH – galaxy formation? Optical QSO Starburst disk: molecular gas, dust, radio continuum
Starbursts in QSO host galaxies? 30% of luminous QSOs (M _B < -27) have L _FIR = 1e13 L _sun (independent of redshift) Z= 2 sample: All L _FIR luminous QSOs detected at 1.4 GHz, and in all cases ‘q’ consistent with star forming galaxy (2.3 +/- 0.3)
Questions Relationships between different high z galaxy types? Halos masses and end-products (spirals, ellipticals)? Is > 1000 M _sun /yr possible, sustainable (Heckman limit)? IMF: top heavy? Star formation in extreme environments (P=100xISM)? Timescales? Dust formation at z>6: >1e8 M _sun in < 0.7 Gyr? What fraction of high z galaxy formation is dust-obscured? Submm galaxies – redshift distribution? radio – FIR correlation: mechanism? vs. redshift? M- relation – coeval SMBH and galaxy formation? QSO dust heating: star formation or AGN? L _FIR from S _250 ? X = gas mass to CO luminosity conversion? L _FIR to dust mass conversion? Pop III stars, minihalos, and first luminous objects: role of radio astronomy?