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Multi-Generation Massive Star-Formation in NGC 3576
A&A 504, 139–159 (2009) Astronomy DOI: 10.1051/0004-6361/200811358 & c ESO 2009 Astrophysics Multi-generation massive star-formation in NGC 3576 C. R. Purcell1,2, V. Minier3,4, S. N. Longmore2,5,6, Ph. André3,4,A.J.Walsh2,7,P.Jones2,8,F.Herpin9,10, T. Hill2,11,12, M. R. Cunningham2, and M. G. Burton2 1 Jodrell Bank Centre for Astrophysics, Alan Turing Building, School of Physics and Astronomy, The University of Manchester, Oxford Road, Manchester M13 9PL, UK e-mail: [email protected] 2 School of Physics, University of New South Wales, Sydney, NSW 2052, Australia 3 CEA, DSM, IRFU, Service d’Astrophysique, 91191 Gif-sur-Yvette, France 4 Laboratoire AIM, CEA/DSM - CNRS - Université Paris Diderot, IRFU/Service d’Astrophysique, CEA-Saclay, 91191 Gif-sur-Yvette, France 5 Harvard-Smithsonian Centre For Astrophysics, 60 Garden Street, Cambridge, MA, 02138, USA 6 CSIRO Australia Telescope National Facillity, PO Box 76, Epping, NSW 1710, Australia 7 Centre for Astronomy, James Cook University, Townsville, QLD 4811, Australia 8 Departmento de Astronoma, Universidad de Chile, Casilla 36-D, Santiago, Chile 9 Université de Bordeaux, Laboratoire d’Astrophysique de Bordeaux, 33000 Bordeaux, France 10 CNRS/INSU, UMR 5804, BP 89, 33271 Floirac Cedex, France 11 School of Physics, University of Exeter, Stocker Road, EX4 4QL, Exeter, UK 12 Leiden Observatory, Leiden University, PO BOX 9513, 2300 RA Leiden, the Netherlands Received 16 November 2008 / Accepted 3 July 2009 ABSTRACT Context. Recent 1.2-mm continuum observations have shown the giant H II region NGC 3576 to be embedded in the centre of an extended filamentary dust-cloud. -
Correction: Corrigendum: the Superluminous Transient ASASSN
LETTERS PUBLISHED: 12 DECEMBER 2016 | VOLUME: 1 | ARTICLE NUMBER: 0002 The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole G. Leloudas1,2*, M. Fraser3, N. C. Stone4, S. van Velzen5, P. G. Jonker6,7, I. Arcavi8,9, C. Fremling10, J. R. Maund11, S. J. Smartt12, T. Krühler13, J. C. A. Miller-Jones14, P. M. Vreeswijk1, A. Gal-Yam1, P. A. Mazzali15,16, A. De Cia17, D. A. Howell8,18, C. Inserra12, F. Patat17, A. de Ugarte Postigo2,19, O. Yaron1, C. Ashall15, I. Bar1, H. Campbell3,20, T.-W. Chen13, M. Childress21, N. Elias-Rosa22, J. Harmanen23, G. Hosseinzadeh8,18, J. Johansson1, T. Kangas23, E. Kankare12, S. Kim24, H. Kuncarayakti25,26, J. Lyman27, M. R. Magee12, K. Maguire12, D. Malesani2, S. Mattila3,23,28, C. V. McCully8,18, M. Nicholl29, S. Prentice15, C. Romero-Cañizales24,25, S. Schulze24,25, K. W. Smith12, J. Sollerman10, M. Sullivan21, B. E. Tucker30,31, S. Valenti32, J. C. Wheeler33 and D. R. Young12 8 12,13 When a star passes within the tidal radius of a supermassive has a mass >10 M⊙ , a star with the same mass as the Sun black hole, it will be torn apart1. For a star with the mass of the could be disrupted outside the event horizon if the black hole 8 14 Sun (M⊙) and a non-spinning black hole with a mass <10 M⊙, were spinning rapidly . The rapid spin and high black hole the tidal radius lies outside the black hole event horizon2 and mass can explain the high luminosity of this event. -
Report from the Dark Energy Task Force (DETF)
Fermi National Accelerator Laboratory Fermilab Particle Astrophysics Center P.O.Box 500 - MS209 Batavia, Il l i noi s • 60510 June 6, 2006 Dr. Garth Illingworth Chair, Astronomy and Astrophysics Advisory Committee Dr. Mel Shochet Chair, High Energy Physics Advisory Panel Dear Garth, Dear Mel, I am pleased to transmit to you the report of the Dark Energy Task Force. The report is a comprehensive study of the dark energy issue, perhaps the most compelling of all outstanding problems in physical science. In the Report, we outline the crucial need for a vigorous program to explore dark energy as fully as possible since it challenges our understanding of fundamental physical laws and the nature of the cosmos. We recommend that program elements include 1. Prompt critical evaluation of the benefits, costs, and risks of proposed long-term projects. 2. Commitment to a program combining observational techniques from one or more of these projects that will lead to a dramatic improvement in our understanding of dark energy. (A quantitative measure for that improvement is presented in the report.) 3. Immediately expanded support for long-term projects judged to be the most promising components of the long-term program. 4. Expanded support for ancillary measurements required for the long-term program and for projects that will improve our understanding and reduction of the dominant systematic measurement errors. 5. An immediate start for nearer term projects designed to advance our knowledge of dark energy and to develop the observational and analytical techniques that will be needed for the long-term program. Sincerely yours, on behalf of the Dark Energy Task Force, Edward Kolb Director, Particle Astrophysics Center Fermi National Accelerator Laboratory Professor of Astronomy and Astrophysics The University of Chicago REPORT OF THE DARK ENERGY TASK FORCE Dark energy appears to be the dominant component of the physical Universe, yet there is no persuasive theoretical explanation for its existence or magnitude. -
Opening PANDORA's Box: APEX Observations of CO In
Astronomy & Astrophysics manuscript no. APEX_CO_ArXiv c ESO 2018 November 8, 2018 Opening PANDORA’s box: APEX observations of CO in PNe L. Guzman-Ramirez1; 2, A. I. Gómez-Ruíz3, H. M. J. Boffin4, D. Jones5; 6, R. Wesson7, A. A. Zijlstra8; 9, C. L. Smith10, and Lars-Ake˚ Nyman2; 10 1 Leiden Observatory, Leiden University, Niels Bohrweg 2, 2333 CA Leiden, The Netherlands e-mail: [email protected] 2 European Southern Observatory, Alonso de Córdova 3107, Santiago, Chile 3 CONACYT Instituto Nacional de Astrofísica, Óptica y Electrónica, Luis E. Erro 1, 72840 Tonantzintla, Puebla, México 4 European Southern Observatory, Karl-Schwarzschild-str. 2, D-85748 Garching, Germany 5 Instituto de Astrofísica de Canarias, E-38205 La Laguna, Tenerife, Spain 6 Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain 7 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 8 Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester, UK 9 Department of Physics & Laboratory for Space Research, University of Hong Kong, Pok Fu Lam Road, Hong Kong 10 Centre for Research in Earth and Space Sciences, York University, 4700 Keele Street, Toronto, ON, M3J 1P3, Canada 11 Joint ALMA Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile Received xx, 2018; accepted xx, 2018 ABSTRACT Context. Observations of molecular gas have played a key role in developing the current understanding of the late stages of stellar evolution. Aims. The survey Planetary nebulae AND their cO Reservoir with APEX (PANDORA) was designed to study the circumstellar shells of evolved stars with the aim to estimate their physical parameters. -
Perrett RTA.Pdf
The Astronomical Journal, 140:518–532, 2010 August doi:10.1088/0004-6256/140/2/518 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. REAL-TIME ANALYSIS AND SELECTION BIASES IN THE SUPERNOVA LEGACY SURVEY∗ K. Perrett1,2, D. Balam3, M. Sullivan4, C. Pritchet5, A. Conley1,6, R. Carlberg1,P.Astier7, C. Balland7,S.Basa8, D. Fouchez9,J.Guy7, D. Hardin7,I.M.Hook3,10, D. A. Howell11,12,R.Pain7, and N. Regnault7 1 Department of Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, ON, M5S 3H4, Canada; [email protected] 2 Network Information Operations, DRDC Ottawa, 3701 Carling Avenue, Ottawa, ON K1A 0Z4, Canada 3 Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada 4 Department of Physics (Astrophysics), University of Oxford, DWB, Keble Road, Oxford OX1 3RH, UK; [email protected] 5 Department of Physics & Astronomy, University of Victoria, P.O. Box 3055, Stn CSC, Victoria, BC V8W 3P6, Canada 6 Center for Astrophysics and Space Astronomy, University of Colorado, 593 UCB, Boulder, CO 80309-0593, USA 7 LPNHE, CNRS-IN2P3 and University of Paris VI & VII, 75005 Paris, France 8 Laboratoire d’Astrophysique de Marseille, Poledel’ˆ Etoile´ Site de Chateau-Gombert,ˆ 38, rue Fred´ eric´ Joliot-Curie, 13388 Marseille cedex 13, France 9 CPPM, CNRS-IN2P3 and University Aix Marseille II, Case 907, 13288 Marseille cedex 9, France 10 INAF, Osservatorio Astronomico di Roma, via Frascati 33, 00040 Monteporzio (RM), Italy 11 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr., Suite 102, Goleta, CA 93117, USA 12 Department of Physics, University of California, Santa Barbara, Broida Hall, Mail Code 9530, Santa Barbara, CA 93106-9530, USA Received 2010 February 17; accepted 2010 June 4; published 2010 July 1 ABSTRACT The Supernova Legacy Survey (SNLS) has produced a high-quality, homogeneous sample of Type Ia supernovae (SNe Ia) out to redshifts greater than z = 1. -
Planetary Nebulae
Planetary Nebulae A planetary nebula is a kind of emission nebula consisting of an expanding, glowing shell of ionized gas ejected from old red giant stars late in their lives. The term "planetary nebula" is a misnomer that originated in the 1780s with astronomer William Herschel because when viewed through his telescope, these objects appeared to him to resemble the rounded shapes of planets. Herschel's name for these objects was popularly adopted and has not been changed. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion years. The mechanism for formation of most planetary nebulae is thought to be the following: at the end of the star's life, during the red giant phase, the outer layers of the star are expelled by strong stellar winds. Eventually, after most of the red giant's atmosphere is dissipated, the exposed hot, luminous core emits ultraviolet radiation to ionize the ejected outer layers of the star. Absorbed ultraviolet light energizes the shell of nebulous gas around the central star, appearing as a bright colored planetary nebula at several discrete visible wavelengths. Planetary nebulae may play a crucial role in the chemical evolution of the Milky Way, returning material to the interstellar medium from stars where elements, the products of nucleosynthesis (such as carbon, nitrogen, oxygen and neon), have been created. Planetary nebulae are also observed in more distant galaxies, yielding useful information about their chemical abundances. In recent years, Hubble Space Telescope images have revealed many planetary nebulae to have extremely complex and varied morphologies. -
Publications RENOIR – 24 Sep 2021 Article
Publications RENOIR { 24 Sep 2021 article 2021 1. The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: one thousand multi-tracer mock catalogues with redshift evolution and systematics for galaxies and quasars of the final data release, C. Zhao et al., Mon. Not. Roy. Astron. Soc 503 (2021) 1149-1173 2. Euclid preparation: XI. Mean redshift determination from galaxy redshift probabilities for cosmic shear tomography, O. Ilbert et al., Euclid Collaboration, Astron. Astrophys. 647 (2021) A117 2020 1. Improving baryon acoustic oscillation measurement with the combination of cosmic voids and galaxies, C. Zhao et al., SDSS Collaboration, Mon. Not. Roy. Astron. Soc 491 (2020) 4554-4572 2. Strong Dependence of Type Ia Supernova Standardization on the Local Specific Star Formation Rate, M. Rigault et al., Nearby Supernova Factory Collaboration, Astron. Astrophys. 644 (2020) A176 3. High-precision Monte-Carlo modelling of galaxy distribution, P. Baratta et al., Astron. Astrophys. 633 (2020) A26 4. Constraints on the growth of structure around cosmic voids in eBOSS DR14, A. J. Hawken et al., J. Cosmol. Astropart. P 2006 (2020) 012 5. SUGAR: An improved empirical model of Type Ia Supernovae based on spectral features, P.-F. L´eget et al., Nearby Supernova Factory Collaboration, Astron. Astrophys. 636 (2020) A46 6. Euclid: Reconstruction of Weak Lensing mass maps for non- Gaussianity studies, S. Pires et al., Euclid Collaboration, Astron. Astrophys. 638 (2020) A141 7. Euclid preparation: VII. Forecast validation for Euclid cosmological probes, A. Blanchard et al., Euclid Collaboration, Astron. Astrophys. 642 (2020) A191 8. Euclid preparation: VI. Verifying the Performance of Cosmic Shear Experiments, P. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Planetary Nebulae
Southern Planetaries 6/27/04 9:20 PM Observatory Tents Nebula Filters by Andover Ngc 60 Meade NGC60 Premier online astronomy For viewing emission and Find, compare and buy Refractor Telescope $181 shop has a selection of planetary nebulae. Telescopes! Simply Fast Free Shipping. Affiliate. observatory dome tents Narrowband and O-III types Savings www.amazon.com www.telescopes.net www.andcorp.com www.Shopping.com Observing Down Under: Part II - Planetary Nebulae by Steve Gottlieb Shapley 1 - AAO This is the second part in a series based on my trip to Australia last summer, covering observations of a few southern showpiece objects. The other parts in the series are: Southern Globular Clusters Southern Galaxies Two Southern Galaxy Groups During the stay at the Magellan Observatory I had full access to an 18" f/4.5 JMI NGT-18, an innovative split-ring truss- tube equatorial with a rotating upper cage assembly. The scope was housed in a 4.5 meter dome (which came in very handy on windy nights) and outfitted with DSC's and it could be converted to use with a bino-viewer. Because I was trying to survey the full gamut of DSO's mostly below -50° (I easily could have spent the entire time just on the Large Magellanic Cloud!), I generally stuck to eye-candy -- and there was plenty to feast on! - and was really loafing it with an 18" on these brighter planetaries (everything below was immediately visible once in the field). Some of these were reobservations for me but from northern California I never had a really good look. -
Euclid: Superluminous Supernovae in the Deep Survey? C
A&A 609, A83 (2018) Astronomy DOI: 10.1051/0004-6361/201731758 & c ESO 2018 Astrophysics Euclid: Superluminous supernovae in the Deep Survey? C. Inserra1; 2, R. C. Nichol3, D. Scovacricchi3, J. Amiaux4, M. Brescia5, C. Burigana6; 7; 8, E. Cappellaro9, C. S. Carvalho30, S. Cavuoti5; 11; 12, V. Conforti13, J.-C. Cuillandre4; 14; 15, A. da Silva10; 16, A. De Rosa13, M. Della Valle5; 17, J. Dinis10; 16, E. Franceschi13, I. Hook18, P. Hudelot19, K. Jahnke20, T. Kitching21, H. Kurki-Suonio22, I. Lloro23, G. Longo11; 12, E. Maiorano13, M. Maris24, J. D. Rhodes25, R. Scaramella26, S. J. Smartt2, M. Sullivan1, C. Tao27; 28, R. Toledo-Moreo29, I. Tereno16; 30, M. Trifoglio13, and L. Valenziano13 (Affiliations can be found after the references) Received 11 August 2017 / Accepted 3 October 2017 ABSTRACT Context. In the last decade, astronomers have found a new type of supernova called superluminous supernovae (SLSNe) due to their high peak luminosity and long light-curves. These hydrogen-free explosions (SLSNe-I) can be seen to z ∼ 4 and therefore, offer the possibility of probing the distant Universe. Aims. We aim to investigate the possibility of detecting SLSNe-I using ESA’s Euclid satellite, scheduled for launch in 2020. In particular, we study the Euclid Deep Survey (EDS) which will provide a unique combination of area, depth and cadence over the mission. Methods. We estimated the redshift distribution of Euclid SLSNe-I using the latest information on their rates and spectral energy distribution, as well as known Euclid instrument and survey parameters, including the cadence and depth of the EDS. -
An X-Ray Tour of Massive Star-Forming Regions with Chandra
An X-ray Tour of Massive Star-forming Regions with Chandra By LEISA K. TOWNSLEY1 1 Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802, USA The Chandra X-ray Observatory is providing fascinating new views of massive star-forming re- gions, revealing all stages in the life cycles of massive stars and their effects on their surroundings. I present a Chandra tour of some of the most famous of these regions: M17, NGC 3576, W3, Tr14 in Carina, and 30 Doradus. Chandra highlights the physical processes that characterize the lives of these clusters, from the ionizing sources of ultracompact HII regions (W3) to superbubbles so large that they shape our views of galaxies (30 Dor). X-ray observations usually reveal hundreds of pre-main sequence (lower-mass) stars accompanying the OB stars that power these great HII region complexes, although in one case (W3 North) this population is mysteriously absent. The most massive stars themselves are often anomalously hard X-ray emitters; this may be a new indicator of close binarity. These complexes are sometimes suffused by soft diffuse X-rays (M17, NGC 3576), signatures of multi-million-degree plasmas created by fast O-star winds. In older regions we see the X-ray remains of the deaths of massive stars that stayed close to their birthplaces (Tr14, 30 Dor), exploding as cavity supernovae within the superbubbles that these clusters created. 1. Revealing the Life Cycle of a Massive Stellar Cluster High-resolution X-ray images from the Chandra X-ray Observatory and XMM-Newton elucidate all stages in the life cycles of massive stars – from ultracompact HII (UCHII) regions to supernova remnants – and the effects that those massive stars have on their surroundings. -
International Astronomical Union Commission 42 BIBLIOGRAPHY of CLOSE BINARIES No. 93
International Astronomical Union Commission 42 BIBLIOGRAPHY OF CLOSE BINARIES No. 93 Editor-in-Chief: C.D. Scarfe Editors: H. Drechsel D.R. Faulkner E. Kilpio E. Lapasset Y. Nakamura P.G. Niarchos R.G. Samec E. Tamajo W. Van Hamme M. Wolf Material published by September 15, 2011 BCB issues are available via URL: http://www.konkoly.hu/IAUC42/bcb.html, http://www.sternwarte.uni-erlangen.de/pub/bcb or http://www.astro.uvic.ca/∼robb/bcb/comm42bcb.html The bibliographical entries for Individual Stars and Collections of Data, as well as a few General entries, are categorized according to the following coding scheme. Data from archives or databases, or previously published, are identified with an asterisk. The observation codes in the first four groups may be followed by one of the following wavelength codes. g. γ-ray. i. infrared. m. microwave. o. optical r. radio u. ultraviolet x. x-ray 1. Photometric data a. CCD b. Photoelectric c. Photographic d. Visual 2. Spectroscopic data a. Radial velocities b. Spectral classification c. Line identification d. Spectrophotometry 3. Polarimetry a. Broad-band b. Spectropolarimetry 4. Astrometry a. Positions and proper motions b. Relative positions only c. Interferometry 5. Derived results a. Times of minima b. New or improved ephemeris, period variations c. Parameters derivable from light curves d. Elements derivable from velocity curves e. Absolute dimensions, masses f. Apsidal motion and structure constants g. Physical properties of stellar atmospheres h. Chemical abundances i. Accretion disks and accretion phenomena j. Mass loss and mass exchange k. Rotational velocities 6. Catalogues, discoveries, charts a.