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251. A galaxy at a redshift z = 6.96

Author

Iye, Masanori, primary, Ota, Kazuaki, additional, Kashikawa, Nobunari, additional, Furusawa, Hisanori, additional, Hashimoto, Tetsuya, additional, Hattori, Takashi, additional, Matsuda, Yuichi, additional, Morokuma, Tomoki, additional, Ouchi, Masami, additional, and Shimasaku, Kazuhiro, additional

Published
2006
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252. The End of the Reionization Epoch Probed by Lyα Emitters atz= 6.5 in the Subaru Deep Field

Author

Kashikawa, Nobunari, primary, Shimasaku, Kazuhiro, additional, Malkan, Matthew A., additional, Doi, Mamoru, additional, Matsuda, Yuichi, additional, Ouchi, Masami, additional, Taniguchi, Yoshiaki, additional, Ly, Chun, additional, Nagao, Tohru, additional, Iye, Masanori, additional, Motohara, Kentaro, additional, Murayama, Takashi, additional, Murozono, Kouji, additional, Nariai, Kyoji, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Sasaki, Toshiyuki, additional, Shioya, Yasuhiro, additional, and Umemura, Masayuki, additional

Published
2006
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253. Lyα Emitters atz= 5.7 in the Subaru Deep Field

Author

Shimasaku, Kazuhiro, primary, Kashikawa, Nobunari, additional, Doi, Mamoru, additional, Ly, Chun, additional, Malkan, Matthew A., additional, Matsuda, Yuichi, additional, Ouchi, Masami, additional, Hayashino, Tomoki, additional, Iye, Masanori, additional, Motohara, Kentaro, additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Sasaki, Toshiyuki, additional, Shioya, Yasuhiro, additional, and Taniguchi, Yoshiaki, additional

Published
2006
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255. Clustering of Lyman Break Galaxies atz= 4 and 5 in the Subaru Deep Field: Luminosity Dependence of the Correlation Function Slope

Author

Kashikawa, Nobunari, primary, Yoshida, Makiko, additional, Shimasaku, Kazuhiro, additional, Nagashima, Masahiro, additional, Yahagi, Hideki, additional, Ouchi, Masami, additional, Matsuda, Yuichi, additional, Malkan, Matthew A., additional, Doi, Mamoru, additional, Iye, Masanori, additional, Ajiki, Masaru, additional, Akiyama, Masayuki, additional, Ando, Hiroyasu, additional, Aoki, Kentaro, additional, Furusawa, Hisanori, additional, Hayashino, Tomoki, additional, Iwamuro, Fumihide, additional, Karoji, Hiroshi, additional, Kobayashi, Naoto, additional, Kodaira, Keiichi, additional, Kodama, Tadayuki, additional, Komiyama, Yutaka, additional, Miyazaki, Satoshi, additional, Mizumoto, Yoshihiko, additional, Morokuma, Tomoki, additional, Motohara, Kentaro, additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Nariai, Kyoji, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Sasaki, Toshiyuki, additional, Sato, Yasunori, additional, Sekiguchi, Kazuhiro, additional, Shioya, Yasuhiro, additional, Tamura, Hajime, additional, Taniguchi, Yoshiaki, additional, Umemura, Masayuki, additional, Yamada, Toru, additional, and Yasuda, Naoki, additional

Published
2006
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257. Large-Scale Filamentary Structure around the Protocluster at Redshift z = 3.1

Author

Matsuda, Yuichi, primary, Yamada, Toru, additional, Hayashino, Tomoki, additional, Tamura, Hajime, additional, Yamauchi, Ryosuke, additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Shimasaku, Kazuhiro, additional, Shioya, Yasuhiro, additional, and Taniguchi, Yoshiaki, additional

Published
2005
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258. The SUBARU Deep Field Project: Lymanα Emitters at a Redshift of 6.6

Author

Taniguchi, Yoshiaki, primary, Ajiki, Masaru, additional, Nagao, Tohru, additional, Shioya, Yasuhiro, additional, Murayama, Takashi, additional, Kashikawa, Nobunari, additional, Kodaira, Keiichi, additional, Kaifu, Norio, additional, Ando, Hiroyasu, additional, Karoji, Hiroshi, additional, Akiyama, Masayuki, additional, Aoki, Kentaro, additional, Doi, Mamoru, additional, Fujita, Shinobu S., additional, Furusawa, Hisanori, additional, Hayashino, Tomoki, additional, Iwamuro, Fumihide, additional, Iye, Masanori, additional, Kobayashi, Naoto, additional, Kodama, Tadayuki, additional, Komiyama, Yutaka, additional, Matsuda, Yuichi, additional, Miyazaki, Satoshi, additional, Mizumoto, Yoshihiko, additional, Morokuma, Tomoki, additional, Motohara, Kentaro, additional, Nariai, Kyoji, additional, Ohta, Koji, additional, Ohyama, Youichi, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Sasaki, Toshiyuki, additional, Sato, Yasunori, additional, Sekiguchi, Kazuhiro, additional, Shimasaku, Kazuhiro, additional, Tamura, Hajime, additional, Umemura, Masayuki, additional, Yamada, Toru, additional, Yasuda, Naoki, additional, and Yoshida, Michitoshi, additional

Published
2005
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259. The Subaru Deep Field: The Optical Imaging Data

Author

Kashikawa, Nobunari, primary, Shimasaku, Kazuhiro, additional, Yasuda, Naoki, additional, Ajiki, Masaru, additional, Akiyama, Masayuki, additional, Ando, Hiroyasu, additional, Aoki, Kentaro, additional, Doi, Mamoru, additional, Fujita, Shinobu S., additional, Furusawa, Hisanori, additional, Hayashino, Tomoki, additional, Iwamuro, Fumihide, additional, Iye, Masanori, additional, Karoji, Hiroshi, additional, Kobayashi, Naoto, additional, Kodaira, Keiichi, additional, Kodama, Tadayuki, additional, Komiyama, Yutaka, additional, Matsuda, Yuichi, additional, Miyazaki, Satoshi, additional, Mizumoto, Yoshihiko, additional, Morokuma, Tomoki, additional, Motohara, Kentaro, additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Nariai, Kyoji, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Sasaki, Toshiyuki, additional, Sato, Yasunori, additional, Sekiguchi, Kazuhiro, additional, Shioya, Yasunori, additional, Tamura, Hajime, additional, Taniguchi, Yoshiaki, additional, Umemura, Masayuki, additional, Yamada, Toru, additional, and Yoshida, Makiko, additional

Published
2004
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260. Large-Scale Structure of Emission-Line Galaxies atz = 3.1

Author

Hayashino, Tomoki, primary, Matsuda, Yuichi, additional, Tamura, Hajime, additional, Yamauchi, Ryosuke, additional, Yamada, Toru, additional, Ajiki, Masaru, additional, Fujita, Shinobu S., additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Shimasaku, Kazuhiro, additional, Shioya, Yasuhiro, additional, and Taniguchi, Yoshiaki, additional

Published
2004
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261. A Subaru Search for Lyα Blobs in and around the Protocluster Region At Redshiftz= 3.1

Author

Matsuda, Yuichi, primary, Yamada, Toru, additional, Hayashino, Tomoki, additional, Tamura, Hajime, additional, Yamauchi, Ryosuke, additional, Ajiki, Masaru, additional, Fujita, Shinobu S., additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Ohta, Kouji, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Shimasaku, Kazuhiro, additional, Shioya, Yasuhiro, additional, and Taniguchi, Yoshiaki, additional

Published
2004
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265. The Discovery of Two Lyman α Emitters beyond Redshift 6 in the Subaru Deep Field,

Author

Kodaira, Keiichi, primary, Taniguchi, Yoshiaki, additional, Kashikawa, Nobunari, additional, Kaifu, Norio, additional, Ando, Hiroyasu, additional, Karoji, Hiroshi, additional, Ajiki, Masaru, additional, Akiyama, Masayuki, additional, Aoki, Kentaro, additional, Doi, Mamoru, additional, Fujita, Shinobu S., additional, Furusawa, Hisanori, additional, Hayashino, Tomoki, additional, Imanishi, Masatoshi, additional, Iwamuro, Fumihide, additional, Iye, Masanori, additional, Kawabata, Koji S., additional, Kobayashi, Naoto, additional, Kodama, Tadayuki, additional, Komiyama, Yutaka, additional, Kosugi, George, additional, Matsuda, Yuichi, additional, Miyazaki, Satoshi, additional, Mizumoto, Yoshihiko, additional, Motohara, Kentaro, additional, Murayama, Takashi, additional, Nagao, Tohru, additional, Nariai, Kyoji, additional, Ohta, Kouji, additional, Ohyama, Youichi, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Sasaki, Toshiyuki, additional, Sekiguchi, Kazuhiro, additional, Shimasaku, Kazuhiro, additional, Shioya, Yasunori, additional, Takata, Tadafumi, additional, Tamura, Hajime, additional, Terada, Hiroshi, additional, Umemura, Masayuki, additional, Usuda, Tomonori, additional, Yagi, Masafumi, additional, Yamada, Toru, additional, Yasuda, Naoki, additional, and Yoshida, Michitoshi, additional

Published
2003
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266. A Search for [CLC]Ly[/CLC]α Emitters at Redshift 3.7

Author

Fujita, Shinobu S., primary, Ajiki, Masaru, additional, Shioya, Yasuhiro, additional, Nagao, Tohru, additional, Murayama, Takashi, additional, Taniguchi, Yoshiaki, additional, Okamura, Sadanori, additional, Ouchi, Masami, additional, Shimasaku, Kazuhiro, additional, Doi, Mamoru, additional, Furusawa, Hisanori, additional, Hamabe, Masaru, additional, Kimura, Masahiko, additional, Komiyama, Yutaka, additional, Miyazaki, Masayuki, additional, Miyazaki, Satoshi, additional, Nakata, Fumiaki, additional, Sekiguchi, Maki, additional, Yagi, Masafumi, additional, Yasuda, Naoki, additional, Matsuda, Yuichi, additional, Tamura, Hajime, additional, Hayashino, Tomoki, additional, Kodaira, Keiichi, additional, Karoji, Hiroshi, additional, Yamada, Toru, additional, Ohta, Kouji, additional, and Umemura, Masayuki, additional

Published
2003
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267. Subaru Deep Survey. II. Luminosity Functions and Clustering Properties of Lyα Emitters atz = 4.86 in the Subaru Deep Field

Author

Ouchi, Masami, primary, Shimasaku, Kazuhiro, additional, Furusawa, Hisanori, additional, Miyazaki, Masayuki, additional, Doi, Mamoru, additional, Hamabe, Masaru, additional, Hayashino, Tomoki, additional, Kimura, Masahiko, additional, Kodaira, Keiichi, additional, Komiyama, Yutaka, additional, Matsuda, Yuichi, additional, Miyazaki, Satoshi, additional, Nakata, Fumiaki, additional, Okamura, Sadanori, additional, Sekiguchi, Maki, additional, Shioya, Yasuhiro, additional, Tamura, Hajime, additional, Taniguchi, Yoshiaki, additional, Yagi, Masafumi, additional, and Yasuda, Naoki, additional

Published
2003
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270. Modification of Postural Response Caused by Footwear Conditions.

Author

Maejima, Hiroshi, primary, Kamoda, Chie, additional, Takayanagi, Kiyomi, additional, Hosoda, Masataka, additional, Kobayashi, Ryuji, additional, Minematsu, Akira, additional, Sasaki, Hisato, additional, Matsuda, Yuichi, additional, Tanaka, Yukiko, additional, Matsuo, Akihisa, additional, Kanemura, Naohiko, additional, Ueda, Tatehiko, additional, and Yoshimura, Osamu, additional

Published
2000
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271. The Effect of Low Calcium Diet on Bone in Ovariectomized Mice.

Author

Minematsu, Akira, primary, Yoshimura, Osamu, additional, Yotsuji, Hirofumi, additional, Ichigo, Hirozo, additional, Takayanagi, Kiyomi, additional, Kobayashi, Ryuji, additional, Hosoda, Masataka, additional, Sasaki, Hisato, additional, Maejima, Hiroshi, additional, Matsuda, Yuichi, additional, Tanaka, Sachiko, additional, Kanemura, Naohiko, additional, and Matsuo, Akihisa, additional

Published
2000
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274. A large Hα survey at z = 2.23, 1.47, 0.84 and 0.40: the 11 Gyr evolution of star-forming galaxies from HiZELS★.

Author

Sobral, David, Smail, Ian, Best, Philip N., Geach, James E., Matsuda, Yuichi, Stott, John P., Cirasuolo, Michele, and Kurk, Jaron

Subjects
GALACTIC evolution, STAR formation, VERY Large Telescope (Chile), STELLAR luminosity function, STELLAR mass, ROBUST control, SURVEYS
Abstract

This paper presents new deep and wide narrow-band surveys undertaken with United Kingdom Infrared Telescope (UKIRT), Subaru and the Very Large Telescope (VLT), a unique combined effort to select large, robust samples of Hα star-forming galaxies at z = 0.40, 0.84, 1.47 and 2.23 (corresponding to look-back times of 4.2, 7.0, 9.2 and 10.6 Gyr) in a uniform manner over ∼2 deg2 in the Cosmological Evolution Survey and Ultra Deep Survey fields. The deep multi-epoch Hα surveys reach a matched 3σ flux limit of ≈3 M⊙ yr−1 out to z = 2.2 for the first time, while the wide area and the coverage over two independent fields allow us to greatly overcome cosmic variance and assemble by far the largest samples of Hα emitters. Catalogues are presented for a total of 1742, 637, 515 and 807 Hα emitters, robustly selected at z = 0.40, 0.84, 1.47 and 2.23, respectively, and used to determine the Hα luminosity function and its evolution. The faint-end slope of the Hα luminosity function is found to be α = −1.60 ± 0.08 over z = 0–2.23, showing no significant evolution. The characteristic luminosity of star-forming galaxies, L*Hα, evolves significantly as log L*Hα(z) = 0.45z + log L*z = 0. This is the first time Hα has been used to trace star formation activity with a single homogeneous survey at z = 0.4–2.23. Overall, the evolution seen with Hα is in good agreement with the evolution seen using inhomogeneous compilations of other tracers of star formation, such as far-infrared and ultraviolet, jointly pointing towards the bulk of the evolution in the last 11 Gyr being driven by a statistically similar star-forming population across cosmic time, but with a strong luminosity increase from z ∼ 0 to ∼2.2. Our uniform analysis allows us to derive the Hα star formation history (SFRH) of the Universe, showing a clear rise up to z ∼ 2.2, for which the simple parametrization log10ρSFR = −2.1(1 + z)−1 is valid over 80 per cent of the age of the Universe. The results reveal that both the shape and normalization of the Hα SFRH are consistent with the measurements of the stellar mass density growth, confirming that our Hα SFRH is tracing the bulk of the formation of stars in the Universe for z < 2.23. The star formation activity over the last ∼11 Gyr is responsible for producing ∼95 per cent of the total stellar mass density observed locally, with half of that being assembled in 2 Gyr between z = 1.2 and 2.2, and the other half in 8 Gyr (since z < 1.2). If the star formation rate density continues to decline with time in the same way as seen in the past ∼11 Gyr, then the stellar mass density of the Universe will reach a maximum which is only 5 per cent higher than the present-day value. [ABSTRACT FROM PUBLISHER]

Published
2013
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277. Effects of lysophosphatidylcholine on coronary microcirculation

Author

Matsuda, Yuichi, primary, Akita, Hozuka, additional, Suematsu, Masakuni, additional, Hirata, Ken-ichi, additional, Inoue, Nobutaka, additional, Katayama, Masaya, additional, Miwa, Yoichi, additional, Kanazawa, Kenji, additional, Iwakabe, Hideki, additional, and Yokoyama, Mitsuhiro, additional

Published
1992
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278. Star formation at z= 1.47 from HiZELS: an H α+[O ii] double-blind study★.

Author

Sobral, David, Best, Philip N., Matsuda, Yuichi, Smail, Ian, Geach, James E., and Cirasuolo, Michele

Subjects
STAR formation, BLIND experiment, INFRARED telescopes, STELLAR luminosity function, COMPARATIVE studies, STELLAR mass
Abstract

ABSTRACT This paper presents the results from the first wide and deep dual narrow-band survey to select Hα and [O ii] line emitters at z= 1.47 ± 0.02, exploiting synergies between the United Kingdom Infrared Telescope and the Subaru telescope by using matched narrow-band filters in the H and z′ bands. The Hα survey at z= 1.47 reaches a 3σ flux limit of FHα≈ 7 × 10−17 erg s−1 cm−2 (corresponding to a limiting star formation rate (SFR) in Hα of ≈7 M⊙ yr−1) and detects ≈200 Hα emitters over 0.7 deg2, while the much deeper [O ii] survey reaches an effective flux of ≈7 × 10−18 erg s−1 cm−2 (SFR in [O ii] of ∼1 M⊙ yr−1), detecting ≈1400 z= 1.47 [O ii] emitters in a matched comoving volume of ∼2.5 × 105 Mpc3. The combined survey results in the identification of 190 simultaneous Hα and [O ii] emitters at z= 1.47. Hα and [O ii] luminosity functions are derived and both are shown to evolve significantly from z∼ 0 in a consistent way. The SFR density of the Universe at z= 1.47 is evaluated, with the Hα analysis yielding ρSFR= 0.16 ± 0.05 M⊙ yr−1 Mpc−3 and the [O ii] analysis ρSFR= 0.17 ± 0.04 M⊙ yr−1 Mpc−3. The measurements are combined with other studies, providing a self-consistent measurement of the star formation history of the Universe over the last ∼11 Gyr. By using a large comparison sample at z∼ 0.1, derived from the Sloan Digital Sky Survey (SDSS), [O ii]/Hα line ratios are calibrated as probes of dust extinction. Hα emitters at z∼ 1.47 show on average AHα≈ 1 mag, the same as found by SDSS in the local Universe. It is shown that although dust extinction correlates with SFR, the relation evolves by about ∼0.5 mag from z∼ 1.5 to ∼0, with local relations overpredicting the dust extinction corrections at high z by that amount. Stellar mass is found to be a much more fundamental extinction predictor, with the same relation between mass and dust extinction being valid at both z∼ 0 and ∼1.5, at least for low and moderate stellar masses. The evolution in the extinction-SFR relation is therefore interpreted as being due to the evolution in median specific SFRs over cosmic time. Dust extinction corrections as a function of optical colours are also derived and shown to be broadly valid at both z∼ 0 and ∼1.5, offering simpler mechanisms for estimating extinction in moderately star-forming systems over the last ∼9 Gyr. [ABSTRACT FROM AUTHOR]

Published
2012
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279. CONSTRAINING DUST AND MOLECULAR GAS PROPERTIES IN Lyα BLOBS AT z ~ 3.

Author

Yujin Yang, Decarli, Roberto, Dannerbauer, Helmut, Walter, Fabian, Weiss, Axel, Leipski, Christian, Dey, Arjun, Chapman, Scott C., Le Floc'h, Emeric, Prescott, Moire K. M., Neri, Roberto, Borys, Colin, Matsuda, Yuichi, Yamada, Toru, Hayashino, Tomoki, Tapken, Christian, and Menten, Karl M.

Subjects
BINARY large objects, GALAXIES, MICROWAVE detectors, ASTRONOMICAL photometry, BOLOMETERS
Abstract

In order to constrain the bolometric luminosities, dust properties, and molecular gas content of giant Lyα nebulae, the so-called Lyα blobs, we have carried out a study of dust continuum and CO line emission in two well-studied representatives of this population at z ~ 3: an Lyα blob discovered by its strong Spitzer Multiband Infrared Photometer 24 µm detection (LABd05) and the Steidel blob 1 (SSA22-LAB01). We find that the spectral energy distribution of LABd05 is well described by an active-galactic-nucleus--starburst composite template with LFIR = (4.0 ± 0.5) x 1012 L⊙, comparable to high-z submillimeter galaxies and ultraluminous infrared galaxies. New Large APEX Bolometer Camera 870 µm measurements rule out the reported Submillimeter Common-User Bolometer Array detection of the SSA22-LAB01 (S850 µm = 16.8 mJy) at the >4σ level. Consistent with this, ultradeep Plateau de Bure Interferometer observations with ~2" spatial resolution also fail to detect any 1.2 mm continuum source down to ≈0.45 mJy beam-1 (3σ). Combined with the existing (sub)millimeter observations in the literature, we conclude that the FIR luminosity of SSA22-LAB01 remains uncertain. No CO line is detected in either case down to integrated flux limits of SvΔV ≲ 0.25-1.0 Jy km s-1, indicating a modest molecular gas reservoir, M(H2) < (1-3) x 1010 M⊙. The non-detections exclude, with high significance (12σ), the previous tentative detection of a CO J = 4-3 line in the SSA22-LAB01. The increased sensitivity afforded by the Atacama Large Millimeter/submillimeter Array will be critical in studying molecular gas and dust in these interesting systems. [ABSTRACT FROM AUTHOR]

Published
2012
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280. KECK SPECTROSCOPY OF LYMAN-BREAK GALAXIES AND ITS IMPLICATIONS FOR THE UV-CONTINUUM AND Lyα LUMINOSITY FUNCTIONS AT z > 6.

Author

Linhua Jiang, Egami, Eiichi, Kashikawa, Nobunari, Walth, Gregory, Matsuda, Yuichi, Shimasaku, Kazuhiro, Nagao, Tohru, Ota, Kazuaki, and Ouchi, Masami

Subjects
SPECTRUM analysis, STELLAR luminosity function, SPECTROSCOPIC imaging, ULTRAVIOLET photometry, STELLAR magnitudes, STELLAR mass, UBV system (Astronomy)
Abstract

We present Keck spectroscopic observations of z > 6 Lyman-break galaxy (LBG) candidates in the Subaru Deep Field (SDF). The candidates were selected as i'-dropout objects down to z' = 27 AB magnitudes from an ultra-deep SDF z'-band image. With the Keck spectroscopy we identified 19 LBGs with prominent Lyα emission lines at 6 ≤ z ≤ 6.4. The median value of the Lyα rest-frame equivalent widths (EWs) is ~50Å, with four EWs > 100 Å. This well-defined spectroscopic sample spans a UV-continuum luminosity range of -21.8 ≤ MUV ≤ -19.5 (0.6 ~ 5 L*UV) and a Lyα luminosity range of (0.3-3) x 1043 erg s-1 (0.3-3 L*Lyα). We derive the UV and Lyα luminosity functions (LFs) from our sample at (z) ~ 6.2 after we correct for sample incompleteness. We find that our measurement of the UV LF is consistent with the results of previous studies based on photometric LBG samples at 5 < z < 7. Our Lyα, LF is also generally in agreement with the results of Lyα-emitter surveys at z ~ 5.7 and 6.6. This study shows that deep spectroscopic observations of LBGs can provide unique constraints on both the UV and Lyα LFs at z > 6. [ABSTRACT FROM AUTHOR]

Published
2011
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281. Subaru Deep Survey. II. Luminosity Functions and Clustering Properties of Lyα Emitters at z = 4.86 in the Subaru Deep FieldBased on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Author

Ouchi, Masami, Shimasaku, Kazuhiro, Furusawa, Hisanori, Miyazaki, Masayuki, Doi, Mamoru, Hamabe, Masaru, Hayashino, Tomoki, Kimura, Masahiko, Kodaira, Keiichi, Komiyama, Yutaka, Matsuda, Yuichi, Miyazaki, Satoshi, Nakata, Fumiaki, Okamura, Sadanori, Sekiguchi, Maki, Shioya, Yasuhiro, Tamura, Hajime, Taniguchi, Yoshiaki, Yagi, Masafumi, and Yasuda, Naoki

Published
2003
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284. Myocardial ischaemia induced by endothelin in the intact rabbit: angiographic analysis.

Author

Hirata, Ken-ichi, Matsuda, Yuichi, Akita, H, Yokoyama, M, and Fukuzaki, H

Abstract

Study objective – The aim was to clarify the effects of endothelin on coronary vasculature in the intact rabbit by coronary angiographic examination.Design – By selective coronary angiography bolus injections of various amounts of endothelin (0.01-1 nmol) were given into the right coronary artery of anaesthetised rabbits. The preventive effects of nifedipine on endothelin induced myocardial ischaemia were examined.Subjects – Adult male Japanese white rabbits (2.7-3.5 kg, n=29) were used for in vivo and in vitro studies.Measurements and main results – Intracoronary administration of 0.1 nmol endothelin led to the delayed filling of contrast medium into the distal coronary artery and the sustained retention of contrast medium in both large and small coronary arteries, associated with distinct ST elevation in leads II, III and aVF on the electrocardiogram. However, endothelin produced no evident constriction at any site in the large epicardial coronary arteries. Intracoronary administration of glyceryl trinitrate (50 μg) or nifedipine (5 μg) failed to reverse myocardial ischaemic changes induced by endothelin. Pretreatment with intravenous administration of nifedipine (3 μg·kg−1) partially inhibited the endothelin induced vasoconstrictor effect on small coronary arteries and subsequent ischaemic changes. In isolated coronary arterial preparation, endothelin produced long lasting contraction in a dose dependent manner [ED50=3.7 (SEM 1.8) nM]. Pretreatment with nifedipine inhibited the maximum contraction induced by endothelin, but did not affect the threshold dose or the half maximal effective dose (ED50). Endothelin (0.1 μM) per se did not produce aggregatory responses of rabbit platelets.Conclusions – Endothelin induced myocardial ischaemia cannot be ascribed to vasospastic constriction of large coronary arteries nor to platelet thrombi, but diffuse constriction of small coronary arteries occurs in the intact rabbit. [ABSTRACT FROM PUBLISHER]

Published
1990

288. Reionization and Galaxy Evolution Probed by z = 7 Ly? Emitters

Author

Ota, Kazuaki, Iye, Masanori, Kashikawa, Nobunari, Shimasaku, Kazuhiro, Kobayashi, Masakazu, Totani, Tomonori, Nagashima, Masahiro, Morokuma, Tomoki, Furusawa, Hisanori, Hattori, Takashi, Matsuda, Yuichi, Hashimoto, Tetsuya, and Ouchi, Masami

Abstract

We have performed narrowband NB973 (bandwidth 200 A centered at 9755 A) imaging of the Subaru Deep Field (SDF) and found two "z=7"/ z = 7 Lya emitter (LAE) candidates down to NB973 "=24.9"/ = 24.9. Carrying out deep follow-up spectroscopy, we identified one of them as a real "z=6.96"/ z = 6.96 LAE. This has established a new redshift record, showing that galaxy formation was in progress just 750 Myr after the big bang. Meanwhile, the Lya line luminosity function of LAEs is known to decline from "z=5.7"/ z = 5.7 to 6.6 in the SDF; "L^{*}"/ L* at "z=6.6"/ z = 6.6 is 40%-60% that at "z=5.7"/ z = 5.7. We also confirm that the number density of "z=7"/ z = 7 LAEs is only 17% of the density at "z=6.6"/ z = 6.6 comparing the latest SDF LAE samples. This series of significant decreases in LAE density with increasing redshift could be the result of galaxy evolution during these epochs. However, using the UV continuum luminosity functions of LAEs and Lyman break galaxies, and a LAE evolution model based on hierarchical clustering, we find that galaxy evolution alone cannot entirely explain the decrease in density. This extra density deficit might reflect the attenuation of the Lya photons from LAEs by the neutral hydrogen possibly left at the last stage of cosmic reionization at "z\sim z [?] 6-7.

Published
2008

289. Luminosity Functions of Lyman Break Galaxies at z ~ 4 and z ~ 5 in the Subaru Deep Field

Author

Yoshida, Makiko, Shimasaku, Kazuhiro, Kashikawa, Nobunari, Ouchi, Masami, Okamura, Sadanori, Ajiki, Masaru, Akiyama, Masayuki, Ando, Hiroyasu, Aoki, Kentaro, Doi, Mamoru, Furusawa, Hisanori, Hayashino, Tomoki, Iwamuro, Fumihide, Iye, Masanori, Karoji, Hiroshi, Kobayashi, Naoto, Kodaira, Keiichi, Kodama, Tadayuki, Komiyama, Yutaka, Malkan, Matthew A., Matsuda, Yuichi, Miyazaki, Satoshi, Mizumoto, Yoshihiko, Morokuma, Tomoki, Motohara, Kentaro, Murayama, Takashi, Nagao, Tohru, Nariai, Kyoji, Ohta, Kouji, Sasaki, Toshiyuki, Sato, Yasunori, Sekiguchi, Kazuhiro, Shioya, Yasuhiro, Tamura, Hajime, Taniguchi, Yoshiaki, Umemura, Masayuki, Yamada, Toru, and Yasuda, Naoki

Abstract

We investigate the luminosity functions of Lyman break galaxies (LBGs) at z ~ 4 and z ~ 5 based on optical imaging data obtained in the Subaru Deep Field project. Three samples of LBGs in a contiguous area of 875 arcmin2 are constructed. One consists of 3808 LBGs at z ~ 4 down to i' = 26.85 selected with the B-R versus R-i' diagram. The other two consist of 539 and 240 LBGs at z ~ 5 down to z' = 26.05 selected with two kinds of two-color diagram: V-i' versus i'-z' and R-i' versus i'-z'. The adopted selection criteria are proved to be fairly reliable by spectroscopic observations. We derive the luminosity functions of the LBGs at rest-frame ultraviolet wavelengths down to MUV = -19.2 at z ~ 4 and MUV = -20.3 at z ~ 5. We find clear evolution of the luminosity function over the redshift range 0 [?] z [?] 6, which is accounted for solely by a change in the characteristic magnitude M*. We examine the evolution of the cosmic star formation rate (SFR) density and its luminosity dependence over 0 [?] z [?] 6. The SFR density contributed from brighter galaxies is found to change more drastically with cosmic time. The contribution from brighter galaxies has a sharp peak around z = 3-4, while that from fainter galaxies evolves relatively mildly with a broad peak at earlier epochs. Combining the observed SFR density with the standard cold dark matter model, we compute the cosmic SFR per unit baryon mass in dark halos, that is, the specific SFR. The specific SFR is found to scale with redshift as (1 + z)3 up to z ~ 4, implying that the efficiency of star formation is on average higher at higher redshift in proportion to the cooling rate within dark halos, while this is not simply the case at z [?] 4.

Published
2006

290. The End of the Reionization Epoch Probed by Ly? Emitters at z = 6.5 in the Subaru Deep Field

Author

Kashikawa, Nobunari, Shimasaku, Kazuhiro, Malkan, Matthew A., Doi, Mamoru, Matsuda, Yuichi, Ouchi, Masami, Taniguchi, Yoshiaki, Ly, Chun, Nagao, Tohru, Iye, Masanori, Motohara, Kentaro, Murayama, Takashi, Murozono, Kouji, Nariai, Kyoji, Ohta, Kouji, Okamura, Sadanori, Sasaki, Toshiyuki, Shioya, Yasuhiro, and Umemura, Masayuki

Abstract

We report an extensive search for Lya emitters (LAEs) at z = 6.5 in the Subaru Deep Field. Subsequent spectroscopy with Subaru and Keck identified eight more LAEs, giving a total of 17 spectroscopically confirmed LAEs at z = 6.5. Based on this spectroscopic sample of 17, complemented by a photometric sample of 58 LAEs, we have derived a more accurate Lya luminosity function of LAEs at z = 6.5, which reveals an apparent deficit at the bright end of ~0.75 mag fainter L*, compared with that observed at z = 5.7. The difference in the LAE luminosity functions between z = 5.7 and 6.5 is significant at the 3 s level, which is reduced to 2 s when cosmic variance is taken into account. This result may imply that the reionization of the universe has not been completed at z = 6.5. We found that the spatial distribution of LAEs at z = 6.5 was homogeneous over the field. We discuss the implications of these results for the reionization of the universe.

Published
2006

291. Lyα Emitters at z= 5.7 in the Subaru Deep Field *†

Author

Shimasaku, Kazuhiro, Kashikawa, Nobunari, Doi, Mamoru, Ly, Chun, Malkan, Matthew A., Matsuda, Yuichi, Ouchi, Masami, Hayashino, Tomoki, Iye, Masanori, Motohara, Kentaro, Murayama, Takashi, Nagao, Tohru, Ohta, Kouji, Okamura, Sadanori, Sasaki, Toshiyuki, Shioya, Yasuhiro, and Taniguchi, Yoshiaki

Abstract

We present the properties of Ly$\alpha$emitters (LAEs) at $z=5.7$in the Subaru Deep Field. A photometric sample of 89 LAE candidates was constructed from narrow-band data down to $\mathit{NB816} = 26.0$(AB) in a continuous $725 \,\mathrm{arcmin}^2$area. Spectra of 39 objects satisfying the photometric selection criteria for LAEs were obtained with Subaru and Keck II Telescopes, among which 28 were confirmed LAEs, one was a nearby galaxy, and eight were unclassified. We also obtained spectra of another 24 NB816-excess objects in the field, identifying six additional LAEs. We find that the Ly$\alpha$luminosity function derived from the photometric sample is reproduced well by a Schechter function with $L^\star = 7.9^{+3.0}_{-2.2} \times 10^{42} \,\mathrm{erg} \,\mathrm{s}^{-1}$and $\phi^\star = 6.3^{+3.0}_{-2.0} \times 10^{-4} \,\mathrm{Mpc}^{-3}$for $\alpha =-1.5$(fixed) over the whole luminosity range of $L \simeq 3 \times 10^{42} \hbox{--} 3 \times 10^{43} \,\mathrm{erg} \,\mathrm{s}^{-1}$. We then measured the rest-frame Ly$\alpha$equivalent widths for the confirmed LAEs, to find that the median among the 28 objects satisfying the photometric selection criteria is $W_{0}^{\mathrm{i}} = 233 \,{Å}$. We infer that 30%-40% of LAEs at $z=5.7$exceed $W_{0}^{\mathrm{i}} = 240 \,{Å}$. These large-EW objects probably cannot be accounted for by ordinary star-forming populations with a Salpeter IMF. We also find that LAEs with fainter far-UV luminosities have larger EWs. Finally, we derived the far-UV luminosity function of LAEs down to $M_{\mathrm{UV}} \simeq-19.6$using the photometric sample, and compared it with that of Lyman-break galaxies (LBGs). We find that as high as about 80% of LBGs at $z \sim 6$have $W_{0}^{\mathrm{i}} \ge 100 \,{Å}$, in sharp contrast to lower-$z$counterparts.

Published
2006
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292. Clustering of Lyman Break Galaxies at z = 4 and 5 in the Subaru Deep Field: Luminosity Dependence of the Correlation Function Slope

Author

Kashikawa, Nobunari, Yoshida, Makiko, Shimasaku, Kazuhiro, Nagashima, Masahiro, Yahagi, Hideki, Ouchi, Masami, Matsuda, Yuichi, Malkan, Matthew A., Doi, Mamoru, Iye, Masanori, Ajiki, Masaru, Akiyama, Masayuki, Ando, Hiroyasu, Aoki, Kentaro, Furusawa, Hisanori, Hayashino, Tomoki, Iwamuro, Fumihide, Karoji, Hiroshi, Kobayashi, Naoto, Kodaira, Keiichi, Kodama, Tadayuki, Komiyama, Yutaka, Miyazaki, Satoshi, Mizumoto, Yoshihiko, Morokuma, Tomoki, Motohara, Kentaro, Murayama, Takashi, Nagao, Tohru, Nariai, Kyoji, Ohta, Kouji, Okamura, Sadanori, Sasaki, Toshiyuki, Sato, Yasunori, Sekiguchi, Kazuhiro, Shioya, Yasuhiro, Tamura, Hajime, Taniguchi, Yoshiaki, Umemura, Masayuki, Yamada, Toru, and Yasuda, Naoki

Abstract

We explored the clustering properties of Lyman break galaxies at z = 4 and 5 with an angular two-point correlation function on the basis of the very deep and wide Subaru Deep Field data. We confirmed the previous result that the clustering strength of LBGs depends on the UV luminosity in the sense that brighter LBGs are more strongly clustered. In addition, we found an apparent dependence of the correlation function slope on UV luminosity for LBGs at both z = 4 and 5. More luminous LBGs have a steeper correlation function. The bias parameter was found to be a scale-dependent function for bright LBGs, whereas it appears to be almost scale-independent for faint LBGs. Luminous LBGs have a higher bias at smaller angular scales, which decreases as the scale increases. To compare these observational results, we constructed numerical mock LBG catalogs based on a semianalytic model of hierarchical clustering combined with high-resolution N-body simulation, carefully mimicking the observational selection effects. The luminosity functions and the overall correlation functions for LBGs at z = 4 and 5 predicted by this mock catalog were found to be almost consistent with the observation. The observed dependence of the clustering on UV luminosity was not reproduced by the model, unless subsamples of distinct halo mass were considered. That is, LBGs belonging to more massive dark halos had steeper and larger amplitude correlation functions. With this model, we found that LBG multiplicity in massive dark halos amplifies the clustering strength at small scales, which steepens the correlation function. The hierarchical clustering model could therefore be reconciled with the observed luminosity dependence of the correlation function if there is a tight correlation between UV luminosity and halo mass. Our finding that the slope of the correlation function depends on luminosity could be an indication that massive dark halos hosted multiple bright LBGs.

Published
2006

293. The environment of large equivalent width Lyα emitters at z ∼ 3.

Author

Kida, Arisa, Kikuta, Satoshi, Matsuda, Yuichi, Boquien, Médéric, Lusso, Elisabeta, Gruppioni, Carlotta, and Tissera, Patricia

Abstract

We present the environmental properties of a sample of 260 Lyα emitters (LAEs) with extremely large equivalent widths (EW0 > 240 Å) at z ∼ 3. Such large EW LAEs may be very low-metal / young starbursts in void regions or Hi gas /galaxies illuminated by ionizing radiation from the QSO. We undertook Subaru/HSC Lyα imaging observations around a hyper luminous QSO at z = 2.84. We identified 3490 LAEs including 260 large EW LAEs. We found that the large EW LAEs tend to lie at galaxy over-dense regions surrounding the QSO, suggesting that most of the large EW LAEs are illuminated by the QSO. From the radial distribution of the large EW LAEs from the QSO, we found that the fraction of large EW LAE shows two excesses in the range of 2 to 5 Mpc and 14 to 16 Mpc from the QSO. If the two peaks are reflected with the QSO activity, the QSO should have episodic lifetimes with ∼10 Myr duration and ∼30 Myr separations. However, we require future spectroscopic observations to investigate if the large EW LAEs far from the QSO are low-metal young starbursts. [ABSTRACT FROM AUTHOR]

Published
2018
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294. Use of hydrolyzed feather meal for broiler chicks (Department of Animal Husbandry)

Author

Matsuda, Yuichi and Shiroma, Sadao

Abstract

沖縄産フェザー・ミールをブロイラー・ヒナに給与してブロイラー飼料としての価値を調べた。供試した品種は, 白色コーニッシユ×白色ロックのF_1で, 3回に亘り飼育試験を行なった。その結果 : 1.第1回試験では, 標準区(日本飼養標準による配合)は, 動物蛋白質を魚粉のみとした区とフェザー・ミールを前期飼料2%, 後期4%配合した区について発育を調べたが, ヒナの発育はフェザー・ミール配合区が魚粉区よりも良い傾向がみられた。高エネルギー区でも魚粉区を対照区としフェザー・ミールを前期に2%, 後期に5%配合した飼料を試験区として発育を調べたが, 8週齢体重は魚粉区1,909.4g, フェザー・ミール区1,842.5gで魚粉区が67.2gで重かったが有意差はみられなかった。飼料要求率は, 標準区でも, 高エネルギー区でも, フェザー・ミール給与区がやや大きい傾向にあった。2.第2回試験は, 沖縄の最も暑い6月下旬から8月中旬の間に行ない魚粉区を対照区とし, フェザー・ミールを前期後期とも5%配合した区を試験区とし, 発育を比較したが, 餌付後3週間は魚粉区が良く有意差がみられた(P, Three trials were conducted with straight run broiler chicks of White cornish x White Rock for 8 weeks to evaluate hydrolyzed feather meal as a protein source in the ration of growing birds. The compositions of the diets used are shown in Tables 1,2 and 3. The results presented in Tables 4,5 and 6 are summarized as follows : It seems that the suggestive amounts of feather meal in the formulated rations are : (1) in the starter, less than 5% of the diet or below 20% of the total protein and (2) in the finisher, 5% of the ration or 24-25% of the total protein. Also, the older chicks seem to make better use of the feather meal protein as compared with the chicks of 1 to 4 weeks of age., 紀要論文

Published
1974

297. Effect of high energy ration for broiler feeding (Department of Animal Husbandry)

Author

Matsuda, Yuichi

Abstract

ブロイラー・ヒナの成長を促進し, 飼料要求率を少くするために高エネルギー飼料給与の効果について試験を行なった。試験には, ブロイラー専用種の白色コーニッシュと白色ロックのF1を用い, ケージ飼育で試験期間は8週間であった。対照区(標準飼料区)は, 日本飼養標準とNRC飼養標準に推奨されている全養分を充たすように配合した飼料を用いた。高エネルギー区は, 対照区に比しCPとTDNを増加し, 前期飼料のCP23%, TDN70%, 後期飼料CP21%, TDN80%とし, 1ポンドの代謝エネルギー(Cal.)をCPで除した値(ME/P)を前期飼料は60,後期70にした。配合割合と成分は, 表1,2に示した。結果は, 表3,4,5,6,に示される。1.発育 : 試験終了時(56日)体重は, 対照区1,550&acd;1,650gの範囲内にあったが, 高エネルギー区は1,750&acd;1,850gで, 後者が100&acd;200g重く, 両区の間に有意差があった。2.飼料要求率 : 対照区は2.5&acd;2.6の範囲内にあったが高エネルギー区は2.17&acd;2.25で高エネルギー区が勝れているように考えられた。3.飼料費 : 飼料単価は高エネルギー区が高価であったが, 1kg増体に要した飼料費は対照区31.8セント, 高エネルギー区30.8セントで両者の間に1セントの差があり高エネルギー区が安価であった。4回に亘って実施したブロイラー試験の結果から, 高エネルギー飼料が, 発育の促進, 飼料要求率の改善, 飼料費低減の面から有利であると考えられた。4.配合飼料に抗生物質を10ppm配合してもブロイラーの発育促進, 飼料要求率の改善に好結果をもたらすという成績は得られなかった。, The feeding experiments were conducted with broiler chicks to determine the effect of high energy ration for broiler production. The trials were carried out for 8 weeks with straight-run chicks made by crossing White Cornish×White Rock. The chicks were reared in cages. The composition of feeds are shown in tables 1 and 2. The results (Tables 3,4,5 and 6) can be summarized as follows : 1. Gains : Average weight at the end of the test ranged from 1,550g to 1,650g in the control, 1,750g to 1,850g in the high energy ration. The difference between two trials was significant that shows the gain was affected favorably by the high energy ration. 2. Feed conversion ranged from 2.50 to 2.60 in the control, 2.17 to 2.25 in the high energy ration. The data shows that the chicks in the high energy ration consumed less feed than that of the control for gain. 3. Feed cost per kilogram of gain was 31.8 cent in the control, 30.8 cent in the high energy ration. The experiment showed that the high energy ration produced broiler more economically than the control., 紀要論文

Published
1972

299. 沖縄における乳牛の泌乳量について

Author

Matsuda, Yuichi

Subjects
fluids and secretions, food and beverages
Abstract

Studies have been conducted to know the amount of milk produced by Holstein cows: which have been raised on the farm of the university of the Ryukyus, and also to know some factors affected the milk production. Six Holstein cows were used for the studies. On account of the university has no enough land to produce the meadow grass, wild grasses such as miscanthus, imperata cylindrica and panicum repens have been fed chiefly. In addition to the wild grass, napier grass produced in the university farm have been used in summer and sugar cane tops in winter. To furnish the nutrient requirement in adequate amount, the concentrates were added to the roughage. The results were as follows: 1. Average milk production in 305 days of lactation period was 4148.5 kg. 2. As wild grasses were unpalatable and poor quality, the cows did not take the proper amount and then it caused poor milk production. Considering the yield of the milk and the persistency curves of lactations, it can be safe: to say that, as far as the wild grass has been used chiefly as the roughage for milk production, it is difficult to display the cow's milk production ability. 3. In Okinawa, the ascent of the body temperature of Holstein cows begins at the end of April following the ascent of the air temperature and in July, the hottest season, the body temperature of the cows reaches often 40℃ or more with the temperature over 30℃. With the ascent of the body temperature of the cows, the reduction of the milk yields has taken place at the end of April and much reduction in July.

Published
1964

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