DOCSLIB.ORG

National Astronomy Meeting 2019 Abstracts

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
National Astronomy Meeting 2019 Abstracts National Astronomy Meeting 2019 Abstracts 1 CONTENTS Springer – Gold Sponsors .................................................................................................. 4 Active Region Laboratories (ActiveRegions) ...................................................................... 5 Bridging the Disciplines of Galactic and Extra-galactic Archaeology (GalArchaeology) ...... 16 Connecting MHD Wave Research from the Sun to the Magnetospheres (MHDWavesSTP) 28 Cosmic Web: Bridging Galaxies and Cosmology (CosmicWeb) ......................................... 36 Cultural and Archaeo-Astronomical Tools in the Digital Age (AstroTools) ........................ 45 Current Developments in Numerical Astrophysics (NumericalAstro) ............................... 48 Education, Outreach and Engagement: What are they and what works? (EduOutrchEngage) ...................................................................................................................................... 56 Electrodynamics and energetics of the ionosphere-thermosphere system (IonosThermos) ...................................................................................................................................... 67 Engaging the public and schools with science through the solar system (EngagementSTP) ...................................................................................................................................... 71 Equality, diversity, and inclusion (EqualityDiversity) ....................................................... 80 Explosive energy release in the solar atmosphere (SolarAtmos) ...................................... 86 Gaia Data Release 2: Contents, Acces and Use (Gaia) .................................................... 102 Galaxy Clusters in the next decade (GalClusters) ........................................................... 107 Galaxy-Black Hole Co-evolution: Observational and Theoretical Perspectives (GalBlackHoles) ............................................................................................................ 114 Gravitational waves & multimessenger astronomy (GravWaves) .................................. 125 Impact of astronomy: ideas, inventions and people (AstroImpact) ................................ 136 Linking the Sun to the Heliosphere – the Solar Orbiter Mission (SolarOrbiter) ............... 140 Machine Learning in Astrophysics (MachineLearning) ................................................... 153 Magnetohydrodynamic Waves and Instabilities in the Solar Atmosphere in the High- Resolution Era (SolarMHDWav) .................................................................................... 161 Mapping the influence of Magnetosphere-Ionosphere interactions on the surface magnetic field and grounded infrastructure (GroundMag) ........................................................... 173 MOONS: The next generation spectrograph for the VLT (MOONS)................................. 181 Open session on Magnetospheric, Ionospheric and Solar-Terrestrial physics (MISTGeneral) .................................................................................................................................... 183 2 Planetary Magnetospheres (Magnetospheres) .............................................................. 206 Pro-Am Collaborations in Astronomy (ProAm) .............................................................. 223 Radiation belt dynamics at Earth and beyond (RadiationBelt) ....................................... 229 Role of shocks in the solar atmosphere and solar-terrestrial environment (SolarSTPShocks) .................................................................................................................................... 240 Studying galaxy evolution from reionization to cosmic noon with the latest-generation multiwavelength facilites (GalEvolution) ....................................................................... 245 The ESA M5 Missions (ESA M5) ..................................................................................... 259 Theory and Observations of the Cycling of Baryons around Galaxies (BaryonGal) .......... 261 Time-domain astronomy with the next-generation Liverpool Telescope (AstroLivT) ...... 270 Transients in the wide-field sky survey era (Transients) ................................................ 281 UV astronomy in the post-HST era (postHST) ................................................................ 288 3 SPRINGER – GOLD SPONSORS Springer is proud to be a gold sponsor of National Astronomy Meeting 2019 in Lancaster. We publish a major collection of research and review journals in this field including Astronomy and Astrophysics Review, Astrophysics and Space Science, Experimental Astronomy, and Space Science Reviews. Springer also publishes a renowned list of astronomy and space sciences books, from academic to popular science. Springer is a leading global scientific, technical and medical portfolio, providing researchers in academia, scientific institutions and corporate R&D departments with quality content through innovative information, products and services. Springer is part of Springer Nature, a global publisher that serves and supports the research community. 4 ACTIVE REGION LABORATORIES (ACTIVEREGIONS) Peter Wyper (Durham University) C. R. DeVore (GSFC), S. K. Antiochos (GSFC) Talk A Numerical Simulation of an Active Region Periphery Helical Jet Coronal jets are observed above minority polarity intrusions throughout the solar corona. Some of the most energetic occur on the periphery of active regions where the magnetic field is strongly inclined. These jets exhibit a non-radial propagation in the low corona as they follow the inclined field, and often have a broad, helical shape. We present a three- dimensional magnetohydrodynamic simulation of such an active region periphery helical jet. Free energy is injected into an initially potential field, creating a sigmoidal flux rope which eventually erupts to produce the helical jet. We find that the eruption results from a combination of magnetic breakout and an ideal kinking of the erupting flux rope. We discuss how the two mechanisms are coupled, and contrast our results with our previous simulations of coronal-hole jets. Dylan Williams (Aberystwyth University) Dylan Williams, Huw Morgan Talk Active longitudes and rotation rates: a large survey of active regions observed by AIA/SDO. A large-scale survey of Active Regions (AR) has been carried out over approximately 8 years, or the entire SDO dataset. Using a 2-stage identification process all observed ARs are identified and tracked in 5 different EUV wavelengths (131, 171, 193, 211 and 304). This reduced set of data leads to several different avenues of research. This first study focuses on active longitudes (AL). Plotting the mean longitudinal positions of these ARs over the entire time period reveals several bands of increased AR frequency drifting faster than the Carrington rotation rate. These bands can last for several years, and are regions that host several distinct ARs over these long periods. Understanding ALs can lead to a better understanding of the production and transport of the magnetic field within the solar interior, and can contribute towards predicting increased space weather risk over long timescales. 5 Natasha Jeffrey (University of Glasgow) Natasha L. S. Jeffrey Invited Active regions, the origin of solar flares, and a laboratory for studying particle acceleration Solar active regions are sites of complex magnetic activity and the origin of transient events like flares, where magnetic energy is released and dissipated in the solar atmosphere. Flares are efficient particle accelerators, and prime laboratories for studying acceleration processes in astrophysics, with a high fraction of the released energy being carried by energetic particles. Over the last decade, our understanding of flare particle acceleration has been enhanced by multi-wavelength observations from X-rays to (E)UV to radio. However, many questions remain about how and where energetic particles are accelerated, and how different plasma environments (e.g., collisions, turbulence) affect the transport and observed properties of energetic particles. We anticipate that proposed missions with direct X-ray imaging capabilities (e.g. FOXSI) could probe high energy processes in active regions in unprecedented detail, while data from a new generation of observatories (e.g. Solar Probe/Solar Orbiter) will help to understand the connection between energetic particles at the Sun and those measured in situ in the heliosphere. Thomas Williams (UCLAN) Thomas Williams, Robert W. Walsh, Amy Winebarger, & the Hi-C team Poster Are We Now Fully Resolving Coronal Loops? The High-resolution Coronal Imager (Hi-C) has been launched three times from White Sands Missile Range. The first launch (Hi-C 1), occurred on 11 July 2012 and during the 345 seconds of data acquisition, Hi-C 1 obtained the highest spatial resolution and highest cadence images of the EUV (19.3 nm) solar corona ever achieved. Those few minutes of data have thus far generated >25 refereed publications and is arguably one of the most scientifically successful sounding rocket payloads ever launched by NASA. Unfortunately, the second launch (Hi-C 2) did not result in any science data. On 29 May 2018, it was launched for a third time (Hi-C 2.1). On this occasion, 329 seconds of 17.2 nm data of target active region AR12712, was captured with a cadence of ~5.5s, and a plate scale of ~0.13x0.13
Load more

Recommended publications
  • A Comparison Study on Thermal Control Techniques for a Nanosatellite Carrying Infrared Science Instrument
    ICES-2020-15 A comparison study on thermal control techniques for a nanosatellite carrying infrared science instrument Shanmugasundaram Selvadurai1, Amal Chandran2, Sunil C Joshi3 and Teo Hang Tong Edwin 4 Nanyang Technological University, Singapore, 639798 David Valentini5 Thales Alenia Space, Cannes, 06150, France Friedhelm Olschewski6 University of Wuppertal, 42119 Wuppertal, Germany Based on current technological advancements and forecasts, nanosatellites will be used for both scientific and defense applications leveraging advantages on both development cost and development lifecycle. As nanosatellites become more capable, there is an increase in demand for high power applications which makes the missions complex from implementing a proper thermal control system (TCS) to dissipate the huge waste heat generated. One of the applications for nanosatellites is advanced infrared imaging for both scientific and military applications. ARCADE (Atmospheric coupling and Dynamics Explorer), a 27U satellite is being developed by Satellite Research Centre (SaRC) at Nanyang Technological University (NTU) for scientific objectives. The main payload AtmoLITE needs a detector cool down at -30°C and to meet this requirement, an appropriate classical TCS is chosen and described in this paper. Nanosatellites carrying infrared, cryogenic or other scientific instruments that need active cooling, should be equipped with a proper TCS within the highly constrained available volume. Another objective of this study is to compare the existing TCS for nanosatellites and adopt a suitable and efficient TCS for a scientific nanosatellite mission carrying a generic science instrument that needs an active cooling of up to 95K. TCS using Heat pipes (HP), single-phase mechanically pumped fluid loop (SMPFL), and two-phase mechanically pumped fluid loop systems (2ΦMPFL) have been extensively used only by larger satellites.
    [Show full text]
  • Report on the Radionet3 Networking Activity
    REPORT ON THE RADIONET3 NETWORKING ACTIVITY TITLE: LOFAR SCIENCE WEEK 2014 A JOINT MEETING COMBINING THE “2014 LOFAR COMMUNITY SCIENCE WORKSHOP” AND A SEPARATE, RELATED SYMPOSIUM ON “FIRST SCIENCE WITH LOFAR’S FIRST ALL-SKY SURVEY” DATE: 7 APRIL – 11 APRIL 2014 TIME: ALL DAY LOCATION: AMSTERDAM, THE NETHERLANDS MEETING WEBPAGE http://www.astron.nl/lofarscience2014/ HOST INSTITUTE: ASTRON (NETHERLANDS INSTITUTE FOR RADIO ASTRONOMY) PARTICIPANTS NO: 105 (COMMUNITY WORKSHOP) / 62 (SURVEY WORKSHOP) MAIN LEADER: ASTRON Project supported by the European Commission Contract no.: 283393 REPORT: 1. Agenda of the meeting The final programmes for both of the workshops are reproduced in their entirety in Appendix A. The programs and presentations are also available from the conference website. 2. Scientific Summary The LOFAR Science Week for 2014 was held April 7-11, 2014 in Amsterdam, NL and brought together roughly 120 members of the LOFAR science community. The week began on Monday afternoon with a LOFAR Users Meeting, open to the whole LOFAR community, organized by ASTRON and intended to provide a forum for users to both learn about the status of the array as well as provide feedback. Members of ASTRON gave updates on the current operational status, ongoing developments, and plans for the coming year. Representative users from the community were also invited to share their personal experiences from using the system. Robert Pizzo and the Science Support team were on hand to answer questions and gathered a lot of good feedback that they will use to improve the user experience for LOFAR. The User’s Meeting was followed on Tuesday by a two day LOFAR Community Science Workshop where nearly 120 members of the LOFAR collaboration came together to present their latest science results and share ideas and experiences about doing science with LOFAR.
    [Show full text]
  • You Every Step of The
    with you Every Step of the Way 2016 ANNUAL REPORT $3.5M From the President TOTAL I am pleased to report that your Alumni Association is stronger and more focused than ever! As a result, we have had a greater impact on the Academy experience SUPPORT for our cadets, supporting their academic, athletic and leadership needs — every step of the way — throughout the entire Academy. TO CGA In the following pages, you will read the stories of five cadets whose lives have IN 2016 been touched by your generosity. Their stories are reflective of the impact of your support on all aspects of cadet life. From providing access to the best coaches, equipment and off-campus competitions that unite our cadets as teams and leaders, to investments in educational programs that build confidence and hone the necessary skills of command — it’s clear in the stories and smiles within, that your Alumni Association continues to define the Long Blue Line. This year, we chose to convey our financial success through the voices of these young men and women, but from the Alumni Association board and staff, let me be the voice of gratitude. Because of the generosity of donors to the Alumni Association, in 2016 we surpassed all previous support to the Academy — providing more than $3.5 million in fulfillment of our mission and goals. Nearly 5,000 donors helped us reach this total, 38% of which were alumni donors. Additionally, 35% of the donations received were given in support to the CGA Today! Fund, our area of greatest need.
    [Show full text]
  • Planck 2011 Conference the Millimeter And
    PLANCK 2011 CONFERENCE THE MILLIMETER AND SUBMILLIMETER SKY IN THE PLANCK MISSION ERA 10-14 January 2011 Paris, Cité des Sciences Monday, January 10th 2011 13:00 Registration 14:00 Claudie Haigneré (Présidente of Universcience) Welcome Planck mission status, Performances, Cross-calibration Jan Tauber (ESA) - Jean-Loup Puget (IAS Orsay) - Reno Mandolesi (INAF/IASF Bologna) Introduction Session chair: François Pajot 14:20 François Bouchet (Institut d'Astrophysique de Paris) 30+5' HFI data and performance (invited on Planck early paper) 14:55 Marco Bersanelli (University of Milano) 30+5' LFI data and performance (invited on Planck early paper) 15:30 Ranga Chary (IPAC Caltech) 30+5' Planck Early Release Compact Source Catalogue (invited on Planck early paper) 16:05 Coffee break 16:30 Goran Pilbratt (European Space Agency) 20+5' The Herschel observatory (invited) Radio sources 16:55 Bruce Partridge (Haverford College) 25+5' Overview (invited) 17:25 Luigi Tofolatti (Universidad de Oviedo) 20+5' Planck radio sources statistics (invited on Planck early paper) 17:50 Francisco Argueso (Universidad de Oviedo) 15+5' A Bayesian technique to detect point sources in CMB maps 18:10 Anna Scaife (Dublin Institute for Advanced Studies) 15+5' The 10C survey of Radio Sources - First Results 18:30 End of day 1 19:00 Welcome reception at the Conference Center Tuesday, January 11th 2011 Radio sources (continued) Session chair: Bruce Partridge 9:00 Anne Lahteenmaki (Aalto University Metsahovi Radio Observatory) 20+5' Planck observations of extragalactic radio
    [Show full text]
  • UC Irvine UC Irvine Previously Published Works
    UC Irvine UC Irvine Previously Published Works Title Astrophysics in 2006 Permalink https://escholarship.org/uc/item/5760h9v8 Journal Space Science Reviews, 132(1) ISSN 0038-6308 Authors Trimble, V Aschwanden, MJ Hansen, CJ Publication Date 2007-09-01 DOI 10.1007/s11214-007-9224-0 License https://creativecommons.org/licenses/by/4.0/ 4.0 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Space Sci Rev (2007) 132: 1–182 DOI 10.1007/s11214-007-9224-0 Astrophysics in 2006 Virginia Trimble · Markus J. Aschwanden · Carl J. Hansen Received: 11 May 2007 / Accepted: 24 May 2007 / Published online: 23 October 2007 © Springer Science+Business Media B.V. 2007 Abstract The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the Universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords Cosmology: general · Galaxies: general · ISM: general · Stars: general · Sun: general · Planets and satellites: general · Astrobiology · Star clusters · Binary stars · Clusters of galaxies · Gamma-ray bursts · Milky Way · Earth · Active galaxies · Supernovae 1 Introduction Astrophysics in 2006 modifies a long tradition by moving to a new journal, which you hold in your (real or virtual) hands. The fifteen previous articles in the series are referenced oc- casionally as Ap91 to Ap05 below and appeared in volumes 104–118 of Publications of V.
    [Show full text]
  • "Is There Life on Venus?" Pdf File
    Home / Space / Specials Is there life on Venus? We call them "Martians" because, in science fiction, Mars has always been the natural home of extraterrestrials. In fact, of all the planets in the solar system, Mars is the prime candidate to host life, after Earth, of course. Indeed, Mars is on the outer edge of the habitable zone, that area around the Sun that delimits the space where the temperature is low enough to ensure that the water remains in a liquid state. And where there's water, it is well known, there's probably life. Yet it's cold on Mars today, and so far, all the probes and rovers we have sent to the surface of the red planet have found no signs of life. Planet Venus At the opposite end of the habitable belt there is Venus, similar in size and "geological" characteristics to our planet – that is, like Earth, it is a rocky planet. However, unlike Earth, Venus is probably one of the most inhospitable places in the Solar System: the temperature on the ground is about 500°C, higher than that recorded on Mercury, the planet closest to the Sun, so the Sun is not directly responsible for that infernal climate. The blame lies with the very extreme greenhouse effect on Venus. We know that the greenhouse effect is due to the presence of gases that trap solar radiation and heat the atmosphere. The main greenhouse gases are carbon dioxide (CO2), methane, water vapour and nitrogen oxides. On Earth we are rightly concerned because the amount of carbon dioxide is increasing due to human activities and with the increase in CO2, temperatures are rising.
    [Show full text]
  • The Arches Cluster out to Its Tidal Radius: Dynamical Mass Segregation and the Effect of the Extinction Law on the Stellar Mass Function
    Astronomy & Astrophysics manuscript no. aa˙paper c ESO 2018 October 31, 2018 The Arches cluster out to its tidal radius: dynamical mass segregation and the effect of the extinction law on the stellar mass function. ? M. Habibi1;3 , A. Stolte1 , W. Brandner2 , B. Hußmann1 , K. Motohara4 1 Argelander Institut fur¨ Astronomie, Universitat¨ Bonn, Auf dem Hugel¨ 71, 53121 Bonn, Germany e-mail: [mhabibi;astolte;hussmann]@astro.uni-bonn.de 2 Max-Planck-Institut fur¨ Astronomie, Konigsstuhl¨ 17, 69117 Heidelberg, Germany e-mail: [email protected] 3 Member of the International Max Planck Research School (IMPRS) for Astronomy and Astrophysics at the Universities of Bonn and Cologne. 4 Institute of Astronomy, The University of Tokyo, Osawa 2-21-1, Mitaka, Tokyo 181-0015, Japan e-mail: [email protected] Received Oct 14, 2012; accepted May 13, 2013 ABSTRACT The Galactic center is the most active site of star formation in the Milky Way Galaxy, where particularly high-mass stars have formed very recently and are still forming today. However, since we are looking at the Galactic center through the Galactic disk, knowledge of extinction is crucial when studying this region. The Arches cluster is a young, massive starburst cluster near the Galactic center. We observed the Arches cluster out to its tidal radius using Ks-band imaging obtained with NAOS/CONICA at the VLT combined with Subaro/Cisco J-band data to gain a full understanding of the cluster mass distribution. We show that the determination of the mass of the most massive star in the Arches cluster, which had been used in previous studies to establish an upper mass limit for the star formation process in the Milky Way, strongly depends on the assumed slope of the extinction law.
    [Show full text]
  • Cubesat-Based Science Missions for Geospace and Atmospheric Research
    National Aeronautics and Space Administration NATIONAL SCIENCE FOUNDATION (NSF) CUBESAT-BASED SCIENCE MISSIONS FOR GEOSPACE AND ATMOSPHERIC RESEARCH annual report October 2013 www.nasa.gov www.nsf.gov LETTERS OF SUPPORT 3 CONTACTS 5 NSF PROGRAM OBJECTIVES 6 GSFC WFF OBJECTIVES 8 2013 AND PRIOR PROJECTS 11 Radio Aurora Explorer (RAX) 12 Project Description 12 Scientific Accomplishments 14 Technology 14 Education 14 Publications 15 Contents Colorado Student Space Weather Experiment (CSSWE) 17 Project Description 17 Scientific Accomplishments 17 Technology 18 Education 18 Publications 19 Data Archive 19 Dynamic Ionosphere CubeSat Experiment (DICE) 20 Project Description 20 Scientific Accomplishments 20 Technology 21 Education 22 Publications 23 Data Archive 24 Firefly and FireStation 26 Project Description 26 Scientific Accomplishments 26 Technology 27 Education 28 Student Profiles 30 Publications 31 Cubesat for Ions, Neutrals, Electrons and MAgnetic fields (CINEMA) 32 Project Description 32 Scientific Accomplishments 32 Technology 33 Education 33 Focused Investigations of Relativistic Electron Burst, Intensity, Range, and Dynamics (FIREBIRD) 34 Project Description 34 Scientific Accomplishments 34 Education 34 2014 PROJECTS 35 Oxygen Photometry of the Atmospheric Limb (OPAL) 36 Project Description 36 Planned Scientific Accomplishments 36 Planned Technology 36 Planned Education 37 (NSF) CUBESAT-BASED SCIENCE MISSIONS FOR GEOSPACE AND ATMOSPHERIC RESEARCH [ 1 QB50/QBUS 38 Project Description 38 Planned Scientific Accomplishments 38 Planned
    [Show full text]
  • Star Formation at the Galactic Center
    Star Formation at the Galactic Center Mark Morris UCLA Outline § The Arena – central molecular zone, & the twisted ring § General dearth of star formation, relative to amount of gas § Orbital infuence on star formation § Mode of star formation: Massive young clusters vs. isolated YSOs § Star formation in the Central parsec § Cyclical star formation in the central parsec ? § Magnetic felds – a pitch for HAWC+ The inner Central Molecular Zone Molinari et al. 2011 … Herschel/SPIRE 250 µm Martin et al. 2004 7 CMZ: ~3 x 10 M8, ±170 pc Warm, turbulent molecular gas" Having large-scale order." overhead view of the! Molinari et al. 2011 twisted ring" Simulation of gas ! distribution in the CMZ" (Sungsoo Kim + 2011)" Henshaw et al. 2016 Top: HNCO, extracted using SCOUSE* *SCOUSE: Semi-automated mul-COmponent Universal Spectral-line fing Engine H2 column density contours from Herschel observations Color-coded to show velocity dispersion. Possible models: Henshaw et al. 2016 (Batersby et al., in prep) Henshaw+16 u Gas distribution dominated by two roughly parallel extended features in longitude-velocity space. u Henshaw+16 à the bulk of molecular line emission associated with the 20 & 50 km/s clouds is just a small segment of one of the extended features, in agreement with the Kruijssen+15 orbit, which places the clouds at a Galactocentric radius of ∼60 pc. u But this in inconsistent with the evidence that Sgr A East is interacting with the 50 km/s cloud and that the 20 km/s cloud is feeding gas into the central parsecs. Star Formation in the CMZ ♦ It has been known for some time that the CMZ has a much higher ratio of dense gas mass to star-formation tracers than elsewhere in the Galaxy [Morris 1989, 1993, Lis & Carlstrom 1994, Yusef-Zadeh et al.
    [Show full text]
  • Arxiv:Astro-Ph/9906299V1 17 Jun 1999 Cec Nttt,Wihi Prtdb H Soito Funiversit NAS5-26555
    HST/NICMOS Observations of Massive Stellar Clusters Near the Galactic Center1 Donald F. Figer2,3, Sungsoo S. Kim2,4, Mark Morris2, Eugene Serabyn5, R. Michael Rich2, Ian S. McLean2 ABSTRACT We report Hubble Space Telescope (HST) Near-infrared Camera and Multi- object Spectrometer (NICMOS) observations of the Arches and Quintuplet clusters, two extraordinary young clusters near the Galactic Center. For the first time, we have identified main sequence stars in the Galactic Center with initial masses well below 10 M⊙. We present the first determination of the initial mass function (IMF) for any population in the Galactic Center, finding an IMF slope which is significantly more positive (Γ ≈ −0.65) than the average for young clusters elsewhere in the Galaxy (Γ ≈ −1.4). The apparent turnoffs in the color-magnitude diagrams suggest cluster ages which are consistent with the ages implied by the mixture of spectral types in the clusters; we find τage ∼ 2±1 Myr for the Arches cluster, and τage ∼ 4±1 Myr for the Quintuplet. We estimate total cluster masses by adding the masses of observed stars down to the 50% completeness limit, and then extrapolating down to a lower mass cutoff 4 of 1 M⊙. Using this method, we find ∼>10 M⊙ for the total mass of the Arches cluster. Such a determination for the Quintuplet cluster is complicated by the double-valued mass-magnitude relationship for clusters with ages ∼> 3 Myr. We arXiv:astro-ph/9906299v1 17 Jun 1999 find a lower limit of 6300 M⊙ for the total cluster mass, and suggest a best 1Based on observations with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc.
    [Show full text]
  • Probing Galaxy Halos Using Background Polarized Radio Sources
    Probing galaxy halos using background polarized radio sources Master’s thesis in Physics and Astronomy ANTON NILSSON Department of Earth and Space Sciences CHALMERS UNIVERSITY OF TECHNOLOGY Gothenburg, Sweden 2016 Probing galaxy halos using background polarized radio sources Anton Nilsson Department of Earth and Space Sciences Radio Astronomy and Astrophysics group Chalmers University of Technology Gothenburg, Sweden 2016 Probing galaxy halos using background polarized radio sources Anton Nilsson © Anton Nilsson, 2016. Supervisor: Cathy Horellou, Department of Earth and Space Sciences Examiner: Cathy Horellou, Department of Earth and Space Sciences Department of Earth and Space Sciences Radio Astronomy and Astrophysics group Chalmers University of Technology SE-412 96 Gothenburg Telephone +46 31 772 1000 Cover: Polarized emission of the radio source J133920+464115 at Faraday depth +20.75 rad m−2 in grayscale. The contours show the total intensity. Typeset in LATEX Printed by Chalmers Reproservice Gothenburg, Sweden 2016 iv Probing galaxy halos using background polarized radio sources Anton Nilsson Department of Earth and Space Sciences Chalmers University of Technology Abstract Linearly polarized radio emission from synchrotron sources undergoes Faraday ro- tation when passing through a magneto-ionized medium. This might be used to search for evidence of ionized halos around galaxies, using polarized radio sources as a probe. In this thesis I analyze the polarization properties of background radio sources from the Taylor et al. (2009) catalog based on observations with the Very Large Array, and correlate these to the angular separation between the radio sources and foreground galaxies. I find a decrease in the amount of polarized radio sources near the galaxies, interpreting this as radio sources being depolarized by galaxy halos.
    [Show full text]
  • OTFM for Fast Mapping & Rapid Data Products
    OTFM for fast mapping & rapid data products Steven T. Myers (NRAO) for the VLASS team 1 B&E Caltech July 2016 The VLA Sky Survey (VLASS) On-the-fly Mosaicking (OTFM) for efficient fast mapping of the sky and pipelines for rapid genera=on of Data Products … wherein we elucidate the sundry benefits of using the recently upgraded Karl G. Jansky Very Large Array to survey large areas of the sky to discover new transient phenomena and illuminate heretofore hidden explosions throughout the Universe, and to explore cosmic magnetism h0ps://science.nrao.edu/science/surveys/vlass 2 B&E Caltech July 2016 Why a new VLA Sky Survey? A New VLA deserves a New Sky Survey https://science.nrao.edu/science/surveys/vlass • Expanded (bandwidth, time resolution) capabilities of Jansky VLA • 20 years since previous pioneering VLA sky surveys – NVSS 45” 1.4GHz (84MHz) 450µJy/bm (2932hrs) 30Kdeg2 2Msrcs – FIRST 5” 1.4GHz (84MHz) 150µJy/bm (3200hrs) 10.6Kdeg2 95Ksrcs • Preparing the way for a new generation of surveys – ASKAP and MeerKAT – SKA phase 1 – new O/IR surveys (i/zPTF, PanSTARRS,DES,LSST), X-ray (eROSITA) • Science Proposal and survey definition by community Survey Science Group (SSG) following AAS 223 workshop in Jan 2014 – community review and approval in March 2015 3 B&E Caltech July 2016 VLASS Survey Science Group A Survey For the Whole Community Proposal Authors: Table 8: VLASS Proposal Contributors, Including VLASS White Paper Authors F. Abdalla, Jose Afonso, A. Amara, David Bacon, Julie Banfield, Tim Bastian, Richard Battye, Stefi A. Baum, Tony Beasley, Rainer Beck, Robert Becker, Michael Bell, Edo Berger, Rob Beswick, Sanjay Bhat- nagar, Mark Birkinshaw, V.
    [Show full text]