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32 results on '"C. Carilli"'

1. Simulations of primary beam effects on the cosmic bispectrum phase observed with the Hydrogen Epoch of Reionization Array

Author

N Charles, G Bernardi, H L Bester, O M Smirnov, C Carilli, P M Keller, N Kern, B Nikolic, N Thyagarajan, E de Lera Acedo, N Fagnoni, M G Santos, USA, GBR, and ZAF

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The 21 cm transition from neutral hydrogen promises to be the best observational probe of the epoch of reionization (EoR). The main difficulty in measuring the 21 cm signal is the presence of bright foregrounds that require very accurate interferometric calibration. Closure quantities may circumvent the calibration requirements but may be, however, affected by direction-dependent effects, particularly antenna primary beam responses. This work investigates the impact of antenna primary beams affected by mutual coupling on the closure phase and its power spectrum. Our simulations show that primary beams affected by mutual coupling lead to a leakage of foreground power into the EoR window, which can be up to ∼104 times higher than the case where no mutual coupling is considered. This leakage is, however, essentially confined at k

Published
2022
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2. The 700 ks Chandra Spiderweb Field:II. Evidence for inverse-Compton and thermal diffuse emission in the Spiderweb galaxy

Author

P. Tozzi, R. Gilli, A. Liu, S. Borgani, M. Lepore, L. Di Mascolo, A. Saro, L. Pentericci, C. Carilli, G. Miley, T. Mroczkowski, M. Pannella, E. Rasia, P. Rosati, C. S. Anderson, A. Calabró, E. Churazov, H. Dannerbauer, C. Feruglio, F. Fiore, R. Gobat, S. Jin, M. Nonino, C. Norman, and H. J. A. Röttgering

Subjects
Galaxies: Clusters: Intracluster Medium, X-Rays: Galaxies: Clusters, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, clusters: intracluster medium [Galaxies], galaxies: clusters [X-rays], clusters: general [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxies: Clusters: General
Abstract

We present the X-ray imaging and spectral analysis of the diffuse emission around the Spiderweb galaxy at z=2.16 and of its nuclear emission, based on a deep (700 ks) Chandra observation. We characterize the nuclear emission and computed the contamination in the surrounding regions due to the wings of the instrument PSF. Then, we quantified the extended emission within 12". We find that the Spiderweb galaxy hosts a mildly absorbed quasar, with modest yet significant variability on a timescale of ~1 year. We find that the emission in the jet regions is well described by a power law with Gamma~2-2.5, and it is consistent with IC upscattering of the CMB photons by the relativistic electrons. We also find a roughly symmetric, diffuse emission within a radius of ~100 kpc. This emission is consistent with thermal bremsstrahlung from a hot ICM with a temperature of kT=2.0_{-0.4}^{+0.7} keV, and a metallicity of Z, 19 pages, 16 figures, accepted in Astronomy & Astrophysics

Published
2022
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3. Detection of microgauss coherent magnetic fields in a galaxy five billion years ago

Author

Rainer Beck, Bryan Gaensler, Charles R. Keeton, Ellen G. Zweibel, C. Carilli, S. A. Mao, Olaf Wucknitz, Aritra Basu, and Phil Kronberg

Subjects
Physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Billion years, Galaxy, Redshift, Magnetic field, Radio telescope, Interstellar medium, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Dynamo theory, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dynamo
Abstract

Magnetic fields play a pivotal role in the physics of interstellar medium in galaxies, but there are few observational constraints on how they evolve across cosmic time. Spatially resolved synchrotron polarization maps at radio wavelengths reveal well-ordered large-scale magnetic fields in nearby galaxies that are believed to grow from a seed field via a dynamo effect. To directly test and characterize this theory requires magnetic field strength and geometry measurements in cosmologically distant galaxies, which are challenging to obtain due to the limited sensitivity and angular resolution of current radio telescopes. Here, we report the cleanest measurements yet of magnetic fields in a galaxy beyond the local volume, free of the systematics traditional techniques would encounter. By exploiting the scenario where the polarized radio emission from a background source is gravitationally lensed by a foreground galaxy at z = 0.439 using broadband radio polarization data, we detected coherent $\mu$G magnetic fields in the lensing disk galaxy as seen 4.6 Gyrs ago, with similar strength and geometry to local volume galaxies. This is the highest redshift galaxy whose observed coherent magnetic field property is compatible with a mean-field dynamo origin., Comment: 29 pages, 5 figures (including Supplementary Information). Published in Nature Astronomy on August 28, 2017

Published
2017
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4. The VLA-COSMOS 3 GHz Large Project: The infrared-radio correlation of star-forming galaxies and AGN to z ≲ 6

Author

J. Delhaize, V. Smolčić, I. Delvecchio, M. Novak, M. Sargent, N. Baran, B. Magnelli, G. Zamorani, E. Schinnerer, E. J. Murphy, M. Aravena, S. Berta, M. Bondi, P. Capak, C. Carilli, P. Ciliegi, F. Civano, O. Ilbert, A. Karim, C. Laigle, O. Le Fèvre, S. Marchesi, H. J. McCracken, M. Salvato, N. Seymour, and L. Tasca

Subjects
Active galactic nucleus, PRIRODNE ZNANOSTI. Fizika. Astronomija i astrofizika, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], 01 natural sciences, Luminosity, Jansky, 0103 physical sciences, NATURAL SCIENCES. Physics. Astronomy and Astrophysics, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, galaxies: evolution, galaxies: star formation, radio continuum: galaxies, infrared: galaxies, evolution [galaxies], Astrophysics::Galaxy Astrophysics, QB, Physics, education.field_of_study, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies [radio continuum], Galaxy, Redshift, Space and Planetary Science, Spectral energy distribution, star formation [galaxies]
Abstract

We examine the behaviour of the infrared-radio correlation (IRRC) over the range 0 2 COSMOS field. We distinguish between objects where emission is believed to arise solely from star-formation, and those where an active galactic nucleus (AGN) is thought to be present. We account for non-detections in the radio or in the infrared using a doubly-censored survival analysis. We find that the IRRC of star-forming galaxies, quantified by the infrared-to-1.4 GHz radio luminosity ratio (qTIR), decreases with increasing redshift: qTIR(z) = (2.88 ± 0.03)(1 + z)- 0.19 ± 0.01. This is consistent with several previous results from the literature. Moderate-to-high radiative luminosity AGN do not follow the same qTIR(z) trend as star-forming galaxies, having a lower normalisation and steeper decrease with redshift. We cannot rule out the possibility that unidentified AGN contributions only to the radio regime may be steepening the observed qTIR(z) trend of the star-forming galaxy population. We demonstrate that the choice of the average radio spectral index directly affects the normalisation, as well as the derived trend with redshift of the IRRC. An increasing fractional contribution to the observed 3 GHz flux by free-free emission of star-forming galaxies may also affect the derived evolution. However, we find that the standard (M82-based) assumption of the typical radio spectral energy distribution (SED) for star-forming galaxies is inconsistent with our results. This suggests a more complex shape of the typical radio SED for star-forming galaxies, and that imperfect K corrections in the radio may govern the derived trend of decreasing qTIR with increasing redshift. A more detailed understanding of the radio spectrum is therefore required for robust K corrections in the radio and to fully understand the cosmic evolution of the IRRC. Lastly, we present a redshift-dependent relation between rest-frame 1.4 GHz radio luminosity and star formation rate taking the derived redshift trend into account.

Published
2017

5. The 2014 ALMA Long Baseline Campaign: An Overview

Author

ALMA Partnership, E. B. Fomalont, C. Vlahakis, S. Corder, A. Remijan, D. Barkats, R. Lucas, T. R. Hunter, C. L. Brogan, Y. Asaki, S. Matsushita, W. R. F. Dent, R. E. Hills, N. Phillips, A. M. S. Richards, P. Cox, R. Amestica, D. Broguiere, W. Cotton, A. S. Hales, R. Hiriart, A. Hirota, J. A. Hodge, C. M. V. Impellizzeri, J. Kern, R. Kneissl, E. Liuzzo, N. Marcelino, R. Marson, A. Mignano, K. Nakanishi, B. Nikolic, J. E. Perez, L. M. Pérez, I. Toledo, R. Aladro, B. Butler, J. Cortes, P. Cortes, V. Dhawan, J. Di Francesco, D. Espada, F. Galarza, D. Garcia-Appadoo, L. Guzman-Ramirez, E. M. Humphreys, T. Jung, S. Kameno, R. A. Laing, S. Leon, J. Mangum, G. Marconi, H. Nagai, L.-A. Nyman, M. Radiszcz, J. A. Rodón, T. Sawada, S. Takahashi, R. P. J. Tilanus, T. van Kempen, B. Vila Vilaro, L. C. Watson, T. Wiklind, F. Gueth, K. Tatematsu, A. Wootten, A. Castro-Carrizo, E. Chapillon, G. Dumas, I. de Gregorio-Monsalvo, H. Francke, J. Gallardo, J. Garcia, S. Gonzalez, J. E. Hibbard, T. Hill, T. Kaminski, A. Karim, M. Krips, Y. Kurono, C. Lopez, S. Martin, L. Maud, F. Morales, V. Pietu, K. Plarre, G. Schieven, L. Testi, L. Videla, E. Villard, N. Whyborn, M. A. Zwaan, F. Alves, P. Andreani, A. Avison, M. Barta, F. Bedosti, G. J. Bendo, F. Bertoldi, M. Bethermin, A. Biggs, J. Boissier, J. Brand, S. Burkutean, V. Casasola, J. Conway, L. Cortese, B. Dabrowski, T. A. Davis, M. Diaz Trigo, F. Fontani, R. Franco-Hernandez, G. Fuller, R. Galvan Madrid, A. Giannetti, A. Ginsburg, S. F. Graves, E. Hatziminaoglou, M. Hogerheijde, P. Jachym, I. Jimenez Serra, M. Karlicky, P. Klaasen, M. Kraus, D. Kunneriath, C. Lagos, S. Longmore, S. Leurini, M. Maercker, B. Magnelli, I. Marti Vidal, M. Massardi, A. Maury, S. Muehle, S. Muller, T. Muxlow, E. O’Gorman, R. Paladino, D. Petry, J. Pineda, S. Randall, J. S. Richer, A. Rossetti, A. Rushton, K. Rygl, A. Sanchez Monge, R. Schaaf, P. Schilke, T. Stanke, M. Schmalzl, F. Stoehr, S. Urban, E. van Kampen, W. Vlemmings, K. Wang, W. Wild, Y. Yang, S. Iguchi, T. Hasegawa, M. Saito, J. Inatani, N. Mizuno, S. Asayama, G. Kosugi, K.-I. Morita, K. Chiba, S. Kawashima, S. K. Okumura, N. Ohashi, R. Ogasawara, S. Sakamoto, T. Noguchi, Y.-D. Huang, S.-Y. Liu, F. Kemper, P. M. Koch, M.-T. Chen, Y. Chikada, M. Hiramatsu, D. Iono, M. Shimojo, S. Komugi, J. Kim, A.-R. Lyo, E. Muller, C. Herrera, R. E. Miura, J. Ueda, J. Chibueze, Y.-N. Su, A. Trejo-Cruz, K.-S. Wang, H. Kiuchi, N. Ukita, M. Sugimoto, R. Kawabe, M. Hayashi, S. Miyama, P. T. P. Ho, N. Kaifu, M. Ishiguro, A. J. Beasley, S. Bhatnagar, J. A. Braatz III, D. G. Brisbin, N. Brunetti, C. Carilli, J. H. Crossley, L. D’Addario, J. L. Donovan Meyer, D. T. Emerson, A. S. Evans, P. Fisher, K. Golap, D. M. Griffith, A. E. Hale, D. Halstead, E. J. Hardy, M. C. Hatz, M. Holdaway, R. Indebetouw, P. R. Jewell, A. A. Kepley, D.-C. Kim, M. D. Lacy, A. K. Leroy, H. S. Liszt, C. J. Lonsdale, B. Matthews, M. McKinnon, B. S. Mason, G. Moellenbrock, A. Moullet, S. T. Myers, J. Ott, A. B. Peck, J. Pisano, S. J. E. Radford, W. T. Randolph, U. Rao Venkata, M. G. Rawlings, R. Rosen, S. L. Schnee, K. S. Scott, N. K. Sharp, K. Sheth, R. S. Simon, T. Tsutsumi, S. J. Wood, National Radio Astronomy Observatory (NRAO), Joint ALMA Observatory (JAO), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Institute for Ethnomedicine, University of Wyoming (UW), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Chimie des métaux de transition et catalyse (CMTC), Centre National de la Recherche Scientifique (CNRS)-Université Louis Pasteur - Strasbourg I, Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Institut Jacques Monod (IJM (UMR_7592)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ESO, European Southern Observatory (ESO), Department of Organic and Polymeric Materials, Tokyo Institute of Technology [Tokyo] (TITECH), Biogeochemistry Research Centre, School of Chemistry, Onsala Space Observatory, Chalmers University of Technology [Göteborg], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), AMOR 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Departamento de Analisis Matematico, Universidad de Málaga [Málaga] = University of Málaga [Málaga], Unité de recherche Zoologie Forestière (URZF), Institut National de la Recherche Agronomique (INRA), IFP Energies nouvelles (IFPEN), Fastopt GmbH, D-20357 Hamburg, Germany, Mathématiques Appliquées Paris 5 (MAP5 - UMR 8145), Université Paris Descartes - Paris 5 (UPD5)-Institut National des Sciences Mathématiques et de leurs Interactions (INSMI)-Centre National de la Recherche Scientifique (CNRS), Departament de Ecologia, Universitat d'Alacant, Centro de Estudios Ambientales del Mediterraneo, INAF - Osservatorio Astrofisico di Arcetri (OAA), Faculty of Medicine, Universidad de Chile = University of Chile [Santiago] (UCHILE), Université Pierre et Marie Curie - Paris 6 (UPMC), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition (ICAN), Université Pierre et Marie Curie - Paris 6 (UPMC)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Laboratoire de génie électrique de Paris (LGEP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Ecole Supérieure d'Electricité - SUPELEC (FRANCE)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Max-Planck-Institut für Radioastronomie (MPIFR), Northern Illinois University (NORTHERN ILLINOIS UNIVERSITY), Northern Illinois University, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], foreign laboratories (FL), CERN [Genève], Departements of Medicine and Microbiology, University of Alabama [Tuscaloosa] (UA), Swinburne University of Technology (Hawthorn campus), San Pedro de Atacama Celestial Explorations (SPACE), San Pedro de Atacama Celestial Explorations, General Electric Medical Systems [Buc] (GE Healthcare), General Electric Medical Systems, Laboratoire de Radiopathologie (LRP), Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de la Santé et de la Recherche Médicale (INSERM), Università degli Studi di Milano [Milano] (UNIMI), Altération génétique des cancers, chimioprévention et réponse thérapeutique, Physikalisches Institut [Köln], Universität zu Köln, Ministère de la santé, National Astronomical Observatory of Japan (NAOJ), National Institute for Materials Science (NIMS), Espaces acoustiques et cognitifs (EAC), Sciences et Technologies de la Musique et du Son (STMS), Institut de Recherche et Coordination Acoustique/Musique (IRCAM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche et Coordination Acoustique/Musique (IRCAM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Mathématiques et Applications - ENS Paris (DMA), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Chemistry and Biochemistry [Bern], University of Bern, Academia Sinica, Department of Marine Organic Biogeochemistry, Royal Netherlands Institute for Sea Research (NIOZ), Faculty of Geosciences, Utrecht University, Faculty of Geosciences, Brain Mind Institute (BMI - EPFL), Ecole Polytechnique Fédérale de Lausanne (EPFL), Departamento de Ingenieria Eléctrica (DIE), Universidad de Concepción [Chile], Laboratório de Bioinformática, Embrapa Recursos Genéticos e Biotecnologia, Graduate School of Engineering [The Univ of Tokyo] (UTokyo), The University of Tokyo (UTokyo), Kyushu University [Fukuoka], Mitsubishi Research Institute, Inc., Department of Computer Science and Automation [Bangalore] (CSA), Indian Institute of Science [Bangalore] (IISc Bangalore), National Radio Astronomy Observatory [Socorro] (NRAO), Occupational Physiology Laboratory (Vandœuvre-Les -Nancy, France), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, University College of London [London] (UCL), Centre for Atmospheric Chemistry [Wollongong] (CAC), University of Wollongong [Australia], Safety science group, Delft University of Technology (TU Delft), Centre d'Investigation Clinique - Innovation Technologique - INSERM - CHU de Grenoble (CIC-IT Grenoble (CIT803)), CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Grenoble Alpes (UGA), Northern Research Station, Forest Research [Great Britain], Department of Helsinki Institute for Information Technology Communications and Networking, Aalto University, University of Washington [Seattle], Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de la Santé et de la Recherche Médicale (INSERM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Research Unit on Cardiovascular and Metabolic Diseases (ICAN), Università degli Studi di Milano = University of Milan (UNIMI), Universität zu Köln = University of Cologne, Universidad de Concepción - University of Concepcion [Chile], Kyushu University, Istituto di Radioastronomia (IRA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Universidad de Málaga [Málaga], Unité de recherche Zoologie Forestière (UZF), Science et Technologie du Lait et de l'Oeuf (STLO), Institut National de la Recherche Agronomique (INRA)-AGROCAMPUS OUEST, Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Mathématiques et de leurs Interactions (INSMI)-Université Paris Descartes - Paris 5 (UPD5), University of Chile [Santiago], Université Pierre et Marie Curie - Paris 6 (UPMC)-Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [APHP], Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-SUPELEC-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Jodrell Bank Centre for Astrophysics, School of Physics, Università degli studi di Milano [Milano], National Institute of Materials Science, Equipe Espaces acoustiques et cognitifs, Université Pierre et Marie Curie - Paris 6 (UPMC)-IRCAM-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-IRCAM-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, Graduate School of Engineering [Tokyo], The University of Tokyo, Center for Atmospheric Chemistry [Wollongong] (CAC), University of Wollongong, CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Joseph Fourier - Grenoble 1 (UJF), Forest Research, Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), École normale supérieure - Paris (ENS Paris), Université Grenoble Alpes (UGA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Grenoble, Joint ALMA Office (JAO), ALMA, Institut Jacques Monod (IJM), Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Mathématiques et de leurs Interactions-Université Paris Descartes - Paris 5 (UPD5), ALMA Observatory, Laboratoire d'analyse et d'architecture des systèmes [Toulouse] (LAAS), Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UPS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique [Toulouse] (INP), Center for Brain Simulation, Ecole Polytechnique Fédérale de Lausanne, Université Joseph Fourier - Grenoble 1 (UJF)-CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM), National Radio Astronomy Observatory ( NRAO ), Joint ALMA Office ( JAO ), University of Wyoming ( UW ), Max-Planck-Institut für Astronomie ( MPIA ), Chimie des métaux de transition et catalyse ( CMTC ), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique ( CNRS ), Istituto di Radioastronomia ( IRA ), Istituto Nazionale di Astrofisica ( INAF ), Institut Jacques Monod ( IJM ), Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), European Southern Observatory ( ESO ), Tokyo Institute of Technology [Tokyo] ( TITECH ), Institut de RadioAstronomie Millimétrique ( IRAM ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Unité de recherche Zoologie Forestière ( UZF ), Institut National de la Recherche Agronomique ( INRA ), IFP Energies nouvelles ( IFPEN ), Science et Technologie du Lait et de l'Oeuf ( STLO ), Institut National de la Recherche Agronomique ( INRA ) -AGROCAMPUS OUEST, Mathématiques Appliquées à Paris 5 ( MAP5 - UMR 8145 ), Université Paris Descartes - Paris 5 ( UPD5 ) -Institut National des Sciences Mathématiques et de leurs Interactions-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition ( ICAN ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Assistance publique - Hôpitaux de Paris (AP-HP)-Institut National de la Santé et de la Recherche Médicale ( INSERM ) -CHU Pitié-Salpêtrière [APHP], Laboratoire de génie électrique de Paris ( LGEP ), Université Paris-Sud - Paris 11 ( UP11 ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -SUPELEC-Centre National de la Recherche Scientifique ( CNRS ), Czech Academy of Sciences [Prague] ( ASCR ), Max-Planck-Institut für Radioastronomie ( MPIFR ), Northern Illinois University ( NORTHERN ILLINOIS UNIVERSITY ), Canadian Space Agency, foreign laboratories ( FL ), University of Alabama [Tuscaloosa] ( UA ), San Pedro de Atacama Celestial Explorations ( SPACE ), General Electric Medical Systems [Buc] ( GE Healthcare ), Laboratoire de Radiopathologie ( LRP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ), Max Planck Institute for Biochemistry, Max-Planck-Institut, Department of Virology, Global COE Program, Nagasaki University-Institute of Tropical Medicine, Sciences et Technologies de la Musique et du Son ( STMS ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -IRCAM-Centre National de la Recherche Scientifique ( CNRS ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -IRCAM-Centre National de la Recherche Scientifique ( CNRS ), Département de Mathématiques et Applications - ENS Paris ( DMA ), École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Centre National de la Recherche Scientifique ( CNRS ) -Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Institut National Polytechnique [Toulouse] ( INP ), Royal Netherlands Institute for Sea Research ( NIOZ ), Departamento de Ingenieria Eléctrica ( DIE ), AUTRES, Department of Computer Science and Automation [Bangalore] ( CSA ), Indian Institute of Science [Bangalore] ( IISc Bangalore ), National Radio Astronomy Observatory [Socorro] ( NRAO ), Computational Science and Engineering Department [Daresbury] ( STFC ), University College of London [London] ( UCL ), Center for Atmospheric Chemistry [Wollongong] ( CAC ), Delft University of Technology ( TU Delft ), Service Hématologie, Hôpital Morvan [Brest]-Centre Hospitalier Régional Universitaire de Brest ( CHRU Brest ), Centre d'Investigation Clinique - Innovation Technologique - INSERM - CHU de Grenoble ( CIC-IT Grenoble (CIT803) ), and Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre Hospitalier Universitaire de Grenoble

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], techniques: high angular resolution, Astronomy and Astrophysics, submillimeter: general, telescopes, Submillimeter Array, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, techniques: interferometric, Environmental science, Millimeter, Baseline (configuration management), instrumentation: interferometers, QB, Remote sensing
Abstract

著者人数: 248名, Accepted: 2015-04-10, 資料番号: SA1150145000

Published
2015
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6. The First Release COSMOS Optical and Near-IR Data and Catalog

Author

P. Capak, H. Aussel, M. Ajiki, H. J. McCracken, B. Mobasher, N. Scoville, P. Shopbell, Y. Taniguchi, D. Thompson, S. Tribiano, S. Sasaki, A. W. Blain, M. Brusa, C. Carilli, A. Comastri, C. M. Carollo, P. Cassata, J. Colbert, R. S. Ellis, M. Elvis, M. Giavalisco, W. Green, L. Guzzo, G. Hasinger, O. Ilbert, C. Impey, K. Jahnke, J. Kartaltepe, J.‐P. Kneib, J. Koda, A. Koekemoer, Y. Komiyama, A. Leauthaud, O. Lefevre, S. Lilly, C. Liu, R. Massey, S. Miyazaki, T. Murayama, T. Nagao, J. A. Peacock, A. Pickles, C. Porciani, A. Renzini, J. Rhodes, M. Rich, M. Salvato, D. B. Sanders, C. Scarlata, D. Schiminovich, E. Schinnerer, M. Scodeggio, K. Sheth, Y. Shioya, L. A. M. Tasca, J. E. Taylor, L. Yan, G. Zamorani, 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), 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), P. Capak, H. Aussel, M. Ajiki, H. J. McCracken, B. Mobasher, N. Scoville, P. Shopbell, Y. Taniguchi, D. Thompson, S. Tribiano, S. Sasaki, A. W. Blain, M. Brusa, C. Carilli, A. Comastri, C. M. Carollo, P. Cassata, J. Colbert, R. S. Elli, M. Elvi, M. Giavalisco, W. Green, L. Guzzo, G. Hasinger, O. Ilbert, C. Impey, K. Jahnke, J. Kartaltepe, J. Kneib, J. Koda, A. Koekemoer, Y. Komiyama, A. Leauthaud, O. L. Fevre, S. Lilly, C. Liu, R. Massey, S. Miyazaki, T. Murayama, T. Nagao, J. A. Peacock, A. Pickle, C. Porciani, A. Renzini, J. Rhode, M. Rich, M. Salvato, D. B. Sander, C. Scarlata, D. Schiminovich, E. Schinnerer, M. Scodeggio, K. Sheth, Y. Shioya, L. A. M., J. E. Taylor, L. Yan, and G. Zamorani

Subjects
Population, Large-scale structure of universe, FOS: Physical sciences, Field of view, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Surveys, 01 natural sciences, Imaging data, Cosmology: Observations, Spectral line, law.invention, Photometry (optics), Telescope, law, 0103 physical sciences, Galaxies: Evolution, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Panchromatic film, Cosmology: Large-Scale Structure of Universe, Cosmology: Observation, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Cosmology: observations, Galaxies: evolution, Astrophysics::Earth and Planetary Astrophysics
Abstract

We present imaging data and photometry for the COSMOS survey in 15 photometric bands between 0.3um and 2.4um. These include data taken on the Subaru 8.3m telescope, the KPNO and CTIO 4m telescopes, and the CFHT 3.6m telescope. Special techniques are used to ensure that the relative photometric calibration is better than 1% across the field of view. The absolute photometric accuracy from standard star measurements is found to be 6%. The absolute calibration is corrected using galaxy spectra, providing colors accurate to 2% or better. Stellar and galaxy colors and counts agree well with the expected values. Finally, as the first step in the scientific analysis of these data we construct panchromatic number counts which confirm that both the geometry of the universe and the galaxy population are evolving., Comment: 19 pages, 13 figures, 14 tables, Accepted to ApJS for COSMOS speciall issue

Published
2007
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7. Lyman Alpha Emitters at Redshift 5.7 in the COSMOS Field

Author

T. Murayama, Y. Taniguchi, N. Z. Scoville, M. Ajiki, D. B. Sanders, B. Mobasher, H. Aussel, P. Capak, A. Koekemoer, Y. Shioya, T. Nagao, C. Carilli, R. S. Ellis, B. Garilli, M. Giavalisco, M. G. Kitzbichler, O. LeFevre, D. Maccagni, E. Schinnerer, V. Smolcic, S. Tribiano, Y. Komiyama, S. Miyazaki, S. S. Sasaki, J. Koda, H. Karoji, CIMATTI, ANDREA, T. Murayama, Y. Taniguchi, N. Z. Scoville, M. Ajiki, D. B. Sander, B. Mobasher, H. Aussel, P. Capak, A. Koekemoer, Y. Shioya, T. Nagao, C. Carilli, R. S. Elli, B. Garilli, M. Giavalisco, M. G. Kitzbichler, O. LeFevre, D. Maccagni, E. Schinnerer, V. Smolcic, S. Tribiano, A. Cimatti, Y. Komiyama, S. Miyazaki, S. S. Sasaki, J. Koda, and H. Karoji

Subjects
Cosmology: Early Universe, Cosmology: Observation, Galaxies: Evolution, Galaxies: Formation, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

We present results from a narrow-band optical survey of a contiguous area of 1.95 deg^2, covered by the Cosmic Evolution Survey (COSMOS). Both optical narrow-band (lambda_c = 8150 AA and Delta_lambda = 120 AA) and broad-band (B, V, g', r', i', and z') imaging observations were performed with the Subaru prime-focus camera, Suprime-Cam on the Subaru Telescope. We provide the largest contiguous narrow-band survey, targetting Ly alpha emitters (LAEs) at z~5.7. We find a total of 119 LAE candidates at z~5.7. Over the wide-area covered by this survey, we find no strong evidence for large scale clustering of LAEs. We estimate a star formation rate (SFR) density of ~7*10^-4 M_sun yr^-1 Mpc^-3 for LAEs at z~5.7, and compare it with previous measurements., 26 pages, 19 figures. to appear in the ApJ Supplement COSMOS Special Issue

Published
2007

8. Probing the First Stars and Black Holes in the Early Universe with the Dark Ages Radio Explorer (DARE)

Author

Stuart D. Bale, Joseph Lazio, A. Loeb, C. Carilli, Jack O. Burns, R. Bradley, Steve R. Furlanetto, Judd D. Bowman, Geraint Harker, and Jonathan R. Pritchard

Subjects
Atmospheric Science, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Aerospace Engineering, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Cosmology, 0103 physical sciences, Galaxy formation and evolution, 010303 astronomy & astrophysics, Reionization, media_common, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Galaxy, Dark Ages Radio Explorer, Universe, Geophysics, 13. Climate action, Space and Planetary Science, Dark Ages, General Earth and Planetary Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A concept for a new space-based cosmology mission called the Dark Ages Radio Explore (DARE) is presented in this paper. DARE's science objectives include (1) When did the first stars form? (2) When did the first accreting black holes form? (3) When did Reionization begin? (4) What surprises does the end of the Dark Ages hold (e.g., Dark Matter decay)? DARE will use the highly-redshifted hyperfine 21-cm transition from neutral hydrogen to track the formation of the first luminous objects by their impact on the intergalactic medium during the end of the Dark Ages and during Cosmic Dawn (redshifts z=11-35). It will measure the sky-averaged spin temperature of neutral hydrogen at the unexplored epoch 80-420 million years after the Big Bang, providing the first evidence of the earliest stars and galaxies to illuminate the cosmos and testing our models of galaxy formation. DARE's approach is to measure the expected spectral features in the sky-averaged, redshifted 21-cm signal over a radio bandpass of 40-120 MHz. DARE orbits the Moon for a mission lifetime of 3 years and takes data above the lunar farside, the only location in the inner solar system proven to be free of human-generated radio frequency interference and any significant ionosphere. The science instrument is composed of a three-element radiometer, including electrically-short, tapered, bi-conical dipole antennas, a receiver, and a digital spectrometer. The smooth frequency response of the antennas and the differential spectral calibration approach using a Markov Chain Monte Carlo technique will be applied to detect the weak cosmic 21-cm signal in the presence of the intense solar system and Galactic foreground emissions., 33 pages, 12 figures; submitted to Advances in Space Research

Published
2011

9. COSMOS : Hubble Space Telescope Observations

Author

N. Scoville, R. G. Abraham, H. Aussel, J. E. Barnes, A. Benson, A. W. Blain, D. Calzetti, A. Comastri, P. Capak, C. Carilli, J. E. Carlstrom, C. M. Carollo, J. Colbert, E. Daddi, R. S. Ellis, M. Elvis, S. P. Ewald, M. Fall, A. Franceschini, M. Giavalisco, W. Green, R. E. Griffiths, L. Guzzo, G. Hasinger, C. Impey, J.‐P. Kneib, J. Koda, A. Koekemoer, O. Lefevre, S. Lilly, C. T. Liu, H. J. McCracken, R. Massey, Y. Mellier, S. Miyazaki, B. Mobasher, J. Mould, C. Norman, A. Refregier, A. Renzini, J. Rhodes, M. Rich, D. B. Sanders, D. Schiminovich, E. Schinnerer, M. Scodeggio, K. Sheth, P. L. Shopbell, Y. Taniguchi, N. D. Tyson, C. M. Urry, L. Van Waerbeke, P. Vettolani, S. D. M. White, L. Yan, 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), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, Cosmology: Observations, 7. Clean energy, 01 natural sciences, Advanced Camera for Surveys, Physical cosmology, Hubble space telescope, Galaxies: Evolution, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Weak gravitational lensing, Physics, Pixel, 010308 nuclear & particles physics, Cosmology: Dark Matter, Galaxies: Formation, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Cosmology: Large-Scale Structure of Universe, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Limiting magnitude, Astrophysics::Earth and Planetary Astrophysics
Abstract

The Cosmic Evolution Survey (COSMOS) was initiated with an extensive allocation (590 orbits in Cycles 12-13) using the Hubble Space Telescope (HST) for high resolution imaging. Here we review the characteristics of the HST imaging with the Advanced Camera for Surveys (ACS) and parallel observations with NICMOS and WFPC2. A square field (1.8$\sq$\deg) has been imaged with single-orbit ACS I-F814W exposures with 50% completeness for sources 0.5\arcsec in diameter at I$_{AB} $ = 26.0 mag. The ACS imaging is a key part of the COSMOS survey, providing very high sensitivity and high resolution (0.09\arcsec FWHM, 0.05\arcsec pixels) imaging and detecting 1.2 million objects to a limiting magnitude of 26.5 (AB). These images yield resolved morphologies for several hundred thousand galaxies. The small HST PSF also provides greatly enhanced sensitivity for weak lensing investigations of the dark matter distribution., Comment: 21 pages, 6 figures -- to appear in COSMOS ApJ Suppl. special issue

Published
2006
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10. Impact of a high-fibre diet on genetic parameters of production traits in growing pigs

Author

V. Déru, A. Bouquet, C. Hassenfratz, B. Blanchet, C. Carillier-Jacquin, and H. Gilbert

Subjects
dietary fibres, feed efficiency, genetic variance, genetic by feed interactions, selection decisions, Animal culture, SF1-1100
Abstract

The use of diets with increased fibre content from alternative feedstuffs less digestible for pigs is a solution considered to limit the impact of increased feed costs on pig production. This study aimed at determining the impact of an alternative diet on genetic parameters for growth, feed efficiency, carcass composition and meat quality traits. A total of 783 Large White pigs were fed a high-fibre (HF) diet and 880 of their sibs were fed a conventional (CO) cereal-based diet. Individual daily feed intake, average daily gain, feed conversion ratio and residual feed intake were recorded as well as lean meat percentage (LMP), carcass yield (CY) and meat quality traits. Pigs fed the CO diet had better performances for growth and feed efficiency than pigs fed the HF diet. They also had lower LMP and higher CY. In addition, pigs fed the CO diet had lower loin percentage and ham percentage and higher backfat percentage. No differences were observed in meat quality traits between diets, except for a* and b* values. For all traits, the genetic variances and heritability were not different between diets. Genetic correlations for traits between diets ranged between 0.80 ± 0.13 and 0.99 ± not estimable, and none were significantly different from 0.99, except for LMP. Thus, traits in both diets were considered as mainly affected by similar sets of genes in the two diets. A genetic correlation lower than 0.80 would justify redesigning the breeding scheme; however, some genetic correlations did not differ significantly from 0.80 either. Therefore, larger populations are needed for a more definitive answer regarding the design of the breeding scheme. To further evaluate selection strategies, a production index was computed within diets for the 29 sires with estimated breeding value reliability higher than 0.35. The rank correlation between indices estimated in the CO and in the HF diet was 0.72. Altogether, we concluded that limited interaction between feed and genetics could be evidenced, and based on these results there is no need to change pig selection schemes to adapt to the future increased use of alternative feedstuffs in production farms.

Published
2020
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11. Digestive efficiency traits in growing pigs are genetically correlated with sow litter traits in the Large White breed

Author

A. Bouquet, V. Déru, B. Blanchet, P. Ganier, L. Flatrès-Grall, B. Ligonesche, C. Carillier-Jacquin, E. Labussière, and H. Gilbert

Subjects
Digestibility coefficients, Feed efficiency, Litter size, Piglet survival, Pig, Animal culture, SF1-1100
Abstract

Digestive efficiency traits are promising selection criteria to improve feed efficiency in pigs. However, the genetic relationships between digestive efficiency and sow reproductive traits are mostly unknown and need to be estimated. In this study, reproductive traits were available for 61 601 litters recorded on 21 719 Large White purebred sows. The traits were comprised of the number of born alive (NBA) and the number of weaned piglets (NWP), the number of stillbirths (NSB) and piglet mortality during suckling (PM). For a subset of 32 518 litters, the mean (MBW) and CV of piglet birth weights (CVBW) were deduced from individual piglet weights as well as the proportion of piglets weighing less than 1 kg (PPL1K). Growth and feed efficiency traits were available for 4 643 Large White male pigs related to sows with reproductive performances. They comprised average daily gain (ADG), daily feed intake (DFI) and feed conversion ratio (FCR). A subset of 1 391 pigs had predictions for digestibility coefficients (DC) of energy, organic matter and nitrogen obtained by analysing faecal samples with near-infrared spectrometry. Estimated heritabilities were low for NBA, NSB, NWP and PM (0.08 ± 0.01 to 0.11 ± 0.01) and low to moderate for litter weight characteristics (0.14 ± 0.02 to 0.38 ± 0.01). Heritability estimates were moderate to high for ADG, DFI and FCR (0.37 ± 0.04 to 0.54 ± 0.05) and moderate for DC traits (0.26 ± 0.06 to 0.38 ± 0.07). Genetic correlations were low between ADG, or alternatively FCR, and reproductive traits. They were significantly different from zero with MBW (0.19 ± 0.06 with ADG and −0.15 ± 0.06 with FCR) and PPL1K (−0.19 ± 0.07 with ADG and 0.18 ± 0.07 with FCR). All genetic correlations between DFI and reproductive traits were low and not significantly different from zero. Genetic correlations between DC traits and NBA were significantly different from zero for DC of organic matter and energy (0.30 ± 0.11), CVBW (

Published
2022
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13. H I 21 CM Line Observations of Damped Lyman Alpha Systems

Author

W. Lane, G. K. Miley, C. Carilli, Robert Braun, and A. G. de Bruyn

Subjects
Radio telescope, Physics, Hydrogen line, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Absorption (electromagnetic radiation), Equivalent width, Astrophysics::Galaxy Astrophysics, Redshift, Galaxy, Spectral line
Abstract

We have used the Westerbork Synthesis Radio Telescope to search for H I 21 cm absorption associated with high redshift damped Ly α systems. We calculate limits to harmonic mean spin temperatures, , for these systems, and find typical lower limits ≈ 103 K, consistent with previous results for other damped Ly α systems. We then analyze the relationship between the total H I column density and the integrated 21 cm absorption line equivalent width, EW21, for damped Ly α systems. We compare these results with similar results for lines of sight through our own galaxy. A trend is seen in which the damped Ly α systems show a systematically lower EW21 at a given total N(H I) than Galactic lines of sight, by a factor ≈ 3 to 5. In the context of a two temperature phase model for the absorbing gas, these results suggest that for a given total neutral hydrogen column density, the damped Ly α systems contain a larger percentage of warm gas than is seen in typical Galactic lines of sight.

Published
1996
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14. Human renin is correctly processed and targeted to the regulated secretory pathway in mouse pituitary AtT-20 cells

Author

L C, Fritz, M A, Haidar, A E, Arfsten, J W, Schilling, C, Carilli, J, Shine, J D, Baxter, and T L, Reudelhuber

Subjects
Enzyme Precursors, Colforsin, Ovary, Fibroblasts, Exocytosis, Cell Line, Mice, Cricetulus, Cricetinae, Pituitary Gland, Renin, Animals, Humans, Female, Pituitary Neoplasms, Amino Acid Sequence, Protein Processing, Post-Translational
Abstract

Renin is formed by intracellular processing of prorenin and catalyzes the conversion of angiotensinogen to angiotensin I, the precursor to angiotensin II. Several tissues synthesize prorenin. However, in man, the kidney is the only known source of circulating renin, raising the possibility that the processing enzyme is unique to that tissue. We have transfected a gene that directs prorenin synthesis in pituitary AtT-20 cells, which are capable of processing other prohormones. The results demonstrate that transfected AtT-20 cells can secrete inactive prorenin, accurately process prorenin to active renin, and be stimulated to release active renin in response to a secretagogue. These data imply that cellular elements capable of directing the processing of prorenin to renin and its correct subcellular compartmentalization may be present in nonrenal cell types and that critical elements of the regulated release of renin that occur in the kidney can be reconstituted in cells in culture.

Published
1987

15. The Chandra COSMOS Survey, I: Overview and Point Source Catalog

Author

Luigi Guzzo, Bahram Mobasher, G. Zamorani, Fabrizio Fiore, Chris Impey, Hermann Brunner, Antonella Fruscione, Takamitsu Miyaji, Simon J. Lilly, Marcella Brusa, Anton M. Koekemoer, Stefano Ettori, Francesca Civano, Yoshiaki Taniguchi, John D. Silverman, James E. Taylor, Martin Elvis, Heng Hao, Michael Rich, Peter Capak, Simonetta Puccetti, Andrew Blain, Guenther Hasinger, David B. Sanders, Richard E. Griffiths, C. Marcella Carollo, Marta Volonteri, Giuseppina Fabbiano, Mara Salvato, Tom Aldcroft, Patrick L. Shopbell, Cristian Vignali, Alexis Finoguenov, Vincenzo Mainieri, N. Z. Scoville, Andrea Comastri, Francesco Damiani, Nico Cappelluti, Chris Carilli, Eva Schinnerer, Daniela Calzetti, Roberto Gilli, C. M. Urry, M. Elvi, F. Civano, C. Vignali, S. Puccetti, F. Fiore, N. Cappelluti, T. L. Aldcroft, A. Fruscione, G. Zamorani, A. Comastri, M. Brusa, R. Gilli, T. Miyaji, F. Damiani, A. Koekemoer, A. Finoguenov, H. Brunner, C.M. Urry, J. Silverman, V. Mainieri, G. Hasinger, R. Griffith, M. Carollo, H. Hao, L. Guzzo, A. Blain, D. Calzetti, C. Carilli, P. Capak, S. Ettori, G. Fabbiano, C. Impey, S. Lilly, B. Mobasher, M. Rich, M. Salvato, D.B. Sander, E. Schinnerer, N. Scoville, P. Shopbell, J.E. Taylor, Y. Taniguchi, and M. Volonteri

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Field (physics), biology, Infrared, Point source, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Limiting, biology.organism_classification, Acis, Space and Planetary Science, Point (geometry), Astrophysics - High Energy Astrophysical Phenomena, catalogs – cosmology: observations – galaxies: evolution – quasars: general – surveys – X-rays: general, Cosmos, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Chandra COSMOS Survey (C-COSMOS) is a large, 1.8 Ms, Chandra} program that has imaged the central 0.5 sq.deg of the COSMOS field (centered at 10h, +02deg) with an effective exposure of ~160ksec, and an outer 0.4sq.deg. area with an effective exposure of ~80ksec. The limiting source detection depths are 1.9e-16 erg cm(-2) s(-1) in the Soft (0.5-2 keV) band, 7.3e(-16) erg cm^-2 s^-1 in the Hard (2-10 keV) band, and 5.7e(-16) erg cm(-2) s(-1) in the Full (0.5-10 keV) band. Here we describe the strategy, design and execution of the C-COSMOS survey, and present the catalog of 1761 point sources detected at a probability of being spurious of, Revised to omit egregious bold facing and fix missing ',' in author list

Published
2009

16. COSBO: The MAMBO 1.2 Millimeter Imaging Survey of the COSMOS Field

Author

H. Voss, Nick Scoville, Manuel Aravena, James E. Aguirre, Andrew Blain, B. Mobasher, D. Thompson, Anton M. Koekemoer, Peter Capak, Karl M. Menten, Günther Hasinger, Chris Carilli, Vernesa Smolčić, Ernst Kreysa, J. Schlaerth, Simon J. Lilly, Marcella Brusa, Yoshi Taniguchi, Eva Schinnerer, Herve Aussel, Frank Bertoldi, Knud Jahnke, Dieter Lutz, F. Bertoldi, C. Carilli, M. Aravena, E. Schinnerer, H. Vo, V. Smolcic, K. Jahnke, N. Scoville, A. Blain, K. M. Menten, D. Lutz, M. Brusa, Y. Taniguchi, P. Capak, B. Mobasher, S. Lilly, D. Thompson, H. Aussel, E. Kreysa, G. Hasinger, J. Aguirre, J. Schlaerth, and A. Koekemoer

Subjects
Luminous infrared galaxy, Physics, Field (physics), Astrophysics::High Energy Astrophysical Phenomena, Bolometer, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Surveys, Redshift, Galaxy, law.invention, Telescope, Space and Planetary Science, law, Millimeter, Area density, Submillimeter, Infrared: Galaxie, Astrophysics::Galaxy Astrophysics
Abstract

The inner 20×20 arcmin2 of the COSMOS field was imaged at 250 GHz (1.2 mm) to an rms noise level of ~1 mJy per 11" beam using the Max-Planck Millimeter Bolometer Array (MAMBO-2) at the IRAM 30 m telescope. We detect 15 sources at significance between 4 and 7 σ, 11 of which are also detected at 1.4 GHz with the VLA with a flux density >24 μJy (3 σ). We identify 12 more lower significance mm sources based on their association with faint radio sources. We present the multifrequency identifications of the MAMBO sources, including VLA radio flux densities, optical and near-infrared identifications, as well as the XMM-Newton X-ray detection for two of the mm sources. We compare radio and optical photometric redshifts and briefly describe the host galaxy morphologies. The colors of the identified optical counterparts suggest most of them to be high-redshift (z~2-3) star-forming galaxies. At least three sources appear lensed by a foreground galaxy. We highlight some MAMBO sources that do not show obvious radio counterparts. These sources could be dusty starburst galaxies at redshifts >3.5. The 250 GHz source areal density in the COSMOS field is comparable to that seen in other deep mm fields. Based on observations with the 30 m telescope of the Institute for Radioastronomy at Millimeter Wavelengths (IRAM), which is funded by the German Max-Planck-Society, the French CNRS, and the Spanish National Geographical Institute. Also based on observations with the Very Large Arrray of the National Radio Astronomy Observatory, which is a facility of the National Science Foundation, operated under cooperative agreement by Associated University Inc. Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under NASA contract NAS 5-26555 also based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan; XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; the European Southern Observatory, Chile; Kitt Peak National Observatory, Cerro Tololo Inter-American Observatory, and the National Optical Astronomy Observatory, which are operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation; and the Canada-France-Hawaii Telescope operated by the National Research Council of Canada, Centre National de la Recherche Scientifique de France and the University of Hawaii.

Published
2007

17. Exploring barriers and facilitators of implementing an at-home SARS-CoV-2 antigen self-testing intervention: The Rapid Acceleration of Diagnostics-Underserved Populations (RADx-UP) initiatives.

Author

Cross LM, DeFosset A, Yusuf B, Conserve D, Anderson R, Carilli C, Kibbe W, Cohen-Wolkowiez M, Richmond A, Corbie G, and Dave G

Subjects
Humans, Self-Testing, Vulnerable Populations, Community Health Services, COVID-19 Testing, SARS-CoV-2, COVID-19 diagnosis, COVID-19 epidemiology
Abstract

Background: Evaluating community-based programs provides value to researchers, funding entities, and community stakeholders involved in program implementation, and can increase program impact and sustainability. To understand factors related to program implementation, we aimed to capture the perspective of community partners engaged in organizing and executing community-engaged programs to distribute COVID-19 at-home tests in underserved communities., Methods: We conducted semi-structured interviews and focus groups with community-based stakeholders informed by the Outcomes for Implementation Research framework., Results: Findings describe how community-engaged communication and dissemination strategies drove program adoption among grassroots stakeholders. Establishing and sustaining trusted relationships was vital to engaging partners with aligned values and capacity. Respondents characterized the programs as generally feasible and appropriate, and community partners felt capable of delivering the program successfully. However, they also described an increased burden on their workforce and desired more significant support. Respondents recognized the programs' community engagement practices as a critical facilitator of acceptability and impact., Discussion: Implementation evaluation aims to inform current and future community outreach and engagement efforts with best practices. As we continue to inform and advance community-engaged disaster response practice, a parallel reimagining of public health funding mechanisms and timelines could provide a foundation for trust, collaboration, and community resiliency that endures beyond a given crisis., Competing Interests: The authors have declared that no competing interests exist., (Copyright: © 2023 Cross et al. This is an open access article distributed under the terms of the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original author and source are credited.)

Published
2023
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18. Attitudes and perceptions about the use of long-acting injectable antipsychotics among behavioral health practitioners.

Author

Schwartz S, Carilli C, Mian T, Ruekert L, and Kumar A

Abstract

Introduction: Long-acting injectable antipsychotics (LAI-As) are important tools for the treatment of schizophrenia, yet they appear to be underutilized. This study will assess practitioner perceptions of LAI-As to elucidate reasons for underuse and uncover new avenues to increase appropriate use., Methods: An anonymous electronic survey was developed and actively distributed to behavioral health care practitioners (MD, DO, PA, NP, PharmD, RN, LCSW). Independent t testing and linear regression analysis was used to assess for interactions between survey responses and individual factors., Results: A total of 146 survey responses were collected from September 3, 2020 to March 17, 2021. On average, participants thought that LAI-As were slightly underutilized in practice. The mean estimated patient acceptance rate for LAI-A therapy was 38.6% ± 29.5% (range = 0%-100%). Participants who were <40 years of age and those with a psychiatric pharmacist at their practice site had significantly higher estimated acceptance rates. The highest-rated barriers to LAI-A use were related to negative patient attitudes, lack of patient education, and access issues (eg, transportation, cost). Respondent characteristics including age, gender identity, geographic location, practice setting, and the presence of a psychiatric pharmacist significantly influenced the perceived impact of these barriers., Discussion: Behavioral health practitioners generally believed that LAI-As were underused, and only one-third of their patients would be accepting of the therapy. Several barriers were perceived as frequently impacting LAI-A use, but these were reduced by the presence of a psychiatric pharmacist. Understanding practitioner perceptions can assist with increasing the use of LAI-As., Competing Interests: Disclosures: The authors have no conflicts of interest to disclose., (© 2022 AAPP. The Mental Health Clinician is a publication of the American Association of Psychiatric Pharmacists.)

Published
2022
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19. Impact of a multidisciplinary educational training program (OverdosED) on knowledge and perceptions of depressant substance use on a college campus.

Author

Musco S, Hargett B, Shollenberger T, Kicklighter J, and Carilli C

Subjects
Humans, Narcotic Antagonists therapeutic use, Pilot Projects, Students, Universities, Drug Overdose drug therapy, Naloxone therapeutic use
Abstract

Objective: Pilot study to assess the efficacy of a multidisciplinary educational training program (OverdosED) designed to increase college students' knowledge of and confidence in their ability to appropriately recognize and respond to suspected overdose on depressant substances. Participants: Undergraduate students ( n  = 92) with Greek life affiliations at a moderately-sized private liberal arts college in the southeastern USA. Methods: Electronic surveys were administered before and after delivery of the training program. Questions assessing knowledge of depressant substance overdose were compared to determine the impact of the educational intervention. Questions assessing participants' confidence in their ability to recognize and respond to overdose and their perceptions of campus culture were also compared. Results: Mean composite scores on knowledge-based questions were significantly higher for the post-intervention survey compared to the pre-intervention survey. Confidence in knowledge also significantly increased after the intervention. Mean scores for survey responses related to campus culture were high at baseline but significantly increased after the intervention. Conclusions: OverdosED successfully increased college students' knowledge of and confidence in their ability to appropriately recognize and respond to suspected overdose on depressant substances, and positively influenced perceptions on campus culture.

Published
2021
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20. Rapidly star-forming galaxies adjacent to quasars at redshifts exceeding 6.

Author

Decarli R, Walter F, Venemans BP, Bañados E, Bertoldi F, Carilli C, Fan X, Farina EP, Mazzucchelli C, Riechers D, Rix HW, Strauss MA, Wang R, and Yang Y

Abstract

The existence of massive (10 11 solar masses) elliptical galaxies by redshift z ≈ 4 (refs 1, 2, 3; when the Universe was 1.5 billion years old) necessitates the presence of galaxies with star-formation rates exceeding 100 solar masses per year at z > 6 (corresponding to an age of the Universe of less than 1 billion years). Surveys have discovered hundreds of galaxies at these early cosmic epochs, but their star-formation rates are more than an order of magnitude lower. The only known galaxies with very high star-formation rates at z > 6 are, with one exception, the host galaxies of quasars, but these galaxies also host accreting supermassive (more than 10 9 solar masses) black holes, which probably affect the properties of the galaxies. Here we report observations of an emission line of singly ionized carbon ([C ii] at a wavelength of 158 micrometres) in four galaxies at z > 6 that are companions of quasars, with velocity offsets of less than 600 kilometres per second and linear offsets of less than 100 kiloparsecs. The discovery of these four galaxies was serendipitous; they are close to their companion quasars and appear bright in the far-infrared. On the basis of the [C ii] measurements, we estimate star-formation rates in the companions of more than 100 solar masses per year. These sources are similar to the host galaxies of the quasars in [C ii] brightness, linewidth and implied dynamical mass, but do not show evidence for accreting supermassive black holes. Similar systems have previously been found at lower redshift. We find such close companions in four out of the twenty-five z > 6 quasars surveyed, a fraction that needs to be accounted for in simulations. If they are representative of the bright end of the [C ii] luminosity function, then they can account for the population of massive elliptical galaxies at z ≈ 4 in terms of the density of cosmic space.

Published
2017
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21. Galaxies at redshifts 5 to 6 with systematically low dust content and high [C II] emission.

Author

Capak PL, Carilli C, Jones G, Casey CM, Riechers D, Sheth K, Carollo CM, Ilbert O, Karim A, LeFevre O, Lilly S, Scoville N, Smolcic V, and Yan L

Abstract

The rest-frame ultraviolet properties of galaxies during the first three billion years of cosmic time (redshift z > 4) indicate a rapid evolution in the dust obscuration of such galaxies. This evolution implies a change in the average properties of the interstellar medium, but the measurements are systematically uncertain owing to untested assumptions and the inability to detect heavily obscured regions of the galaxies. Previous attempts to measure the interstellar medium directly in normal galaxies at these redshifts have failed for a number of reasons, with two notable exceptions. Here we report measurements of the forbidden C ii emission (that is, [C II]) from gas, and the far-infrared emission from dust, in nine typical star-forming galaxies about one billion years after the Big Bang (z ≈ 5-6). We find that these galaxies have thermal emission that is less than 1/12 that of similar systems about two billion years later, and enhanced [C II] emission relative to the far-infrared continuum, confirming a strong evolution in the properties of the interstellar medium in the early Universe. The gas is distributed over scales of one to eight kiloparsecs, and shows diverse dynamics within the sample. These results are consistent with early galaxies having significantly less dust than typical galaxies seen at z < 3 and being comparable in dust content to local low-metallicity systems.

Published
2015
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23. The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field.

Author

Walter F, Decarli R, Carilli C, Bertoldi F, Cox P, Da Cunha E, Daddi E, Dickinson M, Downes D, Elbaz D, Ellis R, Hodge J, Neri R, Riechers DA, Weiss A, Bell E, Dannerbauer H, Krips M, Krumholz M, Lentati L, Maiolino R, Menten K, Rix HW, Robertson B, Spinrad H, Stark DP, and Stern D

Abstract

The Hubble Deep Field provides one of the deepest multiwavelength views of the distant Universe and has led to the detection of thousands of galaxies seen throughout cosmic time. An early map of the Hubble Deep Field at a wavelength of 850 micrometres, which is sensitive to dust emission powered by star formation, revealed the brightest source in the field, dubbed HDF 850.1 (ref. 2). For more than a decade, and despite significant efforts, no counterpart was found at shorter wavelengths, and it was not possible to determine its redshift, size or mass. Here we report a redshift of z = 5.183 for HDF 850.1, from a millimetre-wave molecular line scan. This places HDF 850.1 in a galaxy overdensity at z ≈ 5.2, corresponding to a cosmic age of only 1.1 billion years after the Big Bang. This redshift is significantly higher than earlier estimates and higher than those of most of the hundreds of submillimetre-bright galaxies identified so far. The source has a star-formation rate of 850 solar masses per year and is spatially resolved on scales of 5 kiloparsecs, with an implied dynamical mass of about 1.3 × 10(11) solar masses, a significant fraction of which is present in the form of molecular gas. Despite our accurate determination of redshift and position, a counterpart emitting starlight remains elusive.

Published
2012
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24. A massive protocluster of galaxies at a redshift of z ≈ 5.3.

Author

Capak PL, Riechers D, Scoville NZ, Carilli C, Cox P, Neri R, Robertson B, Salvato M, Schinnerer E, Yan L, Wilson GW, Yun M, Civano F, Elvis M, Karim A, Mobasher B, and Staguhn JG

Abstract

Massive clusters of galaxies have been found that date from as early as 3.9 billion years (3.9 Gyr; z = 1.62) after the Big Bang, containing stars that formed at even earlier epochs. Cosmological simulations using the current cold dark matter model predict that these systems should descend from 'protoclusters'-early overdensities of massive galaxies that merge hierarchically to form a cluster. These protocluster regions themselves are built up hierarchically and so are expected to contain extremely massive galaxies that can be observed as luminous quasars and starbursts. Observational evidence for this picture, however, is sparse because high-redshift protoclusters are rare and difficult to observe. Here we report a protocluster region that dates from 1 Gyr (z = 5.3) after the Big Bang. This cluster of massive galaxies extends over more than 13 megaparsecs and contains a luminous quasar as well as a system rich in molecular gas. These massive galaxies place a lower limit of more than 4 × 10(11) solar masses of dark and luminous matter in this region, consistent with that expected from cosmological simulations for the earliest galaxy clusters.

Published
2011
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25. A kiloparsec-scale hyper-starburst in a quasar host less than 1 gigayear after the Big Bang.

Author

Walter F, Riechers D, Cox P, Neri R, Carilli C, Bertoldi F, Weiss A, and Maiolino R

Abstract

The host galaxy of the quasar SDSS J114816.64+525150.3 (at redshift z = 6.42, when the Universe was less than a billion years old) has an infrared luminosity of 2.2 x 10(13) times that of the Sun, presumably significantly powered by a massive burst of star formation. In local examples of extremely luminous galaxies, such as Arp 220, the burst of star formation is concentrated in a relatively small central region of <100 pc radius. It is not known on which scales stars are forming in active galaxies in the early Universe, at a time when they are probably undergoing their initial burst of star formation. We do know that at some early time, structures comparable to the spheroidal bulge of the Milky Way must have formed. Here we report a spatially resolved image of [C ii] emission of the host galaxy of J114816.64+525150.3 that demonstrates that its star-forming gas is distributed over a radius of about 750 pc around the centre. The surface density of the star formation rate averaged over this region is approximately 1,000 year(-1) kpc(-2). This surface density is comparable to the peak in Arp 220, although about two orders of magnitude larger in area. This vigorous star-forming event is likely to give rise to a massive spheroidal component in this system.

Published
2009
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26. The heating of gas in a galaxy cluster by X-ray cavities and large-scale shock fronts.

Author

McNamara BR, Nulsen PE, Wise MW, Rafferty DA, Carilli C, Sarazin CL, and Blanton EL

Abstract

Most of the baryons in galaxy clusters reside between the galaxies in a hot, tenuous gas. The densest gas in their centres should cool and accrete onto giant central galaxies at rates of 10-1,000 solar masses per year. No viable repository for this gas, such as clouds or new stars, has been found. New X-ray observations, however, have revealed far less cooling below X-ray temperatures than expected, altering the previously accepted picture of cooling flows. As a result, most of the gas must be heated to and maintained at temperatures above approximately 2 keV (ref. 3). The most promising heating mechanism is powerful radio jets emanating from supermassive black holes in the central galaxies of clusters. Here we report the discovery of giant cavities and shock fronts in a distant (z = 0.22) cluster caused by an interaction between a radio source and the hot gas surrounding it. The energy involved is approximately 6 x 10(61) erg, the most powerful radio outburst known. This is enough energy to quench a cooling flow for several Gyr, and to provide approximately 1/3 keV per particle of heat to the surrounding cluster.

Published
2005
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27. The essential signature of a massive starburst in a distant quasar.

Author

Solomon P, Vanden Bout P, Carilli C, and Guelin M

Abstract

Observations of carbon monoxide emission in high-redshift (zeta > 2) galaxies indicate the presence of large amounts of molecular gas. Many of these galaxies contain an active galactic nucleus powered by accretion of gas onto a supermassive black hole, and a key question is whether their extremely high infrared luminosities result from the active galactic nucleus, from bursts of massive star formation (associated with the molecular gas), or both. In the Milky Way, high-mass stars form in the dense cores of interstellar molecular clouds, where gas densities are n(H2) > 10(5) cm(-3) (refs 1, 2). Recent surveys show that virtually all galactic sites of high-mass star formation have similarly high densities. The bulk of the cloud material traced by CO observations, however, is at a much lower density. For galaxies in the local Universe, the HCN molecule is an effective tracer of high-density molecular gas. Here we report observations of HCN emission from the infrared-luminous 'Cloverleaf' quasar (at a redshift zeta = 2.5579). The HCN line luminosity indicates the presence of 10 billion solar masses of very dense gas, an essential feature of an immense starburst, which contributes, together with the active galactic nucleus it harbours, to its high infrared luminosity.

Published
2003
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28. Molecular gas in the host galaxy of a quasar at redshift z = 6.42.

Author

Walter F, Bertoldi F, Carilli C, Cox P, Lo KY, Neri R, Fan X, Omont A, Strauss MA, and Menten KM

Abstract

Observations of molecular hydrogen in quasar host galaxies at high redshifts provide fundamental constraints on galaxy evolution, because it is out of this molecular gas that stars form. Molecular hydrogen is traced by emission from the carbon monoxide molecule, CO; cold H2 itself is generally not observable. Carbon monoxide has been detected in about ten quasar host galaxies with redshifts z > 2; the record-holder is at z = 4.69 (refs 1-3). Here we report CO emission from the quasar SDSS J114816.64 + 525150.3 (refs 5, 6) at z = 6.42. At that redshift, the Universe was only 1/16 of its present age, and the era of cosmic reionization was just ending. The presence of about 2 x 1010 M\circ of H2 in an object at this time demonstrates that molecular gas enriched with heavy elements can be generated rapidly in the youngest galaxies.

Published
2003
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29. A massive reservoir of low-excitation molecular gas at high redshift.

Author

Papadopoulos P, Ivison R, Carilli C, and Lewis G

Subjects
Astronomical Phenomena, Carbon Monoxide, Hydrogen, Spectrum Analysis, Astronomy, Extraterrestrial Environment
Abstract

Molecular hydrogen (H2) is an important component of galaxies because it fuels star formation and the accretion of gas onto active galactic nuclei (AGN), the two processes that can generate the large infrared luminosities of gas-rich galaxies. Observations of spectral-line emission from the tracer molecule carbon monoxide (CO) are used to probe the properties of this gas. But the lines that have been studied in the local Universe-mostly the lower rotational transitions of J = 1 --> 0 and J = 2 --> 1-have hitherto been unobservable in high-redshift galaxies. Instead, higher transitions have been used, although the densities and temperatures required to excite these higher transitions may not be reached by much of the gas. As a result, past observations may have underestimated the total amount of molecular gas by a substantial amount. Here we report the discovery of large amounts of low-excitation molecular gas around the infrared-luminous quasar APM08279+5255 at redshift z = 3.91, using the two lowest excitation lines of 12 CO (J = 1 --> 0 and J = 2 --> 1). The maps confirm the presence of hot and dense gas near the nucleus, and reveal an extended reservoir of molecular gas with low excitation that is 10 to 100 times more massive than the gas traced by the higher-excitation observations. This raises the possibility that significant amounts of low-excitation molecular gas may exist in the environments of high-redshift (z > 3) galaxies.

Published
2001
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30. Infusion of recombinant human prorenin into rhesus monkeys. Effects on hemodynamics, renin-angiotensin-aldosterone axis and plasma testosterone.

Author

Lenz T, Sealey JE, Lappe RW, Carilli C, Oshiro GT, Baxter JD, and Laragh JH

Subjects
Angiotensinogen blood, Animals, Infusions, Intravenous, Kidney drug effects, Macaca mulatta, Recombinant Proteins pharmacology, Renin blood, Enzyme Precursors pharmacology, Hemodynamics drug effects, Renin pharmacology, Renin-Angiotensin System drug effects, Testosterone blood
Abstract

Prorenin, the biosynthetic precursor of active renin, is present in high concentrations in the kidney and reproductive organs. We have proposed that prorenin may be the vehicle of local renin systems, separating the functions of circulating and tissue renin. In the present study, we investigated the effect of increasing plasma prorenin 3- to 4-fold by infusing recombinant prorenin, 400 ng/min for 40 min, into male rhesus monkeys. The prorenin was first warmed to 37 degrees C to reduce the endogenous renin activity to a minimum. The study included a 20 min baseline and a 40 min recovery period. Plasma prorenin increased from 72 +/- 14 ng/mL/h to a maximum of 246 +/- 18 ng/mL/h during the infusion (P less than .001) and fell to 169 +/- 23 ng/mL/h 40 min after the infusion was stopped. Active renin did not change significantly. Plasma aldosterone increased slightly during the prorenin infusion (by 13%) and returned to baseline during the recovery period (P less than .05 compared to the infusion period). Plasma testosterone fell significantly from 1.9 +/- 0.1 ng/mL to 1.6 +/- 0.1 ng/mL during the infusion and further to 1.4 +/- 0.1 ng/mL during the post-infusion period (P less than .05). Blood pressure fell slightly but not significantly. Heart rate, glomerular filtration rate and renal blood flow, as well as urine flow and urine sodium and potassium excretion showed no significant change. These results demonstrate that human recombinant prorenin is not converted to active renin in the circulation of rhesus monkeys.(ABSTRACT TRUNCATED AT 250 WORDS)

Published
1990
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31. Identification of an enzyme in human kidney that correctly processes prorenin.

Author

Shinagawa T, Do YS, Baxter JD, Carilli C, Schilling J, and Hsueh WA

Subjects
Amino Acid Sequence, Animals, Cell Line, Chromatography, Affinity, Chromatography, High Pressure Liquid, Chromatography, Ion Exchange, Cysteine Endopeptidases isolation & purification, Enzyme Precursors isolation & purification, Enzyme Precursors metabolism, Humans, Kidney Cortex enzymology, Kinetics, Molecular Sequence Data, Molecular Weight, Recombinant Proteins isolation & purification, Recombinant Proteins metabolism, Renin isolation & purification, Renin metabolism, Transfection, Cysteine Endopeptidases metabolism, Enzyme Precursors genetics, Kidney enzymology, Protein Processing, Post-Translational, Renin genetics
Abstract

Using pure recombinant human prorenin as a substrate, we have identified an enzyme in human kidney that accurately processes prorenin to active renin (EC 3.4.23.15). In the crude homogenate, the predominant activity of this potential renin-processing enzyme (RPE) converted the Mr 47,000 inactive prorenin to Mr 44,000 active renin and had a pH optimum of approximately 6. The activity was blocked by cysteine protease inhibitors, but not by pepstatin, EDTA, or serine protease inhibitors. This RPE activity was not detected in a similarly prepared homogenate of human chorion decidua tissue, which produces primarily prorenin, or in human plasma. The activity was purified 100-fold by ammonium sulfate precipitation, p-chloromercuribenzoate affinity chromatography, and chromatofocusing. The partially purified enzyme has a Mr of approximately 27,000 and an isoelectric point in the pH 4.8-5.6 range. The activity in the purified RPE preparation had the same pH optimum as that in crude homogenate, cleaved the prosegment at the same site used by the kidney in vivo based on amino-terminal sequencing of the processed renin, and did not degrade prorenin or renin. These data suggest that the cysteine protease we have isolated is a candidate for authentic renal RPE.

Published
1990
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32. Human renin is correctly processed and targeted to the regulated secretory pathway in mouse pituitary AtT-20 cells.

Author

Fritz LC, Haidar MA, Arfsten AE, Schilling JW, Carilli C, Shine J, Baxter JD, and Reudelhuber TL

Subjects
Amino Acid Sequence, Animals, Cell Line, Colforsin pharmacology, Cricetinae, Cricetulus, Enzyme Precursors metabolism, Exocytosis drug effects, Female, Fibroblasts metabolism, Humans, Mice, Ovary, Pituitary Gland drug effects, Pituitary Neoplasms pathology, Protein Processing, Post-Translational, Pituitary Gland metabolism, Renin metabolism
Abstract

Renin is formed by intracellular processing of prorenin and catalyzes the conversion of angiotensinogen to angiotensin I, the precursor to angiotensin II. Several tissues synthesize prorenin. However, in man, the kidney is the only known source of circulating renin, raising the possibility that the processing enzyme is unique to that tissue. We have transfected a gene that directs prorenin synthesis in pituitary AtT-20 cells, which are capable of processing other prohormones. The results demonstrate that transfected AtT-20 cells can secrete inactive prorenin, accurately process prorenin to active renin, and be stimulated to release active renin in response to a secretagogue. These data imply that cellular elements capable of directing the processing of prorenin to renin and its correct subcellular compartmentalization may be present in nonrenal cell types and that critical elements of the regulated release of renin that occur in the kidney can be reconstituted in cells in culture.

Published
1987

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