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

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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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AES is a powerful analytical technique, especially effective when used with plasma sources, producing abundant spectra in characteristic emission lines. The Inductively Coupled Plasma (ICP), in particular, yields superior quantitative analytical data due to its high stability, low noise, low background, and minimal interferences under optimal experimental conditions. However, newer air-operated microwave sources are emerging as promising alternatives that could be more cost-effective than...
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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

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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.
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For AAS measurements, samples must be introduced as clear solutions, often requiring extensive preliminary treatment to dissolve materials like soils, animal tissues, and minerals. Common methods for sample preparation include treatment with hot mineral acids, wet ashing, combustion in closed containers, high-temperature ashing, or fusion with reagents.
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Bringing the Visible Universe into Focus with Robo-AO
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Published on: February 12, 2013

Skylab ultraviolet stellar astronomy experiment S019.

F G O'Callaghan, K G Henize, J D Wray

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

    A stellar spectrograph on Skylab observed 188 star fields. This objective-prism instrument mapped ultraviolet and visible light spectra from space.

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    Published on: October 30, 2012

    Area of Science:

    • Astronomy and Astrophysics
    • Space Science
    • Spectroscopy

    Background:

    • Space-based astronomical observations offer unique advantages for studying stellar spectra.
    • Previous missions have utilized various instruments to capture light from celestial objects.

    Purpose of the Study:

    • To utilize an objective-prism stellar spectrograph on Skylab for astronomical observations.
    • To cover a broad wavelength range from 1300 A to 5000 A.

    Main Methods:

    • A 15-cm aperture objective-prism stellar spectrograph was employed.
    • The instrument featured a specialized optical system with CaF(2) prism and LiF corrector lenses.
    • Observations were made using an articulated mirror system (AMS) for target acquisition.

    Main Results:

    • Data were collected for 188 distinct star fields.
    • Each observed field covered an angular area of 4.0 x 5.0 degrees.
    • The spectrograph successfully operated across the ultraviolet and visible spectrum.

    Conclusions:

    • The Skylab stellar spectrograph provided valuable spectral data from space.
    • The instrument's design enabled observations in a critical wavelength range.
    • The mission demonstrated the utility of objective-prism spectroscopy from an orbital platform.