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  • ASTRONOMY  (4)
  • Biochemistry and Biotechnology  (2)
  • 1990-1994  (5)
  • 1970-1974  (1)
  • 1950-1954
  • 1
    Electronic Resource
    Electronic Resource
    New York, NY [u.a.] : Wiley-Blackwell
    Biotechnology and Bioengineering 15 (1973), S. 377-393 
    ISSN: 0006-3592
    Keywords: Chemistry ; Biochemistry and Biotechnology
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Biology , Process Engineering, Biotechnology, Nutrition Technology
    Notes: A general mathematical model of the chemostat system is developed in order to define an experimental program of dynamic testing. A glucose-limited culture ofSaccharomyces cerevisiae was grown in a chemostat using chemically defined medium. The chemostat was perturbed from an initial steady state by changes in input glucose concentration, dilution rate, pH, and temperature. Dynamic responses of cell mass, glucose, cell number, RNA, and protein concentrations were measured. A number of simulation techniques were used in developing a dynamic mathematical model and in comparing the developed model with experimental data as well as the Monod model. The resulting model was found to be quantitatively accurate and superior to the Monod model. The developed model was interpreted in the light of cell physiology. Adjustment of intracellular RNA fraction was found to be rate limiting in acceleration of cell specific growth rate.
    Additional Material: 14 Ill.
    Type of Medium: Electronic Resource
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  • 2
    ISSN: 0173-0835
    Keywords: Chemistry ; Biochemistry and Biotechnology
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Biology , Chemistry and Pharmacology
    Notes: Lipoprotein(a) resembles low density lipoprotein in structure, except that a unique apolipoprotein (apo), apo(a), is linked to apo B-100. Variations in the number of sequence repeats in the apo(a) gene give rise to a range of isoforms. Depending on the method used, 6-30 apo(a) isoforms have been observed; however, the correspondence of these different isoforms has not been reported, making between-study comparisons difficult. In the present study we address this question by characterizing the apo(a) phenotypes of 48 sera using two previously reported separation methods, sodium dodecyl sulfate-polyacrylamide gel electrophoresis (SDS-PAGE, 3-12% gels) and SDS-agarose gel electrophoresis. In addition, the molecular weight of each isoform was estimated using haptoglobin 2-2 polymers as molecular weight standards. Among the 48 sera, 15 distinct apo(a) isoforms were separated by SDS-PAGE and 28 by SDS-agarose gel electrophoresis. There was excellent correlation between the two nomenclature systems (r = -0.97, p 〈 0.001, by rank correlation), and the ranges were totally overlapping, with the same two isoforms being identified as the largest and smallest by either method. The apparent molecular mass range for the isoforms was 294-624 kDa, which is in close agreement with the theoretical molecular mass range of 238-643 kDa, calculated from the sequence and carbohydrate content of recombinant apo(a). The disparity in number of isoforms between methods was expected, due to the poorer separation of apo(a) by SDS-PAGE; 3.1 ± 1.7 (median, 2.0) SDS-agarose isoforms were combined for each SDS-PAGE isoform. The present study demonstrates that the nomenclature systems for apo(a) isoforms separated by SDS-PAGE or by SDS-agarose gel electrophoresis are well correlated mathematically and encompass the same size range; however, the better resolution of SDS-agarose electrophoresis suggests that it is the method of choice for apo(a) phenotyping. As further apo(a) isoforms are identified, it will be important to address the question of a standardized nomenclature, in order to facilitate between-study comparisons.
    Additional Material: 3 Ill.
    Type of Medium: Electronic Resource
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  • 3
    Publication Date: 2011-08-24
    Description: Imaging spectrometer observations were made of the surface of the Moon during the December 1990 flyby of the Earth-Moon system by the Galileo spacecraft. This article documents this data set and presents analyses of some of the data. The near infrared mapping spectrometer (NIMS) investigation obtained 17 separate mosaics of the Moon in 408 spectral channels between about 0.7 and 5.2 micrometers. The instrument was originally designed to operate in orbit about Jupiter and therefore saturates at many spectral channels for most measurement situations at 1 AU. However, sufficient measurements were made of the Moon to verify the proper operation of the instrument and to demonstrate its capabilities. Analysis of these data show that the NIMS worked as expected and produced measurements consistent with previous ground-based telescopic studies. These are the first imaging spectrometer measurements of this type from space for the Moon, and they illustrate several major points concerning this type of observation and about the NIMS capabilities specifically. Of major importance are the difference between framing and scanning instruments and the effects of the spacecraft and the scan platform on the performance of such and experiment. The science return of subsequent NIMS and other investigation measurements will be significantly enhanced by the experience and results gained.
    Keywords: ASTRONOMY
    Type: Journal of Geophysical Research (ISSN 0148-0227); 99; E3; p. 5,587-5,600
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  • 4
    Publication Date: 2019-06-28
    Description: The IUE Ultraviolet Spectral Atlas of Selected Astronomical Objects (or 'the Atlas'), is based on the data that were available in the IUE archive in 1986, and is intended to be a quick reference for the ultraviolet spectra of many categories of astronomical objects. It shows reflected sunlight from the Moon, planets, and asteroids, and also shows emission from comets. Comprehensive compilations of UV spectra for main sequence, subgiant, giant, bright giant, and supergiant stars are published elsewhere. This Atlas contains the spectra for objects occupying other areas of the Hertzsprung-Russell diagram: pre-main sequence stars, chemically peculiar stars, pulsating variables, subluminous stars, and Wolf-Rayet stars. This Atlas also presents phenomena such as the chromospheric and transition region emissions from late-type stars; composite spectra of stars, gas streams, accretion disks and gas envelopes of binary systems; the behavior of gas ejecta shortly after the outburst of novac and supernovac; and the H II regions, planetary nebulae, and supernova remnants. Population 2 stars, globular clusters, and luminous stars in the Magellanic Clouds, M31, and M33, are also included in this publication. Finally, the Atlas gives the ultraviolet spectra of galaxies of different Hubble types and of active galaxies.
    Keywords: ASTRONOMY
    Type: NASA-RP-1285 , NAS 1.61:1285 , REPT-92B00114
    Format: application/pdf
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  • 5
    Publication Date: 2019-07-27
    Description: Results are presented from observations, made with the SWP spectrograph at low resolution, of Tc-deficient S and C members of the group of chemically peculiar red giant (PRG) stars, which were carried out to search for possible companions to these stars. The results support the hypothesis of Little et al. (1987) and Smith and Lambert (1987, 1988) that the chemical peculiarities of T-deficient S and MS PRG stars have arisen due to mass transfer from white dwarf companions.
    Keywords: ASTRONOMY
    Type: International Colloquium; Sept. 4-7, 1989; Montpellier; France
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  • 6
    Publication Date: 2019-08-28
    Description: This paper describes the collection, reduction, and analysis of 0.4-1.0-micron Mars imaging spectroscopy data obtained during the 1988 and 1990 oppositions from Mauna Kea Observatory and provides a general outline for the acquisition and analysis of similar imaging spectroscopy data sets. The U.H. 2.24-m Wide Field Grism CCD Spectrograph was used to collect 13 3D image cubes covering 90 percent of the planet south of 50 deg N in the 0.4-0.8 micron region and covering 55 percent of the planet south of 50 deg N in the 0.5-1.0 micron region. Spectra extracted from these image cubes reveal the detailed character of the Martian near-UV to visible spectrum. Images at red wavelengths reveal the 'classical' albedo markings at 100-500 km spatial resolution while images at blue wavelengths show little surface feature contrast and are dominated by condensate clouds/hazes and polar ice.
    Keywords: ASTRONOMY
    Type: Experimental Astronomy (ISSN 0922-6435); 2; 5; p. 287-306.
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