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And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
History of Telescopes
1 OUR PLACE IN SPACE Earth: Earth is the third planet from the Sun, and the densest and fifth- largest of the eight planets in the Solar System. It is also the largest of the Solar System’s four terrestrial planets. The Solar System : The Solar System consists of the Sun and those celestial objects bound to it by gravity, all of which were formed from the collapse of a giant molecular cloud approximately 4.6 billion years ago. Of the many objects that orbit the Sun, most of the mass is contained within eight relatively solitary planets whose orbits are almost circular and lie within a nearly flat disc called the ecliptic plane. The four smaller inner planets, Mercury, Venus, Earth and Mars, also called the terrestrial planets, are primarily composed of rock and metal. The four outer planets, the gas giants, are substantially more massive than the terrestrials. They are Jupiter, Saturn, Uranus and Neptune. The Sun: The Sun is the star at the center of the Solar System. It has a diameter of about 1,392,000 kilometers about 109 times that of Earth, and its mass (about 2 × 1030 kilograms, 330,000 times that of Earth) accounts for about 99.86% of the total mass of the Solar System. The Milky way Galaxy: The Milky Way Galaxy is the galaxy in which the Solar System is located. The Milky Way is a barred spiral galaxy that is part of the Local Group of galaxies. It is one of billions of galaxies in the observable universe. The Local Group: The Local Group is the group of galaxies that includes our galaxy, the Milky Way. -
Mirando El Cielo
1 Mirando el cielo Guillermo Sánchez (http://diarium.usal.es/guillermo) Última actualización: 2013-05-11 1.0. Sobre la elaboración es este artículo. Todos los cálculos realizados para elaborar este artículo están realizados con el programa Mathematica , sin embargo Ud no los verá. A veces observará que algún texto aparece en inglés esto es debido a que se muestra directamente el resultado de la salida del programa. Si está interesado en el uso de este programa en cálculos astrónomicos y otros muchos campos puede visitar: http://diarium.usal.es/guillermo/mathematica/ . 1.1. La época dorada de la astronomía y cosmología La contemplación del cielo una noche estrellada, lejos de la contaminación lumínica, es uno de los espectáculos más sobrecogedores del que se puede disfrutar. No es extraño que durante milenios los seres humanos observasen el cielo y se diesen cuenta de que el Sol y la Luna siguen ciclos regulares. La mayoría de las culturas hicieron interpretaciones mitológicas o religiosas de los astros pero también los utilizaron con un sentido práctico, para el establecimiento de calendarios que sirvieron, entre otras cosas, para planificar las cosechas. Por ejemplo, los egipcios asociaban la aparición de Sirio, la estrella más brillante del hemisferio norte (ahora sabemos es un sistema binario), como preludio de la crecida del Nilo. El advenimiento del telescopio hace poco más de 400 años (1609): el número de astros observables paso de tres o cuatro mil astros, que se observan a simple vista, a miles de millones; la luna lejos de ser una esfera perfecta pues estaba cubierta de montañas y cráteres; las estrellas errantes (los planetas) no eran simples puntos de luz, tenían satélites y alguno hasta estaba rodeado de un anillo. -
Stellar Populations at the Center of Ic 16131 Andrew A
THE ASTRONOMICAL JOURNAL, 118:1657È1670, 1999 October ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. STELLAR POPULATIONS AT THE CENTER OF IC 16131 ANDREW A. COLE,2 ELINE TOLSTOY,3 JOHN S. GALLAGHER III,2 JOHN G. HOESSEL,2 JEREMY R. MOULD,4 JON A. HOLTZMAN,5 ABHIJIT SAHA,6 GILDA E. BALLESTER,7 CHRISTOPHER J. BURROWS,8,9 JOHN T. CLARKE,7 DAVID CRISP,10 RICHARD E. GRIFFITHS,11 CARL J. GRILLMAIR,12 JEFF J. HESTER,13 JOHN E. KRIST,8 VIKKI MEADOWS,10 PAUL A. SCOWEN,13 KARL R. STAPELFELDT,10 JOHN T. TRAUGER,10 ALAN M. WATSON,14 AND JAMES R. WESTPHAL15 Received 1999 March 29; accepted 1999 May 26 ABSTRACT We have observed the center of the Local Group dwarf irregular galaxy IC 1613 with the WFPC2 aboard the Hubble Space Telescope in the F439W, F555W, and F814W Ðlters. We analyze the resulting color-magnitude diagrams (CMDs) using the main-sequence and giant-branch luminosity functions and comparisons with theoretical stellar models to derive a preliminary star formation history for this galaxy. We Ðnd a dominant old stellar population (age B7 Gyr), identiÐable by the strong red giant branch (RGB) and red clump populations. From the (V [I) color of the RGB, we estimate a mean metallicity of the intermediate-age stellar population [Fe/H] \[1.38 ^ 0.31. We conÐrm a distance of 715 ^ 40 kpc using the I magnitude of the RGB tip. The main-sequence luminosity function down to I B 25 provides ] ~4 ~1 evidence for a roughly constant star formation rate (SFR) of approximately 3.5 10 M_ yr across the WFPC2 Ðeld of view (0.22 kpc2) during the past 250È350 Myr. -
The Galaxies of the Local Group Sidney Van Den Bergh Frontmatter More Information
Cambridge University Press 978-0-521-03743-3 - The Galaxies of the Local Group Sidney van den Bergh Frontmatter More information The Local Group is a small cluster of galaxies of which 35 members are currently known, including the Milky Way. It is believed that at least half of all galaxies in the Universe belong to similar groups. Galaxies of the Local Group can be used as “stepping stones” to determine the distance to more remote galaxies, and thus they help to measure the size and age of the Universe. Studying stars of differing ages in different members of the Local Group allows us to see how galaxies evolve over timescales in excess of 10 billion years. The oldest stars in the Local Group galaxies also provide critical information on the physical conditions of the early Universe. The Local Group thus provides many valuable clues to understanding the rest of the Universe. This authoritative volume provides a comprehensive and up-to-date synthesis of what is currently known about the Local Group of galaxies. It includes a summary of our knowledge of each of the individual member galaxies, as well as those galaxies previously regarded as possible members. After examining each galaxy in detail, the book goes on to examine the mass, stability, and evolution of the Local Group as a whole. The book includes many important previously unpublished results and conclusions. With characteristic clarity, Professor van den Bergh provides in this book a mas- terful summary of all that is known about the galaxies of the Local Group and their evolution, and he expertly places this knowledge in the wider context of ongoing studies of galaxy formation and evolution, the cosmic distance scale, and the condi- tions in the early Universe. -
November 2020 BRAS Newsletter
A Mars efter Lowell's Glober ca. 1905-1909”, from Percival Lowell’s maps; National Maritime Museum, Greenwich, London (see Page 6) Monthly Meeting November 9th at 7:00 PM, via Jitsi (Monthly meetings are on 2nd Mondays at Highland Road Park Observatory, temporarily during quarantine at meet.jit.si/BRASMeets). GUEST SPEAKER: Chuck Allen from the Astronomical League will speak about The Cosmic Distance Ladder, which explores the historical advancement of distance determinations in astronomy. What's In This Issue? President’s Message Member Meeting Minutes Business Meeting Minutes Outreach Report Asteroid and Comet News Light Pollution Committee Report Globe at Night Member’s Corner – John Nagle ALPO 2020 Conference Astro-Photos by BRAS Members - MARS Messages from the HRPO REMOTE DISCUSSION Solar Viewing Edge of Night Natural Sky Conference Recent Entries in the BRAS Forum Observing Notes: Pisces – The Fishes Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society BRAS YouTube Channel Baton Rouge Astronomical Society Newsletter, Night Visions Page 2 of 24 November 2020 President’s Message Welcome to the home stretch for 2020. The nights are starting earlier and earlier as the weather becomes more and more comfortable and all of our old favorites of the fall and winter skies really start finding their places right where they belong. October was a busy month for us, with several big functions at the Observatory, including two oppositions and two more all night celebrations. By comparison, November is looking fairly calm, the big focus there is going to be our third annual Natural Sky Conference on the 13th, which I’m encouraging people who care about the state of light pollution in our city and the surrounding area to get involved in. -
THE LOCAL GROUP of GALAXIES* Sidney Van Den Bergh
THE LOCAL GROUP OF GALAXIES* Sidney van den Bergh National Research Council of Canada Dominion Astrophysical Observatory Herzberg Institute of Astrophysics 5071 West Saanich Road Victoria, British Columbia, V8X 4M6 Canada e-mail: [email protected] Summary Hubble's (1936, p. 125) view that the Local Group (LG) is "a typical, small group of nebulae which is isolated in the general field" is confirmed by modern data. The total number of certain and probable Group members presently stands at 35. The half-mass radius of the Local Group is found to be Rh . 350 kpc. The zero-velocity surface, which separates the Local Group from the field that is expanding with the Hubble flow, has a radius Ro = 1.18 " 0.15 Mpc. The 12 total mass of the LG is MLG = (2.3 " 0.6) x 10 Mu . Most of this mass appears to be concentrated in the Andromeda and Milky Way subgroups of the LG. The total luminosity of the Local Group is found to be MV = -22.0:. This yields a mass-to-light ratio (in solar units) of M/LV = 44 " 12. The solar motion with respect to the LG is 306 " 18 km s-1 , directed towards an apex at R = 99E " 5E, - 1 and b = -4E " 4E. The velocity dispersion within the LG is Fr = 61 " 8 km s . The galaxies NGC 3109, Antlia, Sextans A and Sextans B appear to form a distinct grouping with Vr = +114 " 12 kpc relative to the LG, that is located * Based, in part, on a series of lectures given at the University of Victoria in the early spring of 1999. -
The Galaxies of the Local Group Sidney Van Den Bergh Index More Information
Cambridge University Press 978-0-521-03743-3 - The Galaxies of the Local Group Sidney van den Bergh Index More information Object Index 30 Doradus, 49, 88, 99, 100, 101, 108, 110, 112–116, DDO 155, 263 121, 124, 131, 134, 135, 139 DDO 187, 263, 279 47 Tucanae, see NGC 104 DDO 210, 5, 7, 194–195, 280, 288 287.5 + 22.5 + 240, 139, 161 DDO 216, 5, 6, 7, 174, 192–194, 280 AE And, 37 DDO 221, 174, 188–191, 280 AF And, see M31V19 DEM 71, 132 Alpha UMi, see Polaris DEM L316, 133 AM 1013-394A, 270, 272 Draco dwarf, 5, 58, 137, 185, 231, 249–252, 256, 259, And I, 5, 234, 235, 236, 237, 242, 280 262, 280 And II, 5, 7, 234, 236, 237, 238, 240, 242, 280 And III, 5, 234, 236, 237, 238, 240, 242, 280 EGB 0419 + 72, 270 And IV, 234 EGB 0427 + 63, see UGC-A92 And V, 5, 7, 237–240, 242, 280 Eridanus, 58, 64, 229 And VI, 5, 7, 240, 241, 242, 280 ESO 121-SC03, 103, 104, 124, 125, 161, 162 And VII, 5, 7, 241, 242, 280 ESO 249-010, 264 Andromeda galaxy, see M31 ESO 439-26, 55 Antlia dwarf, 265–267, 270, 272 Eta Carinae, 37 Aquarius dwarf, see DDO 210 AqrDIG, see DDO 210 F8D1, 2 Arches cluster, see G0.121+0.017 Fornax clusters 1–6, 222, 223, 224 Arp 2, 58, 64, 161, 226, 227, 228, 230, 232 Fornax dwarf 5, 94, 167, 219–226, 231, 256, 259, 260, Arp 220, 113 262, 280 B 327, 24 G 1, 27, 32, 34, 35, 45 BD +40◦ 147, 164 G 105, 35 BD +40◦ 148, 12 G 185, 31 Berkeley 17, 54 G 219, 27, 32 Berkeley 21, 56 G 280, 32 G0.7-0.0, see Sgr B2 C1,20 G0.121 + 0.017, 48 C 107, see vdB0 G1.1-0.1, 49 Camelopardalis dwarf, 241, 242 G359.87 + 0.18, 67 Carina dwarf, 5, 245–247, 256, -
The Galaxies of the Local Group
THE GALAXIES OF THE LOCAL GROUP SIDNEY VAN DEN BERGH CAMBRIDGE UNIVERSITY PRESS P1: GKW/UKS P2: GKW/UKS QC: GKW CB240-FM December 4, 1999 14:59 Char Count= 0 THE GALAXIES OF THE LOCAL GROUP i P1: GKW/UKS P2: GKW/UKS QC: GKW CB240-FM December 4, 1999 14:59 Char Count= 0 Cambridge astrophysics series Series editors Andrew King, Douglas Lin, Stephen Maran, Jim Pringle, and Martin Ward Titles available in this series 7. Spectroscopy of Astrophysical Plasmas by A. Dalgarno and D. Layzer 10. Quasar Astronomy by D. W. Weedman 17. Molecular Collisions in the Interstellar Medium by D. Flower 18. Plasma Loops in the Solar Corona by R. J. Bray, L. E. Cram, C. J. Durrant, and R. E. Loughhead 19. Beams and Jets in Astrophysics edited by P. A. Hughes 20. The Observation and Analysis of Stellar Photospheres by David F. Gray 21. Accretion Power in Astrophysics 2nd Edition by J. Frank, A. R. King, and D. J. Raine 22. Gamma-Ray Astronomy 2nd Edition by P. V. Ramana Murthy and A. W. Wolfendale 23. The Solar Transition Region by J. T. Mariska 24. Solar and Stellar Activity Cycles by Peter R. Wilson 25. 3K: The Cosmic Microwave Background Radiation by R. B. Partridge 26. X-Ray Binaries by Walter H. G. Lewin, Jan van Paradijs, and Edward P. J. van den Heuvel 27. RR Lyrae Stars by Horace A. Smith 28. Cataclysmic Variable Stars by Brian Warner 29. The Magellanic Clouds by Bengt E. Westerlund 30. Globular Cluster Systems by Keith M. -
Centralities of Galaxies in the Weighted Network Model of the Local Group
Selforganizology, 2021 Article Centralities of galaxies in the weighted network model of the local group Emir Haliki Department of Physics, Faculty of Science, Ege University, Izmir, Turkey E-mail: [email protected] Received 15 June 2021 Abstract Little is known about the structures and characteristics of the networks behind galaxy clusters. Considering that the essential interaction between the elements of a cluster is the gravitational attraction, the study has modeled the Local Group, a local galaxy cluster of which the Milky Way is a member, as a weighted network according to gravitational attraction. After the galaxies’ unknown masses have been calculated from their apparent and absolute magnitudes, the gravitational attraction matrix, being the adjacency matrix of the network, would be formed from the matrix of their positions relative to each other. Various centrality measurements known as fundamental network metrics were thus performed to determine if the massive galaxies of the cluster have high centrality values. In the proposed weighted network model, direct and indirect correlations have been observed between centrality values and masses of the galaxies. Keywords network; centrality; gravity; Milky Way; Local Group. Selforganizology ISSN 24100080 URL: http://www.iaees.org/publications/journals/selforganizology/onlineversion.asp RSS: http://www.iaees.org/publications/journals/selforganizology/rss.xml Email: [email protected] EditorinChief: WenJun Zhang Publisher: International Academy of Ecology and Environmental Sciences 1 Introduction Examination of the large-scale structure of the universe has been thought with a network model for a while. As large-scale networks are required to be modeled in such investigations, the study of the intergalactic space has been one of the models where galaxies represent nodes. -
The Faint End of the Centaurus a Satellite Luminosity Function
Draft version January 14, 2019 Typeset using LATEX twocolumn style in AASTeX62 The faint end of the Centaurus A satellite luminosity function D. Crnojevic,´ 1,2 D. J. Sand,3 P. Bennet,2 S. Pasetto,4,1 K. Spekkens,5 N. Caldwell,6 P. Guhathakurta,7 B. McLeod,6 A. Seth,8 J. D. Simon,4 J. Strader,9 and E. Toloba10 1University of Tampa, 401 West Kennedy Boulevard, Tampa, FL 33606, USA 2Department of Physics & Astronomy, Texas Tech University, Box 41051, Lubbock, TX 79409-1051, USA 3Department of Astronomy and Steward Observatory, University of Arizona, 933 N Cherry Ave, Tucson, AZ 85719, USA 4Observatories of the Carnegie Institution for Science, 813 Santa Barbara Street, Pasadena, CA 91101, USA 5Department of Physics and Space Science, Royal Military College of Canada, Box 17000, Station Forces, Kingston, ON K7L 7B4, Canada 6Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA 7Department of Astronomy & Astrophysics, UCO/Lick Observatory, University of California Santa Cruz, 1156 High Street, Santa Cruz, CA 95064, USA 8Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA 9Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 10Department of Physics, University of the Pacific, 3601 Pacific Avenue, Stockton, CA 95211, USA ABSTRACT The Panoramic Imaging Survey of Centaurus and Sculptor (PISCeS) is constructing a wide-field map of the resolved stellar populations in the extended halos of these two nearby, prominent galaxies. We present new Magellan/Megacam imaging of a ∼ 3 deg2 area around Centaurus A (Cen A), which filled in much of our coverage to its south, leaving a nearly complete halo map out to a projected radius of ∼150 kpc and allowing us to identify two new resolved dwarf galaxies. -
The Local Group of Galaxies: (What Are They, and How to Observe Them)
The Local Group of Galaxies: (What are They, and How to Observe Them) Introduction: The Local Group,,,,, Over the years, I’ve clipped and saved interesting articles from the various astronomy related magazines that have come and gone, and some that are still with us. One of my favorite ’observing’ oriented publications was the old ‘Deep Sky’ magazine. In their fall 1984 issue there was a detailed article titled “All About M31”, which was about observing the Great Andromeda Galaxy's internal open and globular clusters and M31's attendant satellite galaxies. They followed that up a few years later in the autumn of 1991 with an article on “Observing the Local Group”. I've held on to those issues over the years, wanting someday to do an observing project based on them. Then more recently both ‘Astronomy’ magazine 'Sky and Telescope' came out with a number of great observing articles on other ‘Local Group’ themed topics such as the December 2013 Sky & Telescope issue - "Exploring the Triangulum Galaxy", and "Local Group Dwarf Galaxies" , and the entire March 2019 issue of ‘Astronomy’ about galaxies. It was that December 2013 Sky& Tel issue that inspired me to finally start an observing project in the spring of 2014 to explore our Local Group of galaxies. So I started diving into these articles with their photographs and finder charts, comparing with what I've observed or video-captured over the years. I was able to identify a number of extra-galactic globular clusters and H-II regions in M31 & M33, along with already having several additional Local Group members video-imaged.