Stellar Intensity Interferometric Capabilities of IACT Arrays*

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1 Stellar Intensity Interferometric Capabilities of IACT Arrays* Dave Kieda Nolan Matthews University of Utah Salt Lake City, Utah *for VERITAS and CTA collaborations

2 Photon Bunching & Intensity Interferometry D= Correlation Distance

3 3 SII Imaging Basic Intensity Interferometry λ B I " Measures correlation in intensity fluctuations (not amplitude!). R R. Hanbury Brown, J. Davis and L. R. Allen, MNRAS 137 (1967) 375.

4 4 SII Imaging Basic Intensity Interferometry Some Pains, But Large Gains: B I " λ -Relatively insensitive to atmospheric turbulence ( turbulence ~ khz, sampling ~100 s MHz ). - Km Baselines possible, operate at blue wavelengths ->sub milli-arcsecond resolution -No need to maintain steady optical interference path between focal planes. -> higher order intensity correlations possible Measures correlation in intensity fluctuations (not amplitude!). -Loss of phase information: Phase recovery needed.

5 5 Signal to Noise Ratio (SNR) in Intensity Interferometry Hanbury Brown 1974; Twiss 1969 Light collection area q.e. of detectors Photo-electron Rate Optical Bandwidth Electronic Bandwidth Integration Time Normalized Visibility Example Calculation: p.e./sec (m v = 1.0, A=100 m 2 = 0.3 ) Hz (for 10nm filter) -250 MHz -1 hour observation - dual polarization -Assume unresolved = 1.0 How to Improve? -Multi-Channel Intensity Interferometer: N %& improvement, (Trippe, 2015) -Redundant baselines: N ()* improvement. -Fast optics & correlators (> 1GHz). Spectral Flux Density (ph s -1 m -2 Hz -1 ) SNR = 200 (assuming ideal system, limited to bright sources)

6 2 nd -order time coherence g (2) & Fourier Image plane g (2) (0,0,0) Lab measurement of g (2) (0, 0, t ) of simulated star/thermal light Matthews, Kieda & LeBohec, accepted in J Opt (2017) +, -,. / +, - /+,. / = g(2) (u, v, t ) = 1 + ½g (1) (u, v, t)½ 2 For II: experimental time resolution t ~ 1 nsec blackbody coherence time t % ~ 4 5 ~ 10 psec g (2) (0,0,0) = 1 + ε ~ small non-gaussian fluctuations => Need large photon counts: 10+ m mirrors m g (1) (u, v, t) : first-order coherence =1 for [u, v, t=0] g (4) u, v, 0 = E I l, m e I"JK *LMNO dl dm I l, m describes the image size and brightness distribution (Van Cittert-Zernike Theorem 1934,1938) l I l, m Reconstructed SII laboratory images stellar disk (left) & binary system (right) Matthews, Kieda & LeBohec, accepted in J Opt (2017)

7 Potential SII at Optical Telescope Arrays VERITAS IACT Array VLTI- Paranal Future CTA/pSCT Array 100 m Excellent instruments for SII: -Large photon collection area (~10 m diameter mirrors) -Optically isochronous (< 5 ns) 100 m to km baselines (milli-arcsec resolution) J. Holder and S. LeBohec, Ap. J. 649 (2006) 399 D. Dravins et al., New Astronomy Reviews 56, 5 (2012) km

8 Potential VERITAS SII Augmentation VERITAS Camera 499 PMT pixels Dual polarization SII pixel (replaces 3 Center PMTs)

9 SII Data Quality Monitor GPS Timecode Generator 10 GB Ethernet 10 MHz 1 PPS WR-SWITCH Module Telescope 2 Single Mode Fiber 50m - 2 km (80 km max) Telescope 3 plastic fiber plastic fiber Telescope 4 Telescope N Telescope ft double shielded RG 223

10 SII Data Quality Monitor 10 GB Ethernet GPS Timecode Generator 10 MHz 1 PPS WR-SWITCH Module Typical SII Augmentation Standalone telescope connected only by fiber optic (White Rabbit, 10G) Telescope 2 Single Mode Fiber 50m - 2 km (80 km max) Telescope 3 plastic fiber plastic fiber Telescope 4 Replace with Custom board in camera? Telescope ft double shielded RG 223 Telescope N

11 Simple VERITAS interferometer simulation Simulated baselines Fourier image Plane sampling (vertical) 100 μ arcsec S. Lebohec et al *`ghost images caused by incomplete sampling of Fourier plane *reflection symmetry of ghost images caused by loss of phase information

12 1-2 km baselines telescopes

13 Simulated Fourier image Planes Reconstructed Binary images Input Binary images Simulated observations of binary stars with different sizes. (m V = 3; T eff = 7000 K; T = 10 h; Dt = 1 ns; l = 500 nm; Dl = 1 nm; QE = 70%) Already changes in stellar radii by only a few micro-arcseconds are well resolved. Better sampling of Fourier image plane-> no ghost images D.Dravins, S.LeBohec, H.Jensen, P.D.Nuñez:, CTA Consortium Optical intensity interferometry with the Cherenkov Telescope Array, Astropart. Phys. 43, 331 (2013)

14 f = 5.6 m, D= 9.6 m, FOV= 8 Pixel = 6 mm ( 11,328 SiPMs) PSFD68= ~ (pix= 0.06 ) CTA-US Schwarzschild-Couder Telescope Prototype is Currently under construction at VERITAS Observatory (Fall 2017 commission)

15 Schwarzschild-Couder two-mirror IACT telescope Wide field of view, excellent spot size RMS spread in arrival time of rays at focal plane as a function of field angle.. On-axis: photon timespread <0.2 nsec rms >>improved g (2) (t) >>reduced observation time 2-4Ghz sampling + SiPM (QE-0.9). SNR = 200 -> SNR =2400! V. Vassiliev, S. Fegan, P. Brousseau: Wide field aplanatic two-mirror telescopes for ground-based g-ray astronomy Astropart.Phys. 28, 10 (2007)

16 IACT Observatories are Excellent Instruments for SII Imaging Digitizing electronics/white Rabbit synchronization Standalone telescopes connected by inexpensive fiber optics km baseline separations now achievable Offline (post-observation) photon correlations Polarization data allows higher S/N, baseline noise estimation Demonstrated correlation using of pipelined FPGA for near real-time processing Higher order correlations may contain additional image information (Ofir & Ribak 2006) Near Term Implementation VERITAS Telescopes (Potential deployment/use in ) m baselines: 100 μ arcsec imaging possible Longer Term Development VLTI visible light feed /single board implementation? CTA/SCT-telescope array implementation : 1-2 km baselines, <100 μ arcsec imaging?

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