M Tanaka

National Astronomical Observatory of Japan, Edo, Tōkyō, Japan

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Publications (790)2054.56 Total impact

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    ABSTRACT: The paper describes a time- and angle-resolved photoemission apparatus consisting of a hemispherical analyzer and a pulsed laser source. We demonstrate 1.48-eV pump and 5.92-eV probe measurements at the 10.5-meV and 240-fs resolutions by use of fairly monochromatic 170-fs pulses delivered from a regeneratively amplified Ti:sapphire laser system operating typically at 250 kHz. The apparatus is capable to resolve the optically filled superconducting peak in the unoccupied states of a cuprate superconductor, Bi2Sr2CaCu2O8 + δ. A dataset recorded on Bi(111) surface is also presented. Technical descriptions include the followings: A simple procedure to fine-tune the spatio-temporal overlap of the pump-and-probe beams and their diameters; achieving a long-term stability of the system that enables a normalization-free dataset acquisition; changing the repetition rate by utilizing acoustic optical modulator and frequency-division circuit.
    Review of Scientific Instruments 11/2014; 85(12). · 1.58 Impact Factor
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    ABSTRACT: The CFHTLS presents a unique data set for weak lensing studies, having high quality imaging and deep multi-band photometry. We have initiated an XMM-CFHTLS project to provide X-ray observations of the brightest X-ray selected clusters within the wide CFHTLS area. Performance of these observations and the high quality of CFHTLS data, allows us to revisit the identification of X-ray sources, introducing automated reproducible algorithms, based on the multi-color red sequence finder. We have also introduced a new optical mass proxy. We provide the calibration of the red sequence observed in the CFHT filters and compare the results with the traditional single color red sequence and photoz. We test the identification algorithm on the subset of highly significant XMM clusters and identify 100% of the sample. We find that the integrated z-band luminosity of the red sequence galaxies correlates well with the X-ray luminosity with a surprisingly small scatter of 0.20 dex. We further use the multi-color red sequence to reduce spurious detections in the full XMM and RASS data sets, resulting in catalogs of 196 and 32 clusters, respectively. We made spectroscopic follow-up observations of some of these systems with HECTOSPEC and in combination with BOSS DR9 data. We also describe the modifications needed to the source detection algorithm in order to keep high purity of extended sources in the shallow X-ray data. We also present the scaling relation between X-ray luminosity and velocity dispersion.
    The Astrophysical Journal 11/2014; · 6.28 Impact Factor
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    ABSTRACT: We present weak lensing and X-ray analysis of 12 low mass clusters from the CFHTLenS and XMM-CFHTLS surveys. We combine these systems with high-mass systems from CCCP and low-mass systems from COSMOS to obtain a sample of 70 systems, which we divide into subsamples of 15 merging and 55 relaxed systems. We measure L-T, M-L and M-T scaling relations and find in all cases that the power-law slopes of the full, merging and relaxed subsamples are consistent. For the M-T we find slopes consistent with the self-similar model, whereas L-T results in steeper and M-L in flatter relations. We find a marginal trend for larger scatter and lower normalisation in the M-L and M-T relations for the merging subsample, which we attribute to triaxiality and substructure. We explore the effects of X-ray cross-calibration and find that Chandra calibration leads to flatter L-T and M-T relations. We also utilise the three surveys making up the sample as overlapping mass bins. For COSMOS and CFHTLS we find slopes consistent with the relation fitted to the full sample, whereas the high mass CCCP sample favours flatter slopes. We also find that intermediate mass systems have a higher mass for their luminosity. Unfortunately our sample does not enable direct measurement of a break at low masses, but we find a trend for enhanced intrinsic scatter in mass at low masses.
    10/2014;
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    ABSTRACT: We study the evolution of the total star formation (SF) activity, total stellar mass and halo occupation distribution in massive halos by using one of the largest X-ray selected sample of galaxy groups with secure spectroscopic identification in the major blank field surveys (ECDFS, CDFN, COSMOS, AEGIS). We provide an accurate measurement of SFR for the bulk of the star-forming galaxies using very deep mid-infrared Spitzer MIPS and far-infrared Herschel PACS observations. For undetected IR sources, we provide a well-calibrated SFR from SED fitting. We observe a clear evolution in the level of SF activity in galaxy groups. The total SF activity in the high redshift groups (0.5<z<1.1) is higher with respect to the low redshift (0.15<z<0.5) sample at any mass by 0.8 ± 0.12 dex. A milder difference (0.35 ± 0.1 dex) is observed between the low redshift bin and the groups at z ∼ 0. We show that the level of SF activity is declining more rapidly in the more massive halos than in the more common lower mass halos. We do not observe any evolution in the halo occupation distribution and total stellar mass-halo mass relations in groups. The picture emerging from our findings suggests that the galaxy population in the most massive systems is evolving faster than galaxies in lower mass halos, consistently with a "halo downsizing" scenario.
    Monthly Notices of the Royal Astronomical Society 09/2014; 000(1). · 4.90 Impact Factor
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    ABSTRACT: The University of Tokyo Atacama Observatory (TAO) is a project to construct a 6.5-meter telescope optimized for infrared observations at the summit of Co. Chajnantor, 5,640 m altitude. The high altitude and low water vapor (0.5mm in 25% percentile) of the site provide wide wavelength coverage from 0.3 to 38 micron including continuous window from 0.9 to 2.5 micron and new windows at wavelength longer than 25 micron. We report on the design and the current status of the mirror, the telescope, the summit and the base facilities in this paper.
    SPIE Astronomical Telescopes + Instrumentation; 07/2014
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    ABSTRACT: A basic design of enclosure and support facilities for the University of Tokyo Atacama observatory (TAO) 6.5-m telescope is described in this paper. The enclosure facility has a carousel shape with an open-space near the ground surface. The upper carousel rotates independently of the telescope. Horizontally opened slit doors, a dozen ventilation windows, wind and moon shields, and an overhead bridge-crane are equipped. For safety reasons, most of maintenance walkways are placed inside of the enclosure facility. An observation floor of the enclosure facility is connected to the support facility via a bridge for maintenance of observation instruments and a primary mirror of the telescope. Air inside of the enclosure and support facilities is exhausted to an underground tunnel.
    SPIE Astronomical Telescopes + Instrumentation; 07/2014
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    ABSTRACT: We performed optical and near-infrared multi-band linear polarimetry for highly reddened Type Ia SN 2014J appeared in M82. SN 2014J exhibits large polarization at shorter wavelengths, reaching $p\simeq 4.8$\% in $B$ band and steeply decreasing with wavelength, while it has almost constant position angle $\sim 40^{\circ}$ over the observed wavelength range. No significant temporal variation is found. Since intrinsic polarization of continuum light from a normal Type Ia supernova is generally weak ($\lesssim 0.3$\%) and the Galactic interstellar polarization component is likely negligibly small, the observed polarization is likely predominantly caused by the interstellar media within M82; however, we cannot completely exclude the possibility that it is caused by circumstellar media. The wavelength dependence of polarization can be explained by the empirical Serkowski-law at wavelengths shorter than $1 \mu$m and by an inverse power-law at wavelengths longer than $0.5 \mu$m. The peak polarization wavelength $\lambda_{\rm max}$ is quite short, $\lesssim 0.4\ \mu$m, suggesting the mean radius of polarizing dust grains is small ($< 0.1 \mu$m). The empirical law between $K$ and $\lambda_{\rm max}$ for the Galactic interstellar polarization is apparently broken, although the positive correlation between $R_{V}=A_{V}/E_{B-V}$ and $\lambda_{\rm max}$ seems to still hold. These facts suggest the nature of the dust grains in M82 is different from that in our Galaxy. These observed properties are similar to those in the other highly reddened Type Ia SNe 1986G and 2006X that have ever been polarimetrically observed, and this high probability suggests that such properties of dust grains are rather common in extragalaxies.
    07/2014;
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    ABSTRACT: We demonstrate monolithic integration of pseudo-spin-MOSFETs (PS-MOSFETs) using vendor-made MOSFETs fabricated in a low-cost multi-project wafer (MPW) product and lab-made magnetic tunnel junctions (MTJs) formed on the topmost passivation film of the MPW chip. The tunneling magnetoresistance (TMR) ratio of the fabricated MTJs strongly depends on the surface roughness of the passivation film. Nevertheless, after the chip surface was atomically flattened by SiO2 deposition on it and successive chemical–mechanical polish (CMP) process for the surface, the fabricated MTJs on the chip exhibits a sufficiently large TMR ratio (>140%) adaptable to the PS-MOSFET application. The implemented PS-MOSFETs show clear modulation of the output current controlled by the magnetization configuration of the MTJs, and a maximum magnetocurrent ratio of 90% is achieved. These magnetocurrent behaviour is quantitatively consistent with those predicted by HSPICE simulations. The developed integration technique using a MPW CMOS chip would also be applied to monolithic integration of CMOS devices/circuits and other various functional devices/materials, which would open the door for exploring CMOS-based new functional hybrid circuits.
    Solid-State Electronics 07/2014; · 1.51 Impact Factor
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    ABSTRACT: The kinetic energy of supernovae (SNe) accompanied by gamma-ray bursts (GRBs) tends to cluster near E52 erg, with 2.E52 erg an upper limit to which no compelling exceptions are found (assuming a certain degree of asphericity), and it is always significantly larger than the intrinsic energy of the GRB themselves (corrected for jet collimation). This energy is strikingly similar to the maximum rotational energy of a neutron star rotating with period 1 ms. It is therefore proposed that all GRBs associated with luminous SNe are produced by magnetars. GRBs that result from black hole formation (collapsars) may not produce luminous SNe. X-ray Flashes (XRFs), which are associated with less energetic SNe, are produced by neutron stars with weaker magnetic field or lower spin.
    Monthly Notices of the Royal Astronomical Society 06/2014; 443(1). · 5.23 Impact Factor
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    ABSTRACT: The electronic and magnetic properties of Fe atoms in the ferromagnetic semiconductor (In,Fe)As codoped with Be have been studied by x-ray absorption spectroscopy (XAS) and x-ray magnetic circular dichroism (XMCD) at the Fe $L_{2,3}$ edge. The XAS and XMCD spectra showed simple spectral line shapes similar to Fe metal, but the ratio of the orbital and spin magnetic moments ($M_\mathrm{orb}$/$M_\mathrm{spin}$) estimated using the XMCD sum rules was significantly larger than that of Fe metal, indicating a significant orbital moment of Fe $3d$ electrons in (In,Fe)As:Be. The positive value of $M_\mathrm{orb}$/$M_\mathrm{spin}$ implies that the Fe $3d$ shell is more than half-filled, which arises from the hybridization of the Fe$^{3+}$ ($d^5$) state with the charge-transfer $d^6\underline{L}$ states, where $\underline{L}$ is a ligand hole in the host valence band. The XMCD intensity as a function of magnetic field indicated hysteretic behavior of the superparamagnetic-like component due to discrete ferromagnetic domains.
    Applied Physics Letters 05/2014; 105(3). · 3.52 Impact Factor
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    ABSTRACT: We present a catalog of 129 X-ray galaxy groups, covering a redshift range 0.04<z<1.23, selected in the ~3 square degree part of the CFHTLS W1 field overlapping XMM observations performed under the XMM-LSS project. We carry out a statistical study of the redshift evolution out to redshift one of the magnitude gap between the first and the second brightest cluster galaxies of a well defined mass-selected group sample. We find that the slope of the relation between the fraction of groups and the magnitude gap steepens with redshift, indicating a larger fraction of fossil groups at lower redshifts. We find that 22.2$\pm$6% of our groups at z$\leq$0.6 are fossil groups. We compare our results with the predictions of three semi-analytic models based on the Millennium simulation. The intercept of the relation between the magnitude of the brightest galaxy and the value of magnitude gap becomes brighter with increasing redshift. This trend is steeper than the model predictions which we attribute to the younger stellar age of the observed brightest cluster galaxies. This trend argues in favor of stronger evolution of the feedback from active galactic nuclei at z<1 compared to the models. The slope of the relation between the magnitude of the brightest cluster galaxy and the value of the gap does not evolve with redshift and is well reproduced by the models, indicating that the tidal galaxy stripping, put forward as an explanation of the occurrence of the magnitude gap, is both a dominant mechanism and is sufficiently well modeled.
    Astronomy and Astrophysics 05/2014; 566. · 4.48 Impact Factor
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    ABSTRACT: We present a catalog of 129 X-ray galaxy groups, covering a redshift range 0.04
    04/2014;
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    ABSTRACT: Long-duration gamma-ray bursts (GRBs) have been found to be associated with broad-lined type-Ic supernovae (SNe), but only a handful of cases have been studied in detail. Prompted by the discovery of the exceptionally bright, nearby GRB130427A (redshift z=0.3399), we aim at characterising the properties of its associated SN2013cq. This is the first opportunity to test directly the progenitors of high-luminosity GRBs. We monitored the field of the Swift long duration GRB130427A using the 3.6-m TNG and the 8.2-m VLT during the time interval between 3.6 and 51.6 days after the burst. Photometric and spectroscopic observations revealed the presence of the type Ic SN2013cq. Spectroscopic analysis suggests that SN2013cq resembles two previous GRB-SNe, SN1998bw and SN2010bh associated with GRB980425 and XRF100316D, respectively. The bolometric light curve of SN2013cq, which is significantly affected by the host galaxy contribution, is systematically more luminous than that of SN2010bh ($\sim$ 2 mag at peak), but is consistent with SN1998bw. The comparison with the light curve model of another GRB-connected SN2003dh, indicates that SN2013cq is consistent with the model when brightened by 20%. This suggests a synthesised radioactive $^{56}$Ni mass of $\sim 0.4 M_\odot$. GRB130427A/SN2013cq is the first case of low-z GRB-SN connection where the GRB energetics are extreme ($E_{\rm \gamma, iso} \sim 10^{54}$ erg). We show that the maximum luminosities attained by SNe associated with GRBs span a very narrow range, but those associated with XRFs are significantly less luminous. On the other hand the isotropic energies of the accompanying GRBs span 6 orders of magnitude (10$^{48}$ erg $< E_{\rm \gamma, iso} <$ 10$^{54}$ erg), although this range is reduced when corrected for jet collimation. The GRB total radiated energy is in fact a small fraction of the SN energy budget.
    Astronomy and Astrophysics 04/2014; 567. · 4.48 Impact Factor
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    ABSTRACT: We studied the chronology of galactic bulge and disc formation by analysing the relative contributions of these components to the B-band rest-frame luminosity density at different epochs. We present the first estimate of the evolution of the fraction of rest-frame B-band light in galactic bulges and discs since redshift z~0.8. We performed a bulge-to-disc decomposition of HST/ACS images of 3266 galaxies in the zCOSMOS-bright survey with spectroscopic redshifts in the range 0.7 < z < 0.9. We find that the fraction of B-band light in bulges and discs is $(26 \pm 4)%$ and $(74 \pm 4)%$, respectively. When compared with rest-frame B-band measurements of galaxies in the local Universe in the same mass range ($10^{9} M_{\odot}\lessapprox M \lessapprox 10^{11.5} M_{\odot}$), we find that the B-band light in discs decreases by ~30% from z~0.7-0.9 to z~0, while the light from the bulge increases by ~30% over the same period of time. We interpret this evolution as the consequence of star formation and mass assembly processes, as well as morphological transformation, which gradually shift stars formed at half the age of the Universe from star-forming late-type/irregular galaxies toearlier types and ultimately into spheroids.
    Astronomy and Astrophysics 03/2014; 564. · 4.48 Impact Factor
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    ABSTRACT: We have developed an Electron-Tracking Compton Camera (ETCC) for an all-sky survey at the MeV gamma-ray band. The ETCC consists of a gaseous tracker and a position sensitive scintillation camera to measure the momentum of the Compton-recoil electron and the scattering gamma ray so that we can reconstruct the energy and momentum of the incident gamma ray photon by photon. Also the ETCC has strong background rejection methods using tracking information such as the dE/dx particle identification and theCompton kinematics test. To confirm feasibility of observing celestial objects in space, we performed a balloon experiment to successfully observe the diffuse cosmic and atmospheric gamma rays, which confirmed the effectiveness of the background rejection capability. Based on the first balloon experiment result, we are developing a large ETCC and plan to launch it for the test of the imaging property. The performance of the SMILE-II ETCC is simulated and then it will obtain an effective area of 1.1 cm2 for 200 keV by improving the electron track reconstruction efficiency by a factor of about 10, which results in the detection of Crab nebula at >5σ level for several-hour observation in the middle latitude with an altitude of 40 km.
    Proceedings of the 12th Asia Pacific Physics Conference (APPC12); 03/2014
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    ABSTRACT: We present a large sample of 183 extreme emission-line galaxies (EELGs) at redshift 0.11 < z < 0.93 selected from the 20k zCOSMOS Bright Survey by their unusually large [OIII]5007 equivalent widths. Based on emission-line diagnostics, 165 purely star-forming EELGs and 18 narrow-line AGN candidates are identified. Using multiwavelength COSMOS photometry, HST-ACS I-band imaging and optical zCOSMOS spectroscopy we characterize their main physical properties. EELGs are small (R_50 ~ 1.3 kpc), low-mass (M*/Msol~10^7-10^10) galaxies forming stars at unusually high rates (SFR~0.1-35 Msol/yr), being among the highest specific SFRs galaxies in zCOSMOS. Consistently, the EELGs are luminous and extremely compact at rest-frame UV wavelengths and include strong Ly$\alpha$ emitters, as revealed by GALEX spectroscopy. Using both direct and strong-line methods, we show that zCOSMOS EELGs are low-metallicity systems (12+log(O/H)=8.16 in the median) including several extremely metal-deficient galaxies (<10% solar). Finally, HST-ACS I-band images reveal that ~80% of the EELGs show non-axisymmetric morphologies, including clumpy and tadpole galaxies, and a significant fraction (~29%) of galaxies with additional low surface brightness features strongly suggesting recent or ongoing interactions. As star-forming dwarfs in the local Universe, EELGs are preferably found in relative isolation. While only very few EELGs belong to compact groups, almost one third of them are found in spectroscopically confirmed loose pairs or triplets. The zCOSMOS EELGs are galaxies caught in a transient and probably early period of their evolution, where they are efficiently building-up a significant fraction of their present-day stellar mass in an ongoing galaxy-wide starburst. Therefore, the EELGs constitute an ideal benchmark for comparison studies between low- and high-redshift low-mass star-forming galaxies.
    03/2014;
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    ABSTRACT: Joint contributions of the Pierre Auger and Telescope Array Collaborations to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013: cross-calibration of the fluorescence telescopes, large scale anisotropies and mass composition.
    10/2013;
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    ABSTRACT: Since the first light observation of ANIR in June 2009, we have been carrying out a Paα narrow-band imaging survey of nearby luminous infrared galaxies (LIRGs). Because Paα is the strongest hydrogen recombination line in the infrared wavelength ranges, it is a good and direct tracer of dust-enshrouded star forming regions, and enables us to probe the star formation activities in LIRGs. We find that LIRGs have two star-forming modes. The origin of the two modes probably come from differences between merging stage and/or star-forming process.
    10/2013;
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    ABSTRACT: Fossil groups are considered the end product in a galaxy group's evolution -- a massive central galaxy that dominates the luminosity budget of the group, as the outcome of efficient merging between intermediate-luminosity members. Little is however known about the faint satellite systems of fossil groups. Here we present a SUBARU/Suprime-Cam wide-field, deep imaging study in the B- and R-band of the nearest fossil group NGC 6482 (M_{tot}\sim4\times10^{12}M_{\sun}), covering the virial radius out to 310 kpc. We perform detailed completeness estimations and select group member candidates by a combination of automated object detection and visual inspection. A fiducial sample of 48 member candidates down to M_R -10.5 mag is detected, making this study the deepest of a fossil group up to now. We investigate the photometric scaling relations, the colour-magnitude relation, and the luminosity function of our galaxy sample. We find evidence of recent and ongoing merger events among bright group galaxies. The colour-magnitude relation is comparable to that of nearby galaxy clusters, and exhibits significant scatter at the faintest luminosities. The completeness-corrected luminosity function is dominated by early-type dwarfs and is characterized by a faint end slope \alpha=-1.32\pm0.05. We conclude that the NGC 6482 fossil group shows photometric properties consistent with those of regular galaxy clusters and groups, including a normal abundance of faint satellites.
    Astronomy and Astrophysics 09/2013; · 4.48 Impact Factor
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    ABSTRACT: We present an analysis of cool outflowing gas around galaxies, traced by MgII absorption lines in the co-added spectra of a sample of 486 zCOSMOS galaxies at 1 < z < 1.5. These galaxies span a range of stellar masses (9.45< log[M*/Msun]<10.7) and star formation rates (0.14 < log [SFR/Msun/yr] < 2.35). We identify the cool outflowing component in the MgII absorption and find that the equivalent width of the outflowing component increases with stellar mass. The outflow equivalent width also increases steadily with the increasing star formation rate of the galaxies. At similar stellar masses the blue galaxies exhibit a significantly higher outflow equivalent width as compared to red galaxies. The outflow equivalent width shows strong effect with star formation surface density ({\Sigma}SFR) of the sample. For the disk galaxies, the outflow equivalent width is higher for the face-on systems as compared to the edge-on ones, indicating that for the disk galaxies, the outflowing gas is primarily bipolar in geometry. Galaxies typically exhibit outflow velocities ranging from -200 km/s to -300 km/s and on average the face-on galaxies exhibit higher outflow velocity as compared to the edge-on ones. Galaxies with irregular morphologies exhibit outflow equivalent width as well as outflow velocities comparable to face on disk galaxies. These galaxies exhibit minimum mass outflow rates > 5-7 Msun/yr and a mass loading factor ({\eta} = dMout/dt /SFR) comparable to the star formation rates of the galaxies.
    07/2013;

Publication Stats

9k Citations
2,054.56 Total Impact Points

Institutions

  • 2013–2014
    • National Astronomical Observatory of Japan
      • Okayama Astrophysical Observatory
      Edo, Tōkyō, Japan
    • Hiroshima University
      • Division of Physical Sciences
      Hirosima, Hiroshima, Japan
  • 1991–2014
    • The University of Tokyo
      • • Department of Electrical Engineering and Information Systems
      • • Institute for the Physics and Mathematics of the Universe (IPMU)
      • • Institute for Solid State Physics
      • • Department of Astronomy
      • • Department of Electrical and Electronics Engineering
      • • Department of Physics
      Edo, Tōkyō, Japan
    • Tokyo Metropolitan Hiroo Hospital
      • Department of Pathology
      Edo, Tōkyō, Japan
    • Japan Research Institute
      Japan
  • 1973–2013
    • Kyushu University
      • • Division of Surgery
      • • Department of Surgery and Oncology
      • • Faculty of Medical Sciences
      • • Division of Internal Medicine
      Hukuoka, Fukuoka, Japan
  • 2012
    • Tokai University
      Hiratuka, Kanagawa, Japan
    • Honolulu University
      Honolulu, Hawaii, United States
  • 2011–2012
    • The Astronomical Observatory of Brera
      Merate, Lombardy, Italy
    • Paris Diderot University
      Lutetia Parisorum, Île-de-France, France
  • 2010–2012
    • French National Centre for Scientific Research
      • • Institut de recherche en astrophysique et planétologie (IRAP)
      • • Institut d'astrophysique spatiale (IAS)
      Lutetia Parisorum, Île-de-France, France
    • National Institute of Polar Research
      Tatikawa, Tōkyō, Japan
    • Pierre and Marie Curie University - Paris 6
      • Institut d'astrophysique de Paris
      Paris, Ile-de-France, France
    • Max Planck Institute for Extraterrestrial Physics
      Arching, Bavaria, Germany
  • 2000–2012
    • National Institute for Fusion Science
      Tokitsu-chō, Gifu, Japan
  • 2006–2011
    • Japan Atomic Energy Agency
      • • Quantum Beam Science Directorate
      • • Advanced Photon Research Center
      Muramatsu, Niigata, Japan
  • 1925–2011
    • European Southern Observatory
      Arching, Bavaria, Germany
  • 1993–2010
    • Tohoku University
      • • Research Center of Atmospheric and Oceanic Studies
      • • Institute of Multidisciplinary Research for Advanced Materials (IMRAM)
      • • Institute of Development, Aging and Cancer
      Sendai, Kagoshima-ken, Japan
    • Tokyo Junshin Women's College
      • Department of Pathology
      Edo, Tōkyō, Japan
    • Hirosaki University
      Khirosaki, Aomori Prefecture, Japan
    • University of Tsukuba
      • Division of Experimental Psychology & Behavioral Neuroscience
      Tsukuba, Ibaraki, Japan
  • 2009
    • Laboratoire d’Informatique Fondamentale de Marseille
      Marsiglia, Provence-Alpes-Côte d'Azur, France
    • California Institute of Technology
      • Spitzer Science Center
      Pasadena, California, United States
    • Tokyo Gakugei University
      Koganei, Tōkyō, Japan
  • 1994–2009
    • Nara Medical University
      • Department of Urology
      Nara-shi, Nara, Japan
  • 2008
    • Ehime University
      • Department of Physics
      Matuyama, Ehime, Japan
    • SPring-8
      Saitama, Saitama, Japan
  • 1999–2006
    • University of Occupational and Environmental Health
      • • Department of Obstetrics and Gynecology
      • • School of Medicine
      Kitakyūshū, Fukuoka, Japan
  • 1989–2005
    • Osaka City University
      • • Department of Biochemistry
      • • Faculty of Science
      Ōsaka, Ōsaka, Japan
  • 2003
    • Osaka University
      • Institute of Laser Engineering
      Ibaraki, Osaka-fu, Japan
  • 2002
    • Noguchi Thyroid Clinic and Hospital Foundation
      Бэппу, Ōita, Japan
    • High Energy Accelerator Research Organization
      • Institute of Materials Structure Science
      Tsukuba, Ibaraki, Japan
  • 2001
    • Otsu Red Cross Hospital
      Ōtu, Shiga, Japan
    • Kyushu Rosai Hospital
      Kitakyūshū, Fukuoka, Japan
    • Kyoto University
      • Faculty of Integrated Human Studies
      Kyoto, Kyoto-fu, Japan
  • 1996–2001
    • Kanazawa University
      • Cancer Research Institute
      Kanazawa-shi, Ishikawa-ken, Japan
    • Nikko Memorial Hospital
      Hidachi, Ibaraki, Japan
    • Kyushu Kosei Nenkin Hospital
      Kitakyūshū, Fukuoka, Japan
  • 1992–2001
    • National Institute for Basic Biology
      Okazaki, Aichi, Japan
    • Rikkyo University
      • Department of Physics
      Tokyo, Tokyo-to, Japan
  • 1981–2001
    • Kyoto Prefectural University of Medicine
      • • Department of Anatomy
      • • Division of Anatomy and Neurobiology
      • • Department of Anesthesiology
      Kioto, Kyōto, Japan
  • 1996–2000
    • Fukuoka University
      • • Department of Sports Science
      • • Department of Gastroenterology
      Hukuoka, Fukuoka, Japan
  • 1992–1999
    • Hokkaido University Hospital
      • Division of Urology
      Sapporo-shi, Hokkaido, Japan
  • 1998
    • St. Luke's International Hospital
      Edo, Tōkyō, Japan
  • 1990–1998
    • Shinshu University
      Shonai, Nagano, Japan
  • 1994–1997
    • Tokyo Medical and Dental University
      • Department of Medicine
      Edo, Tōkyō, Japan
  • 1993–1997
    • The Graduate University for Advanced Studies
      Миура, Kanagawa, Japan
  • 1995
    • Toyohashi Heart Center
      Toyohasi, Aichi, Japan
    • Osaka Kyoiku University
      Ōsaka, Ōsaka, Japan
  • 1994–1995
    • Niigata University
      • Division of Neuropathology
      Niahi-niigata, Niigata, Japan
  • 1988–1994
    • Gunma University
      • Department of Neurology
      Maebashi, Gunma Prefecture, Japan