They Produced the Nearest Supernova in 300 Years, Are Connected by a Giant Stream of Matter, and May Collide with the Milky Way
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The Parkes H I Survey of the Magellanic System
A&A 432, 45–67 (2005) Astronomy DOI: 10.1051/0004-6361:20040321 & c ESO 2005 Astrophysics The Parkes H I Survey of the Magellanic System C. Brüns1,J.Kerp1, L. Staveley-Smith2, U. Mebold1,M.E.Putman3,R.F.Haynes2, P. M. W. Kalberla1,E.Muller4, and M. D. Filipovic2,5 1 Radioastronomisches Institut, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany e-mail: [email protected] 2 Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710, Australia 3 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA 4 Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA 5 University of Western Sydney, Locked Bag 1797, Penrith South, DC, NSW 1797, Australia Received 24 February 2004 / Accepted 27 October 2004 Abstract. We present the first fully and uniformly sampled, spatially complete H survey of the entire Magellanic System with high velocity resolution (∆v = 1.0kms−1), performed with the Parkes Telescope. Approximately 24 percent of the southern skywascoveredbythissurveyona≈5 grid with an angular resolution of HPBW = 14.1. A fully automated data-reduction scheme was developed for this survey to handle the large number of H spectra (1.5 × 106). The individual Hanning smoothed and polarization averaged spectra have an rms brightness temperature noise of σ = 0.12 K. The final data-cubes have an rms noise of σrms ≈ 0.05 K and an effective angular resolution of ≈16 . In this paper we describe the survey parameters, the data- reduction and the general distribution of the H gas. The Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) are associated with huge gaseous features – the = Magellanic Bridge, the Interface Region, the Magellanic Stream, and the Leading Arm – with a total H mass of M(H ) 8 2 4.87 × 10 M d/55 kpc ,ifallH gas is at the same distance of 55 kpc. -
Fixed Stars More Than the Wandering Planets Used by Modern Astrologers
Ancients used the fixed stars more than the wandering planets used by modern astrologers. With improved technical abilities due to software enhancements, the fixed stars are beginning to make a return in present day astrology. The information contained in these pages is just a sampling of the stars and their meanings. It is designed to encourage you to look at the subject in a deeper level. When you blend the meaning of the fixed stars with the natal planets in your chart, it adds a great deal of texture to the understanding of your planet/star combination. I normally use a three degree orb of influence between stars and planets, but the commonly accepted orb is only one degree. A research project I did several years ago indicated that people felt the effects of the stars from this wider distance (which can amount to millions of miles). For example, if the planet Mercury in your natal chart is at 17° Gemini, then you will find on page four that item T is the star Rigel in the Orion constellation. Stars that are in the feet of a constellation are considered to be teacher stars in that they bring higher information down to earth to be used. Mercury represents communications, education, writing, and short trips. Combined, this could be a teacher of higher information, possibly a person who travels or writes as part of the teaching process. Again, this is a partial list of stars. Listed below are some of the books and references I have used. REFERENCE: The interpretations come from Bernadette Brady’s “Book of Fixed Stars”, the Solar Maps software program http://www.bernadettebrady.com/; , Ebertin-Hoffman’s book Fixed Stars,” Vivian Robson’s “The Fixed Stars & Constellations in Astrology” and miscellaneous sources. -
VMC – the VISTA Survey of the Magellanic System Metallicity Of
Dr Maria‐Rosa Cioni VMC – the VISTA survey of the Magellanic System (Gal-Exgal survey) Metallicity of stellar populaons Moon of stellar populaons ESO spectroscopic survey workshop ESO-Garching, Germany, 9-10 March 2009 The VISTA survey of the Magellanic System ESO Public Survey 2009-2014 The most sensive near‐IR survey across the LMC, SMC, The team Bridge and part of the Stream M. Cioni, K. Bekki, G. Clemenni, W. de Blok, J. Emerson, C. Evans, R. de Grijs, B. Gibson, L. Girardi, M. Groenewegen, 4m Telescope V. Ivanov, M. Marconi, C. Mastropietro, B. Moore, R. Napiwotzki, T. Naylor, J. Oliveira, V. Ripepi, J. van Loon, M. Wilkinson, P. Wood 1.5 deg2 FOV United Kingdom, Italy, Belgium, Chile, France, Switzerland, South Africa, Australia http://star.herts.ac.uk/~mcioni/vmc/ 0. Observe the Magellanic System 2 ≈180 deg 3 filters ‐ YJKs 15 epochs (12 in KS and 3 in YJ; once simultaneous colours) S/N=10 at: Y=21.9, J=21.4, Ks=20.3 (Ks≈19 single epoch) Seeing 0.8 arcsec – average Spaal resoluon 0.34 pix/arcsec (0.51 arcsec instrument PSF) Service mode observing 1840 hours / 240 nights http://star.herts.ac.uk/~mcioni/vmc/ I. Derive the spaally resolved SFH Synthec diagram of a typical LMC stellar field as expected from VMC data. This field covers 1 VISTA detector! Accuracy: metallicity S/N=10 0.1 dex and age 20% in 0.1 deg2 Kerber et al 2009 http://star.herts.ac.uk/~mcioni/vmc/ II. Trace the 3D structure as a funcon of me The LMC is a few kpc thick and the SMC up to 20 kpc RR Lyrae stars are excellent distance indicators in the near‐IR First applicaon to the LMC bar to derive the LMC distance (Szewczyk et al 2008) – 0.2 kpc accuracy The structure of the Magellanic System will be measured using Cepheid variables, the red clump luminosity, the p of the red giant brach, etc. -
Constructing a Galactic Coordinate System Based on Near-Infrared and Radio Catalogs
A&A 536, A102 (2011) Astronomy DOI: 10.1051/0004-6361/201116947 & c ESO 2011 Astrophysics Constructing a Galactic coordinate system based on near-infrared and radio catalogs J.-C. Liu1,2,Z.Zhu1,2, and B. Hu3,4 1 Department of astronomy, Nanjing University, Nanjing 210093, PR China e-mail: [jcliu;zhuzi]@nju.edu.cn 2 key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, PR China 3 Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China 4 Graduate School of Chinese Academy of Sciences, Beijing 100049, PR China e-mail: [email protected] Received 24 March 2011 / Accepted 13 October 2011 ABSTRACT Context. The definition of the Galactic coordinate system was announced by the IAU Sub-Commission 33b on behalf of the IAU in 1958. An unrigorous transformation was adopted by the Hipparcos group to transform the Galactic coordinate system from the FK4-based B1950.0 system to the FK5-based J2000.0 system or to the International Celestial Reference System (ICRS). For more than 50 years, the definition of the Galactic coordinate system has remained unchanged from this IAU1958 version. On the basis of deep and all-sky catalogs, the position of the Galactic plane can be revised and updated definitions of the Galactic coordinate systems can be proposed. Aims. We re-determine the position of the Galactic plane based on modern large catalogs, such as the Two-Micron All-Sky Survey (2MASS) and the SPECFIND v2.0. This paper also aims to propose a possible definition of the optimal Galactic coordinate system by adopting the ICRS position of the Sgr A* at the Galactic center. -
The Dunhuang Chinese Sky: a Comprehensive Study of the Oldest Known Star Atlas
25/02/09JAHH/v4 1 THE DUNHUANG CHINESE SKY: A COMPREHENSIVE STUDY OF THE OLDEST KNOWN STAR ATLAS JEAN-MARC BONNET-BIDAUD Commissariat à l’Energie Atomique ,Centre de Saclay, F-91191 Gif-sur-Yvette, France E-mail: [email protected] FRANÇOISE PRADERIE Observatoire de Paris, 61 Avenue de l’Observatoire, F- 75014 Paris, France E-mail: [email protected] and SUSAN WHITFIELD The British Library, 96 Euston Road, London NW1 2DB, UK E-mail: [email protected] Abstract: This paper presents an analysis of the star atlas included in the medieval Chinese manuscript (Or.8210/S.3326), discovered in 1907 by the archaeologist Aurel Stein at the Silk Road town of Dunhuang and now held in the British Library. Although partially studied by a few Chinese scholars, it has never been fully displayed and discussed in the Western world. This set of sky maps (12 hour angle maps in quasi-cylindrical projection and a circumpolar map in azimuthal projection), displaying the full sky visible from the Northern hemisphere, is up to now the oldest complete preserved star atlas from any civilisation. It is also the first known pictorial representation of the quasi-totality of the Chinese constellations. This paper describes the history of the physical object – a roll of thin paper drawn with ink. We analyse the stellar content of each map (1339 stars, 257 asterisms) and the texts associated with the maps. We establish the precision with which the maps are drawn (1.5 to 4° for the brightest stars) and examine the type of projections used. -
Hubble Space Telescope Observer’S Guide Winter 2021
HUBBLE SPACE TELESCOPE OBSERVER’S GUIDE WINTER 2021 In 2021, the Hubble Space Telescope will celebrate 31 years in operation as a powerful observatory probing the astrophysics of the cosmos from Solar system studies to the high-redshift universe. The high-resolution imaging capability of HST spanning the IR, optical, and UV, coupled with spectroscopic capability will remain invaluable through the middle of the upcoming decade. HST coupled with JWST will enable new innovative science and be will be key for multi-messenger investigations. Key Science Threads • Properties of the huge variety of exo-planetary systems: compositions and inventories, compositions and characteristics of their planets • Probing the stellar and galactic evolution across the universe: pushing closer to the beginning of galaxy formation and preparing for coordinated JWST observations • Exploring clues as to the nature of dark energy ACS SBC absolute re-calibration (Cycle 27) reveals 30% greater • Probing the effect of dark matter on the evolution sensitivity than previously understood. More information at of galaxies http://www.stsci.edu/contents/news/acs-stans/acs-stan- • Quantifying the types and astrophysics of black holes october-2019 of over 7 orders of magnitude in size WFC3 offers high resolution imaging in many bands ranging from • Tracing the distribution of chemicals of life in 2000 to 17000 Angstroms, as well as spectroscopic capability in the universe the near ultraviolet and infrared. Many different modes are available for high precision photometry, astrometry, spectroscopy, mapping • Investigating phenomena and possible sites for and more. robotic and human exploration within our Solar System COS COS2025 initiative retains full science capability of COS/FUV out to 2025 (http://www.stsci.edu/hst/cos/cos2025). -
Chapter 8.Pdf
CHAeTER 8 INFLUENCE OF PULSARS ON SUPERNOVAE In recent years there has been a great deal of effort to understand in detail the observed light curves of type I1 supernovae. In the standard approach, the observed light curve is to be understood in terms of an initial deposition of thermal energy by the blast wave; and a more gradual input of thermal energy due to radioactive decay of iron-peak elements is invoked to explain the behaviour at later times. The consensus is that the light curves produced by these models are in satisfactory agreement with those observed. In this chapter we discuss the characteristics of the expected light curve, if in addition to the abovementioned sources of energy, there is a continued energy input from an active central pulsar. We argue that in those rare cases when the energy loss rate of the pulsar is comparable to the luminosity of the supernova near light maximum, the light curve will be characterized by an extended plateau phase. The essential reason for this is that the pulsar luminosity is expected to decline over timescales which are much longer than the timescale of, say, radioactive decay. The light curve of the recent supernova in the Large Magellanic Cloud is suggestive of continued energy input from an active pulsar. A detection of strong W,X -ray and 1-ray plerion after the ejecta becomes optically thin will be a clear evidence of the pulsar having powered the light curve. CONTENTS CHAPTER 8 INFLUENCE OF PULSARS ON SUPERNOVAE 8.1 INTRODUCTION ................... 8-1 8.2 EARLIER WORK .................. -
HI in the M31/M33 Environment
HI in the M31/M33 Environment A thesis presented to the faculty of the College of Arts and Sciences of Ohio University In partial fulfillment of the requirements for the degree Master of Science Nicole L. Free November 2010 © 2010 Nicole L. Free. All Rights Reserved. 2 This thesis titled HI in the M31/M33 Environment by NICOLE L. FREE has been approved for the Department of Physics and Astronomy and the College of Arts and Sciences by Felix J. Lockman Adjunct Professor of Physics and Astronomy Joseph C. Shields Professor of Physics and Astronomy Benjamin M. Ogles Dean, College of Arts and Sciences 3 ABSTRACT FREE, NICOLE L., M.S., November 2010, Physics and Astronomy HI in the M31/M33 Environment (70 pp.) Director of Thesis: Felix J. Lockman and Joseph C. Shields With recent debate about a reported neutral hydrogen, HI, streamer between M33 and M31, we set out to determine the existence of the HI streamer. Using the National Radio Astronomy Observatory’s 100 m Green Bank Telescope, with 9.1´ angular resolution, we mapped the HI in the region from Wright’s Cloud and M33 through the location of the streamer features, as reported by Braun and Thilker (2004). To verify the findings of Braun and Thilker, we also performed pointed observations at two of the three local maxima within their maps. From our observations, we were able to confirm the existence of the three local maxima points. The three features have column densities ranging from 2.3 to 5.4 , with most being of the order of magnitude of the latter. -
The Distance to the Large Magellanic Cloud
Proceedings Astronomy from 4 perspectives 1. Cosmology The distance to the large magellanic cloud Stefan V¨olker (Jena) In the era of modern cosmology it is necessary to determine the Hubble constant as precise as possible. Therefore it is important to know the distance to the Large Mag- ellanic Cloud (LMC), because this distance forms the fundament of the cosmological distance ladder. The determination of the LMC's distance is an suitable project for highschool students and will be presented in what follows. Calculating the distance to the LMC using the supernova SN 1987 A [1, 2] By combining the angular size α of an object with its absolute size R, one can calculate the distance d (at least for our cosmological neighborhood) using the equation R R d = ≈ (1) tan α α and the approximation d R. In the case of the SN 1987 A students can measure the angular size of the circumstellar ring on the Hubble Space Telescope (HST) image (Figure 1). The absolute size of the ring can be derived from the delay time due to light-travel effects seen in the emission light curve (also Figure 1). Once the supernova exploded, the UV-flash started 1,00 0,75 0,50 intensity (normalized) 0,25 0 0 500 1000 time t/d ESA/Hubble tP1' tP2' Figure 1: left: HST picture of the SN 1987 A; right: emission light curve of the circumstellar [2, 3] propagating and reached the whole ring at the same time, which started emitting immediately. The additional distance x is linked to the delay time by the equation x = c · ∆t = c · (t 0 − t 0 ). -
ASKAP and Meerkat Surveys of the Magellanic Clouds
ASKAP and MeerKAT surveys of the Magellanic Clouds Jacco Th. van Loon Lennard-Jones Laboratories, Keele University, ST5 5BG, United Kingdom E-mail: [email protected] The GASKAP Team Hector Arce, Amanda Bailey, Indra Bains, Ayesha Begum, Kenji Bekki, Nadya Ben Bekhti, Joss Bland-Hawthorn, Kate Brooks, Chris Brunt, Michael Burton, James Caswell, Maria Cunningham, John Dickey, Kevin Douglas, Simon Ellingsen, Jayanne English, Robert Estalella, Alyson Ford, Tyler Foster, Bryan Gaensler, Jay Gallagher, Steven Gibson, José Girart, Paul Goldsmith, José F. Gómez, Yolanda Gómez, Anne Green, James Green, Matt Haffner, Carl Heiles, Fabian Heitsch, Patrick Hennebelle, Tomoya Hirota, Melvin Hoare, Hiroshi Imai, Hideyuki Izumiura, Gilles Joncas, Paul Jones, Peter Kalberla, Ji-hyun Kang, Akiko Kawamura, Jürgen Kerp, Charles Kerton, Bon-Chul Koo, Roland Kothes, Stan Kurtz, Maša Laki´cevi´c, Tom Landecker, Alex Lazarian, Nadia Lo, Felix Lockman, Loris Magnani, Naomi McClure-Griffiths, Karl Menten, Victor Migenes, Marc-Antoine Miville-Deschênes, Erik Muller, Akiharu Nakagawa, Hiroyuki Nakanishi, Jun-ichi Nakashima, David Nidever, Lou Nigra, Josh Peek, Miguel Pérez-Torres, Chris Phillips, Mary Putman, Anthony Remijan, Philipp Richter, Peter arXiv:1009.0717v1 [astro-ph.GA] 3 Sep 2010 Schilke, Yoshiaki Sofue, Snežana Stanimirovi´c, Daniel Tafoya, Russ Taylor, Wen-Wu Tian, Lucero Uscanga, Jacco van Loon, Maxim Voronkov, Bart Wakker, Andrew Walsh, Tobias Westmeier, Benjamin Winkel, Ellen Zweibel The MagiKAT Team Gemma Bagheri, Amanda Bailey, Sudhanshu Barway, -
Revealing the Ionization Properties of the Magellanic Stream Using Optical Emission
The Astrophysical Journal, 851:110 (26pp), 2017 December 20 https://doi.org/10.3847/1538-4357/aa992a © 2017. The American Astronomical Society. All rights reserved. Revealing the Ionization Properties of the Magellanic Stream Using Optical Emission K. A. Barger1,2 , G. J. Madsen3, A. J. Fox4 , B. P. Wakker5 , J. Bland-Hawthorn6 , D. Nidever7 , L. M. Haffner8,9 , Jacqueline Antwi-Danso1,10, Michael Hernandez1, N. Lehner2 , A. S. Hill11,12 , A. Curzons6, and T. Tepper-García6 1 Department of Physics and Astronomy, Texas Christian University, Fort Worth, TX 76129, USA 2 Department of Physics, University of Notre Dame, Notre Dame, IN 46556, USA 3 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 4 Space Telescope Science Institute, Baltimore, MD 21218, USA 5 Supported by NASA/NSF, affiliated with Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706, USA 6 Sydney Institute for Astronomy, School of Physics A28, University of Sydney, NSW 2006, Australia 7 National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ, 85719, USA 8 Department of Astronomy, University of Wisconsin-Madison, Madison, WI 53706, USA 9 Space Science Institute, Boulder, CO 80301, USA 10 Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA 11 Departments of Physics and Astronomy, Haverford College, Haverford, PA 19041, USA 12 CSIRO Astronomy and Space Science, Marsfield, NSW 1710, Australia Received 2017 May 1; revised 2017 November 6; accepted 2017 November 6; published 2017 December 18 Abstract The Magellanic Stream, a gaseous tail that trails behind the Magellanic Clouds, could replenish the Milky Way (MW) with a tremendous amount of gas if it reaches the Galactic disk before it evaporates into the halo. -
The Magellanic System's Interactive Formations
Publ. Astron. Soc. Aust., 2000, 17, 1–5. The Magellanic System’s Interactive Formations M. E. Putman Research School of Astronomy & Astrophysics, Australian National University, Private Bag, Weston Creek PO, ACT 2611, Australia [email protected] Received 1999 November 17, accepted 2000 January 7 Abstract: The interaction between the Galaxy and the Magellanic Clouds has resulted in several high-velocity complexes which are connected to the Clouds. The complexes are known as the Magellanic Bridge, an HI connection between the Large and Small Magellanic Clouds, the Magellanic Stream, a 10 100 HI lament which trails the Clouds, and the Leading Arm, a diuse HI lament which leads the Clouds. The mechanism responsible for these features formation remains under some debate, with the lack of detailed HI observations being one of the limiting factors in resolving the issue. Here I present several large mosaics of HI Parkes All-Sky Survey (HIPASS) data which show the full extent of the three Magellanic complexes at almost twice the resolution of previous observations. These interactive features are connected, but unique in their spatial and velocity distribution. The dierences may shed light on their origin and present environment. Dense clumps of HI along the sightline to the Sculptor Group, which may or may not be associated with the Magellanic complexes, are also discussed. Keywords: intergalactic medium — Local Group — Magellanic Clouds — galaxies: HI 1 Introduction this by providing a marked improvement in spatial Almost every galaxy in the Universe is either resolution compared to previous HVC surveys (see currently, or was at some time, part of an interacting Putman & Gibson 1999), and revealing previously system.