Problems and Alternatives to Lambda Cold Dark Matter - Berkeley ...

Problems and Alternatives to 

Lambda Cold Dark Matter 

Tonatiuh Matos 

http://www.fis.cinvestav.mx/~tmatos/ 

http://www.iac.edu.mx 

The LCDM 

Some Problems of the LCDM 

Some Alternatives

• Space-time: FLRW 

• Matter: DM (p = 0), DE (p = -ρ), b (p = 0), 

rad (p = 1/3 ρ), ν (p = 1/3 ρ), etc.

• Space-time: FLRW 

• Matter: DM (p = 0), DE (p = -ρ), b (p = 0), 

rad (p = 1/3 ρ), ν (p = 1/3 ρ), etc. 

• Inflation 

• BBN 

• CMB 

• Structure formation 

The Standard Model of 

Cosmology: LCDM


Cosmology: LCDM


Cosmology: LCDM 

4



CDM Paradigme 

• 1.- The DM fluctuation spectrum at recombination is detemined by a small 

number of physical paramenters. 

4



CDM Paradigme 



• 2.- After recombination, the amplitude of the baryonic fluctuations rapidly 

grows to match that of the DM fluctuations. 

4



CDM Paradigme 





• 3.- Smaller-mass fluctutions grow to nonlineartity and virialize and then are 

hirarchically clustered within successively larger bound systems. 

4



CDM Paradigme 





• 3.- Smaller-mass fluctutions grow to nonlineartity and virialize and then are 

hirarchically clustered within successively larger bound systems. 

10 8−12 M⊙ 

• 4.- Ordinary matter in bound systems of total mass cools rapidly 

enough within the DM halos to form galaxies, while larger mass fluctutations 

form clusters 

4

z=18.3 


Cosmology: LCDM

z=18.3 


Cosmology: LCDM

z=5.7 


Cosmology: LCDM

z=1.4 


Cosmology: LCDM

z=0 


Cosmology: LCDM


Cosmology: LCDM


Cosmology: LCDM



7



Ωχ h 2 = 3 × 10−27 cm 3 s −1 

σv 

σv ∼ 3 × 10 −26 cm 3 s −1 

7

Candidates: 

Axions 

Sterile neutrinos 

MSSM: neutralino, 

gravitino, etc. 



Ωχ h 2 = 3 × 10−27 cm 3 s −1 

σv 

σv ∼ 3 × 10 −26 cm 3 s −1 

7

Candidates: 

Axions 

Sterile neutrinos 

MSSM: neutralino, 

gravitino, etc. 



Ωχ h 2 = 3 × 10−27 cm 3 s −1 

σv 

σv ∼ 3 × 10 −26 cm 3 s −1 

Observations: 

1.- Detection of products of 

annihilation or decay of these particles 

2.-Interactions with nuclei in 

underground detectors 

7

Dama/Libra 

8

Dama/Libra 

8

But a light WIMP, (10-100GeV, 

CoGeNT collaboration) is in 

tension with the first 

XENON100 results. 

Aprile, E. et al. First dark matter results from the 

XENON100 experiment. arXiv:1005.0380. 

Dama/Libra 

8

• 1 km 3 Antartic ice with 

• Fotoelectric sensors 

• Ready in 2011

IceCube Neutrino Telescope in Antartic 

• 1 km 3 Antartic ice with 

• Fotoelectric sensors 

• Ready in 2011

ANTARES –Telescopio de Neutrinos en el 

Mediterraneo

ANTARES –Telescopio de Neutrinos en el 

Mediterraneo 

11

γ 

χχ → γγ

Telescopio HESS, 

Namibia (2004) 

γ 

rays satellites 

GLAST Satellite 

Start 11. Juni 2008 

χχ → γγ 

MAGIC I, II(const), La Palma

LHC 

LHC in CERN (Genf) 

2009

SuperCDMS 1TG 

Lux (3 T liq Xe) 

Xenon 1T 

Xenon 100 

Direct search 

of WIMP’s 

Gianfranco Bertone, Nature,468(2010)389 

CDMS II 

4 parameters 

7 parameters

SuperCDMS 1TG 

Lux (3 T liq Xe) 

Xenon 1T 

Xenon 100 

Direct search 

of WIMP’s 

Gianfranco Bertone, Nature,468(2010)389 

CDMS II 

4 parameters 

7 parameters


Cosmology: Problems 

• Extreme fine tuning 

• Coincidence 

• Cuspy central density profiles 

• Missing Satellites Problem 

• No-fit of the early assembly of galaxies 

• Galaxies seems to be simpler 

• Voids are too empty 

• No-detection of DM 

• etc.


Cosmology: Problems 

• Cuspy central density profiles 

• Missing Satellites Problem 

• No-fit of the early assembly of galaxies 

• Galaxies seems to be simpler 

• Voids are too empty 

• No-detection of DM 

• etc.

Galaxy´s density 

Observed 

Theory 

ρNFW = 1 

x 

ρNFW ∼ 1 

x 

ρ ∼ 1 

x α 

0 < α < 1 

δ0ρ0 

(1 + x) 2 

17

Galaxy’s Density 

Galaxy´s density 

Observed 

Theory 

ρNFW = 1 

x 

ρNFW ∼ 1 

x 

ρ ∼ 1 

x α 

0 < α < 1 

δ0ρ0 

(1 + x) 2 

17

W. J. G. de Blok, Stacy S. McGaugh, Albert Bosma, and Vera C. Rubin. ApJ Letters 552(2001)L24 

18

Galaxy’s Center: Observations 

W. J. G. de Blok, Stacy S. McGaugh, Albert Bosma, and Vera C. Rubin. ApJ Letters 552(2001)L24 

18


Joshua D. Simon, Alberto D. Bolatto, Adam Leroy, and Leo Blitz, astro-ph/0310193 

19

NFW 


20

Galaxy’s Center: Simulations

Galaxy’s Center: Simulations 

F. Gobernato, et. al., NATURE, Vol 463, 14 January 2010






F. Gobernato, et. al., NATURE, Vol 463, 14 January 2010 

General results from several samples 

including THINGS, HI survey of uniform 

and high quality data, imply that Tri-axiality 

and non-circular motions cannot explain 

the CDM/NFW cusp/core discrepancy 

ej: J. van Eymeren, C. Trachternach, B. S. Koribalski and R.- 

J. Dettmar: A&A arXiv:0906.4654

No evidence for internal features 

or star formation that could be the 

result of tidal processes or star 

formation induced by the cluster 

environment. 

ej: Samantha J. Penny, Christopher J. Conselice, 

Sven De Rijcke and Enrico V. Held: 

Mon. Not. R. Astron. Soc. 393, 1054–1062 (2009), 

etc. 


F. Gobernato, et. al., NATURE, Vol 463, 14 January 2010 

General results from several samples 

including THINGS, HI survey of uniform 

and high quality data, imply that Tri-axiality 

and non-circular motions cannot explain 

the CDM/NFW cusp/core discrepancy 

ej: J. van Eymeren, C. Trachternach, B. S. Koribalski and R.- 

J. Dettmar: A&A arXiv:0906.4654

Stellar Mass Predictions 

Till Sawala, Qi Guo, Cecilia Scannapieco, Adrian Jenkins and Simon White. Mon. Not. R. Astron. To appear. 

23

Stellar Mass Predictions 

Till Sawala, Qi Guo, Cecilia Scannapieco, Adrian Jenkins and Simon White. Mon. Not. R. Astron. To appear. 

The dwarf galaxies formed in 

hydrodynamical simulations 

are almost two orders of 

magnitude more luminous 

than expected for haloes of 

this mass. 

23

Velocity predictions 

Jesús Zavala, et. al. The Astrophysical Journal, 700:1779–1793, 2009 August 1 

24

Velocity predictions 

Jesús Zavala, et. al. The Astrophysical Journal, 700:1779–1793, 2009 August 1 

The simulation with CDM predicts 

a steep rise in the VF toward lower 

velocities; for Vmax = 35 km/s, it 

forecasts ∼10 times more sources 

than the ones observed. If 

confirmed by the complete 

ALFALFA survey, these results 

indicate a potential problem for the 

CDM paradigm 

24

Missing Satellites Problem

Missing Satellites Problem

Missing Satellites Problem 

26

Missing Satellites Problem 

26

Galaxies appear simpler than 

expected 

M. J. Dysney, et. al. Vol 455(2008)1082 

R90 ∝ R50 

Lg ∝ R 3 50 

MHI ∝ R 2 50 

Md ∝ Lg 

Σ = Lg/R 2 50 ∝ L 1/3 

g 

Whereas 

Lg/R 3 50 

Md/R 3 50 

∝ R50 

are independent of the size 

of the galaxy

Galaxies appear simpler than 

expected 

M. J. Dysney, et. al. Vol 455(2008)1082 

Such a degree of organization 

appears to be at odds with 

hierarchical galaxy formation, a 

central tenet of the cold dark 

matter model in cosmology.

Voids are too empty 

P. J. E. Peebles & A. Nusser, Nature 465(2010)565 

28



It is not clear why objects 

that might have been 

assembled in such very 

different ways, from different 

ancestral objects, should 

have had evolutionary tracks 

that converged to show 

small dispersions around 

simple power law forms for 

their size–luminosity 

relations. 

Nair, P. B., van den Bergh, S. & Abraham, 

R. G. The environmental dependence of 

the luminosity-size relation for galaxies. 

Astrophys. J. 715, 606–622 (2010). 

28



In short, the general 

insensitivity of galaxies to 

their environments is not 

expected in standard ideas. It 

would help if galaxies were 

more rapidly assembled, as 

they could then evolve as 

more nearly isolated island 

universes. 

28

Early assembly of the most 

massive galaxies 

Chris A. Collins, et. al. Nature, 458(2009)603

Early assembly of the most 

massive galaxies 

Chris A. Collins, et. al. Nature, 458(2009)603 

This suggest a new 

picture in which 

brightest cluster 

galaxies experience an 

early period of rapid 

growth rather than 

prolonged hierarchical 

assembly.

Pieter G. van Dokkum et. al. NATURE, Vol 460, 6 August 2009. The Astrophysical Journal, 677:L5–L8, 2008 April 10 

30

Early Galaxies 

Compactness 


30

Early Galaxies 

Compactness 


z=2.3 Galaxies 

31

1E 0657-56, "Bullet Cluster” 

2006 

32

Clusters Collisons 

Mastropietro, C., & Burkert, A. 2008, MNRAS, 389, 967 


2006 

The morphology of X-ray maps, the height 

of the projected temperature jump and the 

displacement of the gas peaks are best 

simulated by 6:1 encounters with initial 

velocity 3000 km/s 

32

The only way to fit the observational data 

using NFW profiles would be to assume 

a mass ratio as small as 2.7:1, which 

would not reproduce X-ray data. 


Mastropietro, C., & Burkert, A. 2008, MNRAS, 389, 967 


2006 

The morphology of X-ray maps, the height 

of the projected temperature jump and the 

displacement of the gas peaks are best 

simulated by 6:1 encounters with initial 

velocity 3000 km/s 

32

MACS J0025.4-1222 

2008 


33

MACS J0025.4-1222 

2008 


J. Lee & E. Komatsu, ApJ, 718(2010)60 

33

MACS J0025.4-1222 

2008 


J. Lee & E. Komatsu, ApJ, 718(2010)60 

Gpc 3 /h 3 

With a large-volume (27 ) 

cosmological N-body MICE simulation, the 

probability of finding 3000 km/s is between 

3.3 x 10 and 3.6 x . 

−11 10 −9 

33

Shaun A. Thomas, Filipe B. Abdalla, and Ofer Lahav. arXiv:1012.2272 

. 

. 

. 

0.55

Large scale structure anomaly 

Shaun A. Thomas, Filipe B. Abdalla, and Ofer Lahav. arXiv:1012.2272 

. 

. 

. 

0.55

Some Alternatives 

SM Extentions GR Extentions

• Self-Interacting DM 

• Warm DM 

• Super Heavy DM 

• Self-Annihilating DM 

• Decaying DM 

• Extra Symmetries, 

• Repulsive DM 

• Fuzzy DM 

• k-essence 

• Scalar Field DM 

(BEC DM), etc. 


SM Extentions GR Extentions


• Warm DM 






• Fuzzy DM 

• k-essence 




SM Extentions GR Extentions 

• Scalar Field DM (BEC DM) 

• MOND -> MOND+ 

• f(R) 

• Extra Dimensions 

• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.

Self-Interacting and Warm DM 

Rachel Kuzio de Naray, Gregory D. Martinez, James S. Bullock, Manoj Kaplinghat. ApJ161(2010) 710L 

38



39



ED3,4 

Th1,2 

Qρ = ¯ρ 

¯σ 3 

39



ED3,4 

Th1,2 

Qρ = ¯ρ 

¯σ 3 

The inferred cores do not 

provide motivation to prefer 

WDM or SIDM over other 

dark matter models 

39



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.

pbar/p 

1e-04 

1e-05 

Pamela Constrains 

New Constraints from PAMELA anti-proton data on Annihilating and Decaying DM Ilias Cholis 

arXiv:1007.1160 

0.001 

m = 1 TeV, BF = 28, AMS-02 expectation 

W + W - 

m = 10 TeV, BF = 2200, AMS-02 expectation 

Background 

PAMELA Data 

1e-06 

0.1 1 10 

kinetic energy (GeV) 

100 

42


43

DM lifetime [s] 

10 27 

10 26 

10 25 

10 24 

10 23 

µ+µ final state - dSph, without IC 

Ursa Minor 

Ursa Major II 

Bootes I 

Sextans 

Fornax 

Draco 

Sculptor 

Coma Berenices 

Galactic + EG 

Previous Constraints 


Leanna Dugger, Tesla E. Jeltemaa and Stefano Profumo, JCAP12(2010)015 

PAMELA 

PAMELA 

+FERMI 

100 1000 10000 

DM mass [GeV] 


10 27 

10 26 

10 25 

10 24 

10 23 

10 22 

PAMELA 

µ+µ final state - M31 

NFW, point-like source, D 0 =10 28 cm 2 /s 

Extended source, M vir , D 0 =10 28 cm 2 /s 



PAMELA 

+FERMI 

Galactic + EG 


43 

1000 10000 

DM mass [GeV]


10 27 

10 26 

10 25 

10 24 

10 23 

µ+µ final state - dSph, without IC 

Ursa Minor 

Ursa Major II 

Bootes I 

Sextans 

Fornax 

Draco 

Sculptor 

Coma Berenices 

Galactic + EG 



Leanna Dugger, Tesla E. Jeltemaa and Stefano Profumo, JCAP12(2010)015 

PAMELA 

PAMELA 

+FERMI 

100 1000 10000 

DM mass [GeV] 

These results put strong constraints on the 

possibility of ascribing to decaying dark matter 

both the increasing positron fraction reported 

by PAMELA and the high-energy feature in the 

electron-positron spectrum measured by Fermi 


10 27 

10 26 

10 25 

10 24 

10 23 

10 22 

PAMELA 

µ+µ final state - M31 





PAMELA 

+FERMI 

Galactic + EG 


43 

1000 10000 

DM mass [GeV]



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.

Extra Symmetries 

A. de la Macorra, C. Stephan-Otto, Phys. Rev. Lett. 87 (2001) 271301 

The starting point is a dark gauge group “DG” whose particles interact with the 

standard model only via gravity. 

The gauge coupling constant becomes strong at lower energies, it will bind the 

elementary dark fields together at the phase transition or condensation scale Λc. 

Above this scale the particles are massless and at the condensation scale Λc they 

acquire a mass of the order of Λc. 

The elementary fields will form gauge invariant particles due to the strong coupling. 

These particles are dark “mesons” and dark “baryons”. 

45


A. de la Macorra, C. Stephan-Otto, Phys. Rev. Lett. 87 (2001) 271301 

The starting point is a dark gauge group “DG” whose particles interact with the 

standard model only via gravity. 

The gauge coupling constant becomes strong at lower energies, it will bind the 

elementary dark fields together at the phase transition or condensation scale Λc. 

Above this scale the particles are massless and at the condensation scale Λc they 

acquire a mass of the order of Λc. 

The elementary fields will form gauge invariant particles due to the strong coupling. 

These particles are dark “mesons” and dark “baryons”. 

Ej: The model with SU(3) gauge group has 6 chiral + antichiral fields with 

97.5 degrees of freedom, a condensation scale Λc = 42 eV and an 

inverse power potential with V = Λ , n = 2/3. 

This model gives a warm DM with a free streaming scale λfs < 0.6 Mpc 

and an equation of state parameter for the DE wDEo=−0.9 with Ωm = 0.27, 

ΩDEo = 0.73. 

4+n 

c φ −n 

45


46


Cosmological Scalar Fields Unification. Perez-Lorenzana, et. al. Phys. Rev. D77, (2008), 063507 

Invariant under 

SU(1, 1) 

46

L = 1 


Cosmological Scalar Fields Unification. Perez-Lorenzana, et. al. Phys. Rev. D77, (2008), 063507 

Invariant under 

SU(1, 1) 

2 [∂µφ∂ µ φ + ∂µφ ∗ ∂ µ φ ∗ ] 

46


47

35 

30 

25 

20 

15 

10 

5 

0 

4 


2 

0 

y0 k y 

-2 

-4 

-1 

-0,5 

0 

0,5 

1 

l k f 

47



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.

Repulsive, Fuzzy and 

Scalar Field DM 

49

Repulsive, Fuzzy and 

Scalar Field DM 

49

Ideas 

Matos-Guzman 2000 

P. J. E. Peebles 2000

Ideas 

Perez-Lorenzana-et. al. 2007 

Matos-Guzman 2000 

P. J. E. Peebles 2000 

Ureña-Lopez-et. al. 2000 

Ureña-Lopez-Liddle 2007 

Cervantes-Rodriguez 2001

Bose-Einstein Condensates 

☐☐☐☐ 

= 0

The Cosmology

The Cosmology 

Φ 2 as Dark Matter. T. Matos, A. Vázquez & J.A. Magaña. MNRAS, 389, (2009) 13957.

The Cosmology 

Φ 2 as Dark Matter. T. Matos, A. Vázquez & J.A. Magaña. MNRAS, 389, (2009) 13957.

Linear regime of perturbations

Linear regime of perturbations 

δ ¨ Φ +3Hδ ˙ Φ − 1 

a 2 ∇2 δΦ + V,ΦΦ δΦ +2V,Φ φ =0


δ ¨ Φ +3Hδ ˙ Φ +(− 1 

a 2 ∇2 − m 2 )δΦ +2V,Φ φ =0


δ ¨ Φk +3Hδ ˙ Φk +( 1 

a 2 k2 − m 2 )δΦk +2V,Φ φ =0


δ ¨ Φk +3Hδ ˙ Φk +( 1 

a 2 k2 − m 2 )δΦk +2V,Φ φ =0


δ ¨ Φk +3Hδ ˙ Φk +( 1 

a 2 k2 − m 2 )δΦk +2V,Φ φ =0

Galactic Collapse of Scalar Field Dark Matter. 

M.Alcubierre, F. S. Guzmán, T. Matos, D. Núñez, L. A. Ureña and P. Wiederhold. CQG 19(2002)5017. arXiv:gr-qc /0110102.

Scalar Field Fluctuation = Halo 

Galactic Collapse of Scalar Field Dark Matter. 

M.Alcubierre, F. S. Guzmán, T. Matos, D. Núñez, L. A. Ureña and P. Wiederhold. CQG 19(2002)5017. arXiv:gr-qc /0110102. 

• M ≈ 0.1 M 2 Planck/m Φ 

• If m Φ ≈ 10-22 eV 

• M ≈10 12 Mo

Weak Field Limit 

A. Bernal, et. al. Flat Central Density Profiles from Scalar Field Dark Matter Halo. Rev. Mex. A.A. 44, (2008), 149-160

T. Harko & C. G. Bhömer JCAP 0706:025,(2007) arXiv:0705.4158

Density Profiles 

T. Harko & C. G. Bhömer JCAP 0706:025,(2007) arXiv:0705.4158

Density Profiles LSB Galaxies

Density Profiles LSB Galaxies

Hydrodinamical version of the 

Linear regime of perturbations



62



65



66

0.0001 

9e-05 

8e-05 

7e-05 

6e-05 

5e-05 

4e-05 

3e-05 

2e-05 

1e-05 



0 

0 0.0002 0.0004 0.0006 0.0008 0.001 0.0012 

t 

 

67

SFDM



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.

M. Milgrom. Acta Phys.Polon.B32:3613,2001. e-Print: astro-ph/0112069 

71

MOND and MOND+ 

R. H. Sanders. The Astrophysical Journal, 512:L23–L26, 1999 February 10 

72


J. D. Bekenstain. PHYSICAL REVIEW D, VOLUME 70, 083509 

73

EG = 1 

β 

Υgm 

Υgg 


R. Reyes, R. Mandelbaum, U. Seljak, T. Baldauf, J. E. Gunn, L. Lombriser & R. E. Smith. NATURE, Vol 464, 11 March 2010 

74


S. Mendoza, X. Hernandez, J.C. Hidalgo & T. Bernal. arXiv: 1006.5037 

75



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.



• Warm DM 






• Fuzzy DM 

• k-essence 






• f(R) 


• etc.

f(R) 

Yong-Seon Song, Hiranya Peiris, and Wayne Hu. Phys.Rev.D76:063517,2007 

78

f(R) 

Dark matter as a geometric effect in f(R) gravity C. G. Böhmer, T. Harko, F. S.N. Lobo. Astroparticle Physics 29 (2008) 386–392 

A Model of f(R) Gravity as an Alternative for Dark Matter in Spiral Galaxies. S. Asgari. Applied Physics Research. Vol. 2, No.1, 2010 

79

T. Damour & Esposito-Farèse. PRL 70(1993)2220 

f(R) 

J. Khoury & A. Weltman. PRL 93(2004)171104 

80

Extra Dimensions 

81

Hidden Brane Visible Brane 

Scalar Field 

Extra Dimensions 

M. A. G-Aspeitia, et. al. Gen Relativ Gravit (2011) 43:315–329 

b0 

Standard Model 

81

Conclusion

Conclusion 

• We are in the threshold for a new 

era in Cosmology, Science and 

Thought

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