Design of novel bioactive materials through organic modification of calcium silicate

Bioactive ceramics have attractive feature for bone repair such as direct bone-bonding in the body. However their clinical application is limited to low loaded portions due to their inappropriate mechanical performances such as higher brittleness and lower flexibility than natural bone. The essential condition for artificial materials to show bioactivity is formation of bone-like apatite on their surfaces in body environment. This apatite formation is triggered by silanol (Si–OH) group on the material surfaces and release of Ca2+. These findings bring us an idea that novel bioactive materials with high flexibility can be designed by organic modification of calcium silicate. We synthesized organic–inorganic hybrids from organic polymers including 2-hydroxyethylmethacrylate (HEMA), starch and alginate by modification with alkoxysilane and calcium chloride. The hybrids formed apatite on their surfaces in simulated body fluid (SBF, Kokubo solution). Such a modification was also effective for providing conventional polymethylmethacrylate (PMMA)-based bone cement with bioactivity.IX Conference and Exhibition of the European Ceramic Society: June 19-23, 2005, Portorož, Sloveni

A comparative profile of urinary scent signals of two endangered Japanese populations of leopard cat

Two subspecies of mainland leopard cats (Prionailurus bengalensis), Iriomote cats (Prionailurus bengalensis iriomotensis), and Tsushima leopard cats (Prionailurus bengalensis euptilurus), are small, endangered felids that are endemic to the Japanese islands, Iriomote-jima and Tsushima, respectively. Both subspecies have an estimated population size of only about 100 individuals each. Therefore, it is crucial to expand our understanding of these subspecies to successfully conserve them. While their morphology, anatomy, ecology, pathology, and genetics are well studied, little is known about their physiology regulated in subspecies-specific manners. This study characterized their urinary volatile and nonvolatile organic compounds, with which individuals express their physiological status and territorial ownership. We found significantly higher levels of 3-mercapto-3-methyl-1-butanol and its structural analogs, which are scent signals of domestic cats, in the urinary headspace of Iriomote cats than in that of Tsushima leopard cats. There were no differences in the urinary levels of felinine, an amino acid that acts as a precursor of 3-mercapto-3-methyl-1-butanol, suggesting the variation of catalytic activities for decomposing felinine to 3-mercapto-3-methyl-1-butanol between subspecies. Both subspecies exhibited physiological proteinuria due to the secretion of carboxylesterase 5A, also known as cauxin, for the production of felinine. In conclusion, while the two endangered Japanese subspecies of mainland leopard cats share similar genetic backgrounds, urinary contents of metabolites vary between the subspecies. We suggest that after the separation into two subspecies, the regulation of the metabolic pathway for 3-mercapto-3-methyl-1-butanol production likely evolved differently in each subspecies in response to their specific environments

A star-bursting proto-cluster in making associated to a radio galaxy at z=2.53 discovered by H_alpha imaging

We report a discovery of a proto-cluster in vigorous assembly and hosting strong star forming activities, associated to a radio galaxy USS 1558-003 at z=2.53, as traced by a wide-field narrow-band H_alpha imaging with MOIRCS on Subaru Telescope. We find 68 H_alpha emitters with dust-uncorrected SFRs down to 8.6 Msun/yr. Their spatial distribution indicates that there are three prominent clumps of H_alpha emitters, one surrounding the radio galaxy and another located at ~1.5 Mpc away to the south-west, and the other located in between the two. These contiguous three systems are very likely to merge together in the near future and may grow to a single more massive cluster at later times. Whilst most H_alpha emitters reside in the "blue cloud" on the color--magnitude diagram, some emitters have very red colors with J-Ks>1.38(AB). Interestingly, such red H_alpha emitters are located towards the faint end of the red sequence, and they tend to be located in the high density clumps. We do not see any statistically significant difference in the distributions of individual star formation rates or stellar masses of the H_alpha emitters between the dense clumps and the other regions, suggesting that this is one of the notable sites where the progenitors of massive galaxies in the present-day clusters were in their vigorous formation phase. Finally, we find that H_alpha emission of the radio galaxy is fairly extended spatially over ~4.5 arcsec. However it is not as widespread as its Lya halo, meaning that the Lya emission is indeed severely extended by resonant scattering.Comment: 14 pages, 11 figures, 3 tables, accepted for publication in Ap

Factors responsible for elevated plasma B-type natriuretic peptide levels in severe aortic stenosis: Comparison between elderly and younger patients

AbstractBackgroundElevated plasma B-type natriuretic peptide (BNP) is a predictor of outcome and helpful for risk stratification in aortic stenosis (AS). However, left ventricular (LV) diastolic dysfunction progresses with aging and may also influence plasma BNP levels in elderly patients. We hypothesized that plasma BNP levels may be influenced by age in severe AS, and that factors that affect the elevation of plasma BNP levels may be different between elderly and younger patients with AS.MethodsWe performed echocardiography in 341 patients with severe AS [aortic valve area (AVA)<1.0cm2] and classified them into two groups by age (elderly ≥75 years old, n=201; younger patients <75 years old, n=140). We used multivariate linear regression analysis to assess the factors that determine plasma BNP levels in both groups.ResultsAge was found to be one of the independent determinants of plasma BNP levels in all patients (β=0.135, p=0.005). Although AVA was similar in the two groups, plasma BNP levels and E/e′ were significantly higher in elderly than younger patients [133.0 (IQR, 73.3–329.7)pg/dl vs 92.8 (IQR, 40.6–171.8)pg/dl, p<0.01; 20±8 vs 16±6, p<0.01, respectively). In multivariate stepwise linear regression analysis, AVA index, LV ejection fraction, mass index, E/e′, estimated systolic pulmonary artery pressure (eSPAS), and the presence of atrial fibrillation were independent determinants of plasma BNP levels in younger patients. In contrast, the independent determinants of plasma BNP levels in elderly patients were LV ejection fraction, mass index, E/e′, eSPAS, the presence of atrial fibrillation, age, and hemoglobin levels, but not AVA index.ConclusionsThere may be differences in the factors that influence plasma BNP levels between elderly and younger patients with severe AS. In elderly patients, plasma BNP levels may be influenced more by these factors than AS severity compared with younger patients

A Census of Star-Forming Galaxies at z = 1-3 in the Subaru Deep Field

Several UV and near-infrared color selection methods have identified galaxies at z = 1-3. Since each method suffers from selection biases, we have applied three leading techniques (Lyman break, BX/BM, and BzK selection) simultaneously in the Subaru Deep Field. This field has reliable ({\Delta}z/(1 + z) = 0.02--0.09) photometric redshifts for ~53,000 galaxies from 20 bands (1500{\AA}--2.2{\mu}m). The BzK, LBG, and BX/BM samples suffer contamination from z<1 interlopers of 6%, 8%, and 20%, respectively. Around the redshifts where it is most sensitive (z~1.9 for star-forming BzK, z~1.8 for z~2 LBGs, z~1.6 for BM, and z~2.3 for BX), each technique finds 60-80% of the census of the three methods. In addition, each of the color techniques shares 75-96% of its galaxies with another method, which is consistent with previous studies that adopt identical criteria on magnitudes and colors. Combining the three samples gives a comprehensive census that includes ~90% of z-phot = 1-3 galaxies, using standard magnitude limits similar to previous studies. In fact, we find that among z = 1-2.5 galaxies in the color selection census, 81-90% of them can be selected by just combining the BzK selection with one of the UV techniques (z~2 LBG or BX and BM). The average galaxy stellar mass, reddening and SFRs all decrease systematically from the sBzK population to the LBGs, and to the BX/BMs. The combined color selections yield a total cosmic SFR density of 0.18 $\pm$ 0.03 M_sun yr^{-1} Mpc^{-3} for K_AB <= 24. We find that 65% of the star formation is in galaxies with E(B-V) > 0.25 mag, even though they are only one-fourth of the census by number.Comment: 26 pages, 30 figures, 9 tables, emulateapj format. Modified to match the final ApJ versio

High star formation activity in the central region of a distant cluster at z=1.46

We present an unbiased deep [OII] emission survey of a cluster XMMXCS J2215.9-1738 at z=1.46, the most distant cluster to date with a detection of extended X-ray emission. With wide-field optical and near-infrared cameras (Suprime-Cam and MOIRCS, respectively) on Subaru telescope, we performed deep imaging with a narrow-band filter NB912 (lambda_c=9139A, Delta_lambda=134A) as well as broad-band filters (B, z', J and Ks). From the photometric catalogues, we have identified 44 [OII] emitters in the cluster central region of 6'x6' down to a dust-free star formation rate of 2.6 Msun/yr (3 sigma). Interestingly, it is found that there are many [OII] emitters even in the central high density region. In fact, the fraction of [OII] emitters to the cluster members as well as their star formation rates and equivalent widths stay almost constant with decreasing cluster-centric distance up to the cluster core. Unlike clusters at lower redshifts (z<1) where star formation activity is mostly quenched in their central regions, this higher redshift 2215 cluster shows its high star formation activity even at its centre, suggesting that we are beginning to enter the formation epoch of some galaxies in the cluster core eventually. Moreover, we find a deficit of galaxies on the red sequence at magnitudes fainter than ~M*+0.5 on the colour-magnitude diagram. This break magnitude is brighter than that of lower redshift clusters, and it is likely that we are seeing the formation phase of more massive red galaxies in the cluster core at z~1. These results may indicate inside-out and down-sizing propagation of star formation activity in the course of cluster evolution.Comment: 12 pages, 9 figures, 1 table, accepted for publication in MNRA

The characteristic response of domestic cats to plant iridoids allows them to gain chemical defense against mosquitoes

ネコのマタタビ反応の謎を解明 --マタタビ反応はネコが蚊を忌避するための行動だった--. 京都大学プレスリリース. 2021-01-21.Domestic cats and other felids rub their faces and heads against catnip (Nepeta cataria) and silver vine (Actinidia polygama) and roll on the ground as a characteristic response. While this response is well known, its biological function and underlying mechanism remain undetermined. Here, we uncover the neurophysiological mechanism and functional outcome of this feline response. We found that the iridoid nepetalactol is the major component of silver vine that elicits this potent response in cats and other felids. Nepetalactol increased plasma β-endorphin levels in cats, while pharmacological inhibition of μ-opioid receptors suppressed the classic rubbing response. Rubbing behavior transfers nepetalactol onto the faces and heads of respondents where it repels the mosquito, Aedes albopictus. Thus, self-anointing behavior helps to protect cats against mosquito bites. The characteristic response of cats to nepetalactol via the μ-opioid system provides an important example of chemical pest defense using plant metabolites in nonhuman mammals