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Larmor-resonant Sodium Excitation for Laser Guide Stars Ron Holzlöhner S. Rochester 1 D. Budker 2,1 D. Bonaccini Calia ESO LGS Group 1 Rochester Scientific.

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Presentation on theme: "Larmor-resonant Sodium Excitation for Laser Guide Stars Ron Holzlöhner S. Rochester 1 D. Budker 2,1 D. Bonaccini Calia ESO LGS Group 1 Rochester Scientific."— Presentation transcript:

1 Larmor-resonant Sodium Excitation for Laser Guide Stars Ron Holzlöhner S. Rochester 1 D. Budker 2,1 D. Bonaccini Calia ESO LGS Group 1 Rochester Scientific LLC, 2 Dept. of Physics, UC Berkeley AO4ELT3 Florence, 28 May 2013

2 Slide 2 E-ELT laser baseline: 20W cw with 12% repumping  5 Mph/s/m 2 at Nasmyth (at zenith in median sodium; 12 Mph/s/m 2 on ground) There may be situations when flux is not sufficient for some instruments (low sodium, large zenith angle, non-photometric night, full moon, etc.) No unique definition of LGS availability; details quite complicated E-ELT Project has expressed interest in exploring paths to raise the return flux Two avenues: 1.Raise cw power  Laser development (e.g., Raman fiber amplifiers) 2.Raise coupling efficiency s ce  Explore new laser formats Will focus on option 2 Are E-ELT LGS lasers powerful enough?

3 Sky Maps Paranal Sim. cw return flux on ground [10 6 ph/s/m 2 ] ζ = 60° B 3.6! Becoming more independent of field angle would be particularly beneficial in Paranal:  Flux varies strongly with angle to B-field  B-field inclination is only 21°  most of the time this angle is large

4 Slide 4 Three major impediments of sodium excitation: 1) Larmor precession ( m: angular momentum z-component ) 2) Recoil (radiation pressure)  3) Transition saturation (at 62 W/m 2 in fully pumped sodium) What factors limit the return flux? m B Laser time v spont. emission excited (P 3/2 ) ground (S 1/2 ) + 50 kHz θ

5 Aligned “Peanut” with axis along z  preferred axis. z x y Oriented “Pumpkin” pointing in z-direction  preferred direction. z x y Unpolarized Sphere centered at origin, equal probability in all directions. z x y Visualization of Atomic Polarization Draw 3D surface where distance from origin equals the probability to be found in a stretched state ( m = F ) along this direction. Credit: D. Kimball, D. Budker et al., Physics 208a course at UC Berkeley

6 torque causes polarized atoms to precess:   B  Precession in Magnetic Field Credit: E. Kibblewhite Credit: D. Kimball, D. Budker et al., Physics 208a course at UC Berkeley

7 Slide 7 Efficiency per Atom with Repumping Model narrow-line cw laser, circular polarization ψ : Return flux per atom, normalized by irradiance [unit ph/s/sr/atom/(W/m 2 )] θ: angle of laser to B-field (design laser for θ = π /2) Symbols: Monte Carlo simulation, lines: Bloch Blue curve peaks near 50 W/m 2, close to Na saturation at 60 W/m 2 : Race to beat Larmor Irradiance (W/m 2 ) Is there a way to harness the efficiency at peak of green curve? 20W cw laser in mesosphere Peak efficiency Transition saturation 62 W/m 2

8 Slide 8 Pulse the laser resonantly with Larmor rotation: like stroboscope, Larmor period: 3 – 6.2 μs (Field in Paranal: G at 92km) Used for optical magnetometry: Yields bright resonance in D 2a of about 20% at 0.3…1.0 W/m 2, narrow resonance of ca. 1.5% FWHM * ) Recent proposal by Hillman et al. to pulse at 9% duty cycle, 20W average power, 47/0.09 = 522 W/m 2 and a linewidth of 150 MHz  47/15 ≈ 3 W/m 2 /vel.class  near optimum avg. power Paranal simulation: s ce = 374 ph/s/W/(atoms/m 2 ), vs. ca. s ce ≈ 250 for cw (all at 90° and Paranal conditions) hence about 1.5 times more (!) s ce becomes almost independent of field angle Increased irradiance also broadens the resonance Larmor Resonant Pulsing *) PNAS /pnas (2011) (arXiv: )PNASarXiv:

9 Slide 9 B = 0.23 G, θ = 90°, q = 9%, 150 MHz linewidth Return is fairly linear vs. irradiance Steady state reached after ca. 50 periods = 300μs (S- damping time) Some Simulation Details

10 Slide 10 Can achieve 14 Mph/s/m 2 at 10W, 28 Mph/s/m 2 at 20W (D 2a +D 2b ) Peak efficiency reached above 10W Very strong atomic polarization towards (F=m=2) of 60–70% Simulated Performance F = m = 2 F = m = W/m 2 Ground States Excited States

11 A small rep rate detuning shows up first at low peak irradiance Reduces pumping efficiency, induces polarization oscillations Variation in Paranal: –0.22%/year, –0.39%/10km altitude Larmor Detuning On resonance1% detuned2% detuned I p = 27 W/m 2 I p = 221 W/m 2

12 Slide 12 Lasers with pulses of ~0.5 μs and peak power 200W hard to build (150/2=75 MHz linewidth not large enough to sufficiently mitigate SBS) Multiplex cw laser to avoid wasting beam power?  Spatiotemporally: use one laser to sequentially produce multiple stars  In frequency: Chirp laser continuously, e.g. from – MHz (11 vel.c.)  In frequency: Periodically address several discrete velocity classes  Or modulate the polarization state? (probably less beneficial) Can in principle profit from “snowplowing” by up-chirping, although chirp rate of ~110 MHz/6.2μs = 17.7 MHz/μs is very high Numerical optimization of modulation scheme; runs are time- consuming (order 48–72 CPU h per irradiance step) Issue: Avoid F=1 downpumping, in particular at 60 MHz offset Best Laser Format?

13 Downpumping D2bD2b D2aD2a Graphic by Unger Prefer (F = 2, m = ±2)  (F = 3, m = ±3) cycling transition 3S 1/2  3P 3/2 transition F = I + J : Total angular momentum I = 3/2 : Nuclear spin J = L + S : Total electronic angular momentum (sum of orbital and spin parts) 40 MHz grid Excitation from D2a narrow-band laser

14 Slide 14 Scan across >= 9 discrete velocity classes Blue-shift to achieve “snowplowing” via atomic recoil Avoid downpumping  leave 40 MHz or >> 60 MHz gaps, but… …without exceeding the sodium Doppler curve (1.05 GHz FWHM) Frequency Scanning Schemes 9 × 40 MHz4 × 110 MHz

15 Slide 15 Hyperfine State Populations Time  Excitation  excited states F = 1 ground states F = 2 ground states Larmor period first pulse Plot hyperfine state evolution for a selection of velocity classes Visualize Larmor precession, downpumping, excitation

16 Slide 16 Hyperfine State Analysis: 9 × 40 MHz 60 MHz

17 Slide 17 Larmor precession reduces the return flux efficiency by factor 2; forces high irradiance to combat population mixing Can mitigate population mixing by stroboscopic illumination resonant with Larmor frequency (~160 kHz in Chile, ~330 kHz in continental North America and Europe) Realize with pulsed laser of ~20W average power and < 10% duty cycle, 150 MHz linewidth: Raise efficiency by factor 1.5 ! …which is hard to build (> 200 W peak power, M 2 < 1.1) Alternative: Frequency modulation (chirping/frequency multiplexing schemes) Caveats: Observe 60 MHz downpumping trap and target ~3–5 W/m 2 /v.c. on time average, frequency sensitive, modulator not easy to build Format optimization is work in progress Conclusions CW laser format is good, but leaves room for improvement

18 F I N E GRAZIE! Slide 18

19 Slide 19 Would like to frequency modulate over 100 MHz (or even 300 MHz) at >80% efficiency Either sawtooth or step function with 160 kHz rep rate (Paranal) Need to maintain excellent beam quality and beam pointing Option1: Free-space AOM. Pro: Proven technique, reasonable efficiency. Con: 100+ MHz is very broadband, variation of beam pointing or position when changing frequency? Option 2: Free-space EOM using carrier-suppressed SSB. Requires an interferometric setup, may be difficult to realize at high power+efficiency Option 3: Modulate seed laser. Pro: Possibly reduce SBS (fiber transmission time is in μs range). Con: Cavity locking difficult (piezo bandwidth would need to be in MHz range), combine with PDH sidebands? Frequency Shifters

20 Slide 20 Hyperfine State Analysis: 4 ×110 MHz

21 Slide 21 Some Commercial Frequency Shifters 1 Brimrose Corp.

22 Slide 22 No More Plots…How Do We Build it?

23 Slide 23 Some Commercial Frequency Shifters 2 Brimrose Corp.

24 Slide 24 Some Commercial Frequency Shifters 3 A.A REFERENCE Materi al Wavelength (nm) Aperture(mm²)Frequency(MHz)Polar Deflection angle (mrd) Efficiency MQ200-B30A Br SiO x /- 60 MQ110-B30A1-UVSiO x /- 60 MCQ110-B30A2-VISQuartz x /- 532nm> 70 MT350-B120-A0.12-VIS TeO2-L x /- 60 MT250-B100-A0.5-VISTeO2-L x /- 60 MT250-B100-A0.2-VISTeO2-L x /- 60 MT200-B100A0.5-VISTeO2-L x /- 60 MT200-B100A0.2-VISTeO2-L x /- 60 MT110-B50A1-VISTeO2-L x /- 60 MT110-B50A1.5-VISTeO2-L x /- 60 MT80-B30A1-VISTeO2-L x 280 +/- 65 MT80-B30A1.5-VISTeO2-L x 280 +/- 65

25 Seems that AOM/EOM specs are very challenging (no “eierlegende Wollmilchsau” in AOMs, quote by Mr. Jovanovic, Pegasus Optik GmbH) Really no way to modulate in the IR and double?  Frequency shift is doubled, hence +/– 25 MHz may be enough  Could be done after seed laser with fiber-coupled AOM and thus also shift the PDH sidebands  Would need fast adjustment of optical path length in cavity (RF active crystal? LBO not suitable, but has been done e.g. with MgO:LiNbO 3 ) …or else consider a pulsed laser? Slide 25 To Frequency Shift, or not? Egg-laying wool milk swine: Broadband, highly efficient, high power, no aberrations, constant pointing. And cheap!

26 Slide 26 Schrödinger equation of density matrix, first quantization dρ/dt = Aρ + b = 0 Models ensemble of sodium atoms, 100–300 velocity groups Takes into account all 24 Na states, Doppler broadening, spontaneous and stimulated emission, saturation, collisional relaxation, Larmor precession, recoil, finite linewidth lasers Collisions change velocity and spin (“v-damping,S-damping”) More rigorous and faster than Monte Carlo rate equations Based on AtomicDensityMatrix package, Written in Mathematica v.6+, publicly available [“Optimization of cw sodium laser guide star efficiency”, Astronomy & Astrophysics 520, A20] Bloch Equation Simulation

27 Slide 27 EOMs for Repumping Vendors: New Focus, Qubig Used free-space EOM in “Wendelstein” transportable LGS system Issues with peak power (photodarkening, coatings, cooling) Taken from Affordable way to retrofit pulsed lasers

28 Slide 28 Most Important: Laser power, sodium abundance (seasonal) Circular polarization state ☼ D 2b repumping (power fraction q≈12%, GHz spacing) ☼ (Peak) power per velocity class ☼ Overlap with sodium Doppler curve (but: implicit repumping) ☼ For return flux on ground: zenith angle, atmospheric transmission 2 Somewhat Important: Angle to B-field (θ), strength of B-field |B| (hence geographic location) Atomic collision rates (factor 10 variation across mesosphere) Less Important: Seeing, launched wavefront error, launch aperture (beware: spot size) Sodium profile, spectral shape (for given number of velocity classes) What is crucial for good return flux? Could improve on the crucial parameters (☼)

29 M F = -1M F = 0M F = 1 z F = 1 F ’ = 0 Light linearly polarized along z can create alignment along z-axis. Optical pumping Credit: D. Kimball, D. Budker et al., Physics 208a course at UC Berkeley

30 M F = -1M F = 0M F = 1 z F = 1 F ’ = 0 Light linearly polarized along z can create alignment along z-axis. Medium is now transparent to light with linear polarization along z ! Optical pumping Credit: D. Kimball, D. Budker et al., Physics 208a course at UC Berkeley

31 M F = -1M F = 0M F = 1 z F = 1 F ’ = 0 Light linearly polarized along z can create alignment along z-axis. Medium strongly absorbs light polarized in orthogonal direction! Optical pumping. Credit: D. Kimball, D. Budker et al., Physics 208a course at UC Berkeley

32 Optical pumping process polarizes atoms. Optical pumping is most efficient when laser frequency (  l ) is tuned to atomic resonance frequency (  0 ). Optical pumping

33 Precession in Magnetic Field Interaction of the magnetic dipole moment with a magnetic field causes the angular momentum to precess – just like a gyroscope!   =  dF dt  =   B     g F  B F  B   dF dt   B   ==  L = g F  B B B  , F    


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