ABSTRACT
Astrophotonics is an emerging field that focuses on the development of photonic components for astronomical instrumentation. With ongoing advancements, astrophotonic solutions are already becoming an integral part of existing instruments. A recent example is the 60M ESO GRAVITY instrument at the Very Large Telescope Interferometer, Chile, that makes heavy use of photonic components. We envisage far-reaching applications in future astronomical instruments, especially those intended for the new generation of extremely large telescopes and in space. With continued improvements in extreme adaptive optics, the case becomes increasingly compelling. The joint issue of JOSA B and Applied Optics features more than 20 state-of-the-art papers in diverse areas of astrophotonics. This introduction provides a summary of the papers that cover several important topics, such as photonic lanterns, beam combiners and interferometry, spectrographs, OH suppression, and coronagraphy.
ABSTRACT
The design of a complex phase mask (CPM) for inscribing multi-notch fiber Bragg grating filters in optical fibers for OH suppression in astronomy is presented. We demonstrate the steps involved in the design of a complex mask with discrete phase steps, following a detailed analysis of fabrication constraints. The phase and amplitude of the complex grating is derived through inverse modelling from the desired aperiodic filter spectrum, following which the phase alone is encoded into the surface relief of a CPM. Compared to a complicated "running-light" Talbot interferometer based inscription setup where the phase of the inscribing beam is controlled by electro- or acousto-optic modulators and synchronized to a moving fiber translation stage, CPM offers the well-known convenience and reproducibility of the standard phase mask inscription technique. We have fabricated a CPM that can suppress 37 sky emission lines between 1508 nm to 1593 nm, with a potential of increasing to 99 channels for suppressing near-infrared (NIR) OH-emission lines generated in the upper atmosphere and improving the performance of ground-based astronomical telescopes.
ABSTRACT
A grating-less fiber vector bend sensor is demonstrated using a standard single mode fiber spliced to a multimode fiber as a multimode interference device. The ring-shaped light intensity distribution at the end of the multimode fiber is subject to a vector transition in response to the fiber bend. Instead of comprehensive imaging processing for the analysis, the image can be tapped out by a seven-core fiber spliced to the other end of the multimode fiber. The seven-core fiber is further guided to seven single mode fibers via a commercial fan-out device. By comparing the relative light intensities received at the seven outputs, both the bend radius and its direction can be determined. Experiment has shown that a slight bend displacement of 10 µm over a 1.2-cm-long multimode fiber in the X direction (bend angle of 0.382°) causes a distinctive power imbalance of 4.6 dB between two chosen outputs (numbered C4 and C7). For the same displacement in the Y direction, the power ratio between the previous two outputs C4 and C7 remains constant, while the imbalance between another pair (C3 and C4) rises significantly to 7.0 dB.
