History of IGM

1
History of IGM
Epoch of Reionization (EoR)

• bench-mark in cosmic
• structure formation
• indicating the first
• luminous structures

2
The Gunn Peterson Effect
Fast reionization at z6.3 opaque at
l_obs
f(HI) 0.001 at z 6.3
Fan et al 2003
3
WMAP Large scale polarization of CMB (Kogut et
al.)
20deg

• Thompson scattering at EoR
• t_e Ln_es_e 0.17
• F(HI)

4
Near-edge of reionization GP Effect
Fan et al. 2002

• Fairly Fast
• f(HI) 1e-3 at z 6.4 (0.87Gyr)
• f(HI)
• Problem t_Lya 1 for
• f(HI) 0.001

5
Radio astronomical probes of the Epoch of
Reionization and the 1st luminous objects

• CMB large scale polarization
• Objects within EoR Molecular gas, dust, star
  formation, first AGN unbiased by obscuration
  (dust, HI)
• Neutral IGM HI 21cm emission and absorption

• SKA level 0 science team Carilli, Furlanetto,
  Briggs, Gnedin, Rawlings, Falcke
• Material from chapters by Blain, van der Hulst,
  Jarvis, Jackson, Falcke

6
Objects within the EoR Star forming galaxy at
z6.56 (Hu et al) SFR 10 M_sun/yr
7
Objects within EoR Luminous QSO 114852 at z6.4

• highest redshift quasar known
• L_bol 1e14 L_sun
• central black hole 1-5 x 109 Msun (Willot
  etal.)
• clear Gunn Peterson trough (Fan etal.)

8
dust in high-z quasars
MAMBO surveys of z2 DPSSSDSS QSOs
114852

• 30 of luminous QSOs have S250 2 mJy L_FIR
  1e13 L_sun, independent of redshift from z1.5 to
  6.4
• FIR thermal emission from warm dust

9
114852 z6.42 MAMBO 250 GHz detection S_250
5.0 /- 0.6 mJy L_FIR 1.2e13 L_sun,
M_dust 7e8 M_sun
3

10
VLA Detection of Molecular Gas at z6.419
50 MHz channels (320 kms-1, Dz0.008) noise
57 mJy, D array, 1.5 beam
46.6149 GHz CO 3-2
Off channels

• M(H_2) 2e10 M_sun
• Size
• Size 0.2 (T_B/50K)-1/2

11
IRAM Plateau de Bure confirmation
n2
(6-5)
(7-6)
(3-2)

• FWHM 305 km/s
• z 6.419 /- 0.001

• Tkin100K, nH2105cm-3

12
VLA imaging of CO3-2 at 0.4 and 0.15 resolution
rms50uJy at 47GHz

• Separation 0.3 1.7 kpc
• T_B 20K T_B (starburst)
• Merging galaxies?
• Or Dissociation by QSO?

• CO extended to NW by 1 (5.5 kpc) tidal(?)
  feature
• M_dyn 6e10 M_sun

13
114852 starburstAGN?
S_1.4 55 /- 12 uJy
IRAS 2Jy sample (Yun)
104846
114852

• SFR(5 M_sun) 1400 M_sun/year host spheroid
  formation in 5e7 yrs at z 6?
• SMBH formation n x 2.4e7 yr (Loeb, Wyithe,)
• Coeval formation of galaxy/SMBH at z6?

14
Beelen et al. 2004
15
Cosmic Stromgren Sphere

• Accurate redshift from CO z6.419
• optical high ionization lines off by 1000s km/s
  (Dz0.03)
• Proximity effect photons leaking from
  6.32

z6.32
White et al. 2003

• Ionized sphere around QSO R 4.7 Mpc time
  bounded Stromgren sphere
• t_qso 1e5 R3 f(HI) 1e7yrs

16
Loeb Rybicki 2000
17
Constraints on neutral fraction at z6.4

• GP f(HI) 0.001
• If f(HI) 0.001, then t_qso 1e4 yrs
  implausibly short? (see also J10300524 z6.28,
  J104846 z6.23 using MgII lines)
• Probability arguments suggest f(HI) 0.1 at
  z6.4 much better limit than GP

Wyithe and Loeb 2003 f_lt 1e7 yr
18
Near-edge of reionization GP Strom. Spheres
Fan et al. 2002

• Very Fast?
• f(HI) 1e-1 at z 6.4 (0.87Gyr)
• f(HI)

19
Gas and dust during the EoR

• FIR luminous galaxy at z6.42 1e13 Lsun
• observe dust, gas, star formation, AGN
• Merging(?) galaxy Molecular gas mass
• 2x1010 M_sun, M_dyn 6e10 M_sun
• Early enrichment of heavy elements
• and dust produced in the first
• stars star formation commenced at
• 0.4 Gyr after the big bang
• Coeval formation of SMBH stars in
• earliest galaxies break-down of M-s 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 z6.4?

20
Radio studies of the first luminous objects
Radio Continuum studies of normal star forming
galaxies
1e13 L_sun
1e12 L_sun
1e11 L_sun
Hopkins model of galaxy evolution 7000 galaxies
at z 5 per FoV at 1.4 GHz per 8hr integration
(but cf. Jackson)
21
SKA and CO
M 82

• VLA 3s in 3 hrs for L_FIR 1e13 M_sun
  (HLIRG)
• SKA (20 40 GHz) 3s in 3hrs for L_FIR 1e11
  M_sun (LIRG)

22
SKA and ALMA Optimal CO searches (Carilli
Blain)
EoR

• 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

23
Cloverleaf z2.56, Grav. Lens mag. 11x VLA
detection of HCN emission at 22 GHz n(H_2)
1e5 cm-3 (vs. CO n(H_2) 1e3 cm-3) (Solomon,
vd Bout, Carilli)
24

• Radio-loud AGN within the EOR?
• Radio loud QSO fraction 10 to z5.8 (Petric
  2003)
• Models expect 0.05 to 0.5 deg-2 at z 6
  with S_151 6 mJy (out of 100 total)

Haiman Hui 2004
1.4e5 at z 6
S_151 6mJy
2240 at z 6
Carilli 2002
25
GMRT 230 MHz 0924-220 z5.2

• Continuum point source 0.55 Jy
• Noise limited spectra s5.5 mJy/channel
• HI 21cm absorption at z5.200? t 4, Dv 130
  km/s N(HI) 9e20 (Ts/100K) cm-2

26
Radio quiet AGN within the EoR (Falcke)
-- 50 radio detection rate

• Deep integration with SKA
• Detect 1e7 M_sun BHs to z10 with Eddtington
  limited accretion
• Detect 1e9 M_sun BHs with 1 Eddington accretion

27
Continuum sensitivity of future telescopes Arp
220 vs z
Panchromatic view of the first luminous objects
stars, star formation, gas, dust, dark matter,
(accreting) black holes
28

• SKA Design Goals
• Max. Baselines
• CO/molecules at least 50 at
• Synchrotron baselines out to 1000 km
• Frequency range
• - at least to 22 GHz (A/T 10000)
• - major gains if extended to 40 GHz

29
Z10 lensed star forming galaxy? (Pello 2004)
L_app 4e11 L_sun LBG dust correction (5x)
L_FIR 2e12L_sun S_250 0.6 mJy 4s ALMA
detection in 1 minute! S (CO 4-3 at 42 GHz)
0.06 mJy 4s EVLA detection in 30hr
30
The Future Probing the EoR!

• Study physics of the first luminous sources in
  the EoR!
• This can only be done at near-IR to radio
  wavelengths
• Currently limited to pathological systems
  (HLIRGs)
• SKA sensitivity is critical for study of normal
  galaxies

z6.4