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arXiv 2024年

作者： Price, Sedona H. Bezanson, Rachel Labbe, Ivo Furtak, Lukas J. de Graaff, Anna Greene, Jenny E. Kokorev, Vasily Setton, David J. Suess, Katherine A. Brammer, Gabriel Cutler, Sam E. Leja, Joel Pan, Richard Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Atek, Hakim Burgasser, Adam J. Chemerynska, Iryna Dayal, Pratika Feldmann, Robert Förster Schreiber, Natascha M. Fudamoto, Yoshinobu Fujimoto, Seiji Glazebrook, Karl Goulding, Andy D. Khullar, Gourav Kriek, Mariska Marchesini, Danilo Maseda, Michael V. Miller, Tim B. Muzzin, Adam Nanayakkara, Themiya Nelson, Erica Oesch, Pascal A. Shipley, Heath Smit, Renske Taylor, Edward N. van Dokkum, Pieter Williams, Christina C. Zitrin, Adi Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Physics Department Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States Kavli Institute for Particle Astrophysics and Cosmology Department of Physics Stanford University StanfordCA94305 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 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 Physics and Astronomy Tufts University 574 Boston Ave. MedfordMA02155 United States Denmark Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Department of Astronomy & Astrophysics UC San Diego La Jolla CA United States Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Department of Astrophysics University of Zurich CH-8057 Switzerland Max-Planck-Institut für extraterrestrische Physik Giessenbachstrasse 1 Garching85748 Germany Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Leiden Observatory

We present the design and observations of low resolution JWST/NIRSpec PRISM spectroscopy from the Ultradeep NIRSpec and NIRCam ObserVations before the Epoch of Reionization (UNCOVER) Cycle 1 JWST Treasury program. Targets are selected using JWST/NIRCam photometry from UNCOVER and other programs, and cover a wide range of categories and redshifts to ensure the legacy value of the survey. These categories include the first galaxies at z 10, faint galaxies during the Epoch of Reionization (z ∼ 6 − 8), high redshift AGN (z 6), Population III star candidates, distant quiescent and dusty galaxies (1 z 6), and filler galaxies sampling redshift–color–magnitude space from z ∼ 0.1 − 13. Seven NIRSpec MSA masks across the extended Abell 2744 cluster were observed, along with NIRCam parallel imaging in 8 filters (F090W, F115W, F150W, F200W, F277W, F356W, F410M, F444W, F480M) over a total area of ∼26 arcmin2, overlapping existing HST coverage from programs including the Hubble Frontier Fields and BUFFALO. We successfully observed 553 objects down to mF444W ∼ 30AB, and by leveraging mask overlaps, we reach total on-target exposure times ranging from 2.4 − 16.7h. We demonstrate the success rate and distribution of confirmed redshifts, and also highlight the rich information revealed by these ultradeep spectra for a subset of our targets. An updated lens model of Abell 2744 is also presented, including 14 additional spectroscopic redshifts and finding a total cluster mass of MSL = (2.1 ± 0.3) × 1015 M☉. We publicly release reduced 1D and 2D spectra for all objects observed in Summer 2023 along with a spectroscopic redshift catalog and the updated lens model of the cluster (https://***/***). Copyright © 2024, The Authors. All rights reserved.

关键词： Prisms

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Evidence for Extended Hydrogen-Poor CSM in the Three-Peaked Light Curve of Stripped Envelope Ib Supernova

arXiv

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arXiv 2022年

作者： Zenati, Yossef Wang, Qinan Bobrick, Alexey DeMarchi, Lindsay Glanz, Hila Rozner, Mor Rest, Armin Metzger, Brian D. Margutti, Raffaella Gomez, Sebastian Smith, Nathan Toonen, Silvia Bright, Joe S. Norman, Colin Foley, Ryan J. Gagliano, Alexander Krolik, Julian H. Smartt, Stephen J. Villar, Ashley V. Narayan, Gautham Fox, Ori Auchettl, Katie Brethauer, Daniel Clocchiatti, Alejandro Coelln, Sophie V. Coppejans, Deanne L. Dimitriadis, Georgios Doroszmai, Andris Drout, Maria Jacobson-Galan, Wynn Gao, Bore Ridden-Harper, Ryan Kilpatrick, Charles Donald Laskar, Tanmoy Matthews, David Rest, Sofia Smith, Ken W. Stauffer, Candice McKenzie Stroh, Michael C. Strolger, Louis-Gregory Terreran, Giacomo Pierel, Justin D.R. Piro, Anthony L. Physics and Astronomy Department Johns Hopkins University BaltimoreMD21218 United States Technion - Israel Institute of Technology Physics department Haifa3200002 Israel Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Space Telescope Science Institute 3700 San Martin Dr. BaltimoreMD21218 United States Department of Physics Columbia Astrophysics Laboratory Columbia University Pupin Hall New YorkNY10027 United States Center for Computational Astrophysics Flatiron Institute 162 5th Ave New YorkNY10010 United States Department of Astronomy and Astrophysics University of California BerkeleyCA94720 United States Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States Anton Pannekoek Institute for Astronomy University of Amsterdam Amsterdam1090 GE Netherlands Department of Astronomy University of California BerkeleyCA94720-3411 United States Astrophysics Department of Physics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green St IL61801 United States Center for Astrophysical Surveys National Center for Supercomputing Applications UrbanaIL61801 United States Center for Astrophysical Surveys UrbanaIL61801 United States Astrophysics Research Centre School of Mathematics and Physics Queens University Belfast BelfastBT7 1NN United Kingdom Department of Astronomy and Astrophysics Pennsylvania State University 525 Davey Laboratory 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 School of Physics The University of Melbourne VIC3010 Australia Australia Insti

We present multi-band ATLAS photometry for SN 2019tsf, a stripped-envelope Type Ib supernova (SESN). The SN shows a triple-peaked light curve and a late (re-)brightening, making it unique among stripped-envelope systems. The re-brightening observations represent the latest photometric measurements of a multi-peaked Type Ib SN to date. As late-time photometry and spectroscopy suggest no hydrogen, the potential circumstellar material (CSM) must be H-poor. Moreover, late (>150 days) spectra show no signs of narrow emission lines, further disfavouring CSM interaction. On the contrary, an extended CSM structure is seen through a follow-up radio campaign with Karl G. Jansky Very Large Array (VLA), indicating a source of bright optically thick radio emission at late times, which is highly unusual among H-poor SESNe. We attribute this phenomenology to an interaction of the supernova ejecta with spherically-asymmetric CSM, potentially disk-like, and we present several models that can potentially explain the origin of this rare Type Ib supernova. The warped disc model paints a novel picture, where the tertiary companion perturbs the progenitors CSM, that can explain the multi-peaked light curves of SNe, and here we apply it to SN 2019tsf. This SN 2019tsf is likely a member of a new sub-class of Type Ib SNe and among the recently discovered class of SNe that undergo mass transfer at the moment of explosion. © 2022, CC BY-SA.

关键词： Supernovae

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Broad-Line AGN at 3.5 < z < 6: The Black Hole Mass Function and a Connection with Little Red Dots

arXiv

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arXiv 2024年

作者： Taylor, Anthony J. Finkelstein, Steven L. Kocevski, Dale D. Jeon, Junehyoung Bromm, Volker Amorín, Ricardo O. Haro, Pablo Arrabal Backhaus, Bren E. Bagley, Micaela B. Bañados, Eduardo Bhatawdekar, Rachana Brooks, Madisyn Calabrò, Antonello Chávez Ortiz, Óscar A. Cheng, Yingjie Cleri, Nikko J. Cole, Justin W. Davis, Kelcey Dickinson, Mark Donnan, Callum Dunlop, James S. Ellis, Richard S. Fernández, Vital Fontana, Adriano Fujimoto, Seiji Giavalisco, Mauro Grazian, Andrea Guo, Jingsong Hathi, Nimish P. Holwerda, Benne W. Hirschmann, Michaela Inayoshi, Kohei Kartaltepe, Jeyhan S. Khusanova, Yana Koekemoer, Anton M. Kokorev, Vasily Larson, Rebecca L. Leung, Gene C.K. Lucas, Ray A. McLeod, Derek J. Napolitano, Lorenzo Onoue, Masafusa Pacucci, Fabio Papovich, Casey Pérez-González, Pablo G. Pirzkal, Nor Somerville, Rachel S. Trump, Jonathan R. Wilkins, Stephen M. Yung, L.Y. Aaron Zhang, Haowen Department of Astronomy The University of Texas at Austin AustinTX United States Department of Physics and Astronomy Colby College WatervilleME04901 United States Apartado 3004 Granada18080 Spain NSF's National Optical-Infrared Astronomy Research Laboratory 950 N. Cherry Ave. TucsonAZ85719 United States Department of Physics University of Connecticut 196 Auditorium Road Unit 3046 StorrsCT06269 United States Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Camino Bajo del Castillo s/n Villanueva de la Cañada Madrid28692 Spain INAF - Osservatorio Astronomico di Roma via di Frascati 33 Monte Porzio Catone00078 Italy University of Massachusetts Amherst 710 North Pleasant Street AmherstMA01003-9305 United States Department of Astronomy and Astrophysics The Pennsylvania State University University ParkPA16802 United States Institute for Computational and 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 Physics and Astronomy Texas A&M University College StationTX77843-4242 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Texas A&M University College StationTX77843-4242 United States Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom SUPA Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom Instituto de Investigación Multidisciplinar en Ciencia y Tecnología Universidad de La Serena Raul Bitrán 1305 La Serena2204000 Chile Jagtvej 128 Copenhagen NDK2200 Denmark Niels Bohr Institute University of Copenhagen Lyngbyvej 2 Copenhagen ØDK2100 Denmark INAF-Osservatorio Astronomico di Padova Vicolo dell'

We present a sample of 50 Hα detected broad-line active galactic nuclei (BLAGN) at redshifts 3.5 opt > 0), independent of the contributions of emission lines to the broadband photometry. We construct the black hol... 详细信息

关键词： Active Galactic Nuclei

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UNCOVER: Illuminating the Early Universe — JWST/NIRSpec Confirmation of z > 12 Galaxies

arXiv

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arXiv 2023年

作者： Wang, Bingjie Fujimoto, Seiji Labbé, Ivo Furtak, Lukas J. Miller, Tim B. Setton, David J. Zitrin, Adi Atek, Hakim Bezanson, Rachel Brammer, Gabriel Leja, Joel Oesch, Pascal A. Price, Sedona H. Chemerynska, Iryna Cutler, Sam E. Dayal, Pratika van Dokkum, Pieter Goulding, Andy D. Greene, Jenny E. Fudamoto, Y. Khullar, Gourav Kokorev, Vasily Marchesini, Danilo Pan, Richard Weaver, John R. Whitaker, Katherine E. Williams, Christina C. 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 The University of Texas at Austin AustinTX78712 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Department of Astronomy Yale University New HavenCT06511 United States Department of Physics & Astronomy Northwestern University IL60201 United States Department of Physics & Astronomy and PITT PACC University of Pittsburgh PittsburghPA15260 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago ParisF-75014 France Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Department of Astronomy University of Massachusetts AmherstMA01003 United States Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo Japan Department of Physics & Astronomy Tufts University MA02155 United States NSF’s National Optical-Infrared Astronomy Research Laboratory TucsonAZ85719 United States Steward Observatory University of Arizona TucsonAZ8

Observations of high-redshift galaxies provide a critical direct test to the theories of early galaxy formation, yet to date, only three have been spectroscopically confirmed at z > 12. Due to strong gravitational lensing over a wide area, the galaxy cluster field A2744 is ideal for searching for the earliest galaxies. Here we present JWST/NIRSpec observations of two galaxies: a robust detection at (formula presented), and a plausible candidate at (formula presented). The galaxies are discovered in JWST/NIRCam imaging and their distances are inferred with JWST/NIRSpec spectroscopy, all from the JWST Cycle 1 UNCOVER Treasury survey. Detailed stellar population modeling using JWST NIRCam and NIRSpec data corroborates the primeval characteristics of these galaxies: low mass (∼ 108 M☉), young, rapidly-assembling, metal-poor, and star-forming. Interestingly, both galaxies are spatially resolved, having lensing-corrected rest-UV effective radii on the order of 300–400 pc, which are notably larger than other spectroscopically confirmed systems at similar redshifts. The observed dynamic range of z 10 sizes spans over 1 order of magnitude, implying a significant scatter in the size–mass relation at early times. Deep into the epoch of reionization, these discoveries elucidate the emergence of the first galaxies. Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

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PLUMED Tutorials: a collaborative, community-driven learning ecosystem

arXiv

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arXiv 2024年

作者： Tribello, Gareth A. Bonomi, Massimiliano Bussi, Giovanni Camilloni, Carlo Armstrong, Blake I. Arsiccio, Andrea Aureli, Simone Ballabio, Federico Bernetti, Mattia Bonati, Luigi Brookes, Samuel G.H. Faidon Brotzakis, Z. Capelli, Riccardo Ceriotti, Michele Chan, Kam-Tung Cossio, Pilar Dasetty, Siva Donadio, Davide Ensing, Bernd Ferguson, Andrew L. Fraux, Guillaume Gale, Julian D. Gervasio, Francesco Luigi Giorgino, Toni Herringer, Nicholas S.M. Hocky, Glen M. Hoff, Samuel E. Invernizzi, Michele Languin-Cattoën, Olivier Leone, Vanessa Limongelli, Vittorio Lopez-Acevedo, Olga Marinelli, Fabrizio Martinez, Pedro Febrer Masetti, Matteo Mehdi, Shams Michaelides, Angelos Murtada, Mhd Hussein Parrinello, Michele Piaggi, Pablo M. Pietropaolo, Adriana Pietrucci, Fabio Pipolo, Silvio Pritchard, Claire Raiteri, Paolo Raniolo, Stefano Rapetti, Daniele Rizzi, Valerio Rydzewski, Jakub Salvalaglio, Matteo Schran, Christoph Seal, Aniruddha Zadeh, Armin Shayesteh Silva, Tomás F.D. Spiwok, Vojtěch Stirnemann, Guillaume Sucerquia, Daniel Tiwary, Pratyush Valsson, Omar Vendruscolo, Michele Voth, Gregory A. White, Andrew D. Wu, Jiangbo Centre for Quantum Materials and Technology School of Mathematics and Physics Queen’s University Belfast United Kingdom Institut Pasteur Université Paris Cité CNRS UMR 3528 Computational Structural Biology Unit Paris France Via Bonomea 265 Trieste34136 Italy Department of Biosciences University of Milano Milano Italy School of Molecular and Life Sciences Curtin University GPO Box U1987 PerthWA6845 Australia Coriolis Pharma Fraunhoferstrasse 18b Martinsried82152 Germany School of Pharmaceutical Sciences University of Geneva Rue Michel-Servet 1 GenevaCH-1206 Switzerland Institute of Pharmaceutical Sciences of Western Switzerland University of Geneva GenevaCH-1206 Switzerland Swiss Bioinformatics Institute University of Geneva GenevaCH-1206 Switzerland Via Celoria 26 Milan20133 Italy Department of Biomolecular Sciences University of Urbino "Carlo Bo" Piazza Rinascimento 6 Urbino61029 Italy Department of Pharmacy and Biotechnology Alma Mater Studiorum University of Bologna Via Belmeloro 6 Bologna40126 Italy Atomistic Simulations Italian Institute of Technology Genova Italy Yusuf Hamied Department of Chemistry University of Cambridge CambridgeCB2 1EW United Kingdom Institute for Bioinnovation Biomedical Sciences Research Center "Alexander Fleming" Vari16672 Greece Laboratory of Computational Science and Modeling Institut des Matériaux École Polytechnique Fédérale de Lausanne Lausanne1015 Switzerland Department of Chemistry University of California Davis DavisCA95616 United States Center for Computational Mathematics Flatiron Institute New YorkNY10010 United States Center for Computational Biology Flatiron Institute New YorkNY10010 United States Pritzker School of Molecular Engineering University of Chicago ChicagoIL60637 United States AI4Science Lab Informatics Institute University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands Computational Chemistry Group Van’t Hoff Institute for Molecular Sciences Unive

In computational physics, chemistry, and biology, the implementation of new techniques in a shared and open source software lowers barriers to entry and promotes rapid scientific progress. However, effectively training new software users presents several challenges. Common methods like direct knowledge transfer and in-person workshops are limited in reach and comprehensiveness. Furthermore, while the COVID-19 pandemic highlighted the benefits of online training, traditional online tutorials can quickly become outdated and may not cover all the software’s functionalities. To address these issues, here we introduce "PLUMED Tutorials", a collaborative model for developing, sharing, and updating online tutorials. This initiative utilizes repository management and continuous integration to ensure compatibility with software updates. Moreover, the tutorials are interconnected to form a structured learning path and are enriched with automatic annotations to provide broader context. This paper illustrates the development, features, and advantages of PLUMED Tutorials, aiming to foster an open community for creating and sharing educational resources. © 2024, CC BY.

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A "Black Hole Star" Reveals the Remarkable Gas-Enshrouded Hearts of the Little Red Dots

arXiv

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arXiv 2025年

作者： Naidu, Rohan P. Matthee, Jorryt Katz, Harley de Graaff, Anna Oesch, Pascal Smith, Aaron Greene, Jenny E. Brammer, Gabriel Weibel, Andrea Hviding, Raphael Chisholm, John Labbé, Ivo Simcoe, Robert A. Witten, Callum Atek, Hakim Baggen, Josephine F.W. Belli, Sirio Bezanson, Rachel Boogaard, Leindert A. Bose, Sownak Covelo-Paz, Alba Dayal, Pratika Fudamoto, Yoshinobu Furtak, Lukas J. Giovinazzo, Emma Goulding, Andy Gronke, Max Heintz, Kasper E. Hirschmann, Michaela Illingworth, Garth Inoue, Akio K. Johnson, Benjamin D. Leja, Joel Leonova, Ecaterina McConachie, Ian Maseda, Michael V. Natarajan, Priyamvada Nelson, Erica Setton, David J. Shivaei, Irene Sobral, David Stefanon, Mauro Tacchella, Sandro Toft, Sune Torralba, Alberto van Dokkum, Pieter van der Wel, Arjen Volonteri, Marta Walter, Fabian Wang, Bingjie Watson, Darach MIT Kavli Institute for Astrophysics and Space Research 70 Vassar Street CambridgeMA02139 United States Am Campus 1 Klosterneuburg3400 Austria Department of Astronomy & Astrophysics University of Chicago 5640 S Ellis Avenue ChicagoIL60637 United States Max-Planck-Institut f"ur Astronomie K"onigstuhl 17 HeidelbergD-69117 Germany Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Copenhagen Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen Denmark Department of Physics The University of Texas at Dallas RichardsonTX75080 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States Department of Astronomy The University of Texas at Austin AustinTX78712 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Institut d’Astrophysique de Paris CNRS Sorbonne Universit’e 98bis Boulevard Arago Paris75014 France Department of Astronomy Yale University New HavenCT06511 United States Dipartimento di Fisica e Astronomia Università di Bologna Bologna Italy Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Leiden Observatory Leiden University PO Box 9513 Leiden2300 RA Netherlands Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Center for Frontier Science Chiba University 1-33 Yayoi-cho Inage-ku Chiba263-8522 Japan Department of Physics Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Max Planck Institute for Astrophysics Karl-Schwarzschild-Str. 1 Garching85748 Germany Institute of Physics Lab for Galaxy Evolution and Spectral Modelling EPFL Observatory of Sauverny Chemin Pegasi 51 Versoix1290 Switzerland Department of

The physical processes that led to the formation of billion solar mass black holes within the first 700 million years of cosmic time remain a puzzle1–3. Several theoretical scenarios have been proposed to seed and rapidly grow black holes4–7, but direct observations of these mechanisms remain elusive. Here we present a source 660 million years after the Big Bang that displays singular properties: among the largest Hydrogen Balmer breaks reported at any redshift, broad multi-peaked Hβ emission, and Balmer line absorption in multiple transitions. We model this source as a "black hole star" (BH*) where the Balmer break and absorption features are a result of extremely dense, turbulent gas forming a dust-free "atmosphere" around a supermassive black hole8, 9. This source may provide evidence of an early black hole embedded in dense gas – a theoretical configuration proposed to rapidly grow black holes via super-Eddington accretion10–14. Radiation from the BH* appears to dominate almost all observed light, leaving limited room for contribution from its host galaxy. We demonstrate that the recently discovered "Little Red Dots" (LRDs)15–19 with perplexing spectral energy distributions20–26 can be explained as BH*s embedded in relatively brighter host galaxies. This source provides evidence that SMBH masses in the LRDs may be over-estimated by orders of magnitude – the BH* is effectively dust-free contrary to the steep dust corrections applied while modeling LRDs9, 16, 27, 28, and the physics that gives rise to the complex line shapes and luminosities may deviate from assumptions underlying standard scaling relations. © 2025, CC BY.

关键词： Cosmology

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JWST UNCOVER: The Overabundance of Ultraviolet-luminous Galaxies at z > 9

arXiv

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arXiv 2023年

作者： Chemerynska, Iryna Atek, Hakim Furtak, Lukas J. Zitrin, Adi Greene, Jenny E. Dayal, Pratika Weibel, Andrea Fujimoto, Seiji Kokorev, Vasily Goulding, Andy D. Williams, Christina C. Nanayakkara, Themiya Bezanson, Rachel Brammer, Gabriel Cutler, Sam E. Labbe, Ivo Leja, Joel Pan, Richard Price, Sedona H. van Dokkum, Pieter Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Institut d'Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Physics Department Ben-Gurion University of the Negev PO Box 653 Be'er-Sheva8410501 Israel Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland Department of Astronomy The University of Texas at Austin AustinTX78712 United States Department of Astrophysical Sciences Princeton University PrincetonNJ08544 United States NSF's National Optical-Infrared Astronomy Research Laboratory TucsonAZ85719 United States Steward Observatory University of Arizona TucsonAZ85721 United States Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Australia Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 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 Physics & Astronomy Tufts University MA02155 United States Astronomy Department Yale University 219 Prospect St New HavenCT06511 United States

Over the past year, JWST has uncovered galaxies at record-breaking distances up to z ∼ 13. The JWST UNCOVER (ultra-deep NIRSpec and NIRcam observations before the epoch of reionization) program has obtained ultra-deep multiwavelength NIRCam imaging of the massive galaxy cluster Abell 2744 over ∼ 45 arcmin2 down to ∼ 29.5 AB mag. Here, we present a robust ultraviolet (UV) luminosity function derived through lensing clusters at 9 UV 9 in recent JWST studies. In particular, a double power-law (DPL) describes better the bright-end of the luminosity function compared to the classical Schechter form. The number density of these bright galaxies is 10-100 times larger than theoretical predictions and previous findings based on Hubble Space Telescope (HST) observations. Additionally, we measure a star formation rate density of ρSFR = 10−2.64 Mo yr−1 Mpc−3 at these redshifts, which is 4 to 10 times higher than galaxy formation models that assume a constant star formation efficiency. Future wide-area surveys and accurate modeling of lensing-assisted observations will reliably constrain both the bright and the dim end of the UV luminosity function at z > 9, which will provide key benchmarks for galaxy formation models. © 2023, CC BY.

关键词： Stars

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UNCOVER: A NIRSpec Identification of a Broad Line AGN at z = 8.50

arXiv

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arXiv 2023年

作者： Kokorev, Vasily Fujimoto, Seiji Labbe, Ivo Greene, Jenny E. Bezanson, Rachel Dayal, Pratika Nelson, Erica J. Atek, Hakim Brammer, Gabriel Caputi, Karina I. Chemerynska, Iryna Cutler, Sam E. Feldmann, Robert Fudamoto, Yoshinobu Furtak, Lukas J. Goulding, Andy D. de Graaff, Anna Leja, Joel Marchesini, Danilo Miller, Tim B. Nanayakkara, Themiya Oesch, Pascal A. Pan, Richard Price, Sedona H. Setton, David J. Smit, Renske Stefanon, Mauro Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Williams, Christina C. Zitrin, Adi Kapteyn Astronomical Institute University of Groningen Groningen9700 AV Netherlands Department of Astronomy The University of Texas at Austin AustinTX78712 United States Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States Department for Astrophysical and Planetary Science University of Colorado BoulderCO80309 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Department of Astronomy University of Massachusetts AmherstMA01003 United States Institute for Computational Science University of Zurich ZurichCH-8057 Switzerland Waseda Research Institute for Science and Engineering Faculty of Science and Engineering Waseda University 3-4-1 Okubo Shinjuku Tokyo169-8555 Japan National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo Japan Physics Department Ben-Gurion University of the Negev P.O. Box 653 Be’er-Sheva84105 Israel Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany 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 Physics & Astronomy Tufts University MA02155 United States Department of Astronomy Yale University New HavenCT06511 United States Department of Physics and Astronomy Northwestern University 1800 Sherman Ave EvanstonIL60201 United States Department of Astronomy University

Deep observations with JWST have revealed an emerging population of red point-like sources that could provide a link between the postulated supermassive black hole seeds and observed quasars. In this work we present a JWST/NIRSpec spectrum from the JWST Cycle 1 UNCOVER Treasury survey, of a massive accreting black hole at z = 8.50, displaying a clear broad-line component as inferred from the Hβ line with FWHM = 3439 ± 413 km s−1, typical of the broad line region of an active galactic nucleus (AGN). The AGN nature of this object is further supported by high ionization, as inferred from emission lines, and a point-source morphology. We compute the black hole mass of log10(MBH/M☉) = 8.17±0.42, and a bolometric luminosity of Lbol ∼ 6.6×1045 erg s−1. These values imply that our object is accreting at ∼ 40% of the Eddington limit. Detailed modeling of the spectral energy distribution in the optical and near-infrared, together with constraints from ALMA, indicate an upper limit on the stellar mass of log10(M∗/M☉) Copyright © 2023, The Authors. All rights reserved.

关键词： Active Galactic Nuclei

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MIGHTEE: The nature of the radio-loud AGN population

arXiv

引用

arXiv 2022年

作者： Whittam, Imogen H. Jarvis, M.J. Hale, C.L. Prescott, M. Morabito, L.K. Heywood, I. Adams, N.J. Afonso, J. An, Fangxia Ao, Y. Bowler, R.A. Collier, J.D. Deane, R.P. Delhaize, J. Frank, B. Glowacki, M. Hatfield, P.W. Maddox, N. Marchetti, L. Matthews, A.M. Prandoni, I. Randriamampandry, S. Randriamanakoto, Z. Smith, D.J.B. Taylor, A.R. Thomas, N.L. Vaccari, M. Astrophysics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Department of Physics and Astronomy University of the Western Cape Robert Sobukwe Road Bellville7535 South Africa School of Physics and Astronomy Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Inter-University Institute for Data Astronomy University of the Western Cape Robert Sobukwe Road Bellville7535 South Africa Centre for Extragalactic Astronomy Department of Physics Durham University DurhamDH1 3LE United Kingdom Institute for Computational Cosmology Department of Physics Durham University DurhamDH1 3LE United Kingdom Department of Physics and Electronics Rhodes University PO Box 94 Grahamstown6140 South Africa Jodrell Bank Centre for Astrophysics University of Manchester Oxford Road Manchester United Kingdom Instituto de Astrofísica e Ciências do Espaço Universidade de Lisboa OAL Tapada da Ajuda LisboaPT1349-018 Portugal Departamento de Física Faculdade de Ciências Universidade de Lisboa Edifício C8 Campo Grande LisbonPT1749-016 Portugal Purple Mountain Observatory Key Laboratory for Radio Astronomy Chinese Academy of Sciences Nanjing China School of Astronomy and Space Science University of Science and Technology of China Hefei China The Inter-University Institute for Data Intensive Astronomy Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa School of Science Western Sydney University Locked Bag 1797 PenrithNSW2751 Australia CSIRO Astronomy and Space Science PO Box 1130 BentleyWA6102 Australia Wits Centre for Astrophysics School of Physics University of the Witwatersrand 1 Jan Smuts Avenue Johannesburg2000 South Africa Department of Physics University of Pretoria Pretoria Hatfield0028 South Africa Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa South African Radio Astro

We study the nature of the faint radio source population detected in the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) Early Science data in the COSMOS field, focusing on the properties of the radio-loud active galactic nuclei (AGN). Using the extensive multi-wavelength data available in the field, we are able to classify 88 per cent of the 5223 radio sources in the field with host galaxy identifications as AGN (35 per cent) or star-forming galaxies (54 per cent). We select a sample of radio-loud AGN with redshifts out to z ∼ 6 and radio luminosities 1020 1.4 GHz/W Hz−1 27 and classify them as high-excitation and low-excitation radio galaxies (HERGs and LERGs). The classification catalogue is released with this work. We find no significant difference in the host galaxy properties of the HERGs and LERGs in our sample. In contrast to previous work, we find that the HERGs and LERGs have very similar Eddington-scaled accretion rates;in particular we identify a population of very slowly accreting AGN that are formally classified as HERGs at these low radio luminosities, where separating into HERGs and LERGs possibly becomes redundant. We investigate how black hole mass affects jet power, and find that a black hole mass & 107.8 M is required to power a jet with mechanical power greater than the radiative luminosity of the AGN (Lmech/Lbol > 1). We discuss that both a high black hole mass and black hole spin may be necessary to launch and sustain a dominant radio jet. © 2022, CC BY.

关键词： Active Galactic Nuclei

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THE ART OF MEASURING PHYSICAL PARAMETERS IN GALAXIES: A CRITICAL ASSESSMENT OF SPECTRAL ENERGY DISTRIBUTION FITTING TECHNIQUES

arXiv

引用

arXiv 2022年

作者： Pacifici, Camilla Iyer, Kartheik G. Mobasher, Bahram da Cunha, Elisabete Acquaviva, Viviana Burgarella, Denis Rivera, Gabriela Calistro Carnall, Adam C. Chang, Yu-Yen Chartab, Nima Cooke, Kevin C. Fairhurst, Ciaran Kartaltepe, Jeyhan Leja, Joel Malek, Katarzyna Salmon, Brett Torelli, Marianna Vidal-García, Alba Boquien, Médéric Brammer, Gabriel G. Brown, Michael J.I. Capak, Peter L. Chevallard, Jacopo Circosta, Chiara Croton, Darren Davidzon, Iary Dickinson, Mark Duncan, Kenneth J. Faber, Sandra M. Ferguson, Harry C. Fontana, Adriano Guo, Yicheng Haeussler, Boris Hemmati, Shoubaneh Jafariyazani, Marziye Kassin, Susan A. Larson, Rebecca L. Lee, Bomee Mantha, Kameswara Bharadwaj Marchi, Francesca Nayyeri, Hooshang Newman, Jeffrey A. Pandya, Viraj Pforr, Janine Reddy, Naveen Sanders, Ryan Shah, Ekta Shahidi, Abtin Stevans, Matthew L. Triani, Dian Puspita Tyler, Krystal D. Vanderhoof, Brittany N. de la Vega, Alexander Wang, Weichen Weston, Madalyn E. Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States NASA Hubble United States Dunlap Institute for Astronomy and Astrophysics University of Toronto 50 St George St TorontoONM5S 3H4 Canada Columbia Astrophysics Laboratory Columbia University 550 West 120th Street New YorkNY10027 United States Department of Physics and Astronomy University of California Riverside 900 University Avenue RiversideCA92521 United States International Centre for Radio Astronomy Research University of Western Australia 35 Stirling Hwy CrawleyWA6009 Australia Research School of Astronomy and Astrophysics Australian National University CanberraACT2611 Australia Australia Physics Department CUNY NYC College of Technology BrooklynNY11201 United States Center for Computational Astrophysics Flatiron Institute New YorkNY10010 United States Aix Marseille Univ CNRS CNES LAM Marseille France European Southern Observatory Karl-Schwarzschild-Str. 2 GarchingD-85748 Germany SUPA Institute for Astronomy University of Edinburgh Royal Observatory EdinburghEH9 3HJ United Kingdom Department of Physics National Chung Hsing University Taichung40227 Taiwan Institute of Astronomy & Astrophysics Academia Sinica Taipei10617 Taiwan AAAS S&T Policy The National Science Foundation 1200 New York Ave NW WashingtonDC20005 United States Astronomy Centre Department of Physics and Astronomy University of Sussex BrightonBN1 9QH United Kingdom School of Physics and Astronomy Rochester Institute of Technology 84 Lomb Memorial Drive RochesterNY14623 United States 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 National Centre for Nuclear Research ul. Pasteura 7

The study of galaxy evolution hinges on our ability to interpret multi-wavelength galaxy observations in terms of their physical properties. To do this, we rely on spectral energy distribution (SED) models which allow us to infer physical parameters from spectrophotometric data. In recent years, thanks to the wide and deep multi-waveband galaxy surveys, the volume of high quality data have significantly increased. Alongside the increased data, algorithms performing SED fitting have improved, including better modeling prescriptions, newer templates, and more extensive sampling in wavelength space. We present a comprehensive analysis of different SED fitting codes including their methods and output with the aim of measuring the uncertainties caused by the modeling assumptions. We apply fourteen of the most commonly used SED fitting codes on samples from the CANDELS photometric catalogs at z ∼ 1 and z ∼ 3. We find agreement on the stellar mass, while we observe some discrepancies in the star formation rate (SFR) and dust attenuation results. To explore the differences and biases among the codes, we explore the impact of the various modeling assumptions as they are set in the codes (e.g., star formation histories, nebular, dust, and AGN models) on the derived stellar masses, SFRs, and AV values. We then assess the difference among the codes on the SFR-stellar mass relation and we measure the contribution to the uncertainties by the modeling choices (i.e., the modeling uncertainties) in stellar mass (∼ 0.1 dex), SFR (∼ 0.3 dex), and dust attenuation (∼ 0.3 mag). Finally, we present some resources summarizing best practices in SED fitting. © 2022, CC BY.

关键词： Galaxies

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