Search

Your search keyword '"Yabe K"' showing total 410 results
Start Over Author "Yabe K"
410 results on '"Yabe K"'

1. The Hyper Suprime-Cam SSP Survey: Overview and Survey Design

Author

Aihara, H., Arimoto, N., Armstrong, R., Arnouts, S., Bahcall, N. A., Bickerton, S., Bosch, J., Bundy, K., Capak, P. L., Chan, J. H. H., Chiba, M., Coupon, J., Egami, E., Enoki, M., Finet, F., Fujimori, H., Fujimoto, S., Furusawa, H., Furusawa, J., Goto, T., Goulding, A., Greco, J. P., Greene, J. E., Gunn, J. E., Hamana, T., Harikane, Y., Hashimoto, Y., Hattori, T., Hayashi, M., Hayashi, Y., Hełminiak, K. G., Higuchi, R., Hikage, C., Ho, P. T. P., Hsieh, B. -C., Huang, K., Huang, S., Ikeda, H., Imanishi, M., Inoue, A. K., Iwasawa, K., Iwata, I., Jaelani, A. T., Jian, H. -Y., Kamata, Y., Karoji, H., Kashikawa, N., Katayama, N., Kawanomoto, S., Kayo, I., Koda, J., Koike, M., Kojima, T., Komiyama, Y., Konno, A., Koshida, S., Koyama, Y., Kusakabe, H., Leauthaud, A., Lee, C. -H., Lin, L., Lin, Y. -T., Lupton, R. H., Mandelbaum, R., Matsuoka, Y., Medezinski, E., Mineo, S., Miyama, S., Miyatake, H., Miyazaki, S., Momose, R., More, A., More, S., Moritani, Y., Moriya, T. J., Morokuma, T., Mukae, S., Murata, R., Murayama, H., Nagao, T., Nakata, F., Niida, M., Niikura, H., Nishizawa, A. J., Obuchi, Y., Oguri, M., Oishi, Y., Okabe, N., Okura, Y., Ono, Y., Onodera, M., Onoue, M., Osato, K., Ouchi, M., Price, P. A., Pyo, T. -S., Sako, M., Okamoto, S., Sawicki, M., Shibuya, T., Shimasaku, K., Shimono, A., Shirasaki, M., Silverman, J. D., Simet, M., Speagle, J., Spergel, D. N., Strauss, M. A., Sugahara, Y., Sugiyama, N., Suto, Y., Suyu, S. H., Suzuki, N., Tait, P. J., Takata, T., Takada, M., Tamura, N., Tanaka, M. M., Tanaka, M., Tanaka, Y., Terai, T., Terashima, Y., Toba, Y., Toshikawa, J., Turner, E. L., Uchida, T., Uchiyama, H., Umetsu, K., Uraguchi, F., Urata, Y., Usuda, T., Utsumi, Y., Wang, S. -Y., Wang, W. -H., Wong, K. C., Yabe, K., Yamada, Y., Yamanoi, H., Yasuda, N., Yeh, S., Yonehara, A., and Yuma, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Hyper Suprime-Cam (HSC) is a wide-field imaging camera on the prime focus of the 8.2m Subaru telescope on the summit of Maunakea in Hawaii. A team of scientists from Japan, Taiwan and Princeton University is using HSC to carry out a 300-night multi-band imaging survey of the high-latitude sky. The survey includes three layers: the Wide layer will cover 1400 deg$^2$ in five broad bands ($grizy$), with a $5\,\sigma$ point-source depth of $r \approx 26$. The Deep layer covers a total of 26~deg$^2$ in four fields, going roughly a magnitude fainter, while the UltraDeep layer goes almost a magnitude fainter still in two pointings of HSC (a total of 3.5 deg$^2$). Here we describe the instrument, the science goals of the survey, and the survey strategy and data processing. This paper serves as an introduction to a special issue of the Publications of the Astronomical Society of Japan, which includes a large number of technical and scientific papers describing results from the early phases of this survey., Comment: 14 pages, 7 figures, 5 tables. Corrected for a typo in the coordinates of HSC-Wide spring equatorial field in Table 5

Published
2017
Full Text
View/download PDF

2. SXDF-UDS-CANDELS-ALMA 1.5 arcmin$^2$ deep survey

Author

Kohno, K., Yamaguchi, Y., Tamura, Y., Tadaki, K., Hatsukade, B., Ikarashi, S., Caputi, K. I., Rujopakarn, W., Ivison, R. J., Dunlop, J. S., Motohara, K., Umehata, H., Yabe, K., Wang, W. -H., Kodama, T., Koyama, Y., Hayashi, M., Matsuda, Y., Hughes, D., Aretxaga, I., Wilson, G. W., Yun, M. S., Ohta, K., Akiyama, M., Kawabe, R., Iono, D., Nakanishi, K., Lee, M., and Makiya, R.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have conducted 1.1 mm ALMA observations of a contiguous $105'' \times 50''$ or 1.5 arcmin$^2$ window in the SXDF-UDS-CANDELS. We achieved a 5$\sigma$ sensitivity of 0.28 mJy, providing a flat sensus of dusty star-forming galaxies with $L_{\rm IR} \sim6\times10^{11}$ $L_\odot$ (for $T_{\rm dust}$ =40K) up to $z\sim10$ thanks to the negative K-correction at this wavelength. We detected 5 brightest sources (S/N$>$6) and 18 low-significance sources (5$>$S/N$>$4; these may contain spurious detections, though). One of the 5 brightest ALMA sources ($S_{\rm 1.1mm} = 0.84 \pm 0.09$ mJy) is extremely faint in the WFC3 and VLT/HAWK-I images, demonstrating that a contiguous ALMA imaging survey is able to uncover a faint dust-obscured population that is invisible in deep optical/near-infrared surveys. We found a possible [CII]-line emitter at $z=5.955$ or a low-$z$ CO emitting galaxy within the field, which may allow us to constrain the [CII] and/or the CO luminosity functions across the history of the universe., Comment: 4 pages, 2 figures, 1 table, to appear in the proceedings of IAU Symposium 319 "Galaxies at High Redshift and Their Evolution over Cosmic Time", eds. S. Kaviraj & H. Ferguson

Published
2016
Full Text
View/download PDF

4. Black hole mass and Eddington ratio distribution functions of X-ray selected broad-line AGNs at z~1.4 in the Subaru XMM-Newton Deep Field

Author

Nobuta, K., Akiyama, M., Ueda, Y., Watson, M. G., Silverman, J., Hiroi, K., Ohta, K., Iwamuro, F., Yabe, K., Tamura, N., Moritani, Y., Sumiyoshi, M., Kimura, M., Maihara, T., Dalton, G., Lewis, I., Bonfield, D., Lee, H., Lake, E. Curtis, Macaulay, E., Clarke, F., Sekiguchi, K., Simpson, C., Croom, S., Ouchi, M., Hanami, H., and Yamada, T.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

In order to investigate the growth of super-massive black holes (SMBHs), we construct the black hole mass function (BHMF) and Eddington ratio distribution function (ERDF) of X-ray-selected broad-line AGNs at z~1.4 in the Subaru XMM-Newton Deep Survey field. In this redshift range, a significant part of the accretion growth of SMBHs is thought to be taking place. Black hole masses of X-ray-selected broad-line AGNs are estimated using the width of the broad MgII line and the 3000A monochromatic luminosity. We supplement the MgII FWHM values with the Ha FWHM obtained from our NIR spectroscopic survey. Using the black hole masses of broad-line AGNs at redshifts between 1.18 and 1.68, the binned broad-line AGN BHMF and ERDF are calculated using the Vmax method. To properly account for selection effects that impact the binned estimates, we derive the corrected broad-line AGN BHMF and ERDF by applying the Maximum Likelihood method, assuming that the ERDF is constant regardless of the black hole mass. We do not correct for the non-negligible uncertainties in virial BH mass estimates. If we compare the corrected broad-line AGN BHMF with that in the local Universe, the corrected BHMF at z~1.4 has a higher number density above 10^8 Msolar but a lower number density below that mass range. The evolution may be indicative of a down-sizing trend of accretion activity among the SMBH population. The evolution of broad-line AGN ERDF from z=1.4 to 0 indicates that the fraction of broad-line AGNs with accretion rate close to the Eddington-limit is higher at higher redshifts., Comment: 23 pages with 18 figures. Accepted for publication in ApJ

Published
2012
Full Text
View/download PDF

5. FMOS near-IR spectroscopy of Herschel selected galaxies: star formation rates, metallicity and dust attenuation at z~1

Author

Roseboom, I. G., Bunker, A., Sumiyoshi, M., Wang, L., Dalton, G., Akiyama, M., Bock, J., Bonfield, D., Buat, V., Casey, C., Chapin, E., Clements, D. L., Conley, A., Curtis-Lake, E., Cooray, A., Dunlop, J. S., Farrah, D., Ham, S. J., Ibar, E., Iwamuro, F., Kimura, M., Lewis, I., Macaulay, E., Magdis, G., Maihara, T., Marsden, G., Mauch, T., Moritani, Y., Ohta, K., Oliver, S. J., Page, M. J., Schulz, B., Scott, Douglas, Symeonidis, M., Takato, N., Tamura, N., Totani, T., Yabe, K., and Zemcov, M.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the properties (e.g. star formation rate, dust attentuation, stellar mass and metallicity) of a sample of infrared luminous galaxies at z \sim 1 via near-IR spectroscopy with Subaru-FMOS. Our sample consists of Herschel SPIRE and Spitzer MIPS selected sources in the COSMOS field with photometric redshifts in the range 0.7 < z-phot < 1.8, which have been targeted in 2 pointings (0.5 sq. deg.) with FMOS. We find a modest success rate for emission line detections, with candidate H{\alpha} emission lines detected for 57 of 168 SPIRE sources (34 per cent). By stacking the near-IR spectra we directly measure the mean Balmer decrement for the H{\alpha} and H{\beta} lines, finding a value of = 0.51\pm0.27 for = 10^12 Lsol sources at = 1.36. By comparing star formation rates estimated from the IR and from the dust uncorrected H{\alpha} line we find a strong relationship between dust attenuation and star formation rate. This relation is broadly consistent with that previously seen in star-forming galaxies at z ~ 0.1. Finally, we investigate the metallicity via the N2 ratio, finding that z ~ 1 IR-selected sources are indistinguishable from the local mass-metallicity relation. We also find a strong correlation between dust attentuation and metallicity, with the most metal-rich IR-sources experiencing the largest levels of dust attenuation., Comment: 13 pages, 7 figures, MNRAS accepted

Published
2012
Full Text
View/download PDF

6. Initial Results from the Nobeyama Molecular Gas Observations of Distant Bright Galaxies

Author

Iono, D., Hatsukade, B., Kohno, K., Kawabe, R., Ikarashi, S., Ichikawa, K., Kodama, T., Motohara, K., Nakajima, T., Nakanishi, K., Ohta, K., Ota, K., Saito, T., Suzuki, K., Tadaki, K., Tamura, Y., Ueda, J., Umehata, H., Yabe, K., Yoshida, T., Yuma, S., Kuno, N., Takano, S., Iwashita, H., Handa, K., Higuchi, A., Hirota, A., Ishikawa, S., Kimura, K., Maekawa, J., Mikoshiba, H., Miyazawa, C., Miyazawa, K., Muraoka, K., Ogawa, H., Onodera, S., Saito, Y., Sakai, T., Takahashi, S., and Yun, M. S.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present initial results from the CO survey toward high redshift galaxies using the Nobeyama 45m telescope. Using the new wide bandwidth spectrometer equipped with a two-beam SIS receiver, we have robust new detections of three high redshift (z=1.6-3.4) submillimeter galaxies (SXDF 1100.001, SDP9, and SDP17), one tentative detection (SDSS J160705+533558), and one non-detection (COSMOS-AzTEC1). The galaxies observed during the commissioning phase are sources with known spectroscopic redshifts from previous optical or from wide-band submm spectroscopy. The derived molecular gas mass and line widths from Gaussian fits are ~10^11 Msun and 430-530 km/s, which are consistent with previous CO observations of distant submm galaxies and quasars. The spectrometer that allows a maximum of 32 GHz instantaneous bandwidth will provide new science capabilities at the Nobeyama 45m telescope, allowing us to determine redshifts of bright submm selected galaxies without any prior redshift information., Comment: 4 pages, 1 figure, PASJ Letter Accepted

Published
2012
Full Text
View/download PDF

7. FIBRE-pac: FMOS image-based reduction package

Author

Iwamuro, F., Moritani, Y., Yabe, K., Sumiyoshi, M., Kawate, K., Tamura, N., Akiyama, M., Kimura, M., Takato, N., Tait, P., Ohta, K., Totani, T., Suzuki, Y., and Tonegawa, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The FIBRE-pac (FMOS image-based reduction package) is an IRAF-based reduction tool for the fiber multiple-object spectrograph (FMOS) of the Subaru telescope. To reduce FMOS images, a number of special techniques are necessary because each image contains about 200 separate spectra with airglow emission lines variable in spatial and time domains, and with complicated throughput patterns for the airglow masks. In spite of these features, almost all of the reduction processes except for a few steps are carried out automatically by scripts in text format making it easy to check the commands step by step. Wavelength- and flux-calibrated images together with their noise maps are obtained using this reduction package., Comment: Accepted for publication in PASJ. 9 pages, 14 figures

Published
2011
Full Text
View/download PDF

8. 'Dark' GRB 080325 in a Dusty Massive Galaxy at z ~ 2

Author

Hashimoto, T., Ohta, K., Aoki, K., Tanaka, I., Yabe, K., Kawai, N., Aoki, W., Furusawa, H., Hattori, T., Iye, M., Kawabata, K. S., Kobayashi, N., Komiyama, Y., Kosugi, G., Minowa, Y., Mizumoto, Y., Niino, Y., Nomoto, K., Noumaru, J., Ogasawara, R., Pyo, T. -S., Sakamoto, T., Sekiguchi, K., Shirasaki, Y., Suzuki, M., Tajitsu, A., Takata, T., Tamagawa, T., Terada, H., Totani, T., Watanabe, J., Yamada, T., and Yoshida, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present optical and near infrared observations of GRB 080325 classified as a "Dark GRB". Near-infrared observations with Subaru/MOIRCS provided a clear detection of afterglow in Ks band, although no optical counterpart was reported. The flux ratio of rest-wavelength optical to X-ray bands of the afterglow indicates that the dust extinction along the line of sight to the afterglow is Av = 2.7 - 10 mag. This large extinction is probably the major reason for optical faintness of GRB 080325. The J - Ks color of the host galaxy, (J - Ks = 1.3 in AB magnitude), is significantly redder than those for typical GRB hosts previously identified. In addition to J and Ks bands, optical images in B, Rc, i', and z' bands with Subaru/Suprime-Cam were obtained at about one year after the burst, and a photometric redshift of the host is estimated to be z_{photo} = 1.9. The host luminosity is comparable to L^{*} at z \sim 2 in contrast to the sub-L^{*} property of typical GRB hosts at lower redshifts. The best-fit stellar population synthesis model for the host shows that a large dust extinction (Av = 0.8 mag) attributes to the red nature of the host and that the host galaxy is massive (M_{*} = 7.0 \times 10^{10} Msun) which is one of the most massive GRB hosts previously identified. By assuming that the mass-metallicity relation for star-forming galaxies at z \sim 2 is applicable for the GRB host, this large stellar mass suggests the high metallicity environment around GRB 080325, consistent with inferred large extinction., Comment: 22 pages, 10 figures, accepted for publication in The Astrophysical Journal

Published
2010
Full Text
View/download PDF

9. Evolution of Star-forming Galaxies seen from Lyman Break Galaxies at $z\sim5$

Author

Ohta, K., Yabe, K., Iwata, I., Sawicki, M., Akiyama, M., Tamura, N., and Aoki, K.

Subjects
Astrophysics
Abstract

Properties of Lyman Break Galaxies at $z\sim5$ are presented and are compared with those at $z\sim 2-3$ LBGs to see evolution of LBGs from $z\sim5$ to $z \sim3-2$. The LBGs at $z\sim5$ are tend to have smaller stellar masses, but they may show large star formation rates and specific star formation rates., Comment: 4 pages, 2 figures, proceedings of the first Subaru International Conference: "Panoramic Views of Galaxy Formation and Evolution", Hayama, Japan, December 2007

Published
2008

26. THE GAS INFLOW AND OUTFLOW RAIL IN STAR-FORMING GALAXIES AT z similar to 1.4

Author

Yabe, K, Ohta, K, Akiyama, M, Iwamuro, F, Tamura, N, Yuma, S, Dalton, G, and Lewis, I

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

© 2015. The American Astronomical Society. All rights reserved.We try to constrain the gas inflow and outflow rate of star-forming galaxies at z ∼ 1.4 by employing a simple analytic model for the chemical evolution of galaxies. The sample is constructed based on a large near-infrared spectroscopic sample observed with Subaru/FMOS. The gas-phase metallicity is measured from the [N II] λ6584/Hα emission line ratio and the gas mass is derived from the extinction corrected Hα luminosity by assuming the Kennicutt-Schmidt law. We constrain the inflow and outflow rate from the least-χ 2 fittings of the observed gasmass fraction, stellar mass, and metallicity with the analytic model. The joint χ 2 fitting shows that the best-fit inflow rate is ∼1.8 and the outflow rate is ∼0.6 in units of star-formation rate. By applying the same analysis to the previous studies at z ∼ 0 and z ∼ 2.2, it is shown that both the inflow and outflow rates decrease with decreasing redshift, which implies the higher activity of gas flow process at higher redshift. The decreasing trend of the inflow rate from z ∼ 2.2 to z ∼ 0 agrees with that seen in previous observational works with different methods, though the absolute value is generally larger than in previous works. The outflow rate and its evolution from z ∼ 2.2 to z ∼ 0 obtained in this work agree well with the independent estimations in previous observational works.

Published
2016
Full Text
View/download PDF

28. A study of selection methods for H alpha-emitting galaxies at z similar to 1.3 for the Subaru/FMOS galaxy redshift survey for cosmology (FastSound)

Author

Tonegawa, M, Totani, T, Akiyama, M, Dalton, G, Glazebrook, K, Iwamuro, F, Sumiyoshi, M, Tamura, N, Yabe, K, Coupon, J, Goto, T, and Spitler, L

Subjects
Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The efficient selection of high-redshift emission galaxies is important for future large galaxy redshift surveys for cosmology. Here we describe the target selection methods for the FastSound project, a redshift survey for Hα-emitting galaxies at z = 1.2-1.5 using Subaru/FMOS to measure the linear growth rate fσ8 via redshift space distortion and constrain the theory of gravity. To select ∼400 target galaxies in the 0.2deg2 FMOS field of view from photometric data of CFHTLS-Wide (u*g′r′i′z ′), we test several different methods based on color-color diagrams or photometric redshift estimates from spectral energy distribution (SED) fitting. We also test the improvement in selection efficiency that can be achieved by adding near-infrared data from the UKIDSS DXS (J). The success rates of Hα detection with FMOS averaged over two observed fields using these methods are 11.3% (color-color, optical), 13.6% (color-color, optical + NIR), 17.3% (photo-z, optical), and 15.1% (photo-z, optical + NIR). Selection from photometric redshifts tends to give a better efficiency than color-based methods, although there is no significant improvement by adding J-band data within the statistical scatter. We also investigate the main limiting factors for the success rate, by using the sample of the HiZELS Hα emitters that were selected by narrow-band imaging. Although the number density of total Hα emitters having higher Hα fluxes than the FMOS sensitivity is comparable with the FMOS fiber density, the limited accuracy of photometric redshift and Hα flux estimations have comparable effects on the success rate of 20% obtained from SED fitting. © 2014 The Author.

Published
2014

29. Abstracts of selected papers presented at the 74th general meeting of the Japanese Society of Gastroenterology

Author

Tsuji, Shingo, Sato, Nobuhiro, Kashiwagi, Toru, Koizumi, Takeo, Imai, Kohzoh, Yachi, Akira, Inoue, Masayasu, Takase, Yasuhiro, Shibuya, Susumu, Hashimoto, D., Yabe, K., Ohkuochi, Nobuhiro, Igarashi, Yutaka, Yajima, Yoshiaki, Matsubara, Shuji, Sata, Michio, Abe, Hirohiko, Tarao, Kazuo, Iimori, Kazuto, Ebata, Toshiaki, Hayasaka, Hiroshi, Mochizuki, Hidetaka, Tamakuma, Shoetsu, Shiratori, Y., Shiina, S., Ogawa, Makoto, Mori, Yoshio, Asanuma, Yoshihiro, Koyama, Kenji, Okada, Mitsuo, Yao, Tsuneyoshi, Chikamochi, Nobuo, Bamba, Tadao, Matsueda, Kei, Umeda, Noritsugu, Matsui, Toshiyuki, Iida, Mitsuo, Hibi, T., Iwao, Y., Fukushima, Tsuneo, Sugita, Akira, Funayama, Yuji, Sato, Toshio, Aoki, Teruaki, Watanabe, Yozo, Matsubara, Youichi, Urakawa, Tomoaki, Ogoshi, Kazuei, Fukuchi, S., Maruyama, Masakazu, Saigenji, Katsunori, Horiguchi, Yuji, Yasuda, Hideki, Isogai, Masatoshi, Yamamoto, Masahiro, Ogawa, Michio, Taguchi, Susumu, Muto, Yasutoshi, Fujiwara, Kenji, Kuroda, Hirofumi, Okita, Kiwamu, Miyazaki, Masaru, Higashiguchi, Takashi, and Yoshimura, Seiko

Published
1988
Full Text
View/download PDF

31. FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation rates, metallicity and dust attenuation at z similar to 1

Author

Roseboom, I. G., Bunker, A., Sumiyoshi, M., Wang, L., Dalton, G., Akiyama, M., Bock, J., Bonfield, D., Buat, V., Casey, C., Chapin, E., Clements, D. L., Conley, A., Curtis-Lake, E., Cooray, A., Dunlop, J. S., Farrah, D., Ham, S. J., Ibar, E., Iwamuro, F., Kimura, M., Lewis, I., Macaulay, E., Magdis, G., Maihara, T., Marsden, G., Mauch, T., Moritani, Y., Ohta, K., Oliver, S. J., Page, M. J., Schulz, B., Scott, Douglas, Symeonidis, M., Takato, N., Tamura, N., Totani, T., Yabe, K., Zemcov, M., Heriot-Watt University [Edinburgh] (HWU), Centre de Recherche en Acquisition et Traitement de l'Image pour la Santé (CREATIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Hospices Civils de Lyon (HCL)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], University of California-University of California, JSR Micro, entreprise, CHANG, Laboratoire de glaciologie et géophysique de l'environnement (LGGE), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), AUTRES, National Center for Atmospheric Research [Boulder] (NCAR), California Institute of Technology (CALTECH), Astronomy Centre, University of Sussex, UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), DoCoMo USA Labs, DoCoMo, Division of Respiratory Medicine and Allergology, Teikyo University School of Medicine, Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), Computing and Mathematical Sciences [Pasadena]], Space Science & Technology Department, Rutheford Appleton Laboratory, National Astronomical Observatory of Japan (NAOJ), Université Jean Monnet [Saint-Étienne] (UJM)-Hospices Civils de Lyon (HCL)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université de Lyon-Institut National des Sciences Appliquées (INSA)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), CHANG (CHANG), Laboratoire d'étude des transferts en hydrologie et environnement (LTHE), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet - Saint-Étienne (UJM)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the properties (e.g. star formation rate, dust attentuation, stellar mass and metallicity) of a sample of infrared luminous galaxies at z \sim 1 via near-IR spectroscopy with Subaru-FMOS. Our sample consists of Herschel SPIRE and Spitzer MIPS selected sources in the COSMOS field with photometric redshifts in the range 0.7 < z-phot < 1.8, which have been targeted in 2 pointings (0.5 sq. deg.) with FMOS. We find a modest success rate for emission line detections, with candidate H{\alpha} emission lines detected for 57 of 168 SPIRE sources (34 per cent). By stacking the near-IR spectra we directly measure the mean Balmer decrement for the H{\alpha} and H{\beta} lines, finding a value of = 0.51\pm0.27 for = 10^12 Lsol sources at = 1.36. By comparing star formation rates estimated from the IR and from the dust uncorrected H{\alpha} line we find a strong relationship between dust attenuation and star formation rate. This relation is broadly consistent with that previously seen in star-forming galaxies at z ~ 0.1. Finally, we investigate the metallicity via the N2 ratio, finding that z ~ 1 IR-selected sources are indistinguishable from the local mass-metallicity relation. We also find a strong correlation between dust attentuation and metallicity, with the most metal-rich IR-sources experiencing the largest levels of dust attenuation., Comment: 13 pages, 7 figures, MNRAS accepted

Published
2012
Full Text
View/download PDF

32. FMOS near-IR spectroscopy of Herschel-selected galaxies: star formation rates, metallicity and dust attenuation at z∼ 1

Author

Roseboom, I G, Bunker, A, Sumiyoshi, M, Wang, L, Dalton, G, Akiyama, M, Bock, J, Bonfield, D, Buat, V, Casey, C, Chapin, E, Clements, D L, Conley, A, Curtis-Lake, E, Cooray, A, Dunlop, J S, Farrah, D, Ham, S J, Ibar, E, Iwamuro, F, Kimura, M, Lewis, I, Macaulay, E, Magdis, G, Maihara, T, Marsden, G, Mauch, T, Moritani, Y, Ohta, K, Oliver, S J, Page, M J, Schulz, B, Scott, Douglas, Symeonidis, M, Takato, N, Tamura, N, Totani, T, Yabe, K, and Zemcov, M

Subjects
QB
Published
2012

33. SXDF-UDS-CANDELS-ALMA 1.5 arcmin2 deep survey

Author

Kohno, K., primary, Yamaguchi, Y., additional, Tamura, Y., additional, Tadaki, K., additional, Hatsukade, B., additional, Ikarashi, S., additional, Caputi, K.I., additional, Rujopakarn, W., additional, Ivison, R.J., additional, Dunlop, J.S., additional, Motohara, K., additional, Umehata, H., additional, Yabe, K., additional, Wang, W.H., additional, Kodama, T., additional, Koyama, Y., additional, Hayashi, M., additional, Matsuda, Y., additional, Hughes, D., additional, Aretxaga, I., additional, Wilson, G.W., additional, Yun, M.S., additional, Ohta, K., additional, Akiyama, M., additional, Kawabe, R., additional, Iono, D., additional, Nakanishi, K., additional, Lee, M., additional, and Makiya, R., additional

Published
2015
Full Text
View/download PDF

36. Effects of PSP Appearance on Development of Motor Time in Mentally Retarded Children

Author

TSUKAHARA, R., AOKI, H., and YABE, K.

Abstract

Developmental changes in motor time of mentally retarded children were studied in connection with PSP appearance in agonist muscle. Forty one out of 55 subjects exhibited PSP during jumping reaction movements, and 14 subjects did not exhibit PSP. Among subjects exhibiting PSP, motor time shortened with increasing MA. Subjects exhibiting no PSP did not show any MA-related changes in motor time. It is suggested that acquistition of PSP and cognitive development contribute to shortening of motor time.

Published
1990

37. BLACK HOLE MASS AND EDDINGTON RATIO DISTRIBUTION FUNCTIONS OF X-RAY-SELECTED BROAD-LINE AGNs ATz∼ 1.4 IN THE SUBARUXMM-NEWTONDEEP FIELD

Author

Nobuta, K., primary, Akiyama, M., additional, Ueda, Y., additional, Watson, M. G., additional, Silverman, J., additional, Hiroi, K., additional, Ohta, K., additional, Iwamuro, F., additional, Yabe, K., additional, Tamura, N., additional, Moritani, Y., additional, Sumiyoshi, M., additional, Takato, N., additional, Kimura, M., additional, Maihara, T., additional, Dalton, G., additional, Lewis, I., additional, Bonfield, D., additional, Lee, H., additional, Curtis-Lake, E., additional, Macaulay, E., additional, Clarke, F., additional, Sekiguchi, K., additional, Simpson, C., additional, Croom, S., additional, Ouchi, M., additional, Hanami, H., additional, and Yamada, T., additional

Published
2012
Full Text
View/download PDF

38. FMOS near-IR spectroscopy ofHerschel-selected galaxies: star formation rates, metallicity and dust attenuation atz∼ 1

Author

Roseboom, I. G., primary, Bunker, A., additional, Sumiyoshi, M., additional, Wang, L., additional, Dalton, G., additional, Akiyama, M., additional, Bock, J., additional, Bonfield, D., additional, Buat, V., additional, Casey, C., additional, Chapin, E., additional, Clements, D. L., additional, Conley, A., additional, Curtis-Lake, E., additional, Cooray, A., additional, Dunlop, J. S., additional, Farrah, D., additional, Ham, S. J., additional, Ibar, E., additional, Iwamuro, F., additional, Kimura, M., additional, Lewis, I., additional, Macaulay, E., additional, Magdis, G., additional, Maihara, T., additional, Marsden, G., additional, Mauch, T., additional, Moritani, Y., additional, Ohta, K., additional, Oliver, S. J., additional, Page, M. J., additional, Schulz, B., additional, Scott, Douglas, additional, Symeonidis, M., additional, Takato, N., additional, Tamura, N., additional, Totani, T., additional, Yabe, K., additional, and Zemcov, M., additional

Published
2012
Full Text
View/download PDF

40. “DARK” GRB 080325 IN A DUSTY MASSIVE GALAXY ATz∼ 2

Author

Hashimoto, T., primary, Ohta, K., additional, Aoki, K., additional, Tanaka, I., additional, Yabe, K., additional, Kawai, N., additional, Aoki, W., additional, Furusawa, H., additional, Hattori, T., additional, Iye, M., additional, Kawabata, K. S., additional, Kobayashi, N., additional, Komiyama, Y., additional, Kosugi, G., additional, Minowa, Y., additional, Mizumoto, Y., additional, Niino, Y., additional, Nomoto, K., additional, Noumaru, J., additional, Ogasawara, R., additional, Pyo, T.-S., additional, Sakamoto, T., additional, Sekiguchi, K., additional, Shirasaki, Y., additional, Suzuki, M., additional, Tajitsu, A., additional, Takata, T., additional, Tamagawa, T., additional, Terada, H., additional, Totani, T., additional, Watanabe, J., additional, Yamada, T., additional, and Yoshida, A., additional

Published
2010
Full Text
View/download PDF

41. Important challenges for line-width-roughness reduction

Author

Yaegashi, Hidetami, primary, Kushibiki, M., additional, Nishimura, E., additional, Shimura, S., additional, Iwao, F., additional, Kawasaki, T., additional, Hasebe, K., additional, Murakami, H., additional, Hara, A., additional, and Yabe, K., additional

Published
2009
Full Text
View/download PDF

43. Flexible composite film for printed circuit board

Author

Yabe, K, Asakura, M, Tanaka, H, and Soda, A

Subjects
Electronics And Electrical Engineering
Abstract

A flexible printed circuit for a printed circuit board in which layers of reaction product composed of a combination of phenoxy resin - polyisocyanate - brominated epoxy resin, and in which the equivalent ratio of those functional groups is hydroxyl group: isocyanate group: epoxy group - 1 : 0.2 to 2 : 0.5 to 3 are laminated on at least one side of saturated polyester film is discussed.

Published
1982

44. Flexible substrate for printed wiring

Author

Asakura, M, Yabe, K, Tanaka, H, and Soda, A

Subjects
Composite Materials
Abstract

A very flexible substrate for printed wiring is disclosed which is composed of a blend of phenoxy resin-polyisocyanate-brominated epoxy resin in which the equivalent ration of the functional groups is hydroxyl grouped: isocyanate group: epoxy group = 1:0.2 to 2:0.5 to 3. The product has outstanding solder resistance and is applied to metal without using adhesives.

Published
1982

Catalog

Books, media, physical & digital resources
See catalog results