What can we learn about neutrinos from cosmology? Credit: SDSS team, Andrew Hamilton Blame: Max Tegmark

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 What have we learned so far?

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Flyabout + SDSS movie

Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy Brief History of the Universe

Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy What do we want to measure? Cosmological functions   (z), G(z,k), P s (k), P t (k)

Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy To 0th order: Cosmological functions   (z), G(z,k), P s (k), P t (k) H(z)

Fluctuation generator Fluctuation amplifier (Graphics from Gary Hinshaw/WMAP team) Hot Dense Smooth Cool Rarefied Clumpy Cosmological functions H(z) P(k,z) To 1st order:

SN Ia+CMB+LSS constraints Yun Wang & MT 2004, PRL 92, H = dlna/dt, H 2   Assumes k=0 Vanilla rules OK!

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Measuring clustering (That’s where the neutrino signal is)

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom z = 1000

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom z = 2.4 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom z = 0.8 Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom Mathis, Lemson, Springel, Kauffmann, White & Dekel 2001 z = 0

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Cmbgg OmOl

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies LSS

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies LSS Clusters Tegmark & Zaldarriaga, astro-ph/ updates

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies LSS Clusters CMB Tegmark & Zaldarriaga, astro-ph/ updates

History (Figure from Wayne Hu) (Figure from WMAP team)

History

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom Guth & Kaiser 2005, Science

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies LSS Clusters CMB Tegmark & Zaldarriaga, astro-ph/ updates

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom Lyman Alpha Forest Simulation: Cen et al 2001 You Quasar Ly  F

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 GRAVITATIONAL LENSING: A1689 imaged by Hubble ACS, Broadhurst et al 2004

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 distorti on Lensing

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley)

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, par movies Ly  LSS Clusters Lensing Tegmark & Zaldarriaga, astro-ph/ updates CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Measuring cosmological parameters

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Neutrinos

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom How neutrinos suppress cosmic fluctuation growth If all the matter can cluster:  a Net growth until today: a today /a primordial ≈ 4700 p ≈ 4700 e -4f Power suppression: P(k)/P(k) primordial ≈ e -8f f ≈ ∑ m i /94.4 eV  dm ≈ ∑ m i /12 eV, So 1 eV cuts power in half. If only a fraction  * can cluster:  a p, where p=[(1+24  * )-1]/4≈  * 3/5 ≈ (1-f ) 3/5 (Bond, Efstathiou & Silk 1980) Distinguish neutrinos from dark energy by time and scale dependence.

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Cmbgg OmOl

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Cmbgg OmOl

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Cmbgg OmOl CMB

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Cmbgg OmOl CMB + P(k)

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Cmbgg OmOl CMB + Ly  F + P(k)

THE FUTURE It's tough to make predictions, especially about the future. Yogi Berra

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Boom zoom Now: WMAP CMB + SDSS gals & Ly  F: ∑ m i < 0.4 eV E.g., Hu & Tegmark astro-ph/ , Hu astro-ph/ , Hannestad et al, astro-ph/ Planck CMB + LSST lensing:  (∑ m i ) ~ 0.04 eV Seljak et al, astro-ph/ , Goobar et al astro-ph/ Future:

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Galaxy clustering progress

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 Why are LRGs so useful?

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 SDSS sphere anim

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 History CMB Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/

LSS Our observable universe

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 LSS Quasars

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 LSS LRG’s

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 LSS Common galaxies

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 LSS Common gals: too dense Quasars: too sparse LRG’s: just right! Why LRG’s are “Goldilocks galaxies”:

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 LSS LRG’s Also more strongly clustered

Max Tegmark Dept. of Physics, MIT FACT ISSworkshop BU, March 8, 2006 LSS Why LRG’s are “just right”: LRG’s have more statistical power than 2 million regular gals (Eisenstein et al 2005)