Evolution and application of the 21 cm signal throughout cosmic history
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Transcript of Evolution and application of the 21 cm signal throughout cosmic history
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Evolution and application of the 21 cm signal
throughout cosmic history
Jonathan Pritchard (CfA-HCO)
Collaborators: Steve Furlanetto (UCLA) Avi Loeb (Harvard) Mario Santos (CENTRA - IST) Alex Amblard (UCI) Hy Trac (CfA)
Renyue Cen (Princeton) Asantha Cooray (UCI)
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2STScIMAR 2008 Overview
1. 21 cm as probe of high-z radiation backgrounds
2. Fluctuations in Ly andX-ray backgrounds lead to 21 cm fluctuations
3. What might 21 cm observations tell usabout first sources?
4. Reionization
5. Experimental prospects
z~30
z~12
z~7
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3STScIMAR 2008 21 cm basics
•21 cm brightness temperature
•21 cm spin temperature
•Use CMB backlight to probe 21cm transition
z=13fobs=100 MHzf21cm=1.4 GHz
z=0
TS TbT
HITK
•3D mapping of HI possible - angles + frequency
•Coupling mechanisms: Radiative transitions (CMB) Collisions Wouthuysen-Field
10S1/2
11S1/2
n0
n1
n1/n0=3 exp(-h21cm/kTs)
•HI hyperfine structure
=21cm
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4STScIMAR 2008 Wouthuysen-Field effect
Lyman
Effective for J>10-21erg/s/cm2/Hz/sr
Ts~T~Tk
W-F recoils 20P1/2
21P1/2
21P1/2
22P1/2
10S1/2
11S1/2 Selection rules: F= 0,1 (Not F=0F=0)
Hyperfine structure of HI
Field 1959
nFLJ
~21 cm
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5STScIMAR 2008 Thermal History
e.g. Furlanetto 2006
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6STScIMAR 2008 21 cm fluctuations
BaryonDensity
Gas Temperature
W-FCoupling
Neutralfraction
Velocitygradient
X-raysources
Lysources
ReionizationCosmology Cosmology
Brightnesstemperature
Amount ofneutral hydrogen
Spin temperature
Velocity(Mass)
b
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7STScIMAR 2008 Angular separation?
•Anisotropy of velocity gradient term allows angular separation
Barkana & Loeb 2005
Bharadwaj & Ali 2004
BaryonDensity
Gas Temperature
W-FCoupling
Neutralfraction
Velocitygradient
•In linear theory, peculiar velocities correlate with overdensities
•Initial observations will average over angle to improve S/N
b
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8STScIMAR 2008 Temporal separation?
BaryonDensity
Gas Temperature
W-FCoupling
Neutralfraction
Velocitygradient
X-raysources
Lysources
ReionizationCosmology Cosmology
Dark AgesTwilight
Brightnesstemperature
b
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9STScIMAR 2008
Fluctuations from the first stars
dV
• Fluctuations in flux from source clustering, 1/r2 law, optical depth,… • Relate fluctuations in Ly and X-ray fluxes to overdensities
•Start with LyBarkana & Loeb 2005
Chen & Miralde-Escude 2006, Chuzhoy & Shapiro 2006, Pritchard & Furlanetto 2006,2007
• Three contributions to Ly flux: continuum & injected from stars + x-ray
continuum injected
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10STScIMAR 2008Determining the first sources
Chuzhoy,Alvarez, & Shapiro 2006
Sources
Spectra
J,* vs J,X
S
Pritchard &Furlanetto 2007
bias source properties density
z=20
dominates
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11STScIMAR 2008 X-ray heating
• Soft X-rays heat closer to source, hard X-rays have long m.f.p.
• X-ray flux -> heating rate -> temperature evolution• Integrated effect - so whole SF history contributes
Pritchard &Furlanetto 2007
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12STScIMAR 2008 Indications of TK
TK<T
TK>T
• Learn about source bias and spectrum in same way as Ly • Constrain heating transition
T dominates
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13STScIMAR 2008 X-ray background?
T x
?
• To avoid giving the idea of certainty…
Extrapolating low-z X-ray:IR correlation gives:Glover & Brand 2003
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14STScIMAR 2008 Reionization
(100 Mpc/h)3 cube, 18803 particle N-body + UV photon ray tracing
X-ray heating and coupling included via simplemodel
Santos, Amblard, JRP, Trac, Cen, Cooray 2008
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15STScIMAR 2008 Ionization history
Xi>0.1
zR~7~0.07
WMAP1WMAP3
WMAP5Zreion=10.8±1.4 (instant)Zreion~9 ±1.4 (extended)
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16STScIMAR 2008 Theory vs Simulation
Furlanetto, Zaldarriaga, Hernquist 2004
• Bubbles imprint “knee” on large scales• Limited agreement at end of reionizationon large scales
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17STScIMAR 2008 Experimental effortsLOFAR: NetherlandsFreq: 120-240 MHzBaselines: 100m-
100km
SKA: S. Africa/Australia ???Freq: 60 MHz-35 GHzBaselines: 20m-
3000km
MWA: AustraliaFreq: 80-300 MHzBaselines: 10m-
1.5km
PAST/21CMA: ChinaFreq: 70-200 MHz
Foregrounds are thebig problem!
More from Judd next
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18STScIMAR 2008 Temporal evolution
Dark agesReionizationPost-reionization
Signal from denseneutral clumps at low z
Pritchard & Loeb 2008
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19STScIMAR 2008 Temporal evolution
x T
?
MWA
SKA
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20STScIMAR 2008 High-z Observations•Need SKA to probe these brightnessfluctuations
•Observe scalesk=0.025-2 Mpc-1
•Easily distinguishtwo models
•Optimistic foregroundremoval
•B~12MHz ->z~1.5
foregroundspoor angular resolution
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21STScIMAR 2008 Low-z Observations
SKA
MWALOFAR
•Low k cutofffrom antennaesize
•Sensitivity ofLOFAR and MWA drops off by z=12
McQuinn et al. 2006
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22STScIMAR 2008 Angular Separation
MWA SKA
LARC
Cosmology
Astrophysics
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23STScIMAR 2008 Conclusions
• Today told a simple story - lots of uncertainty in all attempts at modeling this period
• Can use 21 cm to learn about the first luminous sources via the Ly background
• Temperature fluctuations should give insight into thermalevolution of IGM
• If X-ray heating important, then can learn about early X-ray sources
• Map out reionization topology and evolution• Detailed measurements will require SKA and luck• Beginnings of full theoretical framework coming into being• Early days for 21 cm and still unclear what will and will not be
possible - foregrounds will be determining factor
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24STScIMAR 2008
Bonus material
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25STScIMAR 2008 Redshift slices: Ly
•Pure Ly fluctuations
z=19-20
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26STScIMAR 2008 Redshift slices: Ly/Tz=17-18
•Growing T fluctuationslead first to dip in Tb then to double peak structure
•Double peak requiresT and Ly fluctuationsto have different scaledependence
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27STScIMAR 2008 Redshift slices: Tz=15-16
•T fluctuations dominate over Ly
•Clear peak-trough structure visible
• 2 <0 on largescales indicates TK<T
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28STScIMAR 2008 Redshift slices: T/z=13-14
•After TK>T , thetrough disappears
•As heating continuesT fluctuations die out
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29STScIMAR 2008 Redshift slices: /xz=8-12
•Bubbles imprint featureon power spectra once xi>0.2
•Non-linearities in density fieldbecome important
(TK fluc. not included)
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30STScIMAR 2008 Thermal history
•Ly forest
Hui & Haiman 2003
•IGM retains short term memory of reionization - suggests zR<10•Photoionization heating erases memory of thermal history beforereionization
•CMB temperature
•Knowing TCMB=2.726 K and assuming thermal coupling byCompton scattering followed by adiabatic expansion allows informed guess of high z temperature evolution
??
Zaldarriaga, Hui, & Tegmark 2001
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31STScIMAR 2008 Ionization history
Page et al. 2006
Becker et al. 2005
• WMAP3 measurement of ~0.09 (down from ~0.17)
• Gunn-Peterson Trough
•Universe ionized below z~6, some neutral HIat higher z•black is black
•Integral constraint on ionization history•Better TE measurements+ EE observations
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32STScIMAR 2008 When did things start?
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33STScIMAR 2008 Foregrounds
• Many foregrounds Galactic synchrotron (especially polarized component) Radio Frequency Interference (RFI)
e.g. radio, cell phones, digital radio Radio recombination lines Radio point sources
• Foregrounds dwarf signal: foregrounds ~1000s K vs 10s mK signal
• Strong frequency dependence Tsky-2.6
• Foreground removal exploits smoothness in frequency and spatial symmetries
• Cross-correlation with galaxies also important
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34STScIMAR 2008 Reionization?
WMAP1WMAP3
WMAP5
=0.06 =0.09 =0.12
Zreion~11±1 (instant)
Zreion~9 ±1 (model)
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35STScIMAR 2008 Global history
Heating
HII regions
IGM
expansion
Furlanetto 2006
Adiabaticexpansion
X-rayheating
Comptonheating
+ +
UV ionization recombination+
X-ray ionization recombination+
continuum injectedLy flux
•Sources: Pop. II & Pop. III stars (UV+Ly) Starburst galaxies, SNR, mini-quasar (X-ray)
•Parameters: fstar, X, N, Nion (+ spectra + bias +…)
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36STScIMAR 2008 Angular Separation