M Tanaka

National Astronomical Observatory of Japan, Edo, Tōkyō, Japan

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Publications (761)1905.08 Total impact

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    ABSTRACT: Ultra-deep observations of ECDF-S with Chandra and XMM-Newton enable a search for extended X-ray emission down to an unprecedented flux of $2\times10^{-16}$ ergs s$^{-1}$ cm$^{-2}$. We present the search for the extended emission on spatial scales of 32$^{\prime\prime}$ in both Chandra and XMM data, covering 0.3 square degrees and model the extended emission on scales of arcminutes. We present a catalog of 46 spectroscopically identified groups, reaching a redshift of 1.6. We show that the statistical properties of ECDF-S, such as logN-logS and X-ray luminosity function are broadly consistent with LCDM, with the exception that dn/dz/d$\Omega$ test reveals that a redshift range of $0.2<z<0.5$ in ECDF-S is sparsely populated. The lack of nearby structure, however, makes studies of high-redshift groups particularly easier both in X-rays and lensing, due to a lower level of clustered foreground. We present one and two point statistics of the galaxy groups as well as weak-lensing analysis to show that the detected low-luminosity systems are indeed low-mass systems. We verify the applicability of the scaling relations between the X-ray luminosity and the total mass of the group, derived for the COSMOS survey to lower masses and higher redshifts probed by ECDF-S by means of stacked weak lensing and clustering analysis, constraining any possible departures to be within 30\% in mass. Abridged.
    01/2015;
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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 present APEX LABOCA 870 micron observations of the field around the high-redshift radio galaxy MRC1138-262 at z=2.16. We detect 16 submillimeter galaxies in this ~140 square arcmin bolometer map with flux densities in the range 3-11 mJy. The raw number counts indicate a density of submillimeter galaxies (SMGs) that is up to four times that of blank field surveys. Based on an exquisite multiwavelength database, including VLA 1.4 GHz radio and infrared observations, we investigate whether these sources are members of the protocluster structure at z=2.2. Using Herschel PACS+SPIRE and Spitzer MIPS photometry, we derive reliable far-infrared photometric redshifts for all sources. Follow-up VLT ISAAC and SINFONI near-infrared spectra confirm that four of these SMGs have redshifts of z=2.2. We also present evidence that another SMG in this field, detected earlier at 850 micron, has a counterpart that exhibits Halpha and CO(1-0) emission at z=2.15. Including the radio galaxy and two SMGs with far-IR photometric redshifts at z=2.2, we conclude that at least eight submm sources are part of the protocluster at z=2.16 associated with the radio galaxy MRC1138-262. We measure a star formation rate density SFRD ~1500 Msun yr^-1 Mpc^-3, four magnitudes higher than the global SFRD of blank fields at this redshift. Strikingly, these eight sources are concentrated within a region of 2 Mpc (the typical size of clusters in the local universe) and are distributed within the filaments traced by the Halpha emitters at z=2.2. This concentration of massive, dusty starbursts is not centered on the submillimeter-bright radio galaxy which could support the infalling of these sources into the cluster center. Approximately half (6/11) of the SMGs that are covered by the Halpha imaging data are associated with Halpha emitters, demonstrating the potential of tracing SMG counterparts with this population (abridged).
    Astronomy and Astrophysics 10/2014; 570. · 4.48 Impact Factor
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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: The electronic structure of doped Mn in (Ga,Mn)As is studied by resonant inelastic x-ray scattering. From configuration-interaction cluster-model calculations, the line shapes of the Mn L3 resonant inelastic x-ray scattering spectra can be explained by d-d excitations from the Mn ground state dominated by charge-transferred states, in which hole carriers are bound to the Mn impurities, rather than a pure acceptor Mn2+ ground state. Unlike archetypical d-d excitation, the peak widths are broader than the experimental energy resolution. We attribute the broadening to a finite lifetime of the d-d excitations, which decay rapidly to electron-hole pairs in the host valence and conduction bands through the hybridization of the Mn 3d orbital with the ligand band.
    Physical Review Letters 03/2014; 112(10):107203. · 7.73 Impact Factor
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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: Background Once-daily extended-release tacrolimus (Tac-QD) has been shown to have equivalent efficacy and safety to the twice-daily formulation (Tac-BID) in kidney transplant patients. However, detailed comparison of allograft pathology found on a protocol biopsy (PB) in Tac-QD– versus Tac-BID–based regimens has not been described. Methods We retrospectively investigated 119 de novo living donor kidney transplant patients treated with Tac-QD (n = 90) or Tac-BID (n = 29) and their 3- and 12-month PB results. Other immunosuppressive drugs administered included basiliximab, mycophenolate mofetil, and methylprednisolone. We evaluated daily doses and trough levels of Tac and serum creatinine levels, and compared pathologic findings. Results Daily doses were higher in the Tac-QD group, but trough levels and serum creatinine levels were comparable. On 3- and 12-month PB, the frequency of subclinical rejection was similar between the groups, whereas interstitial fibrosis and tubular atrophy (IF/TA) were less common in the Tac-QD group at 12 months (42.2% vs 20.6%, P = .04). Univariate and multivariate logistic regression analyses revealed that allograft rejection (borderline changes or higher) was associated with IF/TA (odds ratio 4.09, 95% confidence interval 1.76–10.10, P = .001). The Tac-QD–based regimen showed a trend toward the absence of IF/TA but it did not reach statistical significance. Tubular vacuolization and arteriolar hyaline changes were also comparable in the two groups. Conclusions We found a trend toward milder IF/TA, but no significant differences in kidney allograft pathology in patients who were administered Tac-QD– versus Tac-BID–based regimens at 12 months. The effects of Tac-QD on chronic allograft injury must be studied by longer observation.
    Transplantation Proceedings 03/2014; 46(2):395–399. · 0.95 Impact Factor
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    ABSTRACT: Polyomavirus BK nephropathy (BKVN) is an important infectious complication in kidney transplant patients. Regular screening using polymerase chain reaction for BK virus DNA in plasma and urinary cytology is effective for early diagnosis of BKVN. However, methods of follow-up and therapeutic targets are not well described. Ten patients with BKVN who received biweekly urinary cytology and repeat biopsies after diagnosis were retrospectively studied. Histological remission of BKVN was determined when biopsy revealed negative SV40 large T-antigen (TAg) staining. Results of urinary cytology and repeat biopsy findings were compared. Urinary decoy cells disappeared in 8 of 10 patients 55 ± 25 (range 13-79) days after index biopsies. In those cases, allograft function was preserved and the final serum creatinine level was 2.14 ± 1.19 (0.80-4.55) mg/dL after 962 ± 393 (325-1563) days of follow-up. Two cases with persistent urinary decoy cells shedding lost their graft 195 and 362 days later. Amongst 29 repeat biopsies, there were 13 TAg-positive and 16 negative biopsies. In 12 of 13 TAg-positive biopsies (92%), urinary decoy cells were still positive, whereas at the same time in 15 TAg-negative biopsies, decoy cells had already disappeared (94%). Cytology testing is advantageous because of its cost effectiveness. Clearance of decoy cells from urine was closely related to histological remission of BKVN, and may possibly be a therapeutic target in BKVN.
    Transplantation Proceedings 03/2014; 46(2):560-3. · 0.95 Impact Factor
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    ABSTRACT: We investigate the evolution of the star formation rate (SFR)-density relation in the Extended Chandra Deep Field South (ECDFS) and the Great Observatories Origin Deep Survey (GOODS) fields up to z~1.6. In addition to the "traditional method", in which the environment is defined according to a statistical measurement of the local galaxy density, we use a "dynamical" approach, where galaxies are classified according to three different environment regimes: group, "filament-like", and field. Both methods show no evidence of a SFR-density reversal. Moreover, group galaxies show a mean SFR lower than other environments up to z~1, while at earlier epochs group and field galaxies exhibit consistent levels of star formation (SF) activity. We find that processes related to a massive dark matter halo must be dominant in the suppression of the SF below z~1, with respect to purely density-related processes. We confirm this finding by studying the distribution of galaxies in different environments with respect to the so-called Main Sequence (MS) of star-forming galaxies. Galaxies in both group and "filament-like" environments preferentially lie below the MS up to z~1, with group galaxies exhibiting lower levels of star-forming activity at a given mass. At z>1, the star-forming galaxies in groups reside on the MS. Groups exhibit the highest fraction of quiescent galaxies up to z~1, after which group, "filament-like", and field environments have a similar mix of galaxy types. We conclude that groups are the most efficient locus for star-formation quenching. Thus, a fundamental difference exists between bound and unbound objects, or between dark matter haloes of different masses.
    Monthly Notices of the Royal Astronomical Society 10/2013; 437(1). · 5.23 Impact Factor

Publication Stats

12k Citations
1,905.08 Total Impact Points

Institutions

  • 2014
    • National Astronomical Observatory of Japan
      Edo, Tōkyō, Japan
  • 1991–2014
    • Kyushu University
      • • Department of Surgery and Oncology
      • • Division of Surgery
      • • Graduate School of Medical Sciences
      • • Medical Hospital
      • • Faculty of Medical Sciences
      Hukuoka, Fukuoka, Japan
  • 1986–2014
    • The University of Tokyo
      • • Department of Electrical Engineering and Information Systems
      • • Institute for the Physics and Mathematics of the Universe (IPMU)
      • • Department of Astronomy
      • • Department of Electrical and Electronics Engineering
      • • Institute for Solid State Physics
      • • Institute of Industrial Science
      • • Research Center for Advanced Science and Technology
      Edo, Tōkyō, Japan
  • 2013
    • Hiroshima University
      • Division of Physical Sciences
      Hirosima, Hiroshima, Japan
  • 2011–2013
    • University of Maryland, Baltimore County
      Baltimore, Maryland, United States
    • Paris Diderot University
      Lutetia Parisorum, Île-de-France, France
  • 2012
    • Honolulu University
      Honolulu, Hawaii, United States
  • 2011–2012
    • The Astronomical Observatory of Brera
      Merate, Lombardy, Italy
  • 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
    • Max Planck Institute for Extraterrestrial Physics
      Arching, Bavaria, Germany
    • Pierre and Marie Curie University - Paris 6
      • Institut d'astrophysique de Paris
      Paris, Ile-de-France, France
  • 2008–2012
    • National Institute for Fusion Science
      Tokitsu-chō, Gifu, Japan
    • Ehime University
      • Department of Physics
      Matuyama, Ehime, Japan
    • SPring-8
      Saitama, Saitama, Japan
  • 1925–2011
    • European Southern Observatory
      Arching, Bavaria, Germany
  • 1991–2010
    • Hokkaido University
      • • Laboratory of Medicinal Chemistry
      • • Graduate School of Pharmaceutical Sciences
      • • Faculty of Pharmaceutical Sciences
      Sapporo, Hokkaidō, Japan
  • 2009
    • California Institute of Technology
      • Spitzer Science Center
      Pasadena, California, United States
    • Laboratoire d’Informatique Fondamentale de Marseille
      Marsiglia, Provence-Alpes-Côte d'Azur, France
  • 1994–2009
    • Nara Medical University
      • Department of Urology
      Kashihara, Nara, Japan
  • 1993–2009
    • Tohoku University
      • • Institute of Multidisciplinary Research for Advanced Materials (IMRAM)
      • • Institute of Development, Aging and Cancer
      Sendai, Kagoshima, Japan
    • Hirosaki University
      Khirosaki, Aomori Prefecture, Japan
  • 2006–2008
    • NEC Corporation
      Edo, Tōkyō, Japan
  • 2004–2008
    • Kobe College
      Kōbe, Hyōgo, Japan
  • 2007
    • Tokyo Electron
      Edo, Tōkyō, Japan
  • 1999–2006
    • University of Occupational and Environmental Health
      • • Department of Obstetrics and Gynecology
      • • School of Medicine
      Kitakyūshū, Fukuoka, Japan
    • Yale-New Haven Hospital
      New Haven, Connecticut, United States
    • Nagoya University
      • Department of Energy Engineering and Science
      Nagoya-shi, Aichi-ken, Japan
  • 2001–2005
    • Kobe Tokiwa University
      Kōbe, Hyōgo, Japan
    • Osaka City University
      • Department of Biochemistry
      Ōsaka, Ōsaka, Japan
    • Kyushu Rosai Hospital
      Kitakyūshū, Fukuoka, Japan
  • 2002
    • Noguchi Thyroid Clinic and Hospital Foundation
      Бэппу, Ōita, Japan
  • 1993–2001
    • Tokyo Medical and Dental University
      • • Department of Pulmonary Medicine
      • • Department of Internal Medicine
      Edo, Tōkyō, Japan
  • 1992–2001
    • National Institute for Basic Biology
      Okazaki, Aichi, Japan
  • 1991–2001
    • Kanazawa University
      • • Cancer Research Institute
      • • School of Medicine
      Kanazawa-shi, Ishikawa-ken, Japan
  • 1981–2001
    • Kyoto Prefectural University of Medicine
      • • Division of Anatomy and Neurobiology
      • • Department of Anesthesiology
      • • Department of Anatomy
      • • Department of Surgery
      Kioto, Kyōto, Japan
  • 1991–2000
    • Asahi General Hospital
      Asahi, Chiba, Japan
  • 1998
    • St. Luke's International Hospital
      Edo, Tōkyō, Japan
  • 1996
    • Kyushu Kosei Nenkin Hospital
      Kitakyūshū, Fukuoka, Japan
    • Fukuoka University
      • Department of Gastroenterology
      Hukuoka, Fukuoka, Japan
  • 1989–1996
    • Tokyo Metropolitan Hiroo Hospital
      • • Division of Cardiology
      • • Department of Pathology
      Edo, Tōkyō, Japan
  • 1995
    • YAMASA Corporation
      Tiba, Chiba, Japan
    • Gunma University
      • Department of Neurology
      Maebashi, Gunma, Japan
  • 1994–1995
    • Kanazawa Medical University
      • • School of Medicine
      • • Department of Surgery II
      Kanazawa-shi, Ishikawa-ken, Japan
  • 1987–1995
    • Niigata University
      • Division of Neuropathology
      Niahi-niigata, Niigata, Japan
  • 1990–1992
    • Shinshu University
      Shonai, Nagano, Japan