DOCSLIB.ORG

Draco. Nombre En Español: Dragon. Abreviatura: Dra. Localización: Circumpolar

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Draco. Nombre En Español: Dragon. Abreviatura: Dra. Localización: Circumpolar 1 Draco Nombre Latino: Draco. Nombre en Español: Dragon. Abreviatura: Dra. Localización: Circumpolar. Hemisferio Norte. A.R. :17.75 horas. Dec.: 62.51 º. Franja de observación:90 º N – 4 º S. Es una de las constelaciones originales de Ptolomeo que rodea el polo norte celeste, con una “cabeza” poligonal seguida de una larga cola que rodea la Ursa Minor. Existen diversas leyendas sobre el origen del nombre de esta constelación. Pero lo cierto es que todos los dragones siempre tienen la misión de guardianes o de custodios de tesoros. Es importante señalar que en griego, dragón (o δράκων) significa “serpiente”, lo que es importante tener en cuenta a la hora de interpretar los diversos mitos en los que aparece esta constelación, pues nuestro término dragón está demasiado “contaminado” por mitos y leyendas medievales. Algunos autores afirman que es una constelación de origen mesopotámico, cuya representación aparece en bajorrelieves muy antiguos, La serpiente era, junto a animales como el escorpión, el toro, el león o el carnero, uno de los más familiares y frecuentes en la iconografía mesopotámica. En los kudurrus babilonios aparecen varios símbolos característicos de cada dios, representando varias constelaciones. En muchos de ellos se puede ver a una serpiente enroscada en la parte superior del kudurru, junto a otra en la parte central, esta última usualmente identificada con Hidra En Egipto también aparece representada una constelación similar, que abarca parte de la actual Draco; correspondería a la diosa-hipopótamo Isis-Dyamut, que solía representarse con un pequeño cocodrilo en una mano y un remo o una espada en la otra. Sobre su espalda, a modo de capa la cubre un cocodrilo. A veces, en vez de una espada, lleva en la mano una jarra. Desde el segundo milenio antes de Cristo ya se conocía su existencia. A partir del siglo VI a.C., al dragón se le “amputan” las alas, que se convierten en la constelación Ursa Minor. Debemos aclarar que la palabra dragón es de origen Griego, que designaba tanto ese animal como a la serpiente”. Uno de los mitos es el del legendario Cadmo, fundador de Tebas, sembró un puñado de dientes de dragón de los que nacerían los tebanos. Otra historia nos cuenta de un dragón luchando en el bando de los titanes contra los dioses olímpicos: la diosa Atenea se enfrentó a él, lanzándolo a los cielos donde quedó enredado con su propio cuerpo y congelándose de frío. Eratóstenes fue el primero en explicar el mito asociado a esta constelación. Cuenta la historia que en la boda entre Zeus y Hera, Gea regaló a la pareja el árbol de las manzanas de oro. Hera, admirada por el regalo, lo plantó en el jardín de las Hesperides situado cerca del Atlas. Pero como las hijas de Atlas, robaban las manzanas, Hera colocó a la serpiente como guardián. Las manzanas podrían simbolizar, según imágenes de cerámicas áticas del siglo V a.C., la inmortalidad o la eterna juventud. Mientras cumplía con su trabajo fue muerto por Hércules. Pero Hera por su valor y fidelidad lo envió al cielo. Curiosamente en Egipto, se construyeron muchos templos de forma que las estrellas del Dragón, brillaban en unas épocas determinadas sobre el altar. En la lejana China también vieron un dragón en esta constelación, ya que se trataba de un animal muy importante para ese pueblo, que lo considero su símbolo nacional. Según la época del año en que observemos esta zona del cielo, así veremos en distintas posiciones esta constelación, siempre envolviendo a la Osa Menor, La constelación del Dragón se encuentra en una zona del cielo rica de galaxias, junto a las dos Osas. Hace 5000años la estrella inmóvil sobre la que parece girar el firmamento no era la estrella Polar sino la estrella alfa del Dragón. Era conocida por los árabes como Thuban “el dragón”. En el año 200 a.c. cuando los marinos Fenicios colonizaron las costas Mediterráneas, la polar de entonces era esa estrella. Mi libro de las constelaciones. Eladio Miranda Batlle 2 Fig. 86. Constelación Draco (Dragón). Estrellas principales: Thuban: Nombre que dieron los árabes a toda la constelación «Al Thuban»: “el dragón”. Rastaban: Nombre de origen árabe que significa “cabeza de la serpiente”. Eltanin: Del árabe “Al Ras al Tinnin”: “cabeza del dragón”. Visual Abs. Tipo Distancia Estrellas R.A. (h m s) Dec. ( ° ' '' ) mag. mag. Espectral (lt-yr) Gamma (Eltanin) 2.24 -1.04 K5III 148 17 56 36 +51 29 20 Eta (Aldhibain) 2.73 -6.27 G8IIIab 2,050 16 23 59 +61 30 50 Beta (Rastaban) 2.79 -2.44 G2Ib-IIa 361 17 30 26 +52 18 05 Delta (Taïs) 3.07 0.63 G9III 100 19 12 33 +67 39 41 Zeta (Aldhibah) 3.17 -1.90 B6III 320 17 08 47 +65 42 53 Iota (Edasich) 3.29 -1.92 B6III 339 15 24 56 +58 57 58 Chi 3.55 4.01 F7V 26 18 21 03 +72 43 58 Alpha (Thuban) 3.67 -1.21 A0III 308 14 04 23 +64 22 33 Xi (Juza) 3.73 1.06 K2III 111 17 53 32 +56 52 21 Epsilon (Tyl) 3.84 0.59 G8IIIbCN 146 19 48 10 +70 16 04 Lambda (Giausar) 3.82 -1.24 M0IIICa 334 11 31 24 +69 19 52 Kappa 3.85 -2.07 B6IIIpe 498 12 33 29 +69 47 17 Mi libro de las constelaciones. Eladio Miranda Batlle 3 Fig. 87. Objetos interesantes del cielo profundo. NOMBRE Mag. Dimensiones Información Nebulosa planetaria conocida como NGC 6543 8.3 22” x 16” el Ojo de Gato, que tiene un disco irregular NGC 4236 9.6 22.6’ x 6.9’ Galaxia espiral barrada NGC 4125 9.7 6’ x 5.1’ Galaxia elíptica Galaxia vista de perfil en la que se observa una NGC 5866 / banda oscura negra en los bordes provocada 9.9 6.5’ x 3.1’ M 102 por la materia interestelar. Está a una distancia aproximada de la Tierra de 50 millones de años luz. UGC 10822 / Galaxia enana elíptica miembro del Grupo 9.9 33.5’ x 18.9’ Draco Dwarf Local de Galaxias NGC 6503 10.2 7’ x 2.5’ Galaxia espiral NGC 5907 10.3 11.8’ x 1.3’ Galaxia espiral NGC 3147 10.6 4.3’ x 3.7’ Galaxia espiral NGC 4589 10.7 3.4’ x 2.8’ Galaxia elíptica NGC 6340 11 3’ x 2.8’ Galaxia espiral NGC 5982 11.1 3’ x 2.1’ Galaxia elíptica NGC 5985 11.1 5.4’ x 2.7’ Galaxia espiral barrada NGC 6015 11.1 5.4’ x 2.1’ Galaxia espiral NGC 6643 11.1 3.7’ x 1.8’ Galaxia espiral NGC 4750 11.2 2.1’ x 1.9’ Galaxia espiral Mi libro de las constelaciones. Eladio Miranda Batlle 4 NGC 5678 11.3 3.3’ x 1.4’ Galaxia espiral barrada NGC 6140 11.3 6.3’ x 4.6’ Galaxia espiral barrada Mi libro de las constelaciones. Eladio Miranda Batlle .
Load more

Recommended publications
  • HST/WFPC2 Imaging of the Circumnuclear Structure of Llagns
    HST/WFPC2 imaging of the circumnuclear structure of LLAGNs. I Data and nuclear morphology1 Rosa M. Gonz´alez Delgado1, Enrique P´erez1, Roberto Cid Fernandes2, Henrique Schmitt3, (1) Instituto de Astrof´ısica de Andaluc´ıa(CSIC), P.O. Box 3004, 18080 Granada, Spain ([email protected]; [email protected]) (2) Depto. de F´ısica-CFM, Universidade Federal de Santa Catarina, C.P. 476, 88040-900, Florian´opolis, SC, Brazil ([email protected]) (3) Remote Sensing Division, Naval Research Laboratory, Code 7210, 4555 Overlook Avenue, Washington, DC 20375 ([email protected]) (4) Interferometrics, Inc., 13454 Sunrise Valley Drive, Suite 240, Herndon, VA20171 ABSTRACT In several studies of Low Luminosity Active Galactic Nuclei (LLAGNs), we have characterized the properties of the stellar populations in LINERs and LINER/HII Transition Objects (TOs). We have found a numerous class of galac- tic nuclei which stand out because of their conspicuous 0.1–1 Gyr populations. These nuclei were called ”Young-TOs” since they all have TO-like emission line ratios. To advance our knowledge of the nature of the central source in LLAGNs and its relation with stellar clusters, we are carrying out several imaging projects with the Hubble Space Telescope (HST) at near-UV, optical and near-IR wave- lengths. In this paper, we present the first results obtained with observations of the central regions of 57 LLAGNs imaged with the WFPC2 through any of arXiv:0710.4450v1 [astro-ph] 24 Oct 2007 the V (F555W, F547M, F614W) and I (F791W, F814W) filters that are avail- able in the HST archive.
    [Show full text]
  • Radio Sources in Low-Luminosity Active Galactic Nuclei
    A&A 392, 53–82 (2002) Astronomy DOI: 10.1051/0004-6361:20020874 & c ESO 2002 Astrophysics Radio sources in low-luminosity active galactic nuclei III. “AGNs” in a distance-limited sample of “LLAGNs” N. M. Nagar1, H. Falcke2,A.S.Wilson3, and J. S. Ulvestad4 1 Arcetri Observatory, Largo E. Fermi 5, Florence 50125, Italy 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany e-mail: [email protected] 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 4 National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA e-mail: [email protected] Received 23 January 2002 / Accepted 6 June 2002 Abstract. This paper presents the results of a high resolution radio imaging survey of all known (96) low-luminosity active galactic nuclei (LLAGNs) at D ≤ 19 Mpc. We first report new 2 cm (150 mas resolution using the VLA) and 6 cm (2 mas resolution using the VLBA) radio observations of the previously unobserved nuclei in our samples and then present results on the complete survey. We find that almost half of all LINERs and low-luminosity Seyferts have flat-spectrum radio cores when observed at 150 mas resolution. Higher (2 mas) resolution observations of a flux-limited subsample have provided a 100% (16 of 16) detection rate of pc-scale radio cores, with implied brightness temperatures ∼>108 K. The five LLAGNs with the highest core radio fluxes also have pc-scale “jets”.
    [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]
  • Nova Report 2006-2007
    NOVA REPORTNOVA 2006 - 2007 NOVA REPORT 2006-2007 Illustration on the front cover The cover image shows a composite image of the supernova remnant Cassiopeia A (Cas A). This object is the brightest radio source in the sky, and has been created by a supernova explosion about 330 year ago. The star itself had a mass of around 20 times the mass of the sun, but by the time it exploded it must have lost most of the outer layers. The red and green colors in the image are obtained from a million second observation of Cas A with the Chandra X-ray Observatory. The blue image is obtained with the Very Large Array at a wavelength of 21.7 cm. The emission is caused by very high energy electrons swirling around in a magnetic field. The red image is based on the ratio of line emission of Si XIII over Mg XI, which brings out the bi-polar, jet-like, structure. The green image is the Si XIII line emission itself, showing that most X-ray emission comes from a shell of stellar debris. Faintly visible in green in the center is a point-like source, which is presumably the neutron star, created just prior to the supernova explosion. Image credits: Creation/compilation: Jacco Vink. The data were obtained from: NASA Chandra X-ray observatory and Very Large Array (downloaded from Astronomy Digital Image Library http://adil.ncsa.uiuc. edu). Related scientific publications: Hwang, Vink, et al., 2004, Astrophys. J. 615, L117; Helder and Vink, 2008, Astrophys. J. in press.
    [Show full text]
  • Synapses of Active Galactic Nuclei: Comparing X-Ray and Optical Classifications Using Artificial Neural Networks?
    A&A 567, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201322592 & c ESO 2014 Astrophysics Synapses of active galactic nuclei: Comparing X-ray and optical classifications using artificial neural networks? O. González-Martín1;2;??, D. Díaz-González3, J. A. Acosta-Pulido1;2, J. Masegosa4, I. E. Papadakis5;6, J. M. Rodríguez-Espinosa1;2, I. Márquez4, and L. Hernández-García4 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38205 La Laguna, Spain 3 Shidix Technologies, 38320, La Laguna, Spain 4 Instituto de Astrofísica de Andalucía, CSIC, C/ Glorieta de la Astronomía s/n, 18005 Granada, Spain 5 Physics Department, University of Crete, PO Box 2208, 710 03 Heraklion, Crete, Greece 6 IESL, Foundation for Research and Technology, 711 10 Heraklion, Crete, Greece Received 2 September 2013 / Accepted 3 April 2014 ABSTRACT Context. Many classes of active galactic nuclei (AGN) have been defined entirely through optical wavelengths, while the X-ray spectra have been very useful to investigate their inner regions. However, optical and X-ray results show many discrepancies that have not been fully understood yet. Aims. The main purpose of the present paper is to study the synapses (i.e., connections) between X-ray and optical AGN classifications. Methods. For the first time, the newly implemented efluxer task allowed us to analyse broad band X-ray spectra of a sample of emission-line nuclei without any prior spectral fitting. Our sample comprises 162 spectra observed with XMM-Newton/pn of 90 lo- cal emission line nuclei in the Palomar sample.
    [Show full text]
  • New Type of Black Hole Detected in Massive Collision That Sent Gravitational Waves with a 'Bang'
    New type of black hole detected in massive collision that sent gravitational waves with a 'bang' By Ashley Strickland, CNN Updated 1200 GMT (2000 HKT) September 2, 2020 <img alt="Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image." class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190516104725-ngc-4485-nasa-super-169.jpg"> Photos: Wonders of the universe Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image. Hide Caption 98 of 195 <img alt="Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. " class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190502151952-0502-wonders-of-the-universe-super-169.jpg"> Photos: Wonders of the universe Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. Hide Caption 99 of 195 <img alt="A ground-based telescope's view of the Large Magellanic Cloud, a neighboring galaxy of our Milky Way.
    [Show full text]
  • (Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 Umi
    Herschel 400 Observing List, evening of 2015 Oct 15 at Cleveland, Ohio Sunset 17:49, Twilight ends 19:18, Twilight begins 05:07, Sunrise 06:36, Moon rise 09:51, Moon set 19:35 Completely dark from 19:35 to 05:07. Waxing Crescent Moon. All times local (EST). Listing All Classes visible above the perfect horizon and in twilight or moonlight before 23:59. Cls Primary ID Alternate ID Con RA (Ap) Dec (Ap) Mag Size Distance Rise Transit Set Gal NGC 6217 Arp 185 UMi 16h31m48.9s +78°10'18" 11.9 2.6'x 2.1' - 15:22 - Gal NGC 2655 Arp 225 Cam 08h57m35.6s +78°09'22" 11 4.5'x 2.8' - 7:46 - Gal NGC 3147 MCG 12-10-25 Dra 10h18m08.0s +73°19'01" 11.3 4.1'x 3.5' - 9:06 - PNe NGC 40 PN G120.0+09.8 Cep 00h13m59.3s +72°36'43" 10.7 1.0' 3700 ly - 23:03 - Gal NGC 2985 MCG 12-10-6 UMa 09h51m42.0s +72°12'01" 11.2 3.8'x 3.1' - 8:39 - Gal Cigar Galaxy M 82 UMa 09h57m06.5s +69°35'59" 9 9.3'x 4.4' 12.0 Mly - 8:45 - Gal NGC 1961 Arp 184 Cam 05h43m51.6s +69°22'44" 11.8 4.1'x 2.9' 180.0 Mly - 4:32 - Gal NGC 2787 MCG 12-9-39 UMa 09h20m40.5s +69°07'51" 11.6 3.2'x 1.8' - 8:09 - Gal NGC 3077 MCG 12-10-17 UMa 10h04m31.3s +68°39'09" 10.6 5.1'x 4.2' 12.0 Mly - 8:52 - Gal NGC 2976 MCG 11-12-25 UMa 09h48m29.2s +67°50'21" 10.8 6.0'x 3.1' 15.0 Mly - 8:36 - PNe Cat's Eye Nebula NGC 6543 Dra 17h58m31.7s +66°38'25" 8.3 22" 4400 ly - 16:49 - Open NGC 7142 Collinder 442 Cep 21h45m34.2s +65°51'16" 10 12.0' 5500 ly - 20:35 - Gal NGC 2403 MCG 11-10-7 Cam 07h38m20.9s +65°33'36" 8.8 20.0'x 10.0' 11.0 Mly - 6:26 - Open NGC 637 Collinder 17 Cas 01h44m15.4s +64°07'07" 7.3 3.0' 7000 ly - 0:33
    [Show full text]
  • Globular Cluster Systems of Six Shell Galaxies
    A&A 458, 53–67 (2006) Astronomy DOI: 10.1051/0004-6361:20054606 & c ESO 2006 Astrophysics Globular cluster systems of six shell galaxies G. Sikkema1,R.F.Peletier1, D. Carter2, E. A. Valentijn1, and M. Balcells3 1 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands e-mail: [email protected] 2 Astrophysics Research Institute, Liverpool John Moores University, 12 Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK 3 Instituto de Astrofísica de Canarias, vía Láctea s/n, La Laguna 38200, Spain Received 29 November 2005 / Accepted 14 June 2006 ABSTRACT Context. Shells in Elliptical Galaxies are faint, sharp-edged features, believed to provide evidence of a recent (∼0.5−2 × 109 years ago) merger event. We analyse the Globular Cluster (GC) systems of six shell elliptical galaxies, to examine the effects of mergers upon the GC formation history. Aims. We examine the colour distributions, and investigate differences between red and blue globular cluster populations. We present luminosity functions, spatial distributions and specific frequencies (SN ) at 50 kpc radius for our sample. Methods. We present V and I magnitudes for cluster candidates measured with the HST Advanced Camera for Surveys (ACS). Galaxy background light is modelled and removed, and magnitudes are measured in 8 pixel (0.4 arcsec) diameter apertures. Background contamination is removed using counts from Hubble Deep Field South. Results. We find that the colour distributions for NGC 3923 and NGC 5982 have a bimodal form typical of bright ellipticals, with peaks near V − I = 0.92 ± 0.04 and V − I = 1.18 ± 0.06.
    [Show full text]
  • Making a Sky Atlas
    Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.
    [Show full text]
  • Ngc Catalogue Ngc Catalogue
    NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39
    [Show full text]
  • STARDUST Newsletter of the Royal Astronomical Society of Canada Edmonton Centre
    STARDUST Newsletter of the Royal Astronomical Society of Canada Edmonton Centre May 2011 Volume 57 Issue 9 Maria Vergara of Oliver School stands by her award-winning astronomy display. Details on page 4. Inside this Issue Contact Information................................................................................................................................................page 2 Upcoming Events, Meetings, Deadlines, Announcements.....................................................................................page 3 President's Report....................................................................................................................................................page 3 Best Astronomy Award 2011..................................................................................................................................page 4 Book Donations.......................................................................................................................................................page 4 GA Logo Contest! ..................................................................................................................................................Page 5 Observers Report.....................................................................................................................................................page 5 The Planets..............................................................................................................................................................page 6 Stardust
    [Show full text]
  • Constellation : Dra=Le Dragon Nom Distance (Al) Magnitude Type Spectr
    Le Dragon 1 Constellation : Dra=le Dragon Nom distance (al) magnitude type spectr. remarques ααα ou Thuban 200 3,6 M0III βββ ou Alwaïd ou Rastaban 400 2,79 G2Ib γγγ ou Etamin ou Eltanin 150 2,24 K5III δδδ ou Nodus II ou Al Taïs 99 3,07 G9III ννν ou Kuma 100 4,9 et... A6V et.. binaire A: blanche 4,9 A5 B à à 62" ξξξ ou Grumium 200 3,8 K2III ζζζ ou Nodus I ou Adhibah 300 3,17 B6III εεε ou Tyl 146 3,8 et K0III et Etoile double, A : jaune-orange 7 K0 B à 3,4" ιιι ou Edasish ou Ed Asic 100 3.42 et K2IIIet étoile binaire : A : orange 8.87 K7 B à 4'14" A possède 1 planète extrasolaire b : m=8,6MJup. p=550j. d=1,34ua) λλλ ou Gianfar ou Giauzar 125 4,1 M0III ΦΦΦ 270 4,2 A0 Le Dragon 2 σσσ ou ΑΑΑl safi 18 4,7 K0V µµµ ou Arrabis 88 5.66 et F7Vet Binaire A jaune 5.69 F5 B à 2,3" de période 482 ans ψψψ1ψ1 ou Dsiban 72 4,6 et F5IV et binaire A : blanche 5,6 F8 B à 30" ψψψ2ψ222 720 5,4 F2II ηηη 88 2,73 G8III étoile triple (difficile à voir) θθθ 64 4,1 F8IV κκκ 400 3,9 B6III οοο 320 4,6 et G9III Etoile double A : orange 8,2 B : rouge-orange. à 37" Etoile triple liée. 17 et 398 5.38 et B9V 17 A bleue 6.42 A2 B à 3.2" 16 5.50 B9V 16 à 1'29" de 17 39 189 5 et A4 et Etoile triple, A : blanche 7,9 et F8 et B : à 1'30"de A 7,5 A2 C à 3,7" de A Etoile triple 41 et 173 5,74 K2V 41 A : jaune et variable 5,7 F5 B A 18" 40 166 F7 .40 à 3'44" de 41 La Petite Reine un objet STAR d'Harrington , (Little Queen), astérisme ayant la forme d'un W, comme la Grande Reine : Cassiopée.
    [Show full text]