The WISP Paradigm

Javier Redondo

Max Planck Institut (Werner Heisenberg Institut) Munich

MPI 14/12/2009 Hidden Sectors in PBSM

Extensions of SM often include Hidden Sectors Fields coupled to SM only through gravity or high energy “messenger” ﬁelds...

This is the case in string theory (compactiﬁcations produce many particles, new gauge symmetries, and KKs) Desirable for SUSY Also in GUT theories...

Massive Messengers

Standard Model Hidden Sector

e−, ν, q, γ, W ±, Z, g...H a, γ, ψMCP... Hidden Sectors can be quite complicated

we certainly don’t know! Hidden Sector

BIG guys Light guys (live in the mountains) (mass is protected by a symmetry)

Goldstone Chiral Bosons fermions

Gauge and more... Bosons

hard to detect; not only as hidden they have suppressed interactions but as hidden, also heavy! light they have no thresholds and they can have maybe at LHC or ILC... coherent forces

Let symmetry be our guide ! Hidden Sectors can be quite complicated

we certainly don’t know! Hidden Sector

BIG guys Light guys (live in the mountains) (mass is protected by a symmetry)

Goldstone Chiral Bosons WISPsfermions (very) weakly interacting sub-eV Particles Gauge and more... Bosons

hard to detect; not only as hidden they have suppressed interactions but as hidden, also heavy! light they have no thresholds and they can have maybe at LHC or ILC... coherent forces

Let symmetry be our guide ! Axion-like-Particles and Axions

1 µν Axions are GB of a color anomalous U(1) Tr Gµν G a 4fa { } The color anomalous term creates a potential with CP conserving minimum Solution to Strong CP which gives the axion a mass m f 10 10GeV 1 m π π 0.6 meV − − . a f f a a Axion-like-particles have electromagnetic anomaly but no color anomaly,

(Mass, if nonzero comes from small U(1) breaking)

SM 1 µν Msn g F F φ φ 4 φγ µν g α/M Hidden Sector φγ ∼ mess Hidden Photons U(1)EM U(1)hidden ×

γ sin χ µν γ Fµν B Bµ 2 Aµ kinetic mixing eg M with photon sin χ = B Q Q Log i 6π2 A B µ i Loop suppression but NO mass small values can come from mass degeneracy of particles suppression, just a log with opposite charges (GUT...)

4, 16 SUSY, String theory ... sin χ = 10− −

K. R. Dienes, C. F. Kolda, and J. March-Russell. Nucl. Phys., B492:104–118, 1997. Hidden Photons in LARGE volume scenarios Goodsell, Jaeckel, Redondo, Ringwald JHEP11, (2009) 027

tiny kinetic mixings can arise from small coupling constants (Hidden U(1)´s from cycles with LARGE volume q ) q/3 V egh 2πg M sin χ g2 s s ∼ 16π2 h ∝ M Vq Pl Small masses also likely

Stueckelberg #1 2 1 2 m − M γ ∝ V s Stueckelberg #2 2 1/3 2 m − M γ ∝ V s Hidden Higgs Hidden Photons in LARGE volume scenarios Goodsell, Jaeckel, Redondo, Ringwald JHEP11, (2009) 027

tiny kinetic mixings can arise from small coupling constants (Hidden U(1)´s from cycles with LARGE volume q ) q/3 V egh 2πg M sin χ g2 s s ∼ 16π2 h ∝ M Vq Pl Small masses also likely

Stueckelberg #1 2 1 2 m − M γ ∝ V s Stueckelberg #2 2 1/3 2 m − M γ ∝ V s Hidden Higgs Impact of WISPs

- Despite the feebleness of their interactions with SM particles, WISPs can have an enormous impact ... in :

- Astrophysics:

* Stellar evolution (they provide additional mechanisms for stellar cooling)

* Gamma ray propagation (Photon oscillations into WISPs)

- Cosmology

* Big Bang Nucleosynthesis

* CMB physics

* Dark Matter Issues (even give `cold’ Dark Matter candidates) Impact of WISPs

- Despite the feebleness of their interactions with SM particles, WISPs can have an enormous impact ... in :

- Astrophysics:

* StellarThe evolution impact can(they be provide usually additional used to put mechanisms very stringent for stellar bounds cooling)

* GammaBUT ray sometimes propagation can (Photonexplain oscillationssome anomalies into WISPs)(and there are some ...)

It might be very difﬁcult to conﬁrm a WISP this way (For that we need laboratory experiments!)

- Cosmology

* Big Bang Nucleosynthesis

* CMB physics

* Dark Matter Issues (even give `cold’ Dark Matter candidates) WISPS and Stars

Stars have a ﬁnite amount of nuclear fuel

The speed at which it is burned (and thus, the stellar evolution) is limited by the effectiveness of the energy drain from the interior

Main energy losses are: - Photons from the surface - Neutrinos from the core

... WISPs ?? WISPS and Stars

Stars have a ﬁnite amount of nuclear fuel

The speed at which it is burned (and thus, the stellar evolution) is limited by the effectiveness of the energy drain from the interior

Standard Physics (+ WISPs) Main energy losses are: (with many details...) And compared with that can be - Photons from the surface observations ... numerically - Neutrinos from the core simulated ... WISPs ?? Globular Clusters (RG & HB)

• WISP cooling affects differently the different star types: DISTORTS the color-magnitude diagram and CHANGES number counts of RGs, HBs... M15 • Numerical simulations agree with observations at the 10% level, that

allows to set strong constraints (1986) (Luminosity)

(1/Temperature)

10 1 gaγγ 10− GeV−

• Globular Clusters (RG & HB)

allows to set strong constraints (1986) (Luminosity)

(1/Temperature)

More observations are now available and much better 10 1 numerical simulations are possible gaγγ 10− GeV− (Project in collaboration with A. Weiss in MPA)

• White Dwarf Luminosity Function

Raffelt (1986), Isern (2008)

Emission of Axions accelerates the cooling at high temperatures and so Textdecreases the number of hot WDs

Probes the axion Isern et al. claim that an axion (or other1 WISP)0 1 electron coupling g = 10− GeV− 2 helps ﬁtting the expectations gaee 11 2 = 2.8 10− m [eV] cos β 4π × a 2 ma cos β = 0, 5, 10 eV Lifetime of the Sun (MS)

Radiological dating of short lived isotopes implies t 5 109years ⊙ ∼ Solar Models are designed to reproduce the currently observed properties (radius and luminosity) at this age but ...

No solar model can be built with

9 1 > gaγγ > 3 10− GeV− Lx Lstd

G. G. Raffelt and D. S. P. Dearborn, Phys. Rev. D36, 2211 (1987). Solar Helioseismology Probes axions

g = 4.5, 10, 15, 20 10 1 10− GeV−

9 1 9 1 Solar models xwith axion> losses stdare consistent gwith sound> proﬁles3 for10 −g < GeV0.5 1 −10− GeV− L L aγγ ∼ × This corresponds to a 0.05 0.2 L ∼ L⊙

Raffelt (1999) Solar Neutrino Flux

Solar models with axion losses predict higher core temperatures and densities, as a result the neutrino ﬂux is enhanced!

B ﬂux (most recent data) 6 1 1 4.94 10 cm− s− 8.8% × ± SM expectations 6 1 1 4.5 4.6 10 cm− s− 16% ∼ × ±

10 1 g 5 10− GeV− × 10 1 g[10− GeV− ] Raffelt (1999,2007) A summary: general ALPS (pseudoscalars coupled to 2 photons)

10!2 ] !3 1 10 − 10!4 10!5

GeV 10!6 Laboratory

0 !7

1 10

− 10!8 CAST Solar Lifetime GBs !9 Helioseismology

[10 10 Solar Neutrino Flux To k i o γ 10!10 γ

g 10!11 !12 10 Axion Models 10!13 10!6 10!5 10!4 10!3 10!2 10!1 1 10 mALP [eV] Hidden Photons

!18 !16 !14 !12 !10 !8 !6 !4 !2 0 2 4 6 8 10 12 0 0 !1 a EW !1 Rydberg e,Μ !2 Jupiter Earth !2 E774 3# !3 Coulomb !3 !4 E141 !4 CMB !5 CAST E137 !5 hCMB ! Solar !6 !6

Χ Lifetime !7 FIRAS !7 10 !8 !8 Log !9 LSW !9 !10 !10 !11 !11 DDM !12 !12 HB !13 !13 !14 !14 !15 !15 !18 !16 !14 !12 !10 !8 !6 !4 !2 0 2 4 6 8 10 12

Log10 mΓ' eV

! " Helioscopes

Typical bounds from the Sun energy loss cannot compete with Globular Cluster limits.

But we can try to observe WISPs from the Sun! Searching for Axion-like-Particles at CERN: CAST

CAST, K. Zioutas et al., Phys. Rev. Lett. 94, 121301 (2005), hep-ex/0411033. Detect Solar ALPs at earth by means of inverse Primakoff conversion in a strong magnetic ﬁeld

X-ray detector Bext

10!2

] !3 CAST Helioscope, LHC decommissioned magnet

1 10

− 10!4 10!5 !6

GeV 10 !7 0 10 1 !8

− 10 CAST 10!9

[10 !10

γ 10

γ 10!11 g 10!12 10!13 10!6 10!5 10!4 10!3 10!2 10!1 1 10

mALP [eV] CAST Helioscope: Hidden Photons JR, JCAP 07(2008)008, Gninenko and JR Phys. Lett. B 664

Detect Solar hidden photons at earth by oscillations inside a closed cavity

γ γ X X X-ray detector γ B irrelevant

Sensitivities for a low energy (eV) HP search !18 !16 !14 !12 !10 !8 !6 !4 !2 0 2 4 6 8 10 12 0 0 with CAST and SuperKamiokande !1 a EW !1 Rydberg e,Μ !2 Jupiter Earth !2 E774 3# 10!5 10!4 10!3 10!2 !3 Coulomb !3 10!4 10!4 !4 E141 !4 CMB !5 CAST E137 !5 hCMB ! Solar !5 !5 !6 !6 10 CASTkeV 10

Χ Lifetime !7 FIRAS !7 LSW 10 Coulomb !8 !8

Log !6 !6 !9 LSW !9 Χ 10 10 !10 !10 CASTeV !11 !11 !7 !7 !12 !12 10 10 HB !13 !13 SuperK !14 !14 10!8 10!8 !15 !15 !5 ! ! ! !18 !16 !14 !12 !10 !8 !6 !4 !2 0 2 4 6 8 10 12 10 10 4 10 3 10 2

mΓ' eV Log10 mΓ' eV

! " ! " Solar Hidden Photons

While my stay at DESY I realized that Hamburg is an ideal place for a solar HP search Solar Hidden Photons at Hamburg: SHIPS (Solar Hidden Photon Search)

A collaboration of the Hamburger Sternwarte and DESY G. Wiedemann, A. Ringwald, JR, et al. X

While my stay at DESY I realized that Hamburg is an ideal place for a solar HP search (unfortunately... ) Photon-WISP oscillations of astronomical or cosmological radiation

Axion-like Particles Hidden Photons

γ a γ γ BT Primordial or galactic magnetic ﬁelds Photons can convert into WISPs while propagating through the universe this produces distortions in the expected spectra and unusual transparency (The conversion Probabilities depend on the photon frequency)

BT Axion-like-particles with very small mass (<< 10^-10 eV) could be responsible of different observed anomalies :

- Anomalous transparency of Gamma Rays (A. De Angelis, O. Mansutti, and M. Roncadelli, Phys. Rev. D76 (2007) 121301) - Scatter in the Luminosity relations of AGNs (C. Burrage, A.-C. Davis, and D. J. Shaw, Phys. Rev. Lett. 102 (2009) 201101) - Correlation of arrival directions between BL-Lacs and HECR in HiRes and AGASA (M. Fairbairn, T. Rashba, and S. Troitsky, arXiv:0901.4085 [astro-ph.HE].) - Polarization of Quasars (A. Payez, J. R. Cudell, and D. Hutsemekers, AIP Conf. Proc. 1038 (2008) 211–219) Photon-WISP oscillations: creation of a Hidden CMB

Axion-like Particles Hidden Photons

a γ γ BT Primordial magnetic ﬁelds

The Hidden WISP background behaves as relativistic degrees of freedom (as standard neutrinos) contributing to the universe expansion Photon oscillations into WISPs are frequency dependent and they leave their imprint on the CMB spectrum

400

300

P 200 FIRAS data 100 (errors 10 5 ) 0 × 0 5 10 15 20 Ω T Both BBN and CMB anisotropies (+LSS data)are sensitive to FIRAS on COBE measured the CMB spectrum with 10^4 accuracy! the number of effective neutrinos -> Bound ! HIDDEN PHOTONS

eﬀ post recombination weak coupling µ ∆Nν 1 1

10!1 10!1

!2 Coulomb !2 10 10

10!3 10!3

Χ eﬀ 10 10!4 FIRAS Nν > 4.8 10!4 Log 95% C.L. N eﬀ =3.8 10!5 ν 10!5 5 !6 µ > 9 10− !6 10 | | × 10

10!7 10!7

10!8 10!8 10!14 10!13 10!12 10!11 10!10 10!9 10!8 10!7 10!6 10!5 10!4 10!3 10!2 10!1

Log10 mΓ' eV

! " AXION-LIKE PARTICLES

The case of Axions and ALPS is more delicate : Photon-ALP oscillations require a primordial (unmeasured but somehow expected) magnetic ﬁeld AXION-LIKE PARTICLES

The case of Axions and ALPS is more delicate : Photon-ALP oscillations require a primordial (unmeasured but somehow expected) magnetic ﬁeld Photon Oscillations in the Lab: Light-Shining through Walls Ehret te al. NIM A 612, and in preparation

“Axion Like Particle Search” or better ``Any-light-particle-search´´

Low LASER Background detector

Laser as intense/controlled source: A pioneer experiment BFRT (BNL) in early 90’s and 2005 boom: ALPS (DESY), BMV (LNCMP), GammeV (FL), LIPPS (jLab), OSQAR (CERN) Photon Oscillations in the Lab: Light-Shining through Walls Ehret te al. NIM A 612, and in preparation

“Axion Like Particle Search” or better ``Any-light-particle-search´´

Low LASER Background detector

Laser as intense/controlled source: A pioneer experiment BFRT (BNL) in early 90’s andPRELIMINARY 2005 boom: ALPS (DESY), BMV (LNCMP), GammeV (FL), LIPPS (jLab), OSQAR (CERN) Conclusions

- WISPs and Hidden Sectors

- Strong Bounds from Astrophysics and Cosmology

- (Also some possible Hints !)

- Laboratory searches are underway (Helioscopes, Light through Walls)

- Many more things to say! THANK YOU!