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Neutrinos and Cosmology Alessandro Melchiorri Universita di Roma, La Sapienza NOW 2010, Conca-Specchiulla September 7th 2010.

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Presentation on theme: "Neutrinos and Cosmology Alessandro Melchiorri Universita di Roma, La Sapienza NOW 2010, Conca-Specchiulla September 7th 2010."— Presentation transcript:

1 Neutrinos and Cosmology Alessandro Melchiorri Universita di Roma, La Sapienza NOW 2010, Conca-Specchiulla September 7th 2010

2 Komatsu et al, 2010, New WMAP results from 7 years of observations

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4 Komatsu et al, 2010,

5 New Measurements, More Parameters ! Neutrino masses Neutrino effective number Primordial Helium

6 Small scale CMB can probe Helium abundance at recombination.

7 Komatsu et al, 2010,

8 Neutrino background. Changes early ISW. Hint for N>3 ?

9 Gianpiero ManganoGianpiero Mangano, Alessandro Melchiorri, Olga Mena, Gennaro Miele, Anze SlosarAlessandro MelchiorriOlga MenaGennaro MieleAnze Slosar Journal-ref: JCAP0703:006,2007

10 Current constraints on neutrino mass from Cosmology (Fogli et al, 2010 in preparation). Blue: WMAP-7 Red: w7+SN+Bao+H0 Green: w7+CMBsuborb+SN+LRG+H0 (Plot made by Luca Pagano)

11 Blue: WMAP-7 Red: w7+SN+Bao+H0 Green: w7+CMBsuborb+SN+LRG+H0 Current constraints on neutrino mass from Cosmology (Fogli et al, 2010 in preparation). (Plot made by Luca Pagano)

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13 Sudden Reionization As we dont know precisely the details of the reionization history we should consider more general reionization scenarios CAMB Notes, Antony Lewis

14 MHs Reionization Following Mortonson & Hu we can parametrize the reionization history as a free function of the redshift by decomposing the free electron fraction as The principal components S (z) are the eigenfunctions of the Fisher matrix of an ideal, cosmic variance limited, experiment. The principal components S (z) are the eigenfunctions of the Fisher matrix of an ideal, cosmic variance limited, experiment. m are the amplitudes of the S (z) m are the amplitudes of the S (z) x(z) is the WMAP fiducial model at which the FM is computed x fid (z) is the WMAP fiducial model at which the FM is computed M. J. Mortonson and W. Hu ApJ 686, L53 (2008)

15 Impact of generalized reionization on CMB constraints on Neutrino Mass Archidiacono, Cooray, Melchiorri, Pandolfi, 2010, PRD

16 Planck Satellite launch 14/5/2009

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19 Blue: current data Red: Planck

20 Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv: Lets consider not only Planck but also ACTpol (From Atacama Cosmology Telescope, Ground based, results expected by 2013) CMBpol (Next CMB satellite, 2020 ?)

21 Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv: Blue: Planck Red: Planck+ACTpol Green: CMBPol Constraints on Neutrino Mass

22 Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv: Blue: Planck Red: Planck+ACTpol Green: CMBPol Constraints on Neutrino Number

23 Galli, Martinelli, Melchiorri, Pagano, Sherwin, Spergel, PRD submitted, arXiv: Blue: Planck Red: Planck+ACTpol Green: CMBPol Constraints on Helium Abundance

24 Recent CMB measurements fully confirm -CDM. Improved constraints on inflation With future measurements constraints on new parameters related to laboratory Physics could be achieved. In 2012 from Planck we will know: -If the total neutrino mass is less than 0.5eV. -If there is an extra background of relativistic particles. -Helium abundance with 0.01 accuracy.

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