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Neutrino clustering in interacting Dark Energy cosmologies

Neutrino clustering in interacting Dark Energy cosmologies. Valeria Pettorino (ITP, Heidelberg). A decade of DARK ENERGY, Spring Symposium 2008 05.05.08 Baltimore. astro-ph/0802.1515 with D.F.Mota, G.Robbers, C.Wetterich. Interacting Dark Energy. Coupling to neutrinos

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Neutrino clustering in interacting Dark Energy cosmologies

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  1. Neutrino clustering in interacting Dark Energy cosmologies Valeria Pettorino (ITP, Heidelberg) A decade of DARK ENERGY, Spring Symposium 2008 05.05.08 Baltimore astro-ph/0802.1515 with D.F.Mota, G.Robbers, C.Wetterich

  2. Interacting Dark Energy Coupling to neutrinos can be big and can have a significant influence in cosmology  MAVANS: Fardon etal 2004, Afshordi etal 2005, Bjaelde etal 2007, Brookfield etal 2007… Growing neutrinos: Amendola etal 2007, Wetterich 2007, Mota etal 2008, Brouzakis etal 2007 Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

  3. Attractors • V() = M4 exp(- ) • Solutions independent of the initial conditions • DE scales as a constant fraction tracking the background: = n/2 with n = 3(4) in MDE (RDE)  has to increase in recent time! Need a cosmological event that triggers the acceleration Steinhardt, Wang and Zlatev 1999, Liddle & Scherrer 1999, Wetterich 1995, Amendola 2000… Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

  4. Neutrinos become non relativistic Attractor with constant fraction of DE + coupling Neutrino mass grows ( < 0) Neutrinos become non relativistic Neutrinos become non relativistic The coupling to DE turns on and almost stops  Transition to the future attractor: acceleration acceleration Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

  5. (Mota,Pettorino,Robbers,Wetterich 2008) Coupling Dark Energy to neutrinos Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

  6. Dark energy - neutrino connection • Dark energy and neutrino properties are related The present amount of DE is set by a cosmological event and not by ground state properties DE- fluid equation of state Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

  7. (Mota,Pettorino,Robbers,Wetterich 2008) ~Gpc ~20Mpc Neutrino clustering • Neutrino structures become non linear at z ~ 1 for supercluster scales (Mota, Pettorino, Robbers, Wetterich 2008) • At small scales • neutrinos reduce CDM • structures • Stable neutrino lumps • (Brouzakis etal 2007) Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

  8. Conclusions • When neutrinos become non relativistic, they activate the coupling and trigger the acceleration. • Transition from attractor to an almost static dark energy, independent of ground state properties. • Neutrinos first cluster at z ~ 1 at supercluster scales and beyond. • At small scales, neutrinos don’t contribute to the clumping but they reduce cdm structures. • Detection of such a population of large scale structures via gravitational potential or correlation with CMB can be an indication for a new attractive force stronger than gravity. Valeria Pettorino, ITP Heidelberg A decade of Dark Energy, Baltimore, 5-8 May 2008

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