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MAS Mentoring Project Overview 2020
Macarthur Astronomical Society Student Projects in Astronomy A Guide of Teachers and Mentors 2020 (c) Macarthur Astronomical Society, 2020 DRAFT The following Project Overviews are based on those suggested by Dr Rahmi Jackson of Broughton Anglican College. The Focus Questions and Issues section should be used by teachers and mentors to guide students in formulating their own questions about the topic. References to the NSW 7-10 Science Syllabus have been included. Note that only those sections relevant are included. For example, subsections a and d may be used, but subsections b and c are omitted as they do not relate to this topic. A generic risk assessment is provided, but schools should ensure that it aligns with school- based policies. MAS Student Projects in Astronomy page 1 Project overviews Semester 1, 2020: Project Stage Technical difficulty 4 5 6 1 The Moons of Jupiter X X X Moderate to high (extension) NOT available Semester 1 2 Astrophotography X X X Moderate to high 3 Light pollution X X Moderate 4 Variable stars X X Moderate to high 5 Spectroscopy X X High 6 A changing lunarscape X X Low to moderate Recommended project 7 Magnitude of stars X X Moderate to high Recommended for technically able students 8 A survey of southern skies X X Low to moderate 9 Double Stars X X Moderate to high 10 The Phases of the Moon X X Low to moderate Recommended project 11 Observing the Sun X X Moderate MAS Student Projects in Astronomy page 2 Project overviews Semester 2, 2020: Project Stage Technical difficulty 4 5 6 1 The Moons of Jupiter -
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. -
Final Report the Goddard High Resolution Spectrograph Scientific
NASA-CR-204980 Final Report The Goddard High Resolution Spectrograph Scientific Support Contract NAS5-32494 December 13, 1993 - December 12, 1996 Computer Sciences Corporation 4061 Powder Mill Road Calverton, MD 20705 GHRS SSC Final Report i Contents List of Acronyms iv I. Introduction II. Summary of Activities 4 1 Project Support - Subtask 1 4 1.1 Proposal Preparation and Tracking ..................... 4 1.2 SMOV and Post-COSTAR Calibration ................... 5 1.3 In-Orbit Performance Papers ........................ 7 1.4 Operations Studies .............................. 7 1.4.1 GHRS Efficiency ........................... 7 1.4.2 GHRS Low-Noise Orbits ....................... 8 1.5 Meetings and Information Distribution ................... 9 1.6 Public Information .............................. 9 1.7 The World Wide Web ............................ 10 1.8 The GHRS Science Symposium ....................... 11 2 Data Analysis Facility - Subtask 2 12 2.1 Facility Management ............................. 12 2.2 GHRS Archive ................................ 13 2.3 GHRS Team Software ............................ 15 2.4 General Software Support .......................... 15 2.5 Data Bases .................................. 16 2.6 Data Reduction and Analysis Assistance .................. 17 3 Extragalactic Imagery- Subtask 3 17 3.1 Analysis of R136 ............................... 17 3.2 Eta Carinae .................................. 19 3.3 Star Clusters in M33 ............................. 19 3.3.1 NGC 595 ............................... 20 3.3,2 -
A Spectroscopic and Dynamical Study of Binary and Other Cepheids
A spectroscopic and dynamical study of binary and other Cepheids |||||||||||||||||||| A thesis submitted in partial fulfillment of the requirements for the Degree of Doctor of Philosophy in Astronomy in the University of Canterbury by Orlon K. L. Petterson |||||||||{ University of Canterbury 2002 Abstract High resolution observations have been made of a number of southern Cepheids to make an observational and theoretical study of Cepheid variables using radial velocities. The stars studied were part of a long term programme to observe southern variable stars, from which a valuable database of radial velocities gathered over a long period were available. Sixteen ´echelle spectrograph orders in the wavelength region 5400{8600A˚ were used, which included a number of absorption lines covering a range of species and excitation potentials. The line bisector technique was used to measure stellar and telluric lines and to obtain radial velocities. To improve the precision of the radial velocities we used telluric lines to calibrate the observations to a common reference frame. 1 The radial velocities have a precision of 300ms− allowing the detection of velocity 1 ∼ differences of 1 km s− with confidence. The radial velocity data obtained at Mount ∼ John University Observatory (MJUO) was combined with data from various sources to determine the orbits of any Cepheids exhibiting orbital motion. The various orbital parameters were determined for a number of systems and where radial velocities for the companions exist, some estimate of the mass was made. The precision of the radial velocities obtained from MJUO also allowed us to search for line level effects for a number of species among the Cepheid spectra. -
Doktori Disszertacio
Szabados L´aszl´o Uj´ aspektusok a klasszikus cefeid´ak id˝obeli v´altoz´asainak vizsg´alat´aban Ertekez´es´ az MTA doktora c´ım megszerz´es´e´ert Budapest, 1997 Sz¨uleim eml´ek´enek Tartalomjegyz´ek 1. Bevezet´es ....................................... ......................... 1 2. A cefeid´ak – helyzetk´ep J.D. 2 450 000 epoch´ara . ................... 4 2.1 A helyzetk´ep el´e................................ ................... 4 2.2 Megfigyel´esi adatok .............................. .................. 4 2.3 A cefeid´akkal kapcsolatos kutat´asok kiemelked˝oeredm´enyei . 6 2.4 A k¨ozelj¨ov˝ore vonatkoz´okil´at´asok . ..................... 13 3. A stacion´arius pulz´aci´ob´ol meghat´arozhat´omennyis´egek ´es tulajdons´agok 14 3.1 A stacion´arius pulz´aci´o´es a cefeid´ak ´allapotjelz˝oi................... 14 3.2 A f´azisg¨orb´ek Fourier-felbont´asa ´es az s-cefeid´ak.................... 18 4. Eredm´enyek a pulz´aci´os amplit´ud´ovizsg´alata alapj´an .................... 21 4.1 Az amplit´ud´ok peri´odusf¨ugg´ese . .................... 21 4.2 Az amplit´ud´ok ar´any´anak vizsg´alata . ................... 27 4.3 A k´etm´odus´ucefeid´ak amplit´ud´oir´ol . ..................... 33 5. A cefeid´ak kett˝oss´eg´evel kapcsolatos ´uj eredm´enyek ...................... 41 5.1 A kett˝oscsillagok el˝ofordul´asi gyakoris´aga a cefeid´ak k¨oz¨ott......... 41 5.2 Ujabb´ spektroszk´opiai kett˝os¨ok kimutat´asa . ............... 43 5.3 K´ıs´er˝ocsillag kimutat´asa IUE-sz´ınk´epek alapj´an ................... 47 5.4 A k´ıs´er˝ocsillag hat´asa a cefeida pulz´aci´os peri´odus´ara ............ -
The Journal of the Royal Astronomical Society Of
SSouthernouthern SStarstars TTHEHE JJOURNALOURNAL OOFF TTHEHE RROYALOYAL AASTRONOMICALSTRONOMICAL SSOCIETYOCIETY OOFF NNEWEW ZZEALANDEALAND Volume 56, No 2 2017 June ISSN Page0049-1640 1 Royal Astronomical Society Southern Stars of New Zealand (Inc.) Journal of the RASNZ Founded in 1920 as the New Zealand Astronomical Volume 56, Number 2 Society and assumed its present title on receiving the 2017 June Royal Charter in 1946. In 1967 it became a member body of the R oyal Society of New Zealand. P O Box 3181, Wellington 6140, New Zealand [email protected] http://www.rasnz.org.nz CONTENTS Subscriptions (NZ$) for 2017: SWAPA 2017 Ordinary member: $40.00 John Drummond ...................................................... 3 Student member: $20.00 Affi liated society: $3.75 per member. The Louwman Collection of Historic Telescopes Minimum $75.00, Maximum $375.00 William Tobin ........................................................... 6 Corporate member: $200.00 Printed copies of Southern Stars (NZ$): Steve Butler FRASNZ ................................................10 $35.00 (NZ) $45.00 (Australia & South Pacifi c) The Norfolk Island Effect and the Whanagaroa $50.00 (Rest of World) Report Grahame Fraser ..................................................... 11 Auckland Observatory Research in the First 25 Years Council & Offi cers 2016 to 2018 - A Personal View II President: Stan Walker ........................................................... 18 John Drummond P O Box 113, Patutahi 4045. [email protected] Immediate Past President: John Hearnshaw Dep’t Physics & Astronomy, University of Canterbury, Private Bag 4800, Christchurch 8140. [email protected] Vice President: FRONT COVER Nicholas Rattenbury The Department of Physics, Peter Louwman in the midst of his collection of historic The University of Auckland, telescopes at The Hague, Netherlands. 38 Princes St, Auckland. -
VSS Newsletter – May 2010
Newsletter 2010/2 2010 May From the Director NACAA and the FUTURE Thomas Richards [email protected] Variable star enthusiasts were well represented amongst the hundred-plus attendees at the NACAA conference at Canberra this Easter. Well organised and with high quality pa- pers and posters, it was altogether an exhilarating few days. The theme was "Amateur Astronomy in the Online Age". David Benn started things rolling with a workshop "Variable Star Data Visualisation and Analysis with Vstar". His Vstar software is being developed under contract to AAVSO for online use in the CitizenSky programme - and is already available there. The confer- ence paper sessions kicked off on Saturday morning with the first John Perdrix Address (John founded NACAA) by myself. More of this below. Variable star papers in the con- ference were: Tom Richards: Opportunities and Plans: the Directions of Southern Hemisphere Variable Star Research Alan Plummer: Variable Stars: Observing Stellar Evolution David O'Driscoll: Robotic Research for the Amateur Astronomer Simon O'Toole: The Ubiquity of Exoplanets Tom Richards: Round-table - Variable Stars Planning Session INDEX From the Director Tom Richards 1 Editor’s Comments Stan Walker 3 Stars of the Month Stan Walker 4 Stars That Go Out Stephen Hovell/Stan Walker 5 The Dual Maxima Mira Project Stan Walker 7 The ESP Bug Phil Evans 8 Remarks on Two Possible Cataclysmic Variables Mati Morel 14 CCD Notes—What is the Time on the Sun Tom Richards 16 Here and There 18 Eclipsing Binaries for Fun and Profit—Part IV Bob Nelson 19 The Bright Cepheid Project Stan Walker 31 V1243 Aquilae—A Remarkable Alignment Tom Richards 32 Contact Information 37 It's good to report that David O'Driscoll won the Astral Award for the best presentation. -
The COLOUR of CREATION Observing and Astrophotography Targets “At a Glance” Guide
The COLOUR of CREATION observing and astrophotography targets “at a glance” guide. (Naked eye, binoculars, small and “monster” scopes) Dear fellow amateur astronomer. Please note - this is a work in progress – compiled from several sources - and undoubtedly WILL contain inaccuracies. It would therefor be HIGHLY appreciated if readers would be so kind as to forward ANY corrections and/ or additions (as the document is still obviously incomplete) to: [email protected]. The document will be updated/ revised/ expanded* on a regular basis, replacing the existing document on the ASSA Pretoria website, as well as on the website: coloursofcreation.co.za . This is by no means intended to be a complete nor an exhaustive listing, but rather an “at a glance guide” (2nd column), that will hopefully assist in choosing or eliminating certain objects in a specific constellation for further research, to determine suitability for observation or astrophotography. There is NO copy right - download at will. Warm regards. JohanM. *Edition 1: June 2016 (“Pre-Karoo Star Party version”). “To me, one of the wonders and lures of astronomy is observing a galaxy… realizing you are detecting ancient photons, emitted by billions of stars, reduced to a magnitude below naked eye detection…lying at a distance beyond comprehension...” ASSA 100. (Auke Slotegraaf). Messier objects. Apparent size: degrees, arc minutes, arc seconds. Interesting info. AKA’s. Emphasis, correction. Coordinates, location. Stars, star groups, etc. Variable stars. Double stars. (Only a small number included. “Colourful Ds. descriptions” taken from the book by Sissy Haas). Carbon star. C Asterisma. (Including many “Streicher” objects, taken from Asterism. -
From the Director
Newsletter 2010/1 2010 February From the Director Tom Richards [email protected] TOOs and RFOs Have you noticed the latest one-upmanship game? Use acronyms but don't decode them. Then your reader feels most inferior for not knowing instantly what those capital letters mean. Why, I've probably committed this sin in my articles in this Newsletter. And I could go on about the wonderful opportunity acronyms offer for wandering apostrophes too (or TOO). Anyway, on to TOOs (not TOO's). Or should I be a real pedant and talk of TsOO like GsG for Governors General? A most significant part of the contribution an amateur VSO (heh heh – it's you, an ob- server of variable stars) can make, as we all know, is to contribute observations of some- thing important that has just happened – a Target of Opportunity. The commonest class of such events are the outbursts of one sort or another of cataclysmic variables, from a nova eruption to a dwarf nova superoutburst. There have been a spate of such down- south events lately among them the recurrent nova U Sco, the peculiar dwarf nova VX For, and novae in Eridanus, Ophiuchus and Sagittarius. Other types of events get people excited too: the outburst of the luminous blue variable R71 in the LMC (surely you know INDEX From the Director Tom Richards 1 And a Bit from the Editor Stan Walker 3 Stars of the Quarter Stan Walker 5 TT Arietis: An Exciting CV For Amateurs Too Stephen Hovell 7 A Personal Project Eric Rumbo 14 Bright Star Monitor South Tom Richards 16 The Crows Nest Observatory Roland Idaczyk 17 Equatorial Eclipsing Binaries—Pisces Cetus Tom Richards 19 CCD Column—What Exposure to use Tom Richards 23 Green Island Observatory Yenal Ogmen 24 Visual Variable Star Observations Glen Schrader 25 How Good Can Visual Measures Be? Stan Walker 29 The Nova that Everyone’s Watching - U Scorpii Erupts Tom Richards 30 Contact Information 32 that acronym?), and the brightening of Eta Carinae, are just two that come to mind. -
Dr. Azriel Goldschmidt Lawrence Berkeley Lab
Vol. 55, No. 5 – May 2007 May 16, 2007 – General Meeting 7:00 pm Doors Open . 7:30 pm Announcements . 8:00 pm Speaker DR. AZRIEL GOLDSCHMIDT LAWRENCE BERKELEY LAB LOOKING AT THE UNIVERSE WITH DIFFERENT EYES: THE ICE CUBE HIGH-ENERGY NEUTRINO TELESCOPE Why make dozens of mile and a half deep holes in the Antarctic ice at the South Pole? Why bury in them thousands of glass spheres with light sensors? What do we hope to learn by looking for neutrinos coming from the cosmos? How can we learn about the inner workings of gamma ray bursters, supernovae or active galactic nuclei by looking for neutrinos coming from them? In this talk I will offer answers to these questions and describe how the IceCube telescope detects high‐ energy neutrinos, measures their energy and determines from where they came, thus opening a new window through which to look at our universe. Dr. Azriel Goldschmidt is a staff physicist at the Lawrence Berkeley National Laboratoryʹs Nuclear Science division. Since 1996 he has been doing research in neutrino astrophysics, currently with the IceCube neutrino telescope at the South Pole. Originally from Argentina, Dr. Goldschmidt received his B.Sc. in physics from the Technion Israel Institute of Technology and his Ph.D. in particle physics from the University of California at Berkeley. In recent years his work has focused on the development, implementation and operation of a data acquisition system for the IceCube high energy neutrino telescope. 2007 Club Officers & Contacts Club Telescopes The SFAA owns eight very fine, easy to use, President Kenneth Frank [email protected] loaner telescopes well-suited for deep sky, Vice President Jorge Morales vicepresident@sfaa- planets, and star parties. -
Introduction to the Bright Cepheids Charts
INTRODUCTION TO THE CHARTS These charts have been produced using Project Pluto’s Guide 8 compiled by Bill Gray. Most are vertical but some, where the comprison stars lie more east-west, are horizontal. The scale is variable for the same reasons. Historically, variable star charts have depended upon the availability of sequences and attempts to improve these from the visual values of the Cordoba Durchmusterung and similar visual catalogues have not always been successful. From about 1960 onward good photoelectric measures became available, but these were limited in the number of stars measured except for specific fields. Colour photometry does not need more than 3-4 com- parison and check stars. More recently, satellite surveys have measured a very large number of stars but using filters which don’t correspond to either the response of the eye or the V of the UBV system. Many of these measures have, however, been transformed to a more or less standard sys- tem and are homogeneous at the bright levels which is what we’re interested in. So val- ues for all stars in the range of a particular star’s variability are noted on each chart. Only known variable stars are not so marked. There is a margin at top and bottom of the se- quence to allow for the eye’s different response—and for the thought that some of the quoted ranges of these Cepheids might be slightly incorrect. No attempt has been made to select stars of a standard colour as this is not possible given the stars available. -
Thirty-Six New Variable Stars
3 79 4152 380 Nahe Konjunktionen J upiters rnit AG.-Sternen. Durch die kiirzlich von Dr. Graff in A. N. 4143 mit- ahnliche Phanomene, die ja fur die Positionsbestimmung der geteilte Beobachtung einer wahrscheinlich stattgehabten Be- Trabanten auch an den einschliefienden Tagen von grooer deckung eines Fixsterns durch einen Jupitermond wurde ich Bedeutung sind, zu erwarten seien. Besonders bemerkens- veranlafit, zu untersuchen, ob vielleicht in der nachsten Zeit wert erscheinen mir die nachstehenden drei Konjunktionen. Konj. in RA. in M. 2. Gr. IR AG. Berl. B Gr. a aPP. 8 aPP. %-%+ 1907 Febr. 9d 6h23m 2236 8.7 6h 6mr4?52 -1-23'27' 22!'6 +36!6 April 3 8 59 2301 7.3 6 13 39.19 +23 30 20.5 -37.5 P 14 22 I 2366 7.8 6 I9 52.45 +23 29 34.4 + 2.8 Bei den beiden ersten Sternen ist die kleinste Distanz etwa oh9 vor dem Untergange Jupiters. Perth kann nur den des Sterns vom Jupiterrande I 5!'9 resp. 2010, wahrend bei Austritt, Wellington auf Neu-Seeland nur den Eintritt beob- dem dritten eine fast zentrale Bedeckung stattfindet, die achten. Vielleicht gelingt es, trotz der verhaltnismafiig grofien jedoch nur in Australien beobachtet werden kann. Fur die Lichtschwache des Sterns den Eintritt, dessen Beobachtung Sternwarten von New South Wales (Lange ca. loh 6stl. von durch die schwache Phase Jupiters etwas erleichtert wird, Gr., siidl. Breite 30") geht die Sonne um 5h7 unter; der zu fixieren. Eintritt erfolgt um etwa 7h1, der Austritt um 8h9 Ortszeit, Berlin, I 907 Jan. I 6.