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Kim, Youngsam,Mulay, Sandip V.,Choi, Minsuk,Yu, Seungyoon B.,Jon, Sangyong,Churchill, David G. Royal Society of Chemistry 2015 Chemical Science Vol.6 No.10
<▼1><P>Outstanding glutathione chemosensing selectivity with a new coumarin-based probe is reported and discussed in the context of live cell experiments; the point of attack is flanked by two proximal carbonyl groups.</P></▼1><▼2><P>A phenyl-selenium-substituted coumarin probe was synthesized for the purpose of achieving highly selective and extremely rapid detection of glutathione (GSH) over cysteine (Cys)/homocysteine (Hcy) without background fluorescence. The fluorescence intensity of the probe with GSH shows a ∼100-fold fluorescent enhancement compared with the signal generated for other closely related amino acids, including Cys and Hcy. Importantly, the substitution reaction with the sulfhydryl group of GSH at the 4-position of the probe, which is doubly-activated by two carbonyl groups, occurs extremely fast, showing subsecond maximum fluorescence intensity attainment; equilibrium was reached within 100 ms (UV-vis). The probe selectivity for GSH was confirmed in Hep3B cells by confocal microscopy imaging.</P></▼2>
Fluorescent Ultraviolet Spectra of Molecular Hydrogen in Star Forming Clouds
박수종,Dae-Hee Lee,Ewine F. van Dishoeck,민경욱,Youngsam Yu 한국물리학회 2003 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.42 No.III
The far-UV photons from the newly born stars make Photo-dissociation Regions (PDRs) on the surfaces of the nearby molecular clouds. In the PDRs, molecular hydrogens which absorb the far- UV photons in the Lyman-Werner bands are electrically excited, and then de-excited to the ground electrical states, emitting far-UV lines. These observations are only possible from space telescopes and can be one of the scientic purposes of the rst Korean scientic satellite. In order to prove the feasibility of observations for various celestial sources, we run a radiative transfer code to simulate the H2 uorescent lines with various physical conditions, i.e., gas density, gas temperature, external far-UV eld strength, and spectral energy distribution of the external UV eld. The code considers bound-continuum transitions as well as bound-bound transitions. The total uorescent intensities and the spectral shapes depend on the physical conditions. By observing the far-UV spectra from the PDRs, we can study the interaction of the young stars with the ambient clouds and the evolution process of the star forming clouds.