Dwarf Galaxies Between Galaxy Clusters

Total Page:16

File Type:pdf, Size:1020Kb

Dwarf Galaxies Between Galaxy Clusters research highlights SPECTROMETRY COMPLEX NETWORKS To better understand the structure and Connect the dots Bring the noise dynamics of galaxies, Noam Libeskind and Nature 523, 67–70 (2015) Nature Commun. (in the press); preprint at co-workers use the Cosmicflows-2 survey http://arxiv.org/abs/1408.1168 (2015) of peculiar velocities to map the movement NPG of local galaxies out to 150 parsecs. They The Black Death spread across Europe find a filament of dark matter bridging the leaving few in its wake, so it’s natural to Local Group and the massive Virgo cluster think about it as a wave of devastation. roughly 50 million light years away. It is But spare a thought for how it might have simultaneously being stretched by the travelled, had the afflicted been able to hop Virgo cluster and squeezed by the Local Void on an airplane: long-distance flights foster plus smaller voids from the sides. the appearance of clusters in the spatial This dark matter ‘superhighway’ channels evolution of a contagion, with potentially dwarf galaxies between galaxy clusters. more disastrous consequences. And now, Other studies have revealed that dwarf Dane Taylor and colleagues have used a well- galaxies are often compressed into planes known model to map contagions in space, that are possibly co-rotating. The authors showcasing a technique for predicting — show that four out of the five vast planes of and perhaps controlling — spreading on dwarf galaxies are aligned with the main complex networks. direction of compression (and the direction Many networks are connected by of expansion of the Local Void). This How many scientists would love to have a spatially constrained edges (like roads connection between large-and small-scale small and cheap spectrometer? Jie Bao and on a map, for example), but may also structures will help refine models, such as the Moungi Bawendi have come up with a solution incorporate additional edges connecting prevailing cold dark matter model. MC by integrating almost two-hundred absorptive distant nodes. Taylor et al. cast these long- filter arrays made of colloidal quantum dots range connections as a source of noise RANDOM WALKS and a charge-coupled device detector into a in an otherwise geometric network, and Competitive advantage coin-sized digital camera capable of resolving observed two competing phenomena: Phys. Rev. E 91, 062815 (2015) spectral peaks separated by mere nanometres. wavefront propagation on the underlying Such resolution and compactness may find geometric network, and the formation of Many a statistical physicist looking for applications in medicine or space exploration. clusters due to the noisy edges. Within their stochastic processes to study will have Colloidal quantum dots can be thought model, the team found regimes in which considered competitive team sports and of as artificial atoms whose absorption and the spreading was almost unaffected by the wondered about the dynamics at play, and emission properties can be designed during noise edges — hinting at a possible means of perhaps even thought about how they fabrication by controlling their size and contagion control. AK might best be modelled and understood. composition. This flexibility allowed Bao and Appreciating their complexity is one thing, Bawendi to create 195 unique broadband DWARF GALAXIES but making meaningful insights that filters covering a spectral range of 300 nm. Plane speaking might translate into quantitative predictive The spectrum was efficiently reconstructed by Mon. Not. R. Astron. Soc. 452, 1052–1059 (2015) capability is altogether more challenging. measuring a set of light intensities in parallel Aaron Clauset and colleagues have with an array detector whose elements were Matter, as well as dark matter, is not focused on a simple, yet decisive, each set to one filter. uniformly distributed throughout the characteristic of sporting contests, namely Besides their minimal size and cost, one Universe. There are clumps, filaments and the times in a game when the lead changes. advantage of these spectrometers is the voids, for example, the Local Void — a vast Using random walk theory, they showed that possibility to enhance spectral resolution and emptiness — near our own Local Group the number of lead changes in any individual range simultaneously — simply by adding of galaxies that includes the Milky Way, game follows a Gaussian distribution. more dots. IG Andromeda and many dwarf galaxies. More surprisingly, they also show that the probability that the last lead will change and VALLEYTRONICS the time when the largest lead size occurs follow the same bimodal distribution that Jump across Phys. Rev. Appl. 4, 014002 (2015) diverges at the start and the end of the game. Finally, they evaluated the probability that The electronic band structure of certain semiconductors can contain conically shaped valleys. any given lead is ‘safe’ and maintained until When there are two non-equivalent valleys, such as in graphene, the system has an additional the game is over. quantum number, known as the valley index. In much the same way that the electron spin is Most importantly for sports fans, the used in spintronic devices, valleytronic devices aim to make use of the valley index. authors demonstrated a good agreement Many of the materials that offer this valley degree of freedom are single layers, but how do with an exhaustive body of empirical data, these valley electronic states move between layers? Ryosuke Akashi and colleagues have now particularly in the case of professional shown that the stacking geometry can control how many dimensions the valley states travel in. basketball, where the number of scoring Using monolayers of a typical transition metal dichalcogenide, the authors showed that the events in each game is very high. Sport isn’t motion of valley electronic states was confined to just one of the two-dimensional monolayers random; it’s a random walk. AT for a particular type of stacking, known as 3R stacking. For 2H stacking, on the other hand, the valley states could jump between different monolayers, and travel in three dimensions. LF Written by May Chiao, Luke Fleet, Iulia Georgescu, Abigail Klopper and Andrea Taroni . 620 NATURE PHYSICS | VOL 11 | AUGUST 2015 | www.nature.com/naturephysics © 2015 Macmillan Publishers Limited. All rights reserved.
Recommended publications
  • Cosmicflows-3: Cosmography of the Local Void
    Draft version May 22, 2019 Preprint typeset using LATEX style AASTeX6 v. 1.0 COSMICFLOWS-3: COSMOGRAPHY OF THE LOCAL VOID R. Brent Tully, Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA Daniel Pomarede` Institut de Recherche sur les Lois Fondamentales de l'Univers, CEA, Universite' Paris-Saclay, 91191 Gif-sur-Yvette, France Romain Graziani University of Lyon, UCB Lyon 1, CNRS/IN2P3, IPN Lyon, France Hel´ ene` M. Courtois University of Lyon, UCB Lyon 1, CNRS/IN2P3, IPN Lyon, France Yehuda Hoffman Racah Institute of Physics, Hebrew University, Jerusalem, 91904 Israel Edward J. Shaya University of Maryland, Astronomy Department, College Park, MD 20743, USA ABSTRACT Cosmicflows-3 distances and inferred peculiar velocities of galaxies have permitted the reconstruction of the structure of over and under densities within the volume extending to 0:05c. This study focuses on the under dense regions, particularly the Local Void that lies largely in the zone of obscuration and consequently has received limited attention. Major over dense structures that bound the Local Void are the Perseus-Pisces and Norma-Pavo-Indus filaments sepa- rated by 8,500 km s−1. The void network of the universe is interconnected and void passages are found from the Local Void to the adjacent very large Hercules and Sculptor voids. Minor filaments course through voids. A particularly interesting example connects the Virgo and Perseus clusters, with several substantial galaxies found along the chain in the depths of the Local Void. The Local Void has a substantial dynamical effect, causing a deviant motion of the Local Group of 200 − 250 km s−1.
    [Show full text]
  • The Hestia Project: Simulations of the Local Group
    MNRAS 000,2{20 (2020) Preprint 13 August 2020 Compiled using MNRAS LATEX style file v3.0 The Hestia project: simulations of the Local Group Noam I. Libeskind1;2 Edoardo Carlesi1, Rob J. J. Grand3, Arman Khalatyan1, Alexander Knebe4;5;6, Ruediger Pakmor3, Sergey Pilipenko7, Marcel S. Pawlowski1, Martin Sparre1;8, Elmo Tempel9, Peng Wang1, H´el`ene M. Courtois2, Stefan Gottl¨ober1, Yehuda Hoffman10, Ivan Minchev1, Christoph Pfrommer1, Jenny G. Sorce11;12;1, Volker Springel3, Matthias Steinmetz1, R. Brent Tully13, Mark Vogelsberger14, Gustavo Yepes4;5 1Leibniz-Institut fur¨ Astrophysik Potsdam (AIP), An der Sternwarte 16, D-14482 Potsdam, Germany 2University of Lyon, UCB Lyon 1, CNRS/IN2P3, IUF, IP2I Lyon, France 3Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. 1, D-85748, Garching, Germany 4Departamento de F´ısica Te´orica, M´odulo 15, Facultad de Ciencias, Universidad Aut´onoma de Madrid, 28049 Madrid, Spain 5Centro de Investigaci´on Avanzada en F´ısica Fundamental (CIAFF), Facultad de Ciencias, Universidad Aut´onoma de Madrid, 28049 Madrid, Spain 6International Centre for Radio Astronomy Research, University of Western Australia, 35 Stirling Highway, Crawley, Western Australia 6009, Australia 7P.N. Lebedev Physical Institute of Russian Academy of Sciences, 84/32 Profsojuznaja Street, 117997 Moscow, Russia 8Potsdam University 9Tartu Observatory, University of Tartu, Observatooriumi 1, 61602 T~oravere, Estonia 10Racah Institute of Physics, Hebrew University, Jerusalem 91904, Israel 11Univ. Lyon, ENS de Lyon, Univ. Lyon I, CNRS, Centre de Recherche Astrophysique de Lyon, UMR5574, F-69007, Lyon, France 12Univ Lyon, Univ Lyon-1, Ens de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, F-69230, Saint-Genis-Laval, France 13Institute for Astronomy (IFA), University of Hawaii, 2680 Woodlawn Drive, HI 96822, USA 14Department of Physics, Massachusetts Institute of Technology, Cambridge, MA 02139, USA Accepted | .
    [Show full text]
  • How Fast Can You Go
    Traveling on Earth How fast can you go . Fast walking 2 m/s . Fast running 12 m/s You are always moving, even when you are standing still. Below are some . Automobile 30 m/s speeds to ponder. All values are expressed in meters per second. Japanese Bullet Train 90 m/s . Passenger Aircraft, 737 260 m/s You are Travelling . Concord Supersonic Aircraft 600 m/s . Bullet 760 m/s . Earth's rotation, at North Pole 0 m/s . Earth's rotation, at New York City 354 m/s . Earth's rotation, at the Equator 463 m/s Going to Space . Earth orbiting Sun 29,780 m/s The escape velocity is the minimum speed needed for a free, non-propelled . Sun orbiting Milky Way Galaxy 230,000 m/s object (e.g. bullet) to escape from the gravitational influence of a massive body. It is slower the farther away from the body the object is, and slower . Milky Way moving through space 631,000 m/s for less massive bodies. Your total speed in New York City 891,134 m/s . Earth 11,186 m/s . Moon 2,380 m/s Solar System Objects . Mars 5,030 m/s Planets closer to the Sun travel faster: . Jupiter 60,200 m/s . Mercury orbiting Sun 47,870 m/s . Milky Way (from Sun's orbit) 500,000 m/s . Venus orbiting Sun 35,020 m/s . Earth orbiting Sun 29,780 m/s References . Mars orbiting Sun 24,077 m/s https://en.wikipedia.org/wiki/Galactic_year . Jupiter orbiting Sun 13,070 m/s https://en.wikipedia.org/wiki/Tropical_year .
    [Show full text]
  • Arxiv:1807.06205V1 [Astro-Ph.CO] 17 Jul 2018 1 Introduction2 3 the ΛCDM Model 18 2 the Sky According to Planck 3 3.1 Assumptions Underlying ΛCDM
    Astronomy & Astrophysics manuscript no. ms c ESO 2018 July 18, 2018 Planck 2018 results. I. Overview, and the cosmological legacy of Planck Planck Collaboration: Y. Akrami59;61, F. Arroja63, M. Ashdown69;5, J. Aumont99, C. Baccigalupi81, M. Ballardini22;42, A. J. Banday99;8, R. B. Barreiro64, N. Bartolo31;65, S. Basak88, R. Battye67, K. Benabed57;97, J.-P. Bernard99;8, M. Bersanelli34;46, P. Bielewicz80;8;81, J. J. Bock66;10, 7 12;95 57;92 71;56;57 2;6 45;32;48 42 85 J. R. Bond , J. Borrill , F. R. Bouchet ∗, F. Boulanger , M. Bucher , C. Burigana , R. C. Butler , E. Calabrese , J.-F. Cardoso57, J. Carron24, B. Casaponsa64, A. Challinor60;69;11, H. C. Chiang26;6, L. P. L. Colombo34, C. Combet73, D. Contreras21, B. P. Crill66;10, F. Cuttaia42, P. de Bernardis33, G. de Zotti43;81, J. Delabrouille2, J.-M. Delouis57;97, F.-X. Desert´ 98, E. Di Valentino67, C. Dickinson67, J. M. Diego64, S. Donzelli46;34, O. Dore´66;10, M. Douspis56, A. Ducout57;54, X. Dupac37, G. Efstathiou69;60, F. Elsner77, T. A. Enßlin77, H. K. Eriksen61, E. Falgarone70, Y. Fantaye3;20, J. Fergusson11, R. Fernandez-Cobos64, F. Finelli42;48, F. Forastieri32;49, M. Frailis44, E. Franceschi42, A. Frolov90, S. Galeotta44, S. Galli68, K. Ganga2, R. T. Genova-Santos´ 62;15, M. Gerbino96, T. Ghosh84;9, J. Gonzalez-Nuevo´ 16, K. M. Gorski´ 66;101, S. Gratton69;60, A. Gruppuso42;48, J. E. Gudmundsson96;26, J. Hamann89, W. Handley69;5, F. K. Hansen61, G. Helou10, D. Herranz64, E. Hivon57;97, Z. Huang86, A.
    [Show full text]
  • Local Galaxy Flows Within 5
    A&A 398, 479–491 (2003) Astronomy DOI: 10.1051/0004-6361:20021566 & c ESO 2003 Astrophysics Local galaxy flows within 5 Mpc?;?? I. D. Karachentsev1,D.I.Makarov1;11,M.E.Sharina1;11,A.E.Dolphin2,E.K.Grebel3, D. Geisler4, P. Guhathakurta5;6, P. W. Hodge7, V. E. Karachentseva8, A. Sarajedini9, and P. Seitzer10 1 Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR 369167, Russia 2 Kitt Peak National Observatory, National Optical Astronomy Observatories, PO Box 26732, Tucson, AZ 85726, USA 3 Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany 4 Departamento de F´ısica, Grupo de Astronom´ıa, Universidad de Concepci´on, Casilla 160-C, Concepci´on, Chile 5 Herzberg Fellow, Herzberg Institute of Astrophysics, 5071 W. Saanich Road, Victoria, B.C. V9E 2E7, Canada 6 Permanent address: UCO/Lick Observatory, University of California at Santa Cruz, Santa Cruz, CA 95064, USA 7 Department of Astronomy, University of Washington, Box 351580, Seattle, WA 98195, USA 8 Astronomical Observatory of Kiev University, 04053, Observatorna 3, Kiev, Ukraine 9 Department of Astronomy, University of Florida, Gainesville, FL 32611, USA 10 Department of Astronomy, University of Michigan, 830 Dennison Building, Ann Arbor, MI 48109, USA 11 Isaac Newton Institute, Chile, SAO Branch Received 10 September 2002 / Accepted 22 October 2002 Abstract. We present Hubble Space Telescope/WFPC2 images of sixteen dwarf galaxies as part of our snapshot survey of nearby galaxy candidates. We derive their distances from the luminosity of the tip of the red giant branch stars with a typical accuracy of 12%.
    [Show full text]
  • Arxiv:0705.4139V2 [Astro-Ph] 14 Dec 2007 the Bulk Motion of the Local Sheet Away from the Local Void
    Our Peculiar Motion Away from the Local Void R. Brent Tully, Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 and Edward J. Shaya University of Maryland, Astronomy Department, College Park, MD 20743 and Igor D. Karachentsev. Special Astrophysical Observatory, Nizhnij Arkhyz, Karachaevo-Cherkessia, Russia and H´el`eneM. Courtois, Dale D. Kocevski, and Luca Rizzi Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 and Alan Peel University of Maryland, Astronomy Department, College Park, MD 20743 ABSTRACT The peculiar velocity of the Local Group of galaxies manifested in the Cosmic Microwave Background dipole is found to decompose into three dominant components. The three compo- nents are clearly separated because they arise on distinct spatial scales and are fortuitously almost orthogonal in their influences. The nearest, which is distinguished by a velocity discontinuity at ∼ 7 Mpc, arises from the evacuation of the Local Void. We lie in the Local Sheet that bounds the void. Random motions within the Local Sheet are small and we advocate a reference frame with respect to the Local Sheet in preference to the Local Group. Our Galaxy participates in arXiv:0705.4139v2 [astro-ph] 14 Dec 2007 the bulk motion of the Local Sheet away from the Local Void. The component of our motion on an intermediate scale is attributed to the Virgo Cluster and its surroundings, 17 Mpc away. The third and largest component is an attraction on scales larger than 3000 km s−1 and centered near the direction of the Centaurus Cluster. The amplitudes of the three components are 259, 185, and 455 km s−1, respectively, adding collectively to 631 km s−1 in the reference frame of the Local Sheet.
    [Show full text]
  • A List of Nearby Dwarf Galaxies Towards the Local Void in Hercules-Aquila
    ASTRONOMY & ASTROPHYSICS MARCH I 1999, PAGE 221 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 135, 221–226 (1999) A list of nearby dwarf galaxies towards the Local Void in Hercules-Aquila V.E. Karachentseva1,2, I.D. Karachentsev1,3, and G.M. Richter4 1 Visiting astronomer, Astrophysikalisches Institut Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany 2 Astronomical Observatory of Kiev University, Observatorna 3, 254053, Kiev, Ukraine 3 Special Astrophysical Observatory, Russian Academy of Sciences, N. Arkhyz, KChR, 357147, Russia 4 Astrophysicalisches Institut Potsdam, an der Sternwarte 16, D-14482 Potsdam, Germany Received July 6; accepted September 21, 1998 Abstract. Based on film copies of the POSS-II we in- Our main goal was to search for new nearby dwarf spected a wide area of ∼ 6000ut◦ in the direction of the galaxies in this Local Void. Because the Local Void begins h m ◦ nearest cosmic void: {RA = 18 38 , D =+18,V0 < actually just beyond the Local Group edge, we obtain here 1500 km s−1}. As a result we present a list of 78 nearby unprecedently a low threshold for detection of very faint dwarf galaxy candidates which have angular diameters dwarf galaxies in a void, which is an order of magnitude 0 00 ∼> 0.5 and a mean surface brightness ∼< 26 mag/ut .Of lowerthanfordetectioninothervoids. them 22 are in the direction of the Local Void region. To measure their redshifts, a HI survey of these objects is undertaken on the 100 m Effelsberg telescope. 2. Field of the search Key words: galaxies: general — galaxies: dwarf To outline the position of the Local Void on the sky, we reproduce in Fig.
    [Show full text]
  • The NOG Sample: Selection of the Sample and Identification of Galaxy Systems
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server The NOG sample: selection of the sample and identification of galaxy systems Giuliano Giuricin, Christian Marinoni, Lorenzo Ceriani, Armando Pisani Dept. of Astronomy, Trieste Univ. and SISSA, Trieste, Italy Abstract. In order to map the galaxy density field in the local universe, we select the Nearby Optical Galaxy (NOG) sample, which is a volume- limited (cz 6000 km/s) and magnitude{limited (B 14 mag) sample of ≤ ≤ 7076 optical galaxies which covers 2/3 (8.29 sr) of the sky ( b > 20◦)and has a good completeness in redshift (98%). | | In order to trace the galaxy density field on small scales, we iden- tify the NOG galaxy systems by means of both the hierarchical and the percolation friends of friends methods. The NOG provides high resolution in both spatial sampling of the nearby universe and morphological galaxy classification. The NOG is meant to be the first step towards the construction of a statistically well- controlled galaxy sample with homogenized photometric data covering most of the celestial sphere. 1. The selection of the NOG Relying, in general, on photometric data tabulated in LEDA (Paturel et al. 1997), we select the Nearby Optical Galaxies (NOG) sample, a sample of 7076 galaxies which lie at b > 20◦, have recession velocities (in the Local Group frame) cz 6000 km/s,| | and have corrected total blue magnitudes B 14 mag. We have incorporated≤ numerous new redshifts given by the Optical≤ Redshift Survey (Santiago et al.
    [Show full text]
  • New Hubble Image of Galaxy NGC 6503 10 June 2015
    Lost in space: New Hubble image of galaxy NGC 6503 10 June 2015 and a neighbour is never far away. But this galaxy, known as NGC 6503, has found itself in a lonely position, shown here at the edge of a strangely empty patch of space called the Local Void. This new NASA/ESA Hubble Space Telescope image shows a very rich set of colours, adding to the detail seen in previous images. NGC 6503 is only some 18 million light-years away from us in the constellation of Draco (The Dragon), making it one of the closest neighbours from our Local Group. It spans some 30 000 light-years, about a third of the size of the Milky Way. The galaxy's lonely location led stargazer Stephen James O'Meara to dub it the "Lost-In-Space galaxy" in his 2007 book Hidden Treasures. This galaxy does not just offer poetic inspiration; it Most galaxies are clumped together in groups or is also the subject of ongoing research. The Hubble clusters. A neighboring galaxy is never far away. But this Legacy ExtraGalactic UV Survey (LEGUS) is galaxy, known as NGC 6503, has found itself in a lonely exploring a sample of nearby galaxies, including position, at the edge of a strangely empty patch of space NGC 6503, to study their shape, internal structure, called the Local Void. The Local Void is a huge stretch of and the properties and behaviour of their stars. This space that is at least 150 million light-years across. It survey uses 154 orbits of time on Hubble; by seems completely empty of stars or galaxies.
    [Show full text]
  • Troels Haugbølle [email protected]
    An Inhomogeneous World View Modern Cosmology – Benasque August 2010 Troels Haugbølle [email protected] Niels Bohr Institute, University of Copenhagen Collaborators: David Alonso Tamara Davis Juan Garcia-Bellido Benjamin Sinclair Julian Vicente We live in an Accelerating & Isotropic Universe Type Ia Supernovae Perlmutter, Physics Today (2003) 0.0001 26 Supernova Cosmology Project 24 High-Z Supernova Search 0.001 22 fainter Calan/Tololo 25 empty 0.01 Supernova Survey 0 20 mass 0.2 0.4 0.6 1.0 1 density 18 24 0.1 with vacuum energy Relative brightness 16 1 23 without vacuum energy 14 0.01 0.02 0.04 0.1 22 Accelerating Universe magnitude 21 Decelerating Universe 20 0.2 0.4 0.6 1.0 redshift 0.8 0.7 0.6 0.5 Scale of the Universe (NASA Lambda archive) [relative to today's scale] The Standard ΛCDM model The numbers t0 = 13.73 ± 0.13are Gyr impressive, Age of Universe -1 -1 H0 = 70.1 ± 1.3but km can s Mpc we trust Expansion rate the model ??? Ωb = 0.0462 ± 0.0015 Baryon density Ωc = 0.233 ± 0.013 Dark Matter density ΩΛ = 0.721 ± 0.015 Dark energy density ns = 0.960 ± 0.014 Scalar spectral index 2 -9 ΔR = 2.46 ± 0.09 10 Fluctuation amplitude The Pillars of the ΛCDM model • General Relativity • The FRW model of a homogeneous universe • Dark Matter & fields with strange equations of state The Pillars of the ΛCDM model Modify Gravity • General Relativity • The FRW model of a homogeneous universe • Dark Matter & fields with strange equations of state The PillarsAlternative of the ScenarioΛCDM model • General Relativity Modify the Geometry • The FRW model of a homogeneous universe • Dark Matter & fields with strange equations of state Alternative scenario I Its Swiss Cheese The filling factor of small voids is > 80%; light rays will go through small locally open universes The universe is full of holes, like a Swiss Cheese Alternative scenario I Its Swiss ΛCheese ? Since voids becomes bigger and bigger we get apparent acceleration But randomising the positions of the voids removes the effect.
    [Show full text]
  • Read Book 400 Billion Stars Kindle
    400 BILLION STARS PDF, EPUB, EBOOK Paul McAuley | 240 pages | 14 Oct 2009 | Orion Publishing Co | 9780575090033 | English | London, United Kingdom 400 Billion Stars PDF Book So, all in all, a good read and McAuley has easily become one of my most favorite writers working today. Astronomical Society of the Pacific Conference Series. January 9, It's an impressive debut for Paul McCauley, and almost more along the lines of a novella rather than a space opera. At this speed, it takes around 1, years for the Solar System to travel a distance of 1 light-year, or 8 days to travel 1 AU astronomical unit. Archived from the original on September 16, Dame; P. Milky Way. Retrieved September 15, Bibcode : NatAs. Archived PDF from the original on May 14, Here, an elongated object such as a galaxy is viewed through an elongated slit, and the light is refracted using a device such as a prism. Main article: Local Group. Archived from the original on November 5, In , a star in the galactic halo, HE , was estimated to be about Return to Book Page. February 13, Carina-Sagittarius Arm. The Huffington Post. If you picked the quarter as being the average mass of a single coin, you might get one answer for the total number of coins. She's also a scientist, and when a small planet begins to manifest some unusual signs she is sent to investigate. If these arms contain an overdensity of stars compared to the average density of stars in the Galactic disk, it would be detectable by counting the stars near the tangent point.
    [Show full text]
  • Arxiv:1306.0091V4 [Astro-Ph.CO] 13 Jun 2013
    Draft version June 14, 2013 A Preprint typeset using LTEX style emulateapj v. 5/2/11 COSMOGRAPHY OF THE LOCAL UNIVERSE Hel´ ene` M. Courtois1,2 1University of Lyon; UCB Lyon 1/CNRS/IN2P3; IPN Lyon, France and 2Institute for Astronomy (IFA), University of Hawaii, 2680 Woodlawn Drive, HI 96822, USA Daniel Pomarede` 3 3CEA/IRFU, Saclay, 91191 Gif-sur-Yvette, France R. Brent Tully2 1Institute for Astronomy (IFA), University of Hawaii, 2680 Woodlawn Drive, HI 96822, USA Yehuda Hoffman4 4Racah Institute of Physics, Hebrew University, Jerusalem 91904, Israel and Denis Courtois5 Lyc´ee international, 38300 Nivolas-vermelle, France Draft version June 14, 2013 ABSTRACT The large scale structure of the universe is a complex web of clusters, filaments, and voids. Its properties are informed by galaxy redshift surveys and measurements of peculiar velocities. Wiener Filter reconstructions recover three-dimensional velocity and total density fields. The richness of the elements of our neighborhood are revealed with sophisticated visualization tools. A key component of this paper is an accompanying movie. The ability to translate and zoom helps the viewer fol- low structures in three dimensions and grasp the relationships between features on different scales while retaining a sense of orientation. The ability to dissolve between scenes provides a technique for comparing different information, for example, the observed distribution of galaxies, smoothed repre- sentations of the distribution accounting for selection effects, observed peculiar velocities, smoothed and modeled representations of those velocities, and inferred underlying density fields. The agreement between the large scale structure seen in redshift surveys and that inferred from reconstructions based on the radial peculiar velocities of galaxies strongly supports the standard model of cosmology where structure forms from gravitational instabilities and galaxies form at the bottom of potential wells.
    [Show full text]