29 june 2005 caroline herschel distinguished lecture rachel webster 1
TRANSCRIPT
29 June 2005
Caroline Herschel Distinguished Lecture
Rachel Webster
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29 June 2005
Caroline Herschel Distinguished Lecture
Rachel Webster
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29 June 2005
Caroline Herschel Distinguished Lecture
Rachel Webster
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The End Of the ‘Dark Ages’: new telescopes
shedding new light
Rachel WebsterUniversity of Melbourne
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Outline
• Brief History of Hydrogen• What is Reionisation?• New Telescopes: MWA (&
others)
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Caroline Herschel Distinguished Lecture
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Outline
• Brief History of Hydrogen• What is Reionisation?• New Telescopes: MWA (&
others)Acknowledgements to a long list of collaborators, including:David Barnes, Frank Briggs, Jackie Hewitt, Colin Lonsdale, Miguel Morales, Stuart Wyithe
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History of the universe:
Miralda-Escude 2003
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History of the universe
JWST
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History of the universe
JWST& MWA
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PrimordialFluctuations
First Stars
Galaxies andClusters
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Evolution of structure
Z=28.6
AndreyKravtsov
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Structure at z=10
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Local Cosmic Web:
HICAT, Meyer atal 2004
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What is Reionisation?
Ly- Ly-
Low z: long mean free path for Ly- (1216Å) and photo-ionizing photons (<912Å)
High z: short mean free path for Ly- (1216Å) and photo-ionizing photons (<912Å)
HIHI
HII
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Spin Temperature: absorption or emission?
• Definition of spin temperature: Given the number of atoms in each of the
hyperfine transition levels of HI,
• Spin temp and CMB temp equal at early times
• Later kinetic temp Tk of gas increases; spin temp coupled to Tk by scattering of Ly photons;
21cm emission
ST
T
n
n *
0
1 exp3 07.0/10* khT
CMBs TT
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Z = 20 15 10 8 7 6
coldHI
HII
< 1 (Gunn-Peterson Effect)
70 MHz 90 MHz 130 160 190 MHz
Lowest possible redshift for reionisation
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Quasars Before Reionisation
3/2
sHI
5s 10
z1106.5τ
x
reionz1A1216o
sourcez1A1216o
HI absorbs photons near Ly- resonance
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Quasars Before Reionisation
3/2
sHI
5s 10
z1106.5τ
x
reionz1A1216o
sourcez1A1216o
HI absorbs photons near Ly- resonance
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• Gunn-Peterson troughs give the overlap redshift for HII at 6<zreion<6.4
• The IGM has a neutral fraction xHI>0.001 at z~6
Fan et al. (2001)Becker et al. (2001)
The data
Gunn-Peterson Trough(total absorption)
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Z = 20 15 10 8 7 6
coldHI
HII
70 MHz 90 MHz 130 160 190 MHz
Highest likely redshift for reionisation
warmHI
WMAP z=15-20
Correlation between polarisation and temperature on large angular scales due to Thomson scattering by electrons
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Detection Expt I: ‘the step’
Shaver etal 1999
Plenty of signal; can the featurebe separated from the bandpass?
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Experiment II: ‘Strömgren Spheres’
HI at IGM temperature
HI warmed by X-rays
HII (no contrast)
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CMB+quasar+foreground
IGMOr ∆z along the line of sight
z along the line-of-sight
Contrast measures xHI
Wyithe & Loeb 2003
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Measuring the size of ‘Strömgren spheres’
skmVc /3300~~0
MpcR
HRV
p
p
5.4~
Ly- at z=6.28
White et al. (ApJ 2003)
source
HI
HII
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Detection Expt III: ‘power spectrum’
Morales &Hewitt 2004
alsoZaldarriagaetal 2004
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Neutral hydrogen is opaque
TheoreticalSimulation:NickGnedin2005
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Early structure was simple
• Theorist’s heaven: excellent progress• Modelling of Stromgren spheres provides
new limits on neutral fraction at z~6: >0.1
tq~106 yrtq~107 yr
Wyithe, Loeb, Carilli 2004
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But it was never going to be easy….
**Foreground radio emission (noise ~102-5 xsignal)
» Synchrotron and free-free emission from MW
(Shaver etal 1999)» Low frequency radio point sources
(Di Matteo etal 2004)
» Free-free emission from IGM electrons(Oh
1999)
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‘Noise’ spectra smooth in frequency robust removal
Santos, Cooray & Knox 2005
Power spectrum
noise
bias x ionisation fraction
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New Telescopes: history
Clarke Lake Radio Obs
Bill Erikson and hisstudents
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New Experiments
• LOFAR – Holland» (Partially) funded, lots of momentum
• PaST - China (Mongolia)» On the ground, collecting data
• LWA - SW USA» Still planning; below 90MHz spread over
400km
• MWA - Western Australia» US-Australian collab, seeking funding
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New Experiments
• LOFAR – Holland» (Partially) funded, lots of momentum
• PaST - China (Mongolia)» On the ground, collecting data
• LWA - SW USA» Still planning; below 90MHz spread over
400km
• MWAMWA - Western Australia- Western Australia» US-Australian collab, seeking fundingUS-Australian collab, seeking funding
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MWA Collaboration
• Project leaders: MIT & MIT-Haystack(technical and scientific)
• Harvard/CFA (scientific)• ATNF(technical)• Melbourne (early deployment &
scientific)• ANU-RSAA, Tasmania (scientific)• Curtin, UWA, OSI (local infrastructure &
scientific)
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Experiments with MWA
• EoR– Stromgren spheres– Power spectrum
• Transients• Coronal Mass Ejections
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Simulated Stromgren Spheres: LFD
100 Hours
1000 Hours
z=6.5,
R=4Mpc
Stu Wyithe, Loeb, Barnesastro-ph/0506045
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Full Array ie 10xLFD
100 Hours
1000 Hours
There are 10’s of Stromgren Spheresin the field-of-view larger than 4Mpc
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Detecting the Power Spectrum with MWA (Bowman & Morales 2005)
Ionized frac. = 0.6
=0
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The SUNCoronal Mass Ejections: measure interplanetaryscintillation and Faraday rotation to describethe behaviour of the solar wind from near the sun tothe earth’s location
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Effect of space weather
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Why Western Australia?
FORTE satellite 131 MHZ
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Mileura Homestead
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The road to Mileura
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Early Deployment Site
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Tile assembly
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Tile 1 from the air
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RFI Environment
30-60 minuteintegrations overfull bandpass
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Sun at 96 MHzYes, that is the FM band …
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Interferometry on an AGN
time
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Galactic Centre at 108MHz
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Specs for MWA-LFD
• Frequency range: 80-300MHz, 32MHz bandwidth[3.8<z(21cm)<16.9]
• 500 tiles 4x4 dipoles in ‘phased array’, 8000m2
• Field-of-view: ~25deg fully steerable, multibeam• Area: 1.5km giving 3.4 arcmins @ 200MHz• 125,000 baselines, 4x109visibilities/0.5sec,
full stokes polarisation
[FPGA-based massively parallel digital hardware]http://web.haystack.mit.edu/arrays/MWA
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Finally……• Tomography of the earliest
structures in universe• Novel `technology telescope’• cheap array design • huge, fast data network• huge collecting area• stunning radio-quiet location
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Strömgren Spheres Expand Faster into Partially Reionised IGM
High neutral fraction:Slow expansion
Low neutral fraction:Fast expansion
neutral IGM ionised IGM
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ground basedradio techniques
10 MHz
350
MWA-LFDMWA-LFD
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furlanetto
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ciardi
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ciardi
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The Surface of Bubble Overlap
• There is a surface on the sky corresponding to the redshifts along different lines of sight where the IGM was most recently partially neutral
Contribution from HII regions
Morales & Hewitt (2004)
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Numerical Simulations of Reionization (Gnedin et al. 2000)
neutral H fraction ionizing intensity
4Mpc << 60Mpc
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Structure on Angular Scales in Emission from the Cosmic Web
• The temperature map, and the size of fluctuations on different scales reveal the topology of reionisation
Tozzi et al. (ApJ 2002)
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Numerical Simulations of Reionization (Gnedin et al. 2000)
neutral H fraction ionizing intensity
neutral H fraction
ionizing intensity
4Mpc << 60Mpc