Pivotal Role of Spin in Celestial Body Motion Mechanics: Prelude to a Spinning Universe
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Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
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A&A 583, A85 (2015) Astronomy DOI: 10.1051/0004-6361/201526795 & c ESO 2015 Astrophysics Reaching the boundary between stellar kinematic groups and very wide binaries III. Sixteen new stars and eight new wide systems in the β Pictoris moving group F. J. Alonso-Floriano1, J. A. Caballero2, M. Cortés-Contreras1,E.Solano2,3, and D. Montes1 1 Departamento de Astrofísica y Ciencias de la Atmósfera, Facultad de Ciencias Físicas, Universidad Complutense de Madrid, 28040 Madrid, Spain e-mail: [email protected] 2 Centro de Astrobiología (CSIC-INTA), ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain 3 Spanish Virtual Observatory, ESAC PO box 78, 28691 Villanueva de la Cañada, Madrid, Spain Received 19 June 2015 / Accepted 8 August 2015 ABSTRACT Aims. We look for common proper motion companions to stars of the nearby young β Pictoris moving group. Methods. First, we compiled a list of 185 β Pictoris members and candidate members from 35 representative works. Next, we used the Aladin and STILTS virtual observatory tools and the PPMXL proper motion and Washington Double Star catalogues to look for companion candidates. The resulting potential companions were subjects of a dedicated astro-photometric follow-up using public data from all-sky surveys. After discarding 67 sources by proper motion and 31 by colour-magnitude diagrams, we obtained a final list of 36 common proper motion systems. The binding energy of two of them is perhaps too small to be considered physically bound. Results. Of the 36 pairs and multiple systems, eight are new, 16 have only one stellar component previously classified as a β Pictoris member, and three have secondaries at or below the hydrogen-burning limit. -
NEWSLETTER August 2015
NEWSLETTER August 2015 New Horizons at Pluto Credit NASA This space is reserved for promoting member's businesses. You can place an advert here for a donation to the group. Issue 11 August 2015 Page 1 Contents Cover 1 Contents 2 About the cover picture New Horizons 3-7 Thanet Astronomy Group Contact Details 8 Member's Meeting Dates and Times 9 Advertisement (West Bay Cafe) 10 What we did last month 11 Junior Members Page 12 Advertisement (Renaissance Glass) 13 Book Review 14 What's in the sky this month 15-17 Member's Page 18-19 Did You Know ? 20 Junior Astronomers Club (JAC & Gill) 21 Executive Committee Messages 22 Adult Word Search 23 Junior Word Search 24 Member's For Sale and Wanted 25 Issue 11 August 2015 Page 2 About the Cover Picture NEW HORIZONS New Horizons at Pluto Credit NASA New Horizons The Mission The New Horizons mission is the first mission to Pluto and the Kuiper Belt This mission has sent a space craft to the outer reaches of our Solar System to look at the dwarf planet Pluto, and beyond into the Kuiper Belt. The Kuiper Belt is the region of our Solar System beyond the orbit of the planet Neptune, about 30 Astronomical Units (AU) from the Sun and out to about 50 AU. This region contains the minor planet Pluto and its moons Charon, Hydra, Nix and Styx along with many comets, asteroids and many other small objects mostly made of ice. The Kuiper Belt - Credit: NASA Issue 11 August 2015 Page 3 About the Cover Picture NEW HORIZONS An AU or Astronomical Unit is equal to the distance between the Sun and the Earth about 93,000,000 miles or 150,000,000 km. -
Information Bulletin on Variable Stars
COMMISSIONS AND OF THE I A U INFORMATION BULLETIN ON VARIABLE STARS Nos November July EDITORS L SZABADOS K OLAH TECHNICAL EDITOR A HOLL TYPESETTING K ORI ADMINISTRATION Zs KOVARI EDITORIAL BOARD L A BALONA M BREGER E BUDDING M deGROOT E GUINAN D S HALL P HARMANEC M JERZYKIEWICZ K C LEUNG M RODONO N N SAMUS J SMAK C STERKEN Chair H BUDAPEST XI I Box HUNGARY URL httpwwwkonkolyhuIBVSIBVShtml HU ISSN COPYRIGHT NOTICE IBVS is published on b ehalf of the th and nd Commissions of the IAU by the Konkoly Observatory Budap est Hungary Individual issues could b e downloaded for scientic and educational purp oses free of charge Bibliographic information of the recent issues could b e entered to indexing sys tems No IBVS issues may b e stored in a public retrieval system in any form or by any means electronic or otherwise without the prior written p ermission of the publishers Prior written p ermission of the publishers is required for entering IBVS issues to an electronic indexing or bibliographic system to o CONTENTS C STERKEN A JONES B VOS I ZEGELAAR AM van GENDEREN M de GROOT On the Cyclicity of the S Dor Phases in AG Carinae ::::::::::::::::::::::::::::::::::::::::::::::::::: : J BOROVICKA L SAROUNOVA The Period and Lightcurve of NSV ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::: W LILLER AF JONES A New Very Long Period Variable Star in Norma ::::::::::::::::::::::::::::::::::::::::::::::::::: :::::::::::::::: EA KARITSKAYA VP GORANSKIJ Unusual Fading of V Cygni Cyg X in Early November ::::::::::::::::::::::::::::::::::::::: -
Arxiv:1603.08040V2 [Astro-Ph.SR] 16 Apr 2016 Visible to the Satellite
Submitted to The Astrophysical Journal Preprint typeset using LATEX style emulateapj v. 5/2/11 THE ALLWISE MOTION SURVEY, PART 2 J. Davy Kirkpatrick1, Kendra Kellogg1,2, Adam C. Schneider3, Sergio Fajardo-Acosta1, Michael C. Cushing3, Jennifer Greco3, Gregory N. Mace4, Christopher R. Gelino1, Edward L. Wright5, Peter R. M. Eisenhardt6, Daniel Stern6, Jacqueline K. Faherty7, Scott S. Sheppard7, George B. Lansbury8, Sarah E. Logsdon5, Emily C. Martin5, Ian S. McLean5, Steven D. Schurr1, Roc M. Cutri1, Tim Conrow1 Submitted to The Astrophysical Journal ABSTRACT We use the AllWISE Data Release to continue our search for WISE-detected motions. In this paper, we publish another 27,846 motion objects, bringing the total number to 48,000 when objects found during our original AllWISE motion survey are included. We use this list, along with the lists of confirmed WISE-based motion objects from the recent papers by Luhman and by Schneider et al. and candidate motion objects from the recent paper by Gagn´eet al. to search for widely separated, common-proper-motion systems. We identify 1,039 such candidate systems. All 48,000 objects are further analyzed using color-color and color-mag plots to provide possible characterizations prior to spectroscopic follow-up. We present spectra of 172 of these, supplemented with new spectra of 23 comparison objects from the literature, and provide classifications and physical interpretations of interesting sources. Highlights include: (1) the identification of three G/K dwarfs that can be used as standard candles -
Una Aproximación Física Al Universo Local De Nebadon
4 1 0 2 local Nebadon de Santiago RodríguezSantiago Hernández Una aproximación física al universo (160.1) 14:5.11 La curiosidad — el espíritu de investigación, el estímulo del descubrimiento, el impulso a la exploración — forma parte de la dotación innata y divina de las criaturas evolutivas del espacio. Tabla de contenido 1.-Descripción científica de nuestro entorno cósmico. ............................................................................. 3 1.1 Lo que nuestros ojos ven. ................................................................................................................ 3 1.2 Lo que la ciencia establece ............................................................................................................... 4 2.-Descripción del LU de nuestro entorno cósmico. ................................................................................ 10 2.1 Universo Maestro ........................................................................................................................... 10 2.2 Gran Universo. Nivel Espacial Superunivesal ................................................................................. 13 2.3 Orvonton. El Séptimo Superuniverso. ............................................................................................ 14 2.4 En el interior de Orvonton. En la Vía Láctea. ................................................................................. 18 2.5 En el interior de Orvonton. Splandon el 5º Sector Mayor ............................................................ 19 -
Incidental Tables
Sp.-V/AQuan/1999/10/27:16:16 Page 667 Chapter 27 Incidental Tables Alan D. Fiala, William F. Van Altena, Stephen T. Ridgway, and Roger W. Sinnott 27.1 The Julian Date ...................... 667 27.2 Standard Epochs ...................... 668 27.3 Reduction for Precession ................. 669 27.4 Solar Coordinates and Related Quantities ....... 670 27.5 Constellations ....................... 672 27.6 The Messier Objects .................... 674 27.7 Astrometry ......................... 677 27.8 Optical and Infrared Interferometry ........... 687 27.9 The World’s Largest Optical Telescopes ........ 689 27.1 THE JULIAN DATE by A.D. Fiala The Julian Day Number (JD) is a sequential count that begins at Noon 1 Jan. 4713 B.C. Julian Calendar. 27.1.1 Julian Dates of Specific Years Noon 1 Jan. 4713 B.C. = JD 0.0 Noon 1 Jan. 1 B.C. = Noon 1 Jan. 0 A.D. = JD 172 1058.0 Noon 1 Jan. 1 A.D. = JD 172 1424.0 A Modified Julian Day (MJD) is defined as JD − 240 0000.5. Table 27.1 gives the Julian Day of some centennial and decennial dates in the Gregorian Calendar. 667 Sp.-V/AQuan/1999/10/27:16:16 Page 668 668 / 27 INCIDENTAL TABLES Table 27.1. Julian date of selected years in the Gregorian calendar [1, 2]. Julian day at noon (UT) on 0 January, Gregorian calendar Jan. 0.5 JD Jan. 0.5 JD Jan. 0.5 JD Jan. 0.5 JD 1500 226 8923 1910 241 8672 1960 243 6934 2010 245 5197 1600 230 5447 1920 242 2324 1970 244 0587 2020 245 8849 1700 234 1972 1930 242 5977 1980 244 4239 2030 246 2502 1800 237 8496 1940 242 9629 1990 244 7892 2040 246 6154 1900 241 5020 1950 243 3282 2000 245 1544 2050 246 9807 Century years evenly divisible by 400 (e.g., 1600, 2000) are leap years. -
Uncovering the Orbit of the Hercules Dwarf Galaxy
MNRAS 000,1{15 (2019) Preprint 3 December 2019 Compiled using MNRAS LATEX style file v3.0 Uncovering the Orbit of the Hercules Dwarf Galaxy Alexandra L. Gregory1?, Michelle L. M. Collins1, Denis Erkal1, Erik Tollerud2, Maxime Delorme1, Lewis Hill1, David J. Sand3, Jay Strader4 Beth Willman5, 1Department of Physics, University of Surrey, Guildford, GU2 7XH, Surrey, UK 2Space Telescope Science Institute, 3700 San Martin Dr, Baltimore, MD 21218, USA 3Department of Astronomy/Steward Observatory, 933 North Cherry Avenue, Rm. N204, Tucson, AZ 85721-0065, USA 4Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 5National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Avenue, Tucson, AZ 85719, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We present new chemo{kinematics of the Hercules dwarf galaxy based on Keck II{ DEIMOS spectroscopy. Our 21 confirmed members have a systemic velocity of vHerc = −1 +1:4 −1 46:4 1:3 kms and a velocity dispersion σv;Herc = 4:4−1:2 kms . From the strength of the± Ca II triplet, we obtain a metallicity of [Fe/H]= 2:48 0:19 dex and dispersion +0:18 − ± of σ[Fe=H] = 0:63−0:13 dex. This makes Hercules a particularly metal{poor galaxy, placing it slightly below the standard mass{metallicity relation. Previous photometric and spectroscopic evidence suggests that Hercules is tidally disrupting and may be on a highly radial orbit. From our identified members, we measure no significant velocity gradient. By cross{matching with the second Gaia data release, we determine an ∗ uncertainty{weighted mean proper motion of µα = µα cos(δ) = 0:153 0:074 mas −1 −1 − ± yr , µδ = 0:397 0:063 mas yr . -
1. Which of the Following Statements Is Incorrect Concerning Sidereal Days and Solar Days?
1. Which of the following statements is incorrect concerning sidereal days and solar days? A. One sidereal day is defined as the time taken for the Earth to make one complete rotation on its axis B. One sidereal day is 3.9 minutes longer than one solar day C. The time difference between one sidereal day and one solar day accounts for the daily slight shift in the position of stars D. The time difference between one sidereal day and one solar day is due to the simultaneous rotation of the Earth about its axis and the revolution of Earth around the Sun 2. The Earth’s aphelion is the position of the Earth on its orbit that is most distant from the Sun. At which time of the year is the Earth furthest from the Sun? A. 3 January B. 21 June C. 3 July D. 21 December 3. Which of the following statements is incorrect regarding solar eclipses? A. During a total solar eclipse, the corona of the Sun becomes visible. B. If the umbra region of the eclipse does not reach the Earth, an annular eclipse will be seen C. A solar eclipse track on Earth runs from the west to the east D. An eclipse that occurred in December 4, 2002 will be seen again in December 14, 2018, in accordance with the Saros cycle 4. The Milankovitch cycles concern about the movement of Earth on its axis and its orbit around the Sun. These cycles include the Earth’s orbit eccentricity, its precession period and its obliquity. -
195 9Apj. . .130. .629B the HERCULES CLUSTER OF
.629B THE HERCULES CLUSTER OF NEBULAE* .130. G. R. Burbidge and E. Margaret Burbidge 9ApJ. Yerkes and McDonald Observatories Received March 26, 1959 195 ABSTRACT The northern of two clusters of nebulae in Hercules, first listed by Shapley in 1933, is an irregular group of about 75 bright nebulae and a larger number of faint ones, distributed over an area about Io X 40'. A set of plates of parts of this cluster, taken by Dr. Walter Baade with the 200-inch Hale reflector, is shown and described. More than three-quarters of the bright nebulae have been classified, and, of these, 69 per cent are spirals or irregulars and 31 per cent elliptical or SO. Radial velocities for 7 nebulae were obtained by Humason, and 10 have been obtained by us with the 82-inch reflector. The mean red shift is 10775 km/sec. From this sample, the total kinetic energy of the nebulae has been esti- mated. By measuring the distances between all pairs on a 48-inch Schmidt enlargement, the total poten- tial energy has been estimated. From these results it is concluded that, if the cluster is to be in a stationary state, the average galactic mass must be ^1012Mo. Three possibilities are discussed: that the masses are indeed as large as this, that there is a large amount of intergalactic matter, and that the cluster is expanding. The data for the Coma and Virgo clusters are also reviewed. It is concluded that both the Hercules and the Virgo clusters are probably expanding, but the situation is uncertain in the case of the Coma cluster. -
Radio Investigations of Clusters of Galaxies
• • RADIO INVESTIGATIONS OF CLUSTERS OF GALAXIES a study of radio luminosity functions, wide-angle head-tailed radio galaxies and cluster radio haloes with the Westerbork Synthesis Radio Telescope proefschrift ter verkrijging van degraad van Doctor in de Wiskunde en Natuurwetenschappen aan de Rijksuniversiteit te Leiden, op gezag van de Rector Magnificus Or. D.J. Kuenen, hoogleraar in de Faculteit der Wiskunde en Natuurwetenschappen, volgens besluit van het College van Dekanen te verdedigen op woensdag 20 december 1978 teklokke 15.15 uur door Edwin Auguste Valentijn geboren te Voorburg in 1952 Sterrewacht Leiden 1978 elve/labor vincit - Leiden Promotor: Prof. Dr. H. van der Laan aan Josephine aan mijn ouders Cover: Some radio contours (1415 MHz) of the extended radio galaxies NGC6034, NGC6061 and 1B00+1SW2 superimposed to a smoothed galaxy distribution (number of galaxies per unit area, taken from Shane) of the Hercules Superoluster. The 90 % confidence error boxes of the Ariel VandUHURU observations of the X-ray source A1600+16 are also included. In the region of overlap of these two error boxes the position of a oD galaxy is indicated. The combined picture suggests inter-galactic material pervading the whole superaluster. CONTENTS CHAPTER 1 GENERAL INTRODUCTION AND SUMMARY 9 PART 1 OBSERVATIONS OF THE COI1A CLUSTER AT 610 MHZ 15 CHAPTER 2 COMA CLUSTER GALAXIES 17 Observation of the Coma Cluster at 610 MHz (Paper III, with W.J. Jaffe and G.C. Perola) I Introduction 17 II Observations 18 III Data Reduction 18 IV Radio Source Parameters 19 V Optical Data 20 VI The Radio Luminosity Function of the Coma Cluster Galaxies 21 a) LF of the (E+SO) Galaxies 23 b) LF of the (S+I) Galaxies 25 c) Radial Dependence of the LF 26 VII Other Properties of the Detected Cluster Galaxies 26 a) Spectral Indexes b) Emission Lines VIII The Central Radio Sources 27 a) 5C4.85 = NGC4874 27 b) 5C4.8I - NGC4869 28 c) Coma C 29 CHAPTER 3 RADIO SOURCES IN COMA NOT IDENTIFIED WITH CLUSTER GALAXIES 31 Radio Data and Identifications (Paper IV, with G.C. -
Gaia DR2 White Dwarfs in the Hercules Stream Santiago Torres1,2, Carles Cantero1, María E
A&A 629, L6 (2019) Astronomy https://doi.org/10.1051/0004-6361/201936244 & c ESO 2019 Astrophysics LETTER TO THE EDITOR Gaia DR2 white dwarfs in the Hercules stream Santiago Torres1,2, Carles Cantero1, María E. Camisassa3,4, Teresa Antoja5, Alberto Rebassa-Mansergas1,2, Leandro G. Althaus3,4, Thomas Thelemaque6, and Héctor Cánovas7 1 Departament de Física, Universitat Politècnica de Catalunya, c/Esteve Terrades 5, 08860 Castelldefels, Spain e-mail: [email protected] 2 Institute for Space Studies of Catalonia, c/Gran Capità 2-4, Edif. Nexus 104, 08034 Barcelona, Spain 3 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Paseo del Bosque s/n, 1900 La Plata, Argentina 4 Instituto de Astrofísica de La Plata, UNLP-CONICET, Paseo del Bosque s/n, 1900 La Plata, Argentina 5 Institut de Ciències del Cosmos, Universitat de Barcelona (IEEC-UB), Martí i Franquès 1, 08028 Barcelona, Spain 6 Industrial and Informatic Systems Deparment, EPF - École d’Ingénieurs, 21 boulevard Berthelot, 34000 Montpellier, France 7 European Space Astronomy Centre (ESA/ESAC), Operations Deparment, Villanueva de la Cañada, 28692 Madrid, Spain Received 5 July 2019 / Accepted 7 August 2019 ABSTRACT Aims. We analyzed the velocity space of the thin- and thick-disk Gaia white dwarf population within 100 pc by searching for signatures of the Hercules stellar stream. We aimed to identify objects belonging to the Hercules stream, and by taking advantage of white dwarf stars as reliable cosmochronometers, to derive a first age distribution. Methods. We applied a kernel density estimation to the UV velocity space of white dwarfs.