ライフサイエンスコーパス: spectral line

1 results in the observed narrowing of the EPR spectral line.

2 mal and nonthermal continuum models, with no spectral lines.

3 is accompanied by substantial broadening of spectral lines.

4 A emits bright signals in the phosphorus (P) spectral line against a low-contrast background, showed

5 levels, the mechanisms of the broadening of spectral lines, and the selected parameters of the spect

6 e unmodified mismatched G.A duplex exhibited spectral line broadening at neutral pH, suggesting a mix

7 as replaced by diamagnetic Zn(2+) to prevent spectral line broadening of the Q(A)(.-) due to magnetic

8 In contrast, at Q-band, most of the spectral lines due to the DMPO/.SG were separated from t

9 tion, we successfully obtained well-resolved spectral lines even without time-gated detection.

10 ition energy can be resolved into a separate spectral line for each photon number state of the microw

11 using the periodic Doppler shift of stellar spectral lines have recently achieved a precision of 60

12 We detect spectral lines in 23 out of 26 sources and multiple line

13 In addition, doubling of spectral lines in all of the observed samples provides e

14 finding, coupled with the observation of Tc spectral lines in certain stars, shows that the majority

15 Broadening of spectral lines is a signature of chemical exchange pheno

16 Probe deuteration resulted in a narrow spectral line of 1.2 G compared to a nondeuterated analo

17 f about two millikelvin in the 21-centimetre spectral line of atomic hydrogen associated with stars a

18 ned in situ by cross-calibration between the spectral lines of different charge states, and even diff

19 or the lowfield spectral line, the remaining spectral lines of DMPO/ .SG virtually over-lap with thos

20 n shown that in these objects the rotational spectral lines of molecular hydrogen observed at mid-inf

21 ectric quadrupole moment, which broadens the spectral lines, often over several megahertz.

22 s by measuring the gravitational redshift of spectral lines produced in the neutron star photosphere.

23 From the spectral line profiles, the molecules can be distinguish

24 y Gaussian fitting, and modifications in the spectral lines, respectively, also suggested complex for

25 The changes in the EPR spectral line shape and the rotational correlation time

26 ate lifetime broadening contributions to the spectral line shape arising from electronic-vibrational

27 Similar spectral line shape changes of FR3 are caused by the Frd

28 b and MGPPIXMb show no temperature-dependent spectral line shape changes suggestive of Jahn-Teller dy

29 folded polypeptide ligand, showed changes in spectral line shape consistent with restricted motion of

30 Finally, 2D spectral line shape evolution reveals that it takes the

31 om the electron paramagnetic resonance (EPR) spectral line shape of the reduced [2Fe-2S] cluster, whi

32 In wild-type E. coli QFR, HQNO causes EPR spectral line shape perturbations of the iron-sulfur clu

33 ch of the residues on SecB showed changes in spectral line shape upon addition of SecA.

34 significant inhomogenous contribution to the spectral line shape, which is quantified by simulations.

35 e followed, appearing as evolution of the 2D spectral line-shape during the first 200 fs after excita

36 The EPR spectral line shapes and the influence of nonpolar O2 or

37 lysis of the electron paramagnetic resonance spectral line shapes and the influence of O2 on the satu

38 The spectral line shapes are accurately reproduced using a H

39 urface facing the aqueous phase, and the EPR spectral line shapes at these sites indicate considerabl

40 (II) zero field splitting and broadening the spectral line shapes but had no effect on oxidized enzym

41 The dramatically different spectral line shapes for both aggregates are shown to ar

42 Furthermore, electron paramagnetic resonance spectral line shapes of sites in the N-terminal domain a

43 The spectral line shapes were analyzed as a function of side

44 Spectral line shapes were analyzed in terms of side-chai

45 des were analyzed on the basis of 31P and 2H spectral line shapes, order parameters, and T1 relaxatio

46 vast amount of information contained in the spectral line shapes, the problems with sensitivity and

47 none does not alter the [2Fe-2S] cluster EPR spectral line shapes, which remain indicative of one ubi

48 -PLB with CD3-Ala15 exhibit strong isotropic spectral line shapes.

49 Our studies show that the spectral line splits into distinctive spinon and holon e

50 ons and as a result, except for the lowfield spectral line, the remaining spectral lines of DMPO/ .SG

51 ver more than 80 days, red colour and narrow spectral lines, which seem inconsistent with those obser

52 Improvement of spectral line width from 4.8 Hz to 3.5 Hz was observed a

53 and experimental evidence suggests that the spectral line width is a result of multiple, discrete el

54 ibutions (sigma = 0.5-2%) are obtained whose spectral line widths are dominated (73-83%) by the intri

55 verse correlation was also found between the spectral line widths of coated SWCNTs and the efficiency

56 photoluminescence intensity and narrowing of spectral line widths with electrolyte addition, indicati

57 orporation of a capillary spinner to improve spectral line widths, and (3) facile sample changing via