Carlos Muñoz

Carlos Muñoz

Fermi-LAT prospects for the detection of µνSSM gravitino dark matter

DSU 2011, Beijing, September 26-30

Crucial Moment for SUSY in next few years, since the LHC is working

Carlos Muñoz 2SSM gravitino DM

OUTLINE

Assuming that SUSY will be discovered at the LHC, the question is:what SUSY model do we expect to be the one to be observed ?

MSSM, NMSSM, BRpV,... ..., may be SSM

Its interest resides in the fact that it solves simultaneously the µ problem of the MSSM and the origin of neutrino masses

The solution implies that R-parity is explicitly broken

In models without R parity the LSP is no longer stable

Thus the neutralino or the sneutrino cannot be used as candidates for DM

Gravitino as a DM candidate in the SSM Detection using Fermi-LAT ?

SUSY has a very important problem, the so-called µ problem:

+ µ H1 H2MSSM W =

µ H1 H2 is necessary to generate Higgsino masses.Present experimental bounds imply: µ ≥ 100 GeV What is the origin of µ, and why is so small: MW << MPlanck


SSM

: EW seesawNo ad-hoc scales

The scale will appearthrough the soft terms

We will also have the three heavy neutrinos with masses

EW

m mD2/MM = (YH2)2/(k R GeV = 10-

2 eV

The last type of terms in (1) is allowed by all symmetries, and avoids the presence of a Goldstone boson associated to a global U(1) symmetry.

López-Fogliani, C.M., PRL 2006

c (+1)

~H2 (-1)

H1 (+1)

Size of the breaking: Y 0 the R are no longer neutrinos, they are just ordinary singlets like the S of the NMSSM: S H1 H2 + SSS, and R-parity is conserved is small because the EW seesaw implies Y≤

S (-1)

~H2 (-1)

H1 (+1)

~

R-parity is explicitly broken: a vertex with only one SUSY particle


neutralino-neutrino mass matrix

~

B

g1e.g. this diagram determines the bino-neutrino mixing

g1 /M1 | -6–-8

Thus the photino content of the neutrino:

Since in the minimization equation for , Y≤ is present producing -4 GeV

Ghosh, Roy, “Neutrino masses and mixing, lightest neutralino decays and a solution to the problem in supersymmetry”, JHEP 04 (2009) 069 Bartl, Hirsch, Vicente, Liebler, Porod, “LHC phenomenology of the SSM”, JHEP 05

(2009) 120

* Decay of the lightest neutralino as LSP. Branching ratios show correlations with neutrino mixing angles, which can be tested at the LHC.

* The neutralino-LSP may decay within the detectors but with a length large enough to show a displaced vertex

Since R-parity is broken, the phenomenology of the SSM is going to be very different from the one of the MSSM/NMSSM, producing interesting signals at LCH

* The neutral Higgses are mixed with the right- and left-handed sneutrinos producing 8x8 scalar mass matrices, and therefore their decays at the LHC will be peculiar

Fidalgo, López-Fogliani, C.M., Ruiz de Austri, “The Higgs sector of the SSM and collider physics”,

JHEP 2011 Carlos Muñoz 7SSM gravitino DM

Carlos Muñoz SSM gravitino DM 8

Gravitino as a dark matter candidate in the SSM

Also talks studying gravitino dark matter in other modelsby A. Ibarra and J. Valle

Choi, López-Fogliani, C. M., Ruiz de Austri, JCAP 2010


• Gravitino as a DM candidate in models where R-parity is broken

The gravitino also decays through the interaction gravitino-photon-photino ():

due to the photino-neutrino mixing after sneutrinos develop VEVs , opening the channel

Takayama, Yamaguchi, 2000

Nevertheless, it is supressed both by the Planck mass and the small R-parity breaking,

thus the lifetime of the gravitino can be longer than the age of the Universe (1017 s)

In the SSM: U g1 /M1 -6–

-8

Carlos Muñoz 10

DETECTION

Decays of gravitinos in the galactic halo, at a sufficiently high rate, would produce gamma rays The FERMI gamma-ray space telescope,

launched on June 2008, might in principle detect these gamma rays

Buchmuller, Covi, Hamaguchi, Ibarra, Yanagida, 07 Bertone, Buchmuller, Covi, Ibarra, 07; Ibarra, Tran, 08Ishiwata, Matsumoto, Moroi, 08

SSM gravitino DM

The integration extends over the line of sight

The gravitino decays into a photon and neutrino, and the photonproduces a monochromatic line at energies equal to E= m3/2/2

Since Fermi-LAT covers an energy range 30 MeV – 300 GeV, gravitinos with masses between 60 MeV – 600 GeV could in principle be tested

An interesting possibility could be to search for DM in the Galactic Center, where the DM density is larger The problem is that the conventional astrophysics in the galactic center is not well understood: the modeling of the diffuse emission, unresolved sources, etc.

Talk by Gomez-Vargas about the galactic center

Carlos Muñoz 11SSM


correspond to the 5-month measurement reported by Fermi-LAT 0912.0973

K.Y. Choi, D.E. López-Fogliani, C. M., R. Ruiz de Austri, 0906.3681


Values of the gravitino mass larger than 10 GeV are disfavoured, as well as lifetimes smaller than about (3-5) x 1027 s.

In the SSM: U g1 /M1 -6–

-8


Values of the gravitino mass larger than about 4 GeV are excluded,as well as between 2 - 4 GeV with lifetimes smaller than about 6 x 1028 s

Fermi-LAT presented constrainst on monochromatic emission

Using 11 month data: derived limits between 30-200 GeV, 1001.4836

Using 23 month data: derived limits above 7 GeV, talk Feb. 2011

This affects the gravitino with amass larger than 14 GeV,leaving our region of interest unconstrained

Vertongen & Weniger, extended the line analysis of the Fermi-LAT data to 1-300 GeV in the region |b|>10º 1101.2610


Gómez-Vargas, Fornasa, Zandanel, Cuesta, C.M., Prada, Yepes, in preparation

Nearby clusters of galaxies are also attractive targets

-they are more distant, but very massive and very dark matter dominated-typically lie at high galactic latitudes where the contamination from galactic gamma-ray background emission is low

Explore the prospects for detecting SSM gravitino dark matter in galaxy clusters using the prediction for 5 years of operation of the Fermi-LAT telescope

Gravitino dark matter detection in nearby extragalactic structures

Strategy: 1-obtain the dark matter distribution from a constrained N-body simulation from the CLUES project talk by G. Yepes

Cuesta et al., 2010

2-obtain the flux multiplying the values in the map by the particle physics factor, and use this result as an input for the Fermi-LAT observation simulations

The The μνμνSSMSSM

17SSM gravitino DMCarlos Muñoz

Yuksel, Kistler, 0711.2906Choi et al, 0906.3681

Vertonger, Weniger, 1101.2610

Gómez-Vargas et al, in preparation

Conclusions

Solving the problem with neutrinos gives rise to the SSM

Only one scale in the model: the soft SUSY-breaking scale TeV

The model can be tested at the LHC

19Carlos Muñoz SSM gravitino DM

• The gravitino can be a candidate for dark matter, and since

R-parity is broken, might be detected by Fermi-LAT through its

decay producing gamma rays • No observation up to now excludes large regions of the parameter space, e.g. m3/2 < 4 GeV

Carlos Muñoz 20Direct WIMP Searches

21Carlos Muñoz SSM

Backup Slides

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22

* The neutralino-LSP may decay within the detectors but with a length large enough to show a displaced vertex

e.g. two-body decays

three-body decays e.g.

The decay lenght is basically determined by the mass of the neutralino LSP and the experimentally measured neutrino masses

Carlos Muñoz SSM 23

Bartl, Hirsch, Vicente, Liebler, Porod, JHEP 05

(2009) 120 e.g.

Carlos Muñoz

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