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IR Frequency Region: X–H Stretching01:24

IR Frequency Region: X–H Stretching

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In IR spectroscopy, signals produced by the X−H bonds (such as C−H, O−H, or N−H) can be observed in the frequency range of  2700–4000 cm–1. The C−H stretching vibration forms sharp bands in the region 2850–3000 cm–1. The presence of the O−H stretching vibration leads to the forming of an absorption band in the frequency range 3650–3200 cm−1. At the same time, N−H stretching can be confirmed by absorption bands in...
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The dipole moment of a bond is the product of the partial charge on either atom and the distance between them. Dipole moments influence the efficiency of IR absorption and the peak intensity. When a bond with a dipole moment is placed in an electric field, the direction of the field determines if the bond is compressed or stretched. Electromagnetic radiation consists of an electric field component that rapidly reverses direction. It follows that polar bonds are alternately stretched and...
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IR Spectroscopy: Molecular Vibration Overview01:24

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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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Identical bonds within a polyatomic group can stretch symmetrically (in-phase) or asymmetrically (out-of-phase). Similar to hydrogen bonding, these vibrations also influence the shape of the IR peak. Generally, asymmetric stretching frequencies are higher than symmetric stretching frequencies. For example, primary amines exhibit two distinct IR peaks between 3300–3500 cm−1 corresponding to the symmetric and asymmetric N-H stretching, while secondary amines exhibit a single...
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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...
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Organic molecules primarily contain carbon and hydrogen atoms. While all the hydrogen isotopes are NMR-active, protium or hydrogen-1 is the most abundant. It has a significant energy separation between its nuclear spin states due to its large gyromagnetic ratio. As per Boltzmann's distribution, an increase in the energy separation implies a greater excess population of nuclei available for excitation, resulting in a strong NMR absorption signal.
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The CH3D Absorption Spectrum Near 1.58 μm: Extended Line Lists and Rovibrational Assignments.

Ons Ben Fathallah1, Anastasiya Lembei1, Michael Rey2

  • 1CNRS, LIPhy, University Grenoble Alpes, 38000 Grenoble, France.

Molecules (Basel, Switzerland)
|November 27, 2024
PubMed
Summary

This study analyzes monodeuterated methane (CH3D) spectra to refine its absorption lines, crucial for planetary D/H ratio measurements. New assignments and energy values improve understanding of CH3D

Keywords:
CH3DCH4HITRANTheoReTSTitanabsorption spectroscopymethanerovibrational assignments

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Area of Science:

  • Atmospheric Spectroscopy
  • Molecular Physics
  • Planetary Science

Background:

  • Monodeuterated methane (CH3D) significantly impacts absorption in the 1.58 μm transparency window.
  • Its spectrum, particularly the 3ν2 band, is vital for planetary applications like D/H ratio determination.

Purpose of the Study:

  • To analyze the CH3D spectrum in the 6099-6530 cm−1 region at room temperature and 81 K.
  • To derive empirical lower-state energy values and assign spectral transitions.
  • To compare experimental data with theoretical predictions.

Main Methods:

  • High-sensitivity differential absorption spectroscopy was used to record CH3D spectra.
  • The 2T-method was employed to derive lower-state energies from temperature-dependent line intensity ratios.
  • Rovibrational assignments were made by comparing experimental data with the TheoReTS variational line list and confirmed using Ground-State Combination Difference (GSCD) relations.

Main Results:

  • An elaborated room-temperature line list (11,189 lines) was combined with an 81 K list (8962 lines).
  • Approximately 4800 empirical lower-state energy values were derived.
  • 2890 transitions were assigned to twenty bands, with fifteen newly reported, showing good agreement with variational calculations.
  • Upper-state energies were determined with high precision (10−3 cm−1).

Conclusions:

  • The study provides an improved spectral line list for CH3D, enhancing its utility in planetary atmospheric analysis.
  • The validated assignments and energy values contribute to a more accurate understanding of CH3D's spectroscopic properties.
  • The findings support the use of CH3D spectroscopy for precise D/H ratio measurements in planetary science.