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Elderly patients who undergo major abdominal surgery are potentially at a higher risk of perioperative mortality and postoperative complications. Although laparoscopic surgery has been widely accepted as a less invasive surgical procedure for colorectal diseases, the benefits for elderly patients have not been validated. To compare postoperative outcomes and long-term survival between laparoscopic and open colorectal surgery in the elderly population. A literature search was electronically performed to identify all studies comparing postoperative outcomes between laparoscopic and open colorectal resections in the elderly population. Primary outcomes were postoperative mortality and complications, and the secondary outcome was long-term survival. Overall, 30 studies (70,946 patients) met our inclusion criteria. Laparoscopic surgery was significantly associated with a decreased risk of perioperative mortality [odds ratio (OR), 0.55; 95 % confidence interval (CI), 0.45–0.68; P

It is reported that about 20% of patients with small cell lung cancer (SCLC) receive third-line chemotherapy. We conducted a retrospective study to investigate the outcome and prognostic factors of patients with SCLC who receive third-line chemotherapy.The medical records of patients with SCLC who received third-line chemotherapy at our institution were reviewed. Overall survival (OS) from the initiation of third-line chemotherapy was evaluated, and the association between OS and patient characteristics was assessed by the log-rank test.A total of 73 patients with SCLC were treated with cytotoxic drugs between 2004 and 2012, and 19 patients received third-line chemotherapy. Median OS from initiation of third-line chemotherapy was 8.5 months. Patients with higher body mass index (BMI) (P = 0.0071), lower levels of lactate dehydrogenase (LDH) (P = 0.0036), higher levels of hemoglobin (P = 0.048), longer time to progression (TTP) from the initiation of second-line treatment (P = 0.0036), and better response to second-line treatment (P = 0.029) had longer duration of OS.It is suggested that TTP and tumor response in second-line chemotherapy, serum levels of LDH and hemoglobin, and BMI at initiation of third-line chemotherapy could be possible prognostic factors.

Although incisional hernia (IH) is a common complication of abdominal surgery, the incidence rate and risk factors are not well known. The objectives of this study are to determine the incidence rate of IH following colorectal cancer surgery and to describe the associated risk factors. Between 2005 and 2010, patients who underwent surgery to treat colorectal cancer were examined. The diagnosis of IH was performed by CT scan, and the visceral fat area (VFA) and subcutaneous fat area (SFA) at the level of the umbilicus were calculated using a 3D-image analysis system. Survival analysis was used to assess the incidence and risk factors of IH. A total of 626 patients (326 open, 300 laparoscopic) were included in this study, with median follow-up of 54 (range 2–97) months. Forty patients were diagnosed with postoperative IH, and the cumulative, 5-year incidence of IH was 7.3 %. Univariate analysis revealed that age, body mass index, waist circumference, hip circumference, open laparotomy, wound infection, VFA, and SFA were significantly associated with incidence of IH. Multivariate analysis revealed that age [hazard ratio (HR) 1.043 (1.005–1.083), p = 0.027], open laparotomy [HR 4.410 (1.018–19.095), p = 0.047], and SFA [HR 1.013 (1.004–1.022), p = 0.005] were significant risk factors for developing IH. Higher age and SFA, along with open surgery, are risk factors for developing IH.

The efficacy of docetaxel, vinorelbine, or gemcitabine monotherapy in previously untreated elderly patients with non-small cell lung cancer has been reported.Pemetrexed monotherapy has shown clinically equivalent efficacy to docetaxel, a standard therapeutic option, in patients with previously treated non-small cell lung cancer and in those with a lower incidence of toxicity such as febrile neutropenia.In the present study, we aimed to investigate the efficacy and toxicity of pemetrexed in previously untreated elderly patients with non-squamous cell lung cancer and compare the results with those of docetaxel, considered a standard chemotherapeutic agent.We retrospectively reviewed the medical records of patients with non-squamous cell lung cancer with wild-type(or unknown)epidermal growth factor receptor status who received pemetrexed or docetaxel monotherapy as first-line chemotherapy.We analyzed 6 patients with lung adenocarcinoma in the pemetrexed group and 6 patients with lung adenocarcinoma in the docetaxel group. The median progression-free survival was 3.6 months for patients receiving pemetrexed and 3.1 months for those receiving docetaxel(p=0.45). The median overall survival was 14.8 months in the pemetrexed group and 10.9 months in the docetaxel group(p=0.36).Patients who received docetaxel were more likely to have grade 3 or 4 neutropenia and febrile neutropenia than those receiving pemetrexed.However, 2 patients who received pemetrexed showed grade 3 pneumonitis.Pemetrexed monotherapy is a promising treatment for previously untreated elderly patients with non-squamous cell lung cancer.

The usefulness of the Palliative Prognostic Index (PPI) has been successfully validated in a variety of clinical settings. However, while lung cancer is the leading cause of death worldwide, patients with lung cancer accounted for only 6.9-25.8 % of the study populations in these previous studies. We conducted a retrospective study to evaluate the usefulness of the PPI for survival prediction in patients with lung cancer. Patients with lung cancer who were admitted to our hospital between 2009 and 2013 to receive palliative care were enrolled. The association between the Palliative Prognostic Index, determined based on the data recorded in the clinical charts at the last admission to our hospital, and survival was evaluated. The patient group with a PPI of >6 showed a significantly shorter survival time than the patient group with a PPI of ≤ 6 (P < 0.0001, log-rank test). The sensitivity and specificity of the PPI determined using the cutoff value of 6 for predicting less than 3 weeks of survival were 61.3 and 86.8 %, respectively. However, the sensitivity decreased to 50.0 % when the assessment was carried out in only patients with small cell lung carcinoma. Our findings suggest the existence of a close association between the PPI and survival in patients with lung cancer receiving palliative care. However, the sensitivity of the index for predicting less than 3 weeks of survival was relatively low in patients with small cell lung carcinoma.

We conduct a deep narrow-band imaging survey of 13 Ly$\alpha$ blobs (LABs) located in the SSA22 proto-cluster at z~3.1 in the CIV and HeII emission lines in an effort to constrain the physical process powering the Ly$\alpha$ emission in LABs. Our observations probe down to unprecedented surface brightness limits of 2.1 $-$ 3.4 $\times$ 10$^{-18}$ erg s$^{-1}$ cm$^{-2}$ arcsec$^{-2}$ per 1 arcsec$^2$ aperture (5$\sigma$) for the HeII$\lambda$1640 and CIV$\lambda$1549 lines, respectively. We do not detect extended HeII and CIV emission in any of the LABs, placing strong upper limits on the HeII/Ly$\alpha$ and CIV/Ly$\alpha$ line ratios, of 0.11 and 0.16, for the brightest two LABs in the field. We conduct detailed photoionization modeling of the expected line ratios and find that, although our data constitute the deepest ever observations of these lines, they are still not deep enough to rule out a scenario where the Ly$\alpha$ emission is powered by the ionizing luminosity of an obscured AGN. Our models can accommodate HeII/Ly$\alpha$ and CIV/Ly$\alpha$ ratios as low as $\simeq$0.05 and $\simeq$0.07 respectively, implying that one needs to reach surface brightness as low as 1 $-$ 1.5 $\times$ 10$^{-18}$ erg s$^{-1}$ cm$^{-2}$ arcsec$^{-2}$ (at 5$\sigma$) in order to rule out a photoionization scenario. These depths will be achievable with the new generation of image-slicing integral field units such as VLT/MUSE or Keck/KCWI. We also model the expected HeII/Ly$\alpha$ and CIV/Ly$\alpha$ in a different scenario, where Ly$\alpha$ emission is powered by shocks generated in a large-scale superwind, but find that our observational constraints can only be met for shock velocities $v_{\rm s} \gtrsim$ 250 km s$^{-1}$, which appear to be in conflict with recent observations of quiescent kinematics in LABs., Comment: 24 pages, 13 figures, submitted to ApJ

Aims/Introduction: It has been reported that metabolic syndrome is associated with impaired lung function, and abdominal obesity is regarded as the most important determinant of this association. We evaluated the association between a component of metabolic syndrome, indices of body composition, including the total adipose tissue content, lean bodyweight and visceral adipose tissue content, as assessed by bioimpedance analysis, and lung function. Materials and Methods: A total of 516 participants responded to our questionnaire to determine the smoking status and history of past diseases. Waist circumference, height, bodyweight, percent forced expiratory volume in 1 s (%FEV1) and percent forced vital capacity (%FVC) were measured. Fasting blood samples were obtained to determine the serum levels of high‐density lipoprotein and triglyceride, and also the blood glucose. The body composition, including the total adipose tissue content and lean bodyweight, was measured, and the visceral adipose tissue content was estimated as the visceral adipose tissue level, by the bioimpedance analysis method. Results: Waist circumference, estimated visceral adipose tissue level and blood pressure were significantly associated with the %FEV1, and the serum high‐density lipoprotein cholesterol was significantly associated with the %FVC in men, after adjustment for age, smoking history, and past histories of bronchial asthma and ischemic heart disease. However, this association was not detected in women. Conclusions: We found an association between the visceral adipose tissue level as estimated by the bioimpedance analysis method and lung function. (J Diabetes Invest, doi: 10.1111/j.2040‐1124.2011.00189.x, 2011)

This paper focuses on under-expanded gaseous flow at a straight micro-tube exit. The pitot total pressure of gas flow (jet) in the downstream region from a straight micro-tube exit was measured by a total pressure pitot tube to accumulate data for validation of numerical results. A micro-tube of 495μm in diameter and 56.3 mm in length and a total pressure pitot tube of 100 μm in outer diameter were used. The pitot total pressure was measured at intervals of 0.1 mm in both the flow and radial directions. The measurement was done for the mass flow rates of 9.71 × 10−5 kg/s and 1.46 × 10−4 kg/s. The data were accumulated for validation of the numerical results to reveal the characteristics of the under-expanded gas flow at the exit of a micro-tube. Comparisons were conducted for numerical results of corresponding cases and a slight discrepancy can be seen between numerical and experimentally measured pitot total pressures.

We conduct a statistical analysis of a combined sample of direct imaging data, totalling nearly 250 stars. The stars cover a wide range of ages and spectral types, and include five detections ($\kappa$ And b, two $\sim$60 M$_{\rm J}$ brown dwarf companions in the Pleiades, PZ Tel B, and CD$-$35 2722B). For some analyses we add a currently unpublished set of SEEDS observations, including the detections GJ 504b and GJ 758B. We conduct a uniform, Bayesian analysis of all stellar ages using both membership in a kinematic moving group and activity/rotation age indicators. We then present a new statistical method for computing the likelihood of a substellar distribution function. By performing most of the integrals analytically, we achieve an enormous speedup over brute-force Monte Carlo. We use this method to place upper limits on the maximum semimajor axis of the distribution function derived from radial-velocity planets, finding model-dependent values of $\sim$30--100 AU. Finally, we model the entire substellar sample, from massive brown dwarfs to a theoretically motivated cutoff at $\sim$5 M$_{\rm Jup}$, with a single power law distribution. We find that $p(M, a) \propto M^{-0.65\pm0.60} a^{-0.85\pm0.39}$ (1$\sigma$ errors) provides an adequate fit to our data, with 1.0--3.1\% (68\% confidence) of stars hosting 5--70 $M_{\rm Jup}$ companions between 10 and 100 AU. This suggests that many of the directly imaged exoplanets known, including most (if not all) of the low-mass companions in our sample, formed by fragmentation in a cloud or disk, and represent the low-mass tail of the brown dwarfs., Comment: ApJ in press, replaced with accepted version. Methodology clarified, conclusions mostly unchanged

We present the results from a 1.1 mm imaging survey of the SSA22 field, known for having an overdensity of z=3.1 Lyman-alpha emitting galaxies (LAEs), taken with the AzTEC camera on the Atacama Submillimeter Telescope Experiment (ASTE). We imaged a 950 arcmin$^2$ field down to a 1 sigma sensitivity of 0.7-1.3 mJy/beam to find 125 submillimeter galaxies (SMGs) with a signal to noise ratio >= 3.5. Counterpart identification using radio and near/mid-infrared data was performed and one or more counterpart candidates were found for 59 SMGs. Photometric redshifts based on optical to near-infrared images were evaluated for 45 SMGs of these SMGs with Spitzer/IRAC data, and the median value is found to be z=2.4. By combining these estimation with estimates from the literature we determined that 10 SMGs might lie within the large-scale structure at z=3.1. The two-point angular cross-correlation function between LAEs and SMGs indicates that the positions of the SMGs are correlated with the z=3.1 protocluster. These results suggest that the SMGs were formed and evolved selectively in the high dense environment of the high redshift universe. This picture is consistent with the predictions of the standard model of hierarchical structure formation., 17 pages, 9 figures, 7 tables, Accepted for publication in MNRAS

Similar to blood oxygenation level-dependent (BOLD) functional magnetic resonance imaging (fMRI), functional nearinfrared spectroscopy (fNIRS) observes regional hemodynamic responses associated with neuronal activation. However, the conventional criteria for detecting true positive fNIRS and fMRI signals appear to be based on different understandings of cerebral hemodynamics. Considerable numbers of fNIRS studies have ascribed the increase in oxygenated hemoglobin to a typical sign of functional activation, whereas the corresponding BOLD signal in fMRI directly correlates with a decrease in deoxygenated hemoglobin. This inconsistency requires solution through the simultaneous measurements of fNIRS and fMRI. In practice, however, there remain several technical problems associated with conducting simultaneous measurements with high reproducibility. One issue is the precise spatial registration of NIRS optodes in MR images. We prepared marker containers of an annular shape that can be coaxially fixed to the optode. Liquid paraffin with α-tocopheryl acetate, which exhibits a bright contrast in T1-weighted MR images of human heads, was solidified in each container by adding higher fatty acid. A subject wearing the marker-fixed optodes at parietal area participated in preliminary fNIRS and fMRI experiments; the subject was instructed to execute single-sided hand finger tapping. The positions showed that deoxygenated hemoglobin decreases in fNIRS coincided with the BOLD-positive region in fMRI. The prepared marker is chemically stable and repetitively usable. We believe that this simple method contributes precision to the co-registration of fNIRS and fMRI.

While most commercially available functional near-infrared spectroscopy (fNIRS) systems employ optical fibers for both the measurement optode and the transmission cable for optical signals, their material inflexibility presents some problems in stable optode fixation to the head surface and adequate cable lining to the main system. In practice, mechanical fluctuations of optical fibers in fNIRS measurement often lead to motion artifacts in the signals. A few fiberless fNIRS systems are available and equipped with light sources and detectors that directly adhere to the scalp surface. However, their shapes and detection sensitivities are not suitable for usage on a hair-covered head. Based on the commercial fiber-less fNIRS system OEG-16 (Spectratech Inc., Japan), we developed a new source-detector unit that was designed with LEDs for enhanced illumination, avalanche photodiodes instead of photodiodes, and a new holder system. The electrical circuits of the system were modified after the design. By simultaneous implementation of multidistance fNIRS measurement and hemodynamic modality separation on conventional fNIRS data at the bilateral parietal area during single-sided motor tasks, significant functional signals were observed only at the position contralateral to the side of movement. This is the first report describing a fiber-less fNIRS system that can detect functional signals on a hair-covered head. We believe this fiber-less system will improve the utility of fNIRS, particularly in less restraining conditions.

We measure the angular clustering of 33 415 extremely red objects (EROs) in the Elais-N1 field covering 5.33 deg$^{2}$, which cover the redshift range $z=0.8$ to $2$. This sample was made by merging the UKIDSS Deep eXtragalactic Survey (DXS) with the optical Subaru and Pan-STARRS PS1 datasets. We confirm the existence of a clear break in the angular correlation function at $\sim 0.02^{\circ}$ corresponding to $1 h^{-1}$ Mpc at $z\sim1$. We find that redder or brighter EROs are more clustered than bluer or fainter ones. Halo Occupation Distribution (HOD) model fits imply that the average mass of dark matter haloes which host EROs is over $10^{13} h^{-1} M_{\odot}$ and that EROs have a bias ranging from 2.7 to 3.5. Compared to EROs at $z\sim1.1$, at $z\sim1.5$ EROs have a higher bias and fewer are expected to be satellite galaxies. Furthermore, EROs reside in similar dark matter haloes to those that host $10^{11.0} M_{\odot}, Comment: 17 pages, 9 figures, accepted for publication in MNRAS

We present the results of deep K � -a ndJ-band imaging of the field of a proto-cluster region near the radio galaxy 53W002 at z =2 .390 with the Subaru Telescope. The data were analyzed together with deep optical and nearinfrared (NIR) images taken with the Hubble Space Telescope to investigate the properties of ten optically compact emission-line galaxies and candidates. Excluding the three objects which may contain active galactic nuclei, many are faint or undetected at K � (λrest ≈6000 u A), and are therefore revealed to be intrinsically small starbursting objects. On the other hand, we detect few objects with colors and magnitudes expected for quiescent massive galaxies at z =2 . 4i n the f ield.

We report on a wide-area (48' x 9') imaging survey of faint galaxies in R and I bands toward the 1338+27 field where an unusual concentration of five QSOs at z\sim1.1, embedded in a larger-scale clustering of 23 QSOs, is known to exist. Using a quite homogeneous galaxy catalog with a detection completeness limit of I~23.5, we detect a significant clustering signature of faint red galaxies with I > 21 and R-I > 1.2 over a scale extending to ~20h^{-1}_{50} Mpc. Close examination of the color-magnitude diagram, the luminosity function, and the angular correlation function indeed suggests that those galaxies are located at z~1.1 and trace the underlying large-scale structure at that epoch, together with the group of 5 QSOs. Since the whole extent of the cluster of 23 QSOs (~70h^{-1}_{50} Mpc) is roughly similar to the local ``Great Wall'', the area may contain a high-redshift counterpart of superclusters in the local universe., 21 pages including 7 EPS color figures; accepted for publication for the Astrophysical Journal (2001)

A rhodium complex catalyzed the equilibrium acyl transfer reaction between acid fluorides and thioesters. In the presence of fluoride or thiolate acceptors, the reaction could be shifted to either product. RhH(PPh3)4-dppe catalyzed the reaction of acid fluorides and diorgano disulfides in the presence of triphenylphosphine giving thioesters, which was accompanied by triphenylphosphine difluoride. The same complex catalyzed the reaction of aryl thioesters and hexafluorobenzene giving acid fluorides, which was accompanied by 1,4-di(arylthio)-2,3,5,6-tetrafluorobenzenes.

We previously established a transgenic Chinese hamster CHL/IU cell line, designated as KN63, for concurrent analysis of gene mutations and chromosome aberrations. The KN63 cell line contains copies of a shuttle vector with the Escherichia coli gpt gene as a mutational target in its chromosome. To evaluate the sensitivity of the cell line to various types of mutagens, methyl methanesulfonate (MMS), N-ethyl-N-nitrosourea (ENU), mitomycin C (MMC), vincristine sulfate (VIN) and C.I. basic red 9 hydrochloride (CIB) were assayed. KN63 cells were treated with each test chemical and gene mutations were detected in the gpt gene of the shuttle vector rescued from the KN63 cell genome into an E. coli host. Chromosome aberrations were concurrently evaluated by conventional metaphase analysis. MMS, ENU and MMC induced both gene mutations and structural chromosome aberrations in KN63 cells, with more efficient induction of the latter. VIN, a well-known aneugen, produced only numerical changes to chromosomes, while CIB was negative for both types of alteration. KN63 cells were as sensitive to MMS, ENU, MMC and VIN as Chinese hamster cell lines such as CHL, CHO and V79 cells. The characteristics of test chemicals indicated by this system should be useful for understanding endpoints in chemical mutagenesis.

Results of near-infrared (NIR) observations of a type 2 QSO, AX J08494+4454, at z = 0.9, which was identified in our optical follow-up observations of the ASCA Lynx deep survey, are presented. NIR J-band spectroscopic observations show presence of a narrow (FWHM = 470 km s-1) Hα emission line and no strong broad component, which confirms that this object is type 2, as suggested in the previous optical spectroscopy (no broad Hβ emission). IC and K-band imaging observations reveal that this object has a significantly redder color (IC-K = 3.4 mag) than normal type 1 QSOs but has a similar color to those of nearby type 2 Seyfert galaxies and starburst galaxies. The absolute magnitude of this object in B band is much fainter than M for the type 1 QSO luminosity function at z ~ 0.9, but about 1.5 mag brighter than M of the luminosity function for field galaxies at z ~ 0.9. The red color and the faint optical magnitude may be a result of dust extinction, or we may be seeing the host galaxy with a hidden active nucleus.

We have investigated the optical and near-infrared colors of K'-selected galaxies in clusters at z ~ 1.2 near to the radio galaxy 3C 324 using images obtained with the Subaru telescope and archival HST data. The distribution of colors of the galaxies in the cluster region is found to be fairly broad, and it may imply significant scatter in their star-formation histories, although the effect of contamination of field galaxies is uncertain. The red sequence of galaxies whose R-K colors are consistent with passive evolution models for old galaxies is found to be truncated at K' ~ 20 mag, and there are few fainter galaxies with similar red colors in the cluster region. We find that the bulge-dominated galaxies selected by quantitative morphological classification form a broad sequence in the color-magnitude diagram, whose slope is much steeper than that expected from metallicity variations within a passively evolving coeval galaxy population. We argue that the observed color-magnitude sequence can be explained by metallicity and age variations, and the fainter galaxies with K' > 20 mag may be 1-2 Gyr younger than the brighter galaxies. Some spatial segregation of the color and K'-band luminosity is seen in the sky distribution; the redder and the brighter objects tend to be located near 3C 324., 16 pages, 10 figures, accepted for publication in PASJ

We present results of ASCA deep exposure observations and optical identifications of the hardest X-ray source discovered in the ASCA Large Sky Survey project, designated as AX J131501+3141. AX J131501+3141 exhibits a large X-ray absorption of N H = (6 −2 +4 ) × 10 26 H m −2 . The observed X-ray flux was time variable by a factor of 30% in 0.5 year: F X (2–10keV) = (4.8−6.2)×10 −16 J m −2 s −1 . From optical photometric and spectroscopic observations, we found one galaxy with R = 15.6mag in the X-ray error circle, whose emission line ratios are similar to those found in type 2 Seyfert galaxies. Its redshift is determined to be 0.07, hence the absorption-corrected X-ray luminosity is L X ∼ 2 × 10 36 J s −1 (2–10 keV). Accordingly, we conclude that AX J131501+3141 is a type 2 Seyfert galaxy. Discovery of such a low flux and highly absorbed X-ray source could have a significant impact on the origin of the cosmic X-ray background.

We previously reported a significant clustering of red galaxies (R-K=3.5--6) around the radio-loud quasar B2 1335+28 at z=1.086. In this paper, we establish the existence of a rich cluster at the quasar redshift, and study the properties of the cluster galaxies through further detailed analysis of the photometric data. The color distribution of the galaxies in the cluster is quite broad and the fraction of blue galaxies (\sim 70%) is much larger than in intermediate-redshift clusters. Using evolutionary synthesis models, we show that this color distribution can be explained by galaxies with various amounts of star-formation activity mixed with the old stellar populations. Notably, there are about a dozen galaxies which show very red optical-NIR colors but also show significant UV excess with respect to passive-evolution models. They can be interpreted as old early-type galaxies with a small amount of star formation. The fact that the UV-excess red galaxies are more abundant than the quiescent red ones suggests that a large fraction of old galaxies in this cluster are still forming stars to some extent. However, a sequence of quiescent red galaxies is clearly identified on the R-K versus K color-magnitude (C-M) diagram. The slope and zero point of their C-M relation appear to be consistent with those expected for the precursors of the C-M relation of present-day cluster ellipticals when observed at z=1.1. We estimate the Abell richness class of the cluster to be R \sim 1. New X-ray data presented here place an upper limit of L_x < 2 10^{44} erg s^{-1} for the cluster luminosity. Inspections of the wider optical images reveal some lumpy structure, suggesting that the whole system is still dynamically young.

Lyα Blobs (LAB), large, extended Lyα emitters, are enigmatic objects that calls on much attention in the field of galaxy formation and evolution. So far, discovery of more than twenty giant (>60 kpc) LABs have been reported and new searches are on-going. Many of the groups who study LABs attended the workshop in Heidelberg, “Understanding Lyα Emitters”, 2008 October 6–10. We had useful discussions on the various important aspects of LABs including the search or detection methods, origins of the extended Lyα emission, and their physical properties.

We investigate expected sub-mm emission and dust properties of the Lyman Break Galaxies (LBGs) in the Hubble Deep Field (HDF). The SCUBA Deep Survey (Hughes et al., 1998) provides an upper limit of the 850 micron flux densities of the LBGs. With this constraint, we argue that a typical ultra-violet to far-infrared spectral shape of the high-redshift LBGs is rather close to a template spectrum of low-reddening starburst galaxies in the local universe but different from that of heavily dust-enshrouded ultra-luminous far-infrared galaxies like Arp220. We also evaluate the lower-limit temperature of dust in LBGs assuming single- and two-component modified black-body spectrum. To estimate the total amount of energy re-emitted in FIR wavelength, we take two different approaches; model fitting of the UV spectra of LBGs and an empirical method using the relationship between UV spectral shape and UV/FIR flux ratio observed for local starburst galaxies. Both methods give lower-limit temperature of the LBGs as around 40 K, which is higher than the typical dust temperature of local optical- and infrared-selected galaxies. This result is also supported by the comparison of the expected sub-mm flux of the LBGs with the cosmic FIR background radiation. The high dust temperature may indicate the effective massive-star formation or different dust properties in the high-redshift LBGs., 11 pages, 4 figures; The Astrophysical Journal (Letters), in press

We present results of ASCA deep exposure observations of the hardest X-ray source discovered in the ASCA Large Sky Survey (LSS) project, designated as AX J131501+3141. We extract its accurate X-ray spectrum, taking account of the contamination from a nearby soft source (AX J131502+3142), separated only by 1'. AX J131501+3141 exhibits a large absorption of NH = (6 +4 -2)x 10^22 H/cm^2 with a photon index \Gamma = 1.5 +0.7 -0.6. The 2--10 keV flux was about 5 x 10^-13 erg/s/cm^2 and was time variable by a factor of 30% in 0.5 year. From the highly absorbed X-ray spectrum and the time variability, as well as the results of the optical follow-up observations (Akiyama et al. 1998, astro-ph/9801173), we conclude that AX J131501+3141 is a type 2 Seyfert galaxy. Discovery of such a low flux and highly absorbed X-ray source could have a significant impact on the origin of the cosmic X-ray background., Comment: 16 pages, 6 figures, requires AAS Latex macro v4.0, to appear in The Astrophysical Journal, text and figures also available at http://www-cr.scphys.kyoto-u.ac.jp/member/sakano/work/paper/index-e.html

We present 12 CO(J=1–0) observations of the poststarburst nucleus of NGC 4736. Although star in the nuclear region is currently inactive, there is a substantial amount of molecular gas, ∼ 10 7 M⊙, in the central ∼ 300 pc region. Comparing the observed molecular-gas surface density with the threshold gas density for star formation proposed by Kennicutt (1989, AAA 50.157.264), we find that the nuclear gas disk is stable for gravitational instability. We discuss possible scenarios for the nuclear starburst evolution of NGC 4736 in terms of either bar-driven instability fueling or minor-merger driven fueling (or triggering).

A 12CO (J = 2-1) observation of the quasar BR 1202—0725 at z = 4.7, in which a huge amount of molecular gas had been detected in the 12CO (J = 5-4) emission line, was made with the Nobeyama 45-m radio telescope. An upper limit of 1.2 mK in TMB (~ 2.8 mjy) was obtained at a velocity resolution of 25 km s -1 . The physical conditions of the molecular gas were examined using the CO emission-line ratios with the LVG model; the line ratios imply that the molecular gas is dense [n(H2) ~ IO 3 - 5-5 -5 cm -3 ] with a high kinetic temperature (50-100 K). The value of the CO-to-H2 conversion factor in this system is discussed and the molecular-gas mass is estimated to be less than 5.4 x 10 11 M®. Using these values, we tried to sketch the distribution of molecular gas in this system and find the possibility that the system consists of many small dense clouds.

A study of enteroaggregative Escherichia coli (EAggEC) which was recently reported as a causative agent of diarrhea was attempted, by isolating these organisms from the fecal samples collected from sporadic diarrhea patients in Miyazaki Prefecture during the period from January 1993 to April 1998, and by investigating several characteristics of the isolates. By using the PCR method targetting aggR gene which was a transcriptional activator of aggregative adherence fimbria I expression, thirty four strains of aggR(+)-Escherichia coli (E. coli) were detected from 2,652 fecal samples. Twenty nine of these 34 isolates were confirmed as EAggEC by demonstration of aggregative adherence to HEp-2 cells, and the other 5 isolates were not EAggEC because they showed negative adherence to HEp-2 cells. The above mentioned, aggR-PCR method revealed that there were a few non-EAggEC strains with aggR gene. It has been reported that aggregative adherence fimbriae are encoded by the plasmid of about 60 Md. All of the 29 EAggEC isolates possessed plasmids of about 50 Md or more, and these plasmids were suggested to relate to aggregative adherence fimbriae. Sixteen (55%) of the 29 isolates were classified serologically into two serotypes, O111:H21 and O126:H27, and the other 13 isolates were classified into ten groups or more which included a few strains in a group. EAggEC heat-stable enterotoxin 1 (EAST1) gene was demonstrated in nineteen of 29 isolates. In drug susceptibility test, 72%, 59% and 21% of the 29 isolates showed resistance to Ampicillin, Cefazolin, and Streptomycin, respectively.

Objective: To determine the risk for tuberculosis infection in patients with rheumatoid arthritis before the anti-cytokine era in Japan. Patients and methods: A database of a single-institute-based large observational cohort study for rheumatoid arthritis at the Institute of Rheumatology, Tokyo Women’s Medical University, Tokyo, Japan, was analysed. Information on the history of tuberculosis infection was collected by patient self-reporting during April and October 2003. The age-adjusted incidence rate and relative risk for tuberculosis infection were investigated. Results: Among 5044 patients with rheumatoid arthritis, 483 (9.6%) patients claimed to have a history of tuberculosis infection before October 2002. The frequency of history of tuberculosis increased according to the age of the patient. Four cases of new-onset tuberculosis were identified among 5544 patients with rheumatoid arthritis during 1 year. The age-adjusted incidence of tuberculosis was 42.4/100 000 patients. The relative risk for tuberculosis was 3.21 (95% confidence interval (CI) 1.21 to 8.55), and that of men and women was 10.59 (95% CI 3.42 to 32.78) and 1.41 (95% CI 0.2 to 10), respectively. Conclusion: There was an increased risk of tuberculosis infection in Japanese patients with rheumatoid arthritis, especially in male patients before the introduction of anti-tumour necrosis factor treatment. These data should form the basis for the risk management of anti-cytokine treatment in Japan.

The γ-ray burst GRB 050904, detected by the Swift satellite on 4 September last year, is one of the most distant objects ever observed. Its redshift of z = 6.3 equates to an explosion taking place 12.8 billion years ago, when the Universe was a mere 890 million years old. Three groups this week present detailed observations of the γ-ray, X-ray, near-infrared and optical spectra of the afterglow of GRB 050904. The results begin to paint a picture of the conditions prevailing when the parent body exploded and suggest that the γ-ray bursts that we see in the future can be used by cosmologists to probe the early Universe for evidence of star and galaxy formation, nucleosynthesis and reionization. The prompt γ-ray emission from γ-ray bursts (GRBs) should be detectable out to distances of z > 10 (ref. 1), and should therefore provide an excellent probe of the evolution of cosmic star formation, reionization of the intergalactic medium, and the metal enrichment history of the Universe1,2,3,4. Hitherto, the highest measured redshift for a GRB has been z = 4.50 (ref. 5). Here we report the optical spectrum of the afterglow of GRB 050904 obtained 3.4 days after the burst; the spectrum shows a clear continuum at the long-wavelength end of the spectrum with a sharp cut-off at around 9,000 A due to Lyman α absorption at z ≈ 6.3 (with a damping wing). A system of absorption lines of heavy elements at z = 6.295 ± 0.002 was also detected, yielding the precise measurement of the redshift. The Si ii fine-structure lines suggest a dense, metal-enriched environment around the progenitor of the GRB.

We compared the number of faint stars detected in deep survey fields with the current stellar distribution model of the Galaxy and found that the detected number in the H band is significantly smaller than the predicted number. This indicates that M-dwarfs, the major component, are fewer in the halo and the thick disk. We used archived data of several surveys in both the north and south field of GOODS (Great Observatories Origins Deep Survey), MODS in GOODS-N, and ERS and CANDELS in GOODS-S. The number density of M-dwarfs in the halo has to be 20+/-13% relative to that in the solar vicinity, in order for the detected number of stars fainter than 20.5 mag in the H band to match with the predicted value from the model. In the thick disk, the number density of M-dwarfs must be reduced (52+/-13%) or the scale height must be decreased (~600 pc). Alternatively, overall fractions of the halo and thick disks can be significantly reduced to achieve the same effect, because our sample mainly consists of faint M-dwarfs. Our results imply that the M-dwarf population in regions distant from the Galactic plane is significantly smaller than previously thought. We then discussed the implications this has on the suitability of the model predictions for the prediction of non-companion faint stars in direct imaging extrasolar planet surveys by using the best-fit number densities., Comment: 22 pages, 9 figures, accepted for Publications of the Astronomical Society of Japan

We present a new method of analysis for determining the surface geometry of five protoplanetary disks observed with near-infrared imaging polarimetry using Subaru-HiCIAO. Using as inputs the observed distribution of polarized intensity (PI), disk inclination, assumed properties for dust scattering, and other reasonable approximations, we calculate a differential equation to derive the surface geometry. This equation is numerically integrated along the distance from the star at a given position angle. We show that, using these approximations, the local maxima in the PI distribution of spiral arms (SAO 206462, MWC 758) and rings (2MASS J16042165-2130284, PDS 70) are associated with local concave-up structures on the disk surface. We also show that the observed presence of an inner gap in scattered light still allows the possibility of a disk surface that is parallel to the light path from the star, or a disk that is shadowed by structures in the inner radii. Our analysis for rings does not show the presence of a vertical inner wall as often assumed in studies of disks with an inner gap. Finally, we summarize the implications of spiral and ring structures as potential signatures of ongoing planet formation., Comment: 35 pages, 13 figures, 7 tables, accepted by ApJ

This is the third and final paper of our systematic visual search for IRAS galaxies behind the Milky Way at |b| ≤ 15°. This paper presents a catalog of 950 IRAS galaxies with 60 μm flux densities larger than 0.6 Jy located between l = 0° and 150°, of which 293 are newly identified by this search. We made a redshift survey for the identified galaxies and obtained new redshift data of 171 galaxies. We also present newly measured redshifts of 27 IRAS galaxies between l = 150° and 225° at |b| ≤ 15°. In this paper we studied the structure of the Local void using IRAS galaxies and galaxies from the Third Reference Catalogue of Bright Galaxies in the region l = 30°-120° and b = -50° to +30°. The center of the Local void turned out to be located at l ~ 60°, b ~ -15°, and cz ~ 2500 km s-1, and the size is about 2500 km s-1 along the direction toward the center.

We have obtained new deep optical and near-infrared images of the field of the radio-loud quasar 1335.8+2834 at z = 1.086, where an excess in the surface number density of galaxies was reported by Hutchings et al. from optical data. We found a significant clustering of objects with very red optical-near-infrared colors, 4 R - K 6 and 3 I - K 5, near the quasar. The colors and magnitudes of the reddest objects are consistent with those of old (12 Gyr old at z = 0) passively evolving elliptical galaxies seen at z = 1.1, clearly defining a "red envelope" like that found in galaxy clusters at similar or lower redshifts. This evidence strongly suggests that the quasar resides in a moderately rich cluster of galaxies (richness class ≥0). There is also a relatively large fraction of objects with moderately red colors (3.5 < R - K < 4.5) that have a distribution on the sky similar to that of the reddest objects. They may be interpreted as cluster galaxies with some recent or ongoing star formation.

We observed the natural circular dichroism NCD of amino acid films in the soft X-ray region for the first time [M. Tanaka, K. Nakagawa, A. Agui, K. Fujii, A. Yokoya, Physica Scripta, in press]. Based on the success, a new generation of detection system is now under preparation. Vacuum ultraviolet NCD of amino acid films was measured successfully using a polarizing undulator [H. Onuki, Nucl. Instrum. Meth. A 246 (1986) 94] installed at the TERAS electron storage ring at AIST, Tsukuba, Japan. A result of NCD measurement for alanine films is described in detail.

The Mach number and pressure on the outlet plane of a straight micro-tube were investigated numerically for both laminar and turbulent flow cases. The numerical methodology is based on the Arbitrary-Lagrangian-Eulerian (ALE) method. The LB1 turbulence model was used for the turbulent flow case. The compressible momentum and energy equations with the assumption of the ideal gas were solved. The computational domain is extended to the downstream region from the micro-tube outlet. The back pressure was given to the outside of the downstream region. The computations were performed for a tube whose diameter ranges from 50 to 500 μm. The average Mach number on the outlet plane of the fully under-expanded flow depends on the tube diameter and ranges from 1.16 to 1.25. The flow characteristics of the under-expanded gas flow in a straight micro-tube were revealed.

The heat conduction in a two-dimensional square plate at nano/micro scales is investigated using numerical and semi-analytical methodologies which are energy conserving dissipative particle dynamics (DPDe) and Boltzmann transport equation (BTE) with the gray relaxation time approximation. The solution domain was considered to be a two-dimensional square plate surrounded by walls having constant temperatures. The numerical and semi-analytical results for different Knudsen numbers ranging from 0.1 to 10 are presented in form of temperature distributions in the solution domain. These results are compared with each other and the applicability of the DPDe model to two-dimensional structures is discussed.

Diffusive-ballistic heat transport in a two-dimensional square plate was simulated using energy conserving dissipative particle dynamics (DPDe). The solution domain was considered to be a two-dimensional square plate surrounded by walls at constant temperatures, where DPD particles are uniformly distributed. The effects of phonon mean free path was incorporated by its relation to the cutoff radius of energy interaction. This cutoff radius was obtained based on Knudsen number (Kn) using the existing phonon-boundary scattering models. The simulations for 0.1 < Kn < 10 were conducted with different modifications of the cutoff radius. The results are presented in form of temperature distributions in the solution domain and the effect of Knudsen number is discussed.

Hemodynamic modality separation (HMS) is a method for separating the functional near infrared spectroscopy (fNIRS) signal into the cerebral functional and systemic physiological components based on their difference in hemodynamic modalities: 1) Changes in oxyhemoglobin and deoxyhemoglobin (ΔHbO and ΔHbR) in the cerebral capillaries during neural activation negatively correlate with each other; 2) Other physiological hemodynamic changes originating from major vessels cause a positive correlation in ΔHbO and ΔHbR. We applied this simple method to a high-density multichannel (HDM) fNIRS measurement. In the case of functional signal detection in the parietal area of human adults during a single-sided finger-tapping task, conventional fNIRS data showed very unclear signal laterality, while the functional components separated by the HMS method highly localized at the contralateral area of the tapping side. Using the HMS method for HDM NIRS, we successfully explored cerebral activation in the parietal area. This is the first report that HMS method was utilized for the exploratory detection of cerebral activity.

The liquid flow in sub-micron channels is simulated using multi-body dissipative particle dynamics (MDPD) to study the effect of the surface tension between liquid and wall surface on the flow in sub-micon scale. The solution domain is considered to be two-dimensional, where DPD particles are randomly distributed. Periodic boundary condition is employed in the flow direction and the solid walls are created by distributing DPD particles in the additional layers on the top and bottom of the domain. The different surface tensions between liquid and wall surface are obtained by changing the interaction parameters between the liquid and wall DPD particles. The ratio of Capillary number (Ca) to Reynolds number (Re) is used to relate the DPD units to the physical units. The results are shown in the form of slip length and the effect of the surface tension on the liquid flow in sub-micron channels is discussed.

This paper focuses on under-expanded gas flow at a straight mini-tube exit. Pitot total pressure of gas flow (jet) in downstream region from a straight mini-tube exit was measured to give data for validation of numerical results. A mini-tube of 495μm in diameter & 56.3 mm in length and a pitot tube of 100 μm in outer diameter were used. The pitot total pressure was measured every 0.1 mm interval in the flow and radial directions. The measurement was done for the mass flow rates of 9.71×10−5 kg/s and 1.46×10−4 kg/s. The data were accumulated for validation of the numerical result to reveal the characteristics of the under-expanded gas flow at the exit of a mini-tube. Comparisons were conducted for sample computations and a slight discrepancy can be seen between numerical and experimentally measured pitot total pressures.Copyright © 2013 by ASME

We have carried out a redshift survey of an IRAS flux-limited (f60 > 0.6) galaxy sample behind the southern Milky Way, 210° < l < 360° at |b| < 15°. The survey includes redshifts for 951 galaxies, ~500 -of which are new. Of these 951 galaxies, 462 are in the zone 5° < b < 15 ° and 353 are in the zone −15° < b < −5°. Though the innermost region of the Milky Way (|b| = 5°) remains opaque except in the longitude near 240°, the deected galaxies show a high degree of completeness (~70%) in the zones 5° < b < −5° and −15° < b < −5°. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210° < l < 360°, |b| < 15° shows two clusters in the Puppis region (l = 240°, b = −7°, v = 2400 km−1; l = 245° b = −5°, v = 7500 km s−1), the A3627 cluster (l = 325°, b =−7°; v = 4500 km s−1), the S4 cluster (l= =280°, b = 7°; v = 5500 km s−1), and a possible void at l = 245°, v = 3000 km s−1. The region 270° < l < 350° is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus Complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes A velocity histogram of galaxies in the GA region 290° < l < 350°, |b| < 15° reveals a substantial overdensity of galaxies in the velocity range 2400–5000 km s−1. The centroid of this overdensity is located at 4000 km s−1. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500 km s−1 in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30° to -10° and +10° to +45°). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l = 302°, b = +22°) in the north to the major concentration of the Pavo-Indus Supercluster (l = 332°, b = −24°) in the south, through the Miky Way. We conclude that peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.

A polarizing undulator with crossed and retarded magnetic fields is capable of high frequency polarization modulation. We observed the circular dichroism spectra of d-10-camphorsulfonic acid in water by using a fifteen period polarizing undulator which had been installed in the electron storage ring NIJI-II in the Electrotechnical Laboratory as the polarization modulating radiation source.

An Onuki-type polarizing undulator with fifteen-periods was installed in the electron storage ring NIJI-II in the Electrotechnical Laboratory. The polarization characteristics of the radiation from the undulator were studied in the UV region. It was confirmed that the degree of circular polarization was above 95 %.