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The Richness of Compact Radio Sources in NGC 6334D to F S.-N
Astronomy & Astrophysics manuscript no. main c ESO 2021 June 22, 2021 The richness of compact radio sources in NGC 6334D to F S.-N. X. Medina1, S. A. Dzib1, M. Tapia2, L. F. Rodríguez3, and L. Loinard3;4 1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany 2 Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, B. C., CP 22830, Mexico 3 Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia 58089, Mexico 4 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, CdMx C.P. 04510, Mexico e-mail: smedina, sdzib, @mpifr-bonn.mpg.de; [email protected]; l.rodriguez, and l.loinard, @crya.unam.mx Received 2017; ABSTRACT Context. The presence and properties of compact radio sources embedded in massive star-forming regions can reveal important physical properties about these regions and the processes occurring within them. The NGC 6334 complex, a massive star-forming region, has been studied extensively. Nevertheless, none of these studies has focused in its content in compact radio sources. Aims. Our goal here is to report on a systematic census of the compact radio sources toward NGC 6334, and their characteristics. This will be used to try and define their very nature. Methods. We use VLA C band (4–8 GHz) archive data with 000.36 (500 AU) of spatial resolution and noise level of 50 µJy bm−1 to carry out a systematic search for compact radio sources within NGC 6334. We also search for infrared counterparts to provide some constraints on the nature of the detected radio sources. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Scaling Mass Profiles Around Elliptical Galaxies Observed with Chandra
Scaling Mass Profiles around Elliptical Galaxies Observed with Chandra and XMM-Newton Y. Fukazawa1, J. G. Betoya-Nonesa1, J. Pu1, A. Ohto1, and N. Kawano1 Department of Physical Science, School of Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima, Hiroshima 739-8526 [email protected] ABSTRACT We investigated the dynamical structure of 53 elliptical galaxies, based on the Chandra archival X-ray data. In X-ray luminous galaxies, a temperature increases with radius and a gas density is systematically higher at the optical outskirts, indicating a presence of a significant amount of the group-scale hot gas. In contrast, X-ray dim galaxies show a flat or declining temperature profile against radius and the gas density is relatively lower at the optical outskirts. Thus it is found that X-ray bright and faint elliptical galaxies are clearly distinguished by the temperature and gas density profile. The mass profile is well scaled by a virial radius r200 rather than an optical-half radius re, and is quite similar at (0.001 − 0.03)r200 between X-ray luminous and dim galaxies, and smoothly connects to those of clusters of galaxies. At the inner region of (0.001 − 0.01)r200 or (0.1 − 1)re, the mass profile well traces a stellar mass with a constant mass-to- light ratio of M/LB =3 − 10(M⊙/L⊙). M/LB ratio of X-ray bright galaxies rises up steeply beyond 0.01r200, and thus requires a presence of massive dark matter halo. From the deprojection analysis combined with the XMM-Newton data, we arXiv:astro-ph/0509521v1 18 Sep 2005 found that X-ray dim galaxies, NGC 3923, NGC 720, and IC 1459, also have a high M/LB ratio of 20–30 at 20 kpc, comparable to that of X-ray luminous galaxies. -
Jrasc-August'99 Text
Publications and Products of August/août 1999 Volume/volume 93 Number/numero 4 [678] The Royal Astronomical Society of Canada Observer’s Calendar — 2000 This calendar was created by members of the RASC. All photographs were taken by amateur astronomers using ordinary camera lenses and small telescopes and represent a wide spectrum of objects. An informative caption accompanies every photograph. This year all of the photos are in full colour. The Journal of the Royal Astronomical Society of Canada Le Journal de la Société royale d’astronomie du Canada It is designed with the observer in mind and contains comprehensive astronomical data such as daily Moon rise and set times, significant lunar and planetary conjunctions, eclipses, and meteor showers. The 1999 edition received two awards from the Ontario Printing and Imaging Association, Best Calendar and the Award of Excellence. (designed and produced by Rajiv Gupta). Price: $13.95 (members); $15.95 (non-members) (includes taxes, postage and handling) The Beginner’s Observing Guide This guide is for anyone with little or no experience in observing the night sky. Large, easy to read star maps are provided to acquaint the reader with the constellations and bright stars. Basic information on observing the moon, planets and eclipses through the year 2005 is provided. There is also a special section to help Scouts, Cubs, Guides and Brownies achieve their respective astronomy badges. Written by Leo Enright (160 pages of information in a soft-cover book with otabinding which allows the book to lie flat). Price: $15 (includes taxes, postage and handling) Looking Up: A History of the Royal Astronomical Society of Canada Published to commemorate the 125th anniversary of the first meeting of the Toronto Astronomical Club, “Looking Up — A History of the RASC” is an excellent overall history of Canada’s national astronomy organization. -
407 a Abell Galaxy Cluster S 373 (AGC S 373) , 351–353 Achromat
Index A Barnard 72 , 210–211 Abell Galaxy Cluster S 373 (AGC S 373) , Barnard, E.E. , 5, 389 351–353 Barnard’s loop , 5–8 Achromat , 365 Barred-ring spiral galaxy , 235 Adaptive optics (AO) , 377, 378 Barred spiral galaxy , 146, 263, 295, 345, 354 AGC S 373. See Abell Galaxy Cluster Bean Nebulae , 303–305 S 373 (AGC S 373) Bernes 145 , 132, 138, 139 Alnitak , 11 Bernes 157 , 224–226 Alpha Centauri , 129, 151 Beta Centauri , 134, 156 Angular diameter , 364 Beta Chamaeleontis , 269, 275 Antares , 129, 169, 195, 230 Beta Crucis , 137 Anteater Nebula , 184, 222–226 Beta Orionis , 18 Antennae galaxies , 114–115 Bias frames , 393, 398 Antlia , 104, 108, 116 Binning , 391, 392, 398, 404 Apochromat , 365 Black Arrow Cluster , 73, 93, 94 Apus , 240, 248 Blue Straggler Cluster , 169, 170 Aquarius , 339, 342 Bok, B. , 151 Ara , 163, 169, 181, 230 Bok Globules , 98, 216, 269 Arcminutes (arcmins) , 288, 383, 384 Box Nebula , 132, 147, 149 Arcseconds (arcsecs) , 364, 370, 371, 397 Bug Nebula , 184, 190, 192 Arditti, D. , 382 Butterfl y Cluster , 184, 204–205 Arp 245 , 105–106 Bypass (VSNR) , 34, 38, 42–44 AstroArt , 396, 406 Autoguider , 370, 371, 376, 377, 388, 389, 396 Autoguiding , 370, 376–378, 380, 388, 389 C Caldwell Catalogue , 241 Calibration frames , 392–394, 396, B 398–399 B 257 , 198 Camera cool down , 386–387 Barnard 33 , 11–14 Campbell, C.T. , 151 Barnard 47 , 195–197 Canes Venatici , 357 Barnard 51 , 195–197 Canis Major , 4, 17, 21 S. Chadwick and I. Cooper, Imaging the Southern Sky: An Amateur Astronomer’s Guide, 407 Patrick Moore’s Practical -
The Exotic Eclipsing Nucleus of the Ring Planetary Nebula Suwt2
The Exotic Eclipsing Nucleus of the Ring Planetary Nebula SuWt 21 K. Exter,2 Howard E. Bond,3,4 K. G. Stassun5,6 B. Smalley,7 P. F. L. Maxted,7 and D. L. Pollacco8 Received ; accepted 1Based in part on observations obtained with the SMARTS Consortium 1.3- and 1.5- m telescopes located at Cerro Tololo Inter-American Observatory, Chile, and with ESO Telescopes at the La Silla Observatory 2Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA. Current address: Institute voor Sterrenkunde, Katholieke Universiteit Leuven, Leuven, Bel- gium; [email protected] 3Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA; [email protected] 4Visiting astronomer, Cerro Tololo Inter-American Observatory, National Optical As- tronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, under contract with the National Science Foundation. Guest Observer with the arXiv:1009.1919v1 [astro-ph.SR] 10 Sep 2010 International Ultraviolet Explorer, operated by the Goddard Space Flight Center, National Aeronautics and Space Administration. 5Dept. of Physics and Astronomy, Vanderbilt University, Nashville, TN 32735, USA 6Department of Physics, Fisk University, 1000 17th Ave. N, Nashville, TN 37208, USA 7Astrophysics Group, Chemistry & Physics, Keele University, Staffordshire, ST5 5BG, UK 8Queen’s University Belfast, Belfast, UK –2– ABSTRACT SuWt 2 is a planetary nebula (PN) consisting of a bright ionized thin ring seen nearly edge-on, with much fainter bipolar lobes extending perpendicularly to the ring. It has a bright (12th-mag) central star, too cool to ionize the PN, which we discovered in the early 1990’s to be an eclipsing binary. -
The Low-Mass Populations in OB Associations
The Low-mass Populations in OB Associations Cesar´ Briceno˜ Centro de Investigaciones de Astronom´ıa Thomas Preibisch Max-Planck-Institut fur¨ Radioastronomie William H. Sherry National Optical Astronomy Observatory Eric E. Mamajek Harvard-Smithsonian Center for Astrophysics Robert D. Mathieu University of Wisconsin - Madison Frederick M. Walter Stony Brook University Hans Zinnecker Astrophysikalisches Institut Potsdam Low-mass stars (0:1 . M . 1 M ) in OB associations are key to addressing some of the most fundamental problems in star formation. The low-mass stellar populations of OB associa- tions provide a snapshot of the fossil star-formation record of giant molecular cloud complexes. Large scale surveys have identified hundreds of members of nearby OB associations, and revealed that low-mass stars exist wherever high-mass stars have recently formed. The spatial distribution of low-mass members of OB associations demonstrate the existence of significant substructure (”subgroups”). This ”discretized” sequence of stellar groups is consistent with an origin in short-lived parent molecular clouds within a Giant Molecular Cloud Complex. The low-mass population in each subgroup within an OB association exhibits little evidence for significant age spreads on time scales of ∼ 10 Myr or greater, in agreement with a scenario of rapid star formation and cloud dissipation. The Initial Mass Function (IMF) of the stellar populations in OB associations in the mass range 0:1 . M . 1 M is largely consistent with the field IMF, and most low-mass pre-main sequence stars in the solar vicinity are in OB associations. These findings agree with early suggestions that the majority of stars in the Galaxy were born in OB associations. -
MY SO October Showdown Rules
S P A C E - O C T O B E R 2 0 2 0 MY SO STEM SHOWDOWN C O N T E N T , R E C O M M E N D E D M A T E R I A L S & S C O R I N G STEM SHOWDOWN CONTENT The STEM Showdown will consist of a series of online multiple-choice questions. Middle school (Grade 6-9) participant questions will center around the properties and evolution of stars and galaxies as well as their observation using different portions of the electromagnetic spectrum (e.g., Radio, Infrared, Visible, Ultraviolet, X-Ray, Gamma Ray). While high school (Grades 9-12) participants will focus on Star and Galaxy Formation and Evolution. A Showdown participant will have 55- minutes to answer as many questions as possible. The middle school (Grades 6-9) content and skills covered by the Showdown this month is as follows: 1.Stellar and galactic evolution 2.Spectral classification of stars 3.Hubble classification of galaxies 4.Observation using multiple portions of the electromagnetic spectrum 5.The relationship between stellar temperature, radius, and luminosity 6.Magnitude and luminosity scales, distance modulus, inverse square law 7.Identification of the stars, constellations, and deep sky objects included in the list below as they appear on star charts, H-R diagrams, portable star labs, photos, or planetariums. Note: Constellations are underlined; Stars are boldface; Deep Sky Objects are italicized. a.Andromeda: M31 (Andromeda Galaxy) b.Aquila: Altair c.Auriga: Capella d.Bootes: Arcturus e.Cancer: DLA0817g f.Canis Major: Sirius g.Canis Minor: Procyon h.Centaurus: NGC5128 i.Coma Berenices: NGC4676, NGC4555 j.Corvus: NGC4038/NGC4039 k.Crux: Dragonfish Nebula l.Cygnus: Deneb m.Dorado: 30 Doradus, LMC n.Gemini: Castor, Pollux o.Lyra: Vega p.Ophiuchus: Zeta Ophiuchi, Rho Ophiuchi cloud complex q.Orion: Betelgeuse, Rigel & M42 (Orion Nebula) r.Perseus: Algol, NGC1333 Science Olympiad, Inc. -
NGC 6334 and NGC 6357: Hα Kinematics and the Nature of the H II Regions
A&A 587, A135 (2016) Astronomy DOI: 10.1051/0004-6361/201424484 & c ESO 2016 Astrophysics NGC 6334 and NGC 6357: Hα kinematics and the nature of the H II regions D. Russeil1,J.Tigé1,C.Adami1, L. D. Anderson2,3,N.Schneider4,5,A.Zavagno1,M.R.Samal1,P.Amram1, L. Guennou6,1,E.LeCoarer7, A. Walsh8, S. N. Longmore9, and C. Purcell10 1 Aix Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille), UMR 7326, 13388 Marseille, France e-mail: [email protected] 2 Department of Physics and Astronomy, West Virginia University, Morgantown, West Virginia, WV 26506, USA 3 Adjunct Astronomer at the National Radio Astronomy Observatory, PO Box 2, Green Bank, WV 24944, USA 4 LAB/OASU, UMR 5804, CNRS, Université de Bordeaux, 33270 Floirac, France 5 I. Physik. Institut, University of Cologne, 50931 Cologne, Germany 6 IAS, CNRS & Université Paris Sud, Bâtiment 121, 91405 Orsay, France 7 Laboratoire d’Astrophysique de Grenoble, Université Joseph Fourier, CNRS, BP 53, 38041 Grenoble Cedex, France 8 International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, WA 6845, Australia 9 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 10 School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK Received 27 June 2014 / Accepted 18 December 2015 ABSTRACT Aims. NGC 6334 and NGC 6357 are amongst the most active, optically visible Galactic star-forming complexes. They are composed of several H ii regions that have a significant impact on their surrounding. The aim of this paper is to present a kinematic study of the optical H ii regions that belong to NGC 6334 and NGC 6357. -
Prime Focus (10-08)
Highlights of the October Sky. -- -- -- 1st -- -- -- Dusk: Thin crescent Moon visible low in WSW. Look PPrime Focuss 5º or 6º below Venus. A Publication of the Kalamazoo Astronomical Society -- -- -- 6th -- -- -- PM: Moon lower right of Jupiter. October 2008 -- -- -- 7th -- -- -- PM: Moon lower left of Jupiter. ThisThis MonthsMonths KAS EventsEvents -- -- -- 7th -- -- -- First Quarter Moon -- -- -- 14th -- -- -- General Meeting: Friday, October 3 @ 7:00 pm Full Moon Kalamazoo Math & Science Center - See Page 12 for Details -- -- -- 17th -- -- -- Dawn: Mercury visible 5º Observing Session: Saturday, October 4 @ 7:00 pm above the eastern horizon until the 30th. Overwhelming Open Clusters - Kalamazoo Nature Center st -- -- -- 21st -- -- -- Board Meeting: Sunday, October 5 @ 5:00 pm Last Quarter Moon Sunnyside Church - 2800 Gull Road - All Members Welcome AM: Orionid Meteor AM: Orionid Meteor Shower (10 -- 2020 meteorsmeteors per hour). Observing Session: Saturday, October 25 @ 7:00 pm The Great Square - Kalamazoo Nature Center -- -- -- 23rd -- -- -- Dawn: Waning Crescent Moon upper right of Alpha Leonis (Regulus). -- -- -- 24th -- -- -- Dawn: Waning Crescent InsideInside thethe Newsletter.Newsletter. .. .. Moon between Saturn and Regulus. September Meeting Minutes................ p. 2 -- -- -- 25th -- -- -- Board Meeting Minutes......................... p. 3 Dawn: Moon below Saturn Intelligent Imaging................................... p. 4 -- -- -- 25th -- -- -- Dusk: Venus is passing Astronomy Software............................ -
The MASSIVE Survey – X
MNRAS 479, 2810–2826 (2018) doi:10.1093/mnras/sty1649 Advance Access publication 2018 June 22 The MASSIVE Survey – X. Misalignment between kinematic and photometric axes and intrinsic shapes of massive early-type galaxies Irina Ene,1,2‹ Chung-Pei Ma,1,2 Melanie Veale,1,2 Jenny E. Greene,3 Jens Thomas,4 5 6,7 8 9 John P. Blakeslee, Caroline Foster, Jonelle L. Walsh, Jennifer Ito and Downloaded from https://academic.oup.com/mnras/article-abstract/479/2/2810/5042947 by Princeton University user on 27 June 2019 Andy D. Goulding3 1Department of Astronomy, University of California, Berkeley, CA 94720, USA 2Department of Physics, University of California, Berkeley, CA 94720, USA 3Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 4Max Plank-Institute for Extraterrestrial Physics, Giessenbachstr. 1, D-85741 Garching, Germany 5Dominion Astrophysical Observatory, NRC Herzberg Astronomy and Astrophysics, Victoria, BC V9E 2E7, Canada 6Sydney Institute for Astronomy, School of Physics A28, The University of Sydney, NSW 2006, Australia 7ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Australia 8George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA 9Department of Physics, University of California, San Diego, CA 92093, USA Accepted 2018 June 19. Received 2018 June 19; in original form 2018 January 30 ABSTRACT We use spatially resolved two-dimensional stellar velocity maps over a 107 × 107 arcsec2 field of view to investigate the kinematic features of 90 early-type galaxies above stellar mass 1011.5 M in the MASSIVE survey. -
2005 Astronomy Magazine Index
2005 Astronomy Magazine Index Subject index flyby of Titan, 2:72–77 Einstein, Albert, 2:30–53 Cassiopeia (constellation), 11:20 See also relativity, theory of Numbers Cassiopeia A (supernova), stellar handwritten manuscript found, 3C 58 (star remnant), pulsar in, 3:24 remains inside, 9:22 12:26 3-inch telescopes, 12:84–89 Cat's Eye Nebula, dying star in, 1:24 Einstein rings, 11:27 87 Sylvia (asteroid), two moons of, Celestron's ExploraScope telescope, Elysium Planitia (on Mars), 5:30 12:33 2:92–94 Enceladus (Saturn's moon), 11:32 2003 UB313, 10:27, 11:68–69 Cepheid luminosities, 1:72 atmosphere of water vapor, 6:22 2004, review of, 1:31–40 Chasma Boreale (on Mars), 7:28 Cassini flyby, 7:62–65, 10:32 25143 (asteroid), 11:27 chonrites, and gamma-ray bursts, 5:30 Eros (asteroid), 11:28 coins, celestial images on, 3:72–73 Eso Chasma (on Mars), 7:28 color filters, 6:67 Espenak, Fred, 2:86–89 A Comet Hale-Bopp, 7:76–79 extrasolar comets, 9:30 Aeolis (on Mars), 3:28 comets extrasolar planets Alba Patera (Martian volcano), 2:28 from beyond solar system, 12:82 first image of, 4:20, 8:26 Aldrin, Buzz, 5:40–45 dust trails of, 12:72–73 first light from, who captured, 7:30 Altair (star), 9:20 evolution of, 9:46–51 newly discovered low-mass planets, Amalthea (Jupiter's moon), 9:28 extrasolar, 9:30 1:68–71 amateur telescopes. See telescopes, Conselice, Christopher, 1:20 smallest, 9:26 amateur constellations whether have diamond layers, 5:26 Andromeda Galaxy (M31), 10:84–89 See also names of specific extraterrestrial life, 4:28–34 disk of stars surrounding, 7:28 constellations eyepieces, telescope.