The Nulling Coronagraph Using a Nulling Interferometer for Planet Detection in Visible Light with a Single Aperture Telescope

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1 Terrestrial Planet Finder The Nulling Coronagraph Using a Nulling Interferometer for Planet Detection in Visible Light with a Single Aperture Telescope Michael Shao, B. Martin Levine, Duncan Liu, J. Kent Wallace, and Benjamin Lane Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA Presented at the Workshop on Innovative Designs for the Next Large Aperture UV/Optical Telescope (NHST), 10 April 2003 (Acknowledgements: E. Serabyn, B. Mennesson, T. Velusamy, and S. Shaklan)

2 TPF Problem Terrestrial Planet Finder Detection of planets around closest 150 stars and characterization (spectroscopy) for signs of life ~50-120mas IWD angular separation ~m v =5 (F, K,G-type Star) brightness TPF Biomarker Report: 0.7 to 1.0 µm (minimum) 0.5 to 1.1 µm (preferred) 0.75 µm unique Oxygen band not found in the IR starlight suppression required Diffraction control requirement Scattered light control requirement 10-10

3 General Overview Terrestrial Planet Finder Why another coronagraph concept? Nulling interferometer/coronagraph belongs in a class of small inner working distance devices Use 4~5m telescopes instead of 8~10 m telescopes for the TPF mission. If a 4m telescope is $XX dollars, and if the cost of a telescope goes as D 2.5 the cost of a 8m telescope is very (very) high. Orders of magnitude easier to control scattered light, at per airy spot Description of the basic concept 4 beam nulling interferometer Single Mode Fiber Array Experimental demonstrations Deep and Stable Nulling for starlight suppression Fiber Array Progress

4 Terrestrial Planet Finder Large Apertures are NOT Needed in Principle to Detect and Characterize Extra-solar Planets A modest sized aperture telescope can theoretically resolve an extra-solar planet Jupiters at 10 pc D > 0.3m (λ=0.75mm) Earths at 10 pc D > 1.5 m The HST (at 2.4m diameter) is capable of imaging m v =30 stars The major issue is overcoming the contrast between star and planet ( )

5 Nulling Introduction λ /b Terrestrial Planet Finder CCD b λ /2b Transmission Pattern of Nuller On the sky. (Star is at the center) When the light from two pupils are combined, the output can be imaged. The image is an Airy function with diameter 2.44λ/D where D is the telescope diameter. But the intensity of that image is modulated by the fringe pattern (on the sky) where b is the baseline between the pupils. if the star is at a null, the star s image has 0 intensity. If the planet is at the peak, the planet s light is unattenuated. A nulling interferometer that works with a single aperture telescope is different than one that combines light from 2+ telescopes

6 Terrestrial Planet Finder 2-arm vs. 4-arm Nulling Interferometers y 2 ( ) cos 2 sin 2 cos cos 2 cos 4 θ φ φ θ φ θ φ φ φ φ = = + = kb I I kb kb I I A e A e A e A e I y y x x i i i i ( ) [ ] ( ) cos cos cos 1 2 cos 2 sin 4 θ φ φ θ φ θ φ φ ks I ks I I ks I e A e A I x x i i = = = b x s

7 Null Depth Terrestrial Planet Finder Stellar sources have a finite diameter e.g. our 10pc~ 1mas Any cancellation scheme must account for this effect 2 Arm Stellar Leakage (Integrated Null Depth)= 8.2x Arm Stellar Leakage (Integrated Null Depth)=6.7x10-10

8 Ideal performance of Visible Nulling Coronagraph Terrestrial Planet Finder Four-arm interferometer leakage below at θ~λ/d

9 Image of Solar System Simulation of 4m nulling interferometer image after rotation. Terrestrial Planet Finder Integration time for an Solar system at 10pc SNR=5 on Earth in 5.1 hrs SNR=10 on each of 20 spectral Channels in 200 hrs S M V + E J

10 OTA+FSM +Beam Compressor 1 REVISIONS Terrestrial Planet Finder Exit Pupil: Diameter: 0.40 m Primary: Diameter: 4.0 m ROC: m Conic: -1.0 Parent Focal Length: 8.60 m Parent f/#: f/2.15 Off-axis Distance: 3.0 m Effective Focal Length: 8.86 m Compressor Primary: REV DESCRIPTION DATE BY Diameter: ~0.40 m ROC: 4.0 m A Initial Release 01/13/02 JKW Conic: -1.0 Parent Focal Length: 4.0 m Parent f/#: f/5 Off-axis Distance: 0.40 m Effective Focal Length: 2.02 m Stop Compressor Secondary: Diameter: 0.05 m ROC: 0.5 m Conic: -1.0 Parent Focal Length: 0.04 m Parent f/#: f/5 Off-axis Distance: 0.05 m Effective Focal Length: m Exit Diameter: 0.05 m Secondary: Diameter: ~0.40 m ROC: m Conic: -1.0 Parent Focal Length: m Off-Axis Distance: 0.30 m 0.86 m 7.74 m 8.50 m REV: A DESCRIPTION VTPF Telescope ISSUED: 01/04/02

11 Terrestrial Planet Finder Visible Nulling System Concept Y shear MMZ X shear MMZ Beam with X and Y shear, θ 4 null output Telescope Pupil Lenslet and fiberoptic array spatial filter Image plane (real image) ~(64 x 64) Diffraction limited imaging system (λ/10) s + - θ 4 Null in Pupil Overlap b y b x Area Turning/Rotation Mirrors - Baseline is 2 x shear + Single Mode Fiber array enables: 10-9 suppression achieved with 10-7 nuller and 100 lenslets suppression achieved with 10-7 nuller and 1000 lenslets Multiple sub-apertures make the detection less susceptible to Exo- Zodiacal Dust Residual background is incoherent with planet image Preserves field of view

12 Achromatic Nulling Interferometer Demonstration (Shao and Serabyn) Terrestrial Planet Finder Single pupil input Pupil Input Symmetric design Preserves pupil orientation and polarization Pupil shear adjustable variable null baseline Null output Dielectric plates provide achromatic null Bright output Symmetric Beam Splitters Dispersive Components For Achromatic Null + - Variable delay Dispersive Components For Achromatic Null Variable shear, s s

13 Refractive Dispersion Correction (Morgan) Terrestrial Planet Finder Broadband null-- Calculation for nulling depth for common optical glasses, BK7 and Fused Silica. Broadband null optimization Calculation for initial laboratory demonstration t,bk7 = / µm t, F.S. = / µm

14 Nuller #1 Terrestrial Planet Finder Tracking Camera Metrology Local Oscillator DM Bright Output DM Rooftop Shutter Input Phase Plates Phase Plates Shutter Piston/Shearing Rooftop 4 m Metrology Injection Out-of-band Pupil Camera TPF ~ 0.5 m Input Pupil Output Pupil DESCRIPTION VTPF Nuller 1 REV: A Dark Output ISSUED: 01/13/03

15 Terrestrial Planet Finder Tracking Camera Metrology Local Oscillator Proof of Concept Nulling Interferometer DM Bright Output DM Rooftop 4 m Shutter Input Phase Plates Intensity Metrology Injection Phase Plates Shutter Out-of-band Pupil Camera Piston/Shearing Rooftop Dark TPF ~ 0.5 m Output Input Pupil Output Pupil DESCRIPTION VTPF Nuller 1 REV: A Spectral Density ISSUED: 01/13/03 Detector feed Input Light source Symmetric beam splitters Shear Roof Top reflector Phase Roof Top reflector Shutters in front of one roof to measure intensity equalization for each arm First Laboratory Results-- White Light Fringe Scan Optical bench isolated with pads and doors, otherwise ambient laboratory conditions The starlight leakage only depends on the amplitude and phase mismatch inside the fiber Wavelength (nm)

16 Deep Nulls from Monochromatic Light Terrestrial Planet Finder 10 0 dataset time sec Laser diode source ~1nm bw Intensity matched to 0.1~0.2% Polarization aligned Small dither imposed, sync d with scope display. Dither signal demodulated by eye OPD control by hand on pzt voltage knob. Closed loop control currently being integrated Sustained null, Average leakage Best transient null 6x10-7 (6x x10-6 (7x10-9 per airy spot) per airy spot), 40msec sampling ~ Late Nov/Early Dec 2002

17 Laser Metrology Nulling Detector Performance Terrestrial Planet Finder Noise floor = 10pm/ Hz Null ~2.5x10-5 Null ~3.7x10-6

18 Summary Terrestrial Planet Finder Single Aperture Telescope with Visible Nulling based Interferometer System Capable of Imaging and Spectroscopy of Planets (D=4-5m) Concept and Instrument Defined Starlight Suppression is the Most Challenging Technology Steady State 6x10-9, and Transient 7x10-10 Demonstrated Laser Metrology System Integrated Near Term Work Deep Laser Null White Light Null (25-30% band pass) Demonstration of Single Mode Coherent Fiber Array Long Term Experiments: Use of DM to control amplitude and phase channel SMF array System Demonstration on Test Bed

19 Terrestrial Planet Finder Back up Slides

20 Terrestrial Planet Finder Coherent Fiber Array Nulling Requirements Light from Nuller CCD lenslet array Coherent Fiber array Final Imaging optic In a visible TPF based on a nulling interferometer For Earth Detection: Fiber array has ~ 1000 fibers Final image plane has a field of view ~1000 airy spots (~30x30) Average null of 1e-7 means that 1e-7 light spread over 1000 airy spots, or 1e-10 scattered light per airy spot. Nulling requirement (Vis TPF/Earth) is 1e-7 for Q=1, planet flux = scattered light flux 3e-7 for Q=0.3 Requirement for Jupiter Imager ~10~100x easier

21 Single Mode Fiber Array Design and Characterization Terrestrial Planet Finder Commercial (preliminary) fiber array results Irregular gaps between fibers Machine tolerance on metal housing issue Useful for development of: lens array to fiber alignment array characterization procedures Next Generation Array Design Use large mode field diameter Photonic Crystal Fiber (PCF) to relax alignment error requirement Use V-groove type fiber array construction for flexible fiber and lenslet spacing or custom self assembly fixture Custom lens array with focal plane at substrate Precision mapping of lenslet to fiber positions Fiber Array Assemble Using index matching bonding material to relax fiber array polishing requirement Lens Array Index Matching Bonding Material Lens Array

22 Terrestrial Planet Finder Phase Map Single Mode Fiber Array

23 Key Components Terrestrial Planet Finder Deformable mirror, for amplitude and phase control. The MEM s DM is far from perfect but the use of single mode fibers is very tolerant of DM imperfections Need a custom DM, with both piston and tip/tilt control of segmented subapertures Coherent fiber array Currently looking single mode fibers with large mode diameters, to ease alignment of lenslet array to fiber array. Fibers only need to be coherent to ~λ/10, allow ~10um kinks.

24 Summary Terrestrial Planet Finder Visible Nulling Interferometer Summary Achieved sustained null of 7x10-6, and transient null of 6x10-7 with a 1000 fiber bundle, implies scattered light in Visible TPF would be 7x10-9 and 6x10-10 per Airy spot, respectively. Closed-loop metrology systems has been integrated into the interferometer Closed loop testing in progress Only a factor of 2~6 away from what is needed in a visible TPF with a 4m primary, to detect Earths around solar like stars at 10pc. Single Mode Fiber Array Summary Lenslet array center-to-center spacing measured to ±1.33µm Repeatability is ± 0.22 µm In process to build 20 and 80 SMF arrays 5x decrease in position tolerance on lenslet array and alignment

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