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We report here a quite rare case of ductal carcinoma in situ (DCIS) with isolated tumor cells in the sentinel lymph node in a 17-year-old adolescent girl whose mother also had advanced breast cancer. Findings included an elastic mass in the right breast accompanied by serous nipple discharge. DCIS of the breast was diagnosed following core needle biopsy. Although no invasive focus was clearly observed in the mastectomy sample, isolated tumor cells were found in the sentinel lymph node. Although the family refused genetic testing, a hereditary abnormality may have played a role in the carcinogenesis in this case.

We have observed the CH3OH J = 2–1, SiO J = 2–1, C 34 S J = 2–1, H 13 CO + J = 1–0, HN 13 C J = 1–0, CCH N = 1–0, OCS J = 8–7, and SO JN = 22–11 lines toward 20 massive clumps, including Midcourse Space Experiment (MSX )8 μm dark sources (infrared dark clouds) andMSX 8 μm sources, by using the Nobeyama Radio Observatory 45 m telescope. We have found that the velocity widths of the CH3OH and C 34 S lines are broader than those of the H 13 CO + line in the MSX dark sources. On the other hand, they are comparable to the velocity width of the H 13 CO + line in the MSX sources. In addition, the [SiO]/[H 13 CO + ] abundance ratio is found to be enhanced in the MSX dark sources in comparison with the MSX sources. These results suggest that shocks caused by interaction between an outflow and an ambient dense gas would have substantial impact on the chemical composition of the MSX dark sources. The velocity widths of the CH3OH and C 34 S lines relative to that of the H 13 CO + line as well as the [SiO]/[H 13 CO + ] abundance ratio could be used as good tools for investigating evolutionary stages of massive clumps. On the basis of the results, we discuss the chemical and physical evolution of massive clumps.

人工林の「広葉樹林化」を検討するため, 日本語で1978∼2006年に発行された広葉樹関連文献を, 林業・林産関係国内文献データベース (FOLIS) で検索した。研究上の必要性を評価し, S, A, B, Cのランク付けを行った。また県別の文献数の違いやキーワードの時代変遷を国内の施業の歴史とあわせて検討した。検索は「広葉樹」と, 「間伐」, 「除伐」, 「人工林」などを組み合わせ, 総書誌数185誌, 総文献数648件を抽出した。S評価の文献は14件, A評価の文献は59件だった。文献は岐阜県 (16件), 宮崎県 (15件) で多かった。文献内容は時代により変遷し, 「広葉樹施業」や「天然林施業」といったキーワードが減少する一方で, 「多様性」をキーワードに含む論文が増加してきている。「不成績造林」や「間伐」をキーワードとする論文は, いくつかのピークを示しながら, 1980年代から連続的に発表されてきた。「広葉樹林化」は新しい概念であり, これまでの研究を十分に参考にしながら慎重に取り組む必要がある。

Fe–Mg partitioning between post-perovskite and ferropericlase has been studied using a laser-heated diamond anvil cell at pressures up to 154 GPa and 2,010 K which corresponds to the conditions in the lowermost mantle. The composition of the phases in the recovered samples was determined using analytical transmission electron microscopy. Our results reveal that the Fe–Mg partition coefficient between post-perovskite and ferropericlase (K D PPv/Fp ) increases with decreasing bulk iron content. The compositional dependence of K D PPv/Fp on the bulk iron content explains the inconsistency in previous studies, and the effect of the bulk iron content is the most dominant factor compared to other factors, such as temperature and aluminum content. Iron prefers ferropericlase compared to post-perovskite over a wide compositional range, whereas the iron content of post-perovskite (X Fe PPv , the mole fraction) does not exceed a value of 0.10. The iron-rich ferropericlase phase may have significant influence on the physical properties, such as the seismic velocity and electrical conductivity at the core–mantle boundary region.

The authors have previously developed poly(DL-lactic-co-glycolic acid) (PLGA) nanospheres (NSs) as a nanoparticulate drug carrier for pulmonary administration. The present study demonstrates that chitosan (CS)-modified PLGA NSs (CS-PLGA NSs) are preferentially taken up by human lung adenocarcinoma cells (A549). PLGA NSs prepared using a water-oil-water emulsion solvent evaporation method were surface-modified by adsorption of CS. The physicochemical parameters of PLGA NS, including average size and surface charge, were measured to identify which parameter influenced cellular uptake of PLGA NS. Uptake was confirmed using fluorescence spectrophotometry and was visualized in A549 cells with confocal laser scanning microscopy (CLSM). The cytotoxicities of non- and CS-PLGA NS systems were compared in vitro by MTS assay. Cellular uptake of PLGA NS increased with decreasing diameter to the submicron level and with CS-mediated surface modification. Cellular uptake of PLGA NS was energy dependent, as shown by a reduction in uptake at lower incubation temperatures and in hypertonic growth medium used as an inhibitor of clathrin-coated pit endocytosis. CS-PLGA NSs were taken up by A549 cells in an energy-dependent manner, suggesting a clathrin-mediated endocytic process. CS-PLGA NS demonstrated low cytotoxicity, similar to non-PLGA NS.

The melting temperature of Fe–18 wt% Si alloy was determined up to 119 GPa based on a change of laser heating efficiency and the texture of the recovered samples in the laser-heated diamond anvil cell experiments. We have also investigated the subsolidus phase relations of Fe–18 wt% Si alloy by the in-situ X-ray diffraction method and confirmed that the bcc phase is stable at least up to 57 GPa and high temperature. The melting curve of the alloy was fitted by the Simon’s equation, P(GPa)/a = (T m(K)/T 0) c , with parameters, T 0 = 1,473 K, a = 3.5 ± 1.1 GPa, and c = 4.5 ± 0.4. The melting temperature of bcc Fe–18 wt% Si alloy is comparable with that of pure iron in the pressure range of this work. The melting temperature of Fe–18 wt% Si alloy is estimated to be 3,300–3,500 K at 135 GPa, and 4,000–4,200 K at around 330 GPa, which may provide the lower bound of the temperatures at the core–mantle boundary and the inner core–outer core boundary if the light element in the core is silicon.

We have conducted millimeter-wave observations of deuterated species of various carbon-chain molecules toward a low-mass star-forming region, L1527, which shows extraordinary richness of carbon-chain molecules in a vicinity of the protostar (Warm Carbon Chain Chemistry; WCCC). We have detected the spectral lines of l-C3D, C4D, C4HD, DC3N, DC5N, and c-C3HD, where l-C3D and C4HD are detected for the first time in space. The deuterium fractionation ratios are found to be moderate (2% to 7%), although they tend to be higher than those in the starless core, TMC-1. The upper limit to the [CH2DOH]/[CH3OH] ratio is also as low as 3%. Therefore, high deuterium fractionation ratios reported for hot corino sources are not seen in L1527. The observed ratios mean that the depletion of CO onto dust grains had not proceeded far in L1527, compared to the hot corino case. This would be consistent with a short timescale of the starless core phase, as suggested for the possible origin of WCCC.

Fe-Mg partitioning between perovskite and ferropericlase in the MgO-FeO-SiO 2 system has been studied up to about 100 GPa at around 2000 K using a laser-heated diamond anvil cell (LHDAC). The compositions of both phases were determined by using analytical transmission electron microscopy (ATEM) on the recovered samples. Present results reveal that the Fe-Mg apparent partition coefficient between perovskite and ferropericlase [ K D Pv/Fp = ( X Fe Pv X Mg Fp )/( X Mg Pv X Fe Fp )] decreases with increasing pressure for a constant FeO of the system, and it decreases with increasing FeO content of ferropericlase. The gradual decrease of K D Pv/Fp with increasing pressure is consistent with the spin transition in ferropericlase occurring in the broad pressure range from 50 to 100 GPa at around 2000 K.

We studied the age and growth of the lizardfish Saurida elongata using ground thin sections of otoliths (sagittae) from specimens collected in the Tsushima/Korea Strait between May 1999 and June 2001. A total of 695 individuals with fork lengths (FL) ranging from 189 to 478 mm were examined. The frequency of translucent zone occurrence at the outer margin of the otoliths indicated that translucent zones formed once a year between November and February. Most of the males examined were estimated to be 2–7 years old and the females, 3–9 years old. The maximum estimated age of a male specimen was 10 years and that of a female, 11 years. The estimated von Bertalanffy growth curves were FL t = 451{1 − exp[−0.172(t + 2.50)]} and FL t = 515{1 − exp[−0.151(t + 2.47)]} for males and females, respectively. At all ages, the FL at a specific age for females was greater than that for males, suggesting that females of this species grow faster than males.

We have conducted a search for carbon-chain molecules toward 16 protostars with the Mopra 22 m and Nobeyama 45 m telescopes, and have detected high excitation lines from several species, such as C4H (N = 9-8), C4H2(J = 100,10-90,9), CH3CCH(J = 5-4, K = 2), and HC5N(J = 32-31), toward the low-mass protostar, IRAS15398 – 3359 in Lupus. The C4H line is as bright as 2.4 K measured with the Nobeyama 45 m telescope. The kinetic temperature is derived to be 12.6 ± 1.5 K from the K = 1 and K = 2 lines of CH3CCH. These results indicate that the carbon-chain molecules exist in a region of warm and dense gas near the protostar. The observed features are similar to those found toward IRAS04368+2557 in L1527, which shows warm carbon-chain chemistry (WCCC). In WCCC, carbon-chain molecules are produced efficiently by the evaporation of CH4 from the grain mantles in a lukewarm region near the protostar. Our data clearly indicate that WCCC is no longer specific to L1527, but occurs in IRAS15398 – 3359. In addition, we draw attention to a remarkable contrast between WCCC and hot corino chemistry in low-mass star-forming regions. Carbon-chain molecules are deficient in hot corino sources like NGC1333 IRAS4B, whereas complex organic molecules seem to be less abundant in the WCCC sources. A possible origin for such source-to-source chemical variations is suggested to arise from the timescale of the starless-core phase in each source. If this is the case, the chemical composition provides an important clue to explore the variation of star formation processes between sources and/or molecular clouds.

The paper reports the vibration characteristics assessment of grid panels which were furnished in the main structure of 50kg-class micro-satellite ``SOHLA-1''. Three different types of grid panels with dimensions of 141.1 × 423.0 × 10.0mm, triangle-grid-type panel, rectangle-grid-type panel and frame-type panel, were investigated to find their dynamics through impulse test. Vibration characteristics were also simulated by a FEM computer soft NASTRAN. Application of flame-retardant type magnesium alloy to the panel was made to confirm the structural effectiveness of magnesium alloy panel.

We review recent advances in the study of phase transitions of minerals in the Earth’s mantle, including unsolved problems regarding these processes. The phase boundaries of (Mg,Fe)2SiO4 in the mantle transition zone are modified under the wet conditions by changes in thermodynamic properties of its polymorphs because of differences in the water solubilities of these minerals. The shift of phase boundaries has significant implications for the topography of the 410 km and 660 km seismic discontinuities. The post-perovskite phase with CaIrO3 structure exists at pressures above 110 GPa and at high temperature. The effects of Al and Fe on phase transition are under debate. Several post-stishovite phases have been reported but equilibrium boundaries and existence in the real lower mantle are also still debatable. Spin transition occurs in magnesiowustite, perovskite, and post-perovskite phases at high pressures of the lower mantle and core. The pressure interval in the spin transition can be large at high temperature and so the transition might not cause a discrete change in physical properties under real Earth conditions. © 2008 Elsevier B.V. All rights reserved.

The parametric X-ray radiation (PXR) generator system at Laboratory for Electron Beam Research and Application (LEBRA) in Nihon University is a monochromatic and coherent X-ray source with horizontal wavelength dispersion. The energy definition of the X-rays, which depends on the horizontal size of the incident electron beam on the generator target crystal, has been investigated experimentally by measuring the X-ray absorption near edge structure (XANES) spectra on Cu and CuO associated with conventional X-ray absorption imaging technique. The result demonstrated the controllability of the spectrum resolution of XANES by adjusting of the horizontal electron beam size on the target crystal. The XANES spectra were obtained with energy resolution of several eV at the narrowest case, which is in qualitative agreement with the energy definition of the PXR X-rays evaluated from geometrical consideration. The result also suggested that the wavelength dispersive X-ray absorption fine structure measurement associated with imaging technique is one of the promising applications of PXR.

The age and growth of chub mackerel Scomber japonicus collected from the East China Sea and the northern waters off Kyushu between June 2000 and June 2001 were determined by observing the otolith surface after dipping it in xylene. The translucent and opaque zones on the otolith surface were identified, and the number of translucent zones was counted. Monthly changes in the frequency of fish with translucent zones on the otolith margin, and in the marginal increments, indicated that the translucent zones were formed between April and June. The seasonal pattern of annulus formation on the otolith became clear by observing the otoliths of fish with known ages, and the otolith formation in wild fish was consistent with that of fish with known ages. The mean gonadosomatic index of male and female fish was high from March to May, and spawning females were observed from mid-March to mid-May. The estimated ages were 1–5 years for males and 1–6 years for females. The von Bertalanffy growth parameters did not significantly differ between male and female. The model was obtained as FLt=406×{1−exp[−0.372×(t+1.68)]

Advanced applications of parametric X-ray radiation (PXR) such as energy-dispersive X-ray absorption fine structure (DXAFS) analysis and phase-contrast imaging have been developed at the Laboratory for Electron Beam Research and Application (LEBRA) of Nihon University. To improve the electron beam quality and geometrical stability of the target crystal, the cooling-water system for the linac and the PXR target was replaced with a new one capable of more precise control. As a result, the reliability of the experimental data in PXR applications, especially in X-ray imaging, has improved. The effect of the electron beam focusing on the target crystal was also investigated. The results of X-ray imaging with a long propagation distance and measurement of the time-structure of the PXR intensity suggest that the correlation between the electron beam profile and the X-ray coherence is rather complicated. It is possible that incident electrons cause some deformation of the target crystal, becoming the dominant factor restricting the quality of intense PXR.

著者人数：11名, Accepted: 2008-03-30, 資料番号: SA1000295000

Aim: To review of the difference in the health condition between 8020 achievers and 8020 non-achievers covering 25 papers which were published mainly in Japan. Background: A campaign targeting the elderly to retain at least 20 teeth by the time they reach the age of 80 years (8020) has been in place since 1991 in Japan. Results: The percentage of 8020 achievers increased from 10.9% in 1993, 15.3% in 1999 and 24.1% in 2005. The 8020 achievers had a tendency towards a strict upbringing and were not fond of sweets in their childhood. Physical indices such as height, weight, BMI score, bone mineral density, balance ability, grip strength, and exercise function in the 8020 achievers were better than the 8020 non-achievers. A close inverse relationship between the number of teeth and heart rate was recognised. The food intake survey showed that 8020 achievers ate many kinds of food. However, these foods were those with less kilocalories and lower levels of carbohydrate. The 8020 achievers had good activity in daily life (ADL) level, were satisfied with life, and had a higher cumulative survival rate. Oral health conditions including periodontal condition, masticatory ability, occlusal force, occlusal and maxillofacial forms in the 8020 achievers were better than the 8020 non-achievers.

Breast metastases from extra-mammary malignancies, especially those mimicking primary inflammatory breast carcinoma, are extremely rare. We report here two cases of inflammatory breast metastases from gastric or ovarian cancer. Both patients, who had prior advanced malignant disease, presented with unilateral breast redness and swelling with peau d'orange sign, resembling primary inflammatory breast cancer or acute mastitis. Breast biopsy revealed poorly differentiated adenocarcinoma with signet-ring cells or clear cell carcinoma in the lymphatic vessels and the parenchyma without an in situ lesion, similar to primary lesions of the stomach or ovary, respectively. Immunohistochemical staining for estrogen receptor, progesterone receptor, and gross cystic disease fluid protein 15 was of value for correct diagnosis. Since breast metastasis is a sign of poor prognosis of the primary malignant disease, the possibility of breast metastasis should be considered in appropriate patients to preclude unnecessary major surgery.

The millimeter-wave rotational emission lines (404-303 and 505-404) of protonated carbon dioxide, HCO2+(HOCO+), have been detected toward the low-mass Class 0 protostar IRAS 04368+2557 in L1527 with the IRAM 30 m telescope. This is the first detection of HCO2+ except for the Galactic center clouds. The column density of HCO2+ averaged over the beam size (29'') is determined to be 7.6 ? 1010 cm?2, assuming a rotational temperature of 12.3 K. The fractional abundance of gaseous CO2 relative to H2 is estimated from the column density of HCO2+ with the aid of a simplified chemical model. If the HCO2+ emission only comes from the evaporation region of CO2 near the protostar (T 50 K), the fractional abundance of CO2 is estimated to be higher than 6.6 ? 10?4. This is comparable to the elemental abundance of carbon in interstellar clouds, and hence, the direct evaporation of CO2 from dust grain is unrealistic as a source of gaseous CO2 in L1527. A narrow line width of HCO2+ also supports this. On the other hand, the fractional abundance of CO2 is estimated to be 2.9 ? 10?7, if the source size is comparable to the beam size. These results indicate that gaseous CO2 is abundant even in the low-mass star-forming region. Possible production mechanisms of gaseous CO2 are discussed.

Analytical transmission electron microscope (ATEM) is a powerful tool for analyses of the samples recovered from ultrahigh pressure experiments. Recently, Focused Ion Beam (FIB) system has been applied to prepare a TEM foil of sample recovered from laser heated diamond anvil cell (LHDAC). It has some advantages compared to conventional argon ion milling method. In this article, recent advances in the DAC sample preparation for TEM observation using FIB system are reviewed.

The conventional focused ion beam (FIB) sample preparation technique “lift-out method” was modified for the reliable analysis of a laser-heated diamond anvil cell (LHDAC) sample. Box-shaped grooves were prepared in the LHDAC specimen in order to recover a block using a gallium ion beam in the vicinity of the area to be characterized by transmission electron microscope (TEM). The recovered block was fixed on the stage of a copper (or molybdenum) grid and thinned by the gallium ion beam in order to obtain a TEM foil. Our modified lift-out method allows us to thin the entire vertical section (from the upper anvil surface to the lower anvil surface) of the LHDAC sample.

High-pressure and high-temperature experiments on the KAlSi3O8 composition were conducted in a laser-heated diamond-anvil cell at pressures up to 128 GPa, which correspond to the lowermost mantle conditions. In situ synchrotron X-ray diffraction measurements revealed that the hollandite II phase in KAlSi3O8 with a monoclinic symmetry of I2/m was stable over the entire range of mantle conditions, and the tunnel structure formed by the double chains of edge-sharing (Si,Al)O6 octahedra, which could accommodate a larger cation such as potassium, was sustained. The (Si,Al)O6 octahedra in the KAlSi3O8 hollandite II phase showed a similar compression behavior to those in high-pressure silicate structures, such as rutile-type and perovskite-type phases, and were found to be less compressible than the KO8 polyhedra. The KAlSi3O8 hollandite II phase is a potential host mineral for potassium under lower mantle conditions and, therefore, may have a significant influence on geochemistry if potassium feldspar KAlSi3O8 in the Earth's crust is transported into the Earth's mantle through subduction.

We have detected the high-excitation lines of carbon-chain molecules such as C4H2 (J ¼ 100;10Y90;9), C4 H( N ¼ 9Y8, F1, F2), l-C3H2 (41,3Y31,2), and CH3CCH (J ¼ 5Y4, K ¼ 2) toward a low-mass star-forming region, L1527. In particular, the F1 line of C4 Hi s as strong as 1.7 K( TMB). The rotational temperature of C4H2 is determined to be 12:3 � 0:8 K, which is higher than that in TMC-1 (3.8 K). Furthermore, the column density of C4H2 is derived to be about 1/4 of that in TMC-1, indicating that carbon-chain molecules are abundant in L1527 for a star-forming region. Small mapping observations show that the C4H, C4H2, and c-C3H2 emissions are distributed from the infalling envelope to the inner part. Furthermore, we have detected the lines of C5H, HC7N, and HC9N in the 20 GHz region. Sincethecarbon-chainmolecules aregenerallydeficientinstar-forming cores, theaboveresultscannot simply beexplained by the existing chemical models. The following hypothesis is proposed. If the timescale of the prestellar collapse in L1527 were shorter than those of the other star-forming cores, the carbon-chain molecules could survive in thecentralpartofthecore.Inaddition,regenerationprocessesofthecarbon-chainmoleculesduetostarformationactivities would play an important role. Evaporation of CH4 from the grain mantles would drive the regeneration processes.Thepresentobservationsshow newchemistryinawarmanddenseregionneartheprotostars,whichisnamed ‘‘warm carbon-chain chemistry (WCCC).’’ Subject headingg ISM: abundances — ISM: individual (L1527) — ISM: molecules — stars: formation

The millimeter-wave rotational emission line (J = 9–8) of the negative ion, C4H−, has tentatively been detected toward the low-mass Class 0 protostar IRAS 04368+2557 in L1527 with the IRAM 30 m telescope. The column density of C4H− is determined to be 1.1 × 1010 cm−2. The [C4H−]/[C4H] ratio is found to be 6.8 × 10−5, which is much lower than the [C6H−]/[C6H] ratio (0.093). From this result, the rate coefficient for the radiative attachment reaction between C4H and electron is estimated to be as small as 3 × 10−11 cm3s−1 on the basis of the simplified chemical model. The present observation has demonstrated the uniqueness and importance of L1527 in searching for a new carbon-chain molecule in a star-forming region.

We have detected the J = 7-6, 8-7, and 15-14 lines of C6H- toward a low-mass star-forming region of L1527. We have also detected the J = 15/2-13/2 and 33/2-31/2 lines of the corresponding neutral species, C6H, and the 81,8-71,7 line of C6H2 in L1527. This is the first detection of these three species in star-forming regions. The column density of C6H- is (5.8 ± 1.8) × 1010 cm-2, which is comparable to that in TMC-1, although the column density of C6H in L1527 is about 1/5 of that in TMC-1. Hence, the N(C6H-)/N(C6H) ratio is 0.093 ± 0.029, which is higher than that in TMC-1 by a factor of 4. This high anion-to-neutral ratio is discussed in terms of a simplified chemical model.

We have detected the rotational lines of HCOOCH3 toward a Class 0 low-mass protostar, NGC1333 IRAS4B, which is reported to be extremely young according to the dynamical age of the molecular outflow (a few 100 yr). This suggests that the complex organic molecules appear from the very early stage of protostellar evolution. On the other hand, the complex organic molecules are not detected in a more evolved protostar, L1527. We have also found a similar trend in a massive star forming region, NGC2264. The HCOOCH3 emission is almost absent toward IRS1, whereas it is concentrated near MMS3, which is younger than IRS1. In addition, the HCOOCH3 intensity peak is slightly shifted from the dust emission peak, as is seen in the Orion KL Compact Ridge, giving an important clue to solve its origin.

The rotational spectral lines (JN = 32-21 and JN = 21-10) of 13CCS and C13CS have been observed toward a cold dark cloud, TMC-1. The strongest hyperfine component lines of 13CCS and C13CS (JN = 21-10, F = 5/2-3/2) have successfully been detected. The / abundance ratio is determined to be 4.2 ± 2.3 (3 σ). The / ratio is evaluated to be 230 ± 130 (3 σ), and hence, 13CCS is found to be significantly diluted. Such a difference between the 13CCS and C13CS abundances is also found in L1521E, which is a very young core with rich carbon-chain molecules. Therefore, the anomaly is not specific to TMC-1, but seems to be common for the CCS-rich clouds. Furthermore, we have also observed the J = 4-3 transition of 13CCCS and CCC34S in TMC-1 and L1521E and have found that the / ratio is larger than 8.4 (3 σ). This lower limit is considerably larger than the interstellar / ratio of 3, indicating that 13CCCS is diluted as in the case of 13CCS. These results give us strong constraints on the main pathways to produce CCS and CCCS.

We report here a rare form of invasive ductal carcinoma composed of a mass protruding from the tip of the nipple in a 43-year-old woman with hyperprolactinemia. She had been amenorrheic for 15 years following an incomplete pituitary adenomectomy for prolactinoma. She presented with a mass on the left nipple that had been growing for 6 months. Morphologically, the mass resembled adenoma of the nipple. Another mass was located in the subareolar region. She underwent mastectomy after invasive ductal carcinoma was diagnosed. Histopathologically, the tumor of the nipple was invasive ductal carcinoma, which had extended intraductally from another invasive ductal carcinoma in the subareolar region, and had infiltrated the epidermis of the nipple (Paget's disease). MR mammography successfully detected the relationship between the tumors. Postoperatively, the plasma prolactin level was abnormally high, while the plasma estradiol level was quite low, although macro-pituitary adenoma was not detected by MRI. The patient was treated with bromocriptine mesilate, in addition to adjuvant chemotherapy for breast cancer, and the plasma prolactin level has since normalized.

We have mapped two massive clumps, clump A and B, of the AFGL 333 cloud in the N2H+ J = 1-0, CCS JN = 43-32, HC3N J = 5-4, and NH3 (J,K) = (1,1) and (2,2) lines with the Nobeyama Radio Observatory 45 m telescope. Intense N2H+ emission comes from the two clumps, and its overall distribution is similar to that of C18O J = 1-0. On the other hand, the CCS and HC3N emissions are more intense toward clump B than toward clump A. Thus, the column density ratios of [CCS]/[N2 H+] and [HC3N]/[N2H+] tend to be higher toward clump B than toward clump A, indicating that clump B is younger than clump A. This is supported by a fact that the 2MASS sources with H - K > 2 and the Spitzer 24 μm sources are mostly associated with clump A, whereas only a few such sources exist in clump B. Clump B involves a few dense cores that are dark in the mid-infrared maps. Such cores are thought to be good candidates of starless cores for high- or intermediate-mass stars.

Millimeter-wave spectral lines of HCOOCH3 are observed toward a massive star-forming region, NGC 2264 IRS 1, with the Nobeyama 45 m radio telescope and Nobeyama Millimeter Array. The HCOOCH3 emission is not detected toward the dense core around IRS 1, which is the brightest IR source. However, it is definitively detected toward MMS 3, which is thought to contain a high-mass equivalent of a Class 0 protostar. The column density and the fractional abundance of HCOOCH3 in MMS 3 are found to be (4-30) × 1015 cm-2 and (0.7-5.3) × 10-8, respectively, assuming that the range of the excitation temperature is from 50 to 250 K. The fractional abundance is lower by an order of magnitude than that in the compact ridge of Orion KL. On the other hand, the upper limit to the fractional abundance toward IRS 1 is significantly lower than the abundance toward MMS 3. Since MMS 3 is less evolved than IRS 1, this result would indicate that HCOOCH3 preferentially exists in the younger stage of protostellar evolution, as in the case of low-mass star forming regions. The distribution of HCOOCH3 is found to be slightly offset from the dust continuum peak of MMS 3 by 13''. This situation is similar to that found in the compact ridge of Orion KL, which would provide us with an important clue in exploring its peculiar chemistry.

【目的】神経麻痺を伴った腱板断裂の治療法は見解が分かれる．我々は肩関節脱臼後に腋窩神経麻痺を伴った腱板広範囲断裂2例に対し鏡視下腱板修復術を行い良好な成績を得たので報告する．【症例1】60歳，男性．転倒し右肩関節受傷．右肩自力挙上困難にて受傷後6週で初診．右三角筋に筋萎縮，右肩外側に痺れ感を認めた．受傷後3ヶ月で鏡視下腱板修復術施行した．JOA scoreは術前31点が術後1年で94点に改善した．【症例2】47歳，男性．転倒し右肩関節受傷．右肩自力挙上困難にて受傷後3週で初診．右三角筋の筋萎縮，右肩外側に痺れ感を認め，EMGにて右三角筋に安静時脱神経電位を認めた．受傷後1ヶ月で鏡視下腱板修復術を施行した．JOA scoreは術前45点が術後6ヶ月で93点に改善した．【考察】腱板の変性を考えると断裂が大きい場合は神経の回復傾向がみられたら早期に手術を考慮していいのではと考える．

Aims: Understanding the fragmentation and collapse properties of the dense gas during the onset of high-mass star formation. Methods: We observed the massive (~800M_sun) starless gas clump IRDC18310-4 with the Plateau de Bure Interferometer (PdBI) at sub-arcsecond resolution in the 1.07mm continuum andN2H+(3-2) line emission. Results: Zooming from a single-dish low-resolution map to previous 3mm PdBI data, and now the new 1.07mm continuum observations, the sub-structures hierarchically fragment on the increasingly smaller spatial scales. While the fragment separations may still be roughly consistent with pure thermal Jeans fragmentation, the derived core masses are almost two orders of magnitude larger than the typical Jeans mass at the given densities and temperatures. However, the data can be reconciled with models using non-homogeneous initial density structures, turbulence and/or magnetic fields. While most sub-cores remain (far-)infrared dark even at 70mum, we identify weak 70mum emission toward one core with a comparably low luminosity of ~16L_sun, re-enforcing the general youth of the region. The spectral line data always exhibit multiple spectral components toward each core with comparably small line widths for the individual components (in the 0.3 to 1.0km/s regime). Based on single-dish C18O(2-1) data we estimate a low virial-to-gas-mass ratio, 8 pages, 4 figures, A&A in press

Solitary/multiple plasmacytoma of bone, a rare disease as compared to multiple myeloma, is characterized by monoclonal proliferation of plasma cells in local legion (s) of bone, with no bone marrow abnormalities. Monoclonal gammagloblinemia is often absent in these conditions, and useful examinations allowing evaluation of responses to treatment are as yet lacking. Recently, 18F-FDG PET/CT (PET/CT) was reported to be useful for detecting bone lesions. PET/CT is also valuable for predicting the outcomes of patients with solitary plasmacytoma, when applied in combination with the serum free light chain (sFLC) κ/λ ratio. We present a 62-year-old male with multiple plasmacytoma of bone (MPB), in whom PET/CT and the sFLC κ/λ ratio were useful for evaluating the response to treatment. The patient was diagnosed with MPB, with PET/CT showing multiple abnormal tracer uptakes in the scapula, spine, and ribs. The sFLC ratio was markedly elevated, with the κ chain level being especially high. We administered bortezomib and dexamethasone, after which the abnormal uptakes on PET/CT disappeared. The sFLC ratio and the FLC value also normalized, and have remained stable for more than one year, to date, since treatment. In our case, PET/CT and the sFLC κ/λ ratio were found to be extremely useful for monitoring treatment responses.

Spectral line survey observations are conducted toward the high-mass protostar candidate NGC 2264 CMM3 in the 4 mm, 3 mm, and 0.8 mm bands with the Nobeyama 45 m telescope and the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope. In total, 265 emission lines are detected in the 4 mm and 3 mm bands, and 74 emission lines in the 0.8 mm band. As a result, 36 molecular species and 30 isotopologues are identified. In addition to the fundamental molecular species, many emission lines of carbon-chain molecules such as HC5N, C4H, CCS, and C3S are detected in the 4 mm and 3 mm bands. Deuterated molecular species are also detected with relatively strong intensities. On the other hand, emission lines of complex organic molecules such as HCOOCH3, and CH3OCH3 are found to be weak. For the molecules for which multiple transitions are detected, rotation temperatures are derived to be 7-33 K except for CH3OH. Emission lines with high upper-state energies (Eu > 150 K) are detected for CH3OH, indicating existence of a hot core. In comparison with the chemical composition of the Orion KL, carbon-chain molecules and deuterated molecules are found to be abundant in NGC 2264 CMM3, while sulfur-bearing species and complex organic molecules are deficient. These characteristics indicate chemical youth of NGC 2264 CMM3 in spite of its location at the center of the cluster forming core, NGC 2264 C., 70 pages, 35 figures, accepted for publication in ApJ

We have observed the clump G34.43+00.24 MM3 associated with an infrared dark cloud in DNC $J$=3--2, HN$^{13}$C $J$=3--2, and N$_2$H$^+$ $J$=3--2 with the Atacama Large Millimeter/submillimeter Array (ALMA). The N$_2$H$^+$ emission is found to be relatively weak near the hot core and the outflows, and its distribution is clearly anti-correlated with the CS emission. This result indicates that a young outflow is interacting with cold ambient gas. The HN$^{13}$C emission is compact and mostly emanates from the hot core, whereas the DNC emission is extended around the hot core. Thus, the DNC and HN$^{13}$C emission traces warm regions near the protostar differently. The DNC emission is stronger than the HN$^{13}$C emission toward most parts of this clump. The DNC/HNC abundance ratio averaged within a $15^{\prime\prime} \times 15^{\prime\prime}$ area around the phase center is higher than 0.06. This ratio is much higher than the value obtained by the previous single-dish observations of DNC and HN$^{13}$C $J$=1--0 ($\sim$0.003). It seems likely that the DNC and HNC emission observed with the single-dish telescope traces lower density envelopes, while that observed with ALMA traces higher density and highly deuterated regions. We have compared the observational results with chemical-model results in order to investigate the behavior of DNC and HNC in the dense cores. Taking these results into account, we suggest that the low DNC/HNC ratio in the high-mass sources obtained by the single-dish observations are at least partly due to the low filling factor of the high density regions., Comment: accepted to ApJ

A parametric X-ray radiation (PXR) generator system was constructed in 2001 in a dedicated beamline connected to the 125 MeV electron linac of the Laboratory for Electron Beam Research and Application at Nihon University. This generator system consists of two perfect-silicon-crystal plates mounted on precisely moving mechanical setup to achieve a wide tunability. The experimental operation of the PXR generator started early in 2004; X-rays were first observed through this device in April 2004. Application studies using the PXR beam from a 100 MeV electron beam have been conducted since July 2004. Preliminary results suggest the possibility of applying the PXR to advanced X-ray imaging and to the measurement of X-ray absorption fine structure.

We have mapped the W3 giant molecular cloud in the C0 3P1-3P0 ([C I] 492 GHz) and 12CO J = 3-2 emission lines with the Mount Fuji Submillimeter-wave Telescope. The [C I] distribution is extended over the molecular cloud, having peaks at three star forming clouds, W3 Main, W3(OH), and AFGL 333. The [C I] emission is found to be strong in the AFGL 333 cloud, where the 12CO J = 3-2 emission is relatively weak. In order to characterize the physical and chemical states of the AFGL 333 cloud, we have also observed the CO J = 1-0 isotopomer lines and the CCS and N2H+ lines with the Nobeyama Radio Observatory 45 m Telescope. The [C0]/[CO] and [CCS]/[N2H+] abundance ratios are found to be higher in the AFGL 333 cloud than in the W3(OH) cloud, suggesting that the AFGL 333 cloud is younger than the W3(OH) cloud. In the AFGL 333 cloud we have found two massive cores without any sign of active star formation. They are highly gravitationally bound and are regarded as good candidates for a massive prestellar core.

Objectives: To clarify the relationship between oral condition and health status, particularly bone mineral density (BMD), in the elderly aged 80 years or more. Methods: We examined the oral conditions and health status of two groups. One was elderly who lived at home and had at least 20 teeth at the age of 80 (8020 elderly). The other group consisted of elderly people residing in long-term care facilities (institutionalized elderly). The oral conditions we examined were the number of teeth, masticatory ability, occlusal force, stimulated salivary flow rate, saliva buffer ability, community periodontal index (CPI) and salivary occult blood test. The health status indicators we examined were BMD, grip strength, height, weight and body mass index (BMI). Results: The number of teeth, stimulated salivary flow rate, masticatory ability, and occlusal force in the 8020 elderly were significantly higher than in the institutionalized elderly. BMD, grip strength, height, weight and BMI in these 8020 elderly were also significantly higher than in the institutionalized elderly. Masticatory ability and occlusal force in the institutionalized elderly with high BMD (high BMD group) were significantly higher than in the institutionalized elderly with low BMD (low BMD group). Grip strength, height and weight in the high BMD group were higher than in the low BMD group. Conclusions: The 8020 elderly had good oral condition and health status compared to the institutionalized elderly. There may be a relationship between number of teeth and BMD in elderly aged 80–84.

Parametric X-rays (PXR) are a new type of X-ray that are generated by crystal-electron interactions. The Laboratory for Electron Beam Research and Application (LEBRA) at Nihon University generates PXR using a double-crystal system generating electrons from a 100-MeV class LINAC. LEBRA-PXR has potential for use as a wavelength tunable, ultra-high bright X-ray source with a macro-/micro-pulse structure. LEBRA-PXR has an energy-dispersion in the horizontal axis, assumed to be 0.2% in the experimental window, but can be used as monochromatic X-ray source for diffraction using a simple slit-system. A diffraction experiment was successfully carried out by applying an 11 keV, or 1.1273 A, LEBRA-PXR. Near-perfect crystals, such as graphite used for a monochromator showed sharp diffraction peaks. Clear, transparent mineral quartz and fluorapatite crystals also showed sharp diffraction peaks, while the diffraction peaks from clear calcite and silicon powder were not detected. Possible reasons for the lack of diffraction peaks from these materials are discussed. LEBRA-PXR has potential for use in studies on the diffraction of other materials, and is therefore, expected to be a useful tool for crystallographic analysis.

This paper discusses the integrated design of structural shape and controller of high-speed positioning actuators for magnetic recording test stands. To allow highly flexible shape design of the mechanism for the positioning actuator and to improve the calculation efficiency in the structural shape optimization, this paper proposes an integrated design method in which a structural shape is defined like as a skeleton and meats and a genetic algorithm is used to search the combination of the skeleton and meats for obtaining better performance of the closed-loop system in iterative design procedure. The iterative optimization procedure includes the shape and the controller updates. It is shown in design examples that the proposed integrated design method can improve the performance of the positioning actuator according to the performance indices, and the effect is verified.

Compositions and spatial distribution patterns of buried viable seeds, and demographic transition from buried viable seeds to seedlings after clear-cutting were examined in a 75-year-old conifer plantation in southwest Japan. A part of the plantation was cleared in December 1997 and study plots were set up on a cleared site and a preserved site. Soil samples (a total of 105l for the preserved plot and 90l for the cleared plot) were collected from surface soils in spring 1998 and were incubated in a greenhouse for 120 days. There were an estimated 1064 buried viable seeds per square meter from 67 species in the preserved plot and 1754 seeds/m2 from 53 species in the cleared plot. The soil seed bank was from mostly low density species with some high density species, and contained many pioneer species that were absent in the floor vegetation. Buried viable seeds were clumped together, especially in gravity-dispersal species. Although plenty of buried viable seeds were pooled in the soil, few seedling...

We have mapped the W 3 giant molecular cloud in the ([CI]) line with the Mount Fuji Submillimeter-wave Telescope. The [CI] emission is extended over the molecular cloud, having peaks at three star forming clouds; W 3(Main), W 3(OH), and AFGL 333. The [CI] emission is found to be strong in the AFGL 333 cloud. We have also observed the , and lines by using the Nobeyama Radio Observatory 45 m telescope. In the AFGL 333 cloud, we find two massive cores, which are highly gravitationally bound and have no sign of active star formation. The high []/[CO] and [CCS]/[] abundance ratios suggest that the AFGL 333 cloud is younger than the W 3(Main) and W 3(OH) clouds.

We have constructed the Mount Fuji submillimeter-wave telescope at Nishiyasugawara (alt. 3725 m) near the summit of Mt. Fuji (alt. 3774 m). Thanks to the excellent condition of Mt. Fuji, we have successfully carried out the [CI] survey toward more than 40 square degrees of sky, including qrion MC, Taurus MC, Rosetta MC, DR 15, DR 21, NGC 1333, NGC 2264, W 3, W 44, W 51, L 134, p-Oph. Our [CI] survey have revealed that the [CI] 492 GHz emission widely extends to the molecular clouds. The spatial and velocity structures of the [CI] 492 GHz emission resemble those of 13CO J

本報では、基礎基本を押さえるとともに、能動的な学習の展開を目指し、中学校技術・家庭科「技術とものづくり」の学習において、材料の選定と生徒の生活に密着した製作題材の検討を行った。さらに、日常的な評価活動の他に、製作後の活用レポートを取り入れた評価を実施することにより、次のものづくり活動への能動的態度の育成を目指した。