Probing the Ser-Ser-Lys Catalytic Triad Mechanism of Peptide Amidase:  Computational Studies of the Ground State, Transition State, and Intermediate†

Biochemistry ◽  
2004 ◽  
Vol 43 (50) ◽  
pp. 15657-15672 ◽  
Author(s):  
Anna Liza B. Valiña ◽  
Devleena Mazumder-Shivakumar ◽  
Thomas C. Bruice
2018 ◽  
Vol 98 (4) ◽  
Author(s):  
D. Studer ◽  
L. Maske ◽  
P. Windpassinger ◽  
K. Wendt

2019 ◽  
Vol 100 (6) ◽  
Author(s):  
O. S. Kirsebom ◽  
M. Hukkanen ◽  
A. Kankainen ◽  
W. H. Trzaska ◽  
D. F. Strömberg ◽  
...  

2016 ◽  
Vol 94 (1) ◽  
Author(s):  
N. Cieplicka-Oryńczak ◽  
B. Szpak ◽  
S. Leoni ◽  
B. Fornal ◽  
D. Bazzacco ◽  
...  

2007 ◽  
Vol 90 (13) ◽  
pp. 131905 ◽  
Author(s):  
R. Kudrawiec ◽  
S. R. Bank ◽  
H. B. Yuen ◽  
H. Bae ◽  
M. A. Wistey ◽  
...  

1964 ◽  
Vol 42 (6) ◽  
pp. 1311-1323 ◽  
Author(s):  
M. A. Eswaran ◽  
C. Broude

Lifetime measurements have been made by the Doppler-shift attenuation method for the 1.98-, 3.63-, 3.92-, and 4.45-Mev states in O18 and the 1.28-, 3.34-, and 4.47-Mev states in Ne22, excited by the reactions Li7(C12, pγ)O18 and Li7(O16, pγ)Ne22. Branching ratios have also been measured. The results are tabulated.[Formula: see text]The decay of the 3.92-Mev state in O18 is 93.5% to the 1.98-Mev state and 6.5% to the ground state and of the 4.45-Mev state 74% to the 3.63-Mev state, 26% to the 1.98-Mev state, and less than 2% to the ground state. In Ne22, the ground-state transition from the 4.47-Mev state is less than 2% of the decay to the first excited state.


1966 ◽  
Vol 145 (3) ◽  
pp. 982-987 ◽  
Author(s):  
E. J. Dowdy ◽  
J. A. McIntyre

1978 ◽  
Vol 77 ◽  
pp. 131-137
Author(s):  
J.B. Whiteoak

The observation in 1965 of absorption due to the 18 cm ground-state transition of OH in the direction of Cas A (Weinreb et al., 1963) marked the first occasion on which a molecular cloud was detected at radio wavelengths. However, it was not until the later discovery of high-intensity OH emission (Weaver et al., 1965) that attention turned to nearby galaxies. Unfortunately, searches for OH emission in the Magellanic Clouds (McGee et al., 1965; Radhakrishnan, 1967) and in more distant galaxies (Roberts, 1967) were unsuccessful. The first detection of an OH transition, in absorption against the radio continuum of NGC 253 and 3034 (Weliachew, 1971), went almost unnoticed because the results were unconvincing. However, Whiteoak and Gardner (1973) and Nguyen-Q-Rieu et al. (1976) confirmed the existence of the absorption.


Sign in / Sign up

Export Citation Format

Share Document