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arXiv 2022年

作者： Aleo, P.D. Malanchev, K. Sharief, S. Jones, D.O. Narayan, G. Foley, R.J. Villar, V.A. Angus, C.R. Baldassare, V.F. Bustamante-Rosell, M.J. Chatterjee, D. Cold, C. Coulter, D.A. Davis, K.W. Dhawan, S. Drout, M.R. Engel, A. French, K.D. Gagliano, A. Gall, C. Hjorth, J. Huber, M.E. Jacobson-Galán, W.V. Kilpatrick, C.D. Langeroodi, D. Macias, P. Mandel, K.S. Margutti, R. Matasić, F. McGill, P. Pierel, J.D.R. Ramirez-Ruiz, E. Ransome, C.L. Rojas-Bravo, C. Siebert, M.R. Smith, K.W. de Soto, K.M. Stroh, M.C. Tinyanont, S. Taggart, K. Ward, S.M. Wojtak, R. Auchettl, K. Blanchard, P.K. de Boer, T.J.L. Boyd, B.M. Carroll, C.M. Chambers, K.C. DeMarchi, L. Dimitriadis, G. Dodd, S.A. Earl, N. Farias, D. Gao, H. Gomez, S. Grayling, M. Grillo, C. Hayes, E.E. Hung, T. Izzo, L. Khetan, N. Kolborg, A.N. Law-Smith, J.A.P. LeBaron, N. Lin, C.-C. Luo, Y. Magnier, E.A. Matthews, D. Mockler, B. O’Grady, A.J.G. Pan, Y.-C. Politsch, C.A. Raimundo, S.I. Rest, A. Ridden-Harper, R. Sarangi, A. Schrøder, S.L. Smartt, S.J. Terreran, G. Thorp, S. Vazquez, J. Wainscoat, R.J. Wang, Q. Wasserman, A.R. Yadavalli, S.K. Yarza, R. Zenati, Y. Department of Astronomy University of Illinois at Urbana-Champaign 1002 W. Green St. IL61801 United States Fellow United States Center for AstroPhysical Surveys National Center for Supercomputing Applications UrbanaIL61801 United States Sternberg Astronomical Institute Lomonosov Moscow State University 13 Universitetsky pr. Moscow119234 Russia Department of Astronomy and Astrophysics University of California Santa CruzCA95064 United States Gemini Observatory NSF’s NOIRLab 670 N. A’ohoku Place HiloHI96720 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 DARK Niels Bohr Institute University of Copenhagen Jagtvej 128 Copenhagen2200 Denmark Department of Physics & Astronomy Washington State University PullmanWA99164 United States LIGO Laboratory Kavli Institute for Astrophysics and Space Research Massachusetts Institute of Technology 185 Albany St CambridgeMA02139 United States Institute of Astronomy Kavli Institute for Cosmology Madingley Road CambridgeCB3 0HA United Kingdom Department of Astronomy and Astrophysics University of Toronto 50 St. George Street TorontoONM5S 3H4 Canada NSF Graduate Fellow Institute for Astronomy University of Hawaii 2680 Woodlawn Drive HonoluluHI96822 United States Department of Astronomy University of California BerkeleyCA94720 United States Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States Space Telescope Science Institute BaltimoreMD21218 United States Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 1NN United Kingdom School of Physics The University of Melbourne VIC3010 Australia Australia LSSTC Cata

We present the Young Supernova Experiment data Release 1 (YSE DR1), comprised of processed multi-color Pan-STARRS1 (PS1) griz and Zwicky Transient Facility (ZTF) gr photometry of 1975 transients with host-galaxy associations, redshifts, spectroscopic/photometric classifications, and additional data products from 2019 November 24 to 2021 December 20. YSE DR1 spans discoveries and observations from young and fast-rising supernovae (SNe) to transients that persist for over a year, with a redshift distribution reaching z ≈ 0.5. We present relative SN rates from YSE’s magnitude- and volume-limited surveys, which are consistent with previously published values within estimated uncertainties for untargeted surveys. We combine YSE and ZTF data, and create multi-survey SN simulations to train the ParSNIP and SuperRAENN photometric classification algorithms;when validating our ParSNIP classifier on 472 spectroscopically classified YSE DR1 SNe, we achieve 82% accuracy across three SN classes (SNe Ia, II, Ib/Ic) and 90% accuracy across two SN classes (SNe Ia, core-collapse SNe). Our classifier performs particularly well on SNe Ia, with high (>90%) individual completeness and purity, which will help build an anchor photometric SNe Ia sample for cosmology. We then use our photometric classifier to characterize our photometric sample of 1483 SNe, labeling 1048 (∼71%) SNe Ia, 339 (∼23%) SNe II, and 96 (∼6%) SNe Ib/Ic. YSE DR1 provides a training ground for building discovery, anomaly detection, and classification algorithms, performing cosmological analyses, understanding the nature of red and rare transients, exploring tidal disruption events and nuclear variability, and preparing for the forthcoming Vera C. Rubin Observatory Legacy Survey of Space and Time. © 2022, CC BY.

关键词： Supernovae

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NGC 1436: the making of a lenticular galaxy in the Fornax cluster

arXiv

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arXiv 2023年

作者： Loni, Alessandro Serra, Paolo Sarzi, Marc Józsa, Gyula I.G. Anta, M. Pablo Galán-De Zabel, Nikki Kleiner, Dane Maccagni, Filippo M. Molnár, Daniel Ramatsoku, Mpati Loi, Francesca Corsini, Enrico M. Pisano, D.J. Kamphuis, Peter Davis, Timothy A. de Blok, W.J.G. Dettmar, Ralf J. Falcon-Barroso, Jesus Iodice, Enrichetta Lara-López, Maritza A. Loubser, S. Ilani Morokuma-Matsui, Kana Peletier, Reynier Pinna, Francesca Poci, Adriano Smith, Matthew W.L. Trager, Scott C. van de Ven, Glenn Armagh Observatory and Planetarium College Hill ArmaghBT61 9DG United Kingdom INAF Osservatorio Astronomico di Cagliari Via della Scienza 5 CA Selargius09047 Italy Max-Plank-Institut für Radioastronomie Auf dem Hügel 69 Bonn53121 Germany Department of Physics and Electronics Rhodes University PO Box 94 Makhanda6140 South Africa Astrophysics Research Centre School of Mathematics and Physics Queen’s University Belfast BelfastBT7 INN United Kingdom Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa Oude Hoogeveensedijk 4 Dwingeloo7991 PD Netherlands Dipartimento di Fisica e Astronomia G. Galilei Università di Padova vicolo dell’Osservatorio 3 PadovaI-35122 Italy INAF - Osservatorio Astronomico di Padova vicolo dell’Osservatorio 2 PadovaI-35122 Italy Ruhr University Bochum Faculty of Physics and Astronomy Astronomical Institute Bochum44780 Germany School of Physics and Astronomy Cardiff University Queens Buildings The Parade CardiffCF24 3AA United Kingdom Kapteyn Astronomical Institute University of Groningen PO Box 800 GroningenNL−9700 AV Netherlands The Inter-University Institute for Data Intensive Astronomy Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa Instituto de Astrofísica de Canarias Vía Láctea s/n La Laguna Tenerife E-38205 Spain Departamento de Astrofísica Universidad de La Laguna La Laguna TenerifeE-38200 Spain INAF − Astronomical Observatory of Capodimonte Salita Moiariello 16 Naples80131 Italy Madrid28040 Spain Centre for Space Research North−West University Potchefstroom2520 South Africa Center for Computational Sciences University of Tsukuba Ten-nodai 1-1-1 Tsukuba Ibaraki305-8577 Japan Max-Planck-Institut für Astronomie Königstuhl 17 HeidelbergD-69117 Germany Centre for Extragalactic Astronomy University of Durham Stockton Road DurhamDH1 3LE United Kingdom Department of Astrophysics University of Vienna Türkenschanzs

We study the evolutionary path of the Fornax cluster galaxy NGC 1436, which is known to be currently transitioning from a spiral into a lenticular morphology. This galaxy hosts an inner star-forming disc and an outer quiescent disc, and we analyse data from the MeerKAT Fornax Survey, ALMA, and the Fornax 3D survey to study the interstellar medium and the stellar populations of both disc components. Thanks to the combination of high resolution and sensitivity of the MeerKAT data, we find that the HI is entirely confined within the inner star-forming disc, and that its kinematics is coincident with that of the CO. The cold gas disc is now well settled, which suggests that the galaxy has not been affected by any environmental interactions in the last ∼ 1 Gyr. The star formation history derived from the Fornax 3D data shows that both the inner and outer disc experienced a burst of star formation ∼ 5 Gyr ago, followed by rapid quenching in the outer disc and by slow quenching in the inner disc, which continues forming stars to this day. We claim that NGC 1436 has begun to effectively interact with the cluster environment 5 Gyr ago, when a combination of gravitational and hydrodynamical interactions caused the temporary enhancement of the star-formation rate. Furthermore, due to the weaker gravitational binding HI was stripped from the outer disc, causing its rapid quenching. At the same time, accretion of gas onto the inner disc stopped, causing slow quenching in this region. Copyright © 2023, The Authors. All rights reserved.

关键词： Galaxies

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Radiogenomics Consortium Genome-Wide Association Study Meta-Analysis of Late Toxicity After Prostate Cancer Radiotherapy (vol 112, pg 179, 2020)

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JNCI-JOURNAL OF THE NATIONAL CANCER INSTITUTE 2020年第6期112卷 654-654页

作者： Kerns, Sarah L. Fachal, Laura Dorling, Leila Barnett, Gillian C. Baran, Andrea Peterson, Derick R. Hollenberg, Michelle Hao, Ke Di Narzo, Antonio Ahsen, Mehmet Eren Pandey, Gaurav Bentzen, Soren M. Janelsins, Michelle Ellicot, Rebecca M. Pharoah, Paul D. Burnet, Neil G. Dearnaley, David P. Gulliford, Sarah L. Hall, Emma Sydes, Matthew R. Aguado-Barrera, Miguel E. Gomez-Caamano, Antonio Carballo, Ana M. Peleteiro, Paula Lobato-Busto, Ramon Stock, Richard Stone, Nelson N. Ostrer, Harry Usmani, Nawaid Singhal, Sandeep Tsuji, Hiroshi Imai, Takashi Saito, Shiro Eeles, Rosalind DeRuyck, Kim Parliament, Matthew Dunning, Alison M. Vega, Ana Rosenstein, Barry S. West, Catharine M. L. Departments of Radiation Oncology and Surgery University of Rochester Medical Center Rochester NY Department of Oncology Department of Public Health and Primary Care Department of Public Health and Primary Care Centre for Cancer Genetic Epidemiology Strangeways Research Laboratory University of Cambridge Cambridge UK Department of Oncology Cambridge University Hospitals NHS Foundation Trust Cambridge UK Department of Biostatistics and Computational Biology University of Rochester Medical Center Rochester NY Department of Biostatistics and Computational Biology University of Rochester Medical Center Rochester NY Department of Computational Biology University of Rochester Rochester NY Department of Genetics and Genomic Sciences and Icahn Institute for Data Science and Genomic Technology Icahn School of Medicine at Mount Sinai New York NY Department of Genetics and Genomic Sciences and Icahn Institute for Data Science and Genomic Technology Icahn School of Medicine at Mount Sinai New York NY Department of Genetics and Genomic Sciences and Icahn Institute for Data Science and Genomic Technology Icahn School of Medicine at Mount Sinai New York NY Department of Genetics and Genomic Sciences and Icahn Institute for Data Science and Genomic Technology Icahn School of Medicine at Mount Sinai New York NY Division of Biostatistics and Bioinformatics Department of Epidemiology and Public Health University of Maryland Greenebaum Cancer Center School of Medicine University of Maryland Baltimore Departments of Radiation Oncology and Surgery University of Rochester Medical Center Rochester NY Division of Cancer Sciences the University of Manchester Manchester Academic Health Science Centre Christie Hospital Manchester UK Centre for Cancer Genetic Epidemiology Strangeways Research Laboratory University of Cambridge Cambridge UK Department of Oncology Cambridge University Hospitals NHS Foundation Trust Cambridge UK Division of Cancer Sciences the University of Manchester Manches

Background A total of 10%-20% of patients develop long-term toxicity following radiotherapy for prostate cancer. Identification of common genetic variants associated with susceptibility to radiotoxicity might improve risk prediction and inform functional mechanistic *** We conducted an individual patient data meta-analysis of six genome-wide association studies (n = 3871) in men of European ancestry who underwent radiotherapy for prostate cancer. Radiotoxicities (increased urinary frequency, decreased urinary stream, hematuria, rectal bleeding) were graded prospectively. We used grouped relative risk models to test associations with approximately 6 million genotyped or imputed variants (time to first grade 2 or higher toxicity event). Variants with two-sided Pmeta less than 5 × 10−8 were considered statistically significant. Bayesian false discovery probability provided an additional measure of confidence. Statistically significant variants were evaluated in three Japanese cohorts (n = 962). All statistical tests were *** Meta-analysis of the European ancestry cohorts identified three genomic signals: single nucleotide polymorphism rs17055178 with rectal bleeding (Pmeta = 6.2 × 10−10), rs10969913 with decreased urinary stream (Pmeta = 2.9 × 10−10), and rs11122573 with hematuria (Pmeta = 1.8 × 10−8). Fine-scale mapping of these three regions was used to identify another independent signal (rs147121532) associated with hematuria (Pconditional = 4.7 × 10−6). Credible causal variants at these four signals lie in gene-regulatory regions, some modulating expression of nearby genes. Previously identified variants showed consistent associations (rs17599026 with increased urinary frequency, rs7720298 with decreased urinary stream, rs1801516 with overall toxicity) in new cohorts. rs10969913 and rs17599026 had similar effects in the photon-treated Japanese *** This study increases the understanding of the architecture of common gen

关键词： radiation therapy hematuria genes genome single nucleotide polymorphism urinary tract genetics prostate cancer rectal bleeding urinary frequency toxic effect genome-wide association study japanese imputation

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

arXiv

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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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Novel MAB phases and insights into their exfoliation into 2D MBenes

arXiv

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arXiv 2019年

作者： Khazaei, Mohammad Wang, Junjie Estili, Mehdi Ranjbar, Ahmad Suehara, Shigeru Arai, Masao Esfarjani, Keivan Yunoki, Seiji Computational Materials Science Research Team RIKEN Center for Computational Science R-CCS Hyogo Kobe650-0047 Japan State Key Laboratory of Solidification Processing Northwestern Polytechnical University Shaanxi Xi’an710072 China International Center for Materials Discovery School of Materials Science and Engineering Northwestern Polytechnical University Shaanxi Xi’an710072 China Research Center for Functional Materials RCFM National Institute for Materials Science NIMS Tsukuba305-0047 Japan International Center for Materials Nanoarchitectonics National Institute for Materials Science NIMS 1-1 Namiki Ibaraki Tsukuba305-0044 Japan Departments of Mechanical and Aerospace Engineering Physics and Materials Science and Engineering University of Virginia 122 Engineer’s Way CharlottesvilleVA22904 United States Computational Condensed Matter Physics Laboratory RIKEN Cluster for Pioneering Research CPR Saitama Wako351-0198 Japan Computational Quantum Matter Research Team RIKEN Center for Emergent Matter Science CEMS Saitama Wako351-0198 Japan

Considering the recent breakthroughs in the synthesis of novel two-dimensional (2D) materials from layered bulk structures, ternary layered transition metal borides, known as MAB phases, have come under scrutiny as a means of obtaining novel 2D transition metal borides, so-called MBene. Here, based on a set of phonon calculations, we show the dynamic stability of many Al-containing MAB phases, MAlB (M = Ti, Hf, V, Nb, Ta, Cr, Mo, W, Mn, Tc), M2AlB2 (Sc, Ti, Zr, Hf, V, Cr, Mo, W, Mn, Tc, Fe, Rh, Ni), M3Al2B2 (M = Sc, T, Zr, Hf, Cr, Mn, Tc, Fe, Ru, Ni), M3AlB4 (M = Sc, Ti, Zr, Hf, V, Nb, Ta, Cr, Mo, W, Mn, Fe), and M4AlB6 (M = Sc, Ti, Zr, Hf, V, Nb, Ta, Cr, Mo). By comparing the formation energies of these MAB phases with those of their available competing binary M−B and M−Al, and ternary M−Al−B phases, we find that some of the Sc-, Ti-, V-, Cr-, Mo-, W-, Mn-, Tc-, and Fe-based MAB phases could be favorably synthesized in an appropriate experimental condition. In addition, by examining the strengths of various bonds in MAB phases via crystal orbital Hamilton population and spring constant calculations, we find that the B−B and then M−B bonds are stiffer than the M−Al and Al−B bonds. The different strength between these bonds implies the etching possibility of Al atoms from MAB phases, consequently forming various 2D MB, M2B3, and M3B4 MBenes. Furthermore, we employ the nudged elastic band method to investigate the possibility of the structural phase transformation of the 2D MB MBenes into graphene-like boron sheets sandwiched between transition metals and find that the energy barrier of the transformation is less than 0.4 eV/atom. Copyright © 2019, The Authors. All rights reserved.

关键词： Transition metals

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Erratum: “The NANOGrav 15 yr data Set: Search for Signals from New physics” (2023, ApJL 951 L11)

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Astrophysical Journal. Letters 2024年第1期971卷 L27页

作者： Afzal, Adeela Agazie, Gabriella Anumarlapudi, Akash Freedman, Gabriel E Islo, Kristina Jones, Megan L Kaplan, David L McEwen, Alexander Sardesai, Shashwat C Susobhanan, Abhimanyu Vigeland, Sarah J Archibald, Anne M Arzoumanian, Zaven Baker, Paul T Bécsy, Bence Burnette, Rand Case, Robin DeGan, Dallas Deng, Heling Hazboun, Jeffrey S Laal, Nima Sun, Jerry P Taylor, Jacob Jose Juan Blanco-Pillado Blecha, Laura Boddy, Kimberly K Nay, Jonathan Brazier, Adam Brook, Paul R Burke-Spolaor, Sarah Cheeseboro, Belinda D Fiore, William Fonseca, Emmanuel Garver-Daniels, Nate Gentile, Peter A Glaser, Joseph Jennings, Ross J Kaiser, Andrew R Liu, Tingting Lorimer, Duncan R McLaughlin, Maura A Turner, Jacob E Wahl, Haley M Charisi, Maria Gersbach, Kyle A Lamb, William G McMann, Natasha Petrov, Polina Pol, Nihan S Schult, Levi Taylor, Stephen R Wang, Qiaohong Chatterjee, Shami Cordes, James M Cromartie, H Thankful Stella Koch Ocker Chatziioannou, Katerina Hourihane, Sophie Lee, Vincent S H Meyers, Patrick M Chen, Siyuan Cohen, Tyler Cornish, Neil J Crawford, Fronefield Crowter, Kathryn Stairs, Ingrid H Cutler, Curt J Vallisneri, Michele DeCesar, Megan E Demorest, Paul B Stovall, Kevin Dolch, Timothy Drachler, Brendan Lam, Michael T Young, Olivia Richard von Eckardstein Schmitz, Kai Schröder, Tobias Stratmann, Peter Ferrara, Elizabeth C Good, Deborah C Guertin, Lydia Gültekin, Kayhan Johnson, Aaron D Kelley, Luke Zoltan Kerr, Matthew Ray, Paul S Key, Joey S Lazio, T Joseph W Lewandowska, Natalia Rafael R Lino dos Santos Littenberg, Tyson B Luo, Jing Lynch, Ryan S Chung-Pei, Ma Madison, Dustin R McKee, James W Meyers, Bradley W Mingarelli, Chiara M F Mitridate, Andrea Natarajan, Priyamvada Ng, Cherry Nice, David J Swiggum, Joseph K Olum, Ken D Pennucci, Timothy T Perera, Benetge B P Radovan, Henri A Ransom, Scott M Romano, Joseph D Schmiedekamp, Ann Schmiedekamp, Carl Shapiro-Albert, Brent J Siemens, Xavier Simon, Joseph Siwek, Magdalena S Stinebring, Daniel R Tanner Trickle Unal, Caner Verma, Sonali Witt, Caitlin A Wright, David Zu Institute for Theoretical Physics University of Münster D-48149 Münster Germany comments@*** Department of Physics Quaid-i-Azam University Islamabad 45320 Pakistan Center for Gravitation Cosmology and Astrophysics Department of Physics University of Wisconsin-Milwaukee P.O. Box 413 Milwaukee WI 53201 USA Newcastle University NE1 7RU UK X-Ray Astrophysics Laboratory NASA Goddard Space Flight Center Code 662 Greenbelt MD 20771 USA Department of Physics and Astronomy Widener University One University Place Chester PA 19013 USA Department of Physics Oregon State University Corvallis OR 97331 USA Department of Physics University of Basque Country UPV/EHU E-48080 Bilbao Spain EHU Quantum Center University of Basque Country UPV/EHU Bilbao Spain IKERBASQUE Basque Foundation for Science E-48011 Bilbao Spain Physics Department University of Florida Gainesville FL 32611 USA Department of Physics The University of Texas at Austin Austin TX 78712 USA Cornell Center for Astrophysics and Planetary Science and Department of Astronomy Cornell University Ithaca NY 14853 USA Cornell Center for Advanced Computing Cornell University Ithaca NY 14853 USA Institute for Gravitational Wave Astronomy and School of Physics and Astronomy University of Birmingham Edgbaston Birmingham B15 2TT UK Department of Physics and Astronomy West Virginia University P.O. Box 6315 Morgantown WV 26506 USA Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building Morgantown WV 26505 USA Department of Physics and Astronomy Vanderbilt University 2301 Vanderbilt Place Nashville TN 37235 USA Cornell Center for Astrophysics and Planetary Science and Department of Astronomy Cornell University Ithaca NY 14853 USA Division of Physics Mathematics and Astronomy California Institute of Technology Pasadena CA 91125 USA Kavli Institute for Astronomy and Astrophysics Peking University Beijing 100871 People's Republi

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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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Community-developed checklists for publishing images and image analyses

arXiv

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arXiv 2023年

作者： Schmied, Christopher Nelson, Michael S. Avilov, Sergiy Bakker, Gert-Jan Bertocchi, Cristina Bischof, Johanna Boehm, Ulrike Brocher, Jan Carvalho, Mariana Chiritescu, Catalin Christopher, Jana Cimini, Beth A. Conde-Sousa, Eduardo Ebner, Michael Ecker, Rupert Eliceiri, Kevin Fernandez-Rodriguez, Julia Gaudreault, Nathalie Gelman, Laurent Grunwald, David Gu, Tingting Halidi, Nadia Hammer, Mathias Hartley, Matthew Held, Marie Jug, Florian Kapoor, Varun Koksoy, Ayse Aslihan Lacoste, Judith Le Dévédec, Sylvia Le Guyader, Sylvie Liu, Penghuan Martins, Gabriel G. Mathur, Aastha Miura, Kota Llopis, Paula Montero Nitschke, Roland North, Alison Parslow, Adam C. Payne-Dwyer, Alex Plantard, Laure Ali, Rizwan Schroth-Diez, Britta Schütz, Lucas Scott, Ryan T. Seitz, Arne Selchow, Olaf Sharma, Ved P. Spitaler, Martin Srinivasan, Sathya Strambio-De-Castillia, Caterina Taatjes, Douglas Tischer, Christian Jambor, HelenaKlara Fondazione Human Technopole Viale Rita Levi-Montalcini 1 Milano20157 Italy Department of Biomedical Engineering University of Wisconsin-Madison MadisonWI53706 United States Max Planck Institute of Immunobiology and Epigenetics Freiburg79108 Germany Medical BioSciences department Radboud University Medical Centre Nijmegen Netherlands Laboratory for Molecular mechanics of cell adhesions Pontificia Universidad Católica de Chile Santiago Chile Osaka University Graduate School of Engineering Science Japan Euro-BioImaging ERIC Bio-Hub Meyerhofstr. 1 Heidelberg69117 Germany Carl Zeiss AG Carl-Zeiss-Straße 22 Oberkochen73447 Germany BioVoxxel Scientific Image Processing and Analysis Eugen-Roth-Strasse 8 Ludwigshafen67071 Germany Nanophotonics and BioImaging Facility at INL International Iberian Nanotechnology Laboratory 4715-330 Portugal Phi Optics Inc. 1800 S. Oak St Ste 106 ChampaignIL61820 United States Biochemistry Center Heidelberg Heidelberg University Germany Imaging Platform Broad Institute CambridgeMA02142 United States i3S Instituto de Investigação e Inovação Em Saúde and INEB Instituto de Engenharia Biomédica Universidade do Porto Porto Portugal Translational Research Institute Queensland University of Technology 37 Kent Street WoolloongabbaQLD4102 Australia School of Biomedical Sciences Faculty of Health Queensland University of Technology BrisbaneQLD4059 Australia TissueGnostics GmbH Vienna1020 Austria Department of Medical Physics and Biomedical Engineering University of Wisconsin-Madison MadisonWI53706 United States Centre for Cellular Imaging Core Facility Sahlgrenska Academy University of Gothenburg Sweden Allen Institute for Cell Science SeattleWA United States Friedrich Miescher Institute for Biomedical Research Basel Switzerland RNA Therapeutics Institute University of Massachusetts Chan Medical School WorcesterMA01605 United States University of Oklahoma NormanOK United States Advanced Light Microscopy Unit Ce

Images document scientific discoveries and are prevalent in modern biomedical research. Microscopy imaging in particular is currently undergoing rapid technological advancements. However for scientists wishing to publish the obtained images and image analyses results, there are to date no unified guidelines. Consequently, microscopy images and image data in publications may be unclear or difficult to interpret. Here we present community-developed checklists for preparing light microscopy images and image analysis for publications. These checklists offer authors, readers, and publishers key recommendations for image formatting and annotation, color selection, data availability, and for reporting image analysis workflows. The goal of our guidelines is to increase the clarity and reproducibility of image figures and thereby heighten the quality and explanatory power of microscopy data is in publications. © 2023, CC BY-SA.

关键词： Image analysis

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

arXiv

引用

arXiv 2020年

作者： de Falco, Vittorio Battista, Emmanuele Capozziello, Salvatore de Laurentis, Mariafelicia Research Centre for Computational Physics and Data Processing Faculty of Philosophy & Science Silesian University in Opava Bezručovo nám. 13 OpavaCZ-74601 Czech Republic Karlsruhe76128 Germany Hermann-von-Helmholtz-Platz 1 Eggenstein-Leopoldshafen76344 Germany Università degli studi di Napoli "Federico II" Dipartimento di Fisica "Ettore Pancini" Complesso Universitario di Monte S. Angelo Via Cintia Edificio 6 Napoli80126 Italy Istituto Nazionale di Fisica Nucleare Sezione di Napoli Complesso Universitario di Monte S. Angelo Via Cintia Edificio 6 Napoli80126 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 analyse 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 model, it immediately implies the existence of a black hole;while in case of strong departures from such description it means that a wormhole could be present. Finally, we discuss our results and draw the conclusions. Copyright © 2020, The Authors. All rights reserved.

关键词： Gravitation

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A bimodal burst energy distribution of a repeating fast radio burst source

arXiv

引用

arXiv 2021年

作者： Li, D. Wang, Pei Zhu, W.W. Zhang, B. Zhang, X.X. Duan, R. Zhang, Y.K. Feng, Y. Tang, N.Y. Chatterjee, S. Cordes, J.M. Cruces, M. Dai, S. Gajjar, V. Hobbs, G. Jin, C. Kramer, M. Lorimer, D.R. Miao, C.C. Niu, C.H. Niu, J.R. Pan, Z.C. Qian, L. Spitler, L. Werthimer, D. Zhang, G.Q. Wang, F.Y. Xie, X.Y. Yue, Y.L. Zhang, L. Zhi, Q.J. Zhu, Y. CAS Key Laboratory of FAST NAOC Chinese Academy of Sciences Beijing100101 China University of Chinese Academy of Sciences Beijing100049 China Department of Physics and Astronomy University of Nevada Las Vegas Las VegasNV89154 United States CSIRO Astronomy and Space Science PO Box 76 EppingNSW1710 Australia Department of Physics Anhui Normal University Anhui Wuhu241002 China Cornell Center for Astrophysics and Planetary Science Department of Astronomy Cornell University IthacaNY14853 United States Max-Planck-Institut für Radioastronomie Auf dem Hügel 69 BonnD-53121 Germany Department of Astronomy University of California Berkeley BerkeleyCA94720 United States Department of Physics and Astronomy West Virginia University P.O. Box 6315 MorgantownWV26506 United States Center for Gravitational Waves and Cosmology West Virginia University Chestnut Ridge Research Building MorgantownWV United States School of Astronomy and Space Science Nanjing University Nanjing210093 China Ministry of Education Nanjing210093 China Guizhou Normal University Guiyang550001 China School of Physics and Technology Wuhan University Wuhan430072 China Western Sydney University Locked Bag 1797 PenrithNSW2751 Australia Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing Guizhou Normal University Guiyang550001 China

The event rate, energy distribution, and time-domain behaviour of repeating fast radio bursts (FRBs) contains essential information regarding their physical nature and central engine, which are as yet unknown. As the first precisely-localized source, FRB 121102 has been extensively observed and shows non-Poisson clustering of bursts over time and a power-law energy distribution. However, the extent of the energy distribution towards the fainter end was not known. Here we report the detection of 1652 independent bursts with a peak burst rate of 122 hr-1, in 59.5 hours spanning 47 days. A peak in the isotropic equivalent energy distribution is found to be ~ 4.8 × 1037erg at 1.25 GHz, below which the detection of bursts is suppressed. The burst energy distribution is bimodal, and well characterized by a combination of a log-normal function and a generalized Cauchy function. The large number of bursts in hour-long spans allow sensitive periodicity searches between 1 ms and 1000 s. The non-detection of any periodicity or quasi-periodicity poses challenges for models involving a single rotating compact object. The high burst rate also implies that FRBs must be generated with a high radiative efficiency, disfavoring emission mechanisms with large energy requirements or contrived triggering conditions. Copyright © 2021, The Authors. All rights reserved.

关键词： Poisson distribution

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