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Forty years ago, it was proposed that gas-phase organic chemistry in the interstellar medium can be initiated by the methyl cation CH3+(refs. 1–3), but so far it has not been observed outside the Solar System4,5. Alternative routes involving processes on grain surfaces have been invoked6,7. Here we report James Webb Space Telescope observations of CH3+in a protoplanetary disk in the Orion star-forming region. We find that gas-phase organic chemistry is activated by ultraviolet irradiation.

In this randomized, double-blind, placebo-controlled study, we investigated the effects of collagen peptides (CP) containing high concentrations of prolyl-hydroxyproline and hydroxyprolyl-glycine on advanced glycation end products (AGEs) levels in the skin and subcutaneous blood vessel walls. A total of 31 individuals aged 47-87 years were randomly assigned to receive either 5 g/day of fish-derived CP or a placebo for 12 weeks. Body and blood compositions and AGEs levels were measured at the beginning and end of the study. No adverse events were observed, and both groups’ blood and body compositions did not change significantly. However, the CP group had significantly lower AGEs levels and a slightly lower insulin resistance index (homeostasis model assessment ratio [HOMA-R]) than the placebo group. In addition, the percentage changes in AGEs and HOMA-R levels were positively and strongly correlated in both groups. These findings suggest that fish-derived CP may be effective in reducing AGEs levels and improving insulin resistance.Graphical AbstractIngestion of a collagen peptide containing high concentrations of prolyl-hydroxyproline and hydroxyprolyl-glycine reduces advanced glycation end products levels in the skin and subcutaneous blood vessel walls: a randomized, double-blind, placebo-controlled study.

Backgrounds: One-leg standing time (OLST) has been frequently used physical performance measure; however, what muscular characteristics OLST represents remains uncertain. Aim: This cross-sectional study aimed to investigate the association between OLST and muscle characteristics to clarify the possibility of using OLST as a physical performance measure. Methods: Study participants comprised 1144 older adults aged 65 years or older. Computed tomography images provided mid-thigh skeletal muscle cross-sectional area and mean attenuation value. OLST was measured for a maximum of 60 s. Static postural instability was assessed using a posturography. Results: A frequency of OLST < 20 s was increased by quartiles of muscle cross-sectional area (Q1: 33.6, Q2: 12.8, Q3: 13.6, Q4: 11.9%, P< 0.001) and mean attenuation value (Q1: 32.3, Q2: 21.7, Q3: 14.3, Q4: 7.7%, P< 0.001). Results of the multinomial regression analysis indicated that muscle cross-sectional area and mean attenuation value were independently associated with an OLST of less than 20 s. The crude odds ratio of OLST less than 20 s for the lowest quartiles of both cross-sectional area and mean attenuation value was 4.19 (95% CI: 3.01 − 5.84). The cross-sectional area of muscles with greater fat deposition was inversely associated with OLST, while that with smaller fat deposition showed a positive association with OLST, indicating why mean attenuation value and cross-sectional area were independently associated with OLST. No clear relationship was observed with static postural instability. Conclusion: OLST was a simply measurable quantifiable physical measure representing the loss of muscle mass and quality in older adults.

Nonalcoholic fatty liver disease often progresses to cirrhosis and causes liver cancer, but mechanisms of its progression are yet to be elucidated. Although nonalcoholic fatty liver disease is often associated with abnormal portal circulation, there have not been any experimental studies to test its pathogenic role. Here, whether decreased portal circulation affected the pathology of nonalcoholic steatohepatitis (NASH) was examined using congenital portosystemic shunt (PSS) in C57BL/6J mice. Whereas PSS significantly attenuated free radical–mediated carbon tetrachloride injury, it augmented pericellular fibrosis in the centrilobular area induced by a 0.1% methionine choline-deficient l-amino acid–defined high-fat diet (CDAHFD). PSS aggravated ductular reaction and increased the expression of connective tissue growth factor. Pimonidazole immunohistochemistry of the liver revealed that the centrilobular area of PSS-harboring mice was more hypoxic than that of control mice. Although tissue hypoxia was observed in the fibrotic area in CDAHFD-induced NASH in both control and PSS-harboring mice, it was more profound in the latter, which was associated with higher carbonic anhydrase 9 and vascular endothelial growth factor expression and neovascularization in the fibrotic area. Furthermore, partial ligation of the portal vein also augmented pericellular fibrosis and ductular reaction induced by a CDAHFD. These results demonstrate that decreased portal circulation, which induces hypoxia due to disrupted intralobular perfusion, is an important aggravating factor of liver fibrosis in NASH.

Activation of the phosphoinositide 3-kinase–AKT, Yes-associated protein (YAP), and MYC pathways is involved in human liver cancers, including hepatocellular carcinoma (HCC) and cholangiocarcinoma (CC). However, the nature of the interactions among these pathways has remained poorly understood. Herein, we demonstrate the coordination of these pathways during the formation of mouse liver tumors induced by hepatocyte-specific somatic integration of myristoylated AKT, mutant YAP, Myc, or their combinations. Although the introduction of YAP or Myc alone was inefficient in inducing tumors, these proteins accelerated tumorigenesis induced by AKT. The generated tumors demonstrated various histological features: low-grade HCC by AKT/Myc, CC by AKT/YAP, and high-grade HCC by AKT/Myc/YAP. CC induced by AKT/YAP was associated with activation of the Notch pathway. Interestingly, the combination of Myc and YAP generated tumors composed of hepatoblast/stem-like cells expressing mRNA for Afp, Dlk1, Nanog, and Sox2and occasionally forming immature ducts. Finally, immunohistochemical analysis revealed that human HCC and CC were predominantly associated with phosphorylation of S6 and glycogen synthase kinase-3β, respectively, and >60% of CC cases were positive for both phosphorylated glycogen synthase kinase--3β and YAP. Our study suggests that hepatocyte-derived tumors demonstrate a wide spectrum of tumor phenotypes, including HCC, CC, and hepatoblastoma-like, through the combinatory effects of the oncogenic pathways and that the state of the phosphoinositide 3-kinase–AKT pathway is a key determinant of differentiation.

Supplemental Digital Content is available in the text.Liver fibrosis is one of the common complications of transient myeloproliferative disorder (TMD) in Down syndrome (DS), but the exact molecular pathogenesis is largely unknown. We herein report a neonate of DS with liver fibrosis associated with TMD, in which we performed the serial profibrogenic cytokines analyses. We found the active monocyte chemoattractant protein-1 expression in the affected liver tissue and also found that both serum and urinary monocyte chemoattractant protein-1 concentrations are noninvasive biomarkers of liver fibrosis. We also showed a prospective of the future anticytokine therapy with herbal medicine for the liver fibrosis associated with TMD in DS.

AbstractWe examined whether baPWV could be affected by pork collagen peptide (CP) ingestion. Seventy subjects were randomized into two groups (2.5 g/day CP and 2.5 g/day placebo). A significant reduction in baPWV was observed in the CP group compared to the placebo group. This study demonstrated that pork CP may contribute to the prevention of atherosclerosis in elderly.

Asymptomatic cerebral small-vessel disease (cSVD) in elderly individuals are potent risk factors for stroke. In addition to common clinical risk factors, postural instability has been postulated to be associated with cSVD in older frail patients. Here, we conducted a cross-sectional study to understand the possible link between postural instability and asymptomatic cSVD further, namely periventricular hyperintensity, lacunar infarction, and microbleeds, as well as cognitive function, in a middle-aged to elderly general population (n=1387).

Arterial stiffness, a risk factor of brain small vessel diseases (SVD), causes hemodynamic changes. Mechanical stresses, circumferential wall tension (WT), and shear stress (SS) may change with arterial stiffness and be related to SVD. We investigated the associations between mechanical stresses and arterial stiffness and SVD.

Mature hepatocytes are suggested to possess a capacity for bile ductular transdifferentiation, but whether and how hepatocytes contribute to ductular reaction in chronic liver diseases has not been elucidated. We examined whether mouse hepatocytes can transdifferentiate into bile ductular cells in vitro, using a three-dimensional collagen gel culture method, and in vivo, using a liver repopulation model in which β-galactosidase–positive hepatocytes from Alb-Cre × ROSA26R mice were transplanted into the liver of wild-type mice. We further examined the relative contribution of intrinsic hepatocytes in ductular reaction in a hepatocyte lineage–tracing model using Mx1-Cre × ROSA26R mice treated with polyinosinic–polycytidylic acid. Within collagen gels, hepatocytes exhibited branching morphogenesis associated with the emergence of bile duct–like phenotype. In the liver repopulation model, many β-galactosidase–positive, hepatocyte-derived bile ductular structures were identified; these markedly increased after liver injury. In Mx1-Cre × ROSA26R mice, relatively minor but significant contributions of hepatocyte-derived bile ductules were observed in both periportal and centrilobular ductular reaction. As the centrilobular ductular reaction progressed, the portal ducts or ductules migrated toward the injured area and joined with hepatocyte-derived ductules, leaving the portal tract without biliary structures. We conclude that hepatocytes and bile ducts or ductules are important sources of ductular reaction and that the intrahepatic biliary system undergoes remarkable remodeling in response to chronic liver injury.

Osteoporosis and atherosclerosis are the two most common diseases in postmenopausal women. In most cases, they are simultaneously present in the same individual and commonly lead to bone fracture or cardiovascular disease (CVD). Bisphosphonates (BPs) are frequently used in the treatment of osteoporosis and have the ability to increase lumbar spine bone mineral density (L-BMD). BPs may also protect against CVD. A single monthly 50-mg dose of minodronate (monthly minodronate) is now common practice and is highly anticipated to reduce the incidence of both bone fracture and CVD. A useful approach to independently predicting CVD is brachial-ankle pulse wave velocity (baPWV). Here, we directly compared the effects of monthly minodronate with those of a standard single weekly 35-mg dose of alendronate (weekly alendronate) on L-BMD and baPWV in postmenopausal women with osteoporosis across a 12-month period.

Increasing blood pressure (BP) variability is reported to be a cardiovascular risk factor. However, the clinical implications of postprandial hypotension (PHYPO), a commonly observed BP variability in elderly persons, are poorly understood. Here, we investigated the possible associations between postprandial BP decline and asymptomatic cerebral damage in community residents.

Although hepatocyte transplantation (HCTx) is expected to become a useful therapy for human liver diseases, allogenic hepatocytes still tend to be rejected within a short period due to host immunosurveillance. In the present study, we investigated the effect of prior bone marrow transplantation (BMTx) for the engraftment of allogenic hepatocytes using the analbuminemic rat transplantation model. The hepatocytes of Lewis (LEW) rats were not accepted in the liver of retrorsine (RS)/partial hepatectomy (PH)-treated analbuminemic F344 (F344-alb) rats, which express the disparate major histocompatibility complex (MHC) against that of LEW rats. Prior BMTx with the LEW bone marrow cells (BMCs) after sublethal irradiation achieved acceptance and repopulation of LEW hepatocytes in the liver of the RS/PH-treated F344-alb rats, associated with elevation of serum albumin. The replacement of hepatic parenchyma with albumin positive (Alb+) donor hepatocytes and elevation of serum albumin levels were dependent on the bone marrow reconstitution by donor BMCs, which was more efficiently achieved by intrabone marrow (IBM)-BMTx than by intravenous (IV)-BMTx. Our results demonstrate that efficient bone marrow reconstitution by IBM-BMTx enables the replacement of the hepatic parenchyma with allogenic hepatocytes in RS/PH-treated analbuminemic rats without immunosuppressants.

We present a distribution map of the far-infrared [O III] 88 $\mu$m line emission around the 30 Doradus (30 Dor) region in the Large Magellanic Cloud obtained with the Fourier Transform Spectrometer of the Far-Infrared Surveyor on board AKARI. The map reveals that the [O III] emission is widely distributed by more than 10$'$around the super star cluster R 136, implying that the 30 Dor region is affluent with interstellar radiation field that is hard enough to ionize O$^{2+}$. The observed [O III] line intensities are as high as (1–2) $\times$10$^{-6}$W m$^{-2}$sr$^{-1}$on the peripheral regions 4$'$–5$'$away from the center of 30 Dor, which requires gas densities of 60–100 cm$^{-3}$. However, the observed size of the distribution of the [O III] emission is too large to be explained by massive stars in the 30 Dor region enshrouded by clouds with a constant gas density of 10$^{2}$cm$^{-3}$. Therefore, the surrounding structure is likely to be highly clumpy. We also find a global correlation between the [O III] and the far-infrared continuum emission, suggesting that the gas and dust are well mixed in the highly ionized region where the dust survives in clumpy dense clouds shielded from energetic photons.

The Far-Infrared Surveyor (FIS) onboard the AKARI satellite has a spectroscopic capability provided by a Fourier transform spectrometer (FIS–FTS). FIS–FTS is the first space-borne imaging FTS dedicated to far-infrared astronomical observations. We describe the calibration process of the FIS–FTS, and discuss its accuracy and reliability. The calibration is based on observational data of bright astronomical sources as well as two instrumental sources. We have compared the FIS–FTS spectra with the spectra obtained from the Long Wavelength Spectrometer (LWS) of the Infrared Space Observatory (ISO), having a similar spectral coverage. The present calibration method accurately reproduces the spectra of several solar system objects having a reliable spectral model. Under this condition the relative uncertainty of the calibration of the continuum is estimated to be $\pm$15% for SW, $\pm$10% for 70–85 cm$^{-1}$of LW, and $\pm$20% for 60–70 cm$^{-1}$of LW; and the absolute uncertainty is estimated to be $+$35%/$-$55% for SW, $+$35%/$-$55% for 70–85 cm$^{-1}$of LW, and $+$40%/$-$60% for 60–70 cm$^{-1}$of LW. These values have been confirmed by comparisons with theoretical models and previous observations by the ISO / LWS.

We have observed the Quintuplet- and Arches-cluster regions with the Fourier Transform Spectrometer (FTS) of the Far-Infrared Surveyor (FIS) aboard AKARI to investigate the physical conditions of interstellar matter around the clusters. The FIS-FTS mapping data reveal differences in the spatial distribution among the far-infrared [O iii], [N ii], and [C ii] line emissions near the Arches cluster; the emission of an ionic line with a higher ionization potential is distributed closer to the Arches cluster. This clearly indicates that UV photons from the Arches cluster are ionizing the surface of nearby molecular clouds, and penetrating deeper to dissociate the cloud. We have estimated the effective temperature of the Arches cluster to be about 34000 K from the ratio of the [O iii]$/$[N ii] lines.

Massive stars disrupt their natal molecular cloud material through radiative and mechanical feedback processes. These processes have profound effects on the evolution of interstellar matter in our Galaxy and throughout the universe, from the era of vigorous star formation at redshifts of 1–3 to the present day. The dominant feedback processes can be probed by observations of the Photo-Dissociation Regions (PDRs) where the far-ultraviolet photons of massive stars create warm regions of gas and dust in the neutral atomic and molecular gas. PDR emission provides a unique tool to study in detail the physical and chemical processes that are relevant for most of the mass in inter- and circumstellar media including diffuse clouds, proto-planetary disks, and molecular cloud surfaces, globules, planetary nebulae, and star-forming regions. PDR emission dominates the infrared (IR) spectra of star-forming galaxies. Most of the Galactic and extragalactic observations obtained with the James Webb Space Telescope (JWST) will therefore arise in PDR emission. In this paper we present an Early Release Science program using the MIRI, NIRSpec, and NIRCam instruments dedicated to the observations of an emblematic and nearby PDR: the Orion Bar. These early JWST observations will provide template data sets designed to identify key PDR characteristics in JWST observations. These data will serve to benchmark PDR models and extend them into the JWST era. We also present the Science-Enabling products that we will provide to the community. These template data sets and Science-Enabling products will guide the preparation of future proposals on star-forming regions in our Galaxy and beyond and will facilitate data analysis and interpretation of forthcoming JWST observations.

We have undertaken a search for the infrared emission from the intracluster dust in the Coma cluster of galaxies by the Multiband Imaging Photometer for Spitzer. Our observations yield the deepest mid and far-infrared images of a galaxy cluster ever achieved. In each of the three bands, we have not detected a signature of the central excess component in contrast to the previous report on the detection by Infrared Space Observatory (ISO). We still find that the brightness ratio between 70 mm and 160 mm shows a marginal sign of the central excess, in qualitative agreement with the ISO result. Our analysis suggests that the excess ratio is more likely due to faint infrared sources lying on fluctuating cirrus foreground. Our observations yield the 2s upper limits on the excess emission within 100 kpc of the cluster center as 5 x 10-3 MJy sr-1, 6 x 10-2 MJy sr-1, and 7 x 10-2 MJy sr-1, at 24, 70, and 160 mm, respectively. These values are in agreement with those found in other galaxy clusters and suggest that dust is deficient near the cluster center by more than 3 orders of magnitude compared with the interstellar medium.

We report on near- to far-infrared (IR) observations of the nearby elliptical galaxy NGC4589 by AKARI. NGC4589 has a complex stellar rotation field with a position angle difference of 45$^{\circ}$between the kinematic and morphological axes, although its morphology shows a smooth optical profile that closely follows the de Vaucouleurs law. The galaxy has a minor-axis dust lane, which is twisted toward the main stellar rotation. These properties strongly support that the galaxy is a relatively old merger remnant. We have obtained the spatial distributions of dust from far-IR emission and near-IR absorption, separately. We have also estimated the distribution of polycyclic aromatic hydrocarbons (PAHs) from the difference between images in the mid-IR bands. The spatial distributions of the dust and PAHs resemble each other, both showing significant deviations from the smooth stellar distribution. They extend to the main stellar rotation and the direction of the twisted inner dust lane, thus following the relics of the merger. Therefore, a large fraction of the dust and PAHs in NGC4589 are likely to originate from a past merger event.

We have developed an imaging Fourier transform spectrometer (FTS) for space-based far-infrared astronomical observations. The FTS employs newly developed photoconductive detector arrays with a capacitive trans-impedance amplifier, which makes the FTS a completely unique instrument. The FTS was installed as a function of the far-infrared instrument (FIS: Far-Infrared Surveyor) aboard the Japanese astronomical satellite, AKARI, which was launched on 2006 February 21 (UT) from Uchinoura Space Center. The FIS-FTS had been operated for more than one year before liquid helium ran out on 2007 August 26. The FIS-FTS was operated nearly six hundreds times, which corresponds to more than one hundred hours of astronomical observations and almost the same amount of time for calibrations. As expected from laboratory measurements, the FIS-FTS performed well and has produced a large set of astronomical data for valuable objects. Meanwhile, it has become clear that the detector transient effect is a considerable factor for FTSs with photoconductive detectors. In this paper, the instrumentation of the FIS-FTS and interesting phenomena related to FTS using photoconductive detectors are described, and future applications of this kind of FTS system are discussed.

We report the results of the mid-infrared spectroscopy of 14 Galactic star-forming regions with the high-resolution modules of the Infrared Spectrograph (IRS) on board the Spitzer Space Telescope. We detected [Si II] 35 mm, [Fe II] 26 mm, and [Fe III] 23 mm, as well as [S III] 33 mm and H2 S(0) 28 mm emission lines. Using the intensity of [N II] 122 mm or 205 mm and [O I] 146 mm or 63 mm reported by previous observations in four regions, we derived the ionic abundances of Si+/N+ and Fe+/N+ in the ionized gas and Si+/O0 and Fe+/O0 in the photodissociation gas. For all the targets, we derived the ionic abundances of Si+/S2+ and Fe2+/S2+ for the ionized gas. Based on photodissociation and H II region models the gas-phase Si and Fe abundance are suggested to be 3%-100% and <8% of the solar abundance, respectively, for the ionized gas and 16%-100% and 2%-22% of the solar abundance, respectively, for the photodissociation region gas. Since the [Fe II] 26 mm and [Fe III] 23 mm emissions are weak, the high sensitivity of the IRS enables us to derive the gas-phase Fe abundance widely in star-forming regions. The derived gas-phase Si abundance is much larger than that in cool interstellar clouds and that of Fe. The present study indicates that 3%-100% of Si atoms and <22% of Fe atoms are included in dust grains which are destroyed easily in H II regions, probably by the UV radiation. We discuss possible mechanisms to account for the observed trend: mantles which are photodesorbed by UV photons, organometallic complexes, or small grains.

We carried out high spatial resolution N-band imaging and spectroscopic observations of the planetary nebula BD +30 3639 with the Cooled Mid-Infrared Camera and Spectrometer (COMICS) mounted on the Subaru telescope. Mid-infrared images reveal a rectangle shell structure of the nebula extending over 4 '', which is supposed to be formed by the superwind from the central star. We have detected [Ne II] 12.8 mm and the unidentified infrared (UIR) bands at 8.6 and 11.2 mm, together with the broad plateau emission in 11-13 mm. In addition, the spectra clearly indicate the presence of silicate absorption around 10 mm for the first time, which increases sharply at the outside of the shell. This can be attributed to silicate grains that were formed in the O-rich phase of the central star, which is now C-rich. The present data indicate that these silicate grains are located in a very thin shell, suggesting that BD +30 3639 underwent a short period (~100 yr) of a high mass-loss rate (~ 3 x 10[?]3 M yr [?]1) at the last epoch of the O-rich phase. N-band spectra show that the distribution of [Ne II] is not clearly different from that of the UIR band and suggest that the UIR band carriers coexist with the ionized gas to some extent. This may be attributed to a slow destruction of the band carriers in the ionized region of the high electron density. The 10 mm continuum and the 11-13 mm plateau emission are dominant in the shell region, while the UIR 11.2 mm band becomes stronger in the outside of the shell, suggesting a change in the dust composition or the dust size distribution between the shell and the outside of the shell region. On the contrary, the peak wavelength of the UIR 11.2 mm band agrees with the class B spectrum, which is often seen in planetary nebulae, and does not change between the shell and the outside of the shell region. These facts suggest that the UIR band carriers are originally formed in the carbon-rich stellar wind and partially destroyed in the shell by shocks. The change of the UIR band spectrum from class B to A, which is generally seen in H II regions, should take place outside of the nebula.

We present results on mid-infrared imaging and spectroscopic observations of the nearby late-type spiral NGC6946 with the Infrared Camera on board AKARI. Based on mid-infrared imaging with the S7(7$\mu$m) and S11(11$\mu$m) bands, we found that the S7/S11ratios have larger values in the arm region, containing many star-forming regions, than in the interarm. Slit spectra of an interarm and a star-forming region show a series of unidentified infrared (UIR) bands at 6.2, 7.7, 8.6, and 11.2$\mu$m. The strengths of the 6.2, 7.7, and 8.6$\mu$m bands are larger relative to the 11.2$\mu$m band in the star-forming region, than in the interarm, even if the interstellar extinction of $A_V=3$mag towards the star-forming region is taken into account. The increase in the 6.2$\mu$m and 7.7$\mu$m features relative to the 11.2$\mu$m feature is consistent with the ionization model of PAHs. The ratio of the UIR features to the plateau emission under the 7.7$\mu$m and 8.6$\mu$m features and/or the ratio of the 7.6$\mu$m/7.8$\mu$m components in the 7.7$\mu$m feature increase in the star-forming region compared to the interarm. This variation can be accounted for by the hypothesis that the photo-evaporation of PAH clusters produce small free-flying PAHs in the star-forming region. The ratios of 6.2$\mu$m/11.2$\mu$m, 7.7$\mu$m/11.2$\mu$m, and 8.6$\mu$m/11.2$\mu$m may be tools to measure the star-formation activity in remote galaxies if these ratios and their variations are well examined and established for a large sample.

The nearby face-on spiral galaxy M101 has been observed with the Far-Infrared Surveyor onboard AKARI. The far-infrared four-band images reveal fine spatial structures of M101, which include global spiral patterns, giant H II regions embedded in outer spiral arms, and a bar-like feature crossing the center. The spectral energy distribution of the whole galaxy shows the presence of a cold dust component (18$^{+4}_{-10}$K) in addition to a warm dust component (55$^{+9}_{-25}$K). The distribution of the cold dust is mostly concentrated near the center, and appears to be smoothly distributed over the entire extent of the galaxy, whereas the distribution of warm dust indicates some correlation with the spiral arms, and has spotty structures, such as four distinctive bright spots in the outer disk in addition to a bar-like feature near the center, tracing the CO intensity map. The star-formation activity of the giant H II regions that spatially correspond to the former bright spots is found to be significantly higher than that of the rest of the galaxy. The latter warm dust distribution implies that there are significant star-formation activities in the entire bar filled with molecular clouds. Unlike our Galaxy, M101 is a peculiar normal galaxy with extraordinary active star-forming regions.

Far-infrared (IR) images of the nearby Sb galaxy NGC 2841 and the Sc galaxy NGC 2976 at wavelengths of 65, 90, 140, and 160 $\mu$m have been obtained with the Far-Infrared Surveyor (FIS) onboard AKARI. Both galaxies reveal similar morphologies of dust rings. They are, however, significantly different in the dust temperature: a cold ($\sim$21 K) ring for NGC 2841 and a warm ($\sim$30 K) ring for NGC 2976, which presumably reflects the difference in the origin of the ring structure for the different Hubble types of the galaxy. In addition to the dust-ring structure, a warm dust component was detected from the central region of NGC 2841, which may be attributed to heating by its Low-Ionization Nuclear Emission-line Region nucleus. As for NGC 2976, an extended dust component was observed along the minor axis, which shows a distribution somewhat asymmetrical to the galactic disk; this might be associated with the H I bridge in the M 81/M 82 group that NGC 2976 belongs to. By taking advantage of a wealth of the far-IR bands of the FIS, it has been demonstrated that the spectral energy distribution of NGC 2841 is spatially more variable than that of NGC 2976.

We present the observations of the reflection nebulae IC4954 and IC4955 region with the Infrared Camera and the Far-Infrared Surveyor (FIS) on board the infrared astronomical satellite AKARI during its performance verification phase. We obtained 7 band images from 7 to 160$\mu $m with higher spatial resolution and higher sensitivities than previous observations. The spatial variation in the mid-infrared color suggests that the star-formation in IC4954/4955 is progressing from south-west to north-east. The FIS 4-band data from 65$\mu $m to 160$\mu $m allow us to correctly estimate the total infrared luminosity from the region, which is about one sixth of the energy emitted from the existing stellar sources. Five candidates for young stellar objects have been detected as point sources for the first time in the 11$\mu $m image and it is suggested that that current star-formation has been triggered by previous star-formation activities. A wide area map of the size of about $1^\circ$around the IC4954/4955 region was created from the AKARI mid-infrared All-Sky Survey data. Together with the H I 21 cm data, it suggests a large hollow structure of a degree scale, on whose edge the IC4954/4955 region has been created, indicating star formation over three generations in largely different spatial scales.

The Far-Infrared Surveyor (FIS) is one of two focal-plane instruments on the AKARI satellite. FIS has four photometric bands at 65, 90, 140, and 160 $\mu \rm m$, and uses two kinds of array detectors. The FIS arrays and optics are designed to sweep the sky with high spatial resolution and redundancy. The actual scan width is more than eight arcminutes, and the pixel pitch matches the diffraction limit of the telescope. Derived point-spread functions (PSFs) from observations of asteroids are similar to those given by the optical model. Significant excesses, however, are clearly seen around tails of the PSFs, whose contributions are about 30% of the total power. All FIS functions are operating well in orbit, and the performance meets the laboratory characterizations, except for the two longer wavelength bands, which are not performing as well as characterized. Furthermore, the FIS has a spectroscopic capability using a Fourier transform spectrometer (FTS). Because the FTS takes advantage of the optics and detectors of the photometer, it can simultaneously make a spectral map. This paper summarizes the in-flight technical and operational performance of the FIS.

AKARI, the first Japanese satellite dedicated to infrared astronomy, was launched on 2006 February 21, and started observations in May of the same year. AKARI has a 68.5 cm cooled telescope, together with two focal-plane instruments, which survey the sky in six wavelength bands from mid–to far-infrared. The instruments also have a capability for imaging and spectroscopy in the wavelength range 2-180$\mu$m in the pointed observation mode, occasionally inserted into a continuous survey operation. The in-orbit cryogen lifetime is expected to be one and a half years. The All-Sky Survey will cover more than 90% of the whole sky with a higher spatial resolution and a wider wavelength coverage than that of the previous IRAS all-sky survey. Point-source catalogues of the All-Sky Survey will be released to the astronomical community. Pointed observations will be used for deep surveys of selected sky areas and systematic observations of important astronomical targets. These will become an additional future heritage of this mission.

We report on mid- and far-IR Spitzer observations of 7 nearby dusty elliptical galaxies by using the Multiband Imaging Photometer for Spitzer (MIPS) and Infrared Spectrograph (IRS). Our sample galaxies are known to contain excessive amounts of interstellar dust against sputtering destruction in hot plasma filling the interstellar space of elliptical galaxies. In order to study the origin and the properties of the excess dust in the hot plasma, we selected galaxies with a wide range of X-ray luminosities, but similar optical luminosities for our Spitzer Guest Observers (GO1) program. The 7 galaxies were detected at the MIPS 24$\mu$m, 70$\mu$m, and 160$\mu$m bands; the far- to mid-IR flux ratios of relatively X-ray-bright elliptical galaxies are lower than those of X-ray-faint galaxies. From the IRS spectra, polycyclic aromatic hydrocarbon (PAH) emission features were detected significantly from 5 of the 7 galaxies; the emission intensities are weaker as the X-ray luminosity of the galaxy is larger. We have found a correlation between the far- to mid-IR flux ratio and the equivalent width of the PAH emission feature. We have obtained an apparent spatial correspondence between the mid-IR and X-ray distributions in the outer regions for the three X-ray-brightest galaxies in our sample. Possible interpretations for our observational results are discussed.

We have made one-dimensional raster scan observations of the r Oph and s Sco star-forming regions with two spectrometers (SWS and LWS) on board the ISO. In the r Oph region, [Si II] 35 mm, [O I] 63 mm, 146 mm, [C II] 158 mm, and the H2 pure rotational transition lines S(0) to S(3) are detected, and the photodissociation region (PDR) properties are derived as the radiation field scaled by the solar neighborhood value G0 ~ 30-500, the gas density n ~ 250-2500 cm-3, and the surface temperature T ~ 100-400 K. The ratio of [Si II] 35 mm to [O I] 146 mm indicates that silicon of 10%-20% of the solar abundance must be in the gaseous form in the PDR, suggesting that efficient dust destruction is ongoing even in the PDR and that a fraction of the silicon atoms may be contained in volatile forms in dust grains. The [O I] 63 mm and [C II] 158 mm emissions are too weak relative to [O I] 146 mm to be accounted for by standard PDR models. We propose a simple model, in which overlapping PDR clouds along the line of sight absorb the [O I] 63 mm and [C II] 158 mm emissions, and show that the proposed model reproduces the observed line intensities fairly well. In the s Sco region, we have detected three fine-structure lines, [O I] 63 mm, [N II] 122 mm, and [C II] 158 mm, and derived that 30%-80% of the [C II] emission comes from the ionized gas. The upper limit of the [Si II] 35 mm is compatible with the solar abundance relative to nitrogen, and no useful constraint on the gaseous Si is obtained for the s Sco region.

While the remodeling process in myocardial failure involves changes in ventricular structure and performance, it is now appreciated that it is also associated with changes in thin filament composition and function. As is discussed, changes at the level thick filament may affect thin filament activation in heart failure. Alterations in actin, troponin and tropomyosin isoform composition do not appear to be significant factors in human heart failure. In contrast, proteolytic degradation of troponin subunits are likely to be playing a functional role in some forms of cardiomyopathy (e.g. ischemic). Finally, phosphorylation of troponin I and troponin T by kinases (most notably protein kinase C) substantially affect thin filament function in failing human myocardium. These findings indicate that functional deficits in thin filament function in failing myocardium are largely reversible and create the potential for future targeted therapies in the treatment of this deadly disease.

We report the detection of a feature at 65 mm and a broad feature around 100 mm in the far-infrared spectra of the diffuse emission from two active star-forming regions, the Carina Nebula and Sharpless 171. The features are seen in the spectra over a wide area of the observed regions, indicating that the carriers are fairly ubiquitous species in the interstellar medium. A similar 65 mm feature has been detected in evolved stars and attributed to diopside, a Ca-bearing crystalline silicate. The present observations indicate the first detection of a crystalline silicate in the interstellar medium if this identification also holds true for the interstellar feature. A similar broad feature around 90 mm reported in the spectra of evolved stars has been attributed to calcite, a Ca-bearing carbonate mineral. The interstellar feature seems to be shifted to longer wavelengths and have a broader width, although the precise estimate of the feature profile is difficult. As a carrier for the interstellar 100 mm feature, we investigate a possibility that the feature originates from carbon onions, grains consisting of curved graphitic shells. Because of the curved graphitic sheet structure, the optical properties in the direction parallel to the graphitic plane interact with those in the vertical direction in the carbon onion grains. This effect enhances the interband transition feature in the direction parallel to the graphitic plane in the carbon onions, which is suppressed in the graphite particles. Simple calculations suggest that carbon onion grains are a likely candidate for the observed 100 mm feature carrier, but the appearance of the feature is sensitive to the assumed optical properties.

Abstract:  Objectives: To investigate the possibility of applying diffusive air sampling and urinalysis (for mother compound and metabolites) to the monitoring of exposure of factory workers to 1-butanol. Methods: The performance of carbon cloth in adsorbing 1-butanol vapor in air was studied by experimental exposure of the cloth to 1-butanol at 50, 100, 200 or 400 ppm for up to 10 h. 1-Butanol in the exposed cloth was extracted with carbon disulfide and this was followed by gas-chromatographic (GC) analysis. Urine samples were collected from factory workers occupationally exposed to 1-butanol and from rats exposed experimentally to 1-butanol vapour (up to 200 ppm). The urine samples were analyzed by GC without any pretreatment, or after treatment with hydrochloric acid or hydrolase preparation. Results: The performance of the carbon cloth was such that it adsorbed 1-butanol in proportion to the concentration (up to 400 ppm) and the duration (up to 10 h) of exposure, and responded quantitatively to a 15-min exposure up to 400 ppm. The amount of 1-butanol (after enzymic or acid hydrolysis) in post-exposure urine samples from rats was proportional to the exposure intensity. The proportion of free 1-butanol in total 1-butanol (i.e., free+conjugated) in urine was higher after 100 or 200 ppm exposure (35–40%) than after 50 ppm exposure (about 8%). There was a significant increase in total 1-butanol concentration (but not in free 1-butanol) in shift-end urine samples of workers exposed to 1-butanol at concentrations up to 3 ppm. Conclusions: Diffusive sampling with carbon cloth as an adsorbent can be applied to ambient air monitoring of exposure to 1-butanol. Urinalysis for 1-butanol after hydrolysis is sensitive enough to detect occupational 1-butanol vapour exposure at 3 ppm.

Separate Determination by Gas‐Chromatography of Dimethylformamide, Dimethylacetamide, Monomethylformamide and Monomethylacetamide in Urine for Biological Monitoring: Toshio Kawai,et al.Osaka Occupational Health Service Center—A gaschromatographic method is developed, which allows simultaneous determination of N,N‐dimethylformamide (DMF) and N,N‐dimethylacetamide (DMA), as well as their metabolites of N‐monomethylformamide (MMF) and N‐monomethylacetamide (MMA), respectively. Quantitative heat decomposition of N‐hydrcxymethyl‐N‐methylacetamide to N‐monomethylacetamide required an injection port temperature of 225°C or above, similar to the case of conversion from N‐hydroxymethyl‐N‐methylformamide to N‐monomethylformamide. Analysis of urine samples from workers simultaneously exposed to DMF and DMA showed that the separation of small peaks for unidentified materials (which were detected in some urine samples) from that of DMF and DMA was achieved only on a 60 m‐long DB‐1071 column (and not on a 30 m‐long one). The analysis of urine samples from 27 exposed workers showed that both DMF and DMA, in addition to MMF and MMA, were excreted in urine at measurable concentrations. There was a significant correlation between MMF and DMF, and between MMA and DMA; the ratio was about 0.02 to 0.03 for both DMF/MMF and DMA/MMA.

Separate Determination by Gas-Chromatography of Dimethylformamide, Dimethylacetamide, Monomethylformamide and Monomethylacetamide in Urine for Biological Monitoring: Toshio Kawai, et al.Osaka Occupational Health Service Center—A gaschromatographic method is developed, which allows simultaneous determination of N,N-dimethylformamide (DMF) and N,N-dimethylacetamide (DMA), as well as their metabolites of N-monomethylformamide (MMF) and N-monomethylacetamide (MMA), respectively. Quantitative heat decomposition of N-hydrcxymethyl-N-methylacetamide to N-monomethylacetamide required an injection port temperature of 225°C or above, similar to the case of conversion from N-hydroxymethyl-N-methylformamide to N-monomethylformamide. Analysis of urine samples from workers simultaneously exposed to DMF and DMA showed that the separation of small peaks for unidentified materials (which were detected in some urine samples) from that of DMF and DMA was achieved only on a 60 m-long DB-1071 column (and not on a 30 m-long one). The analysis of urine samples from 27 exposed workers showed that both DMF and DMA, in addition to MMF and MMA, were excreted in urine at measurable concentrations. There was a significant correlation between MMF and DMF, and between MMA and DMA; the ratio was about 0.02 to 0.03 for both DMF/MMF and DMA/MMA.

Abstract:  Head-space gas chromatography (GC) and high-performance liquid chromatography (HPLC) (with fluorescence detectors) methods were developed for toluene (TOL-U) and o-cresol (CR-U) in urine, respectively. In order to identify the most sensitive urinary indicator of occupational exposure to toluene vapor (TOL-A) among TOL-U, CR-U, and hippuric acid in urine (HA-U), the two methods together with an HPLC (with untraviolet detectors) method for determination of HA-U were applied in the analysis of end-of-shift urine samples from 115 solvent-exposed workers (exposed to toluene at 4 ppm as geometric mean). Regression analysis showed that TOL-U correlated with TOL-A with a significantly higher correlation coefficient than did HA-U or CR-U. With regard to the TOL-A concentrations at which the exposed subjects could be separated from the nonexposed by the analyte, TOL-U achieved separation at <10 ppm TOL-A, whereas both HA-U and CR-U did so only when TOL-A was 30 ppm or even higher. The ratio of the analyte concentrations at 50 ppm TOL-A to those at 0 ppm TOL-A was also highest for TOL-U. Overall, the results suggest that TOL-U is a better marker of exposure to toluene vapor than HA-U or CR-U.

lEndothelial function and cerebrovascular reactivity were impaired in MS.lEndothelial dysfunction was more noticeable than cerebrovascular reactivity in MS.lDisease severity of MS correlated with the endothelial dysfunction.

Although a technical progress in MRI system has elevated a detection rate of unruptured intracranial cerebral aneurysms (uANs) in the elderly as well as in youth, the management of those in the elderly remain controversial because a surgical indication is based on the balance between its rupture rate and surgical risk. Here we have clarified a change of uANs on MR Angiography, with which evaluated a difference between younger and older patients.

We observed diffuse cosmic and atmospheric gamma rays at balloon altitudes with the Sub-MeV gamma-ray Imaging Loaded-on-balloon Experiment I (SMILE-I) as the first step toward a future all-sky survey with a high sensitivity. SMILE-I employed an electron-tracking Compton camera comprised of a gaseous electron tracker as a Compton-scattering target and a scintillation camera as an absorber. The balloon carrying the SMILE-I detector was launched from the Sanriku Balloon Center of the Institute of Space and Astronautical Science/Japan Aerospace Exploration Agency on 2006 September 1, and the flight lasted for 6.8 hr, including level flight for 4.1 hr at an altitude of 32-35 km. During the level flight, we successfully detected 420 downward gamma rays between 100 keV and 1 MeV at zenith angles below 60deg. To obtain the flux of diffuse cosmic gamma rays, we first simulated their scattering in the atmosphere using Geant4, and for gamma rays detected at an atmospheric depth of 7.0 g cm-2 we found that 50% and 21% of the gamma rays at energies of 150 keV and 1 MeV, respectively, were scattered in the atmosphere prior to reaching the detector. Moreover, by using Geant4 simulations and the QinetiQ atmospheric radiation model, we estimated that the detected events consisted of diffuse cosmic and atmospheric gamma rays (79%), secondary photons produced in the instrument through the interaction between cosmic rays and materials surrounding the detector (19%), and other particles (2%). The obtained growth curve was comparable to Ling's model, and the fluxes of diffuse cosmic and atmospheric gamma rays were consistent with the results of previous experiments. The expected detection sensitivity of a future SMILE experiment measuring gamma rays between 150 keV and 20 MeV was estimated from our SMILE-I results and was found to be 10 times better than that of other experiments at around 1 MeV.