365 Starry Nights by Chet Raymo Detailed Contents
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Art Matching
Art Matching Program Type: Demonstration or Classroom Audience Type: Grade 4–adult Program Description: Students explore how artists from different cultures have used art to represent space-related phenomena. Topics: Moon, space travel, art, stars, sky-watching Process Skills Focus: Critical thinking, observing, creativity. LEARNING OBJECTIVES For Next Generation Science Standards alignment, see end of outline. • Many artists are inspired by astronomy and the universe. • Cultures often have their own interpretations of the sky and celestial phenomena. • Art is one of many ways to capture our observations of and reflections on the sky. TIME REQUIRED Advance Prep Set Up Activity Clean Up 15 minutes 5 minutes 10 minutes 5 minutes SITE REQUIREMENTS • Table or other flat surface • Chairs (optional, but helpful for elderly or young audiences) Art Matching 1 Lenses on the Sky OMSI 2017 PROGRAM FORMAT Segment Format Time Introduction Large group discussion 2 min Art Matching Group Activity 5 min Wrap-Up Large group discussion 3 min SUPPLIES Permanent Supplies Amount Notes Laminated pages showing the artists 5 and their work Laminated cards showing 5 astronomical images ADVANCE PREPARATION • Print out, cut, and laminate the pages showing the artists and their work (at the end of the document). • Print out, cut, and laminate the five cards showing the astronomical images (at the end of the document). • Complete the activity to familiarize yourself with the process. SET UP Spread out the five pages showing the artists and their work on the table. Below the pages, place the five cards showing the astronomical objects. INTRODUCTION 2 minutes Let students speculate before offering answers to any questions. -
The HERACLES View of the H -To-HI Ratio in Galaxies
The HERACLES View of the H2-to-HI Ratio in Galaxies Adam Leroy (NRAO, Hubble Fellow) Fabian Walter, Frank Bigiel, the HERACLES and THINGS teams The Saturday Morning Summary • Star formation rate vs. gas relation on ~kpc scales breaks apart into: A relatively universal CO-SFR relation in nearby disks Systematic environmental scalings in the CO-to-HI ratio • The CO-to-HI ratio is a strong function of radius, total gas, and stellar surface density correlated with ISM properties: dust-to-gas ratio, pressure harder to link to dynamics: gravitational instability, arms • Interpretation: the CO-to-HI ratio traces the efficiency of GMC formation Density and dust can explain much of the observed behavior heracles Fabian Walter Erik Rosolowsky MPIA UBC Frank Bigiel Eva Schinnerer UC Berkeley THINGS plus… MPIA Elias Brinks Antonio Usero Gaelle Dumas U Hertfordshire OAN, Madrid MPIA Erwin de Blok Andreas Schruba Helmut Wiesemeyer U Cape Town IRAM … MPIA Rob Kennicutt Axel Weiss Karl Schuster Cambridge MPIfR IRAM Barry Madore Carsten Kramer Karin Sandstrom Carnegie IRAM MPIA Michele Thornley Daniela Calzetti Kelly Foyle Bucknell UMass MPIA Collaborators The HERA CO-Line Extragalactic Survey First maps Leroy et al. (2009) • IRAM 30m Large Program to map CO J = 2→1 line • Instrument: HERA receiver array operating at 230 GHz • 47 galaxies: dwarfs to starbursts and massive spirals -2 • Very wide-field (~ r25) and sensitive (σ ~ 1-2 Msun pc ) NGS The HI Nearby Galaxy Survey HI Walter et al. (2008), AJ Special Issue (2008) • VLA HI maps of 34 galaxies: -
Rosette Nebula and Monoceros Loop
Oshkosh Scholar Page 43 Studying Complex Star-Forming Fields: Rosette Nebula and Monoceros Loop Chris Hathaway and Anthony Kuchera, co-authors Dr. Nadia Kaltcheva, Physics and Astronomy, faculty adviser Christopher Hathaway obtained a B.S. in physics in 2007 and is currently pursuing his masters in physics education at UW Oshkosh. He collaborated with Dr. Nadia Kaltcheva on his senior research project and presented their findings at theAmerican Astronomical Society meeting (2008), the Celebration of Scholarship at UW Oshkosh (2009), and the National Conference on Undergraduate Research in La Crosse, Wisconsin (2009). Anthony Kuchera graduated from UW Oshkosh in May 2008 with a B.S. in physics. He collaborated with Dr. Kaltcheva from fall 2006 through graduation. He presented his astronomy-related research at Posters in the Rotunda (2007 and 2008), the Wisconsin Space Conference (2007), the UW System Symposium for Undergraduate Research and Creative Activity (2007 and 2008), and the American Astronomical Society’s 211th meeting (2008). In December 2009 he earned an M.S. in physics from Florida State University where he is currently working toward a Ph.D. in experimental nuclear physics. Dr. Nadia Kaltcheva is a professor of physics and astronomy. She received her Ph.D. from the University of Sofia in Bulgaria. She joined the UW Oshkosh Physics and Astronomy Department in 2001. Her research interests are in the field of stellar photometry and its application to the study of Galactic star-forming fields and the spiral structure of the Milky Way. Abstract An investigation that presents a new analysis of the structure of the Northern Monoceros field was recently completed at the Department of Physics andAstronomy at UW Oshkosh. -
Big Halpha Kinematical Sample of Barred Spiral Galaxies - I
BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle To cite this version: O. Hernandez, C. Carignan, P. Amram, L. Chemin, O. Daigle. BhaBAR: Big Halpha kinematical sample of BARred spiral galaxies - I. Fabry-Perot Observations of 21 galaxies. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2005, 360 Issue 4, pp.1201. 10.1111/j.1365-2966.2005.09125.x. hal-00014446 HAL Id: hal-00014446 https://hal.archives-ouvertes.fr/hal-00014446 Submitted on 26 Jan 2021 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Mon. Not. R. Astron. Soc. 360, 1201–1230 (2005) doi:10.1111/j.1365-2966.2005.09125.x BHαBAR: big Hα kinematical sample of barred spiral galaxies – I. Fabry–Perot observations of 21 galaxies O. Hernandez,1,2 † C. Carignan,1 P. Amram,2 L. Chemin1 and O. Daigle1 1Observatoire du mont Megantic,´ LAE, Universitede´ Montreal,´ CP 6128 succ. centre ville, Montreal,´ Quebec,´ Canada H3C 3J7 2Observatoire Astronomique de Marseille Provence et LAM, 2 pl. -
Filter Performance Comparisons for Some Common Nebulae
Filter Performance Comparisons For Some Common Nebulae By Dave Knisely Light Pollution and various “nebula” filters have been around since the late 1970’s, and amateurs have been using them ever since to bring out detail (and even some objects) which were difficult to impossible to see before in modest apertures. When I started using them in the early 1980’s, specific information about which filter might work on a given object (or even whether certain filters were useful at all) was often hard to come by. Even those accounts that were available often had incomplete or inaccurate information. Getting some observational experience with the Lumicon line of filters helped, but there were still some unanswered questions. I wondered how the various filters would rank on- average against each other for a large number of objects, and whether there was a “best overall” filter. In particular, I also wondered if the much-maligned H-Beta filter was useful on more objects than the two or three targets most often mentioned in publications. In the summer of 1999, I decided to begin some more comprehensive observations to try and answer these questions and determine how to best use these filters overall. I formulated a basic survey covering a moderate number of emission and planetary nebulae to obtain some statistics on filter performance to try to address the following questions: 1. How do the various filter types compare as to what (on average) they show on a given nebula? 2. Is there one overall “best” nebula filter which will work on the largest number of objects? 3. -
The Solar System and Its Place in the Galaxy in Encyclopedia of the Solar System by Paul R
Giant Molecular Clouds http://www.astro.ncu.edu.tw/irlab/projects/project.htm Æ Galactic Open Clusters Æ Galactic Structure Æ GMCs The Solar System and its Place in the Galaxy In Encyclopedia of the Solar System By Paul R. Weissman http://www.academicpress.com/refer/solar/Contents/chap1.htm Stars in the galactic disk have different characteristic velocities as a function of their stellar classification, and hence age. Low-mass, older stars, like the Sun, have relatively high random velocities and as a result c an move farther out of the galactic plane. Younger, more massive stars have lower mean velocities and thus smaller scale heights above and below the plane. Giant molecular clouds, the birthplace of stars, also have low mean velocities and thus are confined to regions relatively close to the galactic plane. The disk rotates clockwise as viewed from "galactic north," at a relatively constant velocity of 160-220 km/sec. This motion is distinctly non-Keplerian, the result of the very nonspherical mass distribution. The rotation velocity for a circular galactic orbit in the galactic plane defines the Local Standard of Rest (LSR). The LSR is then used as the reference frame for describing local stellar dynamics. The Sun and the solar system are located approxi-mately 8.5 kpc from the galactic center, and 10-20 pc above the central plane of the galactic disk. The circular orbit velocity at the Sun's distance from the galactic center is 220 km/sec, and the Sun and the solar system are moving at approximately 17 to 22 km/sec relative to the LSR. -
Binocular Universe: Sly Fox September 2010 Phil Harrington
Binocular Universe is available every month on Cloudynights.com Binocular Universe: Sly Fox September 2010 Phil Harrington ast month's Stellafane convention, held atop Breezy Hill outside of Springfield, Vermont, was the best in recent memory. The skies were the Lclearest we've had in years, giving us a chance to enjoy the beauty of the summer Milky Way, which stretched from horizon to horizon. Armed with my trusty 10x50 and 16x70 binoculars, I sat back in my reclining chair and swept the plane of our Galaxy in pursuit of some old friends and new conquests. Above: Summer star map from Star Watch by Phil Harrington Binocular Universe is available every month on Cloudynights.com Above: Finder chart for this month's Binocular Universe. Chart adapted from Touring the Universe through Binoculars Atlas (TUBA), www.philharrington.net/tuba.htm Binocular Universe is available every month on Cloudynights.com Here are a few gems I bumped into along the way as I viewed the tiny constellation of Vulpecula the Fox. Vulpecula is a faint summertime constellation wedged between Cygnus (the Swan) to the north and Sagitta (the Arrow) to the south. None of Vulpecula’s stars shine brighter than magnitude 4.5, so seeing a fox here is a tall order indeed. But the sly Fox holds many binocular treasures for those who the time to seek them out. Vulpecula was created in 1687 by the Polish astronomer Johannes Hevelius. His original drawing showed a small fox carrying a hapless goose in its mouth. He called the combination Vulpecula et Anser ("the little fox and the goose"). -
CARMENES Input Catalogue of M Dwarfs IV. New Rotation Periods from Photometric Time Series
Astronomy & Astrophysics manuscript no. pk30 c ESO 2018 October 9, 2018 CARMENES input catalogue of M dwarfs IV. New rotation periods from photometric time series E. D´ıezAlonso1;2;3, J. A. Caballero4, D. Montes1, F. J. de Cos Juez2, S. Dreizler5, F. Dubois6, S. V. Jeffers5, S. Lalitha5, R. Naves7, A. Reiners5, I. Ribas8;9, S. Vanaverbeke10;6, P. J. Amado11, V. J. S. B´ejar12;13, M. Cort´es-Contreras4, E. Herrero8;9, D. Hidalgo12;13;1, M. K¨urster14, L. Logie6, A. Quirrenbach15, S. Rau6, W. Seifert15, P. Sch¨ofer5, and L. Tal-Or5;16 1 Departamento de Astrof´ısicay Ciencias de la Atm´osfera, Facultad de Ciencias F´ısicas,Universidad Complutense de Madrid, E-280140 Madrid, Spain; e-mail: [email protected] 2 Departamento de Explotaci´ony Prospecci´onde Minas, Escuela de Minas, Energ´ıay Materiales, Universidad de Oviedo, E-33003 Oviedo, Asturias, Spain 3 Observatorio Astron´omicoCarda, Villaviciosa, Asturias, Spain (MPC Z76) 4 Centro de Astrobiolog´ıa(CSIC-INTA), Campus ESAC, Camino Bajo del Castillo s/n, E-28692 Villanueva de la Ca~nada,Madrid, Spain 5 Institut f¨ur Astrophysik, Georg-August-Universit¨at G¨ottingen, Friedrich-Hund-Platz 1, D-37077 G¨ottingen, Germany 6 AstroLAB IRIS, Provinciaal Domein \De Palingbeek", Verbrandemolenstraat 5, B-8902 Zillebeke, Ieper, Belgium 7 Observatorio Astron´omicoNaves, Cabrils, Barcelona, Spain (MPC 213) 8 Institut de Ci`enciesde l'Espai (CSIC-IEEC), Campus UAB, c/ de Can Magrans s/n, E-08193 Bellaterra, Barcelona, Spain 9 Institut d'Estudis Espacials de Catalunya (IEEC), E-08034 Barcelona, Spain 10 -
Winter Constellations
Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the Orion Nebula. -
100 Closest Stars Designation R.A
100 closest stars Designation R.A. Dec. Mag. Common Name 1 Gliese+Jahreis 551 14h30m –62°40’ 11.09 Proxima Centauri Gliese+Jahreis 559 14h40m –60°50’ 0.01, 1.34 Alpha Centauri A,B 2 Gliese+Jahreis 699 17h58m 4°42’ 9.53 Barnard’s Star 3 Gliese+Jahreis 406 10h56m 7°01’ 13.44 Wolf 359 4 Gliese+Jahreis 411 11h03m 35°58’ 7.47 Lalande 21185 5 Gliese+Jahreis 244 6h45m –16°49’ -1.43, 8.44 Sirius A,B 6 Gliese+Jahreis 65 1h39m –17°57’ 12.54, 12.99 BL Ceti, UV Ceti 7 Gliese+Jahreis 729 18h50m –23°50’ 10.43 Ross 154 8 Gliese+Jahreis 905 23h45m 44°11’ 12.29 Ross 248 9 Gliese+Jahreis 144 3h33m –9°28’ 3.73 Epsilon Eridani 10 Gliese+Jahreis 887 23h06m –35°51’ 7.34 Lacaille 9352 11 Gliese+Jahreis 447 11h48m 0°48’ 11.13 Ross 128 12 Gliese+Jahreis 866 22h39m –15°18’ 13.33, 13.27, 14.03 EZ Aquarii A,B,C 13 Gliese+Jahreis 280 7h39m 5°14’ 10.7 Procyon A,B 14 Gliese+Jahreis 820 21h07m 38°45’ 5.21, 6.03 61 Cygni A,B 15 Gliese+Jahreis 725 18h43m 59°38’ 8.90, 9.69 16 Gliese+Jahreis 15 0h18m 44°01’ 8.08, 11.06 GX Andromedae, GQ Andromedae 17 Gliese+Jahreis 845 22h03m –56°47’ 4.69 Epsilon Indi A,B,C 18 Gliese+Jahreis 1111 8h30m 26°47’ 14.78 DX Cancri 19 Gliese+Jahreis 71 1h44m –15°56’ 3.49 Tau Ceti 20 Gliese+Jahreis 1061 3h36m –44°31’ 13.09 21 Gliese+Jahreis 54.1 1h13m –17°00’ 12.02 YZ Ceti 22 Gliese+Jahreis 273 7h27m 5°14’ 9.86 Luyten’s Star 23 SO 0253+1652 2h53m 16°53’ 15.14 24 SCR 1845-6357 18h45m –63°58’ 17.40J 25 Gliese+Jahreis 191 5h12m –45°01’ 8.84 Kapteyn’s Star 26 Gliese+Jahreis 825 21h17m –38°52’ 6.67 AX Microscopii 27 Gliese+Jahreis 860 22h28m 57°42’ 9.79, -
Maps for GLOBE at Night at Latitude 40 , February 23, 21 H Local Time
< 0.50 mag < 1.50 mag < 2.50 mag < 3.50 mag < 4.50 mag < 5.50 mag < 6.50 mag < 7.50 mag Maps for GLOBE at Night at latitude 40◦, February 23, 21 h local time (deep night), assuming rather transparent air. Orion’s belt is 34◦ to the right from the south, at 43◦ height. The brightest fixed star, Sirius, is at left. Jan Hollan, Ecological Institute Veronica and http://www.astro.cz/darksky < 0.50 mag < 1.50 mag < 2.50 mag < 3.50 mag < 4.50 mag < 5.50 mag < 6.50 mag < 7.50 mag Maps for GLOBE at Night at latitude 40◦, March 2, 21 h local time (deep night), assuming rather transparent air. Orion’s belt is 42◦ to the right from the south, at 40◦ height. The brightest fixed star, Sirius, is at left. Jan Hollan, Ecological Institute Veronica and http://www.astro.cz/darksky Betelgeuse Rigel Pollux Procyon Sirius Sirius Arcturus Saturn < 0.50 mag < 1.50 mag S S Betelgeuse Big Dipper Big Big Dipper Big Betelgeuse Rigel Rigel Pollux Pollux Procyon Procyon Sirius Sirius Arcturus Regulus Arcturus Regulus Denebola Denebola Saturn Saturn < 2.50 mag < 3.50 mag S S Procyon Procyon Regulus Regulus Denebola Denebola < 4.50 mag < 5.50 mag Procyon Procyon Regulus Regulus Denebola Denebola < 6.50 mag < 7.50 mag Maps for GLOBE at Night at latitude 40◦, March 23, 21 h local time (Sun at -31◦). Lines from N(E,S,W) to zenith shown (crosses each 10◦). Regulus (α Leonis) is 32◦ to the left from S, at 58◦ height. -
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.