Molecular hydrogen emission lines , 1934, 2. 2 (especially Figure 4) we showed that two fundamentally different kinds of lines excite the H 2 lines: those that form throughout the chromosphere and whose transfer is dominated by the line opacity of the transition itself (H i Lyα, C ii lines), and the other lines (canonical "transition region lines" like Si iv) whose emission Feb 26, 2025 · Using data from the James Webb Space Telescope (JWST) Advanced Deep Extragalactic Survey (JADES), we tentatively detect two molecular hydrogen (H$_2$) fluorescent emission features in high-redshift galaxies at 2. 12μm/2. Nov 12, 2024 · Lines of the Werner and Lyman bands of molecular hydrogen are produced when bright emission lines similar in wavelength to the H 2 transitions excite electrons into the upper energy levels within the molecule. 12 μm, five other H2 May 31, 2016 · Exactly why the molecular emission is low I'm not sure, but I'd guess it's because a low pressure discharge lamp works by colliding electrons with the gas molecules at energies well above the dissociation energy of molecular hydrogen. If the gas is viewed at an angle away only allow the study of molecular gas in the Solar Neighborhood and provide no spatial information on the distribution of H 2. 2004;van Hoof2018;Garc´ıa-Rojas et al. Although morphology of the H 2 emission is typically used to distinguish MHOs, H 2 2. 15, observed by the Spitzer Space Telescope. Objects detected only in other near-IR lines (e.
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