S U M M A R YL-Asparaginase and L-glutaminase activities were detected in many microorganisms and the distribution of these activities was found to be related to the classification of micro-organisms.Among 464 bacteria, the activities occurred in many Gram-negative bacteria and in a few Gram-positive bacteria. Most members of the family Enterobacteriaceae possessed L-asparaginase. L-Asparaginase and L-glutaminase occurred together in a large proportion of pseudomonads. Among Gram-positive bacteria many strains of Bacillus pumilus showed strong L-asparaginase activity. Amidase activities were also observed in several strains in other families.L-Asparaginase activity was not detected in culture filtrates of 261 strains of species of the genera Streptomyces and Nocardia, but L-asparaginase and Lglutaminase were detected when these organisms were sonicated.The amidase activities in culture filtrates of 4158 fungal strains were tested. All the strains of Fusarium species formed L-asparaginase. Organisms of the genera Hjyomyces and Nectria, which are regarded as the perfect stage of the genus Fusarium, also formed L-asparaginase. Several Penicillium species formed L-asparaginase. Two organisms of the family Moniliaceae formed L-glutaminase together with L-asparaginase, and a few ascomycetous fungi formed L-asparaginase or L-glutaminase.Among I 326 yeasts, L-asparaginase or L-glutaminase occurred frequently in certain serological groups of yeasts : VI (Hansenula) group, Cryptococcus group and Rhodotorula group. Many strains of Sporobolomyces species also showed L-asparaginase activity. Several strains of Cryptococcus and Rhodotorula group possessed L-glutaminase and L-asparaginase. L-Glutaminase alone was formed in many strains of Candida scottii and Cryptococcus albidus, both of which are related to Basidiomycetes.
The activities of various types of antiulcer agents against Helicobacter pylori (formerly called Campylobacter pylon) strains were determined by an agar dilution method. Among the compounds tested, two benzimidazole proton pump inhibitors, lansoprazole (AG-1749) and omeprazole, were found to have significant activities against this organism. The activity of lansoprazole was comparable to that of bismuth citrate, with MICs ranging from 3.13 to 12.5 ,ug/ml, and fourfold more potent than that of omeprazole. A major metabolite and two acid-converted rearrangement products of lansoprazole also exhibited good activities comparable or superior to that of the parent compound. Exposure to lansoprazole of H. pylori growing in a liquid medium led to an extensive loss of viability without a reduction in culture turbidity and produced an aberrant bacterial morphology characterized by the irregular constriction of cells and the collapse of cell surface structures. The antibacterial activity of lansoprazole and its related compounds was selective against H. pylori; common aerobic and anaerobic bacteria and Campylobacterjejuni were not inhibited by 100 ,ug/ml.
Context. The radio quasar 3C 454.3 underwent an exceptional optical outburst lasting more than 1 year and culminating in spring 2005. The maximum brightness detected was R = 12.0, which represents the most luminous quasar state thus far observed (M B ∼ −31.4). Aims. In order to follow the emission behaviour of the source in detail, a large multiwavelength campaign was organized by the Whole Earth Blazar Telescope (WEBT). Methods. Continuous optical, near-IR and radio monitoring was performed in several bands. ToO pointings by the Chandra and INTEGRAL satellites provided additional information at high energies in May 2005. Results. The historical radio and optical light curves show different behaviours. Until about 2001.0 only moderate variability was present in the optical regime, while prominent and long-lasting radio outbursts were visible at the various radio frequencies, with higher-frequency variations preceding the lower-frequency ones. After that date, the optical activity increased and the radio flux is less variable. This suggests that the optical and radio emissions come from two separate and misaligned jet regions, with the inner optical one acquiring a smaller viewing angle during the 2004−2005 outburst. Moreover, the colour-index behaviour (generally redder-when-brighter) during the outburst suggests the presence of a luminous accretion disc. A huge mm outburst followed the optical one, peaking in June−July 2005. The high-frequency (37−43 GHz) radio flux started to increase in early 2005 and reached a maximum at the end of our observing period (end of September 2005). VLBA observations at 43 GHz during the summer confirm the brightening of the radio core and show an increasing polarization. An exceptionally bright X-ray state was detected in May 2005, corresponding to the rising mm flux and suggesting an inverse-Compton nature of the hard X-ray spectrum. Conclusions. A further multifrequency monitoring effort is needed to follow the next phases of this unprecedented event.
We systematically surveyed period variations of superhumps in SU UMa-type dwarf novae based on newly obtained data and past publications. In many systems, the evolution of the superhump period is found to be composed of three distinct stages: an early evolutionary stage with a longer superhump period, a middle stage with systematically varying periods, and a final stage with a shorter, stable superhump period. During the middle stage, many systems with superhump periods of less than 0.08 d show positive period derivatives. We present observational characteristics of these stages and give greatly improved statistics. Contrary to an earlier claim, we found no clear evidence for a variation of period derivatives among different superoutbursts of the same object. We present an interpretation that the lengthening of the superhump period is a result of the outward propagation of an eccentricity wave, which is limited by the radius near the tidal truncation. We interpret that late-stage superhumps are rejuvenated excitation of a 3:1 resonance when superhumps in the outer disk are effectively quenched. The general behavior of the period variation, particularly in systems with short orbital periods, appears to follow a scenario proposed in Kato, Maehara, and Monard (2008, PASJ, 60, L23). We also present an observational summary of WZ Sge-type dwarf novae. Many of them have shown long-enduring superhumps during a post-superoutburst stage having longer periods than those during the main superoutburst. The period derivatives in WZ Sge-type dwarf novae are found to be strongly correlated with the fractional superhump excess, or consequently with the mass ratio. WZ Sge-type dwarf novae with a long-lasting rebrightening or with multiple rebrightenings tend to have smaller period derivatives, and are excellent candidates for those systems around or after the period minimum of evolution of cataclysmic variables.
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