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arXiv 2024年

作者： Gianolli, Vittoria Elvezia Bianchi, S. Petrucci, P.-O. Brusa, M. Chartas, G. Lanzuisi, G. Matzeu, G.A. Parra Ursini, F. Behar, E. Bischetti, M. Comastri, A. Costantini, E. Cresci, G. Dadina, M. De, B. Marco, M. De Rosa, A. Fiore, F. Gaspari, M. Gilli, R. Giustini, M. Guainazzi, M. King, A.R. Kraemer, S. Kriss, G. Krongold, Y. La Franca, F. Longinotti, A.L. Luminari, A. Maiolino Marconi, R.A. Mathur, S. Matt, G. Mehdipour, M. Merloni, A. Middei, R. Miniutti, G. Nardini, E. Panessa, F. Perna, M. Piconcelli, E. Ponti, G. Ricci, F. Serafinelli, R. Tombesi, F. Vignali, C. Zappacosta, L. Université Grenoble Alpes CNRS IPAG Grenoble38000 France Dipartimento di Matematica e Fisica Università degli Studi Roma Tre Via della Vasca Navale 84 Roma00146 Italy University of Bologna Via Gobetti 93/2 BolognaI-40129 Italy INAF-Osservatorio di Astrofisica e Scienza dello Spazio di Bologna Via Gobetti 93/3 BolognaI-40129 Italy Villanueva de la Cañada MadridE-28691 Spain Department of Physics and Astronomy College of Charleston CharlestonSC29424 United States Physics Department The Technion Haifa32000 Israel Dipartimento di Fisica Universitá di Trieste Sezione di Astronomia Via G.B. Tiepolo 11 TriesteI-34131 Italy SRON Netherlands Institute for Space Research Niels Bohrweg 4 CA Leiden2333 Netherlands INAF Osservatorio Astrofisico di Arcetri Largo Enrico Fermi 5 Firenze50125 Italy Departament de Física EEBE Universitat Politècnica de Catalunya Av. Eduard Maristany 16 Barcelona08019 Spain INAF Osservatorio Astronomico di Trieste Via G. B. Tiepolo 11 Trieste34143 Italy Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544-1001 United States CSIC-INTA Campus ESAC Camino Bajo del Castillo s/n Villanueva de la Cañada Madrid28692 Spain Keplerlaan 1 Noordwijk2201 AZ Netherlands Department of Physics & Astronomy University of Leicester LeicesterLE1 7RH United Kingdom Astronomical Institute Anton Pannekoek University of Amsterdam Science Park 904 NL-1098 XH Netherlands Department of Physics Institute for Astrophysics and Computational Sciences The Catholic University of America WashingtonDC20064 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Instituto de Astronomía Universidad Nacional Autónoma de México Circuito Exterior Ciudad Universitaria Ciudad de México04510 Mexico INAF Istituto di Astrofisica e Planetologia Spaziali Via Fosso del Cavaliere Roma00133 Italy INAF Osservatorio Astronomico di Roma Via Frascati 33 Monte Po

The detection of blueshifted absorption lines likely associated with ionized iron K-shell transitions in the X-ray spectra of many active galactic nuclei (AGNs) suggests the presence of a highly ionized gas outflowing with mildly relativistic velocities (0.03c - 0.6c) named ultra-fast outflow (UFO). Within the SUBWAYS project, we characterized these winds starting from a sample of 22 radio-quiet quasars at an intermediate redshift (0.1 ≤ z ≤ 0.4) and compared the results with similar studies in the literature on samples of local Seyfert galaxies (i.e., 42 radio-quiet AGNs observed with XMM-Newton at z ≤ 0.1) and high redshift radio-quiet quasars (i.e., 14 AGNs observed with XMM-Newton and Chandra at z ≥ 1.4). The scope of our work is a statistical study of UFO parameters and incidence considering the key physical properties of the sources, such as supermassive black hole (SMBH) mass, bolometric luminosity, accretion rates, and spectral energy distribution (SED) with the aim of gaining new insights into the UFO launching mechanisms. We find indications that highly luminous AGNs with a steeper X-ray/UV ratio, αox, are more likely to host UFOs. The presence of UFOs is not significantly related to any other AGN property in our sample. These findings suggest that the UFO phenomenon may be transient. Focusing on AGNs with UFOs, other important findings from this work include: (1) faster UFOs have larger ionization parameters and column densities;(2) X-ray radiation plays a more crucial role in driving highly ionized winds compared to UV;(3) the correlation between outflow velocity and luminosity is significantly flatter than what is expected for radiatively driven winds;(4) more massive black holes experience higher wind mass losses, suppressing the accretion of matter onto the black hole;(5) the UFO launching radius is positively correlated with the Eddington ratio. Furthermore, our analysis suggests the involvement of multiple launching mechanisms, including radiation p

关键词： Active Galactic Nuclei

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Exploring cosmic origins with CORE: Mitigation of systematic effects

arXiv

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arXiv 2017年

作者： Natoli, P. Ashdown, M. Banerji, R. Borrill, J. Buzzelli, A. de Gasperis, G. Delabrouille, J. Hivon, E. Molinari, D. Patanchon, G. Polastri, L. Tomasi, M. Bouchet, F.R. Henrot-Versillé, S. Hoang, D.T. Keskitalo, R. Kiiveri, K. Kisner, T. Lindholm, V. McCarthy, D. Piacentini, F. Perdereau, O. Polenta, G. Tristram, M. Achucarro, A. Ade, P. Allison, R. Baccigalupi, C. Ballardini, M. Banday, A.J. Bartlett, J. Bartolo, N. Basak, S. Baselmans, J. Baumann, D. Bersanelli, M. Bonaldi, A. Bonato, M. Boulanger, F. Brinckmann, T. Bucher, M. Burigana, C. Cai, Z.-Y. Calvo, M. Carvalho, C.-S. Castellano, G. Challinor, A. Chluba, J. Clesse, S. Colantoni, I. Coppolecchia, A. Crook, M. D'Alessandro, G. de Bernardis, P. de Zotti, G. Di Valentino, E. Diego, J.-M. Errard, J. Feeney, S. Fernandez-Cobos, R. Finelli, F. Forastieri, F. Galli, S. Genova-Santos, R. Gerbino, M. González-Nuevo, J. Grandis, S. Greenslade, J. Gruppuso, A. Hagstotz, S. Hanany, S. Handley, W. Hernandez-Monteagudo, C. Hervías-Caimapo, C. Hills, M. Keihänen, E. Kitching, T. Kunz, M. Kurki-Suonio, H. Lamagna, L. Lasenby, A. Lattanzi, M. Lesgourgues, J. Lewis, A. Liguori, M. López-Caniego, M. Luzzi, G. Maffei, B. Mandolesi, N. Martinez-González, E. Martins, C.J.A.P. Masi, S. Melchiorri, A. Melin, J.-B. Migliaccio, M. Monfardini, A. Negrello, M. Notari, A. Pagano, L. Paiella, A. Paoletti, D. Piat, M. Pisano, G. Pollo, A. Poulin, V. Quartin, M. Remazeilles, M. Roman, M. Rossi, G. Rubino-Martin, J.-A. Salvati, L. Signorelli, G. Tartari, A. Tramonte, D. Trappe, N. Trombetti, T. Tucker, C. Valiviita, J. van de Weijgaert, R. van Tent, B. Vennin, V. Vielva, P. Vittorio, N. Wallis, C. Young, K. Zannoni, M. Dipartimento di Fisica e Scienze della Terra Università di Ferrara Via Saragat 1 Ferrara44122 Italy INFN Sezione di Ferrara Via Saragat 1 Ferrara44122 Italy Astrophysics Group Cavendish Laboratory University of Cambridge J. J. Thomson Avenue CambridgeCB3 0HE United Kingdom Kavli Institute for Cosmology Univerisity of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom APC AstroParticule et Cosmologie Université Paris Diderot CNRS/IN2P3 CEA/lrfu Observatoire de Paris Sorbonne Paris Cité 10 rue Alice Domon et Léonie Duquet Paris Cedex 1375205 France Computational Cosmology Center Lawrence Berkeley National Laboratory BerkeleyCA United States Space Sciences Laboratory University of California BerkeleyCA94720 United States Dipartimento di Fisica Università di Roma La Sapienza P.le A. Moro 2 Roma00185 Italy Dipartimento di Fisica Università di Roma Tor Vergata Via della Ricerca Scientifica 1 RomaI-00133 Italy INFN Sezione di Tor Vergata Via della Ricerca Scientifica 1 RomaI-00133 Italy ParisF-75014 France INAF/IASF Bologna via Gobetti 101 BolognaI-40129 Italy Dipartimento di Fisica Università degli Studi di Milano Via Celoria 16 Milano Italy INAF/IASF Milano Via E. Bassini 15 Milano Italy Laboratoire de l'Accélérateur Linéaire Univ. Paris-Sud CNRS/IN2P3 Université Paris-Saclay Orsay France Department of Physics Gustaf Hällströmin katu 2a University of Helsinki Helsinki Finland Helsinki Institute of Physics University of Helsinki Gustaf Hällströmin katu 2 Helsinki Finland Department of Experimental Physics Maynooth University Maynooth Co. KildareW23 F2H6 Ireland INFN Sezione di Roma P.le Aldo Moro 5 RomaI-00185 Italy Agenzia Spaziale Italiana Science Data Center Via del Politecnico snc Roma00133 Italy INAF - Osservatorio Astronomico di Roma via di Frascati 33 Monte Porzio Catone Italy Instituut-Lorentz for Theoretical Physics Universiteit Leiden Leiden2333 CA Netherlands Department of Theoretical Physics Univ

We present an analysis of the main systematic effects that could impact the measurement of CMB polarization with the proposed CORE space mission. We employ timeline-to-map simulations to verify that the CORE instrumental set-up and scanning strategy allow us to measure sky polarization to a level of accuracy adequate to the mission science goals. We also show how the CORE observations can be processed to mitigate the level of contamination by potentially worrying systematics, including intensity-to-polarization leakage due to bandpass mismatch, asymmetric main beams, pointing errors and correlated noise. We use analysis techniques that are well validated on data from current missions such as Planck to demonstrate how the residual contamination of the measurements by these effects can be brought to a level low enough not to hamper the scientific capability of the mission, nor significantly increase the overall error budget. We also present a prototype of the CORE photometric calibration pipeline, based on that used for Planck, and discuss its robustness to systematics, showing how CORE can achieve its calibration requirements. While a fine-grained assessment of the impact of systematics requires a level of knowledge of the system that can only be achieved in a future study phase, the analysis presented here strongly suggests that the main areas of concern for the CORE mission can be addressed using existing knowledge, techniques and algorithms. Copyright © 2017, The Authors. All rights reserved.

关键词： Calibration

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Two Remarkably Luminous Galaxy Candidates at z ≈ 10 − 12 Revealed by JWST

arXiv

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arXiv 2022年

作者： Naidu, Rohan P. Oesch, Pascal A. van Dokkum, Pieter Nelson, Erica J. Suess, Katherine A. Brammer, Gabriel Whitaker, Katherine E. Illingworth, Garth Bouwens, Rychard Tacchella, Sandro Matthee, Jorryt Allen, Natalie Bezanson, Rachel Conroy, Charlie Labbe, Ivo Leja, Joel Leonova, Ecaterina Magee, Dan Price, Sedona H. Setton, David J. Strait, Victoria Stefanon, Mauro Toft, Sune Weaver, John R. Weibel, Andrea Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. CambridgeMA02139 United States Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Astronomy Department Yale University 52 Hillhouse Ave New HavenCT06511 United States Department for Astrophysical and Planetary Science University of Colorado BoulderCO80309 United States Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Department of Astronomy University of Massachusetts AmherstMA01003 United States Denmark Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Leiden Observatory Leiden University LeidenNL-2300 RA Netherlands Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Cavendish Laboratory University of Cambridge 19 JJ Thomson Avenue CambridgeCB3 0HE United Kingdom Department of Physics ETH Zürich Wolfgang-Pauli-Strasse 27 Zürich8093 Switzerland Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States GRAPPA Anton Pannekoek Institute for Astronomy Insti

The first few hundred Myrs at z > 10 mark the last major uncharted epoch in the history of the Universe, where only a single galaxy (GNz11 at z ≈ 11) is currently spectroscopically confirmed. Here we present a search for luminous z > 10 galaxies with JWST/NIRCam photometry spanning ≈ 1 − 5µm and covering 49 arcmin2 from the public JWST Early Release Science programs (CEERS and GLASS). Our most secure candidates are two MUV ≈ −21 systems: GLASS-z12 and GLASS-z10. These galaxies display abrupt & 1.8 mag breaks in their spectral energy distributions, consistent with complete absorption of flux bluewards of Lyman-α that is redshifted to z = 12.4+0.1−0.3 and z = 10.4+0.4−0.5. Lower redshift interlopers such as quiescent galaxies with strong Balmer breaks would be comfortably detected at > 5σ in multiple bands where instead we find no flux. From SED modeling we infer that these galaxies have already built up ∼ 109 solar masses in stars over the. 300−400 Myrs after the Big Bang. The brightness of these sources enable morphological constraints. Tantalizingly, GLASS-z10 shows a clearly extended exponential light profile, potentially consistent with a disk galaxy of r50 ≈ 0.7 kpc. These sources, if confirmed, join GNz11 in defying number density forecasts for luminous galaxies based on Schechter UV luminosity functions, which require a survey area > 10× larger than we have studied here to find such luminous sources at such high redshifts. They extend evidence from lower redshifts for little or no evolution in the bright end of the UV luminosity function into the cosmic dawn epoch, with implications for just how early these galaxies began forming. This, in turn, suggests that future deep JWST observations may identify relatively bright galaxies to much earlier epochs than might have been anticipated. © 2022, CC BY.

关键词： Galaxies

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How to Build the Virtual Cell with Artificial Intelligence: Priorities and Opportunities

arXiv

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arXiv 2024年

作者： Bunne, Charlotte Roohani, Yusuf Rosen, Yanay Gupta, Ankit Zhang, Xikun Roed, Marcel Alexandrov, Theo AlQuraishi, Mohammed Brennan, Patricia Burkhardt, Daniel B. Califano, Andrea Cool, Jonah Dernburg, Abby F. Ewing, Kirsty Fox, Emily B. Haury, Matthias Herr, Amy E. Horvitz, Eric Hsu, Patrick D. Jain, Viren Johnson, Gregory R. Kalil, Thomas Kelley, David R. Kelley, Shana O. Kreshuk, Anna Mitchison, Tim Otte, Stephani Shendure, Jay Sofroniew, Nicholas J. Theis, Fabian Theodoris, Christina V. Upadhyayula, Srigokul Valer, Marc Wang, Bo Xing, Eric Yeung-Levy, Serena Zitnik, Marinka Karaletsos, Theofanis Regev, Aviv Lundberg, Emma Leskovec, Jure Quake, Stephen R. Department of Computer Science Stanford University StanfordCA United States Genentech South San FranciscoCA United States Chan Zuckerberg Initiative Redwood CityCA United States School of Computer and Communication Sciences School of Life Sciences EPFL Lausanne Switzerland Arc Institute Palo AltoCA United States KTH Royal Institute of Technology Science for Life Laboratory Department of Protein Science Stockholm Sweden Department of Bioengineering Stanford University StanfordCA United States Department of Pharmacology University of California San DiegoCA United States Department of Bioengineering University of California San DiegoCA United States Department of Systems Biology Columbia University New YorkNY United States Cellarity SomervilleMA United States Vagelos College of Physicians and Surgeons Columbia University Irving Medical Center New YorkNY United States Chan Zuckerberg Biohub New YorkNY United States Department of Molecular and Cell Biology University of California Berkeley BerkeleyCA United States Department of Statistics Stanford University StanfordCA United States Chan Zuckerberg Biohub San Francisco CA United States Chan Zuckerberg Institute for Advanced Biological Imaging Redwood CityCA United States Department of Bioengineering University of California BerkeleyCA United States Microsoft Research RedmondWA United States Center for Computational Biology University of California Berkeley BerkeleyCA United States Google Research Mountain ViewCA United States NewLimit San FranciscoCA United States Schmidt city United States Calico Life Sciences LLC San FranciscoCA United States Chan Zuckerberg Biohub Chicago IL United States Northwestern University EvanstonIL United States Cell Biology and Biophysics Unit European Molecular Biology Laboratory Heidelberg Germany Department of Systems Biology Harvard Medical School BostonMA United States Department of Genome Sciences University of Washington SeattleWA Unit

The cell is arguably the most fundamental unit of life and is central to understanding biology. Accurate modeling of cells is important for this understanding as well as for determining the root causes of disease. Recent advances in artificial intelligence (AI), combined with the ability to generate large-scale experimental data, present novel opportunities to model cells. Here we propose a vision of leveraging advances in AI to construct virtual cells, high-fidelity simulations of cells and cellular systems under different conditions that are directly learned from biological data across measurements and scales. We discuss desired capabilities of such AI Virtual Cells, including generating universal representations of biological entities across scales, and facilitating interpretable in silico experiments to predict and understand their behavior using Virtual Instruments. We further address the challenges, opportunities and requirements to realize this vision including data needs, evaluation strategies, and community standards and engagement to ensure biological accuracy and broad utility. We envision a future where AI Virtual Cells help identify new drug targets, predict cellular responses to perturbations, as well as scale hypothesis exploration. With open science collaborations across the biomedical ecosystem that includes academia, philanthropy, and the biopharma and AI industries, a comprehensive predictive understanding of cell mechanisms and interactions has come into reach. © 2024, CC BY.

关键词： Virtual environments

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HYBRID SATELLITE AND TERRESTRIAL NETWORKS

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INTERNATIONAL JOURNAL OF SATELLITE COMMUNICATIONS 1994年第3期12卷 313-327页

作者： CHITRE, DM SHYY, DJ EPHREMIDES, A GUPTA, S COMSAT Laboratories 22300 Comsat Drive Clarksburg MD 20871–9475 USA. Received his B.Sc. from the University of Bombay India an M.A. in mathematics from the University of Cambridge U.K. and a Ph.D. in physics from the University of Maryland. He is currently an Associate Executive Director of the Network Technology Division at COMSAT Laboratories. He has been involved in research and development activities in ISDN VSAT networks data communications and network systems and architectures. Prior to his current positions Dr. Chitre was a Principal Scientist in the Network Technology Division at COMSAT Laboratories. Dr. Chitre joined COMSAT Laboratories in 1980. He has made major contributions to the analysis and architecture of data communication ISDN and BISDN via satellite. Dr. Chitre directs and participates in the international and national standards activities in ISDN BISDN and data communication as they apply to satellite communication. He was Chairman of the Working Group on Protocols and Network Timing Function of the CCIR/CCITT Joint Ad Hoc Group on ISDN/Satellite Matters during 1990–1992. Currently he is the Chairman of the Working Group on New Technologies in the ITU Intersector Coordinating Group (ICG) on Satellite Matters. Dr. Chitre was a programme manager during 1990 and 1991 on a contract from INTELSAT on systems studies on satellite communications systems architectures for ISDN and broadband ISDN systems. Currently he is the technical manager of the DoD Contract on ATM via satellite demonstration and the programme manager for the INTELSAT contract on analysis and top-level specification of INTELSAT ISDN subnetworks and SDH compatible transport network. Received the B.S. degree in electrical engineering from national Chiao-Tung University Hsin-Chu Taiwan in 1983 and the M.S. and Ph.D. degrees in electrical engineering from Georgia Institute of Technology Atlanta GA in 1986 and 1990 respectively. From June 1987 to October 1987 he worked for the Department of Neurology Emory Univers

The role of satellite communications in networks that provide new services, such as frame relay and multimedia, is investigated. Both passive and active (on-board switching/processing) satellite systems are considered. Novel techniques are developed for each system to demonstrate, via detailed analysis and simulation, how the communications bandwidth agility of multipoint/broadcast satellite channels, and the on-board switching/processing, makes it feasible to provide these new services via hybrid satellite and terrestrial networks in a resource-efficient manner.

关键词： HYBRID NETWORKS ON-BOARD processing FRAME RELAY

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An ALMA survey of submillimetre galaxies in the COSMOS field: The extent of the radio-emitting region revealed by 3 GHz imaging with the Very Large Array

arXiv

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arXiv 2017年

作者： Miettinen, O. Novak, M. Smolčić, V. Delvecchio, I. Aravena, M. Brisbin, D. Karim, A. Murphy, E.J. Schinnerer, E. Albrecht, M. Aussel, H. Bertoldi, F. Capak, P.L. Casey, C.M. Civano, F. Hayward, C.C. Ruiz, N. Herrera Ilbert, O. Jiang, C. Laigle, C. Le Fèvre, O. Magnelli, B. Marchesi, S. McCracken, H.J. Middelberg, E. Arancibia, A.M. Muñoz Navarrete, F. Padilla, N.D. Riechers, D.A. Salvato, M. Scott, K.S. Sheth, K. Tasca, L.A.M. Bondi, M. Zamorani, G. Department of Physics University of Zagreb Bijenička cesta 32 ZagrebHR-10000 Croatia Núcleo de Astronomía Facultad de Ingeniería Universidad Diego Portales Av. Ejército 441 Santiago Chile Argelander-Institut für Astronomie Universität Bonn Auf dem Hügel 71 BonnD-53121 Germany National Radio Astronomy Observatory 520 Edgemont Road CharlottesvilleVA22903 United States Max-Planck-Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany AIM Unité Mixte de Recherche CEA CNRS Université Paris VII UMR n158 Paris France Infrared Processing and Analysis Center California Institute of Technology MC 100-22 770 South Wilson Ave. PasadenaCA91125 United States Spitzer Science Center California Institute of Technology PasadenaCA91125 United States Department of Astronomy University of Texas at Austin 2515 Speedway Blvd Stop C1400 AustinTX78712 United States Yale Center for Astronomy and Astrophysics 260 Whitney Avenue New HavenCT06520 United States Harvard-Smithsonian Center for Astrophysics 60 Garden Street CambridgeMA02138 United States Center for Computational Astrophysics Flatiron Institute 162 Fifth Avenue New YorkNY10010 Astronomisches Institut Ruhr-Universität Bochum Universitätstrasse 150 Bochum44801 Germany UMR 7326 Marseille13388 France CAS Key Laboratory for Research in Galaxies and Cosmology Shanghai Astronomical Observatory Nandan Road 80 Shanghai200030 China Chinese Academy of Sciences South America Center for Astronomy Santiago7591245 Chile Sorbonne Universités UPMC Université Paris 6 et CNRS UMR 7095 Institut d’Astrophysique de Paris 98 bis Boulevard Arago Paris75014 France Dipartimento di Fisica e Astronomia Università di Bologna viale Berti Pichat 6/2 Bologna40127 Italy Instituto de Física y Astronomía Universidad de Valparaíso Av. Gran Bretaña 1111 Valparaíso Chile Instituto de Astrofísica Pontificia Universidad Católica de Chile Avda. Vicuña Mackenna 4860 Santiago Chile Centro de Astro-Ingeniería Pontifici

Context. The observed spatial scale of the radio continuum emission from star-forming galaxies can be used to investigate the spatial extent of active star formation, constrain the importance of cosmic-ray transport, and examine the effects of galaxy interactions. Aims. We determine the radio size distribution of a large sample of 152 submillimetre galaxies (SMGs) in the COSMOS field that were pre-selected at 1.1 mm, and later detected with the Atacama Large Millimetre/submillimetre Array (ALMA) in the observed-frame 1.3 mm dust continuum emission at a signal-to-noise (S/N) ratio of ≥ 5. Methods. We used the deep, subarcsecond-resolution (1σ = 2.3 µJy beam−1;0′′ . 75) centimetre radio continuum observations taken by the Karl G. Jansky Very Large Array (VLA)-COSMOS 3 GHz Large Project. Results. One hundred and fifteen of the 152 target SMGs (76% ± 7%) were found to have a 3 GHz counterpart (≥ 4.2σ), which renders the radio detection rate notably high. The median value of the deconvolved major axis full width at half maximum (FWHM) size at 3 GHz is derived to be 0′′ . 59 ± 0′′ . 05, or 4.6 ± 0.4 kpc in physical units, where the median redshift of the sources is z = 2.23 ± 0.13 (23% are spectroscopic and 77% are photometric values). The radio sizes are roughly log-normally distributed, and they show no evolutionary trend with redshift, or difference between different galaxy morphologies. We also derived the spectral indices between 1.4 and 3 GHz, and 3 GHz brightness temperatures for the sources, and the median values were found to be α***4 GHz = −0.67 (S ν ∝ να ) and TB = 12.6 ± 2 K. Three of the target SMGs, which are also detected with the Very Long Baseline Array (VLBA) at 1.4 GHz (AzTEC/C24b, 61, and 77a), show clearly higher brightness temperatures than the typical values, reaching TB (3 GHz) > 104.03 K for AzTEC/C61. Conclusions. The derived median radio spectral index agrees with a value expected for optically thin non-thermal synchrotron radiation, and the

关键词： Normal distribution

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Resolving the nature and putative nebular emission of GS9422: an obscured AGN without exotic stars

arXiv

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arXiv 2024年

作者： Tacchella, Sandro McClymont, William Scholtz, Jan Maiolino, Roberto Ji, Xihan Villanueva, Natalia C. Charlot, Stéphane D'Eugenio, Francesco Helton, Jakob M. Williams, Christina C. Witstok, Joris Bhatawdekar, Rachana Carniani, Stefano Chevallard, Jacopo Curti, Mirko Hainline, Kevin Ji, Zhiyuan Johnson, Benjamin D. Leja, Joel Li, Yijia Maseda, Michael V. Puskás, Dávid Rieke, Marcia Robertson, Brant Shivaei, Irene Silcock, Maddie S. Simmonds, Charlotte Übler, Hannah Willmer, Christopher N.A. Willott, Chris Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Cavendish Laboratory University of Cambridge 19 JJ Thomson Avenue CambridgeCB3 0HE United Kingdom Sorbonne Université CNRS UMR 7095 Institut d'Astrophysique de Paris 98 bis bd Arago Paris75014 France Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States NSF's National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Camino Bajo del Castillo s/n Madrid Villanueva de la Cañada28692 Spain Scuola Normale Superiore Piazza dei Cavalieri 7 PisaI-56126 Italy Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching85748 Germany Center for Astrophysics | Harvard & Smithsonian 60 Garden St. CambridgeMA02138 United States Department of Astronomy & Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational & Data Sciences The Pennsylvania State University University ParkPA16802 United States Institute for Gravitation and the Cosmos The Pennsylvania State University University ParkPA16802 United States Department of Astronomy University of Wisconsin-Madison 475 N. Charter St. MadisonWI53706 United States Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA96054 United States Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High Street Santa CruzCA95064 United States CSIC-INTA Ctra. de Ajalvir km 4 Torrejón de Ardoz MadridE-28850 Spain Centre for Astrophysics Research Department of Physics Astronomy and Mathematics University of Hertfordshire HatfieldAL10 9AB United Kingdom NRC Herzberg 5071 West Saanich Rd VictoriaBCV9E 2E7 Canada

Understanding the sources that power nebular emission in high-redshift galaxies is fundamentally important not only for shedding light onto the drivers of reionisation, but to constrain stellar populations and the growth of black holes. Here we focus on an individual object, GS9422, a galaxy at zspec = 5.943 with exquisite data from the JADES and JEMS surveys, including 14-band JWST/NIRCam photometry and deep NIRSpec prism and grating spectroscopy. We map the continuum emission and nebular emission lines across the galaxy on 0.2-kpc scales. GS9422 has been claimed to have nebular-dominated continuum and an extreme stellar population with top-heavy initial mass *** find clear evidence for different morphologies in the emission lines, the rest-UV and rest-optical continuum emission, demonstrating that the full continuum cannot be dominated by nebular emission. While multiple models reproduce the spectrum reasonably well, our preferred model with a type-2 active galactic nucleus (AGN) and local damped Ly-α (DLA) clouds can explain both the spectrum and the wavelength-dependent morphology. The AGN powers the off-planar nebular emission, giving rise to the Balmer jump and the emission lines, including Ly-α, which therefore does not suffer DLA absorption. A central, young stellar component dominates the rest-UV emission and - together with the DLA clouds - leads to a spectral turn-over. A disc-like, older stellar component explains the flattened morphology in the rest-optical continuum. We conclude that GS9422 is consistent with being a normal galaxy with an obscured, type-2 AGN - a simple scenario, without the need for exotic stellar populations. © 2024, CC BY.

关键词： Galaxies

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Preliminary Target Selection for the DESI Bright Galaxy Survey (BGS)

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research Notes of the AAS 2020年第10期4卷

作者： Omar Ruiz-Macias Pauline Zarrouk Shaun Cole Peder Norberg Carlton Baugh David Brooks Arjun Dey Yutong Duan Sarah Eftekharzadeh Daniel J. Eisenstein Jaime E. Forero-Romero Enrique Gaztañaga ChangHoon Hahn Robert Kehoe Martin Landriau Dustin Lang Michael E. Levi John Lucey Aaron M. Meisner John Moustakas Adam D. Myers Nathalie Palanque-Delabrouille Claire Poppett Francisco Prada Anand Raichoor David J. Schlegel Michael Schubnell Gregory Tarlé David H. Weinberg M. J. Wilson Christophe Yèche Institute for Computational Cosmology Department of Physics Durham University South Road Durham DH1 3LE UK Institute for Data Science Durham University South Road Durham DH1 3LE UK Centre for Extragalactic Astronomy Department of Physics Durham University South Road Durham DH1 3LE UK Department of Physics and Astromomy University College London Gower Street London WC1e 6BT UK NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. Tucson AZ 85719 USA Physics Department Boston University Boston MA 02215 USA Department of Physics and Astronomy The University of Utah 115 South 1400 East Salt Lake City UT 84112 USA Harvard-Smithsonian Center for Astrophysics 60 Garden Street Cambridge MA 02138 USA Departamento de Física Universidad de los Andes Cra. 1 No. 18A-10 CP 111711 Bogotá Colombia Institute of Space Sciences (ICE CSIC) E-08193 Barcelona Spain Institut d'Estudis Espacials de Catalunya (IEEC) E-08034 Barcelona Spain Lawrence Berkeley National Laboratory 1 Cyclotron Road Berkeley CA 94720 USA Berkeley Center for Cosmological Physics UC Berkeley CA 94720 USA Department of Physics Southern Methodist University 3215 Daniel Avenue Dallas TX 75275 USA Perimeter Institute for Theoretical Physics 31 Caroline Street N Waterloo Ontario N2L 2Y5 Canada Department of Physics and Astronomy University of Waterloo Waterloo ON N2L 3G1 Canada Department of Physics and Astronomy Siena College 515 Loudon Road Loudonville NY 12211 USA University of Wyoming 1000 E. University Ave. Laramie WY 82071 USA IRFU CEA Université Paris-Saclay F-91191 Gif-sur-Yvette France Space Sciences Laboratory at University of California 7 Gauss Way Berkeley CA 94720 USA Instituto de Astrofísica de Andalucía (CSIC) Glorieta de la Astronomía E-18080 Granada Spain Institute of Physics Laboratory of Astrophysics Ecole Polytechnique Fédérale de Lausanne (EPFL) Observatoire de Sauverny 1290 Versoix Switzerland Department of Physics University of

The Dark Energy Spectroscopic Instrument (DESI) will execute a nearly magnitude-limited survey of low redshift galaxies (0.05 ≤ z ≤ 0.4, median z ≈ 0.2). Clustering analyses of this Bright Galaxy Survey (BGS) will yield the most precise measurements to date of baryon acoustic oscillations and redshift-space distortions at low redshift. DESI BGS will comprise two target classes: (i) BRIGHT (r < 19.5 mag), and (ii) FAINT (19.5 < r < 20 mag). Here we present a summary of the star-galaxy separation, and different photometric and geometrical masks, used in BGS to reduce the number of spurious targets. The selection results in a total density of ~800 objects deg−2 for the BRIGHT and ~600 objects deg−2 for the FAINT selections. A full characterization of the BGS selection can be found in Ruiz-Macias et al.

关键词： Galaxies Redshift surveys Observational cosmology Large-scale structure of the universe Catalogs

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LiteBIRD Science Goals and Forecasts. Mapping the Hot Gas in the Universe

arXiv

引用

arXiv 2024年

作者： Remazeilles, M. Douspis, M. Rubiño-Martín, J.A. Banday, A.J. Chluba, J. de Bernardis, P. De Petris, M. Hernández-Monteagudo, C. Luzzi, G. Macias-Perez, J. Masi, S. Namikawa, T. Salvati, L. Tanimura, H. Aizawa, K. Anand, A. Aumont, J. Baccigalupi, C. Ballardini, M. Barreiro, R.B. Bartolo, N. Basak, S. Bersanelli, M. Blinov, D. Bortolami, M. Brinckmann, T. Calabrese, E. Campeti, P. Carinos, E. Carones, A. Casas, F.J. Cheung, K. Clermont, L. Columbro, F. Coppolecchia, A. Cuttaia, F. de Haan, T. de la Hoz, E. Torre, S. Della Diego-Palazuelos, P. D’Alessandro, G. Eriksen, H.K. Finelli, F. Fuskeland, U. Galloni, G. Galloway, M. Gervasi, M. Génova-Santos, R.T. Ghigna, T. Giardiello, S. Gimeno-Amo, C. Gjerløw, E. González, R. González Gruppuso, A. Hazumi, M. Henrot-Versillé, S. Hergt, L.T. Herranz, D. Kohri, K. Komatsu, E. Lamagna, L. Lattanzi, M. Leloup, C. Levrier, F. Lonappan, A.I. López-Caniego, M. Maffei, B. Martínez-González, E. Matarrese, S. Matsumura, T. Micheli, S. Migliaccio, M. Monelli, M. Montier, L. Morgante, G. Nagano, Y. Nagata, R. Novelli, A. Omae, R. Pagano, L. Paoletti, D. Pavlidou, V. Piacentini, F. Pinchera, M. Polenta, G. Porcelli, L. Ritacco, A. Ruiz-Granda, M. Sakurai, Y. Scott, D. Shiraishi, M. Stever, S.L. Sullivan, R.M. Takase, Y. Tassis, K. Terenzi, L. Tomasi, M. Tristram, M. Vacher, L. van Tent, B. Vielva, P. Wehus, I.K. Westbrook, B. Weymann-Despres, G. Wollack, E.J. Zannoni, M. Zhou, Y. Avenida los Castros SN Santander39005 Spain Université Paris-Saclay CNRS Institut d’Astrophysique Spatiale Orsay91405 France Instituto de Astrofísica de Canarias La Laguna Canary Islands TenerifeE-38200 Spain Tenerife La LagunaE-38206 Spain IRAP Université de Toulouse CNRS CNES UPS Toulouse France Jodrell Bank Centre for Astrophysics Alan Turing Building Department of Physics and Astronomy School of Natural Sciences The University of Manchester Oxford Road ManchesterM13 9PL United Kingdom Dipartimento di Fisica Università La Sapienza P. le A. Moro 2 Roma Italy INFN Sezione di Roma P.le A. Moro 2 Roma00185 Italy Space Science Data Center Italian Space Agency via del Politecnico Roma00133 Italy Université Grenoble Alpes CNRS LPSC-IN2P3 53 avenue des Martyrs Grenoble38000 France UTIAS The University of Tokyo Chiba Kashiwa277-8583 Japan The University of Tokyo Department of Physics Tokyo113-0033 Japan Dipartimento di Fisica Università di Roma Tor Vergata Via della Ricerca Scientifica 1 Roma00133 Italy Via Bonomea 265 Trieste34136 Italy INFN Sezione di Trieste via Valerio 2 Trieste34127 Italy IFPU Via Beirut 2 Grignano Trieste34151 Italy Dipartimento di Fisica e Scienze della Terra Università di Ferrara Via Saragat 1 Ferrara44122 Italy INFN Sezione di Ferrara Via Saragat 1 Ferrara44122 Italy INAF - OAS Bologna via Piero Gobetti 93/3 Bologna40129 Italy Dipartimento di Fisica e Astronomia "G. Galilei" Università degli Studi di Padova via Marzolo 8 PadovaI-35131 Italy INFN Sezione di Padova via Marzolo 8 PadovaI-35131 Italy INAF Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy School of Physics Indian Institute of Science Education and Research Thiruvananthapuram Maruthamala PO Vithura Kerala Thiruvananthapuram695551 India Dipartimento di Fisica Università degli Studi di Milano Via Celoria 16 Milano20133 Italy INFN Sezione di Milano Via Celoria 16 Milano20133 I

We assess the capabilities of the LiteBIRD mission to map the hot gas distribution in the Universe through the thermal Sunyaev-Zeldovich (SZ) effect. Our analysis relies on comprehensive simulations incorporating various sources of Galactic and extragalactic foreground emission, while accounting for the specific instrumental characteristics of the LiteBIRD mission, such as detector sensitivities, frequency-dependent beam convolution, inhomogeneous sky scanning, and 1/f noise. We implement a tailored component-separation pipeline to map the thermal SZ Compton y-parameter over 98 % of the sky. Despite lower angular resolution for galaxy cluster science, LiteBIRD provides full-sky coverage and, compared to the Planck satellite, enhanced sensitivity, as well as more frequency bands to enable the construction of an all-sky thermal SZ y-map, with reduced foreground contamination at large and intermediate angular scales. By combining LiteBIRD and Planck channels in the component-separation pipeline, we also obtain an optimal y-map that leverages the advantages of both experiments, with the higher angular resolution of the Planck channels enabling the recovery of compact clusters beyond the LiteBIRD beam limitations, and the numerous sensitive LiteBIRD channels further mitigating foregrounds. The added value of LiteBIRD is highlighted through the examination of maps, power spectra, and one-point statistics of the various sky components. After component separation, the 1/f noise from LiteBIRD’s intensity channels is effectively mitigated below the level of the thermal SZ signal at all multipoles. Cosmological constraints on S8 = σ8 (Ωm/0.3)0.5 obtained from the LiteBIRD-Planck combined y-map power spectrum exhibits a 15 % reduction in uncertainty compared to constraints derived from Planck alone. This improvement can be attributed to the increased portion of uncontaminated sky available in the LiteBIRD-Planck combined y-map. Copyright © 2024, The Authors. All rights reserved

关键词： Cosmology

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The ALPINE-ALMA [CII] Survey: The population of [CII]-undetected galaxies and their role in the L[CII]-SFR relation

arXiv

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arXiv 2022年

作者： Romano, Michael Morselli, L. Cassata, P. Ginolfi, M. Schaerer, D. Béthermin, M. Capak, P. Faisst, A. Le Fèvre, O. Silverman, J.D. Yan, L. Bardelli, S. Boquien, M. Dessauges-Zavadsky, M. Fujimoto, S. Hathi, N.P. Jones, G.C. Koekemoer, A.M. Lemaux, B.C. Méndez-Hernández, H. Narayanan, D. Talia, M. Vergani, D. Zamorani, G. Zucca, E. Dipartimento di Fisica e Astronomia Università di Padova Vicolo dell'Osservatorio 3 PadovaI-35122 Italy INAF-Osservatorio Astronomico di Padova Vicolo dell'Osservatorio 5 PadovaI-35122 Italy National Center for Nuclear Research ul. Pasteura 7 Warsaw02-093 Poland Associazione Big Data via Piero Gobetti 101 Bologna40129 Italy European Southern Observatory Karl-Schwarzschild-Strasse 2 Garching85748 Germany Observatoire de Genève Université de Genève 51 Ch. des Maillettes Versoix1290 Switzerland Aix Marseille Univ CNRS CNES LAM Marseille France Infrared Processing and Analysis Center California Institute of Technology PasadenaCA91125 United States IPAC California Institute of Technology 1200 East California Boulevard PasadenaCA91125 United States Kavli Institute for the Physics and Mathematics of the Universe The University of Tokyo Kashiwa Chiba277-8583 Japan Department of Astronomy School of Science The University of Tokyo 7-3-1 Hongo Bunkyo Tokyo113-0033 Japan The Caltech Optical Observatories California Institute of Technology PasadenaCA91125 United States INAF-Osservatorio di Astrofisica e Scienza Dello Spazio via Gobetti 93/3 BolognaI-40129 Italy Universidad de Antofagasta Avenida Angamos 601 Antofagasta Chile Jagtvej 128 Copenhagen NDK22000 Denmark Niels Bohr Institute University of Copenhagen Lyngbyvej 2 Copenhagen ØDK2100 Denmark Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Cavendish Laboratory University of Cambridge 19 J. J. Thomson Ave. CambridgeCB3 0HE United Kingdom Kavli Institute for Cosmology University of Cambridge Madingley Road CambridgeCB3 0HA United Kingdom Department of Physics and Astronomy University of California Davis One Shields Ave. DavisCA95616 United States Gemini Observatory NSF's NOIRLab 670 N. A'ohoku Place HiloHI96720 United States Insituto de Física y Astronomía Universidad de Valparaíso Avda. Gran Bretaña 1111 Valparaíso2340000 Chi

The [CII] 158 μm emission line represents so far one of the most profitable tools for the investigation of the high-redshift galaxies in the early Universe. Being one of the brightest cooling lines in the rest-frame far-infrared regime of star-forming galaxies, it has been successfully exploited as a tracer of star-formation rate (SFR) in local sources. The picture is more complex at higher redshifts, where its usability in this context is still under investigation. Recent results from the ALMA Large Program to INvestigate [CII] at Early times (ALPINE) survey suggest that there is no (or weak) evolution of the L[CII]-SFR relation up to z ∼ 6 but their reliability is hampered by the presence of a large population of [CII] non-detected galaxies. In this work, we characterize the population of [CII] non-detections in ALPINE. By stacking their ALMA spectra, we obtain a signal detected at ∼ 5.1σ, resulting in a [CII] luminosity of log(L[CII]/Lo) ∼ 7.8. When combining this value with those from the [CII] detections, we find a L[CII]-SFR relation with a slope b = 1.14±0.11, in agreement within the uncertainties both with the linear relation found in the local Universe, and with the previous findings from ALPINE at z ∼ 5. This suggests that the [CII] line can be considered a good tracer of star formation up to the distant Universe. Finally, we show that the galaxies of our sample that most deviate from the observed L[CII]-SFR relation could suffer from a less precise redshift estimation, perhaps artificially reducing their [CII] luminosity. In this respect, we claim that there is no evidence in favour of a deficit of [CII] content in high-z galaxies, in contrast with earlier studies. Copyright © 2022, The Authors. All rights reserved.

关键词： Galaxies

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