1. Cosmic ‘Background’Radiation Franceschini 2000

2. The Gunn Peterson Effect Fan et al 2003 z=6.3 z=5.80 z=5.82 z=5.99 z=6.28 Cosmic reionization at z =6.3 => opaque at _obs <1  m Fan et al 2000

3. Radio observations of (obscured) high z galaxies and QSOs Carilli, Bertoldi, Walter, Cox, Yun, Owen, Voss, Beelen, Omont, Fan, Strauss, Menten, Djorgovski, Mahabal, Dannerbauer, Lutz, Genzel, Gnedin, Hasinger    and VLA  observations of ‘submm’ galaxies: contribution of dusty starbursts to the cosmic star formation budget => formation of spheroidal galaxies?  Dust and molecular gas in high redshift QSOs: coeval starburst and AGN at high redshift => coeval formation of SMBH and host galaxies? 3. Observations of the highest redshift objects during the Epoch of Reionization. 4. HI 21cm signal from the neutral IGM during the EoR.

4. MAMBO + IRAM 30m Wide field  imaging and photometry at 250 GHz : rms = 30’ Max-Planck Bolometer array: 133 pixel bolometer camera at 300mK, single mode horns (Kreysa)

5. 1. Wide -field imaging at 1.4 GHz: rms=7uJy, 1” res, FoV=30’ Astrometry => avoid confusion Imaging => AGN vs. Starburst, Lensing? cm-to-mm SEDs => redshifts, star formation rates unhindered by dust 2. Low order CO transitions at 20 to 50 GHz: rms < 0.1 mJy, res < 1” Gas excitation and mass estimates Gas distribution and dynamics, Lensing? Very Large Array

6. Plateau de Bure Interferometer Imaging high order CO lines at 90 to 230 GHz: rms < 0.5 mJy, res < 1” (15% of collecting area of ALMA)

7. Optical – 1e4 Galaxies SCUBA – 1 to 4 ‘Submm Galaxies’ Hughes et al. 1998 Rms=0.5 mJy Peak=7mJy

8. PdBI/VLA position => K = 23.5 (Dunlop et al.) I – K > 5.2 z = 4 +/- 1 S _250 = 2.1 +/- 0.3 mJy S _1.4 = 16 +/- 4 uJy L _FIR =7e12 L _sun Grav. Mag. = 3x ? Difficulty – Optically faint and confused

9. Magic of (sub)mm 350 GHz 250 GHz L _FIR = 1e12 x S _350 (mJy) L _sun for z=0.5 to 8

10. Dust obscured star formation at high z?  Redshift distribution?  AGN contribution?  Relationship to other galaxy populations? 1000x increase in CM density ULIRG to z=2 - 3 Dominate SFRD at high z? (Hughes etal)

11. Possible analog – ULIRG MRK 273 Z=0.037 L _FIR = 1e12 L _sun SFR = 300 M _sun /yr Size = 300 pc M _gas = 3e10 M _sun T _depletion =1e8 yr => ‘starburst’ P _ISM = 100 x P _disk 30kpc 100pc

12. UV selected galaxies – large range in bolometric luminosity, but little correlation of L _uv and L _bol Adelberger 2000

13. Optically faint radio sources (S _1.4 > 40 uJy) – significant overlap with (sub)mm galaxies  Increase sample  Arcsecond positions  Redshifts – cm/mm and optical  Low z bias? I=19 to 23 z=0.1 to 1 spirals I>25 40% detection rate at S _350 > 6mJy = (sub)mm galaxies? Chapman et al. 2003; Richards 1999; Barger 1999

14. Mambo deep fields: bright faint source survey rms = 0.5 to 2 mJy, Total area = 0.5 deg^2 A2125 NTTDF Lockman hole

15. Mapping procedure Raster scan at 4”/sec in AZ 1 hr/map over 240”x200”, rms=2mJy 2Hz, 50” chop Dynamic sched: tau < 0.2 Shift+Add + sky noise subtraction

16. VLA image: N(>40 uJy) = 1 arcmin^-2

17.  70% of S_250 > 2mJy have S_1.4 > 30 uJy (SCUBA finds 60 – 70%) K=21 ‘Typical’ example: A2125-IRAM1 I>25

18. MAMBO sources in NTTDF with arcsec positions (VLA or PdBI) Dannerbauer et al. 2003

19.  Large range in K (> 4 mag)  MAMBO: median K (+limits) = 21.5, I=25.5 (or 70% have K > 20) vs.  SCUBA: median K (+limits) = 19.6, 23.4 (or 36% have K > 20)  5/18 = EROs MAMBO/NTTDFSCUBA/8mJy

20. NTTDF sources with PdBI positions: High redshift + Highly reddened?

21. 8/22 = Radio/Xray = intermediate z AGN? 1?/13 = Xray/MAMBO 8/13 = Radio/MAMBO = high z starbursts? Radio-Xray-MAMBO comparison MAMBO/SCUBA (Eales et al): 6/9 in Lockman hole 14/19 in NTTDF, A2125

22. AGN in (sub)mm Galaxies: Xray observations of CDF-N Alexander et al. 2003  N(H) = 1e23 cm^-2  L _AGN = 1e43-44 erg/s = 0.1 x L_FIR  7/10 = Xray/submm  5/7 = AGN (flat spectrum)

23. AGN in blind (SUB)MM surveys Three brightest sources in MAMBO wide area survey are AGN with variable non-thermal mm emission Z S _250 S _95 S _1.4 1? 60 89 26 mJy 0.29 19 26 24 1.38 12 37 53  Factor 2 more than expected  Good news for ALMA calibration?

24.  100 src/deg^2 with S _250 >3mJy  High luminosity cutoff (non- evolving) – consistent w. ‘Lehnert/Heckman limit’: S _max = 3mJy => L _max = 7.5e11 L _sun L _SB,max = 7e11 (M _gas /1e10) L _sun

25. HST imaging – Chapman et al. 2003  85% interacting  Bigger than Ly Break galaxies (20 vs 10 kpc)  Lower surface brightness than LBGs

26.  Confirmation of optical identification  dynamical mass ~ (2-5) 10 10 M _sun  gas mass ~ (1-7) x 10 10 M _sun  9/11 detected so far Gas reservoirs: CO observations (Neri et al. 2003)

27. Clustering around known high z objects: Radio galaxy 1338-1942 at z=4.1 4x overdensity of mm sources (de Breuck et al. 2003; Ivison et al. 2001) Clustering with other types of sources: Radio companions in 40%

28. Clustering – correlation functions  Very broad z distribution => angular correlation is washed-out  Statistics remain poor (10’s of sources)  Physical correlation => most strongly clustered of high z source populations (no evolutionary connection w. LBGs?) Smail + 2003

29. Redshift distribution: Radio photometric redshifts

30. Radio photometric redshifts: assumptions and pitfalls Radio-FIR holds to high redshift? Garrett 2002 IC losses off CMB L _1.4 L _FIR z=1

31. Radio photometric redshifts: assumptions and pitfalls Universal SED – temperature – redshift degeneracy (Blain 1999) Photometric redshifts for NTTDF MAMBO sources: radio vs. optical (ULIRG template SED) 55K => z=4.1 65K => z=5.1

32. Redshift distribution of MAMBO sources: radio photometric redshifts  50% of radio detections in z=1.5 to 3.5  radio non-detections: 35% at z>3.5? Or cold dust (<30K)? (or spurious sources?)

33. Spectroscopic redshifts: radio-selected sample (Chapman et al. 2003) z _med = 2.4 50% in 1.9 – 2.8 Pitfalls: completeness (50 +/- 20%?) Low redshift bias

34. Modeling the (sub)mm galaxy population (Voss et al. 2003)  60 um luminosity function (Sanders)  SED – SLUGS sample (Dunne+Eales)  Luminosity evolution  High Lum. Cut-off, independent of z

35. Submm BG 60um counts

36. Contribution of (sub)mm galaxies to cosmic star formation Comparable SFR at high z in dusty starbursts as LBGs?

37. (sub)mm Galaxy Properties  z _med = 2.4, 50% in z=1.5 to 3.5, What fraction lies at z > 4 ?  70% have S _1.4 > 30 uJy; 50(+/- 20)% have K > 20  L _FIR = 1e13 L _sun, SFR = 1e3 M _sun /yr  1000x CM density wrt low z ULIRGs; comparable SFRD to LBGs  30% are EROs (R-K > 6), comprise 10% of ERO population  Only 10% of LBGs are (sub)mm gals; clustering => no evolutionary connection?  50(+/- 20)% host AGN, but L _AGN = 0.1 x L _bol  Optically brighter: interacting galaxies, high gas/dyn mass  Highly clustered (but hard to quantify)  S _250 >10 mJy => pop. dominated by flat spectrum AGN

38.  CM density (sub)mm galaxies (corrected for duty cycle) = 1e-4 Mpc^-3 = CM density of > L* ellipticals => Elliptical galaxy formation via major mergers at z = 2 to 3 (Smail et al., Barger et al., Lilly et al., Voss…)?  Strong clustering of submm galaxies  High stellar densities in E/S0 cores = gas densities in ULIRGs (Kormendy and Sanders 1992)  EROs are old, z = 1 ellipticals => z _f > 2 (Daddi 1999)  Stellar ages and uniform properties of low z ellipticals => z _f > 2 (Renzini, Ellis) => (sub)mm galaxies are revealing the formation of large (cluster) elliptical galaxies in massive starbursts at z=2 to 3 (1000 M _sun /yr over 1e8 yrs)?

39. SDSS + DPOSS: 700 at z > 4 30 at z > 5 7 at z > 6 M _B L _bol > 1e14 L _sun M _BH > 1e9 M _sun Hunt 2001 High redshift QSOs

40. QSO host galaxies – M _BH – sigma relation Most low z spheroidal galaxies have SMBH M _BH = 0.002 M _bulge  ‘Causal connection between SMBH and spheroidal galaxy formation’ (Gebhardt et al. 2002)?  Luminous high z QSOs have massive host galaxies (1e12 M _sun )

41. 30% of luminous QSOs have S _250 > 2 mJy, independent of redshift from z=1.5 to 6.4 L _FIR = 1e13 L _sun = 0.1 x L _bol : Dust heating by starburst or AGN? MAMBO surveys of z>2 DPSS+SDSS QSOs 1148+56 z=6.4 2322+1944 z=4.1

42. 2322+1944 z=4.12 CO(1-0) w. VLA (22 GHz): L _FIR = 3e13 L _sun M(H _2 ) = 1e11 M _sun 0.8 mJy

43. A Molecular Einstein Ring: VLA 45 GHz observations of CO2-1 emission from the gravitationally lensed QSO 2322+1944 at z=4.12 (Carilli et al. 2003; Djorgovski et al. 2003) Keck RbandVLA CO2-12” Res=0.5”,  =50uJy

44.  V = 250 km/s/kpc M _dyn = 4e10 (sin(i))^-2

45. CO spatially separated from QSO by 2 kpc => disk? 2322+19: Lens Model

46. => Coeval galaxy and formation SMBH? Rad-FIR SED=M82

47. submm CO + HST 1.4 GHz + optical

48. History of IGM bench-mark in cosmic structure formation indicating the first luminous structures Epoch of Reionization (EoR)

49. z=5.80 z=5.82 z=5.99 z=6.28 The Gunn Peterson Effect Fan et al 2003 Fast reionization at z =6.3 => opaque at _obs <1  m f(HI) > 0.001 at z = 6.3

50. Evolution of the neutral IGM (Gnedin): ‘Cosmic Phase transition’ HI fraction densityGas Temp Ionizing intensity

51. Thompson scattering => polarization Large scale structure (10’s deg) = Thompson scattering at EoR   e = Ln _e   e =0.12 to 0.17 => F(HI) < 0.5 at z=20 WMAP Large scale polarization of CMB (Kogut et al.) GP + WMAP => Reionization Process is complex, extending from z~20-6? (200-800 Million years after Big Bang)

52. Fan et al. 2002 Near-edge of reionization: GP Effect Fairly Fast f(HI) > 1e-3 at z >= 6.4 (0.87Gyr) f(HI) < 1e-4 at z <= 5.7 (1.0 Gyr) Problem:  _Lya >> 1 for f(HI) > 0.001 White et al. 2003

53. highest redshift quasar known L _bol = 1e14 L _sun central black hole: 1-5 x 10 9 M sun ( Willot etal.) clear Gunn Peterson trough (Fan etal.) Objects within EoR: QSO 1148+52 at z=6.4

54. 1148+52 z=6.42: MAMBO detection S _250 = 5.5mJy => L _FIR = 1.3e13 L _sun, M _dust =7e8 M _sun 

55. VLA Detection of Molecular Gas at z=6.419 46.6149 GHz CO 3-2 Off channels 50 MHz ‘channels’ (320 kms -1,  z=0.008) noise: ~57  Jy, D array, 1.5” beam  M(H_2) = 2e10 M _sun  Size < 1.5” (image),  Size > 0.2” (T _B /50K)^-1/2

56. IRAM Plateau de Bure confirmation FWHM = 305 km/s z = 6.419 +/- 0.001 T kin =100K, n H2 =10 5 cm -3  (3-2) (7-6) (6-5)

57. VLA imaging of CO3-2 at 0.17” resolution  Two sources of 0.2” in size and 0.20 mJy => T _B = 20K  ULIRGs: T _B (CO 2-1) = 15 to 50 K (Downes and Solomon 1998), but size is 10x smaller  Separation = 0.3”=2 kpc => M dyn =4e10 M sun (sin i) -2  Merging galaxies? rms=40uJy at 47GHz

58. Phase stability: Fast switching at the VLA 10km baseline rms = 10deg

59. 1148+52: starburst+AGN? SFR = 3000 M _sun /year => coeval formation of SMBH and host galaxy? VLA A array: S _1.4 =46+/-26 uJy

60. M( dust ) = 7e8 M _sun M( H _2 ) = 2e10 M _sun M _dyn = 4e10 (sin i) -2 M _sun M _BH = 3e9 M _sun M _BH –  => M _bulge = 1e12 M _sun ? 1148+52 Mass estimates Gas/dust = 30, typical of ULIRGs Dynamical vs. gas mass => baryon dominated, face-on disk – consistent with blue QSO (rest-frame) spectrum Dynamical vs. ‘bulge’ mass => M –  breaks-down at high z? 1148+52: Masses

61. Cosmic (proper) time  T _univ

62. Timescales for 1148+52 Age of universe: 8.7e8 yr Time since ‘start of reionization’ (z=20?): 6.9e8 yr SMBH formation (n x 1/e): n x 4e7 yr (Loeb, Wyithe,…) Elliptical galaxy (star) formation: 3e7 yr Cosmic Stromgren sphere creation (= QSO activity): 1e7 yr C, O production (3e7 M _sun ): 1e8 yr Fe production (SNe Ia): few e8 yr (Maiolino +, Freudling +)  SF ‘activity’ started early (z > 10), QSO later (Wyithe +) ? Dust formation: 1.4e9yr (AGB winds) => dust formed in high mass stars/SNR (Dunne et al.. 2003) ? => silicate grains?  Timescales

63. Ionizing sphere around QSO Direct Evidence that we are witnessing Re-Ionization of Universe! accurate redshift from CO: z=6.419 (optical high ionization lines can be off by 1000s km s -1 ) proximity effect: Photons leaking from 6.32<z<6.419 z=6.32 ionized sphere around QSO: R = 4.7 Mpc ‘time bounded’ Stromgren sphere: t _qso = 1e5 R^3 f(HI)= 1e7yrs (Haiman and Cen) White et al. 2003

64. Loeb-Rybicki halos

65. Constraints on neutral fraction at z=6.4? (Wyithe and Loeb 2003)  GP => f(HI) > 0.001  If f(HI) = 0.001, then t _qso = 1e4 yrs – implausibly short (see also J1030+0524 z=6.28)  Probability arguments suggest: f(HI) > 0.1 at z=6.4 – much better limit than GP => Very Fast Reionization (F(HI) < 1e-4 at z=5.7)

66. White etal (2002): ‘superluminal’ ionization front  Stromgren sphere expands at close to speed of light => obs Ly  photons emitted just after ionizing photons  “Delay required to allow light to travel from source to the edge of the sphere is exactly compensated by the ‘speedup’ that results from that edge being closer to the observer”  “Expansion law for the observed radius is exactly the same as the expansion law derived ignoring light-travel effects”

67. Gravitational Lensing?  Keck near IR imaging: source < 0.5” at K (Djorgovski)  ACS imaging: point source (Fan priv comm)  CO: Extended by 0.3”  Radio continuum: Foreground cluster, z=0.3 => magnification by 2x?

68. Gas and dust in the first galaxies Luminous (star forming?) galaxy: Far IR Luminosity = 1e13 L sun at z=6.42 Massive (merging?) galaxy: Molecular gas mass = 2x10 10 M _sun, M _dyn = 4e10 (sin i) -2 M _sun Very rapid enrichment of heavy elements and dust produced in the first stars => star formation commenced at 0.5 Gyr after the big bang Coeval formation of SMBH + stars in earliest galaxies (break-down of M-  at high z?) Cosmic Stromgren sphere of 4.7 Mpc => witnessing process of reionization => t _qso = 1e7 * f(HI) yrs => ‘fast’ reionization: f(HI)>0.1 at z=6.4?

69. J1048+4637: A second CO source at z=6.2 CO 6-5

70. Cloverleaf – z=2.56, Grav. Lens mag. 11x VLA detection of HCN emission at 22 GHz => n(H _2 ) > 1e5 cm^-3 (vs. CO n(H _2 ) > 1e4 cm^-3) (Solomon, vd Bout, Carilli)

71. ALMA/EVLA/GBT redshift coverage for CO VLA CO(3-2), PdBI CO 6-5, 7-6 in J1148+5251 @ z=6.42 Epoch of Reionization +other lines: HCN, HCO +, C I, C II, H 2 O, O 2

72. The Future (is now): Probing the EoR! Study physics of the first luminous sources This can only be done at near-IR to radio wavelengths Currently limited to pathological systems (‘HLIRGs’) SKA and ALMA 10- 100x sensitivity is critical for study of ‘normal’ galaxies z 

73. SKA Design Goals Max. Baselines CO/molecules: at least 50% at < 30 km Synchrotron: baselines out to > 1000 km Frequency range - at least to 22 GHz - major gains if extended to 40 GHz

74. 2322+1944 1.4 GHz VLA Radio continuum is cospatial w. molecular gas+dust, not AGN  Star forming disk of radius 2kpc surrounding QSO w. SFR (>5M_sun) = 2000 M _sun /yr

75. 1409+56 z=2.58: CO emission M _dust =1e8 M _sun, M(H _2 ) = 1e10 M _sun

76. Objects within the EoR: Star forming galaxy at z=6.56 (Hu et al)

77. SKA and ALMA: Optimal CO searches (Carilli & Blain)  SKA/ALMA – comparable speed at 22 GHz, SKA clearly faster at 43 GHz (FoV, fractional bandwidth, sensitivity)  SKA/ALMA – complementary: high vs. low order transitions

78. SKA and CO 

79. Radio studies of the first luminous objects CO (+other molecules) at z>4 VLA:   in  hrs for L _FIR = 1e13 M _sun (‘HLIRG’) SKA (20 – 40 GHz): 3  in 3hrs for L _FIR =1e11 M _sun (‘LIRG’) Radio  Continuum studies of star forming galaxies 1e13 L _sun 1e12 L _sun 1e11 L _sun

80. CO results Molecular Gas mass: M H2 = 2x10 10 M sun Size limits: 0.2”<D<1.5” (1”=5.6 kpc) FWHM = 305 km/s Dynamical Mass:M dyn =(3-14)x10 9 M sun (sin i) -2 precise redshift z=6.419 Star formation rate = 3000 M _sun /yr mass in C and O: ~3x10 7 M sun ; -> ISM enrichment must have started at z>8

81. Cloverleaf: z=2.56 Largest (apparent) CO, dust emission at z>2: L _FIR = 2e14L _sun Optical spectrum => QSO, M _v = -29 Imaging => gravitationally magnified by factor 11 CO 7-6 contours HST greyscale (Alloin et al.)

82. Weak correlation of L _FIR – M _B? Dust heating: AGN vs. Star Formation (1e3 M _sun /yr)? M_B > -26: 10% detected at 250 GHz mJy sensitivity M_B < -26: 30% detected

84. CO vs. FIR luminosity: dust (always) => gas Index=1 Index=1.7 40 300  Inceased star formation efficiency with FIR luminosity?  AGN contribution to dust heating?  M(H _2 ) = X * L’(CO) where X = 4 (galaxy), = 0.8 (ULIRGs) => M(H _2 ) = 1e10 to 1e11 M _sun for FIR-luminous z>2 QSOs

85. z = 2 sample 1409+56

86. 1409+56 z=2.58: CO emission M _dust =1e8 M _sun, M(H _2 ) = 1e10 M _sun

87. Z=2 sample: radio observations 8/8 of FIR-luminous QSOs detected at 1.4 GHz at = 0.14 to 1.0 mJy 3/8 non-FIR-luminous QSOs detected, and all 3 are < 0.17 mJy FIR luminous z=2 QSOs follow Radio-FIR correlation for star forming galaxies

88. B1202-0725 at z=4.7 VLA CO 2-1: Size/component = 0.3” = 2 kpc 0.6” 0.3”  Single optical QSO  Double radio/CO/dust source: starburst companion at 30 kpc? M(H _2 ) = 1e11 M _sun  T _B (CO 2-1) = 25 K  ULIRGs: T _B (CO 2-1) = 15 to 50 K (Downes and Solomon 1998), but size is 10x smaller Ly  Hu  + radio cont.

89. 1409+56 VLA + VLBA images at 1.4 GHz T _B < 1.2e5 K = ‘Condon starburst/AGN limit’ 2” 0.1” S _1.4 =1mJy F _1.4 <0.2 mJy/beam Mixed thermal +non-thermal: free-free absorption limits T _B < 1e5 K Empirically followed by low z star forming galaxies

90. HCN in starbursts: star forming gas tracer (Solomon & Gao 2000) CO measures total molecular gas: non-linear with L _FIR HCN measures dense gas directly associated with star formation: linear w. L _FIR => SF efficiency (SFR/total gas mass) rises w. L _FIR, % of dense gas rises with L _FIR Cloverleaf: under-luminous in HCN => some dust heating by AGN? Cloverleaf

91. z = 4 sample 2322+19

92. CO excitation: LVG models n(H_2) > 1e5 cm^-3, T > 70 K => typical of active star forming regions

95. z > 6 sample – probing the EoR