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The weaker peak of NMTNR-4-400 NMTNR-4-400 NMTNR-4-400stallindicatesthe samplower
Other than this peak, we also observed two strong Raman peaks at ~241 and 482 cm−1 and one much weaker peak at ~189 cm−1.
We do see magnetosheath-like fluxes of solar wind origin ions here, though the protons show weaker peak fluxes, as can be expected inside the nominal IMB.
This spectrum shows a peak centred at 285.4 eV with a fwhm of 1.4 eV and a weaker peak at 289 eV.
A PLE spectrum consists of a sharp peak at 454 nm and much weaker peak (or even shoulder) at about 434 nm.
The strong peak near 283.3 eV clearly indicates the existence of carbide bonding [31, 32], and the weaker peak near 287 eV indicates the presence of residual graphitic carbon.
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Roughness causes the major contrast peak to essentially split into several weaker peaks (see Figure 8).
Besides, the weaker peaks assigned to B acid demonstrate the decrease of B acid sites.
The latter has a characteristic IR absorption spectrum with a sharp peak at 1332 cm−1 and broader and weaker peaks at 1115, 1046 and 950 cm−1.
Interestingly, weaker peaks were found enriched towards transcription start sites (TSS).
In addition to the strong peak in the ICF observed for April 2010, we observe additional somewhat weaker peaks, in June and August of 2010.
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