Γ-Ray Searches and the Formation of CDM Halos [ Phd THESIS ]

Total Page:16

File Type:pdf, Size:1020Kb

Γ-Ray Searches and the Formation of CDM Halos [ Phd THESIS ] UNIVERSIDAD DE GRANADA Tesis doctoral Julio 2009 The nature of Dark Matter: γ-ray searches and the formation of CDM halos [ PhD THESIS ] Miguel Angel´ S´anchez Conde Instituto de Astrof´ısica de Andaluc´ıa (CSIC) Memoria de Tesis presentada en la Universidad de Granada para optar al grado de Doctor en Astrof´ısica Directores de tesis: Dr. Francisco Prada Mart´ınez Prof. Mariano Moles Villamate Editor: Editorial de la Universidad de Granada Autor: Miguel Ángel Sánchez Conde D.L.: GR. 3517-2009 ISBN: 978-84-692-6397-6 . A ti, Raquel, por venir al mundo, y a ti, Mar´ıa, por traerla. Y a mis padres, por su apoyo y confianza ciegos. Lo que sabemos es una gota de agua; lo que ignoramos es el oc´eano. - Isaac Newton - Una vez sent´ıel ansia de una sed infinita. - en Azul, de Rub´en Dar´ıo - Una vez m´as percib´ıese raro contraste entre las estrellas y nosotros. La incalculable potencia del Cosmos acrecentaba misteriosamente la verdad de nuestra breve chispa, y el breve e incierto destino de los hombres. - en El hacedor de estrellas, de Olaf Stapledon - . Agradecimientos Siempre quise ser astrof´ısico. Pese a los a˜nos transcurridos, recuerdo con total nitidez aquella tarde de invierno del 91 en la que me compr´emi primer telescopio, cuando a´un no era m´as que un chiquillo de 11 a˜nos. A´un me es posible rememorar la emoci´on e ilusi´on que me embargaban cuando el Universo se iba desvelando ante mi tras aquel peque˜no catalejo. He de reconocer que, afortunadamente, a´un me llena el mismo sentimiento, ahora sin duda m´as maduro. Ha sido un largo camino hasta aqu´ıy hay, por fortuna, mucho que agradecer y muchos a quienes agradecer. En primer lugar, quisiera dar profundamente las gracias a mi director de tesis, Paco Prada. Ciertamente esta Tesis debe verse como producto de un trabajo compartido por ambos a lo largo de estos a˜nos. Su gu´ıa en estos mis primeros y temblorosos pasos en la investigaci´on ha sido fundamental en la consecuci´on de las metas impuestas as´ıcomo en el verdadero conocimiento de mis propias posibilidades. Su ambici´on y motivaci´on cient´ıficas han supuesto para mi un incentivo para llegar siempre m´as all´a, a cuestionarme con curiosidad cient´ıfica cada paso a dar y cada paso dado, a lograr alcanzar objetivos a priori inalcanzables y que luego han demostrado ser tangibles. Gracias tambi´en por tu esfuerzo, dedicaci´on y preocupaci´on en moldearme como un buen cient´ıfico. No puedo dejar de acordarme tambi´en de todos aquellos colegas de profesi´on que a lo largo de estos a˜nos han sido fuente inagotable de conversaci´on cient´ıfica y pasi´on compartida. Gracias especialmente a Mariano Moles por su apoyo y por creer en mi desde el principio, as´ıcomo por compartir conmigo sus vastos conocimientos. Gra- cias tambi´en a mi asiduo colaborador en la distancia, Juan Betancort, por obligarme siempre a ser particularmente met´odico y conciso. Es a a ´el a quien debo por entero mis incursiones en la Cosmolog´ıa m´as te´orica, pero tambi´en la confirmaci´on de mi fe en el valor de los ideales. Mi agradecimiento tambi´en a todo mi grupo de trabajo en el IAA -Alberto, Antonio, Fabio, Hugo, To˜no-, por ayudarme a respirar un ambiente de trabajo m´as cient´ıfico todos los d´ıas, y en definitiva por compartir conmigo este duro aunque apasionante camino. No quiero pasar la oportunidad para agradecer igual- mente a todos aquellos amigos y colegas astrof´ısicos que me han hecho sentirme como uno m´as del gremio siempre: J¨urg Diemand, Mario G´omez, David Paneque, Carlos Delgado, Michele Doro, Radek Wojtak, EwaLokas, Elliott Bloom, Anatoly Klypin, Carlos Mu˜noz, Gustavo Yepes, Daniel Kranich, Abelardo Moralejo. Tambi´en en el viii IAA he contado con la simpat´ıa y ayuda de varias personas que ya permanecer´an en mi memoria como una p´agina m´as de esta Tesis: Antxon Alberdi, Benigno Cantero, Mar´ıa Angeles´ Cort´es, Emilio Garc´ıa, Isabel M´arquez, Paco Navarro, Rafael Parra, Miguel A. P´erez Torres. Es cierto. Siempre quise ser astrof´ısico. Y sin duda lo soy gracias a mi familia, que con una confianza sin l´ımites me alent´osiempre a perseguir mis m´as alocados sue˜nos. Esta Tesis no es sino la mejor muestra de ello. Mis padres, Antonio y Concha, siem- pre me apoyaron incondicionalmente a lo largo de todos estos a˜nos, pese a que esta pasi´on supon´ıa alejarme cientos de kil´ometros de ellos y adem´as con destino incierto. Gracias por darme tanto y exigir tan poco, por moldearme como persona y esculpir en mi vuestra visi´on del mundo, por escuchar, por lanzaros al abismo conmigo sin siquiera preguntar cuando hizo falta... Mi hermano mayor, Alaly, a quien con toda seguridad debo el hecho de haberme dedicado a esto de por vida, y con quien me asom´epor vez primera a los secretos de la Astronom´ıa. Gracias por aquellas noches inolvidables al raso entre las vi˜nas, a un paso de casa pero en realidad muy lejos, entre las estrellas. A mi hermano Jes´us, que encontr´osus propias estrellas en la m´usica, y que siempre ha significado para mi un soplo sincero de cari˜no incondicional y un ejemplo maestro de tes´on y valor ante lo que cada uno ans´ıa. Gracias tambi´en a mis cu˜nadas Mar´ıa Jos´ey Txus, por brindar la felicidad a mis hermanos y formar parte de nosotros. Definitivamente, los valores y el amor de mi familia han impregnado siempre todo lo que he tocado y, por ende, esta Tesis necesariamente encierra una gran dosis del modo de hacer (y de ser) de los S´anchez Conde. En el largo camino hasta aqu´ı, no s´olo los misterios del Cosmos han ido desfilando ante mis ojos, sino tambi´en los de mi propia vida. Mar´ıa, mi esposa y mejor con- fidente y amiga, supone para mi la mayor motivaci´on que es posible imaginar para continuar adelante. Sin duda es ella la luz que ilumina mi camino en esta vasta y tenebrosa oscuridad que es la propia existencia. Ella mejor que nadie sabe de mis triunfos y alegr´ıas, pero tambi´en de mis miedos y fracasos, derrotas y frecuentes tropiezos, pues ha sido ella quien ha compartido m´as de cerca conmigo cada subir y bajar de estos ´ultimos nueve a˜nos. Ella ha sido el b´alsamo necesario para recuperar la serenidad y las ansias de seguir adelante en los momentos dif´ıciles a lo largo de esta tesis. Gracias, cari˜no, por estar siempre a mi lado. Y gracias tambi´en por darme a nuestra Raquel, que ya es la estrella m´as brillante de nuestro cielo particular. Mi agradecimiento tambi´en a mis suegros Miguel y Sole, y a mis cu˜nados Miguel, Ana y Alberto, por tratarme como uno m´as de la familia y comprender el camino al que me ve´ıa abocado por mi pasi´on por las estrellas. Tambi´en tengo mucho que agradecer a aquellos buenos amigos que, por fortuna, me han acompa˜nado a lo largo de mi vida o en distintos momentos de ella. Mi ilusi´on ha permanecido intacta todo este tiempo en buena medida gracias a muchos de mis ix amigos de Almendralejo, que con devoci´on ciega han seguido mi trayectoria y me han aportado seguridad y confianza en mi mismo, adem´as de entregarme su amistad m´as profunda y sincera: Moi, Leandro, Julio, Paco, Jesus, Mario, Lucky, Mart´ın, Zaca, los hermanos Jare˜no. Tambi´en Agust´ın, Alex, Bel´en, Chovis, Diego, Jose, Juan, Marcos, Merch´an, Paco Melado, Patricia, Velarde... ¡C´omo olvidar aquellas noches en el Puente de las Peras (que no de la Espera) trazando nuestros planes de comernos el mundo a la ´unica luz de las estrellas! Bien sab´eis muchos de vosotros que este era el m´as preciado para mi... Tambi´en mis tres a˜nos de estudios en Badajoz me proporcionaron amigos que a´un hoy siguen en mi vida y a los que agradezco enormemente su apoyo continuo y amistad: Pedro, V´ıctor, Juli, Merche, Vicente, Lidia, Miguel A y B, Noelia, Rosal´ıa, Raquel, Luis, Juampe... En Badajoz tambi´en conoc´ı a Antonio, con el que ya entonces compart´ıa aficiones y conocimientos, y con el que luego compartir´ıa d´ıa a d´ıa, y como u˜na y carne, todo sue˜no y todo anhelo. Fue con ´el con quien me embarqu´een mi aventura canaria, en nuestra mutua determinaci´on por llegar a ser lo que ahora somos (esto es, ni m´as ni menos que lo que siempre quisimos ser). Gracias por mantenerte siempre cerca. De esa etapa universitaria canaria, rodeado de mar y a tres meses de casa, debo agradecer que el destino pusiera en mi camino en especial a Luis, con su inagotable vitalidad, a Pl´acido, con sus f´erreos ideales, a Charly, Dar´ıo (en aquella ´epoca el Peludo), Omaira, Mar, Alicia, Manolo, los dos Jorge, Jairo, Rub´en, Teo, Susi, David, Javi, Rebeca. Con ellos compart´ıaquellos a˜nos inolvidables al pie del Teide, y sobre ´el tambi´en, y muchos amaneceres sobre el mar. El destino burl´on ha vuelto a juntarnos a varios de nosotros en Granada, donde nuestra amistad ha madurado y se ha estrechado a´un m´as.
Recommended publications
  • Portrait of a Dramatic Stellar Crib 21 December 2006
    Portrait of a dramatic stellar crib 21 December 2006 most massive stars known. The nebula owes its name to the arrangement of its brightest patches of nebulosity, that somewhat resemble the legs of a spider. They extend from a central 'body' where a cluster of hot stars (designated 'R136') illuminates and shapes the nebula. This name, of the biggest spiders on the Earth, is also very fitting in view of the gigantic proportions of the celestial nebula - it measures nearly 1,000 light-years across and extends over more than one third of a degree: almost, but not quite, the size of the full Moon. If it were in our own Galaxy, at the distance of another stellar nursery, the Orion Nebula (1,500 light-years away), it would cover one quarter of the sky and even be visible in daylight. One square degree image of the Tarantula Nebula and its surroundings. The spidery nebula is seen in the upper- center of the image. Slightly to the lower-right, a web of filaments harbors the famous supernova SN 1987A (see below). Many other reddish nebulae are visible in the image, as well as a cluster of young stars on the left, known as NGC 2100. Credit: ESO Known as the Tarantula Nebula for its spidery appearance, the 30 Doradus complex is a monstrous stellar factory. It is the largest emission nebula in the sky, and can be seen far down in the southern sky at a distance of about 170,000 light- years, in the southern constellation Dorado (The Swordfish or the Goldfish).
    [Show full text]
  • Remerciements – Unité 1
    TVO ILC SNC1D Remerciements Remerciements – Unité 1 Graphs, diagrams, illustrations, images in this course, unless otherwise specified, are ILC created, Copyright © 2018 The Ontario Educational Communications Authority. All rights reserved. Intro Video, Copyright © 2018 The Ontario Educational Communications Authority. All rights reserved. All title artwork and graphics, unless otherwise specified, Copyright © 2018The Ontario Educational Communications Authority. All rights reserved. Logo: Science Presse , Agence Science-Presse, URL: https://www.sciencepresse.qc.ca/, Accessed 14/01/2019. Logo: Curium, Curium, URL: https://curiummag.com/wp-content/uploads/2017/10/logo_ curium-web.png, Accessed 14/01/2019. Logo: Science Étonnante, David Louapre, URL: https://sciencetonnante.wordpress.com/, Accessed 20/03/2018, © 2018 HowStuffWorks, a division of InfoSpace Holdings LLC, a System1 Company. Blog, blogging and blogglers theme, djvstock/iStock/Getty Images Logo: Wordpress, WordPress.com, Automattic Inc., URL: https://wordpress.com/, Accessed 20/03/2018, © The WordPress Foundation. Logo: Wix, Wix.com, Inc., URL: https://static.wixstatic.com/ media/9ab0d1_39d56f21398048df8af89aab0cec67b8~mv1.png, Accessed 14/01/2019. Logo: Blogger, Blogger, Inc., ZyMOS, URL: https://commons.wikimedia.org/wiki/File:Blogger. svg, Accessed 20/03/2018, © Google LLC. HOME A film by Yann Arthus-Bertrand, GoodPlanet Foundation, Europacorp and Elzévir Films, URL: https://www.youtube.com/watch?v=GItD10Joaa0, Published 04/02/2009, Accessed 20/04/2018, Courtesy of the GoodPlanet
    [Show full text]
  • An Artist's Revelation in a Walking Canvas 3 Tale of Ansel Adams
    An Artist’s Revelation in a Walking Canvas 3 Tale of Ansel Adams Negatives Grows Hazy 5 Galaxies of Wire, Canvas and Velvety Soot 8 Single Neurons Can Detect Sequences 10 Antibiotics for the Prevention of Malaria 12 Shared Phosphoproteome Links Remote Plant Species 14 Asteroid Found in Gravitational 'Dead Zone' Near Neptune 15 Scientists Test Australia's Moreton Bay as Coral 'Lifeboat' 17 Hexagonal Boron Nitride Sheets May Help Graphene Supplant Silicon 20 Geologists Reconstruct Earth's Climate Belts Between 460 and 445 Million Years Ago 22 Neurological Process for the Recognition of Letters and Numbers Explained 24 Certain Vena Cava Filters May Fracture, Causing Life-Threatening Complications 26 Citizen Scientists Discover Rotating Pulsar 28 Scientists Outline a 20-Year Master Plan for the Global Renaissance of Nuclear Energy 30 Biochar Can Offset 1.8 Billion Metric Tons of Carbon Emissions Annually 33 Research Reveals Similarities Between Fish and Humans 36 Switchgrass Lessens Soil Nitrate Loss Into Waterways, Researchers Find 38 Free Statins With Fast Food Could Neutralize Heart Risk, Scientists Say 40 Ambitious Survey Spots Stellar Nurseries 42 For Infant Sleep, Receptiveness More Important Than Routine 44 Arctic Rocks Offer New Glimpse of Primitive Earth 46 Learn More in Kindergarten, Earn More as an Adult 48 Giant Ultraviolet Rings Found in Resurrected Galaxies 50 Faster DNA Analysis at Room Temperature 53 Biodiversity Hot Spots More Vulnerable to Global Warming Than Thought 55 Women Feel More Pain Than Men 57 Are We Underestimating
    [Show full text]
  • 2Df-Aaomega Spectroscopy of Massive Stars in the Magellanic Clouds the North-Eastern Region of the Large Magellanic Cloud?,??
    A&A 584, A5 (2015) Astronomy DOI: 10.1051/0004-6361/201525882 & c ESO 2015 Astrophysics 2dF-AAOmega spectroscopy of massive stars in the Magellanic Clouds The north-eastern region of the Large Magellanic Cloud?;?? C. J. Evans1, J. Th. van Loon2, R. Hainich3, and M. Bailey4;2 1 UK Astronomy Technology Centre, Royal Observatory, Blackford Hill, Edinburgh, EH9 3HJ, UK e-mail: [email protected] 2 Astrophysics Group, School of Physical and Geographical Sciences, Lennard-Jones Laboratories, Keele University, ST5 5BG, UK 3 Institute for Physics and Astronomy, University of Potsdam, 14476 Potsdam, Germany 4 Astrophysics Research Institute, Liverpool John Moores University, Liverpool Science Park ic2, 146 Brownlow Hill, Liverpool L3 5RF, UK Received 13 February 2015 / Accepted 5 August 2015 ABSTRACT We present spectral classifications from optical spectroscopy of 263 massive stars in the north-eastern region of the Large Magellanic Cloud. The observed two-degree field includes the massive 30 Doradus star-forming region, the environs of SN1987A, and a number of star-forming complexes to the south of 30 Dor. These are the first classifications for the majority (203) of the stars and include eleven double-lined spectroscopic binaries. The sample also includes the first examples of early OC-type spectra (AAΩ 30 Dor 248 and 280), distinguished by the weakness of their nitrogen spectra and by C IV λ4658 emission. We propose that these stars have relatively unprocessed CNO abundances compared to morphologically normal O-type stars, indicative of an earlier evolutionary phase. From analysis of observations obtained on two consecutive nights, we present radial-velocity estimates for 233 stars, finding one apparent single-lined binary and nine (>3σ) outliers compared to the systemic velocity; the latter objects could be runaway stars or large-amplitude binary systems and further spectroscopy is required to investigate their nature.
    [Show full text]
  • X-Rays Tracing the Star Formation History of the Magellanic Clouds
    X-rays Tracing the Star Formation History of the Magellanic Clouds Dissertation der Fakult¨at fur¨ Physik der Ludwig-Maximilians-Universit¨at Munc¨ hen zur Erlangung des Grades Doktor der Naturwissenschaften Dr. rer. nat. vorgelegt von Manami Sasaki aus Tokio, Japan Munc¨ hen, den 21. Dezember 2001 1. Gutachter: Prof. Dr. Joachim Trump¨ er 2. Gutachter: Prof. Dr. Ralf Bender Tag der mundlic¨ hen Prufung:¨ 14. Mai 2002 Zusammenfassung R¨ontgenstrahlung als Spuren der Sternentstehungsgeschichte in den Magellanschen Wolken Manami Sasaki Galaxien setzen sich aus Sternen und der den interstellaren Raum auffullenden¨ Ma- terie zusammen. Am Ende der Sternentwicklung entstehen Weiße Zwerge, Neutro- nensterne, Schwarze L¨ocher sowie Supernova-Ub¨ erreste, die aufgrund hoher Temper- aturen R¨ontgenstrahlung emittieren. Deshalb liefern astronomische Beobachtungen im R¨ontgenbereich wichtige Erkenntnisse fur¨ das Verst¨andnis des Aufbaus und der Entwicklungsgeschichte von Galaxien. Die Große Magellansche Wolke (Large Magellanic Cloud, LMC) und die Kleine Magellansche Wolke (Small Magellanic Cloud, SMC), jeweils ca. 160.000 und 190.000 Lichtjahre von unserem Sonnensystem entfernt, befinden sich in unmittelbarer Umge- bung unserer Milchstraße und sind somit die am besten geeigneten Objekte fur¨ die Un- tersuchung von Galaxien in ihrer Ganzheit. W¨ahrend der Betriebsphase des R¨ontgen- satelliten ROSAT in den Jahren von 1990 bis 1998 sind etwa 900 Beobachtungen von der LMC und der SMC durchgefuhrt¨ worden, die das Bild der Magellanschen Wolken (MCs) im R¨ontgenlicht enthullten.¨ Erstes Hauptziel dieser Doktorarbeit bestand darin, die erste umfassende Studie der R¨ontgenquellen in den MCs anhand von Archiv-Daten vom ROSAT "High Resolu- tion Imager" (HRI) durchzufuhren.¨ Die Ergebnisse erm¨oglichen in Kombination mit den Quell-Katalogen von Haberl & Pietsch (1999a) und Haberl et al.
    [Show full text]
  • Astro-Ph/0601105
    A Chandra/ACIS Study of 30 Doradus I. Superbubbles and Supernova Remnants Leisa K. Townsley1, Patrick S. Broos1, Eric D. Feigelson1, Bernhard R. Brandl2, You-Hua Chu3, Gordon P. Garmire1, George G. Pavlov1 ABSTRACT We present an X-ray tour of diffuse emission in the 30 Doradus star-forming complex in the Large Magellanic Cloud using high-spatial-resolution X-ray images and spatially-resolved spectra obtained with the Advanced CCD Imaging Spectrometer aboard the Chandra X-ray Observatory. The dominant X-ray feature of the 30 Doradus nebula is the intricate network of diffuse emission generated by interacting stellar winds and supernovae working together to create vast superbubbles filled with hot plasma. We construct maps of the region showing variations 21 −2 in plasma temperature (T = 3–9 million degrees), absorption (NH = 1–6×10 cm ), and 31 −1 −2 absorption-corrected X-ray surface brightness (SX = 3–126×10 ergs s pc ). Enhanced images reveal the pulsar wind nebula in the composite supernova remnant N157B and the Chandra data show spectral evolution from non-thermal synchrotron emission in the N157B core to a thermal plasma in its outer regions. In a companion paper we show that R136, the central massive star cluster, is resolved at the arcsecond level into almost 100 X-ray sources. Through X-ray studies of 30 Doradus the complete life cycle of such a massive stellar cluster can be revealed. Subject headings: HII regions − stars: winds, outflows − galaxies: star clusters − ISM: individual (30 Doradus) − supernova remnants − X-rays: ISM 1. INTRODUCTION which they formed, igniting a new generation of stars.
    [Show full text]
  • The First Broad-Band X-Ray Images and Spectra of the 30 Doradus Region
    A&A 365, L202–L207 (2001) Astronomy DOI: 10.1051/0004-6361:20000049 & c ESO 2001 Astrophysics The first broad–band X-ray images and spectra of the 30 Doradus region in the LMC? K. Dennerl1,F.Haberl1,B.Aschenbach1,U.G.Briel1, M. Balasini4,H.Br¨auninger1, W. Burkert1, R. Hartmann1,G.Hartner1,G.Hasinger3, J. Kemmer6, E. Kendziorra2,M.Kirsch2, N. Krause1, M. Kuster2,D.Lumb5, P. Massa4, N. Meidinger1,E.Pfeffermann1,W.Pietsch1, C. Reppin1,H.Soltau6, R. Staubert2,L.Str¨uder1,J.Tr¨umper1, M. Turner7, G. Villa4, and V. E. Zavlin1 1 Max-Planck-Institut f¨ur extraterrestrische Physik, 85748 Garching, Germany 2 Institut f¨ur Astronomie und Astrophysik der Univ. T¨ubingen, Waldh¨auserstr. 64, 72076 T¨ubingen, Germany 3 Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany 4 Istituto di Fisica Cosmica “G. Occhialini”, Via Bassini 15, 20133 Milano, Italy 5 XMM Science Operations Centre, Space Science Division ESTEC, Postbus 299, 2200 AG Noordwijk, The Netherlands 6 KETEK GmbH, Am Isarbach 30, 85764 Oberschleißheim, Germany 7 Physics and Astronomy Department, University of Leicester, Leicester LE1 7RH, UK Received 13 October 2000 / Accepted 24 October 2000 Abstract. We present the XMM–Newton first light image, taken in January 2000 with the EPIC pn camera during the instrument’s commissioning phase, when XMM–Newton was pointing towards the Large Magellanic Cloud (LMC). The field is rich in different kinds of X-ray sources: point sources, supernova remnants (SNRs) and diffuse X-ray emission from LMC interstellar gas. The observations are of unprecedented sensitivity, reaching a few 1032 erg/s for point sources in the LMC.
    [Show full text]
  • Hubble's Bubbles in the Tarantula Nebula 9 October 2017
    Image: Hubble's bubbles in the Tarantula Nebula 9 October 2017 combined effect of two supernovae—a more recent explosion has pierced the expanding shell of material created by an older explosion. The nebula's especially striking appearance is suspected to be due to a fortuitous viewing angle; the honeycomb effect of the circular shells may not be visible from another viewpoint. Provided by NASA Credit: ESA/Hubble & NASA, Acknowledgements: Judy Schmidt (Geckzilla) At a distance of just 160,000 light-years, the Large Magellanic Cloud is one of the Milky Way's closest companions. It is also home to one of the largest and most intense regions of active star formation known to exist anywhere in our galactic neighborhood—the Tarantula Nebula. This NASA/ESA Hubble Space Telescope image shows both the spindly, spidery filaments of gas that inspired the region's name, and the intriguing structure of stacked "bubbles" that forms the so- called Honeycomb Nebula (to the lower left). The Honeycomb Nebula was found serendipitously by astronomers using ESO's New Technology Telescope to image the nearby SN1987A, the closest observed supernova to Earth for more than 400 years. The nebula's strange bubble-like shape has baffled astronomers since its discovery in the early 1990s. Various theories have been proposed to explain its unique structure, some more exotic than others. In 2010, a group of astronomers studied the nebula and, using advanced data analysis and computer modelling, came to the conclusion that its unique appearance is likely due to the 1 / 2 APA citation: Image: Hubble's bubbles in the Tarantula Nebula (2017, October 9) retrieved 27 September 2021 from https://phys.org/news/2017-10-image-hubble-tarantula-nebula.html This document is subject to copyright.
    [Show full text]
  • SCHENCK-DISSERTATION-2017.Pdf (5.573Mb)
    A CHANDRA STUDY OF SUPERNOVA REMNANTS IN THE LARGE AND SMALL MAGELLANIC CLOUDS by ANDREW COREY SCHENCK Presented to the Faculty of the Graduate School of The University of Texas at Arlington in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT ARLINGTON May 2017 Copyright c by Andrew Corey Schenck 2017 All Rights Reserved To my wife, without whom I would never have achieved my dream. And to my son Fisher Nathaniel Schenck. I miss you terribly. ACKNOWLEDGEMENTS The journey up to this point has been a long one. It has had its ups and downs, its share of fun and anxiety, but time has now come to close this chapter in my life and begin the next. I must start by thanking Sangwook Park, for your patience, advice, and guid- ance throughout my graduate career. I feel honored to have worked along side you and deeply appreciate everything you have done for me. Thanks are also due to the other members of this thesis committee, Manfred Cuntz, Yue Deng, Alex Weiss, and Zizislaw Musielak. Thank you for your time and support during my stay at UTA. With a special thanks to Chris Jackson, I appreciate everything. To our collaborators, David Burrows, Jack Hughes, Jae-Joon Lee, and Koji Mori, thanks for contributing your time and expertise. Finally, thanks to my colleagues and many friends at UTA, Jayant Bhalerao, Seth Post, and Carola Ellinger to name only a few. Thanks for putting up with me throughout these years and I appreciate you being a part of this journey.
    [Show full text]
  • Acknowledgements
    TVO ILC SNC1D Acknowledgements Acknowledgements – Unit 1 Learning activity 1 Blog Definition, Oxford University Press, URL: https://en.oxforddictionaries.com/definition/ blog, Accessed 20/03/2018. Logo: ScienceBlogs, URL: http://scienceblogs.com/, Accessed 20/03/2018, © 2006-2018 ScienceBlogs LLC. ScienceBlogs is a registered trademark of ScienceBlogs LLC. Logo: The Daily Galaxy, URL: http://www.dailygalaxy.com/, Accessed 20/03/2018. Logo: How Stuff Works, URL: https://science.howstuffworks.com/, Accessed 20/03/2018, © 2018 HowStuffWorks, a division of InfoSpace Holdings LLC, a System1 Company. Logo: IOP - Institute of Physics, URL: http://www.iopblog.org/, Accessed 20/03/2018, © Institute of Physics. Blog, blogging and blogglers theme, djvstock/iStock/Getty Images Logo: Wordpress, WordPress.com, Automattic Inc., URL: https://wordpress.com/, Accessed 20/03/2018, © The WordPress Foundation. Logo: Tumblr, Tumblr, Inc., URL: https://www.tumblr.com/, Accessed 20/03/2018, © Tumblr, Inc., a Delaware corporation and wholly-owned subsidiary of Oath Inc., a Delaware corporation. Logo: Blogger, Blogger, Inc., ZyMOS, URL: https://commons.wikimedia.org/wiki/File:Blogger. svg, Accessed 20/03/2018, © Google LLC. HOME - A film by Yann Arthus-Bertrand, Europacorp and Elzévir Films, URL: https://www. youtube.com/watch?v=HAE24kOPAVU&feature=youtu.be, Published 04/02/2009, Accessed 20/04/2018, Courtesy of the GoodPlanet Foundation. Mining dump trucks, aerial photo, dan_prat/iStock/Getty Images Land clearing, lanolan/iStock/Getty Images Hurricane George damage
    [Show full text]
  • Massive Stars and High-Energy Emission in OB Associations
    Massive Stars and High-Energy Emission in OB Associations Proceedings of JENAM 2005 Distant Worlds, July 4-7, 2005, Liège (Belgium) Images © ESA, ESO, NASA. Institut d‘Astrophysique et de Géophysique Edited by: Université de Liège G. Rauw, Y. Nazé, Allée du 6 Août 17, Bat. B5C R. Blomme & E. Gosset B4000-Liège (Belgium) Dépôt légal : D/2005/0480/95 Foreword About 35 astronomers including many experts in the field of massive stars attended the afternoon sessions of the JENAM 2005 workshop —Massive Stars and High-Energy Emission in OB Associations“. In addition to the two plenary talks by Dr Ian Stevens and Prof Thierry Montmerle, two invited reviews by Prof Artemio Herrero and Dr Martin Guerrero as well as 12 contributed talks and nine posters were presented during the workshop. A good number of new exciting results obtained with modern high-resolution optical spectrographs and/or high-energy instruments onboard XMM-Newton, Chandra and INTEGRAL were presented and new questions were raised. Several contributions were devoted to non-thermal phenomena associated with a subset of the massive stars. Many results presented at the workshop seem to demonstrate that non-thermal radio emission of early-type stars is a signature of colliding winds in binary systems. W hile this was already established for W olf-Rayet stars, it becomes now more and more obvious for O stars as well. In this context, the participants emphasized the interest to search for non-thermal X-ray and G- ray emissions from massive binaries. Such a hard X-ray œ soft G-ray emission could also arise from the collision of a supernova remnant with a stellar wind.
    [Show full text]
  • Supernova Remnants in the Magellanic Clouds III: an X-Ray Atlas of LMC Supernova Remnants
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Supernova Remnants in the Magellanic Clouds III: An X-ray Atlas of LMC Supernova Remnants Rosa Murphy Williams, You-Hua Chu, and John R. Dickel Astronomy Department, University of Illinois at Urbana-Champaign, Urbana, IL 61801 Robert Petre NASA/GSFC code 666, Greenbelt, MD 20771 R. Chris Smith Cerro Tololo Inter-American Observatory, La Serena, Chile Maritza Tavarez Astronomy Department, University of Michigan, Ann Arbor, MI 48109-1090 ABSTRACT We have used archival ROSAT data to present X-ray images of thirty-one supernova remnants (SNRs) in the Large Magellanic Cloud (LMC). We have classified these remnants according to their X-ray morphologies, into the categories of Shell-Type, Diffuse Face, Centrally Brightened, Point-Source Dominated, and Irregular. We suggest possible causes of the X-ray emission for each category, and for individual features of some of the SNRs. Subject headings: galaxies: individual (LMC) – ISM: supernova remnants – ISM: kinematics and dynamics – X-rays: ISM 1. Introduction One of the most influential factors in the shaping of the interstellar medium (ISM) is the input of energy from supernova explosions and the subsequent development of their remnants. The long-term evolution of a supernova remnant (SNR) is subject to both the details of the original explosion (initial energy input, explosion asymmetries, etc.) and the characteristics of its surrounding environment. A unique opportunity to study SNRs from different initial conditions, in a wide variety of environments, is provided by the Large Magellanic Cloud (LMC).
    [Show full text]