Towards Advanced Astronomical Imaging: New Techniques of Data Reduction and Their Applications
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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◦. -
Limits from the Hubble Space Telescope on a Point Source in SN 1987A
Limits from the Hubble Space Telescope on a Point Source in SN 1987A The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Graves, Genevieve J. M., Peter M. Challis, Roger A. Chevalier, Arlin Crotts, Alexei V. Filippenko, Claes Fransson, Peter Garnavich, et al. 2005. “Limits from the Hubble Space Telescopeon a Point Source in SN 1987A.” The Astrophysical Journal 629 (2): 944–59. https:// doi.org/10.1086/431422. Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:41399924 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA The Astrophysical Journal, 629:944–959, 2005 August 20 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. LIMITS FROM THE HUBBLE SPACE TELESCOPE ON A POINT SOURCE IN SN 1987A Genevieve J. M. Graves,1, 2 Peter M. Challis,2 Roger A. Chevalier,3 Arlin Crotts,4 Alexei V. Filippenko,5 Claes Fransson,6 Peter Garnavich,7 Robert P. Kirshner,2 Weidong Li,5 Peter Lundqvist,6 Richard McCray,8 Nino Panagia,9 Mark M. Phillips,10 Chun J. S. Pun,11,12 Brian P. Schmidt,13 George Sonneborn,11 Nicholas B. Suntzeff,14 Lifan Wang,15 and J. Craig Wheeler16 Received 2005 January 27; accepted 2005 April 26 ABSTRACT We observed supernova 1987A (SN 1987A) with the Space Telescope Imaging Spectrograph (STIS) on the Hubble Space Telescope (HST ) in 1999 September and again with the Advanced Camera for Surveys (ACS) on the HST in 2003 November. -
A Dozen Colliding Wind X-Ray Binaries in the Star Cluster R 136 in the 30 Doradus Region
A dozen colliding wind X-ray binaries in the star cluster R 136 in the 30 Doradus region Simon F. Portegies Zwart?,DavidPooley,Walter,H.G.Lewin Massachusetts Institute of Technology, Cambridge, MA 02139, USA ? Hubble Fellow Subject headings: stars: early-type — tars: Wolf-Rayet — galaxies:) Magellanic Clouds — X-rays: stars — X-rays: binaries — globular clusters: individual (R136) –2– ABSTRACT We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 32 35 1 X-ray point sources with luminosities between 5 10 and 2 10 erg s− (0.2 × × — 3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type O stars as optical counterparts. Nine of these are within 3:4 pc of R 136, the ∼ central star cluster of NGC 2070. We derive an empirical relation between the X-ray luminosity and the parameters for the stellar wind of the optical counterpart. The relation gives good agreement for known colliding wind binaries in the Milky Way Galaxy and for the identified X-ray sources in NGC 2070. We conclude that probably all identified X-ray sources in NGC 2070 are colliding wind binaries and that they are not associated with compact objects. This conclusion contradicts Wang (1995) who argued, using ROSAT data, that two earlier discovered X-ray sources are accreting black-hole binaries. Five early type stars in R 136 are not bright in X-rays, possibly indicating that they are either: single stars or have a low mass companion or a wide orbit. -
The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia
MNRAS 000,1{20 (2019) Preprint 14 November 2019 Compiled using MNRAS LATEX style file v3.0 The Milky Way's Disk of Classical Satellite Galaxies in Light of Gaia DR2 Marcel S. Pawlowski,1? and Pavel Kroupa2;3 1Leibniz-Institut fur¨ Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany 2Helmholtz-Institut fur¨ Strahlen- und Kernphysik, University of Bonn, Nussallee 14-16, D- 53115 Bonn, Germany 3Charles University in Prague, Faculty of Mathematics and Physics, Astronomical Institute, V Holeˇsoviˇck´ach 2, CZ-180 00 Praha 8, Czech Republic Accepted 2019 November 7. Received 2019 November 7; in original form 2019 August 26 ABSTRACT We study the correlation of orbital poles of the 11 classical satellite galaxies of the Milky Way, comparing results from previous proper motions with the independent data by Gaia DR2. Previous results on the degree of correlation and its significance are confirmed by the new data. A majority of the satellites co-orbit along the Vast Polar Structure, the plane (or disk) of satellite galaxies defined by their positions. The orbital planes of eight satellites align to < 20◦ with a common direction, seven even orbit in the same sense. Most also share similar specific angular momenta, though their wide distribution on the sky does not support a recent group infall or satellites- of-satellites origin. The orbital pole concentration has continuously increased as more precise proper motions were measured, as expected if the underlying distribution shows true correlation that is washed out by observational uncertainties. The orbital poles of the up to seven most correlated satellites are in fact almost as concentrated as expected for the best-possible orbital alignment achievable given the satellite posi- tions. -
VI. Star-Forming Companions of Nearby Field Galaxies
A&A 486, 131–142 (2008) Astronomy DOI: 10.1051/0004-6361:20079297 & c ESO 2008 Astrophysics The Hα Galaxy Survey VI. Star-forming companions of nearby field galaxies P. A. James1, J. O’Neill2, and N. S. Shane1,3 1 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK e-mail: [email protected] 2 Wirral Grammar School for Girls, Heath Road, Bebington, Wirral CH63 3AF, UK 3 Planetary Science Group, Mullard Space Science Laboratory, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK Received 20 December 2007 / Accepted 5 May 2008 ABSTRACT Aims. We searched for star-forming satellite galaxies that are close enough to their parent galaxies to be considered analogues of the Magellanic Clouds. Methods. Our search technique relied on the detection of the satellites in continuum-subtracted narrow-band Hα imaging of the central galaxies, which removes most of the background and foreground line-of-sight companions, thus giving a high probability that we are detecting true satellites. The search was performed for 119 central galaxies at distances between 20 and 40 Mpc, although spatial incompleteness means that we have effectively searched 53 full satellite-containing volumes. Results. We find only 9 “probable” star-forming satellites, around 9 different central galaxies, and 2 more “possible” satellites. After incompleteness correction, this is equivalent to 0.17/0.21 satellites per central galaxy. This frequency is unchanged whether we consider all central galaxy types or just those of Hubble types S0a–Sc, i.e. only the more luminous and massive spiral types. -
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. -
Annual Report 2005
Max Planck Institute t für Astron itu o st m n ie -I k H c e n id la e l P b - e x r a g M M g for Astronomy a r x e b P l la e n id The Max Planck Society c e k H In y s m titu no Heidelberg-Königstuhl te for Astro The Max Planck Society for the Promotion of Sciences was founded in 1948. It operates at present 88 Institutes and other facilities dedicated to basic and applied research. With an annual budget of around 1.4 billion € in the year 2005, the Max Planck Society has about 12 400 employees, of which 4300 are scientists. In addition, annually about 11000 junior and visiting scientists are working at the Institutes of the Max Planck Society. The goal of the Max Planck Society is to promote centers of excellence at the fore- front of the international scientific research. To this end, the Institutes of the Society are equipped with adequate tools and put into the hands of outstanding scientists, who Annual Report have a high degree of autonomy in their scientific work. 2005 Max-Planck-Gesellschaft zur Förderung der Wissenschaften e.V. 2005 Public Relations Office Hofgartenstr. 8 80539 München Tel.: 089/2108-1275 or -1277 Annual Report Fax: 089/2108-1207 Internet: www.mpg.de Max Planck Institute for Astronomie K 4242 K 4243 Dossenheim B 3 D o s s E 35 e n h e N i eckar A5 m e r L a n d L 531 s t r M a a ß nn e he im B e e r r S t tr a a - K 9700 ß B e e n z - S t r a ß e Ziegelhausen Wieblingen Handschuhsheim K 9702 St eu b A656 e n s t B 37 r a E 35 ß e B e In de A5 r r N l kar ec i c M Ne k K 9702 n e a Ruprecht-Karls- ß lierb rh -
The Large Scale Universe As a Quasi Quantum White Hole
International Astronomy and Astrophysics Research Journal 3(1): 22-42, 2021; Article no.IAARJ.66092 The Large Scale Universe as a Quasi Quantum White Hole U. V. S. Seshavatharam1*, Eugene Terry Tatum2 and S. Lakshminarayana3 1Honorary Faculty, I-SERVE, Survey no-42, Hitech city, Hyderabad-84,Telangana, India. 2760 Campbell Ln. Ste 106 #161, Bowling Green, KY, USA. 3Department of Nuclear Physics, Andhra University, Visakhapatnam-03, AP, India. Authors’ contributions This work was carried out in collaboration among all authors. Author UVSS designed the study, performed the statistical analysis, wrote the protocol, and wrote the first draft of the manuscript. Authors ETT and SL managed the analyses of the study. All authors read and approved the final manuscript. Article Information Editor(s): (1) Dr. David Garrison, University of Houston-Clear Lake, USA. (2) Professor. Hadia Hassan Selim, National Research Institute of Astronomy and Geophysics, Egypt. Reviewers: (1) Abhishek Kumar Singh, Magadh University, India. (2) Mohsen Lutephy, Azad Islamic university (IAU), Iran. (3) Sie Long Kek, Universiti Tun Hussein Onn Malaysia, Malaysia. (4) N.V.Krishna Prasad, GITAM University, India. (5) Maryam Roushan, University of Mazandaran, Iran. Complete Peer review History: http://www.sdiarticle4.com/review-history/66092 Received 17 January 2021 Original Research Article Accepted 23 March 2021 Published 01 April 2021 ABSTRACT We emphasize the point that, standard model of cosmology is basically a model of classical general relativity and it seems inevitable to have a revision with reference to quantum model of cosmology. Utmost important point to be noted is that, ‘Spin’ is a basic property of quantum mechanics and ‘rotation’ is a very common experience. -
Afterschool Universe Session 9 Slide Notes: Galaxies
This presentation supports the “Background” material in Session 9 of the Afterschool Universe program. This session is about galaxies. The picture shows the Whirlpool galaxy, a large, iconic, spiral galaxy. 1 Let us summarize the main concepts in this Session. We will discuss these in the rest of this presentation. 2 A galaxy is a huge collection of stars, gas and dust. A typical galaxy has about 100 billion stars (that’s 100,000,000,000 stars!), and light takes about 100,000 years to cross a galaxy (in other words, they are typically 100,000 light years ago). But some galaxies are much bigger and some are much smaller. 3 If you look at the sky from a DARK location, you can see a band of light stretching across the sky which is known as the Milky Way. This is our view of our Galaxy - more precisely, this is our view of the disk of our galaxy as seen from the INSIDE. 4 This picture shows another view of our galaxy taken in the infra-red part of the spectrum. The advantage of the infra-red is that it can penetrate the dust that pervades our galaxy’s disk and let us view the central parts of our galaxy. This picture also shows the full sky. The flat disk and central bulge of our galaxy can be seen in this picture. 5 We live in the suburbs of our galaxy. The Sun and its planetary system are about 25,000 light years from the center of the galaxy. This is about half way out to the edge of the disk. -
16Th HEAD Meeting Session Table of Contents
16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113 -
NASA Astrobiology Institute 2018 Annual Science Report
A National Aeronautics and Space Administration 2018 Annual Science Report Table of Contents 2018 at the NAI 1 NAI 2018 Teams 2 2018 Team Reports The Evolution of Prebiotic Chemical Complexity and the Organic Inventory 6 of Protoplanetary Disk and Primordial Planets Lead Institution: NASA Ames Research Center Reliving the Past: Experimental Evolution of Major Transitions 18 Lead Institution: Georgia Institute of Technology Origin and Evolution of Organics and Water in Planetary Systems 34 Lead Institution: NASA Goddard Space Flight Center Icy Worlds: Astrobiology at the Water-Rock Interface and Beyond 46 Lead Institution: NASA Jet Propulsion Laboratory Habitability of Hydrocarbon Worlds: Titan and Beyond 60 Lead Institution: NASA Jet Propulsion Laboratory The Origins of Molecules in Diverse Space and Planetary Environments 72 and Their Intramolecular Isotope Signatures Lead Institution: Pennsylvania State University ENIGMA: Evolution of Nanomachines in Geospheres and Microbial Ancestors 80 Lead Institution: Rutgers University Changing Planetary Environments and the Fingerprints of Life 88 Lead Institution: SETI Institute Alternative Earths 100 Lead Institution: University of California, Riverside Rock Powered Life 120 Lead Institution: University of Colorado Boulder NASA Astrobiology Institute iii Annual Report 2018 2018 at the NAI In 2018, the NASA Astrobiology Program announced a plan to transition to a new structure of Research Coordination Networks, RCNs, and simultaneously planned the termination of the NASA Astrobiology Institute -
The Deep Near-Infrared Southern Sky Survey (DENIS)
R E P O R T S F R O M O B S E R V E R S The Deep Near-Infrared Southern Sky Survey (DENIS) N. EPCHTEIN, B. DE BATZ, L. CAPOANI, L. CHEVALLIER, E. COPET, P. FOUQUÉ, F. LACOMBE, T. LE BERTRE, S. PAU, D. ROUAN, S. RUPHY, G. SIMON, D. TIPHÈNE, Paris Observatory, France W.B. BURTON, E. BERTIN, E. DEUL, H. HABING, Leiden Observatory, Netherlands J. BORSENBERGER, M. DENNEFELD, F. GUGLIELMO, C. LOUP, G. MAMON, Y. NG, A. OMONT, L. PROVOST, J.-C. RENAULT, F. TANGUY, Institut d’Astrophysique de Paris, France S. KIMESWENGER and C. KIENEL, University of Innsbruck, Austria F. GARZON, Instituto de Astrofísica de Canarias, Spain P. PERSI and M. FERRARI-TONIOLO, Istituto di Astrofisica Spaziale, Frascati, Italy A. ROBIN, Besançon Observatory, France G. PATUREL and I. VAUGLIN, Lyons Observatory, France T. FORVEILLE and X. DELFOSSE, Grenoble Observatory, France J. HRON and M. SCHULTHEIS, Vienna Observatory, Austria I. APPENZELLER AND S. WAGNER, Landessternwarte, Heidelberg, Germany L. BALAZS and A. HOLL, Konkoly Observatory, Budapest, Hungary J. LÉPINE, P. BOSCOLO, E. PICAZZIO, University of São Paulo, Brazil P.-A. DUC, European Southern Observatory, Garching, Germany M.-O. MENNESSIER, University of Montpellier, France 1. The DENIS Project celestial objects and unknown physical efforts which led to a proposal for the processes. DENIS project, aimed at covering the Since the middle of 1994, the ESO The 2.2-micron window is of particular entire southern sky from the ESO site at 1-metre telescope has been dedicated astrophysical interest. It is the longest La Silla, making full-time use of the ESO on a full-time basis to a long-term project wavelength window not much hampered 1-metre telescope.