Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999)...

29
Raul Jimenez University of Pennsylvania www.physics.upenn.edu/~raulj from WMAP web site

Transcript of Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999)...

Page 1: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Raul JimenezUniversity of Pennsylvania

www.physics.upenn.edu/~raulj

from WMAP web site

Page 2: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Supernovae

Standard candles

F

LDL π4

=

Function of geometry and Content of Universe

Page 3: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Vacuum energy Λ(also known as dark energy or cosmological constant)

1917vacuum

V1

V2

E1= ρv V1

E2>E1

Negativepressure!

E2= ρv V2

Λ

Page 4: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

CMBCMB+H prior

SN 1A

2dFGRS

Riess et al. 2002

(w/ Perlmutter et al 1999)

Verde et al. 2002, Percival et al 2001

Spergel et al 2003

Freedman et al 2001

Riess et al ‘04

Vacuum energy?

Dark energy?

from Verde (2003)

Page 5: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

We can “measure” dark energy because of its effects on theexpansion history of the universe: a(t)

SN: measure dL

CMB: A and ISW a(t)LSS or LENSING: g(z) or r(z) a(t)

AGES: H(z) a(t)

''

)'1()1(0

dzdz

dtzzd

z

L ∫ ++=

dt

dz

zzH

ta

ta

)1(

1)(

)(

)(

+−==

&

θ

)]0(/)([022 ρρ zHH =

QQ zwzH ρρ ))(1)((3 +−=&

∫ +Ω+Ω+−=−

z

QQm wz

dzz

dt

dzH

0

2/12/510 ]}

)'1(

'3exp[)0()0({)1(

Page 6: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

1a:WMAP+external data sets:Constraints on Quintessence (?)

12.098.0 ±−=w

(Spergel et al. 2003)

Effective w

Page 7: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Constraints on Quintessence WMAP+external data sets:

(Spergel et al. 2003)

8.0−<w

-1.

-1. -1.

-1.

Effective w

Page 8: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Constraints on Quintessence WMAP+external data sets:

(Spergel et al. 2003)

8.0−<w

-1.

-1. -1.

-1.

Effective w

Page 9: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

1a- WMAP + external data sets results resultsresults

(WMAP team 2003)

2a-2a- Globular clusters agesGlobular clusters ages resultsresults(in collaboration with L. Verde, T. Treu, D. Stern 2003)

1b- CMB X lensing X Rees Sciama Future:ACTFuture:ACT

(Verde & Spergel 2002)

2b- Non-parametric w(z) (Non-parametric w(z) (dzdz//dtdt) ?) ?(in collaboration with Joan Simon, L. Verde 2003-2004)(in collaboration with Joan Simon, L. Verde 2003-2004)

preliminarypreliminary

1:CMB and Large scale structure

2: A cosmologist’s use of stars

LARGE SCALES:

SMALL SCALES:

Page 10: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Assume the universe to be flat: depends on w and age

l1=sound horizon(decoupling)/angular diameter distance (decoupling)

for a fixed value of w, a change in _ mh2 that keeps fixed will also keep age unchanged (Cadwell et al. 1998, Knox et al. 2001, Hu et al. 2001)

2a:Globular clusters ages: THEORY

1l

1l

Effective w

Page 11: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

independent age estimate

Monte Carlo forage of oldest GCpaying carefulattention tosystematics

From Krauss & Chaboyer 2003

M92

2a: Globular clusters ages:

]2]/)ln[(exp[

)()(

2

σσmTt

Tt

AtP −−

−=

OFFSET

Page 12: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

WMAP

68%

90%

age

age

Constraint on “effective” w 2a:Globular clusters ages:

(Jimenez , Verde, Treu, Stern, 2003)Very weak priors on 50 < H < 95 0 < _ m < 0.5

1l

(Page et al. 2003)

Page 13: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

...++Δ

+Θ∇•Δ

≅Δ

SZTT

TT

TT

TT NLPP

γ

Lensing

∫ Φ−

−=Θ*

0 *

* ),(2)(r

drrrrrrr

γγ

drrrtT

T NLNL

),(2 γΦ∂∂

Rees-Sciama

Low z(high l )

High z (low l )

Depends on w,0Ω

Gravitational potential

1b:Dark energy and secondary CMB1b:Dark energy and secondary CMB(Verde, Spergel 2002,PRD)

ISW, but non-linear

Page 14: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

1b: Bispectrum :Luo 1994,…. Spergel Goldberg 1999, Goldberg, Spergel 1999, Komatsu,Spergel 2001 etc…

to couple the high z universe (low ) to thelow z universe (high ) via the weak lensing signal

Balance of 2 competing contributions:

Decay of gravitational potential (non Einstein de Sitter Universe)

Amplification due to non-linear gravitational evolutionBalance depends on Ωm and w

Bl1l 2l 3

m1m2m3 = al1

m1al 2

m2al 3

m3 =l1l 2l 3

m1m2m3

Bl1l 2l 3

ll

Consider primordial, lensing & Rees-Sciama:

Page 15: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

(Verde, Spergel 2002)

Bispectrum: Cross correlating primordial-lensing-Rees Sciama

ACT+WMAP2yr data

Fiducial model

See also Giovi Baccigalupi, Perrotta 2003 for w(z)

Page 16: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

The ACT telescope

The Atacama in Chile5200 meter elevation, dry, low turbulence, close to ALMA

6 m telescope

CCD like array of bolometers

PENN CUNY

Columbia

Toronto

Haverford

Princeton

CatÓlica

100 sq degrees

3 frequencies for SZ

1.7’beam

145, 220, 270 GHz

P.I. Lyman Page

More info: http://www.physics.upenn.edu/act

Page 17: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Arcminute Resolution mm-wave Observations150 GHz

SZ Simulation MBAC on ACT 1.7’beam w/ 2X noise

PLANCK

MAP

PLANCK

1.4°

< 1% ofsurvey area

~2% of highquality area

Page 18: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

from Maor et al. 2000

Reconstructing w: a difficult task

SNAP error

Page 19: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

2b:Reconstruct w(z): use dz/dt

z

Non-parametric!

(from Jimenez & Loeb 2002)

''

)'1()1(0

dzdz

dtzzd

z

L ∫ ++=Note:

dt

dz

zzH

)1(

1)(

+−=

w(z) in here

)()1(2

3

)(2

3

2

5)1(

4

12

2

2

zwz

zwzdt

dz

dt

zd

m +Ω−

++

= −

Page 20: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

Old, passively evolving galaxies

2b:Reconstruct w(z): cosmic chronometers

Is it possible to obtain accurate ages?

(From Jimenez, LV, Treu, Stern 2003)

The Red Envelope

Page 21: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

2b:Simulating the “edge”, error budget, tests for sistematics

See also Jimenez & Loeb 2001

Small burst of SF?

Page 22: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

2b:Reconstruct w(z): Age-redshift relation

z=0

z=0.1

EDR SDSS

Treu sample(field galaxies)

MS1054-0321 (Stern)

53W091, 53W069

WMAPLCDM

Page 23: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

From Bernardi et al. 2003

Low-er z

High-er z

Page 24: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

2b:Reconstruct w(z) with dz/dt: Difficult, BUT:

Battery of tests for effects possible systematics

Relative ages !!!

At 1≈z the rest frame UV spectrum of ellipticals is dominated by main sequence stars

(Jimenez & Loeb 2002, Jimenez , LV, Treu, Stern 2003)

Neutrinos le

sson

You’ve got to be honest with uncertainties

Many high S/N spectra will help improve the statistics.

Page 25: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

The edge for z<0.2

The value of H0

2b:Reconstruct w(z): CAN IT work?

At z=0 dz/dt gives Ho and we have SDSS galaxies:

dt

dz

zzH

)1(

1)(

+−=

Page 26: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

2b: Reconstruct w(z):

Every high-z spectrum helps: Please give generously!

preliminary

2−=w z>1

Linearly tow=0 for 0<z<1

Age-redshift relation

Page 27: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

New data at high-z

w=0w=-1

ACT will observe about 1000 clusters (50000 spectra up to z ~ 1)

Models with arbitrary H0

Page 28: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

The almost “impossible” task of reconstructing the potential

from Maor et al. 2002

Page 29: Raul Jimenez - FCUP...CMB+ CMB H prior SN 1A 2dFGRS Riess et al. 2002 (w/ Perlmutter et al 1999) Verde et al. 2002, Percival et al 2001 Spergel et al 2003 Freedman et al 2001 Riess

The effective w is around –1.It’s important to beat systematics by using cross checks.

The next challenge is to track w(z) possibly in a non-parametric way

I have shown a preliminary attempt to do just this using relative ages

More data are needed More data are needed

12.098.0 ±−=wWMAPext: CG ages: w< -0.8

For the moment, looks like dark energy is consistent with ΛSDSS consistent