beam profile sensitivity of wmap cmb power spectrum
DESCRIPTION
Beam profile sensitivity of WMAP CMB power spectrum. Utane Sawangwit & Tom Shanks Durham University. Standard CDM Model - Issues!. Dark matter – exotic particles as yet undetected! ⇒ 1 in 10 100 fine-tuning coincidence – anthropic? - PowerPoint PPT PresentationTRANSCRIPT
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Beam profile sensitivity
of WMAP CMB power
spectrum
Utane Sawangwit & Tom Shanks Durham University
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Standard CDM Model - Issues!
Dark matter – exotic particles as yet undetected!
⇒ 1 in 10100 fine-tuning coincidence – anthropic?
Even though inflation was set up to get rid of fine-tuning!
has wrong sign for string theory – Anti-de Sitter v. de Sitter
Standard inflation model 10^10⇒ 77 Universes!
Wrong mass function for galaxies!
Downsizing observed v. bottom-up hierarchy predicted
Feedback - more energy now used in preventing stars form than in forming them under gravity
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WMAP 5-Year CMB Map
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WMAP 5-Year Power Spectrum
Universe comprises:
~72% Dark Energy
~24% CDM
~4% Baryons
(Hinshaw et al. 2003, 2006, 2008, Spergel et al. 2003, 2006, 2008)
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And yet…….
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Sensitivity of WMAP Cl to beam
Raw Cl result
Final Cl result
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WMAP beams (Page et al 2003)
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WMAP5 point sources 390 sources detected
(5sigma) in K/Ka/Q/V/W Complete down to ~1Jy 373/390 have 5GHz
counterparts Flat spectrum, <α>= -
0.09 We only use compact
sources (5 GHz GB6/PMN)
Wright et al. (2009)
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WMAP5 Radio Source Profiles
Gaussian
Jupiterbeam
Radio sources
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Comparison with ground-based fluxes
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Potential problems with RS beam
Radio Source Clustering?
Estimate based on bright NVSS source clustering...
…suggests clustering is unlikely explanation
But what about the CMB fluctuations – Eddington effect? - referee
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New: “CMB-free” point sources
CMB-free WMAP5 source detection, Chen & Wright 2009
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New: NVSS 1.4GHz point sources
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New: Monte Carlo Simulations
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Simulations: known source positions
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Source detection
Filter the weighted map with
(Wright et al. 2009, Tegmark et al. 1998)
W
V
Q
Ka
K
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Simulations: after source detection
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WMAP5 Radio Source Profiles
Gaussian
Jupiterbeam
Radio sources
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De-beamed power spectra
Gaussian
Radio sources
Jupiter
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WMAP peak moved to l=330
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A diy beam that works!
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Conclusions
CDM assumes “undiscovered physics” + very finely-tuned + problems in many other areas
Model gained overwhelming support from WMAP
But WMAP power spectra highly sensitive to beam
Radio sources indicate wider beams than expected
Systematic errors on WMAP Cl may therefore increase
May reduce constraints on simpler models
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Example simpler model: low H0, baryon=1
Shanks (1985) - if Ho<40kms-1Mpc-1 then:
X-ray gas → DM in Coma, Mvir/MX =15h1.5
Inflationary baryon=1 model in better agreement with nucleosynthesis Light element abundances baryonh2<0.06 baryon 1 starts to be allowed for low h
Inflation+EdS => =1 => Globular Cluster Ages of 13-16Gyr require Ho<40kms-1Mpc-1
But the first acoustic peak is at l=330, not l=220
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‘Do it Yourself’ (DIY) WMAP beam
bS() is the beam and bl is the beam transfer function
To get the “true” power spectrum, Cl, divide the raw power spectrum, Cl’, by bl
2
Alternatively to get the beam function bl
2, divide raw by true power spectum!
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Beam transfer functions
diy beam functions – divide low H0 Cl by raw WMAP Cl & square root
Power-law radio source beam fits give too much power at l>300
Need spike in bl
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Ed Witten -“Strings
2001”
http://theory.tifr.res.in/strings/Proceedings/witten/22.html
String theory prefers a negative (anti-de Sitter!) rather than the observed positive