1. Optics in Astronomy - Interferometry - Oskar von der Lühe Kiepenheuer-Institut für Sonnenphysik Freiburg, Germany

2. September 2002Optics in Astronomy2 Contents Fundamentals of interferometry Concepts of interferometry Practical interferometry Fundamentals of interferometry –Why interferometry? –Diffraction-limited imaging –A Young‘s interference experiment –Propagation of light and coherence –Theorem of van Cittert - Zernike

3. September 2002Optics in Astronomy3 What is interferometry? superposition of electromagnetic waves –at (radio and) optical wavelengths –infrared: = 20 µm... 1µm –visible: = 1 µm... 0.38 µm which emerge from a single source and transverse different paths to measure their spatio-temporal coherence properties Why interferometry? –to increase the angular resolution in order to –compensate for atmospheric and instrumental aberrations speckle interferometry diluted pupil masks –overcome the diffraction limit of a single telescope by coherent combination of several separated telescopes Topic of this lecture on interferometry? –to increase the angular resolution in order to –compensate for atmospheric and instrumental aberrations speckle interferometry diluted pupil masks –overcome the diffraction limit of a single telescope by coherent combination of several separated telescopes

4. September 2002Optics in Astronomy4 Diffraction limited imaging D telescope aperture focal length F

5. September 2002Optics in Astronomy5 A Young‘s interference experiment diameter D baseline B focal length F wavelength

6. September 2002Optics in Astronomy6 Two-way interferometer I Change of baseline

7. September 2002Optics in Astronomy7 Two-way interferometer II Change of element diameter

8. September 2002Optics in Astronomy8 Two-way interferometer IIa Change of element diameter

9. September 2002Optics in Astronomy9 Two-way interferometer III Change of wavelength

10. September 2002Optics in Astronomy10 Dependence on source position

11. September 2002Optics in Astronomy11 Two-way interferometer IV Change of source position

12. September 2002Optics in Astronomy12 Dependence on internal delay delay 

13. September 2002Optics in Astronomy13 Two-way interferometer V Change of internal delay

14. September 2002Optics in Astronomy14 Monochromatic e. m. waves Time-dependent, monochromatic e.m. field: Time-independent e.m. field fulfils Helmholz equation: C

15. September 2002Optics in Astronomy15 Propagation of field Kirchhoff-Fresnel integral, based on Huyghens‘ principle  r

16. September 2002Optics in Astronomy16 Non-monochromatic waves Spectral decomposition: Propagation of a general e.m. wave: Condition of quasi- monochromatism: Propagation of a quasi- monochromatic wave:

17. September 2002Optics in Astronomy17 Intensity at point of superposition The intensity distribution at the observing screen of the Young‘s interferometer is given by the sum of the intensities originating from the individual apertures plus the expected value of the cross product (correlation) of the fields.

18. September 2002Optics in Astronomy18 Concepts of coherence I (terminology from J. W. Goodman, Statistical Optics) mutual intensity: temporally stationary conditions, with  = t 2 - t 1 complex degree of coherence:

19. September 2002Optics in Astronomy19 Concepts of coherence II self coherence (temporal coherence): complex degree of self coherence: mutual intensity (spatial coherence): complex coherence factor:

20. September 2002Optics in Astronomy20 Concepts of coherence III Coherence is a property of the e.m. field vector! It is important to consider the state of polarisation of the light as orthogonal states of polarisation do not interfere (laws of Fresnel-Arago). Optical designs of interferometers which change the state of polarisaiton differently in different arms produce instrumental losses of coherence and therefore instrumental errors which need calibration.

21. September 2002Optics in Astronomy21 Temporal coherence 1 2R 2Z S2 S1 1 2 coherence time: refined monochromatic condition:

22. September 2002Optics in Astronomy22 Two-way interferometer VI Extended spectral distribution of a point source

23. September 2002Optics in Astronomy23 Two-way interferometer VII Extended spectral distribution source and delay errors

24. September 2002Optics in Astronomy24 Transport of coherence

25. September 2002Optics in Astronomy25 Extended sources

26. September 2002Optics in Astronomy26 Extended, incoherent sources Most astronomical sources of light have thermal origin. The processes emitting radiation are uncorrelated (incoherent) at the atomic level. Mutual intensity at the surface of an incoherent source: Transport of mutual intensity to the interferometer:

27. September 2002Optics in Astronomy27 Celestial sources have large distances S compared to their dimensions. Differences in S can be expanded in first order to simplify the propagation equation. Inclination terms  are set to unity. Linear distances in the source surface are replaced by apparent angles. The transport equation can then be simplified: Theorem of van Cittert - Zernike

28. September 2002Optics in Astronomy28 Intensity distribution in the Young‘s intererometer The complex coherence factor µ is often called the complex visibility. It fulfils the condition

29. September 2002Optics in Astronomy29 Two-way interferometer VII Spatially extended source - double star

30. September 2002Optics in Astronomy30 Two-way interferometer VII Spatially extended source - limb darkened stellar disk

31. September 2002Optics in Astronomy31 Extended sources - not unique?

32. September 2002Optics in Astronomy32 van Cittert - Zernike theorem 2D Fourier transform of source intensity at angular frequency B/ (visibility function) Instrumental cosine term Observed Intensity Response to a point source in direction of  Source intensity

33. September 2002Optics in Astronomy33 What does the vCZT mean? An interferometer projects a fringe onto the source‘s intensity distribution The magnitude of the fringe amplitude is given by the structural content of the source at scales of the fringe spacing The phase of the fringe is given by the position of the fringe which maximises the small scale signal

34. September 2002Optics in Astronomy34 What have we learned? An astronomical interferometer measures spatio-temporal coherene properties of the light emerging from a celestial source. The spatial coherence properties encodes the small scale structural content of the intensity distribution in celestial coordinates. The temporal coherence properties encodes the spectral content of the intensity distribution. The measured interferometer signal depends on structural and spectral content.