Annual Report 2007 ESO
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A Revised View of the Canis Major Stellar Overdensity with Decam And
MNRAS 501, 1690–1700 (2021) doi:10.1093/mnras/staa2655 Advance Access publication 2020 October 14 A revised view of the Canis Major stellar overdensity with DECam and Gaia: new evidence of a stellar warp of blue stars Downloaded from https://academic.oup.com/mnras/article/501/2/1690/5923573 by Consejo Superior de Investigaciones Cientificas (CSIC) user on 15 March 2021 Julio A. Carballo-Bello ,1‹ David Mart´ınez-Delgado,2 Jesus´ M. Corral-Santana ,3 Emilio J. Alfaro,2 Camila Navarrete,3,4 A. Katherina Vivas 5 and Marcio´ Catelan 4,6 1Instituto de Alta Investigacion,´ Universidad de Tarapaca,´ Casilla 7D, Arica, Chile 2Instituto de Astrof´ısica de Andaluc´ıa, CSIC, E-18080 Granada, Spain 3European Southern Observatory, Alonso de Cordova´ 3107, Casilla 19001, Santiago, Chile 4Millennium Institute of Astrophysics, Santiago, Chile 5Cerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena, Chile 6Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackenna 4860, 782-0436 Macul, Santiago, Chile Accepted 2020 August 27. Received 2020 July 16; in original form 2020 February 24 ABSTRACT We present the Dark Energy Camera (DECam) imaging combined with Gaia Data Release 2 (DR2) data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the colour–magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitudes, below the plane, and in the range 230◦ <<255◦. -
Dynamical Evolution of the Hungaria Asteroids ⇑ Firth M
Icarus 210 (2010) 644–654 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Dynamical evolution of the Hungaria asteroids ⇑ Firth M. McEachern, Matija C´ uk , Sarah T. Stewart Department of Earth and Planetary Sciences, Harvard University, 20 Oxford Street, Cambridge, MA 02138, USA article info abstract Article history: The Hungarias are a stable asteroid group orbiting between Mars and the main asteroid belt, with high Received 29 June 2009 inclinations (16–30°), low eccentricities (e < 0.18), and a narrow range of semi-major axes (1.78– Revised 2 August 2010 2.06 AU). In order to explore the significance of thermally-induced Yarkovsky drift on the population, Accepted 7 August 2010 we conducted three orbital simulations of a 1000-particle grid in Hungaria a–e–i space. The three simu- Available online 14 August 2010 lations included asteroid radii of 0.2, 1.0, and 5.0 km, respectively, with run times of 200 Myr. The results show that mean motion resonances—martian ones in particular—play a significant role in the destabili- Keywords: zation of asteroids in the region. We conclude that either the initial Hungaria population was enormous, Asteroids or, more likely, Hungarias must be replenished through collisional or dynamical means. To test the latter Asteroids, Dynamics Resonances, Orbital possibility, we conducted three more simulations of the same radii, this time in nearby Mars-crossing space. We find that certain Mars crossers can be trapped in martian resonances, and by a combination of chaotic diffusion and the Yarkovsky effect, can be stabilized by them. -
Arxiv:1601.00329V3 [Astro-Ph.CO] 19 Aug 2016 Early Data
DES 2015-0085 FERMILAB-PUB-16-003-AE Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed 22 August 2016 (MN LATEX style file v2.2) The Dark Energy Survey: more than dark energy - an overview Dark Energy Survey Collaboration: T. Abbott1, F. B. Abdalla2, J. Aleksic´47, S. Allam3, A. Amara4, D. Bacon6, E. Balbinot46, M. Banerji7;8, K. Bechtol56;57, A. Benoit-Levy´ 13;2;12, G. M. Bernstein10, E. Bertin12;13, J. Blazek14, C. Bonnett15, S. Bridle16, D. Brooks2, R. J. Brunner41;20, E. Buckley- Geer3, D. L. Burke11;17, G. B. Caminha51;52, D. Capozzi6, J. Carlsen6, A. Carnero-Rosell18;19, M. Carollo54, M. Carrasco-Kind20;21, J. Carretero9;47, F. J. Castander9, L. Clerkin2, T. Collett6, C. Conselice55, M. Crocce9, C. E. Cunha11, C. B. D’Andrea6, L. N. da Costa19;18, T. M. Davis49, S. Desai25;24, H. T. Diehl3, J. P. Dietrich25;24, S. Dodelson3;27;58, P. Doel2, A. Drlica-Wagner3, J. Estrada3, J. Etherington6, A. E. Evrard22;29, J. Fabbri2, D. A. Finley3, B. Flaugher3, R. J. Foley21;41, P. Fosalba9, J. Frieman27;3, J. Garc´ıa-Bellido43, E. Gaztanaga9, D. W. Gerdes22, T. Giannantonio8;7, D. A. Goldstein44;37, D. Gruen17;11, R. A. Gruendl20;21, P. Guarnieri6, G. Gutierrez3, W. Hartley4, K. Honscheid14;32, B. Jain10, D. J. James1, T. Jeltema53, S. Jouvel2, R. Kessler27;58, A. King49, D. Kirk2, R. Kron27, K. Kuehn33, N. Kuropatkin3, O. Lahav2;?, T. S. Li23, M. Lima19;35, H. Lin3, M. A. G. Maia19;18, M. Makler51, M. Manera2, C. Maraston6, J. L. -
FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
An Interferometric Study of the Post-AGB Binary 89 Herculis I
A&A 559, A111 (2013) Astronomy DOI: 10.1051/0004-6361/201321616 & c ESO 2013 Astrophysics An interferometric study of the post-AGB binary 89 Herculis I. Spatially resolving the continuum circumstellar environment at optical and near-IR wavelengths with the VLTI, NPOI, IOTA, PTI, and the CHARA Array,, M. Hillen1, T. Verhoelst1,2,H.VanWinckel1, O. Chesneau3,C.A.Hummel4, J. D. Monnier5, C. Farrington6, C. Tycner7, D. Mourard3, T. ten Brummelaar6,D.P.K.Banerjee8,andR.T.Zavala9 1 Instituut voor Sterrenkunde (IvS), KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium e-mail: [email protected] 2 Belgian Institute for Space Aeronomy, 1180 Brussels, Belgium 3 Laboratoire Lagrange, UMR7293, Univ. Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d’Azur, 06300 Nice, France 4 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 5 University of Michigan, 941 Dennison Building, 500 Church Street, Ann Arbor, MI 48109-1090, USA 6 The CHARA Array of Georgia State University, Mt. Wilson Observatory, Mt. Wilson, CA 91023, USA 7 Department of Physics, Central Michigan University, Mt. Pleasant, MI 48859, USA 8 Physical Research Laboratory, Navrangpura, 380009 Ahmedabad, India 9 US Naval Observatory, Flagstaff Station, 10391 W. Naval Obs. Rd., Flagstaff, AZ 86001, USA Received 1 April 2013 / Accepted 25 July 2013 ABSTRACT Context. Binary post-asymptotic giant branch (post-AGB) stars are interesting laboratories to study both the evolution of binaries as well as the structure of circumstellar disks. Aims. A multiwavelength high angular resolution study of the prototypical object 89 Herculis is performed with the aim of identifying and locating the different emission components seen in the spectral energy distribution. -
(3 I" Richard P. Binzel, 1 (.: , FINAL REPORT for NASA GRANT
f i I j .t t_ (3 i" _(.: _,_ Richard P. Binzel, 1 FINAL REPORT FOR NASA GRANT NAG5-3939 RECONNAISSANCE OF NEAR-EARTH OBJECTS Richard P. Binzel (MIT) Principal Investigator Summa_: NASA sponsorship of asteroid research for this grant has resulted in 31)publications and major new results relating near- Earth asteroids _o known meteorite groups, most especially ordina_ chondrites. Analysis of observations continues. Research Objectives What ar_ the relationships between asteroids, comets, and meteorites? All represent primordial sanples from the early solar system, but how have their thermal, collisional, and dynamical evolution differed over the age of the solar system? Achieving such a fundamental understanding of the interrelationships of solar system small bodies has been a cornerstone for work in planetary science over the past three decades and continues to be of highest priority Asteroids, comets, and meteorite source bodies all traverse near-Earth space and are therefore accessible to groundbased observations despite their typically small sizes. As has been demonstrated by rJearly three decades of work, spectroscopic observations represent the most fundamental technique for measuring the physical properties of small solar system bodies. Over visible wavelengths, near-Earth objects observed to date have been found to display a wide range of distinctive spectral properties which appear to span the range between primitive (perhaps cometary) compositions to highly differentiated materials (likely formed in the asteroid belt). In addition, many apparent comet->asteroid transition objects (e.g. 4015 Wilson-Harr_ngton) have been discovered and are in need of substantial follow- up physical study. Thus, the study (,f near-Earth objects is _ for achieving the fundamental science goals of understanding the relationships between asteroids, comets, and meteorites. -
Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties. -
Astronomy Binder
Astronomy Binder Bloomington High School South 2011 Contents 1 Astronomical Distances 2 1.1 Geometric Methods . 2 1.2 Spectroscopic Methods . 4 1.3 Standard Candle Methods . 4 1.4 Cosmological Redshift . 5 1.5 Distances to Galaxies . 5 2 Age and Size 6 2.1 Measuring Age . 6 2.2 Measuring Size . 7 3 Variable Stars 7 3.1 Pulsating Variable Stars . 7 3.1.1 Cepheid Variables . 7 3.1.2 RR Lyrae Variables . 8 3.1.3 RV Tauri Variables . 8 3.1.4 Long Period/Semiregular Variables . 8 3.2 Binary Variables . 8 3.3 Cataclysmic Variables . 11 3.3.1 Classical Nova . 11 3.3.2 Recurrent Novae . 11 3.3.3 Dwarf Novae (U Geminorum) . 11 3.3.4 X-Ray Binary . 11 3.3.5 Polar (AM Herculis) star . 12 3.3.6 Intermediate Polar (DQ Herculis) star . 12 3.3.7 Super Soft Source (SSS) . 12 3.3.8 VY Sculptoris stars . 12 3.3.9 AM Canum Venaticorum stars . 12 3.3.10 SW Sextantis stars . 13 3.3.11 Symbiotic Stars . 13 3.3.12 Pulsating White Dwarfs . 13 4 Galaxy Classification 14 4.1 Elliptical Galaxies . 14 4.2 Spirals . 15 4.3 Classification . 16 4.4 The Milky Way Galaxy (MWG . 19 4.4.1 Scale Height . 19 4.4.2 Magellanic Clouds . 20 5 Galaxy Interactions 20 6 Interstellar Medium 21 7 Active Galactic Nuclei 22 7.1 AGN Equations . 23 1 8 Spectra 25 8.1 21 cm line . 26 9 Black Holes 26 9.1 Stellar Black Holes . -
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). -
Effemeridi Astronomiche Di Milano Per L'anno
Informazioni su questo libro Si tratta della copia digitale di un libro che per generazioni è stato conservata negli scaffali di una biblioteca prima di essere digitalizzato da Google nell’ambito del progetto volto a rendere disponibili online i libri di tutto il mondo. Ha sopravvissuto abbastanza per non essere più protetto dai diritti di copyright e diventare di pubblico dominio. Un libro di pubblico dominio è un libro che non è mai stato protetto dal copyright o i cui termini legali di copyright sono scaduti. La classificazione di un libro come di pubblico dominio può variare da paese a paese. I libri di pubblico dominio sono l’anello di congiunzione con il passato, rappresentano un patrimonio storico, culturale e di conoscenza spesso difficile da scoprire. Commenti, note e altre annotazioni a margine presenti nel volume originale compariranno in questo file, come testimonianza del lungo viaggio percorso dal libro, dall’editore originale alla biblioteca, per giungere fino a te. Linee guide per l’utilizzo Google è orgoglioso di essere il partner delle biblioteche per digitalizzare i materiali di pubblico dominio e renderli universalmente disponibili. I libri di pubblico dominio appartengono al pubblico e noi ne siamo solamente i custodi. Tuttavia questo lavoro è oneroso, pertanto, per poter continuare ad offrire questo servizio abbiamo preso alcune iniziative per impedire l’utilizzo illecito da parte di soggetti commerciali, compresa l’imposizione di restrizioni sull’invio di query automatizzate. Inoltre ti chiediamo di: + Non fare un uso commerciale di questi file Abbiamo concepito Google Ricerca Libri per l’uso da parte dei singoli utenti privati e ti chiediamo di utilizzare questi file per uso personale e non a fini commerciali. -
Ghost Imaging of Space Objects
Ghost Imaging of Space Objects Dmitry V. Strekalov, Baris I. Erkmen, Igor Kulikov, and Nan Yu Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, California 91109-8099 USA NIAC Final Report September 2014 Contents I. The proposed research 1 A. Origins and motivation of this research 1 B. Proposed approach in a nutshell 3 C. Proposed approach in the context of modern astronomy 7 D. Perceived benefits and perspectives 12 II. Phase I goals and accomplishments 18 A. Introducing the theoretical model 19 B. A Gaussian absorber 28 C. Unbalanced arms configuration 32 D. Phase I summary 34 III. Phase II goals and accomplishments 37 A. Advanced theoretical analysis 38 B. On observability of a shadow gradient 47 C. Signal-to-noise ratio 49 D. From detection to imaging 59 E. Experimental demonstration 72 F. On observation of phase objects 86 IV. Dissemination and outreach 90 V. Conclusion 92 References 95 1 I. THE PROPOSED RESEARCH The NIAC Ghost Imaging of Space Objects research program has been carried out at the Jet Propulsion Laboratory, Caltech. The program consisted of Phase I (October 2011 to September 2012) and Phase II (October 2012 to September 2014). The research team consisted of Drs. Dmitry Strekalov (PI), Baris Erkmen, Igor Kulikov and Nan Yu. The team members acknowledge stimulating discussions with Drs. Leonidas Moustakas, Andrew Shapiro-Scharlotta, Victor Vilnrotter, Michael Werner and Paul Goldsmith of JPL; Maria Chekhova and Timur Iskhakov of Max Plank Institute for Physics of Light, Erlangen; Paul Nu˜nez of Coll`ege de France & Observatoire de la Cˆote d’Azur; and technical support from Victor White and Pierre Echternach of JPL. -
Arxiv:2103.07476V1 [Astro-Ph.GA] 12 Mar 2021
FERMILAB-PUB-21-075-AE-LDRD Draft version September 3, 2021 Typeset using LATEX twocolumn style in AASTeX63 The DECam Local Volume Exploration Survey: Overview and First Data Release A. Drlica-Wagner ,1, 2, 3 J. L. Carlin ,4 D. L. Nidever ,5, 6 P. S. Ferguson ,7, 8 N. Kuropatkin ,1 M. Adamow´ ,9, 10 W. Cerny ,2, 3 Y. Choi ,11 J. H. Esteves,12 C. E. Mart´ınez-Vazquez´ ,13 S. Mau ,14, 15 A. E. Miller,16, 17 B. Mutlu-Pakdil ,2, 3 E. H. Neilsen ,1 K. A. G. Olsen ,6 A. B. Pace ,18 A. H. Riley ,7, 8 J. D. Sakowska ,19 D. J. Sand ,20 L. Santana-Silva ,21 E. J. Tollerud ,11 D. L. Tucker ,1 A. K. Vivas ,13 E. Zaborowski,2 A. Zenteno ,13 T. M. C. Abbott ,13 S. Allam ,1 K. Bechtol ,22, 23 C. P. M. Bell ,16 E. F. Bell ,24 P. Bilaji,2, 3 C. R. Bom ,25 J. A. Carballo-Bello ,26 D. Crnojevic´ ,27 M.-R. L. Cioni ,16 A. Diaz-Ocampo,28 T. J. L. de Boer ,29 D. Erkal ,19 R. A. Gruendl ,30, 31 D. Hernandez-Lang,32, 13, 33 A. K. Hughes,20 D. J. James ,34 L. C. Johnson ,35 T. S. Li ,36, 37, 38 Y.-Y. Mao ,39, 38 D. Mart´ınez-Delgado ,40 P. Massana,19, 41 M. McNanna ,22 R. Morgan ,22 E. O. Nadler ,14, 15 N. E. D. Noel¨ ,19 A. Palmese ,1, 2 A. H. G. Peter ,42 E. S.