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6 results on '"National Astronomical Observatories Japan"'

1. Ionizing radiation from AGNs at z > 3.3 with the Subaru Hyper Suprime-Cam Survey and the CFHT Large Area U-band Deep Survey (CLAUDS)

Author

Guillaume Desprez, Marcin Sawicki, Toshihiro Kawaguchi, Nobunari Kashikawa, Jean Coupon, Stéphane Arnouts, Ikuru Iwata, Genoveva Micheva, Masayuki Akiyama, Akio K. Inoue, Stephen Gwyn, Saint Mary's University [Halifax], Osaka University [Osaka], NAOJ, National Astronomical Observatories Japan, National Research Council of Canada (NRC), Laboratoire d'Astrophysique de Marseille (LAM), 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), Université de Genève = University of Geneva (UNIGE), and University of Geneva [Switzerland]

Subjects
Physics, Photon, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Redshift, Flux ratio, Ionizing radiation, Photometry (optics), 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Emissivity, Continuum (set theory), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract

We use deep and wide imaging data from the CFHT Large Area U-band Deep Survey (CLAUDS) and the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) to constrain the ionizing radiation (Lyman Continuum; LyC) escape fraction from AGNs at $z \sim 3 - 4$. For 94 AGNs with spectroscopic redshifts at $3.3 < z < 4.0$, we use their U-band / i-band flux ratios to estimate LyC transmission of individual AGNs. The distribution of their LyC transmission shows values lower than the range of LyC transmission values for IGM of the same redshift range, which suggests that LyC escape fraction of AGNs at $z>3.3$ is considerably lower than unity in most cases. We do not find any trend in LyC transmission values depending on their UV luminosities. Based on the photometry of stacked images we find the average flux ratio of LyC and non-ionizing UV photons escaping from the objects $(f_{LyC}/f_{UV})^{out} = 0.182 \pm 0.043$ for AGNs at $3.3, Comment: 19 pages, 12 figures. Accepted for publication in Monthly Notices of the Royal Astronomical Society

Published
2022

2. Multi-epoch Direct Imaging and Time-Variable Scattered Light Morphology of the HD 163296 Protoplanetary Disk

Author

Rich, Evan A., Wisniewski, John P., Currie, Thayne, Fukagawa, Misato, Grady, Carol A., Sitko, Michael L., Pikhartova, Monika, Abe, Lyu, Brandner, Wolfgang, Brandt, Timothy D., Carson, Joseph C., Chilcote, Jeffrey, Dong, Ruobing, Feldt, Markus, Groff, Tyler, Guyon, Olivier, Henning, Thomas, Hodapp, Klaus W., Janson, Markus, Jovanovic, Nemanja, Kasdin, Jeremy, Knapp, Gillian R., Lozi, Julien, Martinache, Frantz, McElwain, Michael W., Moro-Martin, Amaya, Pyo, Tae-Soo, Serabyn, Eugene, Russel, Ray W., Takami, Michihiro, Thalmann, Christian, Turner, Edwin L., Uyama, Taichi, Wagner, Kevin R., Hashimoto, Jun, Goto, Miwa, Hayano, Yutaka, Hayashi, Masahiko, Hayashi, Saeko S., Ishii, Miki, Iye, Masanori, Kandori, Ryo, Kudo, Tomoyuki, Kusakabe, Nobuhiko, Kuzuhara, Masayuki, Kwon, Jungmi, Matsuo, Taro, Mayama, Satoshi, Miyama, Shoken, Morino, Jun-Ichi, Nakagawa, Takao, Nishimura, Tetsuo, Suto, Hiroshi, Suzuki, Ryuji, Takato, Naruhisa, Terada, Hiroshi, Watanabe, Makoto, Yamada, Toru, Takami, Hideki, Usuda, Tomonori, Tamura, Motohide, NASA Goddard Space Flight Center (GSFC), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Steward Observatory, University of Arizona, Département Sciences de la Fabrication et Logistique (SFL-ENSMSE), École des Mines de Saint-Étienne (Mines Saint-Étienne MSE), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-CMP-GC, Department of Earth System Science and Technology [Fukuoka] (ESST), Kyushu University [Fukuoka], Department of Computer Science [ETH Zürich] (D-INFK), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Subaru Telescope, National Astronomical Observatory of Japan (NAOJ), NAOJ, National Astronomical Observatories Japan, Institut méditerranéen de biodiversité et d'écologie marine et continentale (IMBE), Avignon Université (AU)-Aix Marseille Université (AMU)-Institut de recherche pour le développement [IRD] : UMR237-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Academia Sinica, Institute of Astronomy [ETH Zürich], Department of Physics [ETH Zürich] (D-PHYS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich)- Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Graduate School of Life and Environmental Sciences, University of Tsukuba, Université de Tsukuba = University of Tsukuba, Faculty of Science and Engineering [Waseda], Waseda University, Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Kyushu University, and Waseda University [Tokyo, Japan]

Subjects
planets and satellites: detection, Brightness, 010504 meteorology & atmospheric sciences, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Protoplanetary disk, 01 natural sciences, Observatory, Planet, 0103 physical sciences, Spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, [PHYS]Physics [physics], Earth and Planetary Astrophysics (astro-ph.EP), Physics, Atmospheric models, protoplanetary disks, Astronomy and Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Protoplanet, Astrophysics - Earth and Planetary Astrophysics
Abstract

著者人数: 61名, Accepted: 2019-03-07, 資料番号: SA1190032000

Published
2019

3. SILVERRUSH. V. Census of Ly α , [O iii] λ 5007, H α , and [C ii] 158 μ m Line Emission with ∼1000 LAEs at z = 4.9–7.0 Revealed with Subaru/HSC

Author

Ryohei Itoh, Akio K. Inoue, Olivier Ilbert, Takatoshi Shibuya, Sune Toft, Masami Ouchi, Gustavo Bruzual, Yuichi Harikane, Takashi Kojima, Yoshiaki Ono, Michael Rauch, Iary Davidzon, Peter Capak, Yoshiki Matsuoka, Andreas L. Faisst, Haibin Zhang, Tohru Nagao, Jacopo Chevallard, Masato Onodera, John D. Silverman, Ryo Higuchi, Stéphane Charlot, Seiji Fujimoto, Miftahul Hilmi, Crystal L. Martin, Chien-Hsiu Lee, Institute for Cosmic Ray Research, The University of Tokyo, Institute for Cosmic Ray Research (ICRR), The University of Tokyo (UTokyo), NAOJ, National Astronomical Observatories Japan, Osaka University [Osaka], HE Space Operations BV for ESA/ESTEC, California Institute of Technology (CALTECH), Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, Laboratoire d'Astrophysique de Marseille (LAM), 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), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), and Universidad Nacional Autónoma de México (UNAM)

Subjects
Physics, [PHYS]Physics [physics], 010308 nuclear & particles physics, Star formation, Metallicity, Doubly ionized oxygen, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Luminosity, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Equivalent width, Line (formation)
Abstract

We investigate Lya, [OIII]5007, Ha, and [CII]158um emission from 1124 galaxies at z=4.9-7.0. Our sample is composed of 1092 Lya emitters (LAEs) at z=4.9, 5.7, 6.6, and 7.0 identified by Subaru/Hyper Suprime-Cam (HSC) narrowband surveys covered by Spitzer large area survey with Subaru/HSC (SPLASH) and 34 galaxies at z=5.148-7.508 with deep ALMA [CII]158um data in the literature. Fluxes of strong rest-frame optical lines of [OIII] and Ha (Hb) are constrained by significant excesses found in the SPLASH 3.6 and 4.5um photometry. At z=4.9, we find that the rest-frame Ha equivalent width and the Lya escape fraction f_Lya positively correlate with the rest-frame Lya equivalent width EW^0_Lya. The f_Lya-EW^0_Lya correlation is similarly found at z~0-2, suggesting no evolution of the correlation over z~0-5. The typical ionizing photon production efficiency of LAEs is logxi_ion/[Hz erg^-1]~25.5 significantly (60-100%) higher than those of LBGs at a given UV magnitude. At z=5.7-7.0, there exists an interesting turn-over trend that the [OIII]/Ha flux ratio increases in EW^0_Lya~0-30 A, and then decreases out to EW^0_Lya~130 A. We also identify an anti-correlation between a [CII] luminosity to star-formation rate ratio (L_[CII]/SFR) and EW^0_Lya at the >99% confidence level. We carefully investigate physical origins of the correlations with stellar-synthesis and photoionization models, and find that a simple anti-correlation between EW_Lya^0 and metallicity explains self-consistently all of the correlations of Lya, Ha, [OIII]/Ha, and [CII] identified in our study, indicating detections of metal-poor (~0.03 Zo) galaxies with EW^0_Lya~200 A., 24 pages, 21 figures, accepted in ApJ

Published
2018

4. SPLASH-SXDF Multi-wavelength Photometric Catalog

Author

Vihang Mehta, Claudia Scarlata, Peter Capak, Iary Davidzon, Andreas Faisst, Bau Ching Hsieh, Olivier Ilbert, Matt Jarvis, Clotilde Laigle, John Phillips, John Silverman, Michael A. Strauss, Masayuki Tanaka, Rebecca Bowler, Jean Coupon, Sébastien Foucaud, Shoubaneh Hemmati, Daniel Masters, Henry Joy McCracken, Bahram Mobasher, Masami Ouchi, Takatoshi Shibuya, Wei-Hao Wang, AUTRES, California Institute of Technology (CALTECH), Laboratoire d'Astrophysique de Marseille (LAM), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Space Telescope Science Institute (STSci), Institute for Cosmic Ray Research (ICRR), The University of Tokyo (UTokyo), NAOJ, and National Astronomical Observatories Japan

Subjects
Physics, [PHYS]Physics [physics], Splash, 010308 nuclear & particles physics, Hubble Deep Field, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Photometry (optics), [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Outlier, Median absolute deviation, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Reference frame
Abstract

We present a multi-wavelength catalog in the Subaru-XMM Deep Field (SXDF) as part of the Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH). We include the newly acquired optical data from the Hyper-Suprime Cam Subaru Strategic Program, accompanied by IRAC coverage from the SPLASH survey. All available optical and near-infrared data is homogenized and resampled on a common astrometric reference frame. Source detection is done using a multi-wavelength detection image including the $u$-band to recover the bluest objects. We measure multi-wavelength photometry and compute photometric redshifts as well as stellar masses for $\sim$1.17 million objects over $\sim$4.2 deg$^2$ with $\sim$800,000 objects in the 2.4 deg$^2$ HSC-UltraDeep coverage. Using the available spectroscopic redshifts from various surveys over the range of $0, Comment: 23 pages, 15 figures; accepted for publication in ApJS; comments welcome

Published
2017
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5. A new constraint on the lyα fraction of uv very bright galaxies at redshift 7

Author

Naoki Yasuda, K. Sekiguchi, Yoshiaki Naito, James Dunlop, Kazuhiro Shimasaku, Yuki Okura, Junko Furusawa, Johan P. U. Fynbo, Hisanori Furusawa, Yoshiaki Taniguchi, Toru Yamada, Olivier Le Fevre, Masaru Kajisawa, Masami Ouchi, Tadafumi Takata, Nobunari Kashikawa, Fumiaki Nakata, Masakazu A. R. Kobayashi, NAOJ, National Astronomical Observatories Japan, University of Edinburgh, National Astronomical Observatory of Japan (NAOJ), Faculty of Science and Engineering [Waseda], Waseda University, Department of Civil Engineering, Chuo University (Chuo University), 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), European Project: 267117,EC:FP7:ERC,ERC-2010-AdG_20100224,DARK(2011), Waseda University [Tokyo, Japan], and 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)

Subjects
Physics, 010308 nuclear & particles physics, Cosmology: observations, Galaxies: high-redshift, Galaxies: evolution, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Redshift, Galaxy, Reionization, Space and Planetary Science, Dark ages, 0103 physical sciences, Dark Ages, Alpha decay, Spectroscopy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Equivalent width, Astrophysics - Cosmology and Nongalactic Astrophysics, Line (formation), First stars
Abstract

We study the extent to which very bright (-23.0 < MUV < -21.75) Lyman-break selected galaxies at redshifts z~7 display detectable Lya emission. To explore this issue, we have obtained follow-up optical spectroscopy of 9 z~7 galaxies from a parent sample of 24 z~7 galaxy candidates selected from the 1.65 sq.deg COSMOS-UltraVISTA and SXDS-UDS survey fields using the latest near-infrared public survey data, and new ultra-deep Subaru z'-band imaging (which we also present and describe in this paper). Our spectroscopy has yielded only one possible detection of Lya at z=7.168 with a rest-frame equivalent width EW_0 = 3.7 (+1.7/-1.1) Angstrom. The relative weakness of this line, combined with our failure to detect Lya emission from the other spectroscopic targets allows us to place a new upper limit on the prevalence of strong Lya emission at these redshifts. For conservative calculation and to facilitate comparison with previous studies at lower redshifts, we derive a 1-sigma upper limit on the fraction of UV bright galaxies at z~7 that display EW_0 > 50 Angstrom, which we estimate to be < 0.23. This result may indicate a weak trend where the fraction of strong Lya emitters ceases to rise, and possibly falls between z~6 and z~7. Our results also leave open the possibility that strong Lya may still be more prevalent in the brightest galaxies in the reionization era than their fainter counterparts. A larger spectroscopic sample of galaxies is required to derive a more reliable constraint on the neutral hydrogen fraction at z~7 based on the Lya fraction in the bright galaxies., Comment: 20 pages, 7 figures, accepted for publication in ApJ

Published
2016

6. A search for z= 7.3 Lyα emitters behind gravitationally lensing clusters

Author

Ota, Kazuaki, Richard, Johan, Iye, Masanori, Shibuya, Takatoshi, Egami, Eiichi, Kashikawa, Nobunari, NAOJ, National Astronomical Observatories Japan, Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Steward Observatory, University of Arizona, École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], galaxies: high-redshift, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], cosmology: observations, early Universe, galaxies: evolution, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We searched for z=7.3 Lya emitters (LAEs) behind two lensing clusters, Abell 2390 and CL 0024, with the Subaru Telescope Suprime-Cam and a narrowband NB1006 (FWHM ~ 21 nm centered at 1005 nm). We investigated if there exist objects consistent with the color of z=7.3 LAEs behind the clusters but could not detect any LAEs to the unlensed line limit F(Lya) ~ 6.9 x 10^{-18} erg/s/cm^2. Using several z=7 Lya luminosity functions (LFs) from the literature, we estimated and compared the expected detection numbers of z ~ 7 LAEs in lensing and blank field surveys in the case of using an 8m class ground based telescope. Given the steep bright-end slope of the LFs, when the detector field-of view (FOV) is comparable to the angular extent of a massive lensing cluster, imaging cluster(s) is more efficient in detecting z ~ 7 LAEs than imaging a blank field. However, the gain is expected to be modest, a factor of two at most and likely much less depending on the adopted LFs. The main advantage of lensing-cluster survey, therefore, remains to be the gain in depth and not necessarily in detection efficiency. For much larger detectors, the lensing effect becomes negligible and the efficiency of LAE detection is proportional to the instrumental FOV. We also inspected NB1006 images of three z ~ 7 z-dropouts previously detected in Abell 2390 and found that none of them are detected in NB1006. Two of them are consistent with predictions from the previous studies that they would be at lower redshifts. The other one has a photometric redshift of z ~ 7.3, and if it is at z=7.3, its unlensed Lya line flux would be very faint: F(Lya) < 4.4 x 10^{-18} erg/s/cm^2 (1 sigma upper limit) or rest frame equivalent width of W(Lya) < 26A. Its Lya emission might be attenuated by neutral hydrogen, as recent studies show that the fraction of Lyman break galaxies displaying strong Lya emission is lower at z ~ 7 than at z, Comment: Abstract has been replaced; accepted for publication in Monthly Notices of the Royal Astronomical Society on April 11, 2012

Published
2012

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