Polarimetry

Polarimetry is the measurement and interpretation of the polarization of transverse waves, most notably electromagnetic waves, such as radio or light waves. Typically polarimetry is done on electromagnetic waves that have traveled through or have been reflected, refracted or diffracted by some material in order to characterize that object.[1][2]

Synthetic aperture radar image of Death Valley colored using polarimetry.

plane polarized light:

according to the wave theory of light an ordinary ray of light is consider to be vibrating in all planes of right angles to the direction of its propagation if this ordinary ray of light is passed through a nicol prism the emergent ray has its vibration only in one plane.

Applications

Polarimetry of thin films and surfaces is commonly known as ellipsometry.

Polarimetry is used in remote sensing applications, such as planetary science, astronomy, and weather radar.

Polarimetry can also be included in computational analysis of waves. For example, radars often consider wave polarization in post-processing to improve the characterization of the targets. In this case, polarimetry can be used to estimate the fine texture of a material, help resolve the orientation of small structures in the target, and, when circularly-polarized antennas are used, resolve the number of bounces of the received signal (the chirality of circularly polarized waves alternates with each reflection).

Imaging

In 2003, a visible-near IR (VNIR) Spectropolarimetric Imager with an acousto-optic tunable filter (AOTF) was reported.[3] These hyperspectral and spectropolarimetric imager functioned in radiation regions spanning from ultraviolet (UV) to long-wave infrared (LWIR). In AOTFs a piezoelectric transducer converts a radio frequency (RF) signal into an ultrasonic wave. This wave then travels through a crystal attached to the transducer and upon entering an acoustic absorber is diffracted. The wavelength of the resulting light beams can be modified by altering the initial RF signal.[3] VNIR and LWIR hyperspectral imaging consistently perform better as hyperspectral imagers.[4] This technology was developed at the U.S. Army Research Laboratory.[3]

The researchers reported visible near infrared system (VISNIR) data (.4-.9 micrometers) which required an RF signal below 1 W power. The reported experimental data indicates that polarimetric signatures are unique to manmade items and are not found in natural objects. The researchers state that a dual system, collecting both hyperspectral and spectropolarimetric information, is an advantage in image production for target tracking.[3]

Equipment

A polarimeter is the basic scientific instrument used to make these measurements, although this term is rarely used to describe a polarimetry process performed by a computer, such as is done in polarimetric synthetic aperture radar.

Polarimetry can be used to measure various optical properties of a material, including linear birefringence, circular birefringence (also known as optical rotation or optical rotary dispersion), linear dichroism, circular dichroism and scattering.[5] To measure these various properties, there have been many designs of polarimeters, some archaic and some in current use. The most sensitive are based on interferometers, while more conventional polarimeters are based on arrangements of polarising filters, wave plates or other devices.

Astronomical polarimetry

Polarimetry is used in many areas of astronomy to study physical characteristics of sources including active galactic nuclei and blazars, exoplanets, gas and dust in the interstellar medium, supernovae, gamma-ray bursts, stellar rotation,[6] stellar magnetic fields, debris disks, reflection in binary stars[7] and the cosmic microwave background radiation. Astronomical polarimetry observations are carried out either as imaging polarimetry, where polarization is measured as a function of position in imaging data, or spectropolarimetry, where polarization is measured as a function of wavelength of light, or broad-band aperture polarimetry.

Measuring optical rotation

Optically active samples, such as solutions of chiral molecules, often exhibit circular birefringence. Circular birefringence causes rotation of the polarization of plane polarized light as it passes through the sample.

In ordinary light, the vibrations occur in all planes perpendicular to the direction of propagation. When light passes through a Nicol prism its vibrations in all directions except the direction of axis of the prism are cut off. The light emerging from the prism is said to be plane polarised because its vibration is in one direction. If two Nicol prisms are placed with their polarization planes parallel to each other, then the light rays emerging out of the first prism will enter the second prism. As a result, no loss of light is observed. However, if the second prism is rotated by an angle of 90°, the light emerging from the first prism is stopped by the second prism and no light emerges. The first prism is usually called the polarizer and the second prism is called the analyser.

A simple polarimeter to measure this rotation consists of a long tube with flat glass ends, into which the sample is placed. At each end of the tube is a Nicol prism or other polarizer. Light is shone through the tube, and the prism at the other end, attached to an eye-piece, is rotated to arrive at the region of complete brightness or that of half-dark, half-bright or that of complete darkness. The angle of rotation is then read from a scale. The same phenomenon is observed after an angle of 180°. The specific rotation of the sample may then be calculated. Temperature can affect the rotation of light, which should be accounted for in the calculations.

where:

  • [α]λT is the specific rotation.
  • T is the temperature.
  • λ is the wavelength of light.
  • α is the angle of rotation.
  • l is the length of the polarimeter tube.
  • is the mass concentration of solution.
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See also

References
  1. Mishchenko, M.I.; Yatskiv, Y.S.; Rosenbush, V.K.; Videen, G., eds. (2011). Polarimetric Detection, Characterization and Remote Sensing, Proceedings of the NATO Advanced Study Institute on Special Detection Technique (Polarimetry) and Remote Sensing Yalta, Ukraine 20 September – 1 October 2010, Series: NATO Science for Peace and Security Series C: Environmental Security. NATO Science for Peace and Security Series C: Environmental Security (1st ed.). Springer. ISBN 9789400716353.
  2. Tinbergen, Jaap (2007). Astronomical Polarimetry. Cambridge University Press. ISBN 978-0-521-01858-6.
  3. Goldberg, A.; Stann, B.; Gupta, N. (July 2003). "Multispectral, Hyperspectral, and Three-Dimensional Imaging Research at the U.S. Army Research Laboratory" (PDF). Proceedings of the International Conference on International Fusion [6th]. 1: 499–506.
  4. Makki, Ihab; Younes, Rafic; Francis, Clovis; Bianchi, Tiziano; Zucchetti, Massimo (1 February 2017). "A survey of landmine detection using hyperspectral imaging" (PDF). ISPRS Journal of Photogrammetry and Remote Sensing. 124: 40–53. Bibcode:2017JPRS..124...40M. doi:10.1016/j.isprsjprs.2016.12.009. ISSN 0924-2716.
  5. V. Tuchin (2000). Tissue Optics Light Scattering Methods and Instruments for Medical Diagnosis. Society of Photo Optical. ISBN 978-0-8194-3459-3.
  6. Cotton, Daniel V; Bailey, Jeremy; Howarth, Ian D; Bott, Kimberly; Kedziora-Chudczer, Lucyna; Lucas, P. W; Hough, J. H (2017). "Polarization due to rotational distortion in the bright star Regulus". Nature Astronomy. 1 (10): 690–696. arXiv:1804.06576. Bibcode:2017NatAs...1..690C. doi:10.1038/s41550-017-0238-6.
  7. Bailey, Jeremy; Cotton, Daniel V.; Kedziora-Chudczer, Lucyna; De Horta, Ain; Maybour, Darren (1 April 2019). "Polarized reflected light from the Spica binary system". Nature Astronomy. 3 (7): 636–641. arXiv:1904.01195. Bibcode:2019NatAs...3..636B. doi:10.1038/s41550-019-0738-7.

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