cosmic reionization and the history of the neutral intergalactic medium lanl
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Cosmic reionization and the history of the neutral intergalactic medium LANL Chris Carilli May 23, 2007. Current constraints on the IGM neutral fraction with cosmic epoch (Fan, Carilli, Keating 2006 ARAA) Neutral Intergalactic Medium (IGM) – HI 21cm telescopes, signals, and challenges - PowerPoint PPT PresentationTRANSCRIPT
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Cosmic reionization and the history of the neutral intergalactic medium
LANL
Chris Carilli May 23, 2007
Current constraints on the IGM neutral fraction with cosmic epoch (Fan, Carilli, Keating 2006 ARAA)
Neutral Intergalactic Medium (IGM) – HI 21cm telescopes, signals, and challenges
Objects within reionization – recent observations of molecular gas, dust, and star formation, in the host galaxies of the most distant QSOs, and more…
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Ionized
Neutral
Reionized
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Chris Carilli (NRAO)
Berlin June 29, 2005
WMAP – structure from the big bang
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Hubble Space Telescope Realm of the Galaxies
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Dark Ages
Twilight Zone
Epoch of Reionization
• Last phase of cosmic evolution to be tested • Bench-mark in cosmic structure formation indicating the first luminous structures
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QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
Gnedin 03
Reionization: the movie
8Mpc comoving
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Barkana and Loeb 2001
Constraint I: Gunn-Peterson Effect
z
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Gunn-Peterson Effect
Fan et al 2006
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Gunn-Peterson limits to f(HI)
End of reionization?
f(HI) <1e-4 at z= 5.7
f(HI) >1e-3 at z= 6.3
Difficulties with GP
• to f(HI) conversion requires ‘clumping factor’
• >>1 for f(HI)>0.001 => low f() diagnostic
• GP => Reionization occurs in ‘twilight zone’, opaque for obs <0.9 m
GP = 2.6e4 f(HI) (1+z)^3/2
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Reionization and the CMB
Thomson scatting during reionization (z~10)
Acoustics peaks are ‘fuzzed-out’ during reionization.
Problem: degenerate with intrinsic amplitude of the anisotropies.
Surface of last-scattering z~1000
No reionization
Reionization
CMB angular power spectrum
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TT
TE
EE
Constraint II: CMB large scale polarization -- Thomson scattering during reionization
Scattered CMB quadrapole => polarized
Large scale: horizon scale at reionization ~ 10’s deg
Signal is weak:
TE = 10% TT (few uK)
EE = 1% TT
EE (l ~ 5)~ 0.3+/- 0.1 uK
Page + 06; Spergel 06
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TT
TE
EE
Constraint II: CMB large scale polarization -- Thomson scattering during reionization
e = 0.09+/-0.03
Rules-out high ionization fraction at z> 15
Allows for finite (~0.2) ionization to high z
Most action occurs at z ~ 8 to 14, with f(HI) < 0.5
Page + 06; Spergel 06
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es with CMB polarization:
e = integral measure to recombination=> allows many IGM histories
• Still a 3 result (now in EE vs. TE before)
Combined CMB + GP constraints on reionization
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• Highest redshift quasar known (tuniv = 0.87Gyr)• Lbol = 1e14 Lo
• Black hole: ~3 x 109 Mo (Willot etal.)• Gunn Peterson trough (Fan etal.)
Pushing into reionization: QSO 1148+52 at z=6.4
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1148+52 z=6.42: Gas detection
Off channelsRms=60uJy
46.6149 GHzCO 3-2
• M(H2) ~ 2e10 Mo
• zhost = 6.419 +/- 0.001
(note: zly = 6.37 +/- 0.04)
VLA
IRAM
VLA
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Constrain III: Cosmic Stromgren Sphere
• Accurate zhost from CO: z=6.419+/0.001
• Proximity effect: photons leaking from 6.32<z<6.419
z=6.32
•‘time bounded’ Stromgren sphere: R = 4.7 Mpc• tqso = 1e5 R^3 f(HI)~ 1e7yrs or • f(HI) ~ 1 (tqso/1e7 yr)
White et al. 2003
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Loeb & Rybicki 2000
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CSS: Constraints on neutral fraction at z~6 Nine z~6 QSOs with CO or MgII redshifts: <R> = 4.4 Mpc (Wyithe et al. 05; Fan et al. 06; Kurk et al. 07)
GP => f(HI) > 0.001
If f(HI) ~ 0.001, then <tqso> ~ 1e4 yrs – implausibly short given QSO fiducial lifetimes (~1e7 years)?
Probability arguments + size evolution suggest: f(HI) > 0.05
Wyithe et al. 2005
=tqso/4e7 yrs
90% probability x(HI) > curve
P(>xHI)
Fan et al 2005
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Cosmic Stromgren Surfaces (Hui & Haiman)
• Larger CSS in Ly vs. Ly = Damping wing of Ly?
• Large N(HI) => f(HI) > 0.1
zhost
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Difficulties for Cosmic Stromgren Spheres and Surfaces
(Lidz + 07, Maselli + 07)
Requires sensitive spectra in difficult near-IR band
Sensitive to R: f(HI) R^-3
Clumpy IGM => ragged edges
Pre-QSO reionization due to star forming galaxies, early AGN activity
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Cosmic ‘phase transition’?
Not ‘event’ but complex process, large variance time/space
Current observations suggest: zreion ~ 6 to 14
Good evidence for qualitative change in nature of IGM at z~6
Current probes are all fundamentally limited in diagnostic power
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Studying the pristine neutral IGM using redshifted HI 21cm observations (100 – 200 MHz)
Large scale structure
cosmic density,
neutral fraction, f(HI)
Temp: TK, TCMB, Tspin
)1()10
1)((008.0 2/1 δ +
+= HI
S
CMB fz
TT
1e13 Mo
1e9 Mo
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Multiple experiments under-way: ‘pathfinders’
MWA (MIT/CfA/ANU) LOFAR (NL)
21CMA (China) SKA
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Signal I: Global (‘all sky’) reionization signature in low frequency HI spectra
Ly coupling: Tspin=TK < TCMB
IGM heating: Tspin= TK > TCMB
Gnedin & Shaver 03
140MHz
Signal ~ 20mK < 1e-4 sky
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EDGES (Bowman & Rogers MIT)
All sky reionization HI experiment. Single broadband dipole experiment with (very) carefully controlled systematics + polynomial baseline subtraction (7th order)
Treion < 450mK at z = 6.5 to 10
Sky > 150 K rms = 75 mK
VaTech Dipole Ellingson
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Signal II: HI 21cm Tomography of IGM Zaldarriaga + 2003
z=12 9 7.6
TB(2’) = 10’s mK
SKA rms(100hr) = 4mK
LOFAR rms (1000hr) = 80mK
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Signal III: 3D Power spectrum analysis
SKA
LOFAR
McQuinn + 06
only
+ f(HI)
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N(HI) = 1e13 – 1e15 cm^-2, f(HI/HII) = 1e-5 -- 1e-6
=> Before reionization N(HI) =1e18 – 1e21 cm^-2
Signal IV: Cosmic Web after reionization
Ly alpha forest at z=3.6 ( < 10)
Womble 96
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z=12 z=819mJy
130MHz
• radio G-P (=1%)
• 21 Forest (10%)
• mini-halos (10%)
• primordial disks (100%)
Signal IV: Cosmic web before reionization: HI 21Forest
• Perhaps easiest to detect (use long baselines)
• Requires radio sources: expect 0.05 to 0.5 deg^-2 at z> 6 with S151 > 6 mJy?
159MHz
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GMRT 230 MHz – HI 21cm abs toward highest z (~5.2) radio AGN
0924-220 z=5.2
S230MHz = 0.5 Jy
1”
8GHz Van Breugel et al.
GMRT at 230 MHz = z21cm
RFI = 20 kiloJy !
CO Klamer +
M(H2) ~ 3e10 Mo
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GMRT 230 MHz – HI 21cm abs toward highest z radio AGN (z~5.2)
rms(20km/s) = 5 mJy
229Mhz 0.5 Jy232MHz 30mJy
rms(40km/s) = 3mJy
N(HI) ~ 2e20TS cm^-2 ?
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Signal V: Cosmic Stromgren spheres around z > 6 QSOs
0.5 mJy
LOFAR ‘observation’:
20xf(HI)mK, 15’,1000km/s
=> 0.5 x f(HI) mJy
Pathfinders: Set first hard limits on f(HI) at end of cosmic reionization
Easily rule-out cold IGM (T_s < T_cmb): signal = 360 mK
Wyithe et al. 2006
5Mpc
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Signal VI: pre-reionization HI signal, eg. Baryon Oscillations
Very low frequency (<75MHz)= Long Wavelength Array
Very difficult to detect
Signal: 10 arcmin, 10mk => S30MHz = 0.02 mJy
SKA sens in 1000hrs:
= 20000K at 50MHz =>
rms = 0.2 mJy
Need > 10 SKAs
Need DNR > 1e6
z=50
z=150
Barkana & Loeb 2005
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Challenge I: Low frequency foreground – hot, confused sky
Eberg 408 MHz Image (Haslam + 1982)
• 90% = Galactic foreground.
• Coldest regions: T ~ 100z)^-2.6 K
• 10% = Egal. radio sources = 1 source/deg^2 with S140 > 1 Jy
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Solution: spectral decomposition (eg. Morales, Gnedin…)
Foreground = non-thermal = featureless over ~ 100 MHz
Signal = fine scale structure on scales ~ few MHz
10’ FoV; SKA 1000hrs
Xcorrelation/Power spectral analysis in 3D – different symmetries in freq space
Freq
Signal
Foreground
Signal/Sky ~ 2e-5
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‘Isoplanatic patch’ = few deg = few km
Phase variation proportional to wavelength^2
74MHz Lane 03
Challenge II: Ionospheric phase errors – varying e- content
TID
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Solution:
Wide field ‘rubber screen’ phase self-calibration = ‘peeling’
Virgo A VLA 74 MHz Lane + 02
QuickTime™ and aCinepak decompressor
are needed to see this picture.
15’
Ionospheric phase errors: The Movie
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Challenge III: Interference
100 MHz z=13
200 MHz z=6
Solutions -- RFI Mitigation (Ellingson06)
Digital filtering: multi-bit sampling for high dynamic range (>50dB)
Beam nulling/Real-time ‘reference beam’
LOCATION!
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Beam nulling -- ASTRON/Dwingeloo (van Ardenne)
Factor 300 reduction in power
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VLA-VHF: 180 – 200 MHz Prime focus CSS search Greenhill, Blundell (SAO); Carilli, Perley (NRAO)
Leverage: existing telescopes, IF, correlator, operations
$110K D+D/construction (CfA)
First light: Feb 16, 05
Four element interferometry: May 05
First limits: Winter 06/07
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Project abandoned: Digital TV
KNMD Ch 9
150W at 100km
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RFI mitigation: location, location location…
100 people km^-2
1 km^-2
0.01 km^-2
(Briggs 2005)
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Challenge IV: Extreme computing
LOFAR: IBM Blue Gene/L
“Stella” (Falcke)
• 0.5 Tbit/s input data rate
• 30 Tflop
• ~ 12000 PCs
• Occupying 6 m2
• 150 KW power consumption
~1.7% slower than #1 in Europe
(Barcelona) …
Dutch minister of science
Blue Gene
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Focus: Reionization (power spec,CSS,abs)
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PAPER: Staged Engineering Approach
• Broad band sleeve dipole => 2x2 tile
• 8 dipole test array in GB (06/07) => 64 station array in WA (07/08)
• FPGA-based ‘pocket correlator’ from Berkeley wireless lab => custom design.
BEE2: 5 FPGAs, 500 Gops/s
• S/W Imaging, calibration, PS analysis: Miriad => Python + CASA, including ionospheric ‘peeling’ calibration + MFS
• ‘Peel the problem onion’
100MHz 200MHz
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PAPER: First images/spectra
Cygnus A
1e4Jy
Cas A 1e4Jy
3C392
200Jy
3C348 400Jy
140MHz
180MHz
CygA 1e4Jy
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Destination: Moon!
RAE2 1973
No interference
No ionosphere (?)
Easy to deploy and maintain (high tolerance electroncs + no moving parts)
10MHz
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Radio astronomy – Probing Cosmic Reionization
•‘Twilight zone’: study of first light limited to near-IR to radio
• First constraints: GP, CMBpol => reionization is complex and extended:
z_reion = 6 to 11
• HI 21cm: most direct probe of reionization
•Low freq pathfinders:
All-sky, PS, CSS
• SKA: imaging of IGM
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European Aeronautic Defence and Space Corporation/ASTRON (Falcke)
• Payload = 1000 kg (Ariane V)
• 100 antennas at 1-10 MHz ~ 1/10 SKA
QuickTime™ and aYUV420 codec decompressor
are needed to see this picture.
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END
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•IPS/ISS angular/temporal broadening: 1MHz => 1deg, 5years
•Faraday rotation => no linear polarization
•High sky temperature
•Low power super computing: LOFAR/Blue Gene = 0.15MW
•Lunar ionosphere: p = 0.2 to 1MHz (LUNA19,20 1970’s)?
•Diffraction limits: how sharp is knife’s edge?
Very low frequencies (<10MHz): Lunar challenges
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ARTICLE 22(ITU Radio Regulations)
Space servicesSection V – Radio astronomy in the shielded zone of the Moon
22.22 § 8 1) In the shielded zone of the Moon31 emissions causing harmful inter ference to radio astronomy observations32 and to other users of passive services shall be prohibited in the entire frequency spectrum except in the following bands:
22.23 a) the frequency bands allocated to the space research service using active sensors;
22.24 b) the frequency bands allocated to the space operation service, the Earth exploration-satellite service using active sensors, and the radiolocation service using stations on spaceborne platforms, which are required for the support of space research, as well as for radiocommunications and space research transmissions within the lunar shielded zone.
22.25 2) In frequency bands in which emissions are not prohibited by Nos. 22.22 to 22.24, radio astronomy observations and passive space research in the shielded zone of the Moon may be protected from harmful interference by agreement between administrations concerned.
22.22.1 The shielded zone of the Moon comprises the area of the Moon’s surface and an adjacent volume of space which are shielded from emissions originating within a distance of 100 000 km from the centre of the Earth.
32 22.22.2 The level of harmful interference is determined by agreement between the administrations concerned, with the guidance of the relevant ITU-R Recommendations.
Good “news” …The Moon is radio protected!
• The back side of the moon is declared as a radio protected site within the ITU Radio Regulations
– The IT Radio Regulations are an international treaty within the UN.
– Details are specified in a published ITU Recommendation (this is a non-mandatory recommendation, but is typically adhered to).
Radio astronomy on the moon has been a long-standing goal, protected by international treaties!
Steps need to be taken to protect the pristine and clean nature of the moon.
Lunar communication on the far side needs to be radio quiet.
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Sources responsible for reionization
Luminous AGN: No
Star forming galaxies: maybe -- dwarf galaxies (Bowens05; Yan04)?
mini-QSOs -- unlikely (soft Xray BG; Dijkstra04)
Decaying sterile neutrinos -- unlikely (various BGs; Mapelli05)
Pop III stars z>10? midIR BG (Kashlinsky05), but trecomb < tuniv at z~10
GP => Reionization occurs in ‘twilight zone’, opaque for obs <0.9 m
Needed for reion.
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Radio galaxy spectra: Smooth powerlaw (eg. Cygnus A)
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Tsiolkovsky crater
(100 km diameter)
20°S 129°E
Apollo 15
Tsiolkovsky crater