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Related Concept Videos

Ultraviolet and Visible (UV–Vis) Spectroscopy: Overview01:02

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...
UV–Vis Spectrometers01:14

UV–Vis Spectrometers

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...
Atomic Emission Spectroscopy: Instrumentation01:22

Atomic Emission Spectroscopy: Instrumentation

The instrumentation of atomic emission spectrometry (AES) involves various components, including atomization devices that convert samples into gas-phase atoms and ions. There are two main types of atomization devices: continuous and discrete atomizers.  Continuous atomizers, like plasmas and flames, introduce samples in a constant stream, while discrete atomizers inject individual samples using syringes or autosamplers. The most common discrete atomizer is the electrothermal atomizer.
UV–Vis Spectroscopy: Beer–Lambert Law01:09

UV–Vis Spectroscopy: Beer–Lambert Law

The Beer-Lambert law describes the relationship between absorbance and concentration, which combines the principles established by scientists Johann Heinrich Lambert and August Beer. Lambert's law states that when light passes through a medium, the loss in intensity is directly proportional to the original intensity and the path length of the light. Beer's law proposed that the transmittance of a solution remains constant if the product of concentration and path length is constant. The modern...
UV–Vis Spectrum01:30

UV–Vis Spectrum

When light passes through a substance, a portion of the light is absorbed while the remaining light is reflected or transmitted. If the molecule absorbs light between the wavelengths of 180–400 nm range, the UV spectrum is obtained, and if it absorbs light in the 400–780 nm wavelength range, the visible spectrum is obtained.     
The UV–Vis spectrum of a molecule is the plot of its absorbance versus wavelength. The plot is drawn by taking molar absorptivity (ε) or log ε on the y-axis (ordinate)...
IR Spectrometers01:25

IR Spectrometers

There are two main infrared (IR) spectrophotometers: dispersive IR spectrometers and Fourier transform infrared (FTIR) spectrometers. In a dispersive IR spectrometer, a beam of infrared radiation produced by a hot wire is divided into two parallel equal-intensity beams using mirrors. One beam passes through the sample, while another is a reference beam. The beams then move through the monochromator, which separates the radiations into a continuous spectrum of different frequencies. The...

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Related Experiment Video

Updated: Jun 16, 2026

Bringing the Visible Universe into Focus with Robo-AO
10:35

Bringing the Visible Universe into Focus with Robo-AO

Published on: February 12, 2013

Extreme uv spectroheliometer on the Apollo Telescope Mount.

E M Reeves, M C Huber, J G Timothy

    Applied Optics
    |February 20, 2010
    PubMed
    Summary
    This summary is machine-generated.

    The Skylab solar instrument, a seven-channel spectrometer-spectroheliometer, captured detailed spatial and spectral data across a wide wavelength range. Its design and performance for observing solar features are thoroughly documented.

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    Area of Science:

    • Solar physics
    • Astronomy
    • Astrophysics

    Background:

    • The Skylab mission provided a unique platform for solar observation.
    • Understanding solar features requires advanced spectroscopic instruments.

    Purpose of the Study:

    • To detail the design of the Harvard College Observatory's solar instrument.
    • To describe the operational performance of the spectrometer-spectroheliometer.

    Main Methods:

    • Utilized a seven-channel spectrometer-spectroheliometer.
    • Operated within the 280-1340 Angstrom wavelength range.
    • Employed spatial and spectral scanning modes for solar feature analysis.

    Main Results:

    • The instrument successfully performed spatial and spectral scans.
    • Data was collected across a broad spectrum of solar emissions.
    • The instrument's capabilities for observing diverse solar features were demonstrated.

    Conclusions:

    • The Harvard College Observatory instrument was a versatile tool for solar research.
    • Detailed documentation of the instrument's design and performance is now available.