any light particle search (alps) ii at desy - coupling 5t ... · any light particle search (alps)...

Any light particle search (ALPS) II at DESY.Coupling 5T HERA dipoles with high-power 1064nm CW for physicsbeyond the Standard Model

Babette DöbrichLULI, LaB workshopEcole Polytechnique, Palaiseau, December 3rd2013

high-Power Laser with B-field vs ALPS-II

HI, e.g. pulsed ↓

↓ Standard Model

↓ Detect!

CW ↑ex-LIGO35W

↑ BLOCK Standard Model(except neutrino)

↑ Beyond Standard ModelWeakly Interacting Slim Particles (WISPs) could traverse barrier.ALPS-II is the second ‘light-shining-through-a-wall’ setup at DESY

↑ Detect?

maybe!

Babette Döbrich | LULI, LaB workshop | December 3rd 2013 |

high-Power Laser with B-field vs ALPS-II

HI, e.g. pulsed ↓

↓ Standard Model

↓ Detect!

CW ↑ex-LIGO35W

↑ BLOCK Standard Model(except neutrino)

↑ Beyond Standard ModelWeakly Interacting Slim Particles (WISPs) could traverse barrier.ALPS-II is the second ‘light-shining-through-a-wall’ setup at DESY

↑ Detect?maybe!

Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 2

What we look for, I: Axion-like particles (ALPs)

QCD Axion

ALPs from intermed. string scales

ALPs as cold dark matter

TeV transparency

HB stars

SN Γ-burst

WD cooling

10-10 10-8 10-6 10-4 0.01 1

1. ´ 10-15

1. ´ 10-14

1. ´ 10-13

1. ´ 10-12

1. ´ 10-11

1. ´ 10-10

1. ´ 10-9

1. ´ 10-8

1. ´ 10-7

m@eV D

g aΓ

@GeV

-1 D

> Lint,PS ∼ gφFµνF̃µν massivepseudoscalars: laser in B-field

> QCD Axion, is a hard nut to crack> (m, g)-plane: axion-like particles

> astrophysics indic.: TeV γs[1302.1208] + White Dwarf coolinghint [1204.3565]

> moduli stab. in intermediatestring scale scenarios [1209.2299]

> Dark Matter candidate [1201.5902]

> QCD Axion in exp only tackeledby ADMX, CAST; ALPS-I (2010)model-independent ALPs

> ALPS-IIc “as far as possible!”(explain “c” later!)



ALPS-I

SN Γ-burst

CAST

QCD Axion



TeV transparency

WD cooling

10-10 10-8 10-6 10-4 0.01 1

1. ´ 10-15

1. ´ 10-14

1. ´ 10-13

1. ´ 10-12

1. ´ 10-11

1. ´ 10-10

1. ´ 10-9

1. ´ 10-8

1. ´ 10-7

m @eVD

g aΓ

@GeV

-1 D










ALPS-I

SN Γ-burst

CAST

ALPS-IIc

QCD Axion



TeV transparency

WD cooling

10-10 10-8 10-6 10-4 0.01 1

1. ´ 10-15

1. ´ 10-14

1. ´ 10-13

1. ´ 10-12

1. ´ 10-11

1. ´ 10-10

1. ´ 10-9

1. ´ 10-8

1. ´ 10-7

m @eVD

g aΓ

@GeV

-1 D









What we look for, part II: hidden photons & more

Coulomb

CMBCAST

ALPS-I vacuum H 2010L

ALPS-IIa gas

HPs from intermediate string scales

DNΝeff=1.9

DNΝeff=0.8

DNΝeff=0.08

DNΝeff=0.01

Longitudinal

ALPS-IIa vacuum

ALPS-IIb gas

ALPS-IIb vacuum HP cold Dark Matter

5´10-51´10-4 5´10-40.001 0.005 0.010

10-9

10-8

10-7

10-6

m Γ '@eVD

Χ

> L ∼ χFµνXµν + m2γ̃

2 XµXµ

→ extra U(1),experimentally no need forB-fields, oscillation process

> HPs e.g. from intermediatestring scale scenarios[1206.0819], Dark Mattercandidate [1201.5902]

> ALPS-I, ALPS-IIa, ALPS-IIb> if B-field applied, also

sensitive to minichargedparticles (fractionallycharged hidden matter)Lint ∼ eψ̄ /Aψ + ehh̄ /Xh

> more info: [1311.0029]Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 4

ALPS-I (2010) and upgrades towards ALPS-II

laserhut L

hera magnet

walldetector

Phys. Lett. B 689, 149 (2010)

Any LightParticle Search I

Any LightParticle Search II

Fabry Perot ↗resonatorbefore “wall”

9m, 5THERAdipole

↖ Resonatorafter “wall”

Upgrades from ALPS-I to ALPS-II

x x

B−field

1) more photons → enhancedprobability

2) better single photondetection

3) More (magnetic) length

1) coupled cavities → resonantregeneration (photonself-interference)

2) Transition Edge Sensor -superconducting edge

3) more HERA dipoles (20)!enhance length → tunnel



Phys. Lett. B 689, 149 (2010)

Any LightParticle Search I

Any LightParticle Search II


9m, 5THERAdipole



x x

B−field









Phys. Lett. B 689, 149 (2010)

Any LightParticle Search IAny LightParticle Search II


9m, 5THERAdipole










Plans & Status for Optics, Detector, Magnets

↑ not to scale ↓

> three stages ALPS-II a,b,c(only c has magnets!)

> Optics: high-finesse cavity1064nm across 10m

> Optics: locking principle withinfrared & green working at 1mtestsetup

> Detector: transition edge sensor(superconductor at Tcrit) in ADR(first background [1309.5024])

> Magnets: ‘magnet straightening’(with spare magnets!) working justfine


Plans & Status for Optics, Detector, Magnets

↑ not to scale ↓

Dipol in Hall 55; ex-ALPS I Dipol Quench current [A]unchanged dipole August 2011 5920September 2012 straightened dipole 6072 6056

Current for 5.3 T: 5690A ( base line ALPS II)

25.9.2012

> three stages ALPS-II a,b,c(only c has magnets!)

> Optics: high-finesse cavity1064nm across 10m

> Optics: locking principle withinfrared & green working at 1mtestsetup

> Detector: transition edge sensor(superconductor at Tcrit) in ADR(first background [1309.5024])

> Magnets: ‘magnet straightening’(with spare magnets!) working justfine


Why straightening? Aperture constraints

> PBPC = 5000 for IR,PBRC = 40000 for IR

> pipe aperture limits PB dueto clipping

> large aperture for ALPS-IIaand b (HERA straight)

> ALPS-IIc → effectiveaperture 35mm limits to4+4 dipoles (not enough) atproposed PB but “true”aperture larger (55mm)

> reestablish “true aperture”with pressure props


More: TDR arXiv:1302.5647, arXiv:1309.3965

ALAR

BD

RS RB

BW

RH JDE

DTAKJEvS > THANKS!> Optics: Benno Willke Robin Bähre,

Reza Hodajerdi, Samvel Ghazaryan

> Magnet: Dieter Trines + team

> Detector: Dieter Horns, Friederike

Januschek, Jan Dreyling-Eschweiler,

Jan-Eike von Seggern, Matthias

Schott, Noemie Bastidon

> Safety/Eng.: Richard Stromhagen

> Howto: Ernst-Axel Knabbe

> Science case & miscellanea: Axel

Lindner, Andreas Ringwald, Babette

Döbrich


More?

Bonus material


Comprehensive ALP exclusion plot

whole story see e.g. [arXiv:1311.0029]

SN1987a

SN Γ-burst

ThermalDM

non-Thermal DM

WD cooling hint BBN

EBLX-Rays

Telescopes

CMB

xion

HBHelioscopes

Solar Ν

KSVZaxion

e++e--> Γ+inv.

Beam

DumpLSW

Haloscopes

Vacuum

Birefringence

REAPR, ALPS-II IAXO

ADMX-HF

ADMX

Yale

Transparency hint

-14 -12 -10 -8 -6 -4 -2 0 2 4 6 8 10

-18

-16

-14

-12

-10

-8

-6

-4

-2

Log10 mALP @eVD

Log10g@G

eV-1D

colored regions:> Dark green =

experiments> blue:

astrophysical/cosmological

> gray:astronomical

> light green:planned exp.

> red: favoredparameterregions


Comprehensive HP exclusion plot

whole story see e.g. [arXiv:1311.0029]

Sun

mwLSW

CoulombRydberg

Jupiter Earth

CMB

HB

DPB

LSW

Cosm

ology

Thermal

DM

Dark Radiation

non-Thermal DM

Haloscopes

TSHIPSI

ALPS-II

Yale

UWAADMX

CERN

Helioscope

Stückelberg

anisotropic

Non-zero FI-term

Hidden Higgs HmHh»mý 'L

Stückelber

g isotropic

HlineL

-15 -12 -9 -6 -3 0 3 6

-15

-12

-9

-6

-3

0

-15

-12

-9

-6

-3

0

Log10mA'@eVD

Log10Ε

colored regions:> Dark green

=experiments

> blue: astro-physical/cosmologi-cal

> gray: astro-nomical

> light green:plannedexp.

> red:favoredparameterregions


Detector requirements and TES working principle

↑

pic ad.: Miller Appl.Phys.Lett. 83/4

> Experimental needs> low rates of single infrared

photons (<1/h)> high quantum efficiency

(PIXIS: 1.2%)> low background

> TES working principle

> TES = superconductingabsorber at transition T

> fiber → guide light there> Photon absorption →

current change → pick upby SQUID

> TES from NIST (andAIST) coated e.g.Tungsten (∼ 100mK) orTi/Au (∼ 200mK)



↑

pic ad.: Miller Appl.Phys.Lett. 83/4 > Experimental needs> low rates of single infrared



> TES working principle> TES = superconducting

absorber at transition T> fiber → guide light there> Photon absorption →





↑

pic ad.: Miller Appl.Phys.Lett. 83/4

> Experimental needs> low rates of single infrared



> TES working principle> TES = superconducting

absorber at transition T> fiber → guide light there> Photon absorption →




Milli-Kelvin environment

↓ control rack

↓ cryostat↓ leak detector

> ‘Entropy’ mKenvironment> dry (helium

confined) &compact (onlywater &electricity)

> time at <100mk:48h

> recharge time 1h

> working principle

> 4K pulse-tubestage

> isothermalmagnetization,adiabaticdemagnetization



↓ control rack


10-2 10-1 100 101

temperature T [K]

0.0

0.5

1.0

1.5

2.0

entr

opy S [J

K−1]

0.1T

0.2T

0.5T

1T 2T 5T

isot

herm

al m

agne

tizat

ion

adiabatic demagnetization

warm

-up

recharge cycle

Bmin = 0 TBmax = 6 T




> recharge time 1h> working principle





↓ control rack





> recharge time 1h> working principle




WISP searches with HI-lasers? (personal view!)

x x

DipolmagnetHochint.−Laser

Dipolmagnet

t t1 2

Hochint.−Laser

ωω

ωax

ω inω out

> dipole magnet O(10T ) vs HI laserO(106T ) (over short l and t)

> some established concepts (e.g.LSW) fail: short pulse length, noeasy cavity enhancement

> beyond CW → differentobservables accessible (e.g.WISP-mediated higher harmonics[1006.5579], polariz. [1306.6456])

> higher ω → higher mass, m . ω

> also e.g. KK gravitons maybeaccessible [1203.6366]

> ...difficult, but worth checking what could be done beyond SM


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