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Ultraviolet and Visible (UV–Vis) Spectroscopy: Overview

Ultraviolet and Visible (UV–Vis) Spectroscopy: Overview

Ultraviolet–visible (UV–visible or UV–Vis) spectroscopy is an analytical technique that investigates the interaction between matter and UV–Vis light within the electromagnetic spectrum. This method is widely used for its versatility, simplicity, and relatively quick data acquisition, making it valuable for both qualitative and quantitative analysis. When UV–Vis radiation passes through a material, molecules absorb light depending on the energy required for electronic transitions. As a result...

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The absorbance of UV and visible (UV–visible) radiations is measured using a UV–visible spectrophotometer. Deuterium lamps, which emit UV radiation, and tungsten lamps, which produce radiation in the visible region, are used as light sources in UV–visible spectrophotometers. A monochromator or prism is used for diffraction grating, i.e., to split the incoming radiation into different wavelengths. A system of slits is used to focus the desired wavelength on the sample cell. Samples for...

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Infrared (IR) Spectroscopy: Overview

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When electromagnetic radiation passes through a material, atoms or molecules transition from a lower to a higher energy state by absorbing radiation corresponding to the energy difference between the two states. The absorption of infrared (IR) radiation causes transitions between vibrational energy levels in a molecule. Therefore, IR spectroscopy is a useful analytical tool for determining the molecular structure of molecules.
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UV–Vis Spectroscopy: Woodward–Fieser Rules

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UV–Visible absorption spectra of conjugated dienes arise from the lowest energy π&VeryThinSpace;→&VeryThinSpace;π* transitions. The light-absorbing part of the molecule is called the chromophore, and the substituents directly attached to the chromophore are called auxochromes. A strong correlation exists between the absorption maxima, λmax, and the structure of a conjugated π system. The Woodward–Fieser rules predict the value of λmax for a given structure by adding the contributions...

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In Ultraviolet–Visible (UV–Vis) spectroscopy, the absorption of electromagnetic radiation is used to probe the electronic structure of molecules. This technique provides insights into molecular electronic transitions, particularly the movement of electrons between different molecular orbitals. Radiation is absorbed if the energy of the electromagnetic radiation passing through the molecule is precisely equal to the energy difference between the excited and ground states. During this process,...

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Interferometer-grating spectrograph for high resolution astronomical spectroscopy in the middle uv.

B Bates, D J McCartney, C D McKeith

|March 6, 2010

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A new high-resolution spectrograph enables ultraviolet astronomical spectroscopy from a balloon platform. It achieves spectral resolving power greater than 10^5 using a Fabry-Perot interferometer and grating.

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Area of Science:

Astronomy and Astrophysics
Optical Physics

Background:

Ultraviolet (UV) astronomical spectroscopy requires high spectral resolution for detailed analysis.
Balloon-borne platforms offer stable, above-atmosphere observing conditions for specialized instruments.

Purpose of the Study:

To describe a novel high-resolution spectrograph designed for UV astronomical spectroscopy.
To detail the instrument's capability for achieving high spectral resolving power from a balloon platform.

Main Methods:

Development of a spectrograph utilizing an optically contacted Fabry-Perot interferometer.
Implementation of crossed dispersion with a grating order sorter to enhance spectral resolution.
Integration of the spectrograph onto a moderately stabilized, star-pointing balloon-borne platform.

Main Results:

Achieved a spectral resolving power greater than 10^5.
Demonstrated the feasibility of high-resolution UV spectroscopy from a balloon platform.
The instrument design combines interferometry and grating techniques for superior performance.

Conclusions:

The described spectrograph is a capable instrument for advanced UV astronomical observations.
The combination of a Fabry-Perot interferometer and grating provides exceptional spectral resolution.
Balloon-borne platforms are suitable for deploying high-resolution spectroscopic instruments for astrophysical research.