DOCSLIB.ORG

Snake River Skies the Newsletter of the Magic Valley Astronomical Society

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Snake River Skies the Newsletter of the Magic Valley Astronomical Society Snake River Skies The Newsletter of the Magic Valley Astronomical Society www.mvastro.org Membership Meeting President’s Message Saturday, March 11th 2017 Dear Colleagues, 7:00pm at the Herrett Center for Arts & Science College of Southern Idaho. With all of the snow and water, sometimes astronomy gets lost in the winter months. Fortunately, we have a couple of events coming up that are among our members’ Public Star Party Follows at the favorite activities. Centennial Observatory First, this month’s meeting will be the annual Show and Tell, Saturday, March 11, at Club Officers 7 p.m. in the Herrett Center’s Rick Allen. Anyone who has been working on something, has purchased something, or has simply found another interesting facet Robert Mayer, President of astronomy can come in and spend 10 to 20 informal minutes showing off or [email protected] talking about what he or she is working on. Sometimes it’s a newly built telescope, 208-312-1203 and sometimes it’s a new set of pictures, but last year’s highlight was Jay Naegele surprising us with his Sunsetter Solar Scope. Who knows what we’ll find this time? Tim Frazier, Vice President [email protected] If you do have an interesting item you’d like to share, would you please give me a heads-up so I can plan out an informal schedule? Contact me at Gary Leavitt, Secretary [email protected] so I can make sure everyone gets enough time. [email protected] 208-731-7476 Two weeks later will be the annual Messier Marathon. The main date is Friday, March 24th, while the back-up date is Saturday, March 25th. Whether you’re going Jim Tubbs, Treasurer / ALCOR for all 110 Messier objects, or you’re just glad to get out with the scope after a rough [email protected] winter, come on down to the Jerome Gun Club. If you don’t have a scope, contact 208-404-2999 us, and we’ll bring a loaner. If you want to bring a friend, by all means, bring him or her. This is one of the highlights of the year. David Olsen, Newsletter Editor [email protected] Until then, Clear Views, Rick Widmer, Webmaster [email protected] Magic Valley Astronomical Society is a member of the Astronomical League M-51 imaged by Rick Widmer & Ken Thomason Herrett Telescope Shotwell Camera Calendar for January Sun Mon Tue Wed Thu Fri Sat 1 2 3 4 5 6 7 8 9 10 11 First Quarter MVAS Meeting 51% Visible ↑ at 7:00pm at the Herrett Center Public Star Party Centennial Obs. 12 13 14 15 16 17 18 Full Moon St. Patrick's Day 19 20 21 22 23 24 25 Last Quarter Earth Hour Vernal Observing at Equinox the Centennial Observatory 8:30-9:30pm 26 27 28 29 30 31 New Moon Lunation 1166 1% Visible↑ Snake River Skies is the Newsletter of the Magic Valley Astronomical Society and is published electronically once a month. SkyWatcher is copyrighted, except where noted and credit is via permission of the respective author. SkyWatcher © 2017 by David Olsen for the Magic Valley Astronomical Society, All Rights Reserved. Images used in this newsletter, unless otherwise noted, are in the public domain and are courtesy of NASA, Wikimedia, or from MVAS File Photos. Full Moon names follow the traditional Algonquin First Nation history. Celestial Calendar All times, unless otherwise noted, are Universal Time (UT subtract seven hours and, when appropriate, one calendar day for MST and six hours for MDT as of March 12th) 3/1 Venus is 9.7 degrees north-northwest of the Moon at 2:00; Uranus is 3.4 degrees north-northwest of the Moon at 18:00; the Moon, Mars, and Uranus lie within a circle with a diameter of 4.2 degrees at 20:00; Mars is 4.1 degrees north- northwest of the Moon at 21:00 3/2 Neptune is in conjunction with the Sun at 3:00; Venus is stationary in right ascension at 14:00; asteroid 1 Ceres is 0.8 degree north of the Moon, with an occultation visible from South Georgia, the Antarctic peninsula, and the southern half of South America, at 3:00 3/3 The Moon is at perigee, subtending 32' 23" from a distance of 369,063 kilometers (229,325 miles), at 7:33; asteroid 29 Amphitrite (magnitude +9.1) is at opposition at 12:00 3/4 The Moon is 9.3 degrees south-southeast of the bright open cluster M45 (the Pleiades or Subaru) in Taurus at 10:00; Mercury is 1.0 degree south-southeast of Neptune at 12:00 3/5 The 45%-illuminated Moon is 0.25 degree north-northwest of the first-magnitude star Aldebaran (Alpha Tauri), with an occultation visible from the western Caribbean, Central America, most of the continental United States, Hawaii, Micronesia, and the Solomon Islands, at 3:00; the Lunar X (the Purbach or Werner Cross), an X-shaped Clair-Obscure illumination effect involving various rims and ridges between the craters La Caille, Blanchinus, and Purbach, is predicted to occur at 9:56; 3/6 The Moon is 5.5 degrees south of the bright open cluster M35 in Gemini at 17:00 3/7 Mercury is in superior conjunction with the Sun at 0:00; asteroid 4 Vesta is stationary at 3:00 3/8 The Moon is 10.1 degrees south of the first-magnitude star Pollux (Beta Geminorum) at 7:00; asteroid 41 Daphne (magnitude +9.6) is at opposition at 7:00 3/9 The Moon is 3.6 degrees south of the bright open cluster M44 (the Beehive Cluster or Praesepe) in Cancer at 7:00 3/10 Comet 2P/Encke is at perihelion (0.3359 astronomical unit from the Sun) at 2:00; the Moon is 0.8 degrees south- southwest of the first-magnitude star Regulus (Alpha Leonis) at 22:00; 3/11 The Moon is at the ascending node (longitude 153.4 degrees) at 4:20; the Sun enters Pisces, at longitude 351.6 degrees on the ecliptic, at 23:00 3/12 Daylight Saving Time (DST) begins today; Full Moon (known as the Crow, Lenten, and Sap Moon) occurs at 14:54 3/14 Venus is at its greatest latitude north of the ecliptic plane (3.4 degrees) at 6:00; Jupiter is 2.3 degrees south- southwest of the Moon at 22:00 3/15 The Moon is 6.1 degrees north-northeast of the first-magnitude star Spica (Alpha Virginis) at 3:00; asteroid Pallas is in conjunction with the Sun at 3:00 3/17 Saturn is at western quadrature (i.e., 90 degrees from the Sun) at 22:00 3/18 The Moon is at apogee, subtending 29' 32" from a distance of 404,649 kilometers (251,438 miles), at 17:25; Mercury (magnitude -1.3) is 8.5 degrees south-southeast of Venus (magnitude -4.2) at 18:00; Mercury is at the ascending node at 22:00; the Moon is 9.8 degrees north of the first-magnitude star Antares (Alpha Scorpii) at 23:00 3/20 Saturn is 3.4 degrees south of the Moon at 10:49; the Vernal Equinox occurs at 11:29; 3/21 The Curtiss Cross, an X-shaped Clair-Obscure illumination effect located between the craters Parry and Gambart, is predicted to be at a midpoint at 12:42 3/25 Venus is in inferior conjunction with the Sun at 10:00; the Moon is in descending node (longitude 333.1degrees) at 15:43 3/26 Neptune is 0.01 degree east-northeast of the Moon; Mercury (magnitude -0.8) is 2.1degrees north-northwest of Uranus (magnitude +5.9) at 10:00 3/27 Venus is 10.7 degrees north-northwest of the Moon at 19:00 3/29 Uranus is 3.4 degrees north-northwest of the Moon at 5:00; Mercury is 6.3 degrees NNW of the Moon at 11:00 3/30 The Moon is at perigee, subtending 32' 50" from a distance of 363,854 kilometers (226,088 miles), at 12:32; Mars is 5.3 degrees north-northwest of the Moon at 16:00 3/31 The Moon is 9.2 degrees south-southeast of M45 at 17:00 Titan, Saturn’s largest satellite, was discovered on March 25, 1655 by the Dutch astronomer Christiaan Huygens. The English astronomer Edward Pigott discovered the spiral galaxy M63 (the Black Eye Galaxy) on March 23, 1779. The English astronomer Sir William Herschel discovered Uranus on March 13, 1781. Asteroid 4 Vesta was discovered by the German astronomer Heinrich Wilhelm Matthias Olbers on March 29, 1807. The first photograph of the Moon was taken on March 23, 1840. The Czech astronomer Luboš Kohoutek discovered Comet C/1973 E1 (Kohoutek) on March 7, 1973. The rings of Uranus were discovered on March 10, 1977. The Spanish amateur astronomer Francisco Garcia Diaz Garcia discovered supernova SN 1993 in the spiral galaxy M81 (Bode's Galaxy) on March 28th, 1993. The zodiacal light may be visible in the western sky after sunset from dark locations during the second half of March. The Sun, the Moon, & the Planets The Sun is in Aquarius on March 1st at 0:00 UT. The Sun crosses the celestial equator at 10:29 on March 20th, bringing spring to the northern hemisphere. Brightness, apparent size, illumination, distance from the Earth in astronomical units, and location data for the planets and Pluto on March 1st: Mercury (magnitude -1.3, 4.9", 99%, 1.38 a.u., Aquarius), Venus (magnitude -4.8, 46.9", 17% illuminated, 0.36 a.u., Pisces), Mars (magnitude +1.3, 4.6", 94% illuminated, 2.04 a.u., Pisces), Jupiter (magnitude -2.3, 42.1", 100% illuminated, 4.68 a.u., Virgo), Saturn (magnitude +0.5, 16.2", 100% illuminated, 10.28 a.u., Sagittarius), Uranus (magnitude +5.9, 3.4", 100% illuminated, 20.81 a.u.
Load more

Recommended publications
  • Fourier Dissection of Early-Type Galaxy Bars R
    The Astronomical Journal, 132:1859Y1876, 2006 November # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. FOURIER DISSECTION OF EARLY-TYPE GALAXY BARS R. Buta,1 E. Laurikainen,2 H. Salo,2 D. L. Block,3 and J. H. Knapen4 Received 2006 May 4; accepted 2006 July 14 ABSTRACT This paper reports on a near-infrared survey of early-type galaxies designed to provide information on bar strengths, bulges, disks, and bar parameters in a statistically well-defined sample of S0YSa galaxies. Early-type galaxies have the advantage that their bars are relatively free of the effects of dust, star formation, and spiral structure that com- plicate bar studies in later type galaxies. We describe the survey and present results on a detailed analysis of the rela- tive Fourier intensity amplitudes of bars in 26 early-type galaxies. We also evaluate the ‘‘symmetry assumption’’ of these amplitudes with radius, used recently for bar-spiral separation in later type galaxies. The results show a wide variety of radial Fourier profiles of bars, ranging from simple symmetric profiles that can be represented in terms of a single Gaussian component to both symmetric and asymmetric profiles that can be represented by two overlapping Gaussian components. More complicated profiles than these are also found, often due to multiple barlike features including extended ovals or lenses. Based on the gravitational bar torque indicator Qb, double-Gaussian bars are stronger on average than single-Gaussian bars, at least for our small sample. We show that published numerical simulations in which the bar transfers a large amount of angular momentum to the halo can account for many of the observed profiles.
    [Show full text]
  • Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
    The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al.
    [Show full text]
  • The Local Galaxy Volume
    11-1 How Far Away Is It – The Local Galaxy Volume The Local Galaxy Volume {Abstract – In this segment of our “How far away is it” video book, we cover the local galaxy volume compiled by the Spitzer Local Volume Legacy Survey team. The survey covered 258 galaxies within 36 million light years. We take a look at just a few of them including: Dwingeloo 1, NGC 4214, Centaurus A, NGC 5128 Jets, NGC 1569, majestic M81, Holmberg IX, M82, NGC 2976,the unusual Circinus, M83, NGC 2787, the Pinwheel Galaxy M101, the Sombrero Galaxy M104 including Spitzer’s infrared view, NGC 1512, the Whirlpool Galaxy M51, M74, M66, and M96. We end with a look at the tuning fork diagram created by Edwin Hubble with its description of spiral, elliptical, lenticular and irregular galaxies.} Introduction [Music: Johann Pachelbel – “Canon in D” – This is Pachelbel's most famous composition. It was written in the 1680s between the times of Galileo and Newton. The term 'canon' originates from the Greek kanon, which literally means "ruler" or "a measuring stick." In music, this refers to timing. In astronomy, "a measuring stick" refers to distance. We now proceed to galaxies more distant than the ones in our Local Group.] The Local volume is the set of galaxies covered in the Local Volume Legacy survey or LVL, for short, conducted by the Spitzer team. It is a complete sample of 258 galaxies within 36 million light years. This montage of images shows the ensemble of galaxies as observed by Spitzer. The galaxies are randomly arranged but their relative sizes are as they appear on the sky.
    [Show full text]
  • 1. Introduction
    THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other.
    [Show full text]
  • Lateinischer Name: Deutscher Name: Hya Hydra Wasserschlange
    Lateinischer Name: Deutscher Name: Hya Hydra Wasserschlange Atlas Karte (2000.0) Kulmination um Cambridge 10, 16, Mitternacht: Star Atlas 17 12, 13, Sky Atlas Benachbarte Sternbilder: 20, 21 Ant Cnc Cen Crv Crt Leo Lib 9. Februar Lup Mon Pup Pyx Sex Vir Deklinationsbereic h: -35° ... 7° Fläche am Himmel: 1303° 2 Mythologie und Geschichte: Bei der nördlichen Wasserschlange überlagern sich zwei verschiedene Bilder aus der griechischen Mythologie. Das erste Bild zeugt von der eher harmlosen Wasserschlange aus der Geschichte des Raben : Der Rabe wurde von Apollon ausgesandt, um mit einem goldenen Becher frisches Quellwasser zu holen. Stattdessen tat sich dieser an Feigen gütlich und trug bei seiner Rückkehr die Wasserschlange in seinen Fängen, als angebliche Begründung für seine Verspätung. Um jedermann an diese Untat zu erinnern, wurden der Rabe samt Becher und Wasserschlange am Himmel zur Schau gestellt. Von einem ganz anderen Schlag war die Wasserschlange, mit der Herakles zu tun hatte: In einem Sumpf in der Nähe von Lerna, einem See und einer Stadt an der Küste von Argo, hauste ein unsagbar gefährliches und grässliches Untier. Diese Schlange soll mehrere Köpfe gehabt haben. Fünf sollen es gewesen sein, aber manche sprechen auch von sechs, neun, ja fünfzig oder hundert Köpfen, aber in jedem Falle war der Kopf in der Mitte unverwundbar. Fürchterlich war es, da diesen grässlichen Mäulern - ob die Schlange nun schlief oder wachte - ein fauliger Atem, ein Hauch entwich, dessen Gift tödlich war. Kaum schlug ein todesmutiger Mann dem Untier einen Kopf ab, wuchsen auf der Stelle zwei neue Häupter hervor, die noch furchterregender waren. Eurystheus, der König von Argos, beauftragte Herakles in seiner zweiten Aufgabe diese lernäische Wasserschlange zu töten.
    [Show full text]
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications
    Spiral galaxy HI models, rotation curves and kinematic classifications Theresa B. V. Wiegert A thesis submitted to the Faculty of Graduate Studies of The University of Manitoba in partial fulfillment of the requirements of the degree of Doctor of Philosophy Department of Physics & Astronomy University of Manitoba Winnipeg, Canada 2010 Copyright (c) 2010 by Theresa B. V. Wiegert Abstract Although galaxy interactions cause dramatic changes, galaxies also continue to form stars and evolve when they are isolated. The dark matter (DM) halo may influence this evolu- tion since it generates the rotational behaviour of galactic disks which could affect local conditions in the gas. Therefore we study neutral hydrogen kinematics of non-interacting, nearby spiral galaxies, characterising their rotation curves (RC) which probe the DM halo; delineating kinematic classes of galaxies; and investigating relations between these classes and galaxy properties such as disk size and star formation rate (SFR). To generate the RCs, we use GalAPAGOS (by J. Fiege). My role was to test and help drive the development of this software, which employs a powerful genetic algorithm, con- straining 23 parameters while using the full 3D data cube as input. The RC is here simply described by a tanh-based function which adequately traces the global RC behaviour. Ex- tensive testing on artificial galaxies show that the kinematic properties of galaxies with inclination > 40 ◦, including edge-on galaxies, are found reliably. Using a hierarchical clustering algorithm on parametrised RCs from 79 galaxies culled from literature generates a preliminary scheme consisting of five classes. These are based on three parameters: maximum rotational velocity, turnover radius and outer slope of the RC.
    [Show full text]
  • April Constellations of the Month
    April Constellations of the Month Leo Small Scope Objects: Name R.A. Decl. Details M65! A large, bright Sa/Sb spiral galaxy. 7.8 x 1.6 arc minutes, magnitude 10.2. Very 11hr 18.9m +13° 05’ (NGC 3623) high surface brighness showing good detail in medium sized ‘scopes. M66! Another bright Sb galaxy, only 21 arc minutes from M65. Slightly brighter at mag. 11hr 20.2m +12° 59’ (NGC 3627) 9.7, measuring 8.0 x 2.5 arc minutes. M95 An easy SBb barred spiral, 4 x 3 arc minutes in size. Magnitude 10.5, with 10hr 44.0m +11° 42’ a bright central core. The bar and outer ring of material will require larger (NGC 3351) aperature and dark skies. M96 Another bright Sb spiral, about 42 arc minutes east of M95, but larger and 10hr 46.8m +11° 49’ (NGC 3368) brighter. 6 x 4 arc minutes, magnitude 10.1. Located about 48 arc minutes NNE of M96. This small elliptical galaxy measures M105 only 2 x 2.1 arc minutes, but at mag. 10.3 has very high surface brightness. 10hr 47.8m +12° 35’ (NGC 3379) Look for NGC 3384! (110NGC) and NGC 3389 (mag 11.0 and 12.2) which form a small triangle with M105. NGC 3384! 10hr 48.3m +12° 38’ See comment for M105. The brightest galaxy in Leo, this Sb/Sc spiral galaxy shines at mag. 9.5. Look for NGC 2903!! 09hr 32.2m +21° 30’ a hazy patch 11 x 4.7 arc minutes in size 1.5° south of l Leonis.
    [Show full text]
  • Guide Du Ciel Profond
    Guide du ciel profond Olivier PETIT 8 mai 2004 2 Introduction hjjdfhgf ghjfghfd fg hdfjgdf gfdhfdk dfkgfd fghfkg fdkg fhdkg fkg kfghfhk Table des mati`eres I Objets par constellation 21 1 Androm`ede (And) Andromeda 23 1.1 Messier 31 (La grande Galaxie d'Androm`ede) . 25 1.2 Messier 32 . 27 1.3 Messier 110 . 29 1.4 NGC 404 . 31 1.5 NGC 752 . 33 1.6 NGC 891 . 35 1.7 NGC 7640 . 37 1.8 NGC 7662 (La boule de neige bleue) . 39 2 La Machine pneumatique (Ant) Antlia 41 2.1 NGC 2997 . 43 3 le Verseau (Aqr) Aquarius 45 3.1 Messier 2 . 47 3.2 Messier 72 . 49 3.3 Messier 73 . 51 3.4 NGC 7009 (La n¶ebuleuse Saturne) . 53 3.5 NGC 7293 (La n¶ebuleuse de l'h¶elice) . 56 3.6 NGC 7492 . 58 3.7 NGC 7606 . 60 3.8 Cederblad 211 (N¶ebuleuse de R Aquarii) . 62 4 l'Aigle (Aql) Aquila 63 4.1 NGC 6709 . 65 4.2 NGC 6741 . 67 4.3 NGC 6751 (La n¶ebuleuse de l’œil flou) . 69 4.4 NGC 6760 . 71 4.5 NGC 6781 (Le nid de l'Aigle ) . 73 TABLE DES MATIERES` 5 4.6 NGC 6790 . 75 4.7 NGC 6804 . 77 4.8 Barnard 142-143 (La tani`ere noire) . 79 5 le B¶elier (Ari) Aries 81 5.1 NGC 772 . 83 6 le Cocher (Aur) Auriga 85 6.1 Messier 36 . 87 6.2 Messier 37 . 89 6.3 Messier 38 .
    [Show full text]
  • Astronomy Magazine Special Issue
    γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006.
    [Show full text]
  • The Discovery of Cepheids and a New Distance to NGC 2841 Using the Hubble Space Telescope L
    Rochester Institute of Technology RIT Scholar Works Articles 9-20-2001 The Discovery of Cepheids and a New Distance to NGC 2841 Using the Hubble Space Telescope L. M. Macri Harvard-Smithsonian Center for Astrophysics P. B. Stetson National Research Council of Canada G. D. Bothun University of Oregon W. L. Freedman Observatories of the Carnegie Institute of Washington P. M. Garnavich University of Notre Dame See next page for additional authors Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation L. M. Macri et al 2001 ApJ 559 243 https://doi.org/10.1086/322395 This Article is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Articles by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Authors L. M. Macri, P. B. Stetson, G. D. Bothun, W. L. Freedman, P. M. Garnavich, S. Jha, B. F. Madore, and Michael W. Richmond This article is available at RIT Scholar Works: http://scholarworks.rit.edu/article/1587 To appear in the September 20, 2001 issue of the Astrophysical Journal THE DISCOVERY OF CEPHEIDS AND A NEW DISTANCE TO NGC 2841 USING THE HUBBLE SPACE TELESCOPE† L.M. Macri1, P.B. Stetson2, G.D. Bothun3, W.L. Freedman4, P.M. Garnavich5, S. Jha1, B.F. Madore4,6 & M.W. Richmond7 ABSTRACT We report on the discovery of Cepheids in the spiral galaxy NGC2841, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope.
    [Show full text]
  • Arxiv:2001.00331V2 [Astro-Ph.GA] 27 Feb 2020 Et Al
    Draft version February 28, 2020 Typeset using LATEX twocolumn style in AASTeX62 The Carnegie-Irvine Galaxy Survey. IX. Classification of Bulge Types and Statistical Properties of Pseudo Bulges Hua Gao (高f),1, 2 Luis C. Ho,2, 1 Aaron J. Barth,3 and Zhao-Yu Li4 1Department of Astronomy, School of Physics, Peking University, Beijing 100871, China 2Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China 3Department of Physics and Astronomy, University of California at Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA 4Department of Astronomy, Shanghai Jiao Tong University, Shanghai 200240, China ABSTRACT We study the statistical properties of 320 bulges of disk galaxies in the Carnegie-Irvine Galaxy Survey, using robust structural parameters of galaxies derived from image fitting. We apply the Kormendy relation to classify classical and pseudo bulges and characterize bulge dichotomy with respect to bulge structural properties and physical properties of host galaxies. We confirm previous findings that pseudo bulges on average have smaller S´ersic indices, smaller bulge-to-total ratios, and fainter surface brightnesses when compared with classical bulges. Our sizable sample statistically shows that pseudo bulges are more intrinsically flattened than classical bulges. Pseudo bulges are most frequent (incidence & 80%) in late-type spirals (later than Sc). Our measurements support the picture in which pseudo bulges arose from star formation induced by inflowing gas, while classical bulges were born out of violent processes such as mergers and coalescence of clumps. We reveal differences with the literature that warrant attention: (1) the bimodal distribution of S´ersicindices presented by previous studies is not reproduced in our study; (2) classical and pseudo bulges have similar relative bulge sizes; and (3) the pseudo bulge fraction is considerably smaller in early-type disks compared with previous studies based on one-dimensional surface brightness profile fitting.
    [Show full text]