1,607 research outputs found
Distribution of Si, Fe, and Ni in the Intracluster Medium of the Coma Cluster
We studied the distributions of Si, Fe, and Ni in the intracluster medium
(ICM) of the Coma cluster, one of the largest clusters in the nearby universe,
using XMM-Newton data up to 0.5 r180 and Suzaku data of the central region up
to 0.16 r180. Using the flux ratios of Ly alpha of H-like Si and 7.8 keV blend
to K alpha of He-like Fe, the abundance ratios of Si to Fe and Ni to Fe of the
ICM were derived using APEC model v2.0.1. The Si/Fe ratio in the ICM of the
Coma cluster shows no radial gradient. The emission weighted averages of the
Si/Fe ratio in the ICM within 0.0--0.2 r180, 0.2--0.5 r180, and 0.0--0.5 r180
are 0.97 +- 0.11, 1.05 +- 0.36 and 0.99 +- 0.13, respectively, in solar units
using the solar abundance of Lodders (2003). These values are close to those of
smaller clusters and groups of galaxies. Using the Suzaku data of the central
region, the derived Ni/Fe ratio of the ICM is 0.6--1.5 in solar units,
according to the same solar abundance table. The systematic difference in the
derived abundance ratios by different plasma codes are about 10%. Therefore,
for the ICM in the Coma cluster, the abundance pattern of Si, Fe, and Ni is
consistent with the same mixture of the yields of SN II and SN Ia in our
Galaxy. Within 0.5 r180}, the cumulative iron-mass-to-light ratio increases
with radius, and its radial profile is similar to those of relaxed smaller
clusters with cD galaxies at their center. Considering the observed Si/Fe
ratio, the cumulative metal-mass-to-light ratios at 0.5 r180 are compared with
theoretical expectations.Comment: 10 pages, 7 figures, accepted for publication in PAS
Prediction of Cross-Fitness for Adaptive Evolution to Different Environmental Conditions: Consequence of Phenotypic Dimensional Reduction
How adaptive evolution to one environmental stress improves or suppresses
adaptation to another is an important problem in evolutionary biology. For
instance, in microbiology, the evolution of bacteria to be resistant to
different antibiotics is a critical issue that has been investigated as
cross-resistance. In fact, recent experiments on bacteria have suggested that
the cross-resistance of their evolution to various stressful environments can
be predicted by the changes to their transcriptome upon application of stress.
However, there are no studies so far that explain a possible theoretical
relationship between cross-resistance and changes in the transcriptome, which
causes high-dimensional changes to cell phenotype. Here, we show that a
correlation exists between fitness change in stress tolerance evolution and
response to the environment, using a cellular model with a high-dimensional
phenotype and establishing the relationship theoretically. The present results
allow for the prediction of evolution from transcriptome information in
response to different stresses before evolution. The relevance of this to
microbiological evolution experiments is discussed.Comment: 17pages, 9figure
Spectrum-Free Estimation of Doppler Velocities Using Ultra-Wideband Radar
A method for estimating Doppler velocities using ultra-wideband radar data is presented. Unlike conventional time-frequency analysis, the proposed method can directly obtain Doppler velocities without searching for peaks in a spectrum. By exploiting closed-form solutions for the Doppler velocities, it avoids the trade-off between time and frequency resolution, thus maintaining high time resolution. Both simulations and measurements are used to evaluate the proposed method versus conventional techniques
Frontal Analysis Continuous Capillary Electrophoresis Study on the Interaction of an Amphiphilic Alternating Copolymer with Triton X-100
The interaction of amphiphilic alternating copolymers of sodium maleate and dodecyl vinyl ether (Mal/C12) with a nonionic surfactant, Triton X-100 (TX), was investigated by frontal analysis continuous capillary electrophoresis (FACCE). The binding isotherms obtained from FACCE data were indicative of weak cooperative interaction for all the polymers examined. The cooperative interaction was also analyzed by the Hill model, and the results were compared with the previous results on the interaction of statistical copolymers of sodium 2-acrylamido-2-methylpropanesulfonate and N-dodecylmethacrylamide with TX
Suzaku X-Ray Observations of the Accreting NGC 4839 Group of Galaxies and the Radio Relic in the Coma Cluster
Based on Suzaku X-ray observations, we study the hot gas around the NGC4839
group of galaxies and the radio relic in the outskirts of the Coma cluster. We
find a gradual decline in the gas temperature from 5 keV around NGC4839 to 3.6
keV at the radio relic, across which there is a further, steeper drop down to
1.5 keV. This drop as well as the observed surface brightness profile are
consistent with a shock with Mach number M = 2.2 pm 0.5 and velocity vs = (1410
pm 110) km s^-1. A lower limit of B > 0.33 mu G is derived on the magnetic
field strength around the relic from upper limits to inverse Compton X-ray
emission. Although this suggests that the non-thermal electrons responsible for
the relic are generated by diffusive shock acceleration (DSA), the relation
between the measured Mach number and the electron spectrum inferred from radio
observations are inconsistent with that expected from the simplest,
test-particle theory of DSA. Nevertheless, DSA is still viable if it is
initiated by the injection of a pre-existing population of non-thermal
electrons. Combined with previous measurements, the temperature profile of Coma
in the southwest direction is shallower outside NGC4839 and also slightly
shallower in the outermost region. The metal abundance around NGC4839 is
confirmed to be higher than in its vicinity, implying a significant peak in the
abundance profile that decreases to 0.2 solar toward the outskirts. We
interpret these facts as due to ram pressure stripping of metal-enriched gas
from NGC4839 as it falls into Coma. The relic shock may result from the
combined interaction of pre-existing intracluster gas, gas associated with NGC
4839, and cooler gas flowing in from the large-scale structure filament in the
southwest.Comment: 13 page, accepted for publication in Publications of the Astronomical
Society of Japa
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