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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 | Page 2
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!)
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 3
What we look for, I: Axion-like particles (ALPs)
ALPS-I
SN Γ-burst
CAST
QCD Axion
ALPs from intermed. string scales
ALPs as cold dark matter
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
> 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!)
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 3
What we look for, I: Axion-like particles (ALPs)
ALPS-I
SN Γ-burst
CAST
ALPS-IIc
QCD Axion
ALPs from intermed. string scales
ALPs as cold dark matter
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
> 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!)
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 3
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 5
ALPS-I (2010) and upgrades towards ALPS-II
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 5
ALPS-I (2010) and upgrades towards ALPS-II
Phys. Lett. B 689, 149 (2010)
Any LightParticle Search IAny LightParticle Search II
Fabry Perot ↗resonatorbefore “wall”
9m, 5THERAdipole
↖ Resonatorafter “wall”
Upgrades from ALPS-I to ALPS-II
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 5
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 6
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 6
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 6
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 6
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 6
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 7
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 7
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 8
More?
Bonus material
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 9
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 10
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 11
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)
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 12
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 = superconducting
absorber 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)
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 12
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 = superconducting
absorber 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)
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 12
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 13
Milli-Kelvin environment
↓ control rack
↓ cryostat↓ leak detector
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
> ‘Entropy’ mKenvironment> dry (helium
confined) &compact (onlywater &electricity)
> time at <100mk:48h
> recharge time 1h> working principle
> 4K pulse-tubestage
> isothermalmagnetization,adiabaticdemagnetization
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 13
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 13
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
Babette Döbrich | LULI, LaB workshop | December 3rd 2013 | Page 14