Cosmic collisions dark matter dark energy inflation Max

Cosmic collisions: dark matter, dark energy & inflation Max Tegmark, Penn/MIT

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Measuring clustering Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB 1992 -94 2004 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

De Bernardis et al 2000, Lange et al 2000 CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Tegmark, Jr. , 2001 CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Foreground-cleaned WMAP map from Tegmark, de Oliveira-Costa & Hamilton, astro-ph/0302496 CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB FRONTIERS: • Polarization • Small scales (AKBAR, CBI, Planck, APEX, ACT, SPT, …) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Atacama Cosmology Telescope (ACT): 150 GHz Ground based experiment at Atacama desert, Chile. n = 145, 225 & 265 GHz. Scans only in azimuth with the ability to cross-link elevations. 1. 4° FWHM=1. 7, 1. 1 & 0. 93’. SZ Simulation MBAC on ACT 1. 7’ beam w/ 2 X noise PLANCK Team: D. Benford, S. Boughn, J. Chervenak, A. de Oliveira-Costa, M. Devlin, R. Doriese, L. Ferrarese, J. Fowler, M. Halpern, D. Hughes, J. Hughes, K. Irwin, B. Jain, N. Jarosik, R. Jimenez, J. Klein, A. Kosowsky, R. Lupton, A. Miller, H. Moseley, B. Netterfield, L. Page (P. I. ), B. Partridge, H. Quintana, A. Reiseneggar, U. Seljak, D. Spergel, M. Spergel, S. Staggs, C. Stahle, M. Tegmark, L. Verde, T. Williams, G. Wilson, E. Wollack. More info at http: //www. physics. upenn. edu/act Sensitivity/pixel ~ 2, 8 & 16 m. K (64 nights of quality data).

Atacama Cosmology Telescope (ACT): 150 GHz Ground based experiment at Atacama desert, Chile. n = 145, 225 & 265 GHz. Scans only in azimuth with the ability to cross-link elevations. 1. 4° FWHM=1. 7, 1. 1 & 0. 93’. SZ Simulation MBAC on ACT 1. 7’ beam w/ 2 X noise PLANCK Measure the primary anisotropy beyond the WMAP & Planck resolution limits. Find galaxy clusters at z<1 through SZ effect. Measure the amplitude of the CMB gravitational lensing, and therefore probe the mass power spectrum at 1 Mpc scales at z~1 -2. Detect signature of reonization at z~15 through Vishniac effect. Find all extragalactic mm-wave point sources in 100(o)2 to a sensitivity of 1 m. Jy. More info at http: //www. physics. upenn. edu/act Sensitivity/pixel ~ 2, 8 & 16 m. K (64 nights of quality data).

z = 1000 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Mathis, Lemson, Springel, Kauffmann, White & Dekel 20 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 z = 2. 4

Mathis, Lemson, Springel, Kauffmann, White & Dekel 20 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 z = 0. 8

Mathis, Lemson, Springel, Kauffmann, White & Dekel 20 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 z=0

Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Clusters LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

CMB Clusters LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

CMB Clusters LSS Lya Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

Lyman Alpha Forest Simulation: Cen et al 2001 Lya. F Quasar You Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Clusters LSS Lya Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

CMB Clusters LSS Lensing Lya Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

Gravitational lensing Lensing Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Lensing Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Lensing Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Lensing Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Lensing Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Lensing Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Clusters LSS Lensing Lya Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

Galaxy power spectrum measurements 1999 (Based on compilation by Michael Vogeley) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Clusters LSS Lensing Lya Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Mark Whittle 2004 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

LSS frontiers/SDSS propaganda Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

SDSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Cool new/imminent LSS-measurements: LSS • P(k) from full 2 d. F data set (~250 k gals) • SDSS DR 3 goes public this fall • P(k) from SDSS DR 3 (>300 k gals) • P(k) from SDSS LRG’s (Eisenstein et al) • Angular galaxy clustering from SDSS • Clustering dependence on SDSS galaxy properties (Zehavi et al) • SDSS Lya. F analysis (Mc. Donald et al, Seljak et al) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 • See also Pope et al (2003), Budavari et (2004)

LSS Data & image processing by Robert Lupton & David Schlegel

Angular clustering LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Angular clustering LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

This was from just 400 square degrees: Tegmark et al 2002, for SDSS collab. Dodelson et al 2002, for SDSS collab. Now we have an order of magnitude more, and photometric redshifts. Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Clusters LSS Lya Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Tegmark & Zaldarriaga, astro-ph/0207047 + updates

Measuring parameters Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

CMB + LSS

What’s the Matter? Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

How much dark matter is there? Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

How much dark matter is there? CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

How much dark matter is there? CMB + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

DARK MATTER: • No direct detection • No accelerator detection • No bulge annihilation detection • No astrophysically observed departures from vanilla CDM Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Growth factor (obs/theo) DARK MATTER: Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 0 1 Redshift z 2

Dark energy Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

How much dark energy is there? ed os cl t fla en op Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

How much dark energy is there? Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 ed os cl t fla en op CMB

How much dark energy is there? + ed os cl t fla en op CMB LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 WMAP + SDSS: lots

How much dark energy is there? + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 ed os cl t fla en op CMB

How much dark energy is there? + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 ed os cl t fla en op CMB

• Late Integrated Sachs-Wolfe effect detected by Boughn & Crittenden 2003, Nolta et al 2003, Fosalba et al 2003, Scranton et al 2003, Afshordi et al 2003, Padmanabhan et al in prep • Illustration by Albert Stebbins

Equation of state? Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Nature of the dark energy Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Nature of the dark energy CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Nature of the dark energy CMB + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Nature of the dark energy CMB + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

From Saul Perlmutter’s web site Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Density relative to now THE NATURE OF DARK ENERGY: Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 (Yun Wang & MT, astro-ph/0403292, PRL, in press)

THE NATURE OF DARK ENERGY: Density relative to now (Using SN Ia “gold” data from Riess et al 2004) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 (Yun Wang & MT, astro-ph/0403292, PRL 2004)

THE NATURE OF DARK ENERGY: Density relative to now (Using SN Ia “gold” data from Riess et al 2004) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 (Yun Wang & MT, astro-ph/0403292, PRL, in press)

THE NATURE OF DARK ENERGY: Density relative to now (Using SN Ia “gold” data from Riess et al 2004) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 (Yun Wang & MT, astro-ph/0403292, PRL, in press)

THE NATURE OF DARK ENERGY: Density relative to now (Using SN Ia “gold” data from Riess et al 2004) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 (Yun Wang & MT, astro-ph/0403292, PRL, in press)

DARK ENERGY: • w(z) =-1, w’=w’’=…=0 Dark energy density • No dark energy clustering Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 0 1 Redshift z 2

Inflation Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Testing inflation I: How flat is space? Prediction: Wtot=1. 00000 0. 00001 Observation: Wtot=1. 01 0. 02 (WMAP+SDSS) Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

SN Ia+CMB+LSS constraints

CMB polarization missions Dark Energy missions

Testing inflation II: Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 SDSS collaboration, astro-ph/0310723, PRD 68, 193591

Testing inflation II: Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 SDSS collaboration, astro-ph/0310723, PRD 68, 193591

Testing inflation II: CMB Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 SDSS collaboration, astro-ph/0310723, PRD 68, 193591

Testing inflation II: CMB + LSS Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Planck + SDSS: Dn=0. 008, Dr=0. 012 + LSS ns=0. 96 r=0. 15 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 SDSS collaboration, astro-ph/0310723, PRD 68, 193591

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Planck + SDSS: Dn=0. 008, Dr=0. 012 + LSS ns=0. 96 r=0. 15 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 SDSS collaboration, astro-ph/0310723, PRD 68, 193591

Planck + SDSS: Dn=0. 008, Dr=0. 012 ns=1 r=0 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 SDSS collaboration, astro-ph/0310723, PRD 68, 193591

INFLATION: • n=1, dn/dlnk=d^2 ndlnk = … = 0 Primordial power spectrum P*(k)/k • No gravity waves detected Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004 Wavenumber k [1/Mpc]

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

My wish list: get at the underlying physics by measuring four cosmologicalfunctions: 1) cosmic expansion history H(z) ==> Nature of dark energy 2) linear growth factor g(z, k) ==> Nature of dark energy, dark matter, neutrino 3) primordial scalar power spectrum P*(k) ==> Inflation 4) primordial tensor power spectrum P*T(k) ==> Inflation Note that 1 predicts 4 and (for most inflation models) 3 Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004

Max Tegmark Univ. of Pennsylvania/MIT max@physics. upenn. edu Physics in Collision June 29, 2004