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Migration of newborn neurons is essential for brain morphogenesis and circuit formation, yet controversy exists regarding how neurons generate the driving force against strong mechanical stresses in crowded neural tissues. We found that cerebellar granule neurons adopt differential motility modes in distinct extracellular environments. In 3-dimensional (3D) confinement, actomyosin produces contractile forces at the posterior cell membrane, in addition to the traction force in the leading process that is exclusively observed in 2D cultures. The 3D migration is initiated by activation of a mechanosensitive channel PIEZO1. PIEZO1-induced calcium influx in the soma triggers the PKC-ezrin cascade, which recruits actomyosin to the posterior plasma membrane. Thus, migrating neurons use a mechano-sensing mechanism to activate multiple driving forces to maneuver in irregular brain tissue.One-Sentence SummaryCerebellar granule neurons use a mechanosensor PIEZO1 to switch migratory modes in confined spaces.

The Atacama Large Millimeter/submillimeter Array (ALMA) serendipitously detected H$_2$O $J_{Ka, Kc} = 10_{2,9} - 9_{3,6}$ emission at 321 GHz in NGC 1052. This is the first submillimeter maser detection in a radio galaxy and the most luminous 321-GHz H$_2$O maser known to date with the isotropic luminosity of 1090 $L_{\odot}$. The line profile consists of a broad velocity component with FWHM $= 208 \pm 12$ km s$^{-1}$ straddling the systemic velocity and a narrow component with FWHM $= 44 \pm 3$ km s$^{-1}$ blueshifted by 160 km s$^{-1}$. The profile is significantly different from the known 22-GHz $6_{1,6} - 5_{2,3}$ maser which shows a broad profile redshifted by 193 km s$^{-1}$. The submillimeter maser is spatially unresolved with a synthesized beam of $0^{\prime \prime}.68 \times 0^{\prime \prime}.56$ and coincides with the continuum core position within 12 pc. These results indicate amplification of the continuum emission through high-temperature ($>1000$ K) and dense ($n({\rm H}_2{\rm O}) > 10^4$ cm$^{-3}$) molecular gas in front of the core, 3 figures, Accepted for publication in Publications of Astronomical Society of Japan

We study properties of the interstellar medium, an ingredient of stars, and star formation activity, in four nearby galaxy pairs in the early and mid stages of interaction for both a galaxy scale and a kpc scale. The galaxy-scale Kennicutt-Schmidt law shows that seven of eight interacting galaxies have a star formation rate within a factor of three compared with the best-fit of the isolated galaxies, although we have shown that molecular hydrogen gas is efficiently produced from atomic hydrogen during the interaction in the previous paper. The galaxy-scale specific star formation rate (sSFR) and star formation efficiency (SFE) in interacting galaxies are comparable to those in isolated galaxies. We also investigate SFE and the Kennicutt-Schmidt law on a kpc scale. The spatial distributions of SFE reveal that SFE is locally enhanced, and the enhanced regions take place asymmetrically or at off-centre regions. The local enhancement of SFE could be induced by shock. We find that the index of the Kennicutt-Schmidt law for the interacting galaxies in the early stage is 1.30$\pm$0.04, which is consistent with that of the isolated galaxies. Since CO emission, which is used in the Kennicutt-Schmidt law, is a tracer of the amount of molecular gas, this fact suggests that dense gas, which is more directly connected to star formation, is not changed at the early stage of interaction., 40 pages, 15 figures, 10 tables; accepted for publication in PASJ

The Atacama Large Millimeter/submillimeter Array can achieve unprecedented spatial resolutions of 15 to 5 mas with the longest baselines of 16 km and observing at the highest frequencies of 275–950 GHz (1.09–0.30 mm). Two conditions are paramount for successful observations at these frequencies: a phase calibrator in close proximity to the science target and a stable-enough atmosphere to provide a low residual phase rms post-phase-referencing. We investigate the effect of phase-referencing cycle times, for in-band and band-to-band (B2B) observing techniques, using close and distant phase calibrators, at bands 7, 8, and 9 for baselines >2000 m. We find that (1) the phase rms estimated from baselines longer than the effective baseline increases as a function of time . (2) The expected coherence estimated using the expected phase rms corresponds well to the achieved image coherence. (3) Faster phase-referencing cycle times (

We present a method to mitigate the atmospheric effects (residual atmospheric lines) in single-dish radio spectroscopy caused by the elevation difference between the target and reference positions. The method is developed as a script using the Atmospheric Transmission at Microwaves (ATM) library built into the Common Astronomy Software Applications (CASA) package. We apply the method to the data taken with the Total Power Array of the Atacama Large Millimeter/submillimeter Array. The intensities of the residual atmospheric (mostly O3) lines are suppressed by, typically, an order of magnitude for the tested cases. The parameters for the ATM model can be optimized to minimize the residual line and, for a specific O3 line at 231.28 GHz, a seasonal dependence of a best-fitting model parameter is demonstrated. The method will be provided as a task within the CASA package in the near future. The atmospheric removal method we developed can be used by any radio/millimeter/submillimeter observatory to improve the quality of its spectroscopic measurements., 21 pages, 12 figures, accepted for publication in PASP

The Atacama Large millimeter/submillimeter Array (ALMA) obtains spatial resolutions of 15 to 5 milli-arcsecond (mas) at 275-950GHz (0.87-0.32mm) with 16km baselines. Calibration at higher-frequencies is challenging as ALMA sensitivity and quasar density decrease. The Band-to-Band (B2B) technique observes a detectable quasar at lower frequency that is closer to the target, compared to one at the target high-frequency. Calibration involves a nearly constant instrumental phase offset between the frequencies and the conversion of the temporal phases to the target frequency. The instrumental offsets are solved with a differential-gain-calibration (DGC) sequence, consisting of alternating low and high frequency scans of strong quasar. Here we compare B2B and in-band phase referencing for high-frequencies ($>$289GHz) using 2-15km baselines and calibrator separation angles between $\sim$0.68 and $\sim$11.65$^{\circ}$. The analysis shows that: (1) DGC for B2B produces a coherence loss $$2.42$^{\circ}$ ). (3) For more distant calibrators, B2B is preferred if it provides a calibrator $\sim$2$^{\circ}$ closer than the best in-band calibrator. (4) Decreasing image coherence and poorer image quality occur with increasing phase calibrator separation angle because of uncertainties in the antenna positions and sub-optimal phase referencing. (5) To achieve $>$70% coherence for long-baseline (16 km) band 7 (289GHz) observations, calibrators should be within $\sim$4$^{\circ}$ of the target., Comment: 17 Figures, 10 Tables

In 2017, an Atacama Large Millimeter/submillimeter Array (ALMA) high-frequency long baseline campaign was organized to test image capabilities with baselines up to 16 km at submillimeter (submm) wavelengths. We investigated image qualities using ALMA receiver Bands 7, 8, 9, and 10 (285-875 GHz) by adopting band-to-band (B2B) phase referencing in which a phase calibrator is tracked at a lower frequency. For B2B phase referencing, it is expected that a closer phase calibrator to a target can be used, comparing to standard in-band phase referencing. In the first step, it is ensured that an instrumental phase offset difference between low- and high-frequency Bands can be removed using a differential gain calibration in which a phase calibrator is certainly detected while frequency switching. In the next step, comparative experiments are arranged to investigate the image quality between B2B and in-band phase referencing with phase calibrators at various separation angles. In the final step, we conducted long baseline imaging tests for a quasar at 289 GHz in Band 7 and 405 GHz in Band 8 and complex structure sources of HL Tau and VY CMa at ~670 GHz in Band 9. The B2B phase referencing was successfully applied, allowing us to achieve an angular resolution of 14x11 and 10x8 mas for HL Tau and VY CMa, respectively. There is a high probability of finding a low-frequency calibrator within 5.4 deg in B2B phase referencing, bright enough to use an 8 s scan length combined with a 7.5 GHz bandwidth., Comment: 61 pages, 17 figures, 8 tables

We present spatial variations of the CO J = 2−1/1–0 line ratio (R_(21/10)) in the barred spiral galaxy M83 using Total Power Array (single-dish telescopes) data from the Atacama Large Millimeter/submillimeter Array. While the intensities of these two lines correlate tightly, R_(21/10) varies over the disk, with a disk average ratio of 0.69, and shows the galactic center and a two-arm spiral pattern. It is high (>̰0.7) in regions of high molecular gas surface density (Σ_(mol)), but ranges from low to high ratios in regions of low Σ_(mol). The ratio correlates well with the spatial distributions and intensities of far-ultraviolet (FUV) and infrared (IR) emissions, with FUV being the best correlated. It also correlates better with the ratio of specific intensities at 70 and 350 μm, a proxy for dust temperature, than with the IR intensities. Taken together, these results suggest either a direct or indirect link between the dust heating by the interstellar radiation field and the condition of giant molecular clouds (GMCs), even though no efficient mechanism is known for a thermal coupling of dust and bulk gas in GMCs. We speculate that the large spread of R_(21/10)in low Σ_(mol) regions, mostly at the downstream sides of spiral arms, may be due to the evolution of massive stars after spiral arm passage. Having in a late phase escaped from the spiral arms and their parental clouds, they may contribute to the dust heating by FUV and gas heating by cosmic rays produced by supernovae.

Spherical gold nanoparticles with cationic surfaces were prepared in hexadecyltrimethylammonium (CTA(+)) chloride (CTAC) and CTA(+) bromide (CTAB) solutions. In a CTAC solution, ascorbic acid reduction of gold ions (AuCl4(-)) induced spontaneous nucleation of gold clusters, which resulted in the formation of small gold nanoparticles (

The Atacama Large Millimeter-submillimeter Array (ALMA) radio telescope has commenced science observations of the Sun starting in late 2016. Since the Sun is much larger than the field of view of individual ALMA dishes, the ALMA interferometer is unable to measure the background level of solar emission when observing the solar disk. The absolute temperature scale is a critical measurement for much of ALMA solar science, including the understanding of energy transfer through the solar atmosphere, the properties of prominences, and the study of shock heating in the chromosphere. In order to provide an absolute temperature scale, ALMA solar observing will take advantage of the remarkable fast-scanning capabilities of the ALMA 12m dishes to make single-dish maps of the full Sun. This article reports on the results of an extensive commissioning effort to optimize the mapping procedure, and it describes the nature of the resulting data. Amplitude calibration is discussed in detail: a path that utilizes the two loads in the ALMA calibration system as well as sky measurements is described and applied to commissioning data. Inspection of a large number of single-dish datasets shows significant variation in the resulting temperatures, and based on the temperature distributions we derive quiet-Sun values at disk center of 7300 K at lambda=3 mm and 5900 K at lambda=1.3 mm. These values have statistical uncertainties of order 100 K, but systematic uncertainties in the temperature scale that may be significantly larger. Example images are presented from two periods with very different levels of solar activity. At a resolution of order 25 arcsec, the 1.3 mm wavelength images show temperatures on the disk that vary over about a 2000 K range., Comment: Solar Physics, accepted: 24 pages, 13 figures

We present a new package for joint deconvolution of ALMA 12m, 7m, and Total Power (TP) data, dubbed ``Total Power Map to Visibilities (TP2VIS)". It converts a TP (single-dish) map into visibilities on the CASA platform, which can be input into deconvolvers (e.g., CLEAN) along with 12m and 7m visibilities. A manual is presented in the Github repository (https://github.com/tp2vis/distribute). Combining data from the different ALMA arrays is a driver for a number of science topics, namely those that probe size scales of extended and compact structures simultaneously. We test TP2VIS using model images, one with a single Gaussian and another that mimics the internal structures of giant molecular clouds. The result shows that the better uv coverage with TP2VIS visibilities helps the deconvolution process and reproduces the model image within errors of only 5% over two orders of magnitude in flux., Accepted to PASP. Software distribution: https://github.com/tp2vis/distribute

9,10-Diacetyl-2,7-di- tert- butyl- trans -10b,10c-dimethyl-10b,10c-dihydropyrene annelated with a quinoxaline unit (q-DM-DHP, 3 ) was prepared from 5,13-di- tert -butyl-8,16-dimethyl[2.2]metacyclophane-1,2,9,10-tetraoxide ( 2 ) and o -phenylenediamine in two steps. The photochromic isomers of q-DM-DHP 3 , closed form 3a and open form 3b , were separated by reverse-phase HPLC, and their isolated UV–visible spectra were estimated. The chiral HPLC analyses of q-DM-DHP 3 indicated their planar chirality, and their CD spectra were measured. The photochromic properties and thermodynamic properties of 3 were also discussed based on their UV–visible, 1 H NMR, CD, and fluorescence spectra.

The relationship between molecular gel-forming compound-based double-alkylated L-glutamide-derived functional group-integrated organic phase (Sil-FIP) structure and chromatographic performance is investigated and compared with widely used alkyl phases (C(30), polymeric and monomeric C(18)) as references. The functional group-integrated molecular gel on silica is chemically designed newly in a way that the weak interaction sites are integrated with high orientation and high selectivity can be realized by multiple interactions with the solutes. Its functions can be emphasized by being immobilizable with a terminal carboxyl group and the fact that five amide bonds including β-alanine subunit are integrated per molecule. Furthermore, its self-assembling function can be detected by monitoring of the chiroptical property. Temperature-dependent circular dichroism (CD) intensity was determined as an indicator of chirality for the gel forming compounds. (13)C cross-polarization magic angle spinning (CP/MAS) NMR spectra of the Sil-FIP phase indicate that predominance of gauche conformations exists at higher temperature (above 30 °C). (29)Si CP/MAS NMR were carried out to investigate the degree of cross-linking of the silane and silane functionality of the modified silica. Temperature-dependent (13)C CP/MAS NMR and suspended-state (1)H NMR measurements of the Sil-FIP phase exhibit the dynamic behavior of the alkyl chains. To correlate the NMR and CD results with temperature-dependent chromatographic studies, standard reference materials (SRM 869b and SRM 1647e), column selectivity test mixture for liquid chromatography was employed. Additional shape selectivity text mixtures were also used to clarify the mechanism of shape selectivity performance of Sil-FIP compared with commercially available columns. The evaluation with the spectroscopic and chromatographic analyses presents very important information on the surface morphology of the new organic phase and the molecular recognition process. Integrated and ordered functional groups were investigated to be the main driving force for very high molecular shape selectivity of the Sil-FIP phase.

The drying characteristics of a relatively large wet material immersed in a fluidized bed of inert particles were examined theoretically. Calculations of heat transfer and evaporation of water on the material surface were included in a discrete element method–computational fluid dynamics (DEM-CFD) simulation. Only the preheating and constant drying rate periods were considered in the simulation. Our simulation made it possible to calculate the relation between the behavior of the fluidizing particles and the drying characteristics. The drying rate increased with an increase in the number of fluidizing particles in contact with the material and the number of fluidizing particles changed with time; that is, the drying rate fluctuated. When the drying rate increased, the fluid temperature decreased and the vapor content of the fluid increased around the material; that is, the temperature and vapor content of the fluid were associated with the behavior of the fluidizing particles.

We present the results of the Nobeyama Radio Observatory (NRO) M33 All Disk (30'x30' or 7.3 kpc x 7.3 kpc) Survey of Giant Molecular Clouds (NRO MAGiC) based on 12CO (1-0) observations using the NRO 45-m telescope. The spatial resolution of the resultant map is 19".3, corresponding to 81 pc, which is sufficient to identify each Giant Molecular Cloud (GMC) in the disk. We found clumpy structures with a typical spatial scale of ~100 pc, corresponding to GMCs, and no diffuse, smoothly distributed component of molecular gas at this sensitivity. Closer inspection of the CO and HI maps suggests that not every CO emission is associated with local HI peaks, particularly in the inner portion of the disk (r < 2 kpc), although most of CO emission is located at the local HI peaks in the outer radii. We found that most uncovered GMCs are accompanied by massive star-forming regions, although the star formation rates (SFRs) vary widely from cloud to cloud. The azimuthally averaged H{\sc i} gas surface density exhibits a flat radial distribution. However, the CO radial distribution shows a significant enhancement within the central 1-2 kpc region, which is very similar to that of the SFR. We obtained a map of the molecular fraction, f_mol = Sigma_H_2/(Sigma_HI+Sigma_H_2, at a 100-pc resolution. This is the first f_mol map covering an entire galaxy with a GMC-scale resolution. We find that f_mol tends to be high near the center. The correlation between f_mol and gas surface density shows two distinct sequences. The presence of two correlation sequences can be explained by differences in metallicity, i.e., higher (~ 2-fold) metallicity in the central region (r< 1.5 kpc) than in the outer parts. Alternatively, differences in scale height can also account for the two sequences, i.e., increased scale height toward the outer disk., Accepted for publication in PASJ, See http://www.juen.ac.jp/lab/tosaki/paper/astro-ph/2011/tosaki2011.pdf for a version with full resolution figures

We present wide-field 1.1 mm continuum imaging of the nearby spiral galaxy M 33, conducted with the AzTEC bolometer camera on ASTE. We show that the 1.1 mm flux traces the distribution of dust with T ~20 K. Combined with far-infrared imaging at 160um, we derive the dust temperature distribution out to a galactic radius of ~7 kpc with a spatial resolution of ~100 parsecs. Although the 1.1 mm flux is observed predominantly near star forming regions, we find a smooth radial temperature gradient declining from ~20 K to ~13 K, consistent with recent results from the Herschel satellite. Further comparison of individual regions show a strong correlation between the cold dust temperature and the Ks band brightness, but not with the ionizing flux. The observed results imply that the dominant heating source of cold dust at few hundred parsec scales are due to the non-OB stars, even when associated with star forming regions., Comment: Accepted for publication in PASJ

Pyrene-doped l -glutamide-based lipidic derivatives with different alkyl lengths (Cn-g-Pyr; n = 4, 8 and 12) were newly synthesized. All of the Cn-g-Pyr dissolved and showed thermotopically and lyotropically-induced excimer formations accompanied by induction of the positive Cotton effect in their CD spectra, indicating chirally ordered stacking. However, when C4-g-Pyr and C12-g-Pyr were mixed in a certain molar ratio, an unusual CD pattern from positive to negative ones was observed. In this study, energy transfer efficiency was investigated in a binary system of Cn-g-Pyr with C12-g-TPP. The results revealed that simple modification of the alkyl length of Cn-g-Pyr enables enhancement of the energy transfer efficiency with C12-g-TPP.

The hemisphere-shaped calixarene 1a and its split-hemisphere-shaped isomer 1b were synthesized from [2.1.2.1]metacyclophane (MCP) 3 by pinacol rearrangement and subsequent intramolecular acetalization. Their structures were revealed by X-ray crystallography and 1 H NMR spectroscopy. The temperature-dependence of the intramolecular acetalization to provide 1a and 1b was examined. The results indicated that 1a is the dominant product at high temper a ture s , and the value s of Δ H ° and Δ S ° were estimated to be −18.3±0.37 kJ mol −1 , −59.1±1.12 kJ mol −1 K −1 , respectively. The dinitro derivative 7 and tetranitro derivative s 8 were obtained by ipso -nitration at the upper rims of 1a . The optical resolution and chiral recognition ability of racemic mixture 7 were investigated by HPLC systems.

We have mapped the nearby face-on spiral galaxy M 33 in the 1.1 mm dust continuum using AzTEC on Atacama Submillimeter Telescope Experiment (ASTE). The preliminary results are presented here. The observed dust has a characteristic temperature of ~ 21 K in the central kpc, radially declining down to ~ 13 K at the edge of the star forming disk. We compare the dust temperatures with KS band flux and star formation tracers. Our results imply that cold dust heating may be driven by long-lived stars even nearby star forming regions.

We have conducted all disk imaging of M33 in 12CO(1-0) using the 45-m telescope at Nobeyama Radio Observatory. We present preliminary results of this project. The spatial resolution of ~ 80 pc is comparable to the size of GMCs. The identified GMCs show wide variety in star forming activity. The variety can be regarded as the difference of their evolutionary stage. We found that Kennicutt-Schmidt law breaks in GMC scale (~ 80 pc), although it is still valid in 1 kpc scale. The correlation between molecular gas fraction, fmol = Σ(H2)/Σ(HI+H2) and gas surface density shows two distinct sequences and shows that fmol tends to be higher near the center. We also made partial mapping 12CO(3-2) with ASTE telescope. These data show that the variation of physical properties of molecular gas are correlated with the GMC evolution and mass. That is, GMCs with more active star formation and more mass tend to have higher fraction of dense gas.

We observed five giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) in the 12CO J=1-0 line using the Atacama Large Millimeter/submillimeter Array (ALMA). The sample includes four GMCs with some signs of star formation -- either YSOs, H II regions, and/or young clusters -- and one quiescent GMC without any sign of massive star formation. The data from the ALMA 12 m, 7 m, and Total-Power arrays are jointly deconvolved to obtain high-fidelity images at high spatial resolution (3 arcsec = 0.7 pc). The four star-forming GMCs show very complex structures with clumps and filaments. The quiescent GMC shows a relatively diffuse, extended emission distribution without prominent clumps or filaments. This difference is similar to that between structured molecular gas in Milky Way spiral arms and unstructured gas in the inter-arm regions. We characterize the difference with the brightness distribution function and brightness distribution index. In conjunction with other ALMA studies of GMCs in the LMC, the five GMCs tentatively form an evolutionary trend: from less structured, quiescent GMCs to more structured, actively star-forming GMCs. A future ALMA study will be able to map molecular clouds over the LMC and reveal the evolutionary sequence of molecular clouds., 15 pages, 8 figures

We have mapped the northern area (30' ? 20') of a Local Group spiral galaxy M33 in 12CO(J = 1-0) line with the 45 m telescope at the Nobeyama Radio Observatory. Along with H? and Spitzer 24 ?m data, we have investigated the relationship between the surface density of molecular gas mass and that of star formation rate (SFR) in an external galaxy (Kennicutt-Schmidt law) with the highest spatial resolution (~80 pc) to date, which is comparable to scales of giant molecular clouds (GMCs). At positions where CO is significantly detected, the SFR surface density exhibits a wide range of over four orders of magnitude, from ?SFR 10?10 to ~10?6 M ? yr?1 pc?2, whereas the values are mostly within 10-40 M ? pc?2. The surface density of gas and that of SFR correlate well at an ~1 kpc resolution, but the correlation becomes looser with higher resolution and breaks down at GMC scales. The scatter of the ?SFR- relationship in the ~80?pc resolution results from the variety of star-forming activity among GMCs, which is attributed to the various evolutionary stages of GMCs and to the drift of young clusters from their parent GMCs. This result shows that the Kennicutt-Schmidt law is valid only in scales larger than that of GMCs, when we average the spatial offset between GMCs and star-forming regions, and their various evolutionary stages.

Three thiophene-containing compounds were newly synthesized as low molecular weight blocks to construct non-covalent and highly ordered π-conjugation systems. Typical emission enhancement and quenching based on the J- and H-type orientations, respectively, of the thiophene moiety were realized and controlled by lipid membrane-like phase transition and separation behaviours.

In this study, 9,10-diacetoxyl-2,7-di- tert -butyl- trans -10b,10c-dimethyl-10b,10c-dihydropyrene annelated with a dihydrothieno[3.4- b ]pyrazine unit ( 1a ) was prepared, for the first time, from 5,13-di- tert -butyl-8,16-dimethyl-1,2,9,10-tetrahydroxy[2.2]metacyclophane and 3,4-diaminothiophene in two steps. The photoisomerization property of 1 was investigated by UV and 1 H NMR spectroscopies, and the quantitative isomerization between the more stable dihydropyrene (DHP) form and the less stable metacyclophane-diene (MCPD) form was observed. A thermally induced return reaction from the MCPD to the DHP form was examined at various temperatures, and the reaction rate was 0.0049 min −1 at 45 °C, which is slower than that of the parent MCPD.

The L-glutamide derivative with double long-chain alkyl groups and a pyrenyl head group (Pyr-lipid) worked as organogelator in benzene and cyclohexane. Gelation was brought about through network formation with well-developed fibrous aggregates based on lipid membrane-like highly-oriented structures. Gelation was observed in polymerizable monomers such as methyl methacrylate (MMA) and styrene (St). Extremely intense CD spectra were observed at the absorption band of pyrenyl group in a monomer solution at gel-forming temperature, but the intensity decreased remarkably at the sol-forming temperature. The transparent solid sheet was obtained by photo-irradiation to the MMA gel in a quartz cell. More than 99% of MMA was polymerized even in the gel state and the weight-average molecular weight (M w ) of the resultant polymer was 7.2 × 10 4 g mol -1 . CD spectra indicated that chirally-oriented structures in the gel state were maintained after polymerization of MMA and were stable at the temperature above the original gel-to-sol transition temperature. Fluorescence spectra of Pyr-lipid in the monomer solutions supported that the pyrene excimer was formed in the lipid aggregates and the stabilization of the excimer formation was achieved by polymerization of MMA in the gel state.

Poly(2-N-carbazolylethyl acrylate) with terminal trimethoxysilyl groups was prepared as an organic phase and immobilized onto silica. The retention behavior of the column packed with this carbazole-based polymer-immobilized silica (Sil-CEA) was investigated by using various estrogenic steroids and corticoids in both reversed-phase and normal-phase liquid chromatography. As a result, complete separation was confirmed for eight kinds of steroids with Sil-CEA. The most specific separation with Sil-CEA can be emphasized by the high separation factor (e.g., alpha = 1.39 in methanol-water (7:3, v/v) at 35 degrees C) for 17alpha and 17beta-estradiols, one of the most difficult pairs of isomers in chromatographic separation, whereas for two kinds of commercially available polymeric ODS columns as references alpha = 1.01, only, under the same conditions. Because the excellent separation and retention order with Sil-CEA was maintained even in a normal-phase mobile phase such as a hexane-2-propanol, it is estimated that the CEA phase has multiple interaction mechanisms through stronger interactions such as dipole-dipole, carbonyl-pi, and hydrogen bonding interactions than the hydrophobic effect expected with ODS.

Self-assembling amphiphiles with unique chiroptical properties were derived from L-glutamic acid through omega-aminoalkylation and double long-chain alkylation. These amphiphiles can disperse in various solvents ranging from water to n-hexane. TEM and SEM observations indicate that the improvement in dispersity is induced by the formation of tubular and/or fibrillar aggregates with nanosized diameters, which makes these amphiphiles similar to aqueous lipid membrane systems. Spectroscopic observations, such as UV-visible and CD spectroscopies indicate that the aggregates are constructed on the basis of S- and R-chirally ordered structures through interamide interactions in water and organic media, respectively, and that these chiroptical properties can be controlled thermotropically and lyotropically. It is also reported that the chiral assemblies provide specific binding sites for achiral molecules and then induce chirality for the bonded molecules. Further, the applicability of the amphiphiles to template polymerization is discussed.

We present a new on-the-fly mapping of CO (J = 3-2) line emission with the Atacama Submillimeter Telescope Experiment toward the 8' x 8' (or 10.5 x 10.5 kpc at the distance of 4.5 Mpc) region of the nearby barred spiral galaxy M 83 at an effective resolution of 25''. Due to its very high sensitivity, our CO (J = 3 - 2) map can depict not only spiral arm structures but also spur-like substructures extended in inter-arm regions. This spur-like substructures in CO (J = 3-2) emission are well coincident with the distribution of massive star-forming regions traced by Halpha luminosity and Spitzer/Infrared Array Camera 8 mum emission. We have identified 54 CO (J = 3-2) clumps as Giant Molecular-cloud Associations (GMAs) employing the CLUMPFIND algorithm, and have obtained their sizes, velocity dispersions, virial masses, and CO luminosity masses. We found that the virial parameter alpha, which is defined as the ratio of the virial mass to the CO luminosity mass, is almost unity for GMAs in spiral arms, whereas there exist some GMAs whose alpha are 3-10 in the inter-arm region. We found that GMAs with higher alpha tend not to be associated with massive star-forming regions, whilemore » other virialized GMAs are. Since alpha mainly depends on velocity dispersion of the GMA, we suppose that the onset of star formation in these unvirialized GMAs with higher alpha are suppressed by an increase in internal velocity dispersions of giant molecular clouds within these GMAs due to shear motion.« less

Poly(2-N-carbazolylethyl acrylate) having terminal trimethoxysilyl groups was newly synthesized by radical polymerization and immobilized onto the silica surface (Sil-CEA). The chromatographic property of Sil-CEA was examined by applying polycyclic aromatic hydrocarbons as solutes. Poly(4-vinylpyridine)-modified silica (Sil-VP) and monomeric octadecylated silica (ODS) columns were used as the reference columns. Less sensitivity to molecular hydrophobicity and enhanced molecular planarity selectivity were obtained with Sil-CEA compared to ODS. On the other hand, high retention factors for the analyzed solutes and an opposite elution order for linear and disc-shaped solutes were obtained with Sil-CEA compared with Sil-VP. In this paper, the application for separation of tocopherols was also described.

We report the highest-fidelity observations of the spiral galaxy M51 in CO emission, revealing the evolution of giant molecular clouds (GMCs) vis-a-vis the large-scale galactic structure and dynamics. The most massive GMCs (so-called GMAs) are first assembled and then broken up as the gas flow through the spiral arms. The GMAs and their H2 molecules are not fully dissociated into atomic gas as predicted in stellar feedback scenarios, but are fragmented into smaller GMCs upon leaving the spiral arms. The remnants of GMAs are detected as the chains of GMCs that emerge from the spiral arms into interarm regions. The kinematic shear within the spiral arms is sufficient to unbind the GMAs against self-gravity. We conclude that the evolution of GMCs is driven by large-scale galactic dynamics --their coagulation into GMAs is due to spiral arm streaming motions upon entering the arms, followed by fragmentation due to shear as they leave the arms on the downstream side. In M51, the majority of the gas remains molecular from arm entry through the inter-arm region and into the next spiral arm passage., 6 pages, including 3 figures. Accepted, ApJL

We developed a new and short synthetic route to 2,7-di- TERT-butyl- TRANS-15,16-dimethyldihydropyrene(DHP) via tetra-hydroxy[2.2]metacyclophanein four reaction steps with a total yield of 37%. 2,7-Di- TERT-butyl- TRANS-15,16-dimethyldihydro-pyrenefunctionalized by acetoxy groups at 4-, 5-, 9-, 10-positions wassynthesized via 5,13-di- TERT-butyl-8,16-dimethyl-1,2,9,10-tetra-hydroxy[2.2]MCPin five reaction steps with a yield of 24%, and its DHPstructure was determined by ¹ H NMR spectroscopyand X-ray crystal-structure analysis.

An l -glutamide-functionalized tetraphenylporphyrin derivative has been newly synthesized. This can dissolve in various organic solvents to form nanofibrillar aggregates with both right-handed and left-handed chiral stacking structures among the porphyrin rings. It is also discussed on thermotropic and lyotropic phase transitions between gel and sol states.

Poly(4-vinylpyridine)-modified silica with high grafting density have been prepared by a grafting-from (g-from) approach through radical chain-transfer reactions. The widely used silane coupling agent 3-mercaptopropyltrimethoxysilane was used to prepare thiol-terminated silica. Chain-transfer reaction and polymerization of 4-vinylpyridine was carried out using alpha,alpha'-azobisisobutyronitrile as an initiator. Thiol-terminated silica and polymer-modified silica were both characterized qualitatively and quantitatively. The quantification of the organic phase has been done by thermogravimetric analysis and elemental analysis. Thus, the modified silica was used as a packing material and the retention behavior of polycyclic aromatic hydrocarbons (PAHs) was studied in normal-phase high-performance liquid chromatography. Results were compared with those of poly(4-vinylpyridine)-modified silica prepared by a grafting-to (g-to) approach. Commercially available aminopropyl-bonded silica and bare silica columns were also used as reference columns. The column of poly(4-vinylpyridine)-grafted silica prepared by the g-from method, having higher grafting density, provided the better retentivity and selectivity for PAHs compared to the other reference columns.

We report our recent progress on extragalactic spectroscopic and continuum observations, including HCN(J=1-0), HCO$^+$(J=1-0), and CN(N=1-0) imaging surveys of local Seyfert and starburst galaxies using the Nobeyama Millimeter Array, high-J CO observations (J=3-2 observations using the Atacama Submillimeter Telescope Experiment (ASTE) and J=2-1 observations with the Submillimeter Array) of galaxies, and $\lambda$ 1.1 mm continuum observations of high-z violent starburst galaxies using the bolometer camera AzTEC mounted on ASTE., Comment: 6 pages, 5 figures, To appear in proceedings of "Far-Infrared and Submillimeter Emission of the Interstellar Medium", EAS Publication Series, Bad Honnef, November 2007, Eds. C. Kramer, S. Aalto, R. Simon. See http://www.nro.nao.ac.jp/~f0212kk/FIR07/kk-ver20.pdf for a version with high resolution figures

Three isomers of [1.1]meta-stilbenophane were synthesized by the McMurry reaction of diarylmethane dialdehyde and their crystal structures and photochemical properties were investigated. X-ray crystallographic analyses of these isomers revealed that they were assigned to a trans–trans (t–t) form with a 1,3-alternate conformation, a cis–trans (c–t) form with a distorted-cone conformation, and a cis–cis (c–c) form with a 1,2-alternate conformation. A 1H NMR study indicated that a t–t isomer could be completely transformed into a 35:65 mixture of c–t and c–c isomers by photoirradiation at 254 nm.

Dihydropyrene (DHP) is 14π aromatic compound and applied as an aromatic probe by chemical shift of internal methyl groups in 1H-NMR spectra. DHP containing a nitrogen atom 1a and 2a were designed as photochromic compounds which were restrained thermal-isomerization. 1a and 2a were confirmed as DHP types by 1H-NMR spectra. Chemical shifts of internal methyl groups of 1a and 2a were observed at the lower magnetic field than that of DHP 3a . According to optimized structures of 1a and 3a , it was expected that the internal methyl group located of the out at center of 14π annulene ring. Isomerization to [2.2]metacyclophanediene 1b from DHP 1a by photo-irradiation of visible light was not observed.

[2.1.2.1]Metacyclophane ([2.1.2.1]MCP) 3 containing hydroxyl groups at the bridge is obtained by a pinacol coupling reaction using aluminum powder. The Albright-Gordman oxidation of [2.1.2.1]MCP 3 ...

We report the discovery of a high CO(J=3-2)/CO(J=1-0) ratio gas with an arc-like distribution (``high-ratio gas arc'') surrounding the central star cluster of the supergiant HII region NGC 604 in the nearby spiral galaxy M 33, based on multi-J CO observations of a 5' $\times$ 5' region of NGC 604 conducted using the ASTE 10-m and NRO 45-m telescopes. The discovered ``high-ratio gas arc'' extends to the south-east to north-west direction with a size of $\sim$ 200 pc. The western part of the high-ratio gas arc closely coincides well with the shells of the HII regions traced by H$\alpha$ and radio continuum peaks. The CO(J=3-2)/CO(J=1-0) ratio, R_{3-2/1-0}, ranges between 0.3 and 1.2 in the observed region, and the R_{3-2/1-0} values of the high-ratio gas arc are around or higher than unity, indicating very warm (T_kin > 60 K) and dense (n(H_2) > 10^{3-4} cm^{-3}) conditions of the high-ratio gas arc. We suggest that the dense gas formation and second-generation star formation occur in the surrounding gas compressed by the stellar wind and/or supernova of the first-generation stars of NGC 604, i.e., the central star cluster of NGC 604.

Accepted: 2003-10-29, 資料番号: SA1003561000

Melamine resin microcapsules were prepared by the batch method and microreactor method using sodium dodecyl sulfate (SDS) and 1.6R 6 A-3.5AA as emulsifiers. They contained about 50% toluene as indicated by thermogravimetric (TG) analysis. The mean sizes of the microcapsules obtained by using the microreactor method with SDS and with 1.6R 6 A-3.5AA were 462 ± 199 and 147 ± 31 nm, respectively. Microcapsules prepared by using a microreactor showed smaller particle diameters and a narrower particle size distribution than those obtained using a batch reactor.

An anthrylphenanthroimidazole-type clathrate host, which exhibits fluorescence enhancement behavior with the blue and red shift of the emission maximum upon formation of clathrates with amines, has been developed. The crystals of the title fluorescent clathrate compound with two fluorophores exhibit very different fluorescence behavior with different amines molecules. The crystal structures of the clathrate compounds have been determined by X-ray analysis. On the basis of the spectral data, the fluorescence lifetime and the crystal structures, the effects of the enclathrated guest on the solid-state photophysical properties of the clathrate compounds are discussed.

We present a method to derive positions of molecular clouds along the lines of sight from a comparison between 2.6 mm CO emission lines and 18 cm OH absorption lines, and apply it to the central region of the Milky Way. With some simple but justifiable assumptions, we derive a face-on distribution of the CO brightness and corresponding radial velocity in the Galactic center without the help of kinematical models. The derived face-on distribution of the gas is elongated and inclined so that the Galactic-eastern (positive longitude) side is closer to us. The gas distribution is dominated by a barlike central condensation, whose size is about 500 × 200 pc. The major axis of the condensation is tilted with respect to the line of sight by an angle of ≃70° (tilted by ≃40–50° from the large-scale stellar bar). This geometry resembles the central regions of barred galaxies. The velocity field shows highly noncircular motion in the central condensation. These characteristics agree with a picture in which the kinematics of the gas in the central hundreds of parsecs of the Galaxy is under the strong influence of a barred potential.

The title compound formed crystalline clathrates with ethanol in a 2:1 molar ratio and with water, acetic acid and imidazole in 1:1 molar ratios. The fluorescence behavior of the crystals are greatly dependent on the enclathrated molecules; the intensity increases in order of ethanol water>acetic acid>imidazole. The X-ray crystallographic analyses revealed marked effects of the guest molecules on the intermolecular host-to-host contacts and the intramolecular dihedral angles between the anthryl and phenanthroimidazolyl planes.