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Mass Spectrum01:23

Mass Spectrum

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A mass spectrum is the graphical representation of the relative abundance of the charged fragments in an analyte plotted against their mass-to-charge ratio (m/z). The plot's x-axis represents the ratio of the mass of the charged fragment to the number of charges it carries. The y axis of the plot represents the relative abundance of each charged species. The relative abundance is calculated from the signal intensity of each charged species recorded at the detector. The most intense signal (the...
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When solids, liquids, or condensed gases are heated sufficiently, they radiate some of the excess energy as light. Photons produced in this manner have a range of energies, and thereby produce a continuous spectrum in which an unbroken series of wavelengths is present.
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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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When Infrared (IR) radiation passes through a covalently bonded molecule, the bonds transition from lower to higher vibrational levels. The fundamental vibrational motions that result in infrared absorption can be classified as stretching or bending vibrations.
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Measurement and Analysis of Atomic Hydrogen and Diatomic Molecular AlO, C2, CN, and TiO Spectra Following Laser-induced Optical Breakdown
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Spectrum of hot methane in astronomical objects using a comprehensive computed line list.

Sergei N Yurchenko1, Jonathan Tennyson2, Jeremy Bailey3

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A new methane (CH4) line list, 10to10, with nearly 10 billion transitions improves models of exoplanet and brown dwarf atmospheres. This comprehensive dataset is crucial for accurate characterization, especially in the near-infrared.

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Area of Science:

  • Astrophysics
  • Planetary Science
  • Spectroscopy

Background:

  • Hot methane spectra are vital for understanding environments like flames, cool stars, and exoplanet atmospheres.
  • Existing methane spectroscopic data are incomplete, causing underestimations of opacity at short wavelengths and high temperatures.

Purpose of the Study:

  • To present a new, comprehensive spectroscopic line list for methane (CH4) named 10to10.
  • To provide a dataset applicable to high temperatures (up to 1,500 K) for improved atmospheric modeling.

Main Methods:

  • Development of the 10to10 methane line list, incorporating almost 10 billion transitions.
  • Application of the 10to10 line list to atmospheric models of celestial objects.

Main Results:

  • The 10to10 line list covers a broad spectral range and is valid for temperatures up to 1,500 K.
  • Models using 10to10 show improved agreement with observations for the brown dwarf 2MASS 0559-14.
  • Studies of the exoplanet HD 189733b using 10to10 revealed up to a 20-fold increase in methane abundance.

Conclusions:

  • Accurate characterization of exoplanet and brown dwarf atmospheres requires the inclusion of numerous hot transitions.
  • The 10to10 line list is essential for precise atmospheric studies, particularly in the near-infrared spectrum.