Ultrasensitive force detection and fundamental physics ...
Transcript of Ultrasensitive force detection and fundamental physics ...
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Ultrasensitive force detection and fundamental physics with optically trapped nanospheres
A. Geraci, Northwestern University
Intersections between Nuclear Physics and Quantum Information, Mar. 29, 2018
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Our lab has moved!
Center for Fundamental Physics (CFP)
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Our lab: fundamental physics with resonant sensors
Mechanical Resonance: Optically levitated nanospheres
Spin Resonance:NMR –Laser polarized gases or liquids
New PhysicsGravity at micron scales
Gravitational Waves
Spin-dependent forces• QCD Axion
Techniques
ARIADNE
A. Arvanitaki and AG., Phys. Rev. Lett. 113, 161801 (2014).
AG., S. Papp, and J. Kitching, Phys. Rev. Lett. 105, 101101 (2010).
A. Arvanitaki and AG., Phys. Rev. Lett. 110, 071105 (2013).
G. Ranjit et.al., Phys. Rev. A 91, 051805(R) (2015).
G. Ranjit, M. Cunningham, K. Casey, and AG, Phys. Rev. A,
93, 053801 (2016).
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The Hierarchy Problem: Why is Gravity so small?
For two protons in nucleus:
Strong : Electromagnetic : Weak : Gravity= 20 : 1 : 10 : 10 -7 -36
The Interactions:Strong: Holds nucleons together
Electromagnetic: Acts between charged particles
Weak: Causes certain decays
Gravity: Attraction between masses
The Standard Model Provides an adequate description of the electromagnetic, weak, and strong interactions.
PP
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Testing gravity at short range
/21 1 r
N er
mmGV
Exotic particles (new physics)
m1
r
m2
< 1 mm
• Supersymmetry/string theory(moduli, radion, dilaton)
• Particles in large extra dimensions(Gravitons, scalars, vectors?)
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Landscape for non-Newtonian corrections
E.G. Adelberger, B.R. Heckel, A.E. Nelson, Ann. Rev. Nucl. Part. Sci. 53 77, (2003)
/21 1 r
N er
mmGV
Laboratory
Lunar laser ranging
Planetary
Terrestrial and
satellites
Adapted from Ann. Rev. Nucl. Part. Sci. 53 77 (2003),
PRL 98, 021101 (2007),PRD 78, 022002 (2008),arXiv:1410.7267 (2014)
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Experimental challenge: scaling of gravitational force
m1m2
42
2
232
~4
)3/4(rG
r
rGF NNN
FN 0.1r4
for ~ 20gr / cm3
r~10 µm ; NFN
2110~
In the range of experimental interest:
r
mmGVN
21 2r
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Small forces• Bathroom scales measure 10-1 N
Virus 10-19 N
Dust mite 10-7 N
Carbon atom 10-25 N
E. coli 10-15 N
70 kg ~ 700 N
• AFM measures 10-11 N
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Experimental challenge: electromagnetic background forces
Casimir effect (1948): Electrostatic Patch Potentials:
J. L. Garrett, D. Somers, J. N. MundayJ. Phys.: Condens. Matter 27 (2015) 214012
z
A
FC (z) 2
240
c
z4A
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Force-distance parameter space
Torsion balance experiments(U Washington)
Cantilevers(Stanford)
Casimir measurements (Indiana) /21 1 r
N er
mmGV
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Resonant force detection• Cantilever is like a spring:
Qk
FA
k
FA
)(
)0(
0
Constant force
Driving force on resonance of cantilever 0
Q can be very large >100,000
Amplitude:
F Kx
0 K
m
Sinusoidal driving force
lt
w
F
A
0
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Fundamental limitation: thermal noise
• Random “kicks” are given to cantilever due to finite T of oscillator
Brownian motion – random “kicks” given to particle due to thermal bath
dust particle
fluid molecule
Tkxk B2
1
2
1 2
Fmin 4kkBTb
Q0
1/ 2
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Q
TbkkF B
0
min
4
Fiber
Lens
Cantilever
Silicon Cantilevers: Fmin ~ 10 x 10-18 N/Hz at 4 K at Q=105
w= 50 µml= 250 µmt=0.3 µmw
Example: Silicon microcantilevers
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Improving sensitivity
CM motion decoupled from environment –no clamping, materials losses
Limitations on Q: Clamping, surface imperfections, internal materials losses
Levitate the force sensor!
)(3
][
21
0sphere
2
41
opt
V
EeU
Fiber
Lens
Cantilever
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Levitated optomechanics• Ashkin, Bell Labs, 1970s
• Ashkin (76) Levitation in high vacuum
• Omori (97)
• Recently proposals/experiments for ground state cooling
r=1.5,2,2.5 µm
Optical tweezers biology, biophysics
D.E. Chang et. al., PNAS (2009)
O. Romero-Isart et.al. New J. Phys. (2010)
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Levitated bead experiments
B. Rodenburg et. al, Optica 3, 318-323 (2016)
J. Gieseler, B. Deutsch, R. Quidant et. al.,PRL 109, 103603 (2012).
N. Kiesel, F. Blaser, U. Delic, D. Grass, R. Kaltenbaek, M. Aspelmeyer, doi: 10.1073/pnas.1309167110
J. Millen, T. Deesuwan, P. Barker, J. Anders. Nature Nanotechnology, 2014; DOI: 10.1038/nnano.2014.82
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Projected force sensitivity
Z. Yin, A. Geraci, T. Li, Int. J. Mod. Phys. B 27,1330018 (2013).
Cantilevers
20 zN/Hz1/2 Gieseler, Novotny, Quidant (Nature Phys. 2013)
Seen recently by Novotny groupV. Jain et. al., PRL 116, 243601 (2016)
Photon recoil heating )1(42/1
min mTkF B
Ions
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Projected sensitivity
AG, S.B. Papp, and J. Kitching, Phys. Rev. Lett. 105, 101101 (2010)
nanosphere, d < /2
gold coated SiN membrane
(stationary)
Drive mass
device (Au/Si)
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Experimental Setup
300 nm silica bead
AG, S.B. Papp, and J. Kitching, Phys. Rev. Lett. 105, 101101 (2010)G. Ranjit et.al., PRA 91, 051805(R) (2015).G. Ranjit et.al. , Phys. Rev. A, 93, 053801 (2016).
feedback beams
300 nm silica bead
Dipole beams
Drive mass actuator
Cavity beams
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Drive Mass fabrication
Buried drive mass technique – eliminates corrugation
during polishing process
removing SiliconSilicon
Gold
Gold
20 µm
20 µm
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MEMS actuator• Device for positioning drive mass
100V DC, 10V AC ~5 um displacement
Drive mass
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Standing wave optical trap
feedback beams
m75
Fz(p
N)
z(µm)
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Trap loading• Acceleration required to
release a nanometer-sized sphere from a substrate
Vdriver
~107 g for R=150nm!
2
1
Ra
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Loading optical trap
Optical dipole trap lasers
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Trapping instabilities
Without feedback cooling particle is lost < 1 Torr
Trap depth > 106 K !
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Trapping instabilities
• Radiometric forces
Crooke’s Radiometer
Trap instabilities arise from uneven heating of the sphere surface
Important when mean free path ~ object size
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Radiometric forces
1% temp gradient across surfaceR=1.5 m, I=2 x 109 W/m2
Heating rate > gas damping rate Particle loss Need feedback!
Ranjit et.al., PRA 91, 051805(R)
(2015).
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3D feedback cooling of a nanosphereNeeded to stabilize the particle, damp and cool itMitigate photon recoil heating
𝑥(𝑡)
𝑣𝑥 𝑡
AOM
780 nmQ
TBkKF B
0
min
4
cool
eff
cool
eff
TT
0
00
0
00
Ranjit et.al., PRA 91, 051805(R) (2015).
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Varying feedback power
High Vacuum -- Can decrease cooling rate by > 1 order of magnitude and maintain stable trap
Gas contributes to loss mechanisms near 100 mTorr - 1 Torr range
Ranjit et.al., PRA 91, 051805(R)
(2015).
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Zeptonewton force sensing
Sensitivity Hz/aN37.63.1, xFS
6 zN
G. Ranjit, et.al. , Phys. Rev. A, 93, 053801 (2016).
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Zeptonewton force sensing
Sensitivity Hz/aN37.63.1, xFS
6 zN
Calibration electrodes
ElectrostaticCalibration
Neutral beads stay neutralCharge stays constant over days
90% of beads are neutral
G. Ranjit, et.al. , Phys. Rev. A, 93, 053801 (2016).
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Zeptonewton force sensing
Sensitivity Hz/aN37.63.1, xFS
6 zN
Optical latticecalibration
Useful for neutral objects
Method consistent with electric field approach
G. Ranjit, et.al. , Phys. Rev. A, 93, 053801 (2016).
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Next: Cavity Trapping and cooling
1596nm beam to trap a bead at its antinode localization1064nm beam to cavity cool the CM of bead position readout
300 nm bead
300 nm sphere
Flat gold mirror
Calibration electrodes
a) b)
100 nm sphere
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Future prospects
• Gravitational waves • Quantum limited sensing
• Applications in nuclear physics?
B. P. Abbott et al. (LIGO Scientific Collaboration and Virgo Collaboration)Phys. Rev. Lett. 116, 061102 (2016).
A.G. and H. Goldman, Phys. Rev. D 92, 062002 (2015).A. Arvanitaki and AG, Phys. Rev. Lett. 110, 071105 (2013)A. Pontin, L.S. Mourounas, AG, and P.F. Barker, New J. Phys. 20 023017 (2018).
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Gravitational Wave Detection
• Laser intensity changed to match trap frequency to GW frequency
• For a 100m cavity, h ~ 10-22 Hz -1/2 at high frequency (100kHz)
• Limited by thermal noise in sensor (not laser shot noise)
(a = 75 um, d = 500 nm disc)
GW Strain h = DL/L
J. Weber (1969)
kHz6.1
Position measurement force measurement
10-100m
A. Arvanitaki and AG, Phys. Rev. Lett. 110, 071105 (2013)A. Pontin, L.S. Mourounas, AG, and P.F. Barker, New J. Phys. 20 023017 (2018)
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Fiber based FP Cavity
LLfree
~ 100 m~ 4 mm
Trapped particle High reflectivity mirroror distributed bragg reflector60 mW 1550 nm
Target finesse ~10
A. Pontin, L.S. Mourounas, AG, and P.F. Barker, arXiv:1706.10227New. J. Phys (2018), accepted
𝜔 = 2𝜋 × 100 𝑘𝐻𝑧
k = 2 x 51 kHz
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Quantum “Mechanics”
Sideband cooling of micromechanical motion to the quantum ground stateJ. D. Teufel,1,et.al. Nature 475, 359 (2011).
Laser cooling of a nanomechanical oscillatorinto its quantum ground stateJasper Chan,1, et.al. Nature 478, 89–92(2011)
This is in its quantumground state!
Quantum ground state and single-phonon control of a mechanical resonator A. D. O’Connell et.al. Nature 464, 697 (2010).
TkB
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Sympathetic cooling of a nanoparticle via cold atoms
G. Ranjit, et.al. Phys. Rev. A 91, 013416 (2015).
F=400 Cavity
Optical molassesOptical dipole trap
1d Optical lattice
Chamber 1 Chamber 2
105 87𝑅𝑏 atoms
trapped in an
optical lattice
170 nm sphere
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Matter-wave interferometry
O. Romero-Isart, A. C. Pflanzer, F. Blaser, R. Kaltenbaek, N. Kiesel, M. Aspelmeyer, J. I. Cirac
Phys. Rev. Lett. 107, 020405 (2011).
Bateman, J., S. Nimmrichter, K. Hornberger, and H. Ulbricht,, Nat. Commun. 5, 4788 (2014).
A.G. and H. Goldman, Phys. Rev. D 92, 062002 (2015).
ng acceleration sensing
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Nuclear physics applications?
• Other uses for zeptonewton force sensing
• Rare decaysM. Dietrich, A.G.
b -decay
∆𝑣 =∆𝑝
𝑚~ 10−4𝑚/𝑠
∆𝑝
1𝑀𝑒𝑉(10−17𝑘𝑔
𝑚)
Detectable above thermal noise for 100 nm particle at 3 mK
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Conclusions• Calibrated zeptonewton force sensing with optically
levitated nanospheresMicron-distance gravity tests Casimir forces in new regimes High frequency gravitational waves Other applications??
• Quantum Regime Source for matter wave interferometry Testing quantum behavior at the macro-scale
S. Bose, A. Mazumdar, G. W. Morley, H. Ulbricht, M. Toroš, M. Paternostro, A.G., P.F. Barker, M. S. Kim, and G. Milburn, Phys. Rev. Lett. 119, 240401 (2017)
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Back row (L to R): Cris Montoya (G), William Eom (UG), Jason Lim (UG), Harry Fosbinder-Elkins (UG), Mindy Harkness (UG), Andrew Geraci (PI)Front row (L to R): Ryan Danenberg (UG), Kathleen Wright (UG), Isabella Rodriguez (UG), Chloe Lohmeyer (G), Ohidul Mojumder (UG), Jordan Dargert (G), ChethnGalla (G), Colin Bradley (UG).
Acknowledgements
PHY-1205994PHY-1506431PHY-15065081510484, 1509176
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GW Strain Sensitivity
Size scale: LIGO100 m
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GW sources at high-frequency• Astrophysical Sources
Natural upper bound on GW frequencyinverse BH size ~ 30 kHz
• Beyond standard model physics- QCD Axion Annihilation to gravitons in
cloud around Black holes
R. Brustein et. al. Phys. Lett. B, 361, 45 (1995)
A. Arvanitaki et. al, PRD, 81, 123530 (2010)
- String cosmology- The unknown?
Black hole superradiance
A. Arvanitaki et al. PRD 83, 044026 (2011)
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Projected reach-nanosphere matter-wave interferometer
A.G. and H. Goldman, Phys. Rev. D 92, 062002 (2015).