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Primary Percutaneous Coronary Intervention (PCI) has significantly contributed to reducing the mortality of patients with ST-segment elevation myocardial infarction (STEMI) even in cardiogenic shock and is now the standard of care in most of Japanese institutions. The Task Force on Primary PCI of the Japanese Association of Cardiovascular Interventional and Therapeutics (CVIT) society proposed an expert consensus document for the management of acute myocardial infarction (AMI) focusing on procedural aspects of primary PCI in 2018. Updated guidelines for the management of AMI were published by the European Society of Cardiology (ESC) in 2017 and 2020. Major changes in the guidelines for STEMI patients included: (1) radial access and drug-eluting stents (DES) over bare-metal stents (BMS) were recommended as a Class I indication, (2) complete revascularization before hospital discharge (either immediate or staged) is now considered as Class IIa recommendation. In 2020, updated guidelines for Non-ST-Elevation Myocardial Infarction (NSTEMI) patients, the followings were changed: (1) an early invasive strategy within 24 h is recommended in patients with NSTEMI as a Class I indication, (2) complete revascularization in NSTEMI patients without cardiogenic shock is considered as Class IIa recommendation, and (3) in patients with atrial fibrillation following a short period of triple antithrombotic therapy, dual antithrombotic therapy (e.g., DOAC and single oral antiplatelet agent preferably clopidogrel) is recommended, with discontinuation of the antiplatelet agent after 6 to 12 months. Furthermore, an aspirin-free strategy after PCI has been investigated in several trials those have started to show the safety and efficacy. The Task Force on Primary PCI of the CVIT group has now proposed the updated expert consensus document for the management of AMI focusing on procedural aspects of primary PCI in 2022 version.

Supplemental Material for Preventive Effects of Group Cognitive Behavioral Therapy in First-Year University Students at Risk for Depression: A Non-Randomized Controlled Trial by Sayaka Ogawa, Masaki Hayashida, Jun Tayama, Tatsuo Saigo, Naoki Nakaya, Toshimasa Sone, Masakazu Kobayashi, Peter Bernick, Atsushi Takeoka and Susumu Shirabe in Perceptual and Motor Skills

Product recommendation systems have been instrumental in online commerce since the early days. Their development is expanded further with the help of big data and advanced deep learning methods, where consumer profiling is central. The interest of the consumer can now be predicted based on the personal past choices and the choices of similar consumers. However, what is currently defined as a choice is based on quantifiable data, like product features, cost, and type. This paper investigates the possibility of profiling customers based on the preferred product design and wanted affects. We considered the case of vase design, where we study individual Kansei of each design. The personal aspects of the consumer considered in this study were decided based on our literature review conclusions on the consumer response to product design. We build a representative consumer model that constitutes the recommendation system's core using deep learning. It asks the new consumers to provide what affect they are looking for, through Kansei adjectives, and recommend; as a result, the aesthetic design that will most likely cause that affect., Comment: 11 pages, 10 figures, peer-reviewed at the KEER 2022 conference

Product recommendation systems have been instrumental in online commerce since the early days. Their development is expanded further with the help of big data and advanced deep learning methods, where consumer profiling is central. The interest of the consumer can now be predicted based on the personal past choices and the choices of similar consumers. However, what is currently defined as a choice is based on quantifiable data, like the product features, cost, and type. This paper investigates the possibility of profiling customers based on the preferred product design and wanted affects. We considered the case of vase design, where we study individual Kansei of each design. The personal aspects of the consumer considered in this study were decided based on our literature review conclusions on the consumer response to product design. We build a representative consumer model that constitutes the recommendation system's core using deep learning. It asks the new consumers to provide what affect they are looking for, through Kansei adjectives, and recommend; as a result, the aesthetic design that will most likely cause that affect.

In recent years, deep learning has attracted much attention and various techniques have been proposed. GAN (Generative adversarial networks) is one such method. GAN uses images as the training set and learns to generate new images that are indistinguishable from the training set. In this study, A GAN-based design method that generates new products from the images of the customer's favorite products is proposed. The product images that customers evaluated as preferable are used as the training set of GAN. If the GAN fulfills its capabilities properly, the images generated from a customer's favorite product are more likely to be preferred by the customer. In the case study, the proposed method was applied to chair design. The generated chair images were first evaluated in terms of image quality, and then evaluated by subjects.

Measurements of the luminosity function of active galactic nuclei (AGN) at high redshift ($z\gtrsim 6$) are expected to suffer from field-to-field variance, including cosmic and Poisson variances. Future surveys, such as those from the Euclid telescope and James Webb Space Telescope (JWST), will also be affected by field variance. We use the Uchuu simulation, a state-of-the-art cosmological $N$-body simulation with 2.1 trillion particles in a volume of $25.7~\mathrm{Gpc}^3$, that has sufficient mass resolution to resolve dwarf-size systems, combined with a semi-analytic galaxy and AGN formation model, to generate the Uchuu-$\nu^2$GC catalog, publicly available, that allows us to investigate the field-to-field variance of the luminosity function of AGN. With this Uchuu-$\nu^2$GC model, we quantify the cosmic variance as a function of survey area, AGN luminosity, and redshift. In general, cosmic variance decreases with increasing survey area and decreasing redshift. We find that at $z\sim6-7$, the cosmic variance depends weakly on AGN luminosity, in particular for small survey areas (0.01 and 0.1 deg$^2$). This is because the typical mass of dark matter haloes in which AGN reside does not significantly depend on luminosity. Due to the rarity of AGN, Poisson variance dominates the total field-to-field variance, especially for bright AGN. We discuss uncertainties present in the estimation of the faint-end of the AGN luminosity function from recent observations, and extend this to make predictions for the expected number of AGN and their variance for upcoming observations with Euclid, JWST, and the Legacy Survey of Space and Time (LSST). In particular, we predict that the Euclid deep survey will find 120--240 (16--80) AGN -- depending on the model -- with rest-frame UV absolute magnitude brighter than $-20$ ($-20.5$) at $z=6.3$ ($z=7$) in the Euclid H-band deep survey (abridged)., Comment: 17 pages, 17 figures, submitted to MNRAS, corrected the following link, All Uchuu-$\nu^2$GC data used for this paper is publicly available in our Skies & Universes website http://skiesanduniverses.org/Simulations/Uchuu/

We construct a model of H$��$ emitters (HAEs) based on a semi-analytic galaxy formation model, the New Numerical Galaxy Catalog ($��^2$GC). In this paper, we report our estimate for the field variance of the HAE distribution. By calculating the H$��$ luminosity from the star-formation rate of galaxies, our model well reproduces the observed H$��$ luminosity function (LF) at $z=0.4$. The large volume of the $��^2$GC makes it possible to examine the spatial distribution of HAEs over a region of (411.8 Mpc)$^3$ in the comoving scale. The surface number density of $z=0.4$ HAEs with $L_{\rm H��} \geq 10^{40}$ erg s$^{-1}$ is 308.9 deg$^{-2}$. We have confirmed that the HAE is a useful tracer for the large-scale structure of the Universe because of their significant overdensity ($>$ 5$��$) at clusters and the filamentary structures. The H$��$ LFs within a survey area of $\sim$2 deg$^2$ (typical for previous observational studies) show a significant field variance up to $\sim$1 dex. Based on our model, one can estimate the variance on the H$��$ LFs within given survey areas., 13 pages, 11 figures, accepted for publication in the ApJ

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, We propose a narrowband imaging survey of star-forming galaxies at re-ionisation era. The survey will exploit the widefield imaging capability of SPICA/MCS by using narrowband filter to detect H emission from the redshift 7 less than or equal to z less than or equal to 10. We estimated the feasibility of this survey, showing that the number of detectable sources highly depends on the IMF of the stellar population. Since the age constraints are fairly strong at such high redshifts, and extremely young star-forming galaxies are presumably less dusty, the survey should give the first direct and meaningful constraints on the IMF of population III (popIII) star formation., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027018, レポート番号: JAXA-SP-17-010E

SPICA Science Conference from Exoplanets to Distant Galaxies: SPICA's New Window on the Cool Universe (June 18-21, 2013. Ito Hall, the University of Tokyo), Bunkyou-ku, Tokyo, Japan, Understanding the galaxy dust emission is very important to obtain a full picture of galaxy formation, since it contains rich information about hidden star formation activity, physical properties of interstellar dust, and their role in galaxy formation. From the analysis of infrared spectral energy distribution (SED) of local galaxies which were observed by AKARI, we have found that a dust temperature averaged over the entire galaxy is strongly correlated with total infrared surface brightness, rather than total infrared luminosity. Combining this correlation with our cosmological galaxy formation model, we have computed dust SED of mock galaxies. By using this model, we present can theoretical predictions on the evolution of dusty universe., 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, 資料番号: AA1730027035, レポート番号: JAXA-SP-17-010E

We report the Subaru Hyper Suprime-Cam (HSC) discovery of two Ly$��$ blobs (LABs), dubbed z70-1 and z49-1 at $z=6.965$ and $z=4.888$ respectively, that are Ly$��$ emitters with a bright ($\log L_{\rm Ly��}/{\rm [erg\ s^{-1}]}>43.4$) and spatially-extended Ly$��$ emission, and present the photometric and spectroscopic properties of a total of seven LABs; the two new LABs and five previously-known LABs at $z=5.7-6.6$. The z70-1 LAB shows the extended Ly$��$ emission with a scale length of $1.4\pm 0.2$ kpc, about three times larger than the UV continuum emission, making z70-1 the most distant LAB identified to date. All of the 7 LABs, except z49-1, exhibit no AGN signatures such as X-ray emission, {\sc Nv}$��$1240 emission, or Ly$��$ line broadening, while z49-1 has a strong {\sc Civ}$��$1548 emission line indicating an AGN on the basis of the UV-line ratio diagnostics. We carefully model the point-spread functions of the HSC images, and conduct two-component exponential profile fitting to the extended Ly$��$ emission of the LABs. The Ly$��$ scale lengths of the core (star-forming region) and the halo components are $r_{\rm c}=0.6-1.2$ kpc and $r_{\rm h}=2.0-13.8$ kpc, respectively. The average $r_{\rm h}$ of the LABs falls on the extrapolation of the $r_{\rm h}$-Ly$��$ luminosity relation of the Ly$��$ halos around VLT/MUSE star-forming galaxies at the similar redshifts, suggesting that typical LABs at $z\gtrsim5$ are not special objects, but star-forming galaxies at the bright end., Submitted to ApJ

We present the latest results of a semi-analytic model of galaxy formation, "New Numerical Galaxy Catalogue", which is combined with large cosmological N-body simulations. This model can reproduce statistical properties of galaxies at z < 6.0. We focus on the properties of active galactic nuclei (AGNs) and supermassive black holes, especially on the accretion timescale onto black holes. We find that the number density of AGNs at z < 1.5 and at hard X-ray luminosity 10^{ 44 }< erg/s is underestimated compared with recent observational estimates when we assume the exponentially decreasing accretion rate and the accretion timescale which is proportional to the dynamical time of the host halo or the bulge, as is often assumed in semi-analytic models. We show that to solve this discrepancy, the accretion timescale of such less luminous AGNs instead should be a function of the black hole mass and the accreted gas mass. This timescale can be obtained from a phenomenological modelling of the gas angular momentum loss in the circumnuclear torus and/or the accretion disc. Such models predict a longer accretion timescale for less luminous AGNs at z < 1.0 than bright QSOs whose accretion timescale would be 10^{ 7-8 } yr. With this newly introduced accretion timescale, our model can explain the observed luminosity functions of AGNs at z < 6.0., 31 pages and 29 figures. Accepted for publication in MNRAS

We present Lyα and UV-nebular emission line properties of bright Lyα emitters (LAEs) at z = 6-7 with a luminosity of log LLyα/[erg s-1] = 43-44 identified in the 21 deg2 area of the SILVERRUSH early sample developed with the Subaru Hyper Suprime-Cam survey data. Our optical spectroscopy newly confirms 21 bright LAEs with clear Lyα emission, and contributes to making a spectroscopic sample of 96 LAEs at z = 6-7 in SILVERRUSH. From the spectroscopic sample, we select seven remarkable LAEs as bright as Himiko and CR7 objects, and perform deep Keck/MOSFIRE and Subaru/nuMOIRCS near-infrared spectroscopy reaching the 3 σ flux limit of ∼2 × 10-18 erg s-1 for the UV-nebular emission lines of He II λ1640, CIV λλ1548,1550, and OIII]λλ1661,1666. Except for one tentative detection of C IV, we find no strong UV-nebular lines down to the flux limit, placing the upper limits of the rest-frame equivalent widths (EW0) of ∼2-4 A for CIV, He II, and OIII] lines. We also investigate the VLT/X-SHOOTER spectrum of CR7 whose 6 σ detection of He II is claimed by Sobral et al. Although two individuals and the ESO archive service carefully reanalyzed the X-SHOOTER data that are used in the study of Sobral et al., no He II signal of CR7 is detected, supportive of weak UV-nebular lines of the bright LAEs even for CR7. The spectral properties of these bright LAEs are thus clearly different from those of faint dropouts at z ∼ 7 that have strong UV-nebular lines shown in the various studies. Comparing these bright LAEs and the faint dropouts, we find anti-correlations between the UV-nebular line EW0 and the UV-continuum luminosity, which are similar to those found at z ∼ 2-3.

We present the Ly$\alpha$ luminosity functions (LFs) at $z=$5.7 and 6.6 derived from a new large sample of 1,266 Ly$\alpha$ emitters (LAEs) identified in total areas of 14 and 21 deg$^2$, respectively, based on the early narrowband data of the Subaru/Hyper Suprime-Cam (HSC) survey. Together with careful Monte-Carlo simulations that account for the incompleteness of the LAE selection and the flux estimate systematics in the narrowband imaging, we have determined the Ly$\alpha$ LFs with the unprecedentedly small statistical and systematic uncertainties in a wide Ly$\alpha$ luminosity range of $10^{42.8-43.8}$ erg s$^{-1}$. We obtain the best-fit Schechter parameters of $L^{*}_{{\rm Lya}}=1.6^{+2.2}_{-0.6} (1.7^{+0.3}_{-0.7}) \times10^{43}$ erg s$^{-1}$, $\phi^{*}_{{\rm Lya}}=0.85^{+1.87}_{-0.77}\ (0.47^{+1.44}_{-0.44})\times10^{-4}$ Mpc$^{-3}$, and $\alpha=-2.6^{+0.6}_{-0.4}\ (-2.5^{+0.5}_{-0.5})$ at $z=5.7$ ($6.6$). We confirm that our best-estimate Ly$\alpha$ LFs are consistent with the majority of the previous studies, but find that our Ly$\alpha$ LFs do not agree with the high number densities of LAEs recently claimed by Matthee/Santos et al.'s studies that may overcorrect the incompleteness and the flux systematics. Our Ly$\alpha$ LFs at $z=5.7$ and $6.6$ show an indication that the faint-end slope is very steep ($\alpha \simeq -2.5$), although it is also possible that the bright-end LF results are enhanced by systematic effects such as the contribution from AGNs, blended merging galaxies, and/or large ionized bubbles around bright LAEs. Comparing our Ly$\alpha$ LF measurements with four independent reionization models, we estimate the neutral hydrogen fraction of the IGM to be $x_{\rm HI}=0.3\pm0.2$ at $z=$6.6 that is consistent with the small Thomson scattering optical depth obtained by Planck 2016., Comment: 21 pages, 14 figures, accepted for publication in PASJ special issue

In order to investigate the physical relationship between strong Ly-alpha absorbers (logN_HI>20.0 cm^-2) such as damped Ly-alpha absorption systems (DLAs) and young star-forming galaxies at high redshift, we have conducted narrow-band observations of Ly-alpha emitters (LAEs) in a concentrated region of strong Ly-alpha absorbers at z= 2.3, the J1230+34 field. Using a catalog of Ly-alpha absorbers with logN_HI>20.0 cm^-2 based on the baryon oscillation spectroscopic survey (BOSS), we found 6 fields where 3 or more absorbers are concentrated within a (50 Mpc)^3 cubic box in the comoving scale. Among them, we focus on the J1230+34 field, where 2 DLAs and 2 sub-DLAs present. Our narrow-band imaging observations with Subaru/Suprime-Cam using a custom-made filter, NB400 (lambda_c=4003 A and FWHM=92 A) yield a sample of 149 LAEs in this field. In the large scale (~50 Mpc), we have found no differences between the obtained Ly-alpha luminosity function and those in the blank fields at similar redshifts. We also compare the frequency distribution of the Ly-alpha rest-frame equivalent width (EW_0) in the target field and other fields including both overdensity region and blank field, but find no differences. On the other hand, in the small scale (~10 Mpc), we have found a possible overdensity of LAEs around a DLA with the highest HI column density (N_HI=21.08 cm^-2) in the target field while there are no density excess around the other absorbers with a lower N_HI., 15 pages, 15 figures, Accepted for publication to PASJ

We detect 20 $z=7.0$ Ly$\alpha$ emitter (LAE) candidates to $L({\rm Ly}\alpha) \geq 2 \times 10^{42}$ erg s$^{-1}$ or $0.3$ $L^*_{z=7}$ and in $6.1\times 10^5$ Mpc$^3$ volume in the Subaru Deep Field and the Subaru/XMM-Newton Deep Survey field by 82 and 37 hours of Subaru Suprime-Cam narrowband NB973 and reddest optical $y$-band imaging. We compare their Ly$\alpha$ and UV luminosity functions (LFs) and densities and Ly$\alpha$ equivalent widths (EWs) to those of $z=5.7$, 6.6 and 7.3 LAEs from previous Suprime-Cam surveys. The Ly$\alpha$ LF (density) rapidly declines by a factor of $\times$1.5 (1.9) in $L({\rm Ly}\alpha)$ at $z=5.7-6.6$ (160 Myr), $\times$1.5 (1.6) at $z=6.6-7.0$ (60 Myr) at the faint end and $\times$2.0 (3.8) at $z=7.0-7.3$ (40 Myr). Also, in addition to the systematic decrease in EW at $z=5.7-6.6$ previously found, 2/3 of the $z=7.0$ LAEs detected in the UV continuum exhibit lower EWs than the $z=6.6$ ones. Moreover, while the UV LF and density do not evolve at $z=5.7-6.6$, they modestly decline at $z=6.6-7.0$, implying galaxy evolution contributing to the decline of the Ly$\alpha$ LF. Comparison of the $z=7.0$ Ly$\alpha$ LF to the one predicted by an LAE evolution model further reveals that galaxy evolution alone cannot explain all the decline of Ly$\alpha$ LF. If we attribute the discrepancy to Ly$\alpha$ attenuation by neutral hydrogen, the intergalactic medium transmission of Ly$\alpha$ photons at $z=7.0$ would be $T_{{\rm Ly}\alpha}^{\rm IGM} \leq 0.6-0.7$. It is lower (higher) than $T_{{\rm Ly}\alpha}^{\rm IGM}$ at $z=6.6$ (7.3) derived by previous studies, suggesting rapid increase in neutral fraction at $z > 6$., Comment: 37 Pages, 22 Figures, 10 Tables, Accepted for publication in ApJ

We present the Ly$��$ luminosity functions (LFs) at $z=$5.7 and 6.6 derived from a new large sample of 1,266 Ly$��$ emitters (LAEs) identified in total areas of 14 and 21 deg$^2$, respectively, based on the early narrowband data of the Subaru/Hyper Suprime-Cam (HSC) survey. Together with careful Monte-Carlo simulations that account for the incompleteness of the LAE selection and the flux estimate systematics in the narrowband imaging, we have determined the Ly$��$ LFs with the unprecedentedly small statistical and systematic uncertainties in a wide Ly$��$ luminosity range of $10^{42.8-43.8}$ erg s$^{-1}$. We obtain the best-fit Schechter parameters of $L^{*}_{\rm Lya}=1.6^{+2.2}_{-0.6} (1.7^{+0.3}_{-0.7}) \times10^{43}$ erg s$^{-1}$, $��^{*}_{\rm Lya}=0.85^{+1.87}_{-0.77}\ (0.47^{+1.44}_{-0.44})\times10^{-4}$ Mpc$^{-3}$, and $��=-2.6^{+0.6}_{-0.4}\ (-2.5^{+0.5}_{-0.5})$ at $z=5.7$ ($6.6$). We confirm that our best-estimate Ly$��$ LFs are consistent with the majority of the previous studies, but find that our Ly$��$ LFs do not agree with the high number densities of LAEs recently claimed by Matthee/Santos et al.'s studies that may overcorrect the incompleteness and the flux systematics. Our Ly$��$ LFs at $z=5.7$ and $6.6$ show an indication that the faint-end slope is very steep ($��\simeq -2.5$), although it is also possible that the bright-end LF results are enhanced by systematic effects such as the contribution from AGNs, blended merging galaxies, and/or large ionized bubbles around bright LAEs. Comparing our Ly$��$ LF measurements with four independent reionization models, we estimate the neutral hydrogen fraction of the IGM to be $x_{\rm HI}=0.3\pm0.2$ at $z=$6.6 that is consistent with the small Thomson scattering optical depth obtained by Planck 2016., 21 pages, 14 figures, accepted for publication in PASJ special issue

We detect 20 $z=7.0$ Ly$��$ emitter (LAE) candidates to $L({\rm Ly}��) \geq 2 \times 10^{42}$ erg s$^{-1}$ or $0.3$ $L^*_{z=7}$ and in $6.1\times 10^5$ Mpc$^3$ volume in the Subaru Deep Field and the Subaru/XMM-Newton Deep Survey field by 82 and 37 hours of Subaru Suprime-Cam narrowband NB973 and reddest optical $y$-band imaging. We compare their Ly$��$ and UV luminosity functions (LFs) and densities and Ly$��$ equivalent widths (EWs) to those of $z=5.7$, 6.6 and 7.3 LAEs from previous Suprime-Cam surveys. The Ly$��$ LF (density) rapidly declines by a factor of $\times$1.5 (1.9) in $L({\rm Ly}��)$ at $z=5.7-6.6$ (160 Myr), $\times$1.5 (1.6) at $z=6.6-7.0$ (60 Myr) at the faint end and $\times$2.0 (3.8) at $z=7.0-7.3$ (40 Myr). Also, in addition to the systematic decrease in EW at $z=5.7-6.6$ previously found, 2/3 of the $z=7.0$ LAEs detected in the UV continuum exhibit lower EWs than the $z=6.6$ ones. Moreover, while the UV LF and density do not evolve at $z=5.7-6.6$, they modestly decline at $z=6.6-7.0$, implying galaxy evolution contributing to the decline of the Ly$��$ LF. Comparison of the $z=7.0$ Ly$��$ LF to the one predicted by an LAE evolution model further reveals that galaxy evolution alone cannot explain all the decline of Ly$��$ LF. If we attribute the discrepancy to Ly$��$ attenuation by neutral hydrogen, the intergalactic medium transmission of Ly$��$ photons at $z=7.0$ would be $T_{{\rm Ly}��}^{\rm IGM} \leq 0.6-0.7$. It is lower (higher) than $T_{{\rm Ly}��}^{\rm IGM}$ at $z=6.6$ (7.3) derived by previous studies, suggesting rapid increase in neutral fraction at $z > 6$., 37 Pages, 22 Figures, 10 Tables, Accepted for publication in ApJ

We study the extent to which very bright (-23.0 < MUV < -21.75) Lyman-break selected galaxies at redshifts z~7 display detectable Lya emission. To explore this issue, we have obtained follow-up optical spectroscopy of 9 z~7 galaxies from a parent sample of 24 z~7 galaxy candidates selected from the 1.65 sq.deg COSMOS-UltraVISTA and SXDS-UDS survey fields using the latest near-infrared public survey data, and new ultra-deep Subaru z'-band imaging (which we also present and describe in this paper). Our spectroscopy has yielded only one possible detection of Lya at z=7.168 with a rest-frame equivalent width EW_0 = 3.7 (+1.7/-1.1) Angstrom. The relative weakness of this line, combined with our failure to detect Lya emission from the other spectroscopic targets allows us to place a new upper limit on the prevalence of strong Lya emission at these redshifts. For conservative calculation and to facilitate comparison with previous studies at lower redshifts, we derive a 1-sigma upper limit on the fraction of UV bright galaxies at z~7 that display EW_0 > 50 Angstrom, which we estimate to be < 0.23. This result may indicate a weak trend where the fraction of strong Lya emitters ceases to rise, and possibly falls between z~6 and z~7. Our results also leave open the possibility that strong Lya may still be more prevalent in the brightest galaxies in the reionization era than their fainter counterparts. A larger spectroscopic sample of galaxies is required to derive a more reliable constraint on the neutral hydrogen fraction at z~7 based on the Lya fraction in the bright galaxies., 20 pages, 7 figures, accepted for publication in ApJ

Insulin is a major autoantigen responsible for the pathogenesis of type 1 diabetes, and its B-chain peptide B:9-23 has been suggested to contain critically important epitopes in the NOD mouse. We have previously demonstrated that the altered peptide ligand of B:9-23 peptide with alanine substitutions at positions 16 and 19 (A16,19 APL) suppresses insulitis and reduces the incidence of diabetes when administered intranasally together with cholera toxin (CT). In this study, we extended the previous findings to determine whether mucosal administration of the A16,19APL without the use of toxic CT is efficacious for diabetes prevention. To this end,we linked the A16,19APL to the C-terminus of non-toxic cholera toxin (CTB) B subunit and the chimeric fusion protein was produced in methyloprophic yeast Pichia pastoris. Although intranasal administration of the recombinant CTB-A16,19APL fusion protein extracted fromthe yeast cells failed to prevent the progression to diabetes, oral administration of the live yeast cells producing the chimeric protein resulted in more than 50% reduction of the development of diabetes, albeit the fact that protective efficacy did not reach the significance level by life table analysis (P= 0.08). Furthermore, the expression of insulin autoantibodies was not altered throughout the course of oral immunization experiment. These results demonstrated that the efficacy of recombinant CTB-A16,19APL for oral immunization has much room for improvement. Nevertheless, oral administration of recombinant yeast or other edible materials such as food plants engineered to produce altered autoantigenic peptide could potentially become a novel non-invasive immunotherapeutic strategy for type 1 diabetes. (250 word), Acta medica Nagasakiensia, 54(2), pp.33-38 ; 2009

平成19年度宇宙航行の力学シンポジウム（2007年12月17日-18日. 宇宙航空研究開発機構宇宙科学研究本部）, 相模原市, 神奈川県, Symposium on Flight Mechanics and Astrodynamics 2007 (December 17-18, 2007. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, 資料番号: SA6000011021

本研究では、相手の利己的提案やそれによって生じた自己の内的状態に注意を向けることが、交渉者の心的過程に及ぼす影響について検討した。具体的には、2者間交渉場面において、相手の利己的提案は交渉者に不快情動や利益獲得以外の社会的関心を生じさせ、さらに、そうした内的状態への注意喚起は不快情動やそれに伴う社会的関心を促すと予想した。実験室実験では、注意喚起要因を自己の内的状態に注意を向ける機会がある状況とそうでない状況によって操作し、提案内容要因を相手が利己的な提案をする条件と平等な提案をする条件によって操作した。実験の結果、相手の利己的提案は交渉者に怒りや同一性脅威を喚起し、報復行使や同一性回復に対する関心を促すことが確認された。さらに、こうした内的状態への注意喚起は交渉者の報復行使に対する関心を強めることが示された。, Present study examined negotiator’s mental processes induced by focusing toward negative emotion and concern of him/her that was evoked by egocentric offer of other party of negotiation. In distributive situation, we predicted that the others' egocentric offer induces negative emotion such as anger and threat of identity, and invites motivation of retaliation and retrieval of identity. In addition, we predicted focusing towards such internal process facilitates negative emotion and motivation by the others' egocentric offer. In the laboratory experiment, the factor of egocentricity of the other was manipulated whether egocentric or equivalent offers and the factor of self-focusing was manipulated whether participants had the opportunity to focus self-state or did not. The results indicated first that the egocentric offer evoked anger and threat of identity, motivation of retaliation and retrieval of identity, second that the focusing towards internal process intensified motivation of retaliation.

We present a new cosmological galaxy formation model, $\nu^2$GC, as an updated version of our previous model $\nu$GC. We adopt the so-called "semi-analytic" approach, in which the formation history of dark matter halos is computed by ${\it N}$-body simulations, while the baryon physics such as gas cooling, star formation and supernova feedback are simply modeled by phenomenological equations. Major updates of the model are as follows: (1) the merger trees of dark matter halos are constructed in state-of-the-art ${\it N}$-body simulations, (2) we introduce the formation and evolution process of supermassive black holes and the suppression of gas cooling due to active galactic nucleus (AGN) activity, (3) we include heating of the intergalactic gas by the cosmic UV background, and (4) we tune some free parameters related to the astrophysical processes using a Markov chain Monte Carlo method. Our ${\it N}$-body simulations of dark matter halos have unprecedented box size and mass resolution (the largest simulation contains 550 billion particles in a 1.12 Gpc/h box), enabling the study of much smaller and rarer objects. The model was tuned to fit the luminosity functions of local galaxies and mass function of neutral hydrogen. Local observations, such as the Tully-Fisher relation, size-magnitude relation of spiral galaxies and scaling relation between the bulge mass and black hole mass were well reproduced by the model. Moreover, the model also well reproduced the cosmic star formation history and the redshift evolution of rest-frame ${\it K}$-band luminosity functions. The numerical catalog of the simulated galaxies and AGNs is publicly available on the web., Comment: 25 pages, 21 figures, 2 tables, accepted to PASJ. The numerical catalog of galaxies and AGNs are available at http://cdsarc.u-strasbg.fr/cgi-bin/VizieR?-source=J/PASJ/68/25

International audience; We report a discovery of six massive galaxies with both extremely large Ly alpha equivalent widths (EWs) and evolved stellar populations at z similar to 3. These MAssive Extremely STrong Ly alpha emitting Objects (MAESTLOs) have been discovered in our large-volume systematic survey for strong Ly alpha emitters (LAEs) with 12 optical intermediate-band data taken with Subaru/Suprime-Cam in the COSMOS field. Based on the spectral energy distribution fitting analysis for these LAEs, it is found that these MAESTLOs have (1) large rest-frame EWs of EW0 (Ly alpha) similar to 100-300 angstrom, (2) M-star similar to 10(10.5) -10(11.1) M-circle dot, and (3) relatively low specific star formation rates of SFR/M-star similar to 0.03-1 Gyr(-1). Three of the six MAESTLOs have extended Ly alpha emission with a radius of several kiloparsecs, although they show very compact morphology in the HST/ACS images, which correspond to the rest-frame UV continuum. Since the MAESTLOs do not show any evidence for active galactic nuclei, the observed extended Ly alpha emission is likely to be caused by a star formation process including the superwind activity. We suggest that this new class of LAEs, MAESTLOs, provides a missing link from star-forming to passively evolving galaxies at the peak era of the cosmic star formation history.

平成26年度宇宙科学に関する室内実験シンポジウム (2015年2月23日-24日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 2015 Symposium on Laboratory Experiment for Space Science (July 23-24, 2015. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, 資料番号: SA6000076001

We present a new cosmological galaxy formation model, $��^2$GC, as an updated version of our previous model $��$GC. We adopt the so-called "semi-analytic" approach, in which the formation history of dark matter halos is computed by ${\it N}$-body simulations, while the baryon physics such as gas cooling, star formation and supernova feedback are simply modeled by phenomenological equations. Major updates of the model are as follows: (1) the merger trees of dark matter halos are constructed in state-of-the-art ${\it N}$-body simulations, (2) we introduce the formation and evolution process of supermassive black holes and the suppression of gas cooling due to active galactic nucleus (AGN) activity, (3) we include heating of the intergalactic gas by the cosmic UV background, and (4) we tune some free parameters related to the astrophysical processes using a Markov chain Monte Carlo method. Our ${\it N}$-body simulations of dark matter halos have unprecedented box size and mass resolution (the largest simulation contains 550 billion particles in a 1.12 Gpc/h box), enabling the study of much smaller and rarer objects. The model was tuned to fit the luminosity functions of local galaxies and mass function of neutral hydrogen. Local observations, such as the Tully-Fisher relation, size-magnitude relation of spiral galaxies and scaling relation between the bulge mass and black hole mass were well reproduced by the model. Moreover, the model also well reproduced the cosmic star formation history and the redshift evolution of rest-frame ${\it K}$-band luminosity functions. The numerical catalog of the simulated galaxies and AGNs is publicly available on the web., 25 pages, 21 figures, 2 tables, accepted to PASJ. The numerical catalog of galaxies and AGNs are available at http://cdsarc.u-strasbg.fr/cgi-bin/VizieR?-source=J/PASJ/68/25

We review cerebral hyperperfusion following carotid endarterectomy (CEA). Persistence of cerebral hyperperfusion greater than several days after CEA is associated with development of hyperperfusion syndrome. Postoperative cerebral hyperperfusion, even when asymptomatic, is associated with impairment of cognitive function in patients undergoing CEA. Further, development of hyperperfusion syndrome is associated with persistent postoperative cognitive impairment. Pretreatment with a novel free radical scavenger—edaravone—prevents occurrence of cerebral hyperperfusion itself after CEA. Intraoperative monitoring of transcranial regional cerebral oxygen saturation using near-infrared spectroscopy or monitoring of intraoperative middle cerebral artery blood flow velocity using transcranial Doppler ultrasonography identifies patients at risk for hyperperfusion after CEA. Reduced preoperative cerebrovascular reactivity to acetazolamide is a significant independent predictor of post-CEA hyperperfusion.

レーザーを用いた宇宙太陽発電システムの重要な要素として、半導体材料を利用した太陽光励起半導体レーザー(SEL)を提案している。SELは太陽光エネルギーを長距離伝送にふさわしいレーザー光に直接変換するものである。半導体は少量で太陽光を効率的に吸収できることがメリットであり、その光学的・電子的機能の高い制御性が魅力である。太陽光の高効率吸収と、吸収により発生したキャリアの効率的輸送のために、AlGaAs系化合物半導体を選択している。太陽光の吸収と発生キャリアの輸送に対して、傾斜ポテンシャル構造を提案し、その可能性について検討した。, Solar excited laser (SEL) using semiconductor material is proposed for wireless energy distribution system with laser light in space. The SEL converts solar light directly to laser light suitable for long-distant transmission. Semiconductor has high controllability of its optical and electrical functions which can be utilized for realization of the SEL. AlGaAs system is taken as an appropriate material for highly efficient conversion. Potential structure of the laser device is discussed from aspects of absorption of the solar light and transfer of the produced carrier into the active layer emitting laser light. Non-linear graded potential is mentioned as a possibility to enhance the performance., 資料番号: AA0045915016

平成25年度スペースプラズマ研究会 (2014年2月27日-28日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, Space Plasma Conference FY2013 (February 27-28, 2014. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000077035

平成25年度スペースプラズマ研究会 (2014年2月27日-28日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, Space Plasma Conference FY2013 (February 27-28, 2014. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000077002

We present the evolution of dark matter halos in six large cosmological N-body simulations, called the $��^2$GC (New Numerical Galaxy Catalog) simulations on the basis of the LCDM cosmology consistent with observational results obtained by the Planck satellite. The largest simulation consists of $8192^3$ (550 billion) dark matter particles in a box of $1.12 \, h^{-1} \rm Gpc$ (a mass resolution of $2.20 \times 10^{8} \, h^{-1} M_{\odot}$). Among simulations utilizing boxes larger than $1 \, h^{-1} \rm Gpc$, our simulation yields the highest resolution simulation that has ever been achieved. A $��^2$GC simulation with the smallest box consists of eight billions particles in a box of $70 \, h^{-1} \rm Mpc$ (a mass resolution of $3.44 \times 10^{6} \, h^{-1} M_{\odot}$). These simulations can follow the evolution of halos over masses of eight orders of magnitude, from small dwarf galaxies to massive clusters. Using the unprecedentedly high resolution and powerful statistics of the $��^2$GC simulations, we provide statistical results of the halo mass function, mass accretion rate, formation redshift, and merger statistics, and present accurate fitting functions for the Planck cosmology. By combining the $��^2$GC simulations with our new semi-analytic galaxy formation model, we are able to prepare mock catalogs of galaxies and active galactic nuclei, which will be made publicly available in the near future., 18 pages, 16 figures, accepted, simulation data can be downloaded on http://hpc.imit.chiba-u.jp/~nngc/

15th European Space Mechanisms & Tribology Symposium - ESMATS 2013（September 25-27, 2013.), Noordwijk, The Netherlands., This paper presents the design, analysis and test results of the low-shock payload separation mechanism for the H-IIA launch vehicle. The mechanism is based on a simple and reliable four-bar linkage, which makes the release speed of the marman clamp band tension lower than the current system.The adequacy of the principle for low-shock mechanism was evaluated by some simulations and results of fundamental tests. Then, we established the reliabilitydesign model of this mechanism, and the adequacy of this model was evaluated by elemental tests. Finally, we conducted the system separation tests usingthe payload adapter to which the mechanism was assembled, to confirm that the actual separation shock level satisfied our target., 資料番号: AC1400052000

第13回宇宙科学シンポジウム (2013年1月8日-9日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 13th Space Science Symposium (January 8-9, 2013. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 資料番号: SA6000063204, レポート番号: P2-177

平成24年度宇宙輸送シンポジウム (2013年1月17日-1月18日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)), 相模原市, 神奈川県, Space Transportation FY2012 (January 17-18, 2013. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, Translation title: Development of structure of Epsilon launch vehicle, 資料番号: AA0061856009, レポート番号: STCP-2012-009

第13回宇宙科学シンポジウム (2013年1月8日-9日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 13th Space Science Symposium (January 8-9, 2013. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 18名, 資料番号: SA6000063104, レポート番号: P2-077

Zincblende ZnMgCdS quaternary alloy layers were grown by molecular-beam epitaxy. The ZnMgCdS alloy lattice matched with GaAs and exhibited the band-gap energy of approximately 3 eV. Zn, Mg, and CdS were used as source materials. Cd was replaced by Zn or Mg, and the alloy composition was controlled when the growth temperature was set to approximately 210°C. Low-temperature photoluminescence showed dominant band-edge features indicating the high quality of the epilayer. The epilayer was applied to the metal-semiconductor-metal photodetector, and visible-blind UV sensing characteristics were observed.

第11回宇宙科学シンポジウム (2011年1月5日-7日. 宇宙航空研究開発機構宇宙科学研究所相模原キャンパス), 相模原市, 神奈川県, 11th Space Science Symposium (January 5-7, 2011. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency), Sagamihara, Kanagawa Japan, 超広視野初期宇宙探査衛星WISHは、口径1.5m、約1000平方分角の広視野カメラを持つ宇宙望遠鏡により、宇宙第一世代の銀河を検出し最初期の宇宙での天体形成を探ることを主目的とする計画である。本発表では、WISHで達成される検出限界を推定し、特に初期宇宙の銀河を検出するために必要な望遠鏡および近赤外線カメラのコンポーネントごとの温度要求と、最適なフィルタセットの検討結果を報告する。さらに、銀河進化モデルから予想される光度関数などとの比較を通じて、WISHによる広視野サーベイで期待される超遠方銀河の検出数について議論する。さらに、同一天域の多数回露出によって検出される超新星などのトランジェント天体や、ガンマ線バーストのフォローアップ観測を含め、WISHによって展開が期待される広範囲の研究について概観する。, 形態: カラー図版あり, 形態: CD-ROM1枚, Physical characteristics: Original contains color illustrations, Note: One CD-ROM, 資料番号: AA0065426150

We present theoretical predictions of UV continuum luminosity function (UV LF) and Lya equivalent width (EW) distribution of Lyman alpha emitters (LAEs) in the framework of the hierarchical clustering model of galaxy formation. The model parameters about LAEs were determined by fitting to the observed Lya LF at z=5.7 in our previous study, and the fit indicates that extinction of Lya photons by dust is significantly less effective than that of UV continuum photons, implying clumpy dust distribution in interstellar medium. We then compare the predictions about UV LFs and EW distributions with a variety of observations at z ~ 3-6, allowing no more free parameters and paying careful attention to the selection conditions of LAEs in each survey. We find that the predicted UV LFs and EW distributions are in nice agreement with observed data, and especially, our model naturally reproduces the existence of large EW LAEs (> 240 A) without introducing Pop III stars or top-heavy initial mass function. We show that both the stellar population (young age and low metallicity) and extinction by clumpy dust are the keys to reproduce large EW LAEs. The evidence of EW enhancement by clumpy dust is further strengthened by the quantitative agreement between our model and recent observations about a positive correlation between EW and extinction. The observed trend that brighter LAEs in UV continuum tend to have smaller mean EW is also reproduced, and the clumpy dust is playing an important role again for this trend. We suggested in our previous study that the transmission of intergalactic medium for Lya emission rapidly decreases from z ~ 6 to 7 by the fitting to Lya LFs, and this evidence is quantitatively strengthened by the comparison with the UV LF and EW distribution at z ~ 6.6., 21 pages, 13 figures, 1 table, accepted for publication in ApJ

The three-dimensional (3-D) strain map is useful to elucidate the relationships between microstructures and locally caused deformation and fracture. However, a robust tracking method, which enables error-free tracking in synchrotron radiation computed tomography (SR-CT) images with >10 000 microstructural features, is not currently available. In this study, a model sample was subjected to a tensile test and scanned by the SR-CT technique in order to develop a new tracking method. The developed tracking methods indicated a high tracking ratio and tracking success ratio of nearly 100% in a wide strain range, which included the assumed strain in a practical experiment. It was confirmed that tracking errors produce an incorrect strain distribution in 3-D strain mapping. This study verified the validity of the developed tracking method. The application of this method to high-resolution SR-CT images will make measurement and visualization of the strain distribution possible in three dimensions in bulk materials.

We made a narrowband NB973 (bandwidth of 200A at 9755A) imaging of the Subaru Deep Field (SDF) and found two z=7 Lyman alpha emitter (LAE) candidates down to NB973=24.9. Carrying out deep follow-up spectroscopy, we identified one of them as a real z=6.96 LAE. This has shown that galaxy formation was in progress just 750 Myr after the Big Bang. Meanwhile, the Lyman alpha line luminosity function of LAE is known to decline from z=5.7 to 6.6 in the SDF. L* at z=6.6 is 40-60% of that at z=5.7. We also confirm that the number density of z=7 LAE is only 17% of the density at z=6.6 comparing the latest SDF LAE samples. This series of significant decreases in LAE density with increasing redshift can be the result of galaxy evolution during these epochs. However, using the UV continuum luminosity functions of LAEs, those of Lyman break galaxies, and a LAE evolution model based on the hierarchical clustering, we find that galaxy evolution alone cannot explain all the decrease in density. This extra density deficit can be interpreted as the attenuation of the Lyman alpha photons from LAEs due to a rapid evolution of neutral hydrogen fraction during the ongoing cosmic reionization at z~6.6-7., published in Astrophysical Journal

第２回日本分子イメージング学会総会・学術集会

Objectives: F-18 labeled fluoroacetate (FA) has been developed as a PET tracer for imaging of oxidative metabolism in various tissues. For brain studies, however, the low blood-brain barrier (BBB) permeability of anionic form like FA is a fundamental problem. It is well known that ethyl acetate penetrates easily into the brain, then, is hydrolyzed to acetate rapidly in vivo. Based on these characteristics, we selected F-18 labeled ethyl fluoroacetate (EFA), ethyl-ester of FA, as a potential candidate for PET tracer of oxidative metabolism in brain. In this study, we investigated the possibility of [18F] EFA for brain PET imaging. Methods: BBB permeability was estimated by brain uptake index (BUI) method. Stability of [14C] EFA in plasma was assessed using five animal species. Then, the ester hydrolysis rate in rat brain was assayed both in vitro and in vivo. After these preliminary studies, we performed PET and metabolism studies of [18F] EFA using non-human primates. Results: The BUI of [14C] EFA was 125.9 +- 4.1% (n=4). This value was much higher than [14C] FA and also higher than that of [3H] H2O. The stability studies in plasma showed that [14C] EFA was extremely unstable in rodent, but stable in primate. Dog plasma brought an intermediate rate of degradation. The [14C] EFA was hydrolyzed rapidly in rat brain. These results suggest that EFA can be used as a pro-drug of [18F] FA for cerebral PET studies and the primate is suitable for in vivo experiments. In PET study using common marmosets, [18F] EFA showed higher brain uptake compared to [18F] FA at initial period, and the radioactivity was retained at 90 min after injection. The metabolism studies revealed that [18F] EFA was metabolized to only [18F] FA in arterial blood at 60 min after injection, but was converted to [18F] fluorocitrate in the brain, an intermediate metabolite from FA in the TCA cycle. Conclusions: we confirmed that [18F] EFA has ideal characteristics for brain imaging and it is a possible., Society of nuclear medicine 54rd Annual Meetng

We present a new theoretical model for the luminosity functions (LFs) of Lyman alpha (Lya) emitting galaxies in the framework of hierarchical galaxy formation. We extend a semi-analytic model of galaxy formation that reproduces a number of observations for local and high-z galaxies, without changing the original model parameters but introducing a physically-motivated modelling to describe the escape fraction of Lya photons from host galaxies (f_esc). Though a previous study using a hierarchical clustering model simply assumed a constant and universal value of f_esc, we incorporate two new effects on f_esc: extinction by interstellar dust and galaxy-scale outflow induced as a star formation feedback. It is found that the new model nicely reproduces all the observed Lya LFs of the Lya emitters (LAEs) at different redshifts in z ~ 3-6. Especially, the rather surprisingly small evolution of the observed LAE Lya LFs compared with the dark halo mass function is naturally reproduced. Our model predicts that galaxies with strong outflows and f_esc ~ 1 are dominant in the observed LFs. This is also consistent with available observations, while the simple universal f_esc model requires f_esc << 1 not to overproduce the brightest LAEs. On the other hand, we found that our model significantly overpredicts LAEs at z > 6, and absorption of Lya photons by neutral hydrogen in intergalactic medium (IGM) is a reasonable interpretation for the discrepancy. This indicates that the IGM neutral fraction x_HI rapidly evolves from x_HI << 1 at z < 6 to a value of order unity at z ~ 6-7, which is broadly consistent with other observational constraints on the reionization history., 14 pages, 7 figures, 1 table; accepted to ApJ; the html abstract is replaced to match the accepted version, the .ps and .pdf files are strictly identical between the 2nd and the 3rd versions

The work described in this thesis deals with characterization of DNA binding by the BRCT domain of the large subunit of RFC. Replication Factor C (RFC) is a five protein complex involved in initiating and regulating new DNA synthesis. The first half of the thesis describes region of the RFC and structural determinants of DNA required for productive protein-DNA interaction. The second half describes three-dimensional structure determination of the protein-DNA complex, which consists of the BRCT region of the RFC and doubled stranded DNA. The resulting structure based on the data from NMR and mutagenesis reveals structural conservations of few amino acids among the members of BRCT domain superfamily, which are known to bind either phosphorylated peptide or DNA. The work may help us to identify other potential DNA binding BRCT domains.

The first galaxies in the Universe are built up where cold dark matter (CDM) forms large scale filamentary structure. Although the galaxies are expected to emit numerous Lya photons, they are surrounded by plentiful neutral hydrogen with a typical optical depth for Lya of ~10^5 (HI halos) before the era of cosmological reionization. The HI halo almost follows the cosmological Hubble expansion with some anisotropic corrections around the galaxy because of the gravitational attraction by the underlying CDM filament. In this paper, we investigate the detectability of the Lya emissions from the first galaxies, examining their dependence on viewing angles. Solving the Lya line transfer problem in an anisotropically expanding HI halo, we show that the escape probability from the HI halo is the largest in direction along the filament axis. If the Lya source is observed with a narrow-band filter, the difference of apparent Lya line luminosities among viewing angles can be a factor of > 40 at an extreme case. Furthermore, we evaluate the predicted physical features of the Lya sources and flux magnification by gravitational lensing effect due to clusters of galaxies along the filament. We conclude that, by using the next generation space telescopes like the JWST, the Lya emissions from the first galaxies whose CDM filament axes almost face to us can be detected with the S/N of > 10., 21 pages, 4 figures, 1 table. Accepted for publication in Astrophysical Journal

BACKGROUND AND PURPOSE: Qualitative measurement of regional cerebrovascular reactivity (rCVR) to acetazolamide with single-photon emission CT (SPECT) has been widely used to determine the severity of hemodynamic impairment. We attempted to validate the accuracy of qualitative assessment by using SPECT to detect reduced rCVR compared with rCVR determined quantitatively in patients with unilateral major cerebral artery occlusion. METHODS: Regional cerebral blood flow was assessed with iodine-123-N-isopropyl-p-iodoamphetamine ((123)I-IMP) at rest and after acetazolamide activation in 133 patients with previously symptomatic, unilateral internal carotid or middle cerebral artery occlusion. Quantitative values were calculated by using the (123)I-IMP autoradiographic method and analyzed for each cerebral hemisphere as the percentage change in rCBF between resting and activation studies (%(Hem)). Qualitative rCVR was determined for the target hemisphere distal to the occlusion as the cerebral-interhemispheric asymmetry index (AI(Hem)) and as an index of flow difference between the target cerebral and ipsilateral cerebellar hemispheres (FI(Hem−Cbl)). Values 2 SDs below the mean in healthy volunteers were defined as decreased. RESULTS: Fair agreement was observed between %(Hem) and both AI(Hem) change (resting vs activation, κ = 0.409) and FI(Hem-Cbl) change (resting vs activation, κ = 0.440). When %(Hem) was assumed to represent the true determinant of assessing rCVR, AI(Hem) change and FI(Hem−Cbl) change demonstrated sensitivities of 68% and 78%; specificities, 72% and 76%; positive predictive values, 48% and 56%; false-positive incidences, 28% and 24%; and false-negative incidences, 32% and 22% for detecting patients with reduced rCVR, respectively. CONCLUSION: Subgroups of patients with hemodynamic impairment cannot be accurately defined by using rCVR qualitatively measured with SPECT.

A GaN based ultraviolet (UV) laser diode (LD) was used to study the autofluorescence (AF) spectrum of the normal and tumor human bronchial tissues under ex vivo conditions. The UV LD generates a coherent short wavelength (around 400 nm) light beam with an intensity of about a few watts. AF spectrum data can be obtained without interference by excitation light. A clear blue peak located at around 483 nm was observed along with a green peak at around 560 nm in the normal tissue. The peak intensities observed were very weak for the tumor tissues. The AF imaging and spectrum analysis were performed along with a histopathological study. The spatial distribution of the elastin in the bronchial tissue affected the intensity of the AF whereas the spectrum shape was not affected. Strong AF was observed from regions that include a high density of the elastin. Biopsy measurements were performed for ex vivo samples, and depth profiling of the elastin was studied along with variations of the AF spectrum. AF spectra excited by the UV LD for fluorescence materials including FAD, NADH, and elastin were measured. The spectrum shape of the elastin as well as of NADH was similar to that of normal bronchial tissues.

資料番号: ARDS03125000, レポート番号: 29aVII2