A. Geraci, University of Nevada, Reno

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The Axion Resonant InterAction Detection

Geraci, University of Nevada, Reno Tabletop

Mark Cunningham (UNR) Mindy Harkness (UNR)

(Stanford) Eli Levenson-Falk (Stanford) Sam

(IU) Mike Snow (IU) Erick Smith (IU) Justin

1 The Axion Resonant InterAction Detection Experiment (ARIADNE) A. Geraci, University of Nevada, Reno Tabletop experiments with skyscraper reach Aug 9, 2017 Mark Cunningham (UNR) Mindy Harkness (UNR) Jordan Dargert (UNR) Chloe Lohmeyer (UNR) Harry Fosbinder-Elkins (UNR) Asimina Arvanitaki (Perimeter) Aharon Kapitulnik (Stanford) Eli Levenson-Falk (Stanford) Sam Mumford (Stanford) Josh Long (IU) Chen-Yu Liu (IU) Mike Snow (IU) Erick Smith (IU) Justin Shortino (IU) Inbum Lee (IU) Evan Weisman (IU) Yannis Semertzidis (CAPP) Yun Shin (CAPP) Yong-Ho Lee (KRISS)

Our lab: Fundamental physics with Techniques Mechanical Resonance:

micron scales AG., S. Papp, and J. Kitching, Phys. Rev. Lett.

G. Ranjit, M. Cunningham, K. Casey, and AG, Phys. Rev.

Spin Resonance: NMR Laser polarized gases or liquids ARIADNE

2 Our lab: Fundamental physics with Techniques Mechanical Resonance: Optically levitated nanospheres resonant sensors New Physics Gravity at micron scales AG., S. Papp, and J. Kitching, Phys. Rev. Lett. 105, (2010). G. Ranjit et.al., Phys. Rev. A 91, (R) (2015). G. Ranjit, M. Cunningham, K. Casey, and AG, Phys. Rev. A, 93, (2016). Spin Resonance: NMR Laser polarized gases or liquids ARIADNE Gravitational Waves A. Arvanitaki and AG., Phys. Rev. Lett. 110, (2013). Spin-dependent forces QCD Axion A. Arvanitaki and AG., Phys. Rev. Lett. 113, (2014).

3 Axions Light pseudoscalar particles in many theories Beyond Standard model Peccei-Quinn Axion (QCD) solves strong CP problem θ <10 10 QCD Dark matter candidate Experiments: e.g. ADMX, CAST, LC circuit, Casper R. D. Peccei and H. R. Quinn, Phys. Rev. Lett. 38, 1440 (1977); S. Weinberg, Phys. Rev. Lett. 40, 223 (1978); F. Wilczek, Phys. Rev. Lett. 40, 279 (1978). J. E. Moody and F. Wilczek, Phys. Rev. D 30, 130 (1984).

4 Axion couplings Coupling to electromagnetic field ADMX, DM Radio, LC Circuit (DM) CAST, IAXO (solar) ALPS, ALPS-II (light thru walls) Coupling to gluon field e.g. CASPEr-electric (DM) Coupling to fermions e.g.casper-wind, QUAX (DM)

5 Axion Parameter space CASPEr DM Radio LC Circuit ABRA- CADABRA ARIADNE Orpheus Adapted from Graham, arxiv:

6 QCD Axion parameter space DM Radio LC Circuit ABRACADABRA ARIADNE Orpheus Adapted from

7 Axion and ALP searches Source Coupling Dark Matter (Cosmic) axions Solar axions Photons ADMX, ADMX-HF DM Radio, ABRA- CADABRA, LC Circuit, Orpheus CAST IAXO Nucleons CASPEr-Electric CASPEr-Wind Lab-produced axions Light-shining-thruwalls (ALPS, ALPS-II) ARIADNE

Axions Light pseudoscalar particles in many theories Beyond Standard model Peccei-Quinn Axion (QCD) solves strong CP problem θ <10 10 QCD Dark matter candidate Experiments: e.g. ADMX, CAST, LC circuit, Casper Also mediates spin-dependent forces between matter objects at short range (down to 30 µm) Can be sourced locally R.

8 Axions Light pseudoscalar particles in many theories Beyond Standard model Peccei-Quinn Axion (QCD) solves strong CP problem θ <10 10 QCD Dark matter candidate Experiments: e.g. ADMX, CAST, LC circuit, Casper Also mediates spin-dependent forces between matter objects at short range (down to 30 µm) Can be sourced locally R. D. Peccei and H. R. Quinn, Phys. Rev. Lett. 38, 1440 (1977); S. Weinberg, Phys. Rev. Lett. 40, 223 (1978); F. Wilczek, Phys. Rev. Lett. 40, 279 (1978). J. E. Moody and F. Wilczek, Phys. Rev. D 30, 130 (1984).

9 Axion-exchange between nucleons Scalar coupling θ QCD Pseudoscalar coupling Axion acts a force mediator between nucleons N N ( g N s ) 2 g N s g N P ( g N p ) 2 Monopole-monopole Monopole-dipole dipole-dipole

10 Spin-dependent forces Monopole-Dipole axion exchange ˆ) ˆ ( ) ( / 2 2 r e r r m g g r U a r a f N p N s + = σ λ π λ m f σ r B eff µ Different than ordinary B field Does not couple to angular momentum Unaffected by magnetic shielding Fictitious magnetic field

11 Using NMR for detection m f r σ Spin ½ 3 He Nucleus B eff U = µ B ext Bloch Equations dm dt = γm B 2 B ω = µ N ext Spin precesses at nuclear spin Larmor frequency Axion B eff modifies measured Larmor frequency ω = γb

Constraints on spin dependent forces G. Raffelt, Phys. Rev. D 86, 015001 (2012). Magnetometry experiments G. Vasilakis, et. al, Phys. Rev. Lett. 103, 261801 (2009). K. Tullney,et. al. Phys. Rev. Lett. 111, 100801 (2013) P.

12 Constraints on spin dependent forces G. Raffelt, Phys. Rev. D 86, (2012). Magnetometry experiments G. Vasilakis, et. al, Phys. Rev. Lett. 103, (2009). K. Tullney,et. al. Phys. Rev. Lett. 111, (2013) P.-H. Chu,et. al., Phys. Rev. D 87, (R) (2013). M. Bulatowicz,et. al., Phys. Rev. Lett. 111, (2013). nedm bound θ QCD <10 10 Standard Model lower bound 16 θ >10 QCD

ARIADNE: uses resonant enhancement Spin ½ 3 He Nucleus Oscillate the mass at Larmor frequency B ext B eff = B cos( ωt) B eff U = µ B ext Bloch Equations dm dt = γm B 2 B ω

13 ARIADNE: uses resonant enhancement Spin ½ 3 He Nucleus Oscillate the mass at Larmor frequency B ext B eff = B cos( ωt) B eff U = µ B ext Bloch Equations dm dt = γm B 2 B ω = µ N ext Time varying Axion B eff drives spin precession produces transverse magnetization Amplitude is resonantly enhanced by Q factor ~ ωt 2. Can be detected with a SQUID

14 Concept for ARIADNE Unpolarized (tungsten) segmented cylinder sources B eff Applied Bias field B ext 2 B ω = µ N ext Laser Polarized 3 He gas senses B eff (Indiana U) squid pickup loop Y.-H. Lee (KRISS) Limit: Transverse spin projection noise Superconducting shielding (Stanford) A. Arvanitaki and A. Geraci, Phys. Rev. Lett. 113, (2014).

Hyperpolarized 3 He Ordinary magnetic fields cannot be used to reach near unity polarization exp[ µ N B / k B T ] Optical pumping techniques Indiana U.

15 Hyperpolarized 3 He Ordinary magnetic fields cannot be used to reach near unity polarization exp[ µ N B / k B T ] Optical pumping techniques Indiana U. MEOP apparatus Metastability exchange optical pumping M Batz, P-J Nacher and G Tastevin, Journal of Physics: Conference Series 294 (2011) Rev. Sci. Instrum. 76, (2005)

16 Experimental parameters Rotational stage 3 sample chambers source mass 4 mm 11 segments 100 Hz nuclear spin precession frequency 2 x / cc 3 He density 10 mm x 3 mm x 150 µm volume Separation 200 µm Tungsten source mass (high nucleon density)

17 Sensitivity θ QCD >10 16 θ QCD <10 10 A. Arvanitaki and AG., Phys. Rev. Lett. 113, (2014).

18 Complementarity with nedm experiments Improved nedm measurement reduces thickness of this axion band, Discovery turns it into a line. Still need to measure the mass! θ QCD >10 16 θ QCD <10 10 A. Arvanitaki and AG., Phys. Rev. Lett. 113, (2014).

19 Experimental challenges Magnetic gradients Nonlinearities Barnett Effect Trapped magnetic flux Vibration isolation Magnetic noise from thermal currents Design/Simulation Work: Magnetic gradient reduction strategy Experimental testing in progress: Vibration tests, Shielding factor f test thin-film SC

20 Superconducting Magnetic Shielding Essential to avoid Johnson noise Meissner Effect No magnetic flux across superconducting boundary Method of Images Make image currents mirrored across the superconducting boundary T > T Dipole with image 20 c T < T c

21 The Problem of Unwanted Images mm ARIADNE uses magnetized spheroid Constant interior field 3He 3He 3He BB BB iiii = const. BB iiii mm ii Magnetic shielding introduces image spheroid Interior field varies mm mm 3He BB iiii const. BB iiii mm ii variations in nuclear Larmor frequency 3He 3He BB But want to drive entire sample on resonance 21

22 Flattening Solution 1 coil simple configuration Expected field from spheroid ~1 μt I on the A range Spheroid 1 coil (circular) Symmetry 22

23 Gradient Cancellation No cancellation Gradient cancellation 98 times flatter I = 1.6 A s Frac = 0.17% Sample area enabling T 2 of ~100 s 23

Tuning Solution D Coils Tune field with Helmholtz coils Helmholtz field only flat near the center Geometry restrictions prevent the spheroid from being centered in traditional Helmholtz

24 Tuning Solution D Coils Tune field with Helmholtz coils Helmholtz field only flat near the center Geometry restrictions prevent the spheroid from being centered in traditional Helmholtz coils D coils look like Helmholtz coils when their images are included I Spheroid D coils Inner straight-line currents cancel Outer currents do not One D coil and image (bird s eye view) 24

25 Quartz block assembly Spheriodal pocket Milled spheriodal pocket in quartz 5 um steps Fabrication/polishing tests is process Aug 2017

26 Tungsten Source Mass Prototype 11 segments, 3.8 cm diameter Tungsten Sprocket prototype, Wire EDM Magnetic impurity testing in machined Tungsten using commercial SQUID magnetometer -- Indiana Magnetic impurities below 0.4 ppm

27 Rotary stage vibration and tilt Rotary test chamber Build an interferometer to measure the change in distance (d). We can find theta (Ө) from: Ө= cos -1 ((L-d)/L) Interferometers We can solve for the wobble distance (X) by: X= Lsin(Ө)

28 Fiber-coupled laser interferometers Laser Source 90:10 fiber coupler Reference Photodiode Signal Photodiode Fiber Tip Reflector PZT Fringe visibility ~0.13 Sensitivity ~160 nm/v Shot noise limit ~20 pm/hz 1/2

Speed stability test - direct drive stage Optical encoder Current feedback control VelCmd (THETA) (deg/msec) Stage speed stability error unloaded, in air 3.5 3.0 2.5 2.0 1.5 1.0 0.

29 Speed stability test - direct drive stage Optical encoder Current feedback control VelCmd (THETA) (deg/msec) Stage speed stability error unloaded, in air VelCmd (THETA) (deg/msec) VelFbk (THETA) (deg/msec) VelErr (THETA) (deg/msec) VelErr (THETA) (deg/msec) Time (sec) Rotation speed control 8.3 Hz ~ 1 part in RMS ~ 1 part in 3000 Allows utilization of T2 > 100s Phase Amplitude E-3 1E-4 1E-5 1E-6 1E-7 1E-8 1E-9 1E-10 1E Frequency Frequency

SQUID Magnetometers 1 cm Y.H. Lee, KRISS 1000 Field noise (ft rms / Hz) 100 10 1 0.

30 SQUID Magnetometers 1 cm Y.H. Lee, KRISS 1000 Field noise (ft rms / Hz) Frequency (Hz) 4.5 ft rms / Hz Measured inside a magnetically shielded room (without Nb tube)

Lee, KRISS, Yun Shin (CAPP) Eli Levenson-Falk (Stanford) Nb tube: 23 mm ID 1 mm thick Length

31 Preliminary test of superconductive shielding L-He dewar Y.H. Lee, KRISS, Yun Shin (CAPP) Eli Levenson-Falk (Stanford) Nb tube: 23 mm ID 1 mm thick Length 200 mm Field coil Applied field: μt pp range (at 8 Hz) SQUID magnetometer: Near the center of Nb tube Shielding factor: (0.5-3) x10 9 for transverse field Goal: 10 8 with thin film Nb SC shield tests underway Summer 2017

32 Summary ARIADNE New resonant NMR method Gap in experimental QCD axion searches 0.1 mev < m a < 10 mev Complementary to cavity-type (e.g. ADMX) experiments No need to scan mass, indep. of local DM density Complementary to nedm experiments Next tests shielding (Stanford/Korea), vibration (UNR), 3 He system (Indiana)

Acknowledgements Thank you PHY-1205994 PHY-1506431 PHY-1509176 1510484, 1509176 Jordan Dargert (G) Andrew Geraci (PI) Mindy Harkness (UG) Jason Lim (UG) Ryan Danenberg (UG) Mark Cunningham (G) Jacob

33 Acknowledgements Thank you PHY PHY PHY , Jordan Dargert (G) Andrew Geraci (PI) Mindy Harkness (UG) Jason Lim (UG) Ryan Danenberg (UG) Mark Cunningham (G) Jacob Fausett (UG) Cris Montoya (G) Chethn Galla (G) Chloe Lohmeyer( UG) Kirsten Casey (UG) Bella Rodriguez( UG) Gambhir Ranjit (PD) Not pictured: Apryl Witherspoon (UG), Ohidul Mojumder (UG), Hannah Mason (UG)

shielding requirements more stringent Nuclear spin

34 Dipole-Dipole axion forces Spin-polarized source mass May be competitive with astrophysical bounds Magnetic shielding requirements more stringent Nuclear spin Electron spin A. Arvanitaki and AG., Phys. Rev. Lett. 113, (2014).

Small Scale experiments for fundamental physics

Small Scale experiments for fundamental physics ICTP Summer School on Particle Physics, June 12-15 Part 4 A. Geraci, University of Nevada, Reno Syllabus Introduction New (scalar) forces Gravitational Waves