Bispectral technique for reconstruction the astronomical images with an intensity interferometer
| dc.creator | Zhilyaev, B. E. | |
| dc.date | 2008-06-02 | |
| dc.date.accessioned | 2026-07-07T09:44:18Z | |
| dc.date.available | 2026-07-07T09:44:18Z | |
| dc.description | An extension may be proposed to the intensity interferometer of Hanbury Brown and Twiss to provide the Fourier phase measurement by the use of third-order intensity correlations. It is well known that interferometric reconstruction of astronomical images can be obtained from second-order correlations only when a priory information is used about the object. The third-order intensity correlations contain information about the Fourier phase and need no such assumptions. In the ordinary way we can make measurements of the second-order intensity correlations with an intensity interferometer. We can also calculate the third-order intensity correlations from the data set of measured intensities for each distance triplet. After that we can reconstruct the Fourier phase from third-order correlations by using bipectral technique. When this is combining with the Fourier magnitude obtained from the second-order intensity correlations, we have the ultimate Fourier transform of the source brightness distribution. An inverse Fourier transform recovers the source image. | |
| dc.description | 2 pages, Contribution to the SPIE meeting in Marseille on 27 June 2008 | |
| dc.identifier | https://arxiv.org/abs/0806.0191 | |
| dc.identifier | http://arxiv.org/abs/0806.0191 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/162822 | |
| dc.subject | Astrophysics | |
| dc.subject | Data Analysis, Statistics and Probability | |
| dc.title | Bispectral technique for reconstruction the astronomical images with an intensity interferometer | |
| dc.type | text |