WEIGHING THE UNIVERSEWEIGHING THE UNIVERSE

Celebrating Tsvi PiranCelebrating Tsvi Piran

WEIGHING THE UNIVERSEWEIGHING THE UNIVERSE

Celebrating Tsvi PiranCelebrating Tsvi Piran

Neta A. BahcallPrinceton University

Neta A. BahcallPrinceton University

MAZAL TOV, TSVI!MAZAL TOV, TSVI!

Happy Birthday! PhD, HU, 1976

[ Neta: HU alum; John: HU Honorary Degree ‘03] First papers with J. Shaham, 1975 [my classmate, friend]

1. High Efficiency of the Penrose Mechanism for Particle Collisions 2. Can soft gamma-ray bursts be emitted by accreting black holes 4. Production of gamma-ray bursts near rapidly rotating accreting black

holes 11. SS433 - A massive black hole

GRBs; GR; HEA; NS; Cosmology; Voids.. Over 200 publications IAS Member (with John): 1979-1981; Long-Term Member ‘81-88

Happy Birthday! PhD, HU, 1976

[ Neta: HU alum; John: HU Honorary Degree ‘03] First papers with J. Shaham, 1975 [my classmate, friend]

1. High Efficiency of the Penrose Mechanism for Particle Collisions 2. Can soft gamma-ray bursts be emitted by accreting black holes 4. Production of gamma-ray bursts near rapidly rotating accreting black

holes 11. SS433 - A massive black hole

GRBs; GR; HEA; NS; Cosmology; Voids.. Over 200 publications IAS Member (with John): 1979-1981; Long-Term Member ‘81-88

Pesach 1983, Bahcall’s home, PrincetonTsvi, Bill Press, John, Neta, Orli

Pesach 1983, Bahcall’s home, PrincetonTsvi, Bill Press, John, Neta, Orli

At Safi Bahcall’s Bar-Mitzva, IAS, PrincetonJohn, Neta, Tsvi and mother

At Safi Bahcall’s Bar-Mitzva, IAS, PrincetonJohn, Neta, Tsvi and mother

Mass Density of UniverseMass Density of Universe How much? How distributed?

Mass-to-Light Function Baryon Fraction Cluster Abundance and Evolution Other Large-Scale Structure Obs.

All yield All yield m m ~ 0.25~ 0.25

Mass ~ LightMass ~ Light (on large scales)

How much? How distributed?

Mass-to-Light Function Baryon Fraction Cluster Abundance and Evolution Other Large-Scale Structure Obs.

All yield All yield m m ~ 0.25~ 0.25

Mass ~ LightMass ~ Light (on large scales)

Mass-to-Light FunctionMass-to-Light FunctionM/L(R)M/L(R)

Mass-to-Light FunctionMass-to-Light FunctionM/L(R)M/L(R)

How does M/L depend on scale?How does M/L depend on scale? How and where is the mass distributed?How and where is the mass distributed? How use it to weigh Universe?How use it to weigh Universe?

<M/L><M/L>rep rep LLunivuniv(L(Loo/Vol) = /Vol) = mm(M(Moo/Vol)/Vol)

Determine M, <M/L> of clusters, SCs, LSS

<M/L><M/L> rep rep [[≈ 300h≈ 300h ]

m m ~ 0.2 +-0.05~ 0.2 +-0.05

How does M/L depend on scale?How does M/L depend on scale? How and where is the mass distributed?How and where is the mass distributed? How use it to weigh Universe?How use it to weigh Universe?

<M/L><M/L>rep rep LLunivuniv(L(Loo/Vol) = /Vol) = mm(M(Moo/Vol)/Vol)

Determine M, <M/L> of clusters, SCs, LSS

<M/L><M/L> rep rep [[≈ 300h≈ 300h ]

m m ~ 0.2 +-0.05~ 0.2 +-0.05

Mass-to-Light Function Mass-to-Light Function (Bahcall, Lubin & Dorman ‘95; Bahcall and Fan ‘98)

Mass-to-Light Function Mass-to-Light Function (Bahcall, Lubin & Dorman ‘95; Bahcall and Fan ‘98)

1. M/L flattens on large-scales: M ~ L. End of Dark Matter. 2. Sp + E produce M/L of groups, clusters; Clusters have no excess DM !3. Most of the DM is in huge halos around galaxies (few-100 Kpc)

Ωm = 1.0

Ωm = 0.3Ωm=0.25

Mass-to-Light Function Mass-to-Light Function (Bahcall, Lubin & Dorman ‘95; Bahcall and Fan ‘98)

Mass-to-Light Function Mass-to-Light Function (Bahcall, Lubin & Dorman ‘95; Bahcall and Fan ‘98)

SDSSSDSS Ωm=0.2

Cluster M/Li(R) Profile (SDSS, weak lensing)

2x104 clusters N= 3 to 220 (Sheldon etal 2009)

Cluster M/Li(R) Profile (SDSS, weak lensing)

2x104 clusters N= 3 to 220 (Sheldon etal 2009)

X=R(vir)

Flat >~ 1MpcM ~ L

M/Li(r=22Mpc) vs. Mcl (SDSS; ‘09)M/Li(r=22Mpc) vs. Mcl (SDSS; ‘09)

Flat M/L on large scales; SAME for ALL clusters!Flat M/L on large scales; SAME for ALL clusters!

Ωm= 0.2 +- .03

M/Li vs. R and M (Bahcall & Kulier ‘09)

M/Li vs. R and M (Bahcall & Kulier ‘09)

M/L Function: ConclusionsM/L Function: ConclusionsM/L Function: ConclusionsM/L Function: Conclusions

M/L Function Flattens on Large ScalesM/L Function Flattens on Large Scales M ~ LM ~ L (reaching end of Dark-Matter)

Dark Matter located mostly in large galactic halos ~200s Kpc) Group/Clusters: made up of Sp+E mix (+their halos); no significant additional DM

Cluster M/L increases slightly with M (Li* ; mergers?)

Asymptotic Cluster M/Li(22Mpc) is same for ALL

Groups and Clusters, 362+-54h !

Mass-Density of Univers: Mass-Density of Univers: mm = 0.2 +- 0.03 = 0.2 +- 0.03

M/L Function Flattens on Large ScalesM/L Function Flattens on Large Scales M ~ LM ~ L (reaching end of Dark-Matter)

Dark Matter located mostly in large galactic halos ~200s Kpc) Group/Clusters: made up of Sp+E mix (+their halos); no significant additional DM

Cluster M/L increases slightly with M (Li* ; mergers?)

Asymptotic Cluster M/Li(22Mpc) is same for ALL

Groups and Clusters, 362+-54h !

Mass-Density of Univers: Mass-Density of Univers: mm = 0.2 +- 0.03 = 0.2 +- 0.03

Cluster Abundance and EvolutionCluster Abundance and Evolution Cluster Abundance and EvolutionCluster Abundance and Evolution

Powerful method to determine Powerful method to determine mm and and 88

8 8 = Amplitude of mass fluctuations = Amplitude of mass fluctuations (initial ‘seeds’)(initial ‘seeds’)

nncl cl (z~0)(z~0) 8 8 mm0.6 0.6 ~ ~ 0.350.35

nncl cl (hi z)(hi z) Breaks degeneracy Breaks degeneracy

mm=0.2+-0.05 =0.2+-0.05 andand 88=0.9+-0.1=0.9+-0.1

Powerful method to determine Powerful method to determine mm and and 88

8 8 = Amplitude of mass fluctuations = Amplitude of mass fluctuations (initial ‘seeds’)(initial ‘seeds’)

nncl cl (z~0)(z~0) 8 8 mm0.6 0.6 ~ ~ 0.350.35

nncl cl (hi z)(hi z) Breaks degeneracy Breaks degeneracy

mm=0.2+-0.05 =0.2+-0.05 andand 88=0.9+-0.1=0.9+-0.1

Cluster Mass-FunctionCluster Mass-Function (SDSS)(SDSS)(Bahcall, Dong, et al ‘03)(Bahcall, Dong, et al ‘03)

Best-fit MF: Best-fit MF: mm=0.2 and =0.2 and 88=0.9=0.9

Cluster Mass-FunctionCluster Mass-Function (SDSS)(SDSS)(Bahcall, Dong, et al ‘03)(Bahcall, Dong, et al ‘03)

Best-fit MF: Best-fit MF: mm=0.2 and =0.2 and 88=0.9=0.9

Fit: Fit: mm=0.2=0.2 88=0.9=0.9

mm - - 8 8 constraints from MF: constraints from MF:

mm = 0.2 and = 0.2 and 88 = 0.9 = 0.9

mm - - 8 8 constraints from MF: constraints from MF:

mm = 0.2 and = 0.2 and 88 = 0.9 = 0.9

mm=0.2, =0.2, 88=0.9=0.9

m - 8 constraints from SDSS cluster MF

[Bahcall etal ‘03 Rozo etal ’09]

m - 8 constraints from SDSS cluster MF

[Bahcall etal ‘03 Rozo etal ’09]

mm=0.2, =0.2, 88=0.9=0.9

Cluster Abundance Evolution Cluster Abundance Evolution 88 (Bahcall & Bode ‘03)(Bahcall & Bode ‘03)

Cluster Abundance Evolution Cluster Abundance Evolution 88 (Bahcall & Bode ‘03)(Bahcall & Bode ‘03)

88

Cosmological Constraints Cosmological Constraints (Bahcall & Bode)(Bahcall & Bode)

(from Low and Hi redshift cluster abundance)(from Low and Hi redshift cluster abundance)Cosmological Constraints Cosmological Constraints (Bahcall & Bode)(Bahcall & Bode)

(from Low and Hi redshift cluster abundance)(from Low and Hi redshift cluster abundance)

Hi zHi zLow zLow z

Weighing the UniverseWeighing the UniverseWeighing the UniverseWeighing the Universe

M/L Function M/L Function mm= 0.2 +- 0.05= 0.2 +- 0.05 Baryon Fraction 0.24 +- 0.04Baryon Fraction 0.24 +- 0.04 Cluster Abundance 0.2 +- 0.05Cluster Abundance 0.2 +- 0.05

and Evolution [and Evolution [8 8 == 0.9 +- 0.1]0.9 +- 0.1] Supernovae Ia + Flat 0.25 +- 0.05Supernovae Ia + Flat 0.25 +- 0.05 CMB + LSS + h + Flat 0.25 +- 0.03CMB + LSS + h + Flat 0.25 +- 0.03 m m ≈ 0.23 +- 0.03≈ 0.23 +- 0.03

4% Baryons 4% Baryons

Mass ~ LightMass ~ Light (R >~ 1Mpc)(R >~ 1Mpc)

M/L Function M/L Function mm= 0.2 +- 0.05= 0.2 +- 0.05 Baryon Fraction 0.24 +- 0.04Baryon Fraction 0.24 +- 0.04 Cluster Abundance 0.2 +- 0.05Cluster Abundance 0.2 +- 0.05

and Evolution [and Evolution [8 8 == 0.9 +- 0.1]0.9 +- 0.1] Supernovae Ia + Flat 0.25 +- 0.05Supernovae Ia + Flat 0.25 +- 0.05 CMB + LSS + h + Flat 0.25 +- 0.03CMB + LSS + h + Flat 0.25 +- 0.03 m m ≈ 0.23 +- 0.03≈ 0.23 +- 0.03

4% Baryons 4% Baryons

Mass ~ LightMass ~ Light (R >~ 1Mpc)(R >~ 1Mpc)

Mazal Tov, Tsvi!From the Bahcall’sMazal Tov, Tsvi!

From the Bahcall’s

John Bahcall: “Nova” clip 2003 (‘Dancing’)John Bahcall: “Nova” clip 2003 (‘Dancing’)