Search

Powerful relativistic jets in active galactic nuclei (AGN) are believed to be originated from the accretion of material onto the supermassive black hole (SMBH)1. The nearby radio galaxy M87 is one of the best examples of this phenomenon, and the recent detection of a black-hole shadow with the Event Horizon Telescope provided compelling evidence for this paradigm2. However, whether the central SMBH in M87 has a spin or not, a fundamental parameter of a BH along with the mass, remains unconstrained by observations since the appearance of the photon ring is rather insensitive to the spin2-4. A clue to this challenge is to trace the long-term evolution of the innermost jet base where the central BH and accretion disk tightly regulate its flow dynamics. Here we report an extensive analysis of the morphological evolution of the M87 jet nozzle based on 170 high-resolution radio images spanning more than two decades. The ensemble of the data reveals a periodic (a period of 11 years) variation of the jet direction with a peak-to-peak amplitude of ~10 deg on the sky. A successful fit of a precession model to the data as well as general-relativistic magnetohydrodynamic simulations strongly supports the presence of a spinning BH in M87, inducing a Lense-Thirring precession of a misaligned accretion disk by the frame-dragging effect5. Our results suggest that jet precession with a spinning BH can commonly exist in other more distant AGN but had evaded detection due to the small magnitude and long period of position angle variation.

Because of its proximity and the large size of its black hole, M87 is one of the best targets for studying the launching mechanism of active galactic nucleus jets. Currently, magnetic fields are considered to be an essential factor in the launching and accelerating of the jet. However, current observational estimates of the magnetic field strength of the M87 jet are limited to the innermost part of the jet or to HST-1. No attempt has yet been made to measure the magnetic field strength in between. We aim to infer the magnetic field strength of the M87 jet out to a distance of several thousand $r_s$ by tracking the distance-dependent changes in the synchrotron spectrum of the jet from high-resolution very long baseline interferometry observations. In order to obtain high-quality spectral index maps, quasi-simultaneous observations at 22 and 43 GHz were conducted using the KVN and VERA Array (KaVA) and the VLBA. We compared the spectral index distributions obtained from the observations with a model and placed limits on the magnetic field strengths as a function of distance. The overall spectral morphology is broadly consistent over the course of these observations. The observed synchrotron spectrum rapidly steepens from $\alpha_{22-43 GHz}$ ~ -0.7 at ~ 2 mas to $\alpha_{22-43 GHz}$ ~ -2.5 at ~ 6 mas. A spectral index model in which nonthermal electron injections inside the jet decrease with distance can adequately reproduce the observed trend. This suggests the magnetic field strength of the jet at a distance of 2 - 10 mas (~ 900 $r_s$ - ~ 4500 $r_s$ in the deprojected distance) has a range of $B=(0.3 - 1.0 G)(z/2 mas)^{-0.73}$. Extrapolating to the EHT scale yields consistent results, suggesting that the majority of the magnetic flux of the jet near the black hole is preserved out to ~ 4500 $r_s$ without significant dissipation., Comment: 16 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics

We present the results of our multifrequency observations for 10 ultraluminous infrared galaxies (ULIRGs) made by the Karl G. Jansky Very Large Array at 1.4, 5.5, 9.0, and 14.0 GHz. Our sample is selected from ULIRGs whose active galactic nuclei (AGNs) are not found at optical wavelengths (∼70 per cent of the total ULIRGs), but whose presence is suggested by mid-infrared or submillimetre observations (>50 per cent of the non-AGN ULIRGs at optical wavelengths). The statistical properties of the targets are similar to those of the entire ULIRG sample, which implies that ULIRGs have common radiative processes regardless of the presence of optical AGNs, and thus AGNs might equally contribute to the radio emission of every ULIRG. Although their spectra are mainly explained by starbursts and/or merger activity, some individual sources suggest contributions from AGNs. IRAS 00188−0856, whose optical morphology is not disturbed, shows a large non-thermal fraction and a spectral break at high frequency, which can be explained by synchrotron ageing of non-thermal plasma emitted from AGNs. In addition, we find 100-kpc-scale extended emission associated with IRAS 01004−2237. The two-sided morphology and absence of extended X-ray emission suggest that this system is not induced by a merger in a cluster but originates from AGN activity.

We present the results of second epoch ALMA observations of 321 GHz H$_2$O emission toward two nearby active galactic nuclei, NGC 4945 and the Circinus galaxy, together with Tidbinbilla 70-m monitoring of their 22 GHz H$_2$O masers. The two epoch ALMA observations show that the strengths of the 321 GHz emission are variable by a factor of at least a few, confirming a maser origin. In the second epoch, 321 GHz maser emission from NGC 4945 was not detected, while for the Circinus galaxy the flux density significantly increased and the velocity gradient and dispersion have been measured. With the velocity gradient spanning $\sim$110 km/s, we calculate the disk radius to be $\sim$28 pc, assuming disk rotation around the nucleus. We also estimate the dynamical mass within the central 28 pc to be 4.3 $\times$ 10$^8$ M$_{\odot}$, which is significantly larger than the larger scale dynamical mass, suggesting the velocity gradient does not trace circular motions on that scale. The overall direction of the velocity gradient and velocity range of the blueshifted features are largely consistent with those of the 22 GHz maser emission in a thin disk with smaller radii of 0.1--0.4 pc and molecular outflows within $\sim$1 pc from the central engine of the galaxy, implying that the 321 GHz masers could trace part of the circumnuclear disk or the nuclear outflows., 13 pages, 9 figures, accepted for publication in ApJ

Full list of authors: Cui, Yu-Zhu; Hada, Kazuhiro; Kino, Motoki; Sohn, Bong-Won; Park, Jongho; Ro, Hyun-Wook; Sawada-Satoh, Satoko; Jiang, Wu; Cui, Lang; Honma, Mareki; Shen, Zhi-Qiang; Tazaki, Fumie; An, Tao; Cho, Ilje; Zhao, Guang-Yao; Cheng, Xiao-Peng; Niinuma, Kotaro; Wajima, Kiyoaki; Zhang, Ying-Kang; Kawaguchi, Noriyuki; Algaba, Juan-Carlos; Koyama, Shoko; Hirota, Tomoya; Yonekura, Yoshinori; Sakai, Nobuyuki; Xia, Bo; Jiang, Yong-Bin; Yu, Lin-Feng; Gou, Wei; Hwang, Ju-Yeon; Jiang, Yong-Chen; Sun, Yun-Xia; Jung, Dong-Kyu; Kim, Hyo-Ryoung; Kim, Jeong-Sook; Kobayashi, Hideyuki; Lee, Jee-Won; Lee, Jeong-Ae; Zhang, Hua; Li, Guang-Hui; Xu, Zhi-Qiang; Li, Peng; Oh, Jung-Hwan; Oh, Se-Jin; Oh, Chung-Sik; Oyama, Tomoaki; Roh, Duk-Gyoo; Shibata, Katsunori-M.; Guo, Wen; Zhao, Rong-Bing; Zhong, Wei-Ye; Wang, Jin-Qing; Yang, Wen-Jun; Yan, Hao; Yeom, Jae-Hwan; Li, Bin; Li, Xiao-Fei; Yuan, Jian-Ping; Dong, Jian; Chen, Zhong; Akiyama, Kazunori; Asada, Keiichi; Byun, Do-Young; Hagiwara, Yoshiaki; Hodgson, Jeffrey; Jung, Tae-Hyun; Kim, Kee-Tae; Lee, Sang-Sung; Yi, Kunwoo; Liu, Qing-Hui; Liu, Xiang; Lu, Ru-Sen; Nakamura, Masanori; Trippe, Sascha; Wang, Na; Wang, Xue-Zheng; Zhang, Bo, The East Asian Very Long Baseline Interferometry (VLBI) Network (EAVN) is a rapidly evolving international VLBI array that is currently promoted under joint efforts among China, Japan and Korea. EAVN aims at forming a joint VLBI Network by combining a large number of radio telescopes distributed over East Asian regions. After the combination of the Korean VLBI Network (KVN) and the VLBI Exploration of Radio Astrometry (VERA) into KaVA, further expansion with the joint array in East Asia is actively promoted. Here we report the first imaging results (at 22 and 43 GHz) of bright radio sources obtained with KaVA connected to Tianma 65-m and Nanshan 26-m Radio Telescopes in China. To test the EAVN imaging performance for different sources, we observed four active galactic nuclei (AGN) having different brightness and morphology. As a result, we confirmed that the Tianma 65-m Radio Telescope (TMRT) significantly enhances the overall array sensitivity, a factor of 4 improvement in baseline sensitivity and 2 in image dynamic range compared to the case of KaVA only. The addition of the Nanshan 26-m Radio Telescope (NSRT) further doubled the east-west angular resolution. With the resulting high-dynamic-range, high-resolution images with EAVN (KaVA+TMRT+NSRT), various fine-scale structures in our targets, such as the counter-jet in M87, a kink-like morphology of the 3C 273 jet and the weak emission in other sources are successfully detected. This demonstrates the powerful capability of EAVN to study AGN jets and to achieve other science goals in general. Ongoing expansion of EAVN will further enhance the angular resolution, detection sensitivity and frequency coverage of the network. © 2021 National Astronomical Observatories, CAS and IOP Publishing Ltd., TMRT is operated by Shanghai Astronomical Observatory. NSRT is operated by Xinjiang Astronomical Observatory. KVN is a facility operated at by the Korea Astronomy and Space Science Institute. VERA is a facility operated at National Astronomical Observatory of Japan in collaboration with associated universities in Japan. This work is supported by The Graduate University for Advanced Studies (SOKENDAI). Y.C. is supported by the Japanese Government (MEXT) Scholarship. This work is supported by JSPS KAKENHI Grant Numbers JP18K03656 (M.K.), JP18H03721 (K.N., K.H. and M.K.), JP19H01943 (K.H., F.T. and Y.H.) and JP18KK0090 (K.H. and F.T.). K.H. is supported by the Mitsubishi Foundation (grant number 201911019). J.P. is supported by an EACOA Fellowship awarded by the East Asia Core Observatories Association, which consists of the Academia Sinica Institute of Astronomy and Astrophysics, the National Astronomical Observatory of Japan, the Center for Astronomical Mega-Science, the Chinese Academy of Sciences, and the Korea Astronomy and Space Science Institute. J.P. and I.C. acknowledge the financial support from the National Research Foundation (NRF) of Korea via Global Ph.D. Fellowship Grant 2014H1A2A1018695 and 2015H1A2A1033752, respectively. S.T. acknowledges support from the NRF via Grant 2019R1F1A1059721. This work is supported by the Major Program of the National Natural Science Foundation of China (NSFC, Grant Nos. 11590780 and 11590784), the Knowledge Innovation Program of the Chinese Academy of Sciences (Grant No. KJCX1-YW-18), the Scientific Program of Shanghai Municipality (08DZ1160100) and Key Laboratory for Radio Astronomy, CAS. W.J. acknowledges support from NSFC (Grant No. 11803071). L.C. is supported by the National Key R&D Program of China (Grant No. 2018YFA0404602), the CAS 'Light of West China' Program (Grant No. 2018-XBQNXZ-B-021), the NSFC (Grant Nos. U2031212 and 61931002) and the Youth Innovation Promotion Association of the CAS (Grant No. 2017084). J.C.A. acknowledges support from Fundamental Research Grant Scheme (FRGS) FRGS/1/2019/STG02/UM/02/6. R.S. Lu is supported by the Max Planck Partner Group of the MPG and the CAS and acknowledges the support by the Key Program of the NSFC (Grant No. 11933007) and the Research Program of Fundamental and Frontier Sciences, CAS (Grant No. ZDBS-LY-SLH011)., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Many approaches have been taken to identify new biomarkers of pancreatic ductal carcinoma (PDC). Since animal models can be sampled under controlled conditions, better standardization is possible compared with heterogeneous human studies. Transgenic rats with conditional activation of oncogenic RAS in pancreatic tissue develop PDC that closely resembles the biological and histopathological features of human PDC. Using this model, we evaluated the usefulness of leucine-rich α2-glycoprotein-1 (LRG-1) as a serum marker. In this study, we found that LRG-1 was overexpressed in rat PDC compared with normal pancreas tissue of the control rats. Serum levels of LRG-1 were also significantly higher in rats bearing PDC than in controls. Importantly, chronic pancreatitis in male Wistar Bonn/Kobori rats, which is a widely accepted as a model of chronic pancreatitis, did not cause serum levels of LRG-1 to become elevated. These results strongly support serum LRG-1 as a candidate biomarker for noninvasive diagnosis of PDC. Our models of pancreas cancer provide a useful strategy for evaluation of candidate markers applicable to human cancer.

We present the results of ALMA band-5 (~170 GHz) observations of the merging ultraluminous infrared galaxy, the "Superantennae" (IRAS 19254-7245) at z=0.0617, which has been diagnosed as containing a luminous obscured active galactic nucleus (AGN). In addition to dense molecular line emission (HCN, HCO+, and HNC J = 2-1), we detect a highly luminous (~6e4Lsun) 183 GHz H2O 3(1,3)-2(2,0) emission line. We interpret the strong H2O emission as largely originating in maser amplification in AGN-illuminated dense and warm molecular gas, based on (1) the spatially compact (500 pc) dense molecular emission, and (2) a strikingly different velocity profile from, and (3) significantly elevated flux ratio relative to, dense molecular emission lines. H2O maser emission, other than the widely studied 22 GHz 6(1,6)-5(2,3) line, has been expected to provide important information on the physical properties of gas in the vicinity of a central mass-accreting supermassive black hole (SMBH), because of different excitation energy. We here demonstrate that with highly sensitive ALMA, millimetre 183 GHz H2O maser detection is feasible out to >270 Mpc, opening a new window to scrutinize molecular gas properties around a mass-accreting SMBH far beyond the immediately local universe., 6 pages, 2 figures. MNRAS Letters accepted

Full list of authors: Cho, Ilje; Zhao, Guang-Yao; Kawashima, Tomohisa; Kino, Motoki; Akiyama, Kazunori; Johnson, Michael D.; Issaoun, Sara; Moriyama, Kotaro; Cheng, Xiaopeng; Algaba, Juan-Carlos; Jung, Taehyun; Sohn, Bong Won; Krichbaum, Thomas P.; Wielgus, Maciek; Hada, Kazuhiro; Lu, Ru-Sen; Cui, Yuzhu; Sawada-Satoh, Satoko; Shen, Zhiqiang; Park, Jongho; Jiang, Wu; Ro, Hyunwook; Yi, Kunwoo; Wajima, Kiyoaki; Lee, Jee Won; Hodgson, Jeffrey; Tazaki, Fumie; Honma, Mareki; Niinuma, Kotaro; Trippe, Sascha; An, Tao; Zhang, Yingkang; Lee, Jeong Ae; Oh, Se-Jin; Byun, Do-Young; Lee, Sang-Sung; Kim, Jae-Young; Oh, Junghwan; Koyama, Shoko; Asada, Keiichi; Wang, Xuezheng; Cui, Lang; Hagiwara, Yoshiaki; Nakamura, Masanori; Takamura, Mieko; Hirota, Tomoya; Sugiyama, Koichiro; Kawaguchi, Noriyuki; Kobayashi, Hideyuki; Oyama, Tomoaki; Yonekura, Yoshinori; Kim, Jongsoo; Hwang, Ju-Yeon; Jung, Dong-Kyu; Kim, Hyo-Ryoung; Kim, Jeong-Sook; Oh, Chung-Sik; Roh, Duk-Gyoo; Yeom, Jae-Hwan; Xia, Bo; Zhong, Weiye; Li, Bin; Zhao, Rongbing; Wang, Jinqing; Liu, Qinghui; Chen, Zhong.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited., Sagittarius A* (Sgr A*), the Galactic Center supermassive black hole (SMBH), is one of the best targets in which to resolve the innermost region of an SMBH with very long baseline interferometry (VLBI). In this study, we have carried out observations toward Sgr A* at 1.349 cm (22.223 GHz) and 6.950 mm (43.135 GHz) with the East Asian VLBI Network, as a part of the multiwavelength campaign of the Event Horizon Telescope (EHT) in 2017 April. To mitigate scattering effects, the physically motivated scattering kernel model from Psaltis et al. (2018) and the scattering parameters from Johnson et al. (2018) have been applied. As a result, a single, symmetric Gaussian model well describes the intrinsic structure of Sgr A* at both wavelengths. From closure amplitudes, the major-axis sizes are ∼704 ± 102 μas (axial ratio ∼${1.19}_{-0.19}^{+0.24}$) and ∼300 ± 25 μas (axial ratio ∼1.28 ± 0.2) at 1.349 cm and 6.95 mm, respectively. Together with a quasi-simultaneous observation at 3.5 mm (86 GHz) by Issaoun et al. (2019), we show that the intrinsic size scales with observing wavelength as a power law, with an index ∼1.2 ± 0.2. Our results also provide estimates of the size and compact flux density at 1.3 mm, which can be incorporated into the analysis of the EHT observations. In terms of the origin of radio emission, we have compared the intrinsic structures with the accretion flow scenario, especially the radiatively inefficient accretion flow based on the Keplerian shell model. With this, we show that a nonthermal electron population is necessary to reproduce the source sizes. © 2022. The Author(s). Published by the American Astronomical Society., I.C. and J.P. are supported by the National Research Foundation of Korea (NRF) via a Global PhD Fellowship grant (NRF-2015H1A2A1033752 and NRF-2014H1A2A1018695, respectively). I.C. acknowledges financial support by the Spanish Ministerio de Economía y Competitividad (grants PID2019-108995GB-C21) and the Junta de Andalucía (grant P18-FR-1769). G.-Y.Z. and T.J. are supported by the Korea Research Fellowship Program through the NRF (NRF-2015H1D3A1066561). I.C. and G.-Y.Z. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the "Center of Excellence Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). K.A. is supported by the National Science Foundation (NSF) through grants AST-1440254, AST-1614868, and AST-2034306. This work is partially supported by JSPS KAKENHI grant Nos. JP18K03656 (M.K.), JP18H03721 (K.N., M.K., K.H.), JP18K13594 (T.K.), JP18KK0090 (K.H.), JP19H01943 (K.H.), JP21H01137 (K.H., M.K.), and the Mitsubishi Foundation grant No. 201911019 (K.H.). J.-C.A. acknowledges support from the Malaysian Fundamental Research grant Scheme (FRGS) FRGS/1/2019/STG02 /UM/02/6. M.D.J. acknowledges support from the National Science Foundation (AST-1716536, AST-1935980) and the Gordon and Betty Moore Foundation (GBMF-5278). X.-P.C. and B.-W.S. are supported by Brain Pool Program through the National Research Foundation of Korea (NRF) funded by the Ministry of Science and ICT (2019H1D3A1A01102564). R.-S.L. is supported by the Max Planck Partner Group of the MPG and the CAS and acknowledges the support by the Key Program of the National Natural Science Foundation of China (grant No. 11933007) and Research Program of Fundamental and Frontier Sciences, CAS (grant No. ZDBS-LY-SLH011). J.P. acknowledges financial support through the EACOA Fellowship awarded by the East Asia Core Observatories Association, which consists of the Academia Sinica Institute of Astronomy and Astrophysics, the National Astronomical Observatory of Japan, Center for Astronomical Mega-Science, Chinese Academy of Sciences, and the Korea Astronomy and Space Science Institute. S.T. acknowledges financial support from the NRF via Basic Research grant 2019R1F1A1059721. This work was also supported in part by MEXT SPIRE, MEXT as "Priority Issue on post-K computer" (Elucidation of the Fundamental Laws and Evolution of the Universe) and as "Program for Promoting Researches on the Supercomputer Fugaku" (High-energy astrophysical phenomena in black holes and supernovae). J.S.K. (grant Nos. 2016R1A5A1013277 and 2020R1A2C1007219) and J.O. (grant No. 2021R1A6A3A01086420) has been supported by the Basic Science Research Program through the NRF funded by the Ministry of Education.

Process parameter tolerance of semiconductor device is very important for manufacturability and yield. Pinned Photodiode has by definition the pinned surface potential of the low surface dark current feature and the pinned empty potential well of the no image lag feature with the excellent blue light sensitivity of the ideal quantum efficiency. This paper reports simulation and device characterization of the unique P+PN+P junction type Buried, Depletion and Pinned Photodiode with excellent manufacturability, originally invented in 1975. Related various historical photodiode structures are reviewed, including the metal semiconductor Schottky Barrier photo sensor of Au/ $\beta$ - Ga 2 O 3 type in search for the low leakage and dark current photodiode which led the 1975 invention of the low leakage P+NPNsub junction Pinned Photodiode by Hagiwara.

We present ALMA ~0.02"-resolution observations of the nucleus of the nearby (~14 Mpc) type-2 AGN NGC 1068 at HCN/HCO+/HNC J=3-2 lines, as well as at their 13C isotopologue and vibrationally excited lines, to scrutinize the morphological/dynamical/chemical/physical properties of dense molecular gas in the putative dusty molecular torus around a mass-accreting supermassive black hole. We confirm almost east-west-oriented dense molecular gas emission both morphologically and dynamically, which we regard as coming from the torus. Bright emission is compact (2 pc) part, in both the eastern and western torus. We prefer a scenario of counter-rotating dense molecular gas with innermost almost-Keplerian-rotation and outer slowly rotating (far below Keplerian) components. Our high-spatial-resolution dense molecular line data reveal that torus properties of NGC 1068 are much more complicated than the simple axi-symmetrically rotating torus picture in the classical AGN unification paradigm., 45 pages, 20 Figures. Accepted for publication in ApJ

We present the first astrometry catalog from the Japanese VLBI (very long baseline interferometer) project VERA (VLBI Exploration of Radio Astrometry). We have compiled all the astrometry results from VERA, providing accurate trigonometric annual parallax and proper motion measurements. In total, 99 maser sources are listed in the VERA catalog. Among them, 21 maser sources are newly reported while the rest of 78 sources are referred to previously published results or those in preparation for forthcoming papers. The accuracy in the VERA astrometry are revisited and compared with those from the other VLBI astrometry projects such as BeSSeL (The Bar and Spiral Structure Legacy) Survey and GOBELINS (the Gould's Belt Distances Survey) with the VLBA (Very Long Baseline Array). We have confirmed that most of the astrometry results are consistent with each other, and the largest error sources are due to source structure of the maser features and their rapid variation, along with the systematic calibration errors and different analysis methods. Combined with the BeSSeL results, we estimate the up-to-date fundamental Galactic parameter of $R_{0}=7.92\pm0.16_{\rm{stat.}}\pm0.3_{\rm{sys.}}$~kpc and $\Omega_{\odot}=30.17\pm0.27_{\rm{stat.}}\pm0.3_{\rm{sys.}}$~km~s$^{-1}$~kpc$^{-1}$, where $R_{0}$ and $\Omega_{\odot}$ are the distance from the Sun to the Galactic center and the Sun's angular velocity of the Galactic circular rotation, respectively., Comment: 35 pages, 7 figures, accepted for publication in the Publications of the Astronomical Society of Japan

Human natural killer-1 (HNK-1) epitope, a highly-expressed glycan in the nervous system, is critical for normal synaptic plasticity and spatial learning. HNK-1 epitope modifies N-glycans on several neural glycoproteins, and also modifies O-mannosyl glycans. A branching enzyme for O-mannosyl glycans (GnT-IX, Core M2 synthase) exhibits brain-specific expression, and the product core M2 glycans are also limited to the brain. In a previous study, we showed that cuprizone-induced demyelination increased HNK-1-capped core M2 glycan expression, while GnT-IX deficiency ameliorated demyelination, suggesting that these glycans could be useful diagnostic markers for demyelination status and act as therapeutic targets. Nevertheless, a lack of appropriate detection tools hampered further analysis of HNK-1-capped O-mannosyl glycans. In the present study, we chemoenzymatically synthesized HNK-1-capped core M2 glycans for antibody production, and confirmed that the resulting immune sera reacted with HNK-1-capped core M2 glycans. We then examined several HNK-1-related antibodies, including the Cat-315 antibody, for reactions with HNK-1-capped core M2 glycans. Finally, we confirmed the increased HNK-1 epitope expression in demyelinated brains of cuprizone-fed mice.

To investigate the positive rate for the Cochlin tomo-protein (CTP: an inner ear-specific protein) detection test among patients with inner ear-related clinical manifestations and evaluate the clinical characteristics of definite perilymphatic fistula (PLF).We have performed an ELISA-based CTP detection test using middle ear lavage (MEL) samples from 497 cases of suspected PLF enrolled from 70 clinical centers nationwide between 2014 and 2015. In addition to the CTP-positive rate, audio-vestibular symptoms were compared between CTP-positive and -negative cases.8-50% of patients in category 1 (trauma, middle and inner ear disease cases), and about 20% of those in categories 2, 3 and 4 (external origin antecedent events, internal origin antecedent events, and without antecedent event, respectively) were positive for CTP. In category 1 cases, the earlier tested samples showed a higher CTP-positive rate, whereas no differences were observed in categories 2, 3 or 4. The characteristic clinical features in the earlier tested cases were nystagmus and fistula sign in CTP test-positive cases in category 1, and streaming water-like tinnitus in those in categories 2, 3 and 4.The present study clarified that CTP detection test-positive patients exist at considerable rates among patients with inner ear-related manifestations.

We present the jet kinematics of the flat spectrum radio quasar (FSRQ) 4C +21.35 using time-resolved KaVA very long baseline interferometry array radio maps obtained from September 2014 to July 2016. During two out of three observing campaigns, observations were performed bi-weekly at 22 and 43 GHz quasi-simultaneously. At 22 GHz, we identified three jet components near the core with apparent speeds up to (14.4+/-2.1)c. The timing of the ejection of a new component detected in 2016 is consistent with a gamma-ray flare in November 2014. At 43 GHz, we found four inner jet (, 11 pages, 9 figures, 3 tables. To appear in MNRAS (submitted 2018 June 7; accepted 2019 March 28)

(abridged) Very long baseline interferometry (VLBI) observations at 86$\,$GHz (wavelength, $\lambda = 3\,$mm) reach a resolution of about 50 $\mu$as, probing the collimation and acceleration regions of relativistic outflows in active galactic nuclei. To extend the statistical studies of compact extragalactic jets, a large global 86 GHz VLBI survey of 162 radio sources was conducted in 2010-2011 using the Global Millimeter VLBI Array. The survey data attained a typical baseline sensitivity of 0.1 Jy and a typical image sensitivity of 5 mJy/beam, providing successful detections and images for all of the survey targets. For 138 objects, the survey provides the first ever VLBI images made at 86 GHz. Gaussian model fitting of the visibility data was applied to represent the structure of the sources. The Gaussian model-fit-based estimates of brightness temperature ($T_\mathrm{b}$) at the jet base (core) and in moving regions (jet components) downstream from the core were compared to the estimates of $T_\mathrm{b}$ limits made directly from the visibility data, demonstrating a good agreement between the two methods. The apparent brightness temperature estimates for the jet cores in our sample range from $2.5 \times 10^{9}\,$K to $ 1.3\times 10^{12}\,$K. A population model with a single intrinsic value of brightness temperature, $T_\mathrm{0}$, is applied to reproduce the observed $T_\mathrm{b}$ distribution. It yields $T_\mathrm{0} = (3.77^{+0.10}_{-0.14}) \times 10^{11}\,$K for the jet cores, implying that the inverse Compton losses dominate the emission. In the jet components, $T_\mathrm{0} =(1.42^{+0.16}_{-0.19})\times 10^{11}\,$K is found, slightly higher than the equipartition limit of $\sim5\times 10^{10}\,$K expected for these jet regions. For objects with sufficient structural detail detected, the adiabatic energy losses dominate the observed changes of $T_\mathrm{b}$ along the jet., Comment: 25 pages, 12 figures, 7 tables, accepted for publication in A&A

This paper explains the device structure and operation of image sensors and solar cells. Both are semiconductor devices operating with the same physical principle of detecting photons. A high efficiency of the photon to electron energy conversion is very much desired in both devices. Image sensors now use a very advanced and scaled down CMOS fabrication process technology to achieve high performance features such as the excellent short wave blue light sensitivity for good color reproduction, the low noise and the no image lag picture quality for filmless and mechanical free action cameras. On the other hand, solar cells are still now built with the primitive floating N+P single junction type photodiode to minimize the fabrication process cost but with very low energy conversion efficiency of about 20%. It is explained in details that the depletion region of the PN junction is not the only place where we can achieve photo electron and hole pair separations effectively. The short-wave blue light has only 1000 Å silicon crystal penetration depth. The pinned surface P+P Gaussian doping profile has a very important role to achieve a better photon to energy conversion efficiency, especially for the short-wave blue light. Electrostatic and dynamic behaviors of Pinned Surface P+PNP Double Junction type Dynamic Photo Transistor and Pinned Surface P+PNPN Triple Junction type Dynamic Photo Thyristor are analyzed in details. Both of them are shown to be expected to have much excellent photon-to-electron energy conversion efficiency.

We present recent observation results of Sgr A* at millimeter obtained with VLBI arrays in Korea and Japan.7 mm monitoring of Sgr A* is part of our AGN large project. The results at 7 epochs during 2013-2014, including high resolution maps, flux density and two-dimensional size measurements are presented. The source shows no significant variation in flux and structure related to the G2 encounter in 2014. According to recent MHD simulations by kawashimaet al., flux and magnetic field energy can be expected to increase several years after the encounter; We will keep our monitoring in order to test this prediction.Astrometric observations of Sgr A* were performed in 2015 at 7 and 3.5 millimeter simultaneously. Source-frequency phase referencing was applied and a combined ”core-shift” of Sgr A* and a nearby calibrator was measured. Future observations and analysis are necessary to determine the core-shift in each source.

We study the kinematics of the M87 jet using the first year data of the KVN and VERA Array (KaVA) large program, which has densely monitored the jet at 22 and 43 GHz since 2016. We find that the apparent jet speeds generally increase from $\approx0.3c$ at $\approx0.5$ mas from the jet base to $\approx2.7c$ at $\approx20$ mas, indicating that the jet is accelerated from subluminal to superluminal speeds on these scales. We perform a complementary jet kinematic analysis by using archival Very Long Baseline Array monitoring data observed in $2005-2009$ at 1.7 GHz and find that the jet is moving at relativistic speeds up to $\approx5.8c$ at distances of $200-410$ mas. We combine the two kinematic results and find that the jet is gradually accelerated over a broad distance range that coincides with the jet collimation zone, implying that conversion of Poynting flux to kinetic energy flux takes place. If the jet emission consists of a single streamline, the observed trend of jet acceleration ($\Gamma\propto z^{0.16\pm0.01}$) is relatively slow compared to models of a highly magnetized jet. This indicates that Poynting flux conversion through the differential collimation of poloidal magnetic fields may be less efficient than expected. However, we find a non-negligible dispersion in the observed speeds for a given jet distance, making it difficult to describe the jet velocity field with a single power-law acceleration function. We discuss the possibility that the jet emission consists of multiple streamlines following different acceleration profiles, resulting in jet velocity stratification., Comment: Accepted for publication in ApJ; This is a new version after updating Figure 11 in the manuscript

We present searches for 22 GHz H$_2$O masers toward 36 narrow-line Seyfert 1 galaxies (NLS1s), selected from known NLS1s with $v_{sys}$ $\lesssim$ 41000 km/s. Out of the 36 NLS1s in our sample, 11 NLS1s have been first surveyed in our observations, while the observations of other NLS1s were previously reported in literature. In our survey, no new water maser source from NLS1s was detected at 3 $\sigma$ rms level of 8.4 mJy to 144 mJy, which depends on different observing conditions or inhomogeneous sensitivities of each observation using three different telescopes. It is likely that non-detection of new masers in our NLS1 sample is primarily due to insufficient sensitivities of our observations. Including the five known NLS1 masers, the total detection rate of the H$_2$O maser in NLS1s is not remarkably different from that of type 2 Seyfert galaxies or LINERs. However, more extensive and systematic searches of NLS1 would be required for statistical discussion of the detection rate of the NLS1 maser, compared with that of type 2 Seyferts or LINERs., Comment: 9 pages, 2 figures, accepted for publication in PASJ on 28/03/2018

The advance of CMOS process is still going, but the end is coming into sight. Semiconductor chips with advanced process later than 21nm are so expensive that they are developed only for million selling products. On the other hand, the advanced AI, IoT and big data technologies require more and more computation/communication power with a tightly limited power budget. How we can develop a “Cool chips” in the next decade? And how can the conference “Cool chips” contribute?

Multiple sclerosis (MS) is an inflammatory demyelinating disease of the central nervous system (CNS), and experimental autoimmune encephalomyelitis (EAE) is a well-established animal model of the disease. Here, we examined the pathophysiological role of Kallikrein 6 (Klk6), a serine protease produced by oligodendrocytes (OLs), in EAE using Klk6 knockout (Klk6-/-) mice. Compared with Klk6+/+ (wild-type) mice, Klk6-/- mice showed milder EAE symptoms, including delayed onset and milder paralysis. Loss of Klk6 suppressed matrix metalloprotease-9 expression and diminished the infiltration of peripheral inflammatory cells into the CNS by decreasing blood-brain barrier (BBB) permeability and reducing expression levels of inflammatory cytokines, chemokines and their receptors. Scanning electron microscopic analysis revealed demyelination characterized by myelin detachment from the axons in the early phase of EAE progression (days 3-7) in Klk6+/+ mice but not in Klk6-/- mice. Interestingly, anti-MOG (myelin oligodendrocyte glycoprotein) autoantibody was also detected in the cerebrospinal fluid (CSF) and spinal cord on day 3 after MOG immunization. Furthermore, treatment of primary cultured OLs with anti-MOG autoantibody induced oligodendroglial morphological changes and increases in myelin basic protein and Klk6 expression. We also developed a novel enzyme-linked immunoabsorbent assay method for detecting activated KLK6 in human CSF. In human autopsy brain samples, expression of active KLK6 was detected in OLs using an antibody that specifically recognizes the protein's activated form. Taken together, our findings demonstrate that Klk6 secreted by OLs plays a critical role in the pathogenesis of EAE/MS and that it might serve as a potential therapeutic target for MS.

We present ALMA cycle 0 observations of the luminous merger VV 114. One of the main goals is to investigate mechanisms of molecular line ratio enhancement. Regions with the high 12CO (1–0)/13CO (1–0) and 12CO (3–2)/12CO (1–0) is located at a central filamentary structure (∼6 kpc) in VV 114. The filament consists of the eastern nucleus and the overlap region, where the galaxy disks are colliding. We also investigate these molecular line ratios on the Kennicutt-Schmidt law. VV 114 fills a gap between the “starburst” sequence and the “normal disk” sequence, and regions with the high ratios show the high ΣSFR and ΣH2. We suggest that the high ratios in VV 114 are due to star-forming activities in the both progenitor's nuclei and the merger-induced overlap region.

We report the detection of two CH$_3$OH lines (J$_K$ = 2$_K$-1$_K$ and 3$_K$-2$_K$) between the progenitor's disks ("Overlap") of the mid-stage merging galaxy VV 114 obtained using the Atacama Large Millimeter/submillimeter Array (ALMA) Band 3 and Band 4. The detected CH$_3$OH emission show an extended filamentary structure (~ 3 kpc) across the progenitor's disks with relatively large velocity width (FWZI ~ 150 km/s). The emission is only significant in the "overlap" and not detected in the two merging nuclei. Assuming optically-thin emission and local thermodynamic equilibrium (LTE), we found the CH$_3$OH column density relative to H$_2$ ($X_{\rm CH_3OH}$) peaks at the "Overlap" (~ 8 $\times$ 10$^{-9}$), which is almost an order of magnitude larger than that at the eastern nucleus. We suggest that kpc-scale shocks driven by galaxy-galaxy collision may play an important role to enhance the CH$_3$OH abundance at the "Overlap". This scenario is consistent with that shock-induced large velocity dispersion components of ionized gas have been detected in optical wavelength at the same region. Conversely, low $X_{\rm CH_3OH}$ at the nuclear regions might be attributed to the strong photodissociation by nuclear starbursts and/or putative active galactic nucleus (AGN), or inefficient production of CH$_3$OH on dust grains due to initial high temperature conditions (i.e., desorption of the precursor molecule, CO, into gas-phase before forming CH$_3$OH on dust grains). These ALMA observations demonstrate that CH$_3$OH is a unique tool to address kpc-scale shock-induced gas dynamics and star formation in merging galaxies., 8 pages, 4 figures, 3 tables, accepted for publication in ApJ

Dentin matrix protein 1 (DMP1), a noncollagenous bone matrix protein produced by osteocytes, regulates matrix mineralization and phosphate homeostasis. The lack of a precise assay for circulating DMP1 levels impairs further investigation of the protein's biological significance. Because full-length precursor DMP1 is cleaved into NH2- and COOH-terminal fragments during the secretory process, we developed two new sandwich ELISAs for the NH2- and COOH-terminal fragments of rat DMP1. One of these ELISAs, ELISA 1-2, is based on two affinity-purified polyclonal antibodies against the DMP1-1 and DMP1-2 peptides of the NH2-terminal fragment, whereas the other, ELISA 4-3, is based on two affinity-purified polyclonal antibodies against the DMP1-3 and DMP1-4 peptides of the COOH-terminal fragment. The polyclonal antibodies were characterized in immunohistochemical and liquid chromatography-electrospray ionization tandem mass spectrometry (LC-MS/MS) studies. Immunohistochemical analyses of rat bone using these polyclonal antibodies revealed DMP1 immunoreactivity in osteocytes and pericanalicular matrix, consistent with the previously reported osteocyte-specific expression of DMP1. LC-MS/MS analyses of rat plasma-derived immunoreactive products affinity-extracted with these antibodies revealed the presence of DMP1 in circulating blood. The ELISAs established with these antibodies met accepted standards for reproducibility, repeatability, precision, and accuracy. Circulating DMP1 and levels of other biochemical markers (osteocalcin, Trap5b, Dkk-1, and SOST) were measured in 2-, 4-, 8-, 12-, 18-, 24-, 72-, and 96-week-old Wistar male rats. Circulating DMP1 levels determined by ELISAs 1-2 and 4-3 significantly decreased with age. During rapid skeletal growth (2-12weeks), DMP1 levels measured by ELISA 4-3 were over three times higher than those measured by ELISA 1-2; however, DMP1 levels in old animals (72 and 96weeks) were almost the same when measured by either ELISA. DMP1 levels determined by both ELISAs were most highly positively correlated with the level of Dkk-1, second most highly correlated with the level of osteocalcin, and less highly correlated with the levels of Trap5b and SOST. These novel sandwich ELISAs for rat DMP1 are highly specific and allow precise measurements of circulating DMP1, which may be a new biochemical marker for osteocyte-mediated bone turnover.

Most Alzheimer disease (AD) patients show deposition of amyloid β (Aβ) peptide in blood vessels as well as the brain parenchyma. We previously found that vascular endothelial cells express amyloid β precursor protein (APP) 770, a different APP isoform from neuronal APP695, and produce Aβ. Since the soluble APP cleavage product, sAPP, is considered to be a possible marker for AD diagnosis, sAPP has been widely measured as a mixture of these variants. We hypothesized that measurement of the endothelial APP770 cleavage product in patients separately from that of neuronal APP695 would enable discrimination between endothelial and neurological dysfunctions. Using our newly developed ELISA system for sAPP770, we observed that inflammatory cytokines significantly enhanced sAPP770 secretion by endothelial cells. Furthermore, we unexpectedly found that sAPP770 was rapidly released from activated platelets. We also found that cerebrospinal fluid mainly contained sAPP695, while serum mostly contained sAPP770. Finally, to test our hypothesis that sAPP770 could be an indicator for endothelial dysfunction, we applied our APP770 ELISA to patients with acute coronary syndrome (ACS), in which endothelial injury and platelet activation lead to fibrous plaque disruption and thrombus formation. Development of a biomarker is essential to facilitate ACS diagnosis in clinical practice. The results revealed that ACS patients had significantly higher plasma sAPP770 levels. Furthermore, in myocardial infarction model rats, an increase in plasma sAPP preceded the release of cardiac enzymes, currently used markers for acute myocardial infarction. These findings raise the possibility that sAPP770 can be a useful biomarker for ACS.

A spherosilicate dendrimer (DMS-1) with closely spaced reaction sites (Si-H groups) on the dendrimer surface has been synthesized by stepwise silylation of double-four-ring silicate with chlorotriethoxysilane (ClSi(OEt)(3)) and subsequently with chlorodimethylsilane (ClSiHMe(2)). DMS-1 consists of a maximum of 40 Si atoms in the interior frameworks and 24 reactive Si-H groups on the surface. Because DMS-1 is spherical and about 1.5 nm in diameter, it can be regarded as the smallest well-defined silica-based nanoparticle. DMS-1 also forms molecular crystals and is soluble in typical organic solvents. A molecularly ordered silica-based hybrid can be prepared by heating a cast film of DMS-1 at 180 °C for 5 days. The surface of DMS-1 can be modified by hydrosilylation with 1-hexadecene, triethoxyvinylsilane, and allylic-terminated tetraethylene glycol monomethyl ether. More than 20 Si-H groups out of 24 react with these reagents. The solubilities of the products depend on the modification. DMS-1 is not only a building block for nanohybrids, but also the smallest and most precisely designed siloxane-based nanoparticle.

Transplantation of surrogate β-cells is a promising option for the treatment of insulin-deficient diabetes mellitus in the future. Although pancreatic exocrine cells of rodents have been shown to transdifferentiate into insulin-secreting cells, no studies are reported on human exocrine cells. Here, we report the generation of insulin-secreting cells from exocrine cells of the human pancreas. When cultured in suspension with epidermal growth factor, human pancreatic exocrine cells readily formed spherical cell clusters. Expression of Pdx1 was induced in all 19 cases in which we successfully isolated exocrine cells, and insulin expression was induced in 11 cases. In addition, insulin secretion was evaluated in four cases, and the newly-made cells were found to secrete insulin in response to various stimuli. Although further studies are required to improve both the quality and quantity of such insulin-secreting cells, our data suggest that pancreatic exocrine cells represent a potential source of insulin-secreting cells for treatment of type 1 diabetes. (J Diabetes Invest, doi: 10.1111/j.2040-1124.2010.00095.x, 2011)

We present high-resolution observations (0".2-1".5) of multiple dense gas tracers, HCN and HCO$^+$ ($J$ = 1-0, 3-2, and 4-3), HNC ($J$ = 1-0), and CS ($J$ = 7-6) lines, toward the nearby luminous infrared galaxy VV 114 with the Atacama Large Millimeter/submillimeter Array. All lines are robustly detected at the central gaseous filamentary structure including the eastern nucleus and the Overlap region, the collision interface of the progenitors. We found that there is no correlation between star formation efficiency and dense gas fraction, indicating that the amount of dense gas does not simply control star formation in VV 114. We predict the presence of more turbulent and diffuse molecular gas clouds around the Overlap region compared to those at the nuclear region assuming a turbulence-regulated star formation model. The intracloud turbulence at the Overlap region might be excited by galaxy-merger-induced shocks, which also explains the enhancement of gas-phase CH$_3$OH abundance previously found there. We also present spatially resolved spectral line energy distributions of HCN and HCO$^+$ for the first time, and derive excitation parameters by assuming optically-thin and local thermodynamic equilibrium (LTE) conditions. The LTE model revealed that warmer, HCO$^+$-poorer molecular gas medium is dominated around the eastern nucleus, harboring an AGN. The HCN abundance is remarkably flat ($\sim$3.5 $\times$ 10$^{-9}$) independently of the various environments within the filament of VV 114 (i.e., AGN, star formation, and shock)., 23 pages, 21 figures (downconverted), 5 tables, accepted for publication in ApJ

A bifunctional siloxane cage, where double four-membered ring (D4R) silicate was capped with alkoxyvinylsilyl groups, was synthesized as a novel building block for the formation of inorganic–organi...

Expressed in renal carcinoma (ERC)/mesothelin is a good biomarker for human mesothelioma and has been investigated for its mechanistic rationale during the mesothelioma development. Studies are thus ongoing in our laboratories to assess expression of ERC/mesothelin in sera and normal/proliferative/neoplastic mesothelial tissues of animals untreated or given potentially mesothelioma-inducible xenobiotics, by an enzyme-linked immunosorbent assay (ELISA) for N- and C-(terminal fragments of) ERC/mesothelin and immunohistochemistry for C-ERC/mesothelin. In the present paper, we intend to communicate our preliminary data, because this is the first report to show how and from what stage the ERC/mesothelin expression changes during the chemical induction of mesothelial proliferative/neoplatic lesions. Serum N-ERC/mesothelin levels were 51.4 +/- 5.6 ng/ml in control male Fischer 344 rats, increased to 83.6 +/- 11.2 ng/ml in rats given a single intrascrotal administration of 1 mg/kg body weight of multi-wall carbon nanotube (MWCNT) and bearing mesothelial hyperplasia 52 weeks thereafter, and further elevated to 180 +/- 77 ng/ml in rats similarly treated and becoming moribund 40 weeks thereafter, or killed as scheduled at the end of week 52, bearing mesothelioma. While C-ERC/mesothelin was expressed in normal and hyperplastic mesothelia, the protein was detected only in epithelioid mesothelioma cells at the most superficial layer. It is thus suggested that ERC/mesothelin can be used as a biomarker of mesothelial proliferative lesions also in animals, and that the increase of levels may start from the early stage and be enhanced by the progression of the mesothelioma development.

Mesothelioma is an aggressive cancer often caused by chronic asbestos exposure, and its prognosis is very poor despite the therapies currently used. Due to the long latency period between asbestos exposure and tumor development, the worldwide incidence will increase substantially in the next decades. Thus, novel effective therapies are warranted to improve the prognosis. The ERC/mesothelin gene (MSLN) is expressed in wide variety of human cancers, including mesotheliomas, and encodes a precursor protein cleaved by proteases to generate C-ERC/mesothelin and N-ERC/mesothelin. In this study, we investigated the antitumor activity of C-ERC/mesothelin-specific mouse monoclonal antibody, 22A31, against tumors derived from a human mesothelioma cell line, ACC-MESO-4, in a xenograft experimental model using female BALB/c athymic nude mice. Treatment with 22A31 did not inhibit cell proliferation of ACC-MESO-4 in vitro; however, therapeutic treatment with 22A31 drastically inhibited tumor growth in vivo. 22A31 induced antibody-dependent cell-mediated cytotoxicity by natural killer (NK) cells, but not macrophages, in vitro. Consistently, the F(ab')(2) fragment of 22A31 did not inhibit tumor growth in vivo, nor did it induce antibody-dependent cell mediated cytotoxicity (ADCC) in vitro. Moreover, NK cell depletion diminished the antitumor effect of 22A31. Thus, 22A31 induced NK cell-mediated ADCC and exerted antitumor activity in vivo. 22A31 could have potential as a therapeutic tool to treat C-ERC/mesothelin-expressing cancers including mesothelioma.

Pancreatic ductal adenocarcinoma (PDA) is a highly lethal disease, which is usually diagnosed in an advanced stage. Animal PDA models which reflect the human condition are clearly necessary to develop early diagnostic tools and explore new therapeutic approaches. We have established transgenic rats carrying a mutated H- or K-ras gene (Hras250 and Kras327) controlled by Cre/loxP activation. These animals develop PDA which are histopathologically similar to that in humans. We utilized this model to identify biomarkers to detect early PDA. We report here that serum levels of Erc/Mesothelin are significantly higher in rats bearing PDA than in controls. Importantly, the levels are significantly elevated in rats before grossly visible carcinomas develop. Even in rats with very small microscopic ductal carcinoma lesions, elevated serum Erc/Mesothelin can be detected. We believe this is the first report of a pancreas tumor animal model in which pre-symptomatic lesions can be diagnosed.