Testing cosmological models with the Integrated Sachs-Wolfe effect
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Testing cosmological models with the Integrated Sachs-Wolfe effect
Alvise Raccanelli, Institute of Cosmology and Gravitation,
Portsmouth
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Outline:
•The standard model of cosmology•CMB anisotropies•The ISW effect•Why the ISW is a good test for cosmological models•Results and ongoing projects
2 Alvise RaccanelliTesting cosmological models with the ISW
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Observations of Supernovae Type Ia told us that the universe is accelerating
Alvise RaccanelliTesting cosmological models with the ISW
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The Universe is accelerating; this is caused by something different from the usual gravity
Alvise RaccanelliTesting cosmological models with the ISW
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5 Alvise RaccanelliTesting cosmological models with the ISW
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Hu & White 2004
After the Big Bang, the Universe was hot and dense, and photons were strongly coupled to electrons and protons
Alvise RaccanelliTesting cosmological models with the ISW
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Before the recombination, photons are coupled with matter, so they can not travel to us
The Universe is hot and dense
Alvise RaccanelliTesting cosmological models with the ISW
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After the recombination, photons are free to travel towards us
The Universe become colder and less dense, and at one point protons and electrons form hydrogen (recombination)
Alvise RaccanelliTesting cosmological models with the ISW
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The Last Scattering Surace: why CMB is important
Alvise RaccanelliTesting cosmological models with the ISW
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CMB Experiments
Alvise RaccanelliTesting cosmological models with the ISW
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WMAP
Planck
Alvise RaccanelliTesting cosmological models with the ISW
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The Planck First Light
Alvise RaccanelliTesting cosmological models with the ISW
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Better Power Spectrum at small scale
The Planck BlueBook 2005
Alvise RaccanelliTesting cosmological models with the ISW
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14 Alvise RaccanelliTesting cosmological models with the ISW
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ISW effect: evolving gravitational potential
Alvise RaccanelliTesting cosmological models with the ISW
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Galaxies form inside gravitaional wells left after inflation
Alvise RaccanelliTesting cosmological models with the ISW
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Travelling from the last scattering surface to us, photons pass through gravitational wells. If the potential is static, they will exit with the same energy they had when they entered. If the well is stretched by the dark
energy, photons will experience a shift in energy (and so in temperature)
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But this effect is small compared to other CMB anisotropies
Alvise RaccanelliTesting cosmological models with the ISW
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so we need to cross-correlate this temperature shift with something that can trace potential wells. Galaxies are a biased
tracer of potential wells
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20 Alvise RaccanelliTesting cosmological models with the ISW
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This part tells us where is matter
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This part tells us how the gravitational potential change
Alvise RaccanelliTesting cosmological models with the ISW
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ISW can be used to test the gravitational or the galaxies part:
•Changing the filter of the galaxies allow to test models for the bias relating the visible matter to the mass (including Dark Matter) and the redshift distribution of galaxies
•Changing the filter of the gravitational part allow to test models of gravity
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Results:
Raccanelli et al. 08
Testing Galaxy distribution and bias models
Work with G. De Zotti, S. Matarrese, M. Negrello, A. Bonaldi, G. Tormen
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Results:Testing new Galaxy distribution models
Massardi et al. 10
Work with G. De Zotti, M. Massardi, M. Negrello, A. Bonaldi, S. Ricciardi
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Ongoing projects:•Test of Unified Dark Matter models(with D. Bertacca, D. Pietrobon, S. Matarrese, T. Giannantonio, N. Bartolo, O. Piattella)
•Test of Modified Gravity Models(with F.P. Silva, K. Koyama, T. Giannantonio, G.-B. Zhao)
•ISW with LOFAR data(with W. Percival, M. Jarvis, D. Bacon, S. Rawlings, F. Abdalla)
Alvise RaccanelliTesting cosmological models with the ISW
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Preliminary results for testing UDM models
Bertacca et al., in preparation
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Kobayashi et al. 09
In some modified gravity scenarios we expect a negative cross-correlation, due to the “stronger” dark energy
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Conclusions
• The ISW is a good test for testing different cosmologies•The incoming data from CMB and Large Scale Structure observations will allow a better estimation of cosmological parameters
Alvise RaccanelliTesting cosmological models with the ISW