May 2012 Observers Challenge – M-64
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Central Coast Astronomy Virtual Star Party May 15Th 7Pm Pacific
Central Coast Astronomy Virtual Star Party May 15th 7pm Pacific Welcome to our Virtual Star Gazing session! We’ll be focusing on objects you can see with binoculars or a small telescope, so after our session, you can simply walk outside, look up, and understand what you’re looking at. CCAS President Aurora Lipper and astronomer Kent Wallace will bring you a virtual “tour of the night sky” where you can discover, learn, and ask questions as we go along! All you need is an internet connection. You can use an iPad, laptop, computer or cell phone. When 7pm on Saturday night rolls around, click the link on our website to join our class. CentralCoastAstronomy.org/stargaze Before our session starts: Step 1: Download your free map of the night sky: SkyMaps.com They have it available for Northern and Southern hemispheres. Step 2: Print out this document and use it to take notes during our time on Saturday. This document highlights the objects we will focus on in our session together. Celestial Objects: Moon: The moon 4 days after new, which is excellent for star gazing! *Image credit: all astrophotography images are courtesy of NASA & ESO unless otherwise noted. All planetarium images are courtesy of Stellarium. Central Coast Astronomy CentralCoastAstronomy.org Page 1 Main Focus for the Session: 1. Canes Venatici (The Hunting Dogs) 2. Boötes (the Herdsman) 3. Coma Berenices (Hair of Berenice) 4. Virgo (the Virgin) Central Coast Astronomy CentralCoastAstronomy.org Page 2 Canes Venatici (the Hunting Dogs) Canes Venatici, The Hunting Dogs, a modern constellation created by Polish astronomer Johannes Hevelius in 1687. -
Messier Objects
Messier Objects From the Stocker Astroscience Center at Florida International University Miami Florida The Messier Project Main contributors: • Daniel Puentes • Steven Revesz • Bobby Martinez Charles Messier • Gabriel Salazar • Riya Gandhi • Dr. James Webb – Director, Stocker Astroscience center • All images reduced and combined using MIRA image processing software. (Mirametrics) What are Messier Objects? • Messier objects are a list of astronomical sources compiled by Charles Messier, an 18th and early 19th century astronomer. He created a list of distracting objects to avoid while comet hunting. This list now contains over 110 objects, many of which are the most famous astronomical bodies known. The list contains planetary nebula, star clusters, and other galaxies. - Bobby Martinez The Telescope The telescope used to take these images is an Astronomical Consultants and Equipment (ACE) 24- inch (0.61-meter) Ritchey-Chretien reflecting telescope. It has a focal ratio of F6.2 and is supported on a structure independent of the building that houses it. It is equipped with a Finger Lakes 1kx1k CCD camera cooled to -30o C at the Cassegrain focus. It is equipped with dual filter wheels, the first containing UBVRI scientific filters and the second RGBL color filters. Messier 1 Found 6,500 light years away in the constellation of Taurus, the Crab Nebula (known as M1) is a supernova remnant. The original supernova that formed the crab nebula was observed by Chinese, Japanese and Arab astronomers in 1054 AD as an incredibly bright “Guest star” which was visible for over twenty-two months. The supernova that produced the Crab Nebula is thought to have been an evolved star roughly ten times more massive than the Sun. -
RADIAL VELOCITIES in the ZODIACAL DUST CLOUD
A SURVEY OF RADIAL VELOCITIES in the ZODIACAL DUST CLOUD Brian Harold May Astrophysics Group Department of Physics Imperial College London Thesis submitted for the Degree of Doctor of Philosophy to Imperial College of Science, Technology and Medicine London · 2007 · 2 Abstract This thesis documents the building of a pressure-scanned Fabry-Perot Spectrometer, equipped with a photomultiplier and pulse-counting electronics, and its deployment at the Observatorio del Teide at Izaña in Tenerife, at an altitude of 7,700 feet (2567 m), for the purpose of recording high-resolution spectra of the Zodiacal Light. The aim was to achieve the first systematic mapping of the MgI absorption line in the Night Sky, as a function of position in heliocentric coordinates, covering especially the plane of the ecliptic, for a wide variety of elongations from the Sun. More than 250 scans of both morning and evening Zodiacal Light were obtained, in two observing periods – September-October 1971, and April 1972. The scans, as expected, showed profiles modified by components variously Doppler-shifted with respect to the unshifted shape seen in daylight. Unexpectedly, MgI emission was also discovered. These observations covered for the first time a span of elongations from 25º East, through 180º (the Gegenschein), to 27º West, and recorded average shifts of up to six tenths of an angstrom, corresponding to a maximum radial velocity relative to the Earth of about 40 km/s. The set of spectra obtained is in this thesis compared with predictions made from a number of different models of a dust cloud, assuming various distributions of dust density as a function of position and particle size, and differing assumptions about their speed and direction. -
The Mid-Infrared Extinction Law in the Ophiuchus, Perseus, and Serpens
The Mid-Infrared Extinction Law in the Ophiuchus, Perseus, and Serpens Molecular Clouds Nicholas L. Chapman1,2, Lee G. Mundy1, Shih-Ping Lai3, Neal J. Evans II4 ABSTRACT We compute the mid-infrared extinction law from 3.6−24µm in three molecu- lar clouds: Ophiuchus, Perseus, and Serpens, by combining data from the “Cores to Disks” Spitzer Legacy Science program with deep JHKs imaging. Using a new technique, we are able to calculate the line-of-sight extinction law towards each background star in our fields. With these line-of-sight measurements, we create, for the first time, maps of the χ2 deviation of the data from two extinc- tion law models. Because our χ2 maps have the same spatial resolution as our extinction maps, we can directly observe the changing extinction law as a func- tion of the total column density. In the Spitzer IRAC bands, 3.6 − 8 µm, we see evidence for grain growth. Below AKs =0.5, our extinction law is well-fit by the Weingartner & Draine (2001) RV = 3.1 diffuse interstellar medium dust model. As the extinction increases, our law gradually flattens, and for AKs ≥ 1, the data are more consistent with the Weingartner & Draine RV = 5.5 model that uses larger maximum dust grain sizes. At 24 µm, our extinction law is 2 − 4× higher than the values predicted by theoretical dust models, but is more consistent with the observational results of Flaherty et al. (2007). Lastly, from our χ2 maps we identify a region in Perseus where the IRAC extinction law is anomalously high considering its column density. -
GALAXIES WHAT ARE the DEEP SKY OBJECTS? •Deep-Sky Objects Are Astronomical Objects Other Than Individual Stars and Solar System Objects (Sun, Moon, Planets, Comets)
GALAXIES WHAT ARE THE DEEP SKY OBJECTS? •Deep-sky objects are astronomical objects other than individual stars and solar system objects (Sun, Moon, planets, comets). TYPES OF DEEP SKY OBJECTS •Nebulae •Clusters •Galaxies CHARLES MESSIER • Known for the Messier catalogue of galaxies, nebulae and star clusters M1 to M110 • He was a French astronomer who lived in the 18th century. • He was a comet hunter and the purpose of the catalogue was to record the sky objects that looked as comets but were not comets because they would not move in the sky. UNITS TO MEASURE DISTANCE • A Light-year is the distance that light travels in a year with a speed of approximately 300,000 kilometers per second • Closest star to the Sun is Proxima Centauri at 4.37 light years. • A Parsec is the equal to about 3.26 light years GALAXIES • A galaxy is an enormous collection of gas, dust and billions of stars held together by gravity. One galaxy can have hundreds of billions of stars and be as large as 200,000 light years across. • Galaxy is derived from the Greek galaxias meaning "milky", a reference to the Milky Way. • Many galaxies are believed to have black holes at their active center. The Milky Way's central black hole, known as Sagittarius A, has a mass four million times that of our Sun. GALAXIES FACTS • There are potentially more than 170 billion galaxies in the observable universe. Some, called dwarf galaxies, are very small with about 10 million stars, while others are huge containing an estimated 100 trillion stars. -
Alternate Constellation Guide
ARKANSAS NATURAL SKY ASSOCIATION LEARNING THE CONSTELLATIONS (Library Telescope Manual included) By Robert Togni Cover Image courtesy of Wikimedia. Do not write in this book, and return with scope to library. A personal copy of this guide can be obtained online at www.darkskyarkansas.com Preface This publication was inspired by and built upon Robert (Rocky) Togni’s quest to share the night sky with all who can be enticed under it. His belief is that the best place to start a relationship with the night sky is to learn the constellations and explore the principle ob- jects within them with the naked eye and a pair of common binoculars. Over a period of years, Rocky evolved a concept, using seasonal asterisms like the Summer Triangle and the Winter Hexagon, to create an easy to use set of simple charts to make learning one’s way around the night sky as simple and fun as possible. Recognizing that the most avid defenders of the natural night time environment are those who have grown to know and love nature at night and exploring the universe that it re- veals, the Arkansas Natural Sky Association (ANSA) asked Rocky if the Association could publish his guide. The hope being that making this available in printed form at vari- ous star parties and other relevant venues would help bring more people to the night sky as well as provide funds for the Association’s work. Once hooked, the owner will definitely want to seek deeper guides. But there is no better publication for opening the sky for the neophyte observer, making the guide the perfect companion for a library telescope. -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
The Fornax 3D Project: Dust Mix and Gas Properties in the Center of Early-Type Galaxy FCC 167
Astronomy & Astrophysics manuscript no. FCC167_accepted c ESO 2021 July 11, 2021 The Fornax 3D project: dust mix and gas properties in the center of early-type galaxy FCC 167 ? S. Viaene1; 2; , M. Sarzi3; 1, N. Zabel4, L. Coccato5, E. M. Corsini6; 7, T. A. Davis4, P. De Vis8, P. T. de Zeeuw9; 10, J. Falcón-Barroso11; 12, D.A. Gadotti5, E. Iodice13, M. Lyubenova5, R. McDermid14; 15, L. Morelli16; 6; 7, B. Nedelchev1, F. Pinna11; 12, T. W. Spriggs1, and G. van de Ven5 1 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK 2 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, B-9000 Gent, Belgium 3 Armagh Observatory and Planetarium, College Hill, Armagh, BT61 9DG, UK 4 School of Physics & Astronomy, Cardiff University, Queens Buildings, The Parade, Cardiff, CF24 3AA, UK 5 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching b. München, Germany 6 Dipartimento di Fisica e Astronomia ‘G. Galilei’, Università di Padova, vicolo dell’Osservatorio 3, I-35122 Padova, Italy 7 INAF–Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 8 Institut d’Astrophysique Spatiale, CNRS, Université Paris-Sud, Université Paris-Saclay, Bat. 121, F-91405 Orsay Cedex, France 9 Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands 10 Max-Planck-Institut fuer extraterrestrische Physik, Giessenbachstrasse, 85741 Garching bei Muenchen, Germany 11 Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, E-38200 La Laguna, Tenerife, -
Arxiv:1505.03150V2 [Astro-Ph.GA] 1 Jun 2015 Describe These Geometries
Astronomy & Astrophysics manuscript no. NGC4370arXiv c ESO 2018 October 15, 2018 NGC4370: a case study for testing our ability to infer dust distribution and mass in nearby galaxies S. Viaene1, G. De Geyter1, M. Baes1, J. Fritz1; 2, G.J. Bendo3, M. Boquien4, A. Boselli5, S. Bianchi6, L. Cortese7, P. Côté8, J.-C. Cuillandre9, I. De Looze1; 10, S. di Serego Alighieri6, L. Ferrarese8, S. D. J. Gwyn11, T. M. Hughes1, and C. Pappalardo12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, B-9000 Gent, Belgium e-mail: [email protected] 2 Centro de Radioastronomía y Astrofísica, CRyA, UNAM, Campus Morelia, A.P. 3-72, C.P. 58089, Michoacán, Mexico 3 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK 4 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 5 Laboratoire d’Astrophysique de Marseille, UMR 6110 CNRS, 38 rue F. Joliot-Curie, F-13388 Marseille, France 6 Osservatorio Astrofisico di Arcetri – INAF, Largo E. Fermi 5, 50125 Firenze, Italy 7 Centre for Astrophysics & Supercomputing, Swinburne University of Technology, Mail H30 – PO Box 218, Hawthorn, VIC 3122, Australia 8 National Research Council of Canada, Herzberg Astronomy and Astrophysics, 5071 W. Saanich Road, Victoria, BC V9E2E7, Canada 9 Canada-France-Hawaii Telescope, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743 USA 10 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge, CB3 0HA, UK 11 Canadian Astronomy Data Centre, 5071 West Saanich Rd, Victoria BC, V9E 2E7, Canada 12 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisbon, Portugal October 15, 2018 ABSTRACT Context. -
Spiral Arm Structures Revealed in the M31 Galaxy Yu.N.Efremov
1 Spiral arm structures revealed in the M31 galaxy Yu.N.Efremov Sternberg Astronomical Institute, MSU, Universitetsky pr. 13, Moscow, 11992 Russia Abstract Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. This pattern is observed within the arm region where Beck et al. (1989) detected a strong regular magnetic field with the wavelength twice as large as the spacing between the complexes. Moreover, complexes are located mostly at the extremes of the wavy magnetic field. In this arm, groups of HII regions lie inside star complexes, which, in turn, are located inside the gas–dust lane. In contrast, the southwestern arm of М31 splits into a gas–dust lane upstream and a dense stellar arm downstream, with HII regions located mostly along the boundary between these components of the arm. The density of high-luminosity stars in the southwestern arm is much higher than in the northwestern arm, and the former is not fragmented into star complexes. Furthermore, signatures of the age gradient across the southwestern arm have been found in earlier observations. This drastic difference in the structure of the segments of the same arm (Baade’s arm S4) is probably due mostly to their different pitch angles: the pitch angle is of about 0 º for northwestern part of the arm and about 30 ° in the southwestern segment. According to the classical SDW theory, this might result in lower SFR in the former and in the triggering of high SFR in the latter. -
Galaxy Classification and Evolution
name Galaxy Classification and Evolution Galaxy Morphologies In order to study galaxies and their evolution in the universe, it is necessary to categorize them by some method. A classification scheme generally must satisfy two criteria to be successful: It should act as a shorthand means of identification of the object, and it should provide some insight to understanding the object. We most generally used classification scheme of galaxies is one proposed by Edwin Hubble in 1926. His classification is based entirely on the visual appearance of a galaxy on a photographic plate. Hubble's system lists three basic categories: elliptical galaxies, spiral galaxies, and irregular galaxies. The spirals are divided into two groups, normal and barred. The elliptical galaxies, and both normal and barred spiral galaxies, are subdivided further, as illustrated in the figure, and discussed below. This figure is called the “Hubble Tuning Fork”. The Hubble tuning fork is a classification based on the visual appearance of the galaxies. Originally, when Hubble proposed this classification, he had hoped that it might yield deep insights, just as in the case for classifying stars a century ago. This classification scheme was thought to represent en evolutionary scheme, where galaxies start off as elliptical galaxies, then rotate, flatten and spread out as they age. Unfortunately galaxies turned out to be more complex than stars, and while this classification scheme is still used today, it does not provide us with deeper insights into the nature of galaxies. Image obtained from Wikipedia at http://en.wikipedia.org/wiki/Galaxy_morphological_classification Galaxy Classification & Evolution Laboratory Lab 12 1 Part I — Classification The photocopies of the galaxies are not good enough to be classified You will need to access the images on the computer and look at some of the fine detail. -
Ritgerðin 2. Desember-ÞDH
Stórbrotinn heimur hljóða Kvikmyndatónlist Amélie og Sherlock Holmes Karen Nadia Pálsdóttir Listaháskóli Íslands Tónlistardeild Söngur Stórbrotinn heimur hljóða Kvikmyndatónlist Amélie og Sherlock Holmes Karen Nadia Pálsdóttir Leiðbeinandi: Þorbjörg Daphne Hall Haustönn 2011 Í þessari ritgerð er fjallað um tónlist tveggja kvikmynda, Amélie eftir leikstjórann Jean-Pierre Jeunet og Sherlock Holmes í leikstjórn Guy Ritchie. Sérstaklega eru tónskáld umræddra mynda til umfjöllunar, sem og tónsköpun þeirra, og þau borin saman með áherslu á sameiginleg einkenni. Einnig er stuttlega fjallað um tónlist í kvikmyndum almennt, og stiklað á stóru um þróun kvikmyndatónlistar í Evrópu og Bandaríkjunum. Kvikmyndirnar Amélie og Sherlock Holmes eru ólíkar að mörgu leyti. Til að mynda er sú fyrrnefnda frönsk, framleidd með litlu fjármagni, á meðan sú síðarnefnda er stórmynd og framleidd í kvikmyndaborginni Hollywood. Ætla má að tónlistin í báðum myndum eigi stóran þátt í vinsældum þeirra, en tónskáld myndanna eru þeir Yann Tiersen, Amélie, og Hans Zimmer, Sherlock Holmes. Þeir eru mismunandi tónlistarmenn; Zimmer starfar sem kvikmyndatónskáld en Tiersen sem sjálfstæður tónlistarmaður, og gefur út plötur með eigin efni. Þrátt fyrir að hafa farið sitthvora leiðina sem tónlistarmenn hafa tónskáldin samskonar bakgrunn, úr rokktónlist. Áhrif frá þessum bakgrunni má túlka í tónlist þeirra, en hún á það sameiginlegt að vera oft á tíðum bæði drífandi og framsækin. Tónskáldin notuðu mismunandi aðferðir við tónsköpun fyrir myndirnar. Mikið af tónlist Amélie var af fyrri plötum Tiersens, og sú tónlist sem hann samdi fyrir myndina var ekki samin fyrir ákveðnar persónur né ákveðin atriði, á meðan Zimmer samdi alla tónlistina út frá myndinni sjálfri, með ákveðin atriði og persónur í huga.