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arXiv 2023年

作者： Kilpatrick, Charles D. Foley, Ryan J. Jacobson-Galán, Wynn V. Piro, Anthony L. Smartt, Stephen J. Drout, Maria R. Gagliano, Alexander Gall, Christa Hjorth, Jens Jones, David O. Mandel, Kaisey S. Margutti, Raffaella Ramirez-Ruiz, Enrico Ransome, Conor L. Villar, V. Ashley Coulter, David A. Gao, Hua Matthews, David Jacob Taggart, Kirsty Zenati, Yossef Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Department of Astronomy and Astrophysics University of California BerkeleyCA94720 United States The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Astrophysics Research Centre School of Mathematics and Physics Queen's University Belfast BelfastBT7 1NN United Kingdom Department of Physics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom David A. Dunlap Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada Department of Astronomy University of Illinois 1002 W. Green St. Urbana-ChampaignIL61801 United States Center for Astrophysical Surveys National Center for Supercomputing Applications UrbanaIL61801 United States DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Gemini Observatory NSF's NOIRLab 670 N. A'ohoku Place HiloHI96720 United States Institute of Astronomy Kavli Institute for Cosmology Madingley Road CambridgeCB3 0HA United Kingdom Department of Astronomy and Astrophysics The Pennsylvania State University Davey Lab State College PA16802 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 Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Department of Physics and Astronomy The Johns Hopkins University BaltimoreMD21218 United States ISEF International Fellowship

We present pre-explosion optical and infrared (IR) imaging at the site of the type II supernova (SN II) 2023ixf in Messier 101 at 6.9 Mpc. We astrometrically registered a ground-based image of SN 2023ixf to archival Hubble Space Telescope (HST), Spitzer Space Telescope (Spitzer), and ground-based near-IR images. A single point source is detected at a position consistent with the SN at wavelengths ranging from HST R-band to Spitzer 4.5 µm. Fitting to blackbody and red supergiant (RSG) spectral-energy distributions (SEDs), we find that the source is anomalously cool with a significant mid-IR excess. We interpret this SED as reprocessed emission in a 8600 R☉ circumstellar shell of dusty material with a mass ∼5×10−5 M☉ surrounding a log(L/L☉) = 4.74 ±0.07 and Teff = 3920+200−160 K RSG. This luminosity is consistent with RSG models of initial mass 11 M☉, depending on assumptions of rotation and overshooting. In addition, the counterpart was significantly variable in pre-explosion Spitzer 3.6 µm and 4.5 µm imaging, exhibiting ∼70% variability in both bands correlated across 9 yr and 29 epochs of imaging. The variations appear to have a timescale of 2.8 yr, which is consistent with κ-mechanism pulsations observed in RSGs, albeit with a much larger amplitude than RSGs such as α Orionis (Betelgeuse). © 2023, CC BY.

关键词： Supernovae

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The first JWST spectrum of a GRB afterglow: No bright supernova in observations of the brightest GRB of all time, GRB 221009A

arXiv

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arXiv 2023年

作者： Levan, A.J. Lamb, G.P. Schneider, B. Hjorth, J. Zafar, T. Postigo, A. de Ugarte Sargent, B. Mullally, S.E. Izzo, L. D’Avanzo, P. Burns, E. Fernández, J.F. Agüí Barclay, T. Bernardini, M.G. Bhirombhakdi, K. Bremer, M. Brivio, R. Campana, S. Chrimes, A.A. D’Elia, V. Della Valle, M. De Pasquale, M. Ferro, M. Fong, W. Fruchter, A.S. Fynbo, J.P.U. Gaspari, N. Gompertz, B.P. Hartmann, D.H. Hedges, C.L. Heintz, K.E. Hotokezaka, K. Jakobsson, P. Kann, D.A. Kennea, J.A. Laskar, T. Floc’h, E. Le Malesani, D.B. Melandri, A. Metzger, B.D. Oates, S.R. Pian, E. Piranomonte, S. Pugliese, G. Racusin, J.L. Rastinejad, J.C. Ravasio, M.E. Rossi, A. Saccardi, A. Salvaterra, R. Sbarufatti, B. Starling, R.L.C. Tanvir, N.R. Thöne, C.C. van der Horst, A.J. Vergani, S.D. Watson, D. Wiersema, K. Wijers, R.A.M.J. Xu, Dong Department of Astrophysics IMAPP Radboud University Nijmegen6525 AJ Netherlands Department of Physics University of Warwick CoventryCV4 7AL United Kingdom Astrophysics Research Institute Liverpool John Moores University 146 Brownlow Hill LiverpoolL3 5RF United Kingdom Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 77 Massachusetts Ave CambridgeMA02139 United States DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Australian Astronomical Optics Macquarie University 105 Delhi Road North RydeNSW2113 Australia Artemis Université Côte d’Azur Observatoire de la Côte d’Azur CNRS NiceF-06304 France Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Center for Astrophysical Sciences The William H. Miller III Department of Physics and Astronomy Johns Hopkins University BaltimoreMD21218 United States INAF Osservatorio Astronomico di Brera Via E. Bianchi 46 LC MerateI-23807 Italy Department of Physics and Astronomy Louisiana State University Baton RougeLA70803 United States Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía s/n Granada18008 Spain NASA Goddard Space Flight Center GreenbeltMD20771 United States University of Maryland Baltimore County BaltimoreMD21250 United States 300 Rue de la Piscine Saint Martin d’HèresF-38406 France Universitá degli Studi dell’Insubria Dipartimento di Scienza e Alta Tecnologia via Valleggio 11 Como22100 Italy ASI Italian Space Agency Space Science Data Centre Via del Politecnico snc Rome00133 Italy Monte Porzio CatoneI-00040 Italy Capodimonte Astronomical Observatory INAF-Napoli Salita Moiariello 16 NapoliI-80131 Italy University of Messina Mathematics Informatics Physics and Earth Science Department Via F.D. D’Alcontres 31 Polo Papardo Messina98166 Italy Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States T

We present JWST and Hubble Space Telescope (HST) observations of the afterglow of GRB 221009A, the brightest gamma-ray burst (GRB) ever observed. This includes the first mid-IR spectra of any GRB, obtained with JWST/NIRSPEC (0.6-5.5 micron) and MIRI (5-12 micron), 12 days after the burst. Assuming that the intrinsic spectral slope is a single power-law, with Fν ∝ ν−β, we obtain β ≈ 0.35, modified by substantial dust extinction with AV = 4.9. This suggests extinction above the notional Galactic value, possibly due to patchy extinction within the Milky Way or dust in the GRB host galaxy. It further implies that the X-ray and optical/IR regimes are not on the same segment of the synchrotron spectrum of the afterglow. If the cooling break lies between the X-ray and optical/IR, then the temporal decay rates would only match a post jet-break model, with electron index p Copyright © 2023, The Authors. All rights reserved.

关键词： Supernovae

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An unambiguous AGN and a Balmer break in an Ultraluminous Little Red Dot at z=4.47 from Ultradeep UNCOVER and All the Little Things Spectroscopy

arXiv

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arXiv 2024年

作者： Labbe, Ivo Greene, Jenny E. Matthee, Jorryt Treiber, Helena Kokorev, Vasily Miller, Tim B. Kramarenko, Ivan Setton, David J. Ma, Yilun Goulding, Andy D. Bezanson, Rachel Naidu, Rohan P. Williams, Christina C. Atek, Hakim Brammer, Gabriel Cutler, Sam E. Chemerynska, Iryna Cloonan, Aidan P. Dayal, Pratika de Graaff, Anna Fudamoto, Yoshinobu Fujimoto, Seiji Furtak, Lukas J. Glazebrook, Karl Heintz, Kasper E. Leja, Joel Marchesini, Danilo Nanayakkara, Themiya Nelson, Erica J. Oesch, Pascal A. Pan, Richard Price, Sedona H. Shivaei, Irene Sobral, David Suess, Katherine A. van Dokkum, Pieter Wang, Bingjie Weaver, John R. Whitaker, Katherine E. Zitrin, Adi Centre for Astrophysics and Supercomputing Swinburne University of Technology MelbourneVIC3122 Australia Department of Astrophysical Sciences Princeton University 4 Ivy Lane PrincetonNJ08544 United States Am Campus 1 Klosterneuburg Austria Department of Astronomy The University of Texas at Austin AustinTX78712 United States Northwestern University IL60201 United States Department of Physics and Astronomy PITT PACC University of Pittsburgh PittsburghPA15260 United States MIT Kavli Institute for Astrophysics and Space Research 77 Massachusetts Ave. CambridgeMA02139 United States NSF National Optical-Infrared Astronomy Research Laboratory 950 North Cherry Avenue TucsonAZ85719 United States Institut d’Astrophysique de Paris CNRS Sorbonne Université 98bis Boulevard Arago Paris75014 France Niels Bohr Institute University of Copenhagen Jagtvej 128 København NDK-2200 Denmark Department of Astronomy University of Massachusetts AmherstMA01003 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany 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 Centre for Astrophysics and Supercomputing Swinburne University of Technology PO Box 218 HawthornVIC3122 Australia Denmark Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen N2200 Denmark Department of Astronomy University of Geneva Chemin Pegasi 51 Versoix1290 Switzerland 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 Unite

We present a detailed exploration of the most optically-luminous Little Red Dot (LHα = 1044 erg/s, LV = 1045 erg/s, F444W = 22 AB) discovered by JWST to date. Located in the UNCOVER Abell 2744 field, source A2744−45924 was observed by NIRSpec/PRISM with ultradeep spectroscopy reaching SNR ∼ 100 pix−1, high-resolution 3 − 4 µm NIRCam/Grism spectroscopy from the All the Little Things (ALT) program, and multi-band NIRCam Medium Band imaging from Mega Science. The NIRCam spectra reveal high rest-frame equivalent width WHα,0,broad > 800 Å, broad Hα emission (FWHM ∼ 4500 km/s), on top of narrow, complex Hα absorption. NIRSpec data show exceptionally strong rest-frame ultraviolet (UV) to near-infrared (NIR) Fe II emission (WFeII−UV,0 ∼ 340 Å), UV N IV] λλ1483, 1486 and N III] λ1750, and broad NIR O Iλ8446 emission. The line spectra unambiguously demonstrate a broad-line region (BLR) associated with a possible MBH ∼ 109M supermassive black hole embedded in dense gas, which might explain the non-detection in ultradeep Chandra X-ray data ( 10× underluminous relative to broad LHα). Strong UV Nitrogen lines suggest supersolar N/O ratios due to rapid star formation or intense radiation fields near the AGN. The observed continuum shows a clear Balmer break at rest-frame 3650 Å, which cannot be accounted for by power-law AGN alone. A stellar population model produces an excellent fit with a reddened Balmer break and would imply a massive (M∗ ≈ 8 × 1010 M), old ∼ 500 Myr, compact stellar core, among the densest stellar systems known (ρ ≈ 3 ×106 M/pc2 for Re,optical = 70 ±10 pc), and AGN emission lines with extreme intrinsic equivalent width WHα,0 1000 Å. However, although high M∗ and MBH are supported by evidence of a galaxy overdensity containing 40 galaxies at z = 4.41 − 4.51, deep high-resolution spectroscopy is required to confirm stellar absorption and rule out that the Balmer break is instead caused by dense gas surrounding the AGN. © 2024, CC BY.

关键词： Stars

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Analytical Rayleigh potential for the general relativistic Poynting-Robertson effect

arXiv

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arXiv 2019年

作者： de Falco, Vittorio Battista, Emmanuele Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-746 01 Czech Republic

–We determine the analytic expression of the Rayleigh potential associated to the general relativistic Poynting-Robertson effect. This constitutes the first example of a physical dissipative system treated analytically in General Relativity. The employed approach and further implications are discussed. Copyright © 2019, The Authors. All rights reserved.

关键词： Relativity

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MIGHTEE: Deep 1.4 GHz Source Counts and the Sky Temperature Contribution of Star Forming Galaxies and Active Galactic Nuclei

arXiv

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arXiv 2022年

作者： Hale, C.L. Whittam, I.H. Jarvis, M.J. Best, P.N. Thomas, N.L. Heywood, I. Prescott, M. Adams, N. Afonso, J. An, Fangxia Bowler, R.A.A. Collier, J.D. Cook, R.H.W. Davé, R. Frank, B.S. Glowacki, M. Hatfield, P.W. Kolwa, S. Lovell, C.C. Maddox, N. Marchetti, L. Morabito, L.K. Murphy, E. Prandoni, I. Randriamanakoto, Z. Taylor, A.R. School of Physics and Astronomy Institute for Astronomy University of Edinburgh Royal Observatory Blackford Hill EdinburghEH9 3HJ United Kingdom Sub-Department of Astrophysics University of Oxford Keble Road OxfordOX1 3RH United Kingdom Department of Physics and Astronomy University of the Western Cape Robert Sobukwe Road Bellville Cape Town7535 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 Makhanda6140 South Africa South African Radio Astronomy Observatory 2 Fir Street Black River Park Observatory Cape Town7925 South Africa Inter-University Institute for Data Intensive Astronomy University of the Western Cape Robert Sobukwe Road Bellville Cape Town7535 South Africa Jodrell Bank Centre for Astrophysics Alan Turing Building 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 Chinese Academy of Sciences Nanjing210023 China Jodrell Bank Centre for Astrophysics Department of Physics and Astronomy School of Natural Sciences The University of Manchester ManchesterM13 9PL United Kingdom 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 University of Western Australia CrawleyWA6009 Australia South African Astronomical Observatories P.O. Box 9 Observatory Cape Town7

We present deep 1.4 GHz source counts from ∼5 deg2 of the continuum Early Science data release of the MeerKAT International Gigahertz Tiered Extragalactic Exploration (MIGHTEE) survey down to S1.4GHz ∼15 μJy. Using observations over two extragalactic fields (COSMOS and XMM-LSS), we provide a comprehensive investigation into correcting the incompleteness of the raw source counts within the survey to understand the true underlying source count population. We use a variety of simulations that account for: errors in source detection and characterisation, clustering, and variations in the assumed source model used to simulate sources within the field and characterise source count incompleteness. We present these deep source count distributions and use them to investigate the contribution of extragalactic sources to the sky background temperature at 1.4 GHz using a relatively large sky area. We then use the wealth of ancillary data covering a subset of the COSMOS field to investigate the specific contributions from both active galactic nuclei (AGN) and star forming galaxies (SFGs) to the source counts and sky background temperature. We find, similar to previous deep studies, that we are unable to reconcile the sky temperature observed by the ARCADE 2 experiment. We show that AGN provide the majority contribution to the sky temperature contribution from radio sources, but the relative contribution of SFGs rises sharply below 1 mJy, reaching an approximate 15-25% contribution to the total sky background temperature (Tb ∼100 mK) at ∼15 μJy. © 2022, CC BY.

关键词： Active Galactic Nuclei

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Habitable zones around almost extremely spinning black holes (black sun revisited)

arXiv

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arXiv 2020年

作者： Bakala, Pavel Dočekal, Jan Turoňová, Zuzana Research Centre for Computational Physics and Data Processing Faculty of Philosophy and Science Bezrucovonam. 13 OpavaCZ-746 01 Czech Republic M. R. Stefánik Observatory and Planetarium Sládkovicova 41 Hlohovec920 01 Slovakia INAF - Osservatorio Astronomico di Roma Via Frascati 33 Monteporzio Catone Roma00078 Italy

We analyzed the thermodynamics of hypothetical exoplanets at very low Keplerian circular orbits in close vicinity of rapidly spinning supermassive black holes. Such black hole exoplanets are heated by strongly blueshifted and focused flux of the incoming cosmic microwave background (CMB) and cooled by the cold part of the local sky containing the black hole shadow. This gives rise to a temperature difference, which can drive processes far from thermodynamic equilibrium in a hypothetical life form inhabiting black hole exoplanets, similar to the case of a planet heated by the radiation of the parent star and cooled by the night sky. We found that for a narrow range of radii of very low Keplerian circular orbits and for very high spin of a supermassive black hole, the temperature regime of the black hole exoplanets corresponds to the habitable zone around standard stars. The thermodynamics of black hole exoplanets therefore, in principle, does not exclude the existence of life based on known biology. The peak of the multiblackbody spectral profile of the CMB heating the exoplanet is located in the ultraviolet band, but a significant fraction of the flux comes also in the visible and infrared bands. The minimum mass of a black hole ensuring the resistance to tidal disruption of an Earth-like exoplanet orbiting in the habitable zone is estimated to 1.63 108mo. Copyright © 2020, The Authors. All rights reserved.

关键词： Extrasolar planets

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Ubiquitous broad-line emission and the relation between ionized gas outflows and Lyman continuum escape in Green Pea galaxies

arXiv

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arXiv 2024年

作者： Amorín, R.O. Rodríguez-Henríquez, M. Fernández, V. Vílchez, J.M. Marques-Chaves, R. Schaerer, D. Izotov, Y.I. Firpo, V. Guseva, N. Jaskot, A.E. Komarova, L. Muñoz-Vergara, D. Oey, M.S. Bait, O. Carr, C. Chisholm, J. Ferguson, H. Flury, S.R. Giavalisco, M. Hayes, M.J. Henry, A. Ji, Z. King, W. Leclercq, F. Östlin, G. Pentericci, L. Saldana-Lopez, A. Thuan, T.X. Trebitsch, M. Wang, B. Worseck, G. Xu, X. Unidad Asociada al CSIC Plaza San Juan 1 TeruelE–44001 Spain Departamento de Astronomía Universidad de La Serena Avda. Juan Cisternas 1200 La Serena Chile Gemini Observatory 670 N. A’ohoku Place HiloHI96720 United States University of Michigan Department of Astronomy 323 West Hall 1085 S. University Ave Ann ArborMI48109 United States Instituto de Investigación Multidisciplinar de Investigación y Posgrado Universidad de La Serena Raúl Bitrán 1305 La Serena Chile Instituto de Astrofísica de Andalucía CSIC Apartado de correos 3004 GranadaE-18080 Spain Department of Astronomy University of Geneva 51 Chemin Pegasi Versoix1290 Switzerland Bogolyubov Institute for Theoretical Physics National Academy of Sciences of Ukraine 14-b Metrolohichna str. Kyiv03143 Ukraine Gemini Observatory NSF’s NOIRLab Casilla 603 La Serena Chile Department of Astronomy University of Massachusetts AmherstMA01003 United States Center for Cosmology and Computational Astrophysics Institute for Advanced Study in Physics Zhejiang University Hangzhou310058 China Institute of Astronomy School of Physics Zhejiang University Hangzhou310058 China Department of Astronomy The University of Texas at Austin 2515 Speedway Stop C1400 AustinTX78712-1205 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Department of Astronomy Oskar Klein Centre Stockholm University StockholmSE-106 91 Sweden Center for Astrophysical Sciences Department of Physics & Astronomy Johns Hopkins University BaltimoreMD21218 United States Steward Observatory University of Arizona 933 N. Cherry Avenue TucsonAZ85721 United States INAF - Osservatorio Astronomico di Roma Via di Frascati 33 Monte Porzio Catone00078 Italy Astronomy Department University of Virginia P.O. Box 400325 CharlottesvilleVA22904-4325 United States Kapteyn Astronomical Institute University of Groningen P.O. Box 800 Groningen9700 AV Netherlands Department of Astronom

We report observational evidence of highly turbulent ionized gas kinematics in a sample of 20 Lyman continuum (LyC) emitters (LCEs) at low redshift (z ∼ 0.3). Detailed Gaussian modeling of optical emission line profiles in high-dispersion spectra consistently shows that both bright recombination and collisionally excited lines can be fitted as one or two narrow components with intrinsic velocity dispersion of σ ∼ 40-100 km s−1, in addition to a broader component with σ ∼ 100-300 km s−1, which contributes up to ∼40% of the total flux and is preferentially blueshifted from the systemic velocity. We interpret the narrow emission as highly ionized gas close to the young massive star clusters and the broader emission as a signpost of unresolved ionized outflows, resulting from massive stars and supernova feedback. We find a significant correlation between the width of the broad emission and the LyC escape fraction, with strong LCEs exhibiting more complex and broader line profiles than galaxies with weaker or undetected LyC emission. We provide new observational evidence supporting predictions from models and simulations;our findings suggest that gas turbulence and outflows resulting from strong radiative and mechanical feedback play a key role in clearing channels through which LyC photons escape from galaxies. We propose that the detection of blueshifted broad emission in the nebular lines of compact extreme emission-line galaxies can provide a new indirect diagnostic of Lyman photon escape, which could be useful to identify potential LyC leakers in the epoch of reionization with the JWST. Copyright © 2024, The Authors. All rights reserved.

关键词： Galaxies

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General relativistic Poynting-Robertson effect to diagnose wormholes existence: Static and spherically symmetric case

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Physical Review D 2020年第10期101卷 104037-104037页

作者： Vittorio De Falco Emmanuele Battista Salvatore Capozziello Mariafelicia De Laurentis Research Centre for Computational Physics and Data Processing Faculty of Philosophy and Science Silesian University in Opava Bezručovo nám. 13 CZ-746 01 Opava Czech Republic Institute for Theoretical Physics Karlsruhe Institute of Technology (KIT) 76128 Karlsruhe Germany Institute for Nuclear Physics Karlsruhe Institute of Technology (KIT) Hermann-von-Helmholtz-Platz 1 76344 Eggenstein-Leopoldshafen Germany Università degli studi di Napoli “Federico II ” Dipartimento di Fisica “Ettore Pancini” Complesso Universitario di Monte S. Angelo Via Cintia Edificio 6 80126 Napoli Italy Istituto Nazionale di Fisica Nucleare Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia Edificio 6 80126 Napoli Italy

We derive the equations of motion of a test particle in the equatorial plane around a static and spherically symmetric wormhole influenced by a radiation field including the general relativistic Poynting-Robertson effect. From the analysis of this dynamical system, we develop a diagnostic to distinguish a black hole from a wormhole, which can be timely supported by several and different observational data. This procedure is based on the possibility of having some wormhole metrics, which smoothly connect to the Schwarzschild metric in a small transition surface layer very close to the black hole event horizon. To detect such a metric change, we analyze the emission proprieties from the critical hypersurface (stable region where radiation and gravitational fields balance) together with those from an accretion disk in the Schwarzschild spacetime toward a distant observer. Indeed, if the observational data are well fitted within such a model, it immediately implies the existence of a black hole; while in the case of strong departures from such a description it means that a wormhole could be present. Finally, we discuss our results and draw conclusions.

关键词： Classical black holes General relativity General relativity equations & solutions General relativity formalism Gravitation Singularities In general relativity Accretion disk & black-hole plasma Astronomical black holes Astrophysical electromagnetic fields Numerical simulations in gravitation & astrophysics

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The Optical Light Curve of GRB 221009A: The Afterglow and the Emerging Supernova

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ASTROPHYSICAL JOURNAL LETTERS 2023年第1期946卷 L22-L22页

作者： Fulton, M. D. Smartt, S. J. Rhodes, L. Huber, M. E. Villar., V. A. Moore, T. Srivastav, S. Schultz, A. S. B. Chambers, K. C. Izzo, L. Hjorth, J. Chen, T. -W. Nicholl, M. Foley, R. J. Rest, A. Smith, K. W. Young, D. R. Sim, S. A. Bright, J. Zenati, Y. de Boer, T. Bulger, J. Fairlamb, J. Gao, H. Lin, C. -C. Lowe, T. Magnier, E. A. Smith, I. A. Wainscoat, R. Coulter, D. A. Jones, D. O. Kilpatrick, C. D. McGill, P. Ramirez-Ruiz, E. Lee, K. -S. Narayan, G. Ramakrishnan, V. Ridden-Harper, R. Singh, A. Wang, Q. Kong, A. K. H. Ngeow, C. -C. Pan, Y. -C. Yang, S. Davis, K. W. Piro, A. L. Rojas-Bravo, C. Sommer, J. Yadavalli, S. K. Astrophysics Research Centre School of Mathematics and Physics Queen's University Belfast BT7 1NN UK Department of Physics University of Oxford Denys Wilkinson Building Keble Road Oxford OX1 3RH UK Institute for Astronomy University of Hawai'i 2680 Woodlawn Drive Honolulu HI 96822 USA Department of Astronomy and Astrophysics Pennsylvania State University 525 Davey Laboratory University Park PA 16802 USA Institute for Computational &amp Data Sciences The Pennsylvania State University University Park PA 16802 USA Institute for Gravitation and the Cosmos The Pennsylvania State University University Park PA 16802 USA DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 DK-2200 Copenhagen Denmark Technische Universität München TUM School of Natural Sciences Physik-Department James-Franck-Straße 1 D-85748 Garching Germany Max-Planck-Institut für Astrophysik Karl-Schwarzschild Straße 1 D-85748 Garching Germany Birmingham Institute for Gravitational Wave Astronomy and School of Physics and Astronomy University of Birmingham Birmingham B15 2TT UK Department of Astronomy and Astrophysics University of California Santa Cruz 1156 High St. Santa Cruz CA 95060 USA Space Telescope Science Institute 3700 San Martin Drive Baltimore MD 21218 USA Department of Physics and Astronomy The Johns Hopkins University Baltimore MD 21218 USA Institute for Astronomy University of Hawai'i 34 Ohia Ku St. Pukalani HI 96768-8288 USA Gemini Observatory NSF's NOIRLab 670 N. A'ohoku Place Hilo Hawai'i 96720 USA Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) Northwestern University 1800 Sherman Ave Evanston IL 60201 USA Department of Physics and Astronomy Purdue University 525 Northwestern Avenue West Lafayette Indiana 47907 USA Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green St. IL 61801 USA Center for Astrophysical Surveys National Center for Supercomputing Applications Urbana IL 61801 USA S

We present extensive optical photometry of the afterglow of GRB 221009A. Our data cover 0.9-59.9 days from the time of Swift and Fermi gamma-ray burst (GRB) detections. Photometry in rizy-band filters was collected primarily with Pan-STARRS and supplemented by multiple 1-4 m imaging facilities. We analyzed the Swift X-ray data of the afterglow and found a single decline rate power law f(t) proportional to t(-1.556 +/- 0.002) best describes the light curve. In addition to the high foreground Milky Way dust extinction along this line of sight, the data favor additional extinction to consistently model the optical to X-ray flux with optically thin synchrotron emission. We fit the X-ray-derived power law to the optical light curve and find good agreement with the measured data up to 5-6 days. Thereafter we find a flux excess in the riy bands that peaks in the observer frame at similar to 20 days. This excess shares similar light-curve profiles to the Type Ic broad-lined supernovae SN 2016jca and SN 2017iuk once corrected for the GRB redshift of z = 0.151 and arbitrarily scaled. This may be representative of an SN emerging from the declining afterglow. We measure rest-frame absolute peak AB magnitudes of M-g = -19.8 +/- 0.6 and M-r = - 19.4 +/- 0.3 and M-z = -20.1 +/- 0.3. If this is an SN component, then Bayesian modeling of the excess flux would imply explosion parameters of M-ej = 7.1(-1.7)(+2.4) M-circle dot, M-Ni = 1.0(-0.4)(+0.6) M-circle dot, and nu(ej) = 33,900(-5700)(+5900) km s(-1), for the ejecta mass, nickel mass, and ejecta velocity respectively, inferring an explosion energy of E-kin similar or equal to 2.6-9.0 x 10(52) erg.

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Final results on the 0νββ decay half-life limit of 100Mo from the CUPID-Mo experiment

arXiv

引用

arXiv 2022年

作者： Augier, C. Barabash, A.S. Bellini, F. Benato, G. Beretta, M. Bergé, L. Billard, J. Borovlev, Yu.A. Cardani, L. Casali, N. Cazes, A. Chapellier, M. Chiesa, D. Dafinei, I. Danevich, F.A. De Jesus, M. de Marcillac, P. Dixon, T. Dumoulin, L. Eitel, K. Ferri, F. Fujikawa, B.K. Gascon, J. Gironi, L. Giuliani, A. Grigorieva, V.D. Gros, M. Helis, D.L. Huang, H.Z. Huang, R. Imbert, L. Johnston, J. Juillard, A. Khalife, H. Kleifges, M. Kobychev, V.V. Kolomensky, Yu.G. Konovalov, S.I. Loaiza, P. Ma, L. Makarov, E.P. Mariam, R. Marini, L. Marnieros, S. Navick, X.-F. Nones, C. Norman, E.B. Olivieri, E. Ouellet, J.L. Pagnanini, L. Pattavina, L. Paul, B. Pavan, M. Peng, H. Pessina, G. Pirro, S. Poda, D.V. Polischuk, O.G. Pozzi, S. Previtali, E. Redon, Th. Rojas, A. Rozov, S. Sanglard, V. Scarpaci, J.A. Schmidt, B. Shen, Y. Shlegel, V.N. Singh, V. Tomei, C. Tretyak, V.I. Umatov, V.I. Vagneron, L. Velázquez, M. Welliver, B. Winslow, L. Xue, M. Yakushev, E. Zarytskyy, M. Zolotarova, A.S. Univ Lyon Université Lyon 1 CNRS IN2P3 IP2I-Lyon VilleurbanneF-69622 France National Research Centre Kurchatov Institute Institute of Theoretical and Experimental Physics Moscow117218 Russia Dipartimento di Fisica Sapienza Università di Roma P.le Aldo Moro 2 RomeI-00185 Italy INFN Sezione di Roma P.le Aldo Moro 2 RomeI-00185 Italy IRFU CEA Université Paris-Saclay Gif-sur-YvetteF-91191 France INFN Laboratori Nazionali del Gran Sasso AQ AssergiI-67100 Italy Department of Physics University of California BerkeleyCA94720 United States Université Paris-Saclay CNRS IN2P3 IJCLab Orsay91405 France Nikolaev Institute of Inorganic Chemistry Novosibirsk630090 Russia Dipartimento di Fisica Università di Milano-Bicocca MilanoI-20126 Italy INFN Sezione di Milano-Bicocca MilanoI-20126 Italy Institute for Nuclear Research Kyiv03028 Ukraine Institute for Astroparticle Physics Karlsruhe Institute of Technology Karlsruhe76021 Germany Nuclear Science Division Lawrence Berkeley National Laboratory BerkeleyCA94720 United States Gran Sasso Science Institute L'AquilaI-67100 Italy Fudan University Shanghai200433 China Massachusetts Institute of Technology CambridgeMA02139 United States Institute for Data Processing and Electronics Karlsruhe Institute of Technology Karlsruhe76021 Germany Department of Nuclear Engineering University of California BerkeleyCA94720 United States Physik Department Technische Universität München GarchingD-85748 Germany Department of Modern Physics University of Science and Technology of China Hefei230027 China LSM Laboratoire Souterrain de Modane Modane73500 France Laboratory of Nuclear Problems JINR Moscow region Dubna141980 Russia Department of Physics & Astronomy Northwestern University EvanstonIL60208 United States Université Grenoble Alpes CNRS Grenoble INP SIMAP Saint Martin d'Héres38402 France

The CUPID-Mo experiment to search for 0νββ decay in 100Mo has been recently completed after about 1.5 years of operation at Laboratoire Souterrain de Modane (France). It served as a demonstrator for CUPID, a next generation 0νββ decay experiment. CUPID-Mo was comprised of 20 enriched Li2100MoO4 scintillating calorimeters, each with a mass of ∼ 0.2 kg, operated at ∼20 mK. We present here the final analysis with the full exposure of CUPID-Mo (100Mo exposure of 1.47 kg×year) used to search for lepton number violation via 0νββ decay. We report on various analysis improvements since the previous result on a subset of data, reprocessing all data with these new techniques. We observe zero events in the region of interest and set a new limit on the 100Mo 0νββ decay half-life of T1/20ν > 1.8 × 1024 year (stat.+syst.) at 90% CI. Under the light Majorana neutrino exchange mechanism this corresponds to an effective Majorana neutrino mass of 〈mββ〉 © 2022, CC BY.

关键词： Calorimeters

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