In many spectroscopic and photonics applications, it is desirable to work with light that has been polarized in a particular direction. In this article we explore what polarization is, and how it may be obtained from an unpolarized light source.

Light that has been polarized is useful because it enables the user to be selective over what part of the electromagnetic spectrum is used (whether for photography, night-vision, coloured lighting or analytical measurement). Of course, this filtering of light can offer the user a finer level of detail for their application, similarly to a sharp knife or a small paint brush.

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Many interactions of light with matter depend on its polarization. For example, at a reflective interface, components of light whose polarizations are oriented perpendicular to the plane of incidence are reflected more strongly than those oriented parallel to it. At one angle of incidence in particular – Brewster’s Angle – the reflected ray is completely polarized perpendicular to the plane of incidence.

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EM radiation has an electric and magnetic field component which oscillates in phase perpendicular to each other and to the direction in which the radiation propagates. These two oscillating fields are often visualised as in the diagram above and are continually self-propagating.

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For waves with their electric fields perpendicular to the wires, the electrons cannot move far across the wires (remember, the diameter of the wires are much smaller than the wavelength of light). So the perpendicular light passes through un-blocked (save for very small amounts).

Spectroscopy is the study of the spectra produced when material interacts with or emits light. It is the key to revealing details that cannot be uncovered through a picture. A spectrograph — sometimes called a spectroscope or spectrometer — breaks the light from a single material into its component colors the way a prism splits white light into a rainbow. It records this spectrum, which allows scientists to analyze the light and discover properties of the material interacting with it. Spectroscopy is as crucial as imaging to understanding the universe.

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To learn more about what spectroscopy can do, check out #SpectroscopySolutions for more insights into the applications XRF and FTIR can fit.

A spectrum is a rainbow! This rainbow is created when a beam of white light is broken into its component colors, such as with a prism. The colors formed are ordered according to their wavelength. When scientists look at this rainbow, they examine how intense the light is in each color. Is blue brighter than yellow, or is this specific red brighter than this other red?

What we generally refer to as “light” is more correctly known as ‘electromagnetic radiation’ (often abbreviated as EM radiation). The the main characteristics of electromagnetic radiation are its frequency and wavelength (λ). We broadly classify frequency into types of EM radiation, such as radio waves, microwaves, terahertz, infrared, visible light, ultraviolet, X-rays and gamma rays. In this sequence, radio waves are radiation with the lowest frequency (and largest wavelength) and gamma rays have the highest frequency (and shortest wavelength).

All elements absorb and emit specific wavelengths of light that correspond to those energy levels. An absorption spectrum is a spectrum of light transmitted through a substance, showing dark lines or bands where light has been absorbed by atoms, causing a dip in the spectrum. An emission spectrum is made by electrons falling down the energy ladder. It’s what you get when you look at hot gas, which is heated by something out of the line of sight. This heating moves the electrons up the ladder, then when they fall down the ladder some of the light they emit comes to you. This results in bright, colored spikes due to atoms releasing light at those wavelengths.

Light carries information about the material with which it interacts. Different materials interact differently with light, and we can use light to understand what something is made of. All matter is made of atoms. Electrons go around the nucleus of an atom at different allowed energies, like rungs on a ladder. Light with the exact energy needed to go between rungs can be absorbed, but not others. Electrons fall down to lower rungs, emitting light at the specific energy of the difference between the rungs. This allows different atoms and molecules to emit different colors of light. Sodium’s spectrum does not look like nitrogen’s spectrum — nor like the spectrum of any other element.

When material interacts with light, properties of that material are stamped on the light. This stamp is like a specific fingerprint for each element and molecule. By examining the intensity of light in each color, scientist can work backward to infer the properties of the material, such as an object’s size, temperature, motion, and composition, that touched the light along the way.

Hubble’s spectrographs reveal important details of many aspects of our universe. Below are examples of the many spectroscopic findings from Hubble.

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The orientation of the electric field plane is known as the “polarization direction” (E). This can be broken down into three basic categories:

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A spectrograph passes light coming into the telescope through a tiny hole or slit in a metal plate to isolate light from a single area or object. This light is bounced off a special grating, which splits the light into its different wavelengths (just like a prism makes rainbows). The split light lands on a detector, which records the spectrum that is formed.

Controlling reflections is an important application of polarizers. If the specific interactions with the surface are of interest, then the polarizer can be oriented parallel to select only the reflected rays; if the reflections are an unwanted source of measurement noise, the polarizer can be oriented to reduce them.

Wire Grid Polarizers are included in the Specac polarizer product range. It consists of an array of fine parallel conductive wires placed perpendicular to the incident beam, with the spacing of the wires being smaller than the wavelength of the light being filtered.

Specac provide a range of infrared wire grid polarizers for use in analytical testing across the mid-and-far-infrared spectrum of light. Some of these are compatible with our spectrometer accessories, allowing the user to mount a polarizing filter directly into an accessory or sample cell, further refining their analysis.

Hubble’s ultraviolet spectroscopy is one of its most powerful contributions to the astronomical community, and this capability will not be replaced or superseded by any mission in the near future. Ultraviolet spectroscopy tells us certain things about the universe, while visible and infrared spectroscopy tells us others. By combining Hubble’s ultraviolet spectroscopy with the infrared spectroscopic capabilities of the James Webb Space Telescope, the two telescopes can achieve scientific results together that neither could achieve alone.

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Some light waves will be parallel to these wires and those electrons will move along the wires instead of passing through to the other side of the filter. Any electrons that are not angled at the same plane as the wires (perpendicular) do not collide and are therefore free to move to the other side.

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Hubble is famous for the images captured by its cameras, but it often also relies on its spectrographs. Spectrographs collect data that tell scientists how much light comes out at each wavelength. These data reveal important details about the makeup of atmospheres on exoplanets, the compositions of stars and nebulas, the motion of galaxies and more.