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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 . -
Cerncourier-April17 213X282 E.Indd 1 22.02.17 11:37 Uhr CERNCOURIER Www
CERN Courier April 2017 Astrowatch Optimize your LLRF with excellent jitter perfor- C OMPILED BY M ARC TÜRLER , ISDC AND O BSERVATORY OF THE U NIVERSITY OF G ENEVA , AND CHIPP, U NIVERSITY OF Z URICH Gravitational lens challenges cosmic expansion mance measurements Low phase noise oscillators are essential in the development, verification Using galaxies as vast gravitational lenses, . agreement with other recent determinations and optimization of every particle accelerator. In a single instrument the et al Visit us at an international group of astronomers has in the local universe using classical ¸FSWP provides best-in-class noise and jitter sensitivity, ultra-fast made an independent measurement of how cosmic-distance ladder methods. One of measurement speed and the benefit of an internal low phase noise oscillator. IPAC in Copenhagen, fast the universe is expanding. The newly these, by Adam Riess and collaborators, finds measured expansion rate is consistent with an even higher value of the Hubble constant ❙ Superior jitter measurement down to 0.3 Hz offset Booth 46 and 47 –1 –1 earlier findings in the local universe based on (H0 = 73.2±1.7 km s Mpc ) and has therefore ❙ Measurement of additive phase noise at the push of a button more traditional methods, but intriguingly triggered a lot of interest in recent months. ❙ Internal low phase noise oscillator coupled with enhanced cross- ESA/Hubble; NASA, Suyu remains higher than the value derived by the The reason is that such values are in correlation functionality Planck satellite – a tension that could hint at tension with the precise determination new physics. -
Rak a Malý Lev Na Rozhraní Zimní a Jarní Oblohy Uprostřed Jarního Trojúhelníku Leží Malé Souhvězdí, Po Němž Máme Na Zemi Pojmenovaný Obratník
Pozorování © Nigel Sharp, Mark Hanna/NOAO/AURA/NSF Rak a Malý lev Na rozhraní zimní a jarní oblohy uprostřed jarního trojúhelníku leží malé souhvězdí, po němž máme na Zemi pojmenovaný obratník. Souhvězdí Raka. V minulosti totiž právě v tomto souhvězdí dosahovalo Slunce největší deklinace. Dnes, díky precesi, k tomu dochází v souhvězdí Blíženců. Rak je v antice zpodobňován jako krab pomáhající Hydře v boji proti Herkulovi. Chaldejci zde zase viděli místo, kudy sestupují duše na Zem, aby zde přijaly fyzické tělo. Ve starověkém Egyptě toto souhvězdí znali již v roce 2 000 př. n. l. Nenápadné souhvězdí Malého lva najdeme mezi Lvem a Velkou medvědicí. Toto nenápadné a ve městě v podstatě neviditelné souhvězdí se na oblohu dostalo až v novověku díky Janu Heveliovi, definitivně se Malý lev na obloze zabydlel až ve 20. století, kdy byla na Valném shromáždění IAU přijata dnešní podoba souhvězdí. M 67 Rak leží na ekliptice, proto můžeme být někdy svědky zákrytu jeho hvězd Měsícem, asi 580 ly. Skutečný rektascenze deklinace jasnost rozměry výjimečně i planetou. Nejjasnější hvězda, průměr je asi 13 ly. α Cnc, se jmenuje Acubens, což znamená Stáří se odhaduje na α Cnc 8h 58,9m 11° 50′ 4,3+11,8 11″ „klepeto“, a dosahuje 4. velikosti. Jedná se 730 mil. let. První ι Cnc 8h 47,1m 28° 44′ 4,1+6,0 30″ o dvojhvězdu. Ve vzdálenosti 11″ se nachází pozoroval M 44 již druhá složka 11. velikosti. Celý systém je Galileo Galilei a roz- M 44 8h 40m 19° 40′ 3,5 95′ od nás vzdálen asi 170 ly. -
CERN Courier – Digital Edition Welcome to the Digital Edition of the April 2017 Issue of CERN Courier
I NTERNATIONAL J OURNAL OF H IGH -E NERGY P HYSICS CERNCOURIER WELCOME V OLUME 5 7 N UMBER 3 A PRIL 2 0 1 7 CERN Courier – digital edition Welcome to the digital edition of the April 2017 issue of CERN Courier. Theory in motion Few scientific disciplines enjoy such a close connection with mathematics as particle physics, and at the heart of this relationship lies quantum field theory. Quantum electrodynamics famously predicts quantities, such as the anomalous magnetic moment of the electron, which agree with observations at the level of 10 decimal places, while the Higgs boson existed on paper half a century before the Large Hadron Collider (LHC) flushed it out for real. Driven by the strong performance of the LHC experiments, there has been a burst of activity in recent months concerning next-to-next-to-leading order (NNLO) calculations in quantum chromodynamics to ensure that theory keeps up with the precision of LHC measurements. As the cover feature in this issue explains, cracking the complex NNLO problem demands novel algorithms, mathematical ingenuity and computational muscle. Theorists are also trying to make sense of a number of “exotic” hadrons that have turned up in recent years in experiments such as LHCb and which do not naturally fit the simple quark model. Sticking with the strong-force theme, we also report on 30 years of heavy-ion physics and how recent measurements at the LHC and RHIC are closing in on the evolution of the quark–gluon plasma. Finally, we describe new forward detectors that from this year will allow the LHC to analyse photon–photon collisions in the ongoing search for new physics. -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
National Gypsum Construction Guide
12TH EDITION 09 20 00/NGC National Gypsum Construction Guide ® HOW TO USE THE NATIONAL GYPSUM COMPANY GYPSUM CONSTRUCTION GUIDE NATIONAL GYPSUM PRODUCTS FOR ALL YOUR TRADEMARKS BUILDING NEEDS Your National Gypsum Company “Gypsum Construction The following names are trademarks owned by National Guide” has been carefully developed to provide you with a Gypsum Company or its subsidiary, National Gypsum comprehensive guide to the entire range of National Gypsum Properties, LLC: products. We have attempted to give you the most accurate, DURABASE® KAL-KOTE® up-to-date information in a clear, concise, easy-to-read DURASAN® KAL-MESH® format. Because it is important for us to ensure our guide is ® ® user-friendly, we welcome your comments. Please write EASY FINISH MULTI-FLEX us at: National Gypsum Company Technical Services EDGE GRIPTM NGC® Department, 2001 Rexford Road, Charlotte, N.C. 28211 or EXCELLENCE ACROSS 1-800 NATIONAL® ® call 1-800-NATIONAL (1-800-628-4662) U.S.A. or Canada. THE BOARD PERFECT SPRAY® 2 For your easy reference and accessibility to this information, we e XP™ PERMABASE® ® have placed all of our Sweet’s material in this section. For a E-Z STRIP PERMABASE FLEX® complete copy of our literature call 1-800-NATIONAL. ® FIRE-SHIELD PROFORM® TM FIRE-SHIELD C SEASPRAY MVR® CAD DRAWINGS AND SPECIFICATIONS ® GOLD BOND SHAFTLINER® ® To assist you in your design process, all CAD drawings and GOLD BOND 54 SHAFTLINER XP® specifications are available at www.nationalgypsum.com. ® GRIDMARX SOUNDBREAK™ Computer aided design (CAD) drawings are in DXF, DWG and ® GRIDSTONE STA-SMOOTH® GIF file formats. -
An Analysis of the Environment and Gas Content of Luminous Infrared Galaxies
Abstract Title of Dissertation: An Analysis of the Environment and Gas Content of Luminous Infrared Galaxies Bevin Ashley Zauderer, Doctor of Philosophy, 2010 Dissertation directed by: Professor Stuart N. Vogel Department of Astronomy Luminous and ultraluminous infrared galaxies (U/LIRGs) represent a population among the most extreme in our universe, emitting an extraordinary amount of energy at infrared wavelengths from dust heated by prolific star formation and/or an active galactic nucleus (AGN). We present three investigations of U/LIRGs to better understand their global environment, their interstellar medium properties, and their nuclear region where molecular gas feeds a starburst or AGN. To study the global environment, we compute the spatial cluster-galaxy amplitude, Bgc, for 76 z < 0.3 ULIRGs. We find the environment of ULIRGs is similar to galaxies in the field. Comparing our results with other galactic populations, we conclude that ULIRGs might be a phase in the lives of AGNs and QSOs, but not all moderate-luminosity QSOs necessarily pass through a ULIRG phase. To study the interstellar medium properties, we observe H I and other spectral lines in 77 U/LIRGs with the Arecibo telescope. We detect H I in emission or absorption in 61 of 77 galaxies, 52 being new detections. We compute the implied gas mass for galaxies with emission, and optical depths and column densities for the seven sources with absorption detections. To study the molecular gas in the nuclear region of LIRG Arp 193, sub-arcsecond scale angular resolution is required and a method of atmospheric phase correction imperative. We present results of a large experiment observing bright quasars to test the limitations of the Combined Array for Research in Millimeter Astronomy’s Paired Antenna Calibration System (C-PACS) for atmospheric phase correction. -
Binocular Challenges
This page intentionally left blank Cosmic Challenge Listing more than 500 sky targets, both near and far, in 187 challenges, this observing guide will test novice astronomers and advanced veterans alike. Its unique mix of Solar System and deep-sky targets will have observers hunting for the Apollo lunar landing sites, searching for satellites orbiting the outermost planets, and exploring hundreds of star clusters, nebulae, distant galaxies, and quasars. Each target object is accompanied by a rating indicating how difficult the object is to find, an in-depth visual description, an illustration showing how the object realistically looks, and a detailed finder chart to help you find each challenge quickly and effectively. The guide introduces objects often overlooked in other observing guides and features targets visible in a variety of conditions, from the inner city to the dark countryside. Challenges are provided for viewing by the naked eye, through binoculars, to the largest backyard telescopes. Philip S. Harrington is the author of eight previous books for the amateur astronomer, including Touring the Universe through Binoculars, Star Ware, and Star Watch. He is also a contributing editor for Astronomy magazine, where he has authored the magazine’s monthly “Binocular Universe” column and “Phil Harrington’s Challenge Objects,” a quarterly online column on Astronomy.com. He is an Adjunct Professor at Dowling College and Suffolk County Community College, New York, where he teaches courses in stellar and planetary astronomy. Cosmic Challenge The Ultimate Observing List for Amateurs PHILIP S. HARRINGTON CAMBRIDGE UNIVERSITY PRESS Cambridge, New York, Melbourne, Madrid, Cape Town, Singapore, Sao˜ Paulo, Delhi, Dubai, Tokyo, Mexico City Cambridge University Press The Edinburgh Building, Cambridge CB2 8RU, UK Published in the United States of America by Cambridge University Press, New York www.cambridge.org Information on this title: www.cambridge.org/9780521899369 C P. -
190 Index of Names
Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea -
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 -
The Sudden Death of the Nearest Quasar Hannyʼs Voorwerp and Its Cousins Shed Light on Black Hole Accretion
The Sudden Death of the Nearest Quasar Hannyʼs Voorwerp and its cousins shed light on black hole accretion Dan Evans Harvard-Smithsonian Center for Astrophysics & Elon University Key collaborators: Kevin Schawinski, William Keel, Meg Urry, Shanil Virani, Chris Lintott, Priyamvada Natarajan Hanny van Arkel, Richard Proctor, Hannah Hutchins, Elizabeth Baeten, Massimo Mezzoprete, Elizabeth Siegel, Aida Berges, voyager1682002, Caro, Christian Manteuffel... 430,000+ Zooniverse Citizen Scientists Schawinski et al. 2010, ApJ Letters, 724, L30 Science Questions What is the time scale on which quasar phases turn on and off? What do rapid “deaths” tell us about black hole accretion physics? Are “dead” quasars the real culprits in quasar feedback? Discovered by citizen scientist Hanny van Arkel in 2007 Named by GZ forum members after discoverer Spectroscopic Properties z=0.05 - same as IC 2497 Lintott, Schawinski et al. (2009) Spectroscopic Properties Low Density Gas: [S II] λ6717/6731 ratio is density sensitive and lies in the low density limit (ne < 50 cm−3) AGN Photoionized: He II λ4616 and [NeV] λλ3346,3426 + [OIII] imply high ionization parameter, log U = −2.2 (need v ~ 400km/s to get lines due to shock) Low Metallicity: [N II]/Hα and [S II]/Hα indicate low metallicity of ~0.1-0.2 Zsolar Lintott, Schawinski et al. (2009) 1.4 GHz continuum 9 10 Msun of HI From: WSRT, Jozsa et al. (2010) HST F184W How luminous? • Template SED from Elvis et al. (1994) • Scaled SED to match the minimum UV luminosity to ionize the Voorwerp • Find Lbol ~ 1046 erg/s • L2-10 keV ~ 8x1044 erg/s Quasar - Lbol ~1046 erg/s! Why donʼt we see a quasar? 1. -
Extended X-Ray Emission in the IC€2497 – Hanny's Voorwerp System
MNRAS 457, 3629–3636 (2016) doi:10.1093/mnras/stw230 Advance Access publication 2016 January 29 Extended X-ray emission in the IC 2497 – Hanny’s Voorwerp system: energy injection in the gas around a fading AGN Downloaded from https://academic.oup.com/mnras/article-abstract/457/4/3629/2589023 by Pontificia Universidad Catolica de Chile user on 11 June 2019 Lia F. Sartori,1‹ Kevin Schawinski,1‹ Michael Koss,1 Ezequiel Treister,2 W. Peter Maksym,3 William C. Keel,4 C. Megan Urry,5 Chris J. Lintott6 and O. Ivy Wong7 1Institute for Astronomy, Department of Physics, ETH Zurich,¨ Wolfgang-Pauli-Strasse 27, CH-8093 Zurich,¨ Switzerland 2Departamento de Astronom´ıa, Universidad de Concepcion,´ Casilla 160-C, Concepcion,´ Chile 3Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 4Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL 35487, USA 5Yale Center for Astronomy & Astrophysics, Physics Department, PO Box 208120, New Haven, CT 06520, USA 6Oxford Astrophysics, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK 7ICRAR, The University of Western Australia M468, 35 Stirling Highway, Crawley, WA 6009, Australia Accepted 2016 January 25. Received 2016 January 25; in original form 2015 November 27 ABSTRACT We present deep Chandra X-ray observations of the core of IC 2497, the galaxy associated with Hanny’s Voorwerpand hosting a fading AGN. We find extended soft X-ray emission from 42 44 −1 hot gas around the low intrinsic luminosity (unobscured) AGN (Lbol ∼ 10 –10 erg s ). The temperature structure in the hot gas suggests the presence of a bubble or cavity around the 54 55 fading AGN (Ebub ∼ 10 –10 erg).