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Research Notes of the AAS 2019年第7期3卷

作者： Alice Allen P. Wesley Ryan Robert J. Nemiroff Astrophysics Source Code Library University of Maryland College Park USA Michigan Technological University USA

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Three-dimensional kinematic reconstruction of the optically-emitting, high-velocity, oxygen-rich ejecta of supernova remnant N132D

arXiv

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arXiv 2020年

作者： Law, Charles J. Milisavljevic, Dan Patnaude, Daniel J. Plucinsky, Paul P. Gladders, Michael D. Schmidt, Judy Sravan, Niharika Banovetz, John Sano, Hidetoshi McGraw, Jordan M. Takahashi, George Orlando, Salvatore Center for Astrophysics Harvard & Smithsonian 60 Garden St. CambridgeMA02138 United States Department of Physics and Astronomy Purdue University 525 Northwestern Avenue West LafayetteIN47907 United States Department of Astronomy & Astrophysics University of Chicago 5640 South Ellis Avenue ChicagoIL60637 United States Astrophysics Source Code Library Michigan Technological University 1400 Townsend Drive HoughtonMI49931 United States Institute for Advanced Research Nagoya University Furo-cho Chikusa-ku Nagoya464-8601 Japan Department of Physics Nagoya University Furo-cho Chikusa-ku Nagoya464-8601 Japan Research Computing ITaP Purdue University West LafayetteIN47907 United States INAF—Osservatorio Astronomico di Palermo "G.S. Vaiana" Piazza del Parlamento 1 PalermoI-90134 Italy

We present a three-dimensional kinematic reconstruction of the optically-emitting, oxygen-rich ejecta of supernova remnant N132D in the Large Magellanic Cloud. Data were obtained with the 6.5 m Magellan telescope in combination with the IMACS+GISMO instrument and survey [O III] λλ4959, 5007 line emission in a ∼30 × 30 region centered on N132D. The spatial and spectral resolution of our data enable detailed examination of the optical ejecta structure. The majority of N132D’s optically bright oxygen ejecta are arranged in a torus-like geometry tilted approximately 28◦ with respect to the plane of the sky. The torus has a radius of 4.4 pc (DLMC/50 kpc), exhibits a blue-shifted radial velocity asymmetry of −3000 to +2300 km s−1, and has a conspicuous break in its circumference. Assuming homologous expansion from the geometric center of O-rich filaments, the average expansion velocity of 1745 km s−1 translates to an age since explosion of 2450 ± 195 yr. A faint, spatially-separated "runaway knot" (RK) with total space velocity of 3650 km s−1 is nearly perpendicular to the torus plane and coincident with X-ray emission that is substantially enhanced in Si relative to the LMC and N132D’s bulk ejecta. These kinematic and chemical signatures suggest that the RK may have had its origin deep within the progenitor star. Overall, the main shell morphology and high-velocity, Si-enriched components of N132D have remarkable similarity with that of Cassiopeia A, which was the result of a Type IIb supernova explosion. Our results underscore the need for further observations and simulations that can robustly reconcile whether the observed morphology is dominated by explosion dynamics or shaped by interaction with the environment. Copyright © 2020, The Authors. All rights reserved.

关键词： Oxygen

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The Green Monster hiding in front of Cas A: JWST reveals a dense and dusty circumstellar structure pockmarked by ejecta interactions

arXiv

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arXiv 2024年

作者： De Looze, Ilse Milisavljevic, Dan Temim, Tea Dickinson, Danielle Fesen, Robert Arendt, Richard G. Chastenet, Jeremy Orlando, Salvatore Vink, Jacco Barlow, Michael J. Kirchschlager, Florian Priestley, Felix D. Raymond, John C. Rho, Jeonghee Sartorio, Nina S. Scheffler, Tassilo Schmidt, Franziska Blair, William P. Fox, Ori Fryer, Christopher Janka, Hans-Thomas Koo, Bon-Chul Laming, J. Martin Matsuura, Mikako Patnaude, Dan Relaño, Mónica Rest, A. Schmidt, Judy Smith, Nathan Sravan, Niharika Sterrenkundig Observatorium Ghent University Krijgslaan 281 - S9 GentB-9000 Belgium Purdue University Department of Physics and Astronomy 525 Northwestern Ave West LafayetteIN47907 United States Integrative Data Science Initiative Purdue University West LafayetteIN47907 United States Princeton University 4 Ivy Ln PrincetonNJ08544 United States Purdue University Department of Physics and Astronomy 525 Northwestern Ave West LafayetteIN47907 United States 6127 Wilder Lab Department of Physics and Astronomy Dartmouth College HanoverNH03755 United States Center for Space Sciences and Technology University of Maryland Baltimore County BaltimoreMD21250 United States Code 665 NASA/GSFC 8800 Greenbelt Road GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States INAF Osservatorio Astronomico di Palermo Piazza del Parlamento 1 Palermo90134 Italy Anton Pannekoek Institute for Astronomy & GRAPPA University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands SRON Netherlands Institute for Space Research Niels Bohrweg 4 CA Leiden2333 Netherlands Department of Physics and Astronomy University College London Gower Street LondonWC1E 6BT United Kingdom School of Physics & Astronomy Cardiff University The Parade CardiffCF24 3AA United Kingdom Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States SETI Institute 339 Bernardo Ave. Ste. 200 Mountain ViewCA94043 United States Department of Physics and Astronomy Seoul National University Gwanak-ro 1 Gwanak-gu Seoul08826 Korea Republic of The William H. Miller III Department of Physics and Astronomy Johns Hopkins University 3400 N. Charles Street BaltimoreMD21218 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Center for Theoretical Astrophysics Los Alamos National Laboratory Los AlamosNM87545 Unite

JWST observations of the young Galactic supernova remnant Cassiopeia A revealed an unexpected structure seen as a green emission feature in colored composite MIRI F1130W and F1280W images – hence dubbed the Green Monster – that stretches across the central parts of the remnant in projection. Combining the kinematic information from NIRSpec and MIRI MRS with the multi-wavelength imaging from NIRCam and MIRI, we associate the Green Monster with circumstellar material that was lost during an asymmetric mass-loss phase. MIRI images are dominated by dust emission but its spectra show emission lines from Ne, H and Fe with low radial velocities indicative of a CSM nature. An X-ray analysis of this feature in a companion paper (Vink et al. 2024) supports its CSM nature and detects significant blue shifting, thereby placing the Green Monster on the near side, in front of the Cas A SN remnant. The most striking features of the Green Monster are dozens of almost perfectly circular 1′′ − 3′′ sized holes, most likely created by interaction between high-velocity SN ejecta material and the CSM. Further investigation is needed to understand whether these holes were formed by small 8000–10500 km s−1 N-rich ejecta knots that penetrated and advanced out ahead of the remnant’s 5000 - 6000 km s−1 outer blastwave, or by narrow ejecta fingers that protrude into the forward-shocked CSM. The detection of the Green Monster provides further evidence of the highly asymmetric mass-loss that Cas A’s progenitor star underwent prior to its explosion. © 2024, CC BY.

关键词： Supernovae

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A JWST Survey of the Supernova Remnant Cassiopeia A

arXiv

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arXiv 2024年

作者： Milisavljevic, Dan Temim, Tea De Looze, Ilse Dickinson, Danielle Laming, J. Martin Fesen, Robert Raymond, John C. Arendt, Richard G. Vink, Jacco Posselt, Bettina Pavlov, George G. Fox, Ori D. Pinarski, Ethan Subrayan, Bhagya Schmidt, Judy Blair, William P. Rest, Armin Patnaude, Daniel Koo, Bon-Chul Rho, Jeonghee Orlando, Salvatore Janka, Hans-Thomas Andrews, Moira Barlow, Michael J. Burrows, Adam Chevalier, Roger Clayton, Geoffrey Fransson, Claes Fryer, Christopher Gomez, Haley L. Kirchschlager, Florian Lee, Jae-Joon Matsuura, Mikako Niculescu-Duvaz, Maria Pierel, Justin D.R. Plucinsky, Paul P. Priestley, Felix D. Ravi, Aravind P. Sartorio, Nina S. Schmidt, Franziska Shahbandeh, Melissa Slane, Patrick Smith, Nathan Sravan, Niharika Weil, Kathryn Wesson, Roger Wheeler, J. Craig Purdue University Department of Physics and Astronomy 525 Northwestern Ave West LafayetteIN47907 United States Integrative Data Science Initiative Purdue University West LafayetteIN47907 United States Princeton University 4 Ivy Ln PrincetonNJ08544 United States Sterrenkundig Observatorium Ghent University Krijgslaan 281 - S9 GentB-9000 Belgium Space Science Division Code 7684 Naval Research Laboratory WashingtonDC20375 United States 6127 Wilder Lab Department of Physics and Astronomy Dartmouth College HanoverNH03755 United States Center for Astrophysics Harvard & Smithsonian 60 Garden Street CambridgeMA02138 United States Center for Space Sciences and Technology University of Maryland Baltimore County BaltimoreMD21250 United States NASA/GSFC 8800 Greenbelt Road GreenbeltMD20771 United States Center for Research and Exploration in Space Science and Technology NASA/GSFC GreenbeltMD20771 United States Anton Pannekoek Institute for Astronomy & GRAPPA University of Amsterdam Science Park 904 Amsterdam1098 XH Netherlands SRON Netherlands Institute for Space Research Niels Bohrweg 4 CA Leiden2333 Netherlands Department of Astrophysics University of Oxford Denys Wilkinson Building Keble Road OxfordOX1 3RH United Kingdom Department of Astronomy & Astrophysics Pennsylvania State University 525 Davey Lab University ParkPA16802 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Astrophysics Source Code Library Michigan Technological University 1400 Townsend Drive HoughtonMI49931 United States The William H. Miller III Department of Physics and Astronomy Johns Hopkins University 3400 N. Charles Street BaltimoreMD21218 United States Department of Physics and Astronomy Seoul National University Seoul08861 Korea Republic of SETI Institute 189 Bernardo Ave. Ste. 200 Mountain ViewCA94043 United States Department of Physics and Astronomy Seoul National University Gwanak-ro 1 G

We present initial results from a JWST survey of the youngest Galactic core-collapse supernova remnant Cassiopeia A (Cas A), made up of NIRCam and MIRI imaging mosaics that map emission from the main shell, interior, and surrounding circumstellar/interstellar material (CSM/ISM). We also present four exploratory positions of MIRI/MRS IFU spectroscopy that sample ejecta, CSM, and associated dust from representative shocked and unshocked regions. Surprising discoveries include: 1) a web-like network of unshocked ejecta filaments resolved to ∼ 0.01 pc scales exhibiting an overall morphology consistent with turbulent mixing of cool, low-entropy matter from the progenitor’s oxygen layer with hot, high-entropy matter heated by neutrino interactions and radioactivity, 2) a thick sheet of dust-dominated emission from shocked CSM seen in projection toward the remnant’s interior pockmarked with small (∼ 1′′) round holes formed by 0′′ . 1 knots of high-velocity ejecta that have pierced through the CSM and driven expanding tangential shocks, 3) dozens of light echoes with angular sizes between ∼ 0′′ . 1 to 1′ reflecting previously unseen fine-scale structure in the ISM. NIRCam observations place new upper limits on infrared emission ( 20 nJy at 3 µm) from the neutron star in Cas A’s center and tightly constrain scenarios involving a possible fallback disk. These JWST survey data and initial findings help address unresolved questions about massive star explosions that have broad implications for the formation and evolution of stellar populations, the metal and dust enrichment of galaxies, and the origin of compact remnant objects. © 2024, CC BY.

关键词： Supernovae

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A giant umbrella-like stellar stream around the tidal ring galaxy NGC 922

arXiv

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arXiv 2022年

作者： Martínez-Delgado, David Roca-Fàbrega, Santi Miró-Carretero, Juan Gómez-Flechoso, Maria Angeles Román, Javier Donatiello, Giuseppe Schmidt, Judy Lang, Dustin Akhlaghi, Mohammad Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía GranadaE-18080 Spain Instituto de Astronomía Universidad Nacional Autónoma de México Apartado Postal 106 B. C. EnsenadaC. P. 22800 Mexico Departamento de Física de la Tierra y Astrofísica Universidad Complutense de Madrid MadridE-28040 Spain Fac. CC. Físicas Universidad Complutense de Madrid Plaza de las Ciencias 1 MadridE-28040 Spain Kapteyn Astronomical Institute University of Groningen PO Box 800 Groningen9700 AV Netherlands Instituto de Astrofísica de Canarias c/Vía Láctea s/n Tenerife La Laguna38205 Spain Departamento de Astrofísica Universidad de La Laguna La LagunaE-38200 Spain UAI - Unione Astrofili Italiani/P.I. Sezione Nazionale di Ricerca Profondo Cielo Oria72024 Italy Astrophysics Source Code Library University of Maryland 4254 Stadium Drive College ParkMD20742 United States Perimeter Institute for Theoretical Physics 31 Caroline St N Waterloo Canada Unidad Asociada al CSIC Plaza San Juan 1 Teruel44001 Spain

Context. Tidal ring galaxies are observed rarely in the local universe due to their intrinsically transient nature. The tidal ring structures are the result of strong interactions between gas-rich stellar disks and smaller galactic systems and do not last longer than ∼500 Myr therefore, these are perfect scenarios where to find the debris of recently accreted dwarf galactic systems. Aims. Our goal is to study the low surface brightness stellar structures around the NGC 922 tidal ring galaxy, and to revise the hypothesis of its formation at the light of these new data. Methods. We present new deep images of the NGC 922 tidal ring galaxy and its surroundings from the DESI Legacy survey data and from our observations with an amateur telescope. These observations are compared with results from high-resolution N-body simulations designed to reproduce an alternative formation scenario for this peculiar galaxy. Results. Our new observations unveil that the low surface brightness stellar tidal structures around NGC 922 are much more complex than reported in previous works. In particular, the formerly detected tidal spike-like structure at the northeast of the central galaxy disk is not connected with the dwarf companion galaxy PGC 3080368, which has been suggested as the intruder triggering the ring formation of NGC 922. The deep images reveal that this tidal structure is mainly composed by a fainter giant umbrella-like shape and thus it was formed from the tidal disruption of a different satellite. Using the broad-band g, r and z DESI LS images, we measured the photometric properties of this stellar stream, estimating a total absolute magnitude in r-band of Mr= -17.0 ± 0.03 magn and a total stellar mass for the stream between 6.9 -8.5 ×108 M☉. We perform a set of N-body simulations to reproduce the observed NGC922-intruder interaction, suggesting a new scenario for the formation of its tidal ring from the infall of a gas rich satellite around 150 Myr ago. Finally, our deep

关键词： Galaxies

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Crepuscular rays from the highly inclined active galactic nucleus in IC 5063

arXiv

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arXiv 2020年

作者： Maksym, W. Peter Schmidt, Judy Keel, William C. Fabbiano, Giuseppina Fischer, Travis C. Bland-Hawthorn, Joss Barth, Aaron J. Elvis, Martin Oosterloo, Tom Ho, Luis C. Kim, Minjin Hwang, Hyunmo Mayer, Evan Center for Astrophysics Harvard-Smithsonian 60 Garden St. CambridgeMA02138 United States Astrophysics Source Code Library University of Maryland 4254 Stadium Drive College ParkMD20742 United States Department of Physics and Astronomy University of Alabama Box 870324 TuscaloosaAL35487 United States Space Telescope Science Institute 3700 San Martin Drive BaltimoreMD21218 United States Sydney Institute of Astronomy School of Physics University of Sydney Australia ARC Centre of Excellence for All Sky Astrophysics in 3D Australia Department of Physics and Astronomy University of California at Irvine 4129 Frederick Reines Hall IrvineCA92697-4575 United States ASTRON Netherlands Institute for Radio Astronomy Postbus 2 AA Dwingeloo7990 Netherlands Kapteyn Astronomical Institute University of Groningen Postbus 800 Groningen9700 AV Netherlands Kavli Institute for Astronomy and Astrophysics Peking University Beijing100871 China Department of Astronomy School of Physics Peking University Beijing100871 China Department of Astronomy and Atmospheric Sciences College of Natural Sciences Kyungpook National University Daegu41566 Korea Republic of Independent researcher TucsonAZ85719 United States

On Earth near sunset, the sun may cast "crepuscular rays" such that clouds near the horizon obscure the origin of light scattered in bright rays. In principle, AGN should be able to produce similar effects. Using new Hubble Space Telescope (HST) near-infrared and optical observations, we show that the active galaxy IC 5063 contains broad radial rays extending to ∼> 11 kpc from the nucleus. We argue that the bright rays may arise from dusty scattering of continuum emission from the active nucleus, while the dark rays are due to shadowing near the nucleus, possibly by a warped torus. We also consider alternative AGN-related and stellar origins for the extended light. Copyright © 2020, The Authors. All rights reserved.

关键词： Galaxies

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Hidden depths in the local Universe: The Stellar Stream Legacy Survey

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Astronomy and astrophysics 2023年 671卷

作者： Martínez-Delgado, David Cooper, Andrew P. Román, Javier Pillepich, Annalisa Erkal, Denis Pearson, Sarah Moustakas, John Laporte, Chervin F. P. Laine, Seppo Akhlaghi, Mohammad Lang, Dustin Makarov, Dmitry Borlaff, Alejandro S. Donatiello, Giuseppe Pearson, William J. Miró-Carretero, Juan Cuillandre, Jean-Charles Domínguez, Helena Roca-Fàbrega, Santi Frenk, Carlos S. Schmidt, Judy Gómez-Flechoso, María A. Guzman, Rafael Libeskind, Noam I. Dey, Arjun Weaver, Benjamin A. Schlegel, David Myers, Adam D. Valdes, Frank G. Instituto de Astrofísica de Andalucía CSIC Glorieta de la Astronomía Granada18080 Spain Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Mönchhofstr. 12-14 Heidelberg69120 Germany Institute of Astronomy Department of Physics National Tsing Hua University Kuang Fu Rd. Sec. 2 Hsinchu30013 Taiwan Center for Informatics and Computation in Astronomy National Tsing Hua University Kuang Fu Rd. Sec. 2 Hsinchu30013 Taiwan Max Planck Institut für Astronomie Königstuhl 17 Heidelberg69117 Germany Department of Physics University of Surrey GuildfordGU27XH United Kingdom Center for Cosmology and Particle Physics Department of Physics New York University 726 Broadway New YorkNY10003 United States Siena College Department of Physics & Astronomy 515 Loudon Road LoudonvilleNY12211 United States University of Tokio Chiba277-8583 Japan IPAC Caltech Mail Code 314-6 1200 E. California BLVd. PasadenaCA91125 United States Calle Vía Láctea s/n Tenerife La Laguna38205 Spain Facultad de Física Universidad de la Laguna Avda. Astrofísico Fco. Sánchez s/n Tenerife La Laguna38200 Spain Perimeter Institute for Theoretical Physics 31 Caroline St N Waterloo Canada Special Astrophysical Observatory Russian Academy of Sciences Nizhnij Arkhyz369167 Russia NASA Ames Research Center Moffett FieldCA94035 United States UAI -Unione Astrofili Italiani P.I. Sezione Nazionale di Ricerca Profondo Cielo Oria72024 Italy National Centre for Nuclear Research ul. Pasteura 7 Warszawa02-093 Poland Departamento de Física de la Tierra y Astrofísica Universidad Complutense de Madrid Plaza de las Ciencias Madrid28040 Spain AIM CEA CNRS Université Paris-Saclay Université de Paris Orme des Merisiers Gif-sur-Yvette91191 France CSIC Campus UAB Carrer de Magrans Barcelona08193 Spain Institute for Computational Cosmology Department of Physics Durham University South Road DurhamDH1 3LE United Kingdom Astrophysics Source Code Librar

Context. Mergers and tidal interactions between massive galaxies and their dwarf satellites are a fundamental prediction of the Lambda-cold dark matter cosmology. These events are thought to provide important observational diagnostics of non-linear structure formation. Stellar streams in the Milky Way and Andromeda are spectacular evidence for ongoing satellite disruption. However, constructing a statistically meaningful sample of tidal streams beyond the Local Group has proven a daunting observational challenge, and the full potential for deepening our understanding of galaxy assembly using stellar streams has yet to be realised. Aims. Here we introduce the Stellar Stream Legacy Survey, a systematic imaging survey of tidal features associated with dwarf galaxy accretion around a sample of ~3100 nearby galaxies within z ~ 0.02, including about 940 Milky Way analogues. Methods. Our survey exploits public deep imaging data from the DESI Legacy Imaging Surveys, which reach surface brightness as faint as ~29 mag arcsec2 in the r band. As a proof of concept of our survey, we report the detection and broad-band photometry of 24 new stellar streams in the local Universe. Results. We discuss how these observations can yield new constraints on galaxy formation theory through comparison to mock observations from cosmological galaxy simulations. These tests will probe the present-day mass assembly rate of galaxies, the stellar populations and orbits of satellites, the growth of stellar halos, and the resilience of stellar disks to satellite bombardment. © 2023 The Authors.

关键词： Galaxies

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Nine best practices for research software registries and repositories: A concise guide

arXiv

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arXiv 2020年

作者： Monteil, Alain Gonzalez-Beltran, Alejandra Ioannidis, Alexandros Allen, Alice Lee, Allen Bandrowski, Anita Wilson, Bruce E. Mecum, Bryce Du, Cai Fan Robinson, Carly Garijo, Daniel Katz, Daniel S. Long, David Milliken, Genevieve Ménager, Hervé Hausman, Jessica Spaaks, Jurriaan H. Fenlon, Katrina Vanderbilt, Kristin Hwang, Lorraine Davis, Lynn Fenner, Martin Crusoe, Michael R. Hucka, Mike Wu, Mingfang Hong, Neil Chue Teuben, Peter Stall, Shelley Druskat, Stephan Carnevale, Ted Morrell, Tom INRIA HAL Software Heritage France Science and Technology Facilities Council UK Research and Innovation United Kingdom CERN Zenodo Australia University of Maryland Astrophysics Source Code Library United States Arizona State University CoMSES Net United States UCSD SciCrunch United States Oak Ridge National Laboratory ORNL Distributed Active Archive Center for Biogeochemical Dynamics United States NCEAS UC Santa Barbara CodeMeta United States ISchool University of Texas at Austin CiteAs United States DOE OSTI Italy Information Sciences Institute University of Southern California Ontosoft United States University of Illinois at Urbana-Champaign Associate EiC for JOSS FORCE11 Software Citation Implementation Working Group United States Brigham Young University IEEE GRS Remote Sensing Code Library United States NYU Bobst Library IASGE United States Institut Pasteur ELIXIR bio.tools France Jet Propulsion Laboratory PO.DAAC United States Netherlands eScience Center Research Software Directory Netherlands University of Maryland ISchool United States Environmental Data Initiative IMCR Computational Infrastructure for Geodynamics UC Davis United States DataCite FORCE11 Software Citation Implementation Working Group Germany CWL Debian-Med Caltech SBML COMBINE United States Australian Research Data Commons Australia Software Sustainability Institute University of Edinburgh FORCE11 Software Citation Implementation Working Group United Kingdom University of Maryland United States American Geophysical Union AGU Data Services United States University Jena Humboldt-Universität zu Berlin Germany Neuroscience Department Yale University ModelDB United States Caltech CaltechDATA United States

Scientific software registries and repositories serve various roles in their respective disciplines. These resources improve software discoverability and research transparency, provide information for software citations, and foster preservation of computational methods that might otherwise be lost over time, thereby supporting research reproducibility and replicability. However, developing these resources takes effort, and few guidelines are available to help prospective creators of registries and repositories. To address this need, we present a set of nine best practices that can help managers define the scope, practices, and rules that govern individual registries and repositories. These best practices were distilled from the experiences of the creators of existing resources, convened by a Task Force of the FORCE11 Software Citation Implementation Working Group during the years 2019–2020. We believe that putting in place specific policies such as those presented here will help scientific software registries and repositories better serve their users and their disciplines. © 2020, CC BY.

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Elevating the role of software as a product of the research enterprise

arXiv

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arXiv 2019年

作者： Smith, Arfon M. Norman, Dara Cruz, Kelle Desai, Vandana Bellm, Eric Lundgren, Britt Economou, Frossie Nord, Brian D. Schafer, Chad Narayan, Gautham Harrington, Joseph Tollerud, Erik Sipőcz, Brigitta Pickering, Timothy Peeples, Molly S. Berriman, Bruce Teuben, Peter Rodriguez, David Gradvohl, Andre Shamir, Lior Allen, Alice Brownstein, Joel R. Ginsburg, Adam Sinha, Manodeep Hummels, Cameron Smith, Britton Stevance, Heloise Price-Whelan, Adrian Cherinka, Brian Chan, Chi-kwan Kartaltepe, Jeyhan Turk, Matthew Weiner, Benjamin Modjaz, Maryam Nemiroff, Robert J. Kerzendorf, Wolfgang Laginja, Iva Dong, Chuanfei Merín, Bruno Sobeck, Jennifer Buzasi, Derek Faherty, Jacqueline K. Momcheva, Ivelina Connolly, Andrew Golkhou, V. Zach Space Telescope Science Institute NOAO Hunter College-CUNY IPAC University of Washington University of North Carolina Ashville LSST Fermilab/University of Chicago Carnegie Mellon University University of Central Florida STScI MMT Observatory Space Telescope Science Institute JHU University of Maryland University of Campinas Kansas State University Astrophysics Source Code Library University of Maryland University of Utah NRAO Swinburne University of Technology Caltech University of Edinburgh University of Sheffield University of Auckland Princeton United States Steward Observatory Rochester Institute of Technology School of Information Sciences NYU Michigan Technological University ESO ESAC Florida Gulf Coast University American Museum of Natural History University of Washington

Software is a critical part of modern research, and those responsible for its development must be retained in the workforce to maximize the scientific return from petabyte-scale datasets. This white paper will present current challenges and suggest practical solutions for elevating the role of software as a product of the research enterprise. Copyright © 2019, The Authors. All rights reserved.

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Quantifying feedback from narrow line region outflows in nearby active galaxies. II. spatially resolved mass outflow rates for the QSO2 markarian 34

arXiv

引用

arXiv 2018年

作者： Revalski, M. Dashtamirova, D. Crenshaw, D.M. Kraemer, S.B. Fischer, T.C. Schmitt, H.R. Gnilka, C.L. Schmidt, J. Elvis, M. Fabbiano, G. Storchi-Bergmann, T. Maksym, W.P. Gandhi, P. Department of Physics and Astronomy Georgia State University 25 Park Place AtlantaGA30303 United States Institute for Astrophysics and Computational Sciences Department of Physics Catholic University of America WashingtonDC20064 United States Astrophysics Science Division Goddard Space Flight Center Code 665 GreenbeltMD20771 United States Naval Research Laboratory WashingtonDC20375 United States Designer/Developer for the Astrophysics Source Code Library Harvard-Smithsonian Center for Astrophysics 60 Garden St. CambridgeMA02138 United States Departamento de Astronomia Universidade Federal Do Rio Grande Do Sul if CP 15051 Porto Alegre RS91501-970 Brazil Department of Physics and Astronomy University of Southampton SouthamptonSO17 3RT United Kingdom James Webb Space Telescope NASA Postdoctoral Program Fellow

We present spatially resolved mass outow rate measurements (Mout) for the narrow line region of Markarian 34, the nearest Compton-thick type 2 quasar (QSO2). Spectra obtained with the Hubble Space Telescope and at Apache Point Observatory reveal complex kinematics, with distinct signatures of outow and rotation within 2 kpc of the nucleus. Using multi-component photoionization models, we find that the outow contains a total ionized gas mass of M ≈ 1.6 × 106Mo. Combining this with the kinematics yields a peak outow rate of Mout≈ 2.0 ± 0.4 Mo yr-1at a distance of 470 pc from the nucleus, with a spatially integrated kinetic energy of E ≈ 1:4 × 1055erg. These outows are more energetic than those observed in Mrk 573 and NGC 4151, supporting a correlation between luminosity and outow strength even though they have similar peak outow rates. The mix of rotational and outowing components suggests that spatially resolved observations are required to determine accurate outow parameters in systems with complex kinematics. (See appended erratum for updated values.). Copyright © 2018, The Authors. All rights reserved.

关键词： Kinematics

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