Flight Skill: Pilot

Total Page:16

File Type:pdf, Size:1020Kb

Flight Skill: Pilot ADVENTURES IN SPACE Space Travel Space and Distance By way of introduction to this section, one does well to remember the sage advice of The Hitchhiker’s Guide to the Galaxy: “Space is big. Really big. You just won't believe how vastly, hugely, mind-bogglingly big it is. I mean, you may think it's a long way down the road to the chemist, but that's just peanuts to space.” Distance between objects in space is measured in two units—light-minutes (lm) which is used to describe the distance between relatively small objects, meaning anything the size of a planet or smaller; and light-years (ly) which describes the distance between stars, star-like objects like black holes, and massive objects such as nebulae. Time Span Increments Span: How Far Away Am I? Second/Round Minute Light-minutes and light-years determine the true distance Hour between objects, but what you really need to know is how long Day it takes to travel those distances. That time period is called Month Span. Year Decade For example, a setting may assume that travelling Century between planets can be done in a matter of days. In that case, Millennium we would say that its Span is Days. By default, light-years have spans four levels longer than light-minutes. So if a setting’s light-minute span is Days, then its light-year span is Centuries. This is based on a very rigid interpretation of interstellar distances—GMs are encouraged to bend this rule to better fit their narrative. Spans naturally vary from one setting to another. Longer spans grant a sense of vastness to the galaxy as it takes tremendous lengths of time to travel great distances, while shorter spans lead to more fast paced, action packed storytelling. The GM and Players should put serious thought into how they want their game to flow when figuring out their spans. Velocity: How Fast am I? When talking about how fast a Craft is moving, we use the term Velocity. Velocity is measured in light-minutes or light-years per span. If light-minutes are measured in Hours, then Velocity is lm per hour, and if light-years are measured in Months, then your Velocity is ly per month. Example: The rapid response vehicle Moonage Daydream is stationed in the Adhafera System in orbit around the third planet, Leonix. A bounty comes down the wire for Zelma Rubia, the notorious thief who has shocked the galaxy by stealing the magnificently sculpted F-Ring of the planet Mohapatra. The Moonage immediately sets a course for Adhafera’s fourth planet, Orissa, to get in contact with their black market informant. Orissa is 20 lm from Leonix, and in this universe, travel between planets is measured in hours. The Moonage Daydream has a total Thrust of 3d; if they were to travel to Orissa at their normal cruising speed, they would do so at a Velocity of 3 lm/hour, meaning it would take almost 7 hours to reach Orissa. Instead, their captain orders them to push their engines to reach Orissa faster, giving them a Velocity of 5 lm/hour. At that Velocity, they will reach Orissa in just 4 hours. Thrust: Conventional Spaceflight A Craft travels through space at a rate determined by its Thrust, which describes its conventional means of spaceflight. This may encompass simple rocket propulsion or more sophisticated systems like ion engines, Hawking drives or nuclear bombs detonated against a pressure plate. Cruising Speed Unless the Craft’s Thrust systems are damaged or destroyed, it can always travel at a Velocity equal to its Thrust. This represents Cruising Speed-- the pace at which the Craft can normally move without putting stress on its engines or flight crew. Cruising Speed doesn’t require any dice rolls or Flight Skills-- it’s the equivalent of casually walking down the street to borrow a cup of sugar from your neighbor. Full Speed: Going Faster If cruising speed isn’t cutting it, a Craft can open up the throttle and accelerate. This requires a dice roll using the Craft’s Thrust plus a relevant Flight Skill-- usually Pilot, Operation or Specialty [Thrust]. If the roll has a Set, add the Width to the Craft’s Thrust to generate its Velocity, called its Full Speed. A Craft can only travel at Full Speed for so long without straining its engines. This time limit is measured using the light-minute span of the distance you are travelling, and is equal to your Thrust. Therefore, a Craft with 3d in Thrust and measuring lm in days can travel at Full Speed for 3 days. When the Craft exceeds that time limit, it needs to slow down to Cruising Speed to allow its engines to recover. This recovery period is the same as the amount of time the Craft is able to travel at Full Speed (so 3 hours at Full Speed requires 3 hours at Cruising Speed to cool off). If that isn’t an option, like if the crew is pursuing their arch nemesis as he tries to escape through a wormhole, then they can keep their Full Speed at the cost of engine damage. If a Craft exceeds its Full Speed safety limit, then it will take damage each lm span that ticks by. Remember the Thrust + Flight Skill roll you did to accelerate to Full Speed? Well the Width from its Set becomes Shock Damage inflicted on every Hit Location housing a Thrust System. Example Zelma Rubia boasted on the Net that in 6 hours she will steal the ruby encrusted ninth moon of Bastilet, the gas giant on the very edge of the Adhafera System. At 25 lm away, the Moonage Daydream races to Bastilet at Full Speed to catch her before she can cement her already legendary reputation. The Moonage’s navigator rolls Pilot + Thrust and gets a set of 2x5, so he adds 2 to the Craft’s 3d in Thrust, setting their Full Speed Velocity at 5 lm/hour. At that rate, they’ll reach Bastilet in 5 hours, but after 3 hours of flight their engines are exhausted. Knowing that they’ll never reach Bastilet in time if they slow down, the captain orders them to keep their current Velocity. For the last two hours of the flight, the Moonage Daydream takes 2 Shock each hour to the Hit Locations housing her Thrust systems, arriving at Bastilet with 4 Shock to each and an hour to stop the heist. Max Speed: Pushing the Envelope The absolute fastest Velocity that a Craft can travel at is its Max Speed. Max Speed is a dangerous, unstable mode of travel that pushes a Craft’s engines well beyond their designed parameters. Max Speed requires the same roll of Thrust + Flight Skill, but the resulting Set needs a minimum Height of 5. A successful roll for Max Speed gives the Craft a Velocity of Width plus double its Thrust. This Velocity comes at a severe cost: every span that passes incurs Shock damage to all Thrust locations equal to the Width of the Max Speed roll. Unlike Full Speed, there’s no time span in which Max Speed is safe to use-- even a brief burst of Max Speed will hurt a Craft’s propulsion systems. How Big is a Star System? To give an idea of how Planetary Units relate to the distance between Planets, the following chart details our Solar System, showing how far various planets are from the Sun. This can be used as a helpful reference to give you some sense of big a Solar System can be, and how far apart planets inside the system can be. Body Miles (millions) Light-minutes (lm) Sun - - Mercury 36 3 Venus 67 6 Earth 93 8 Mars 141 12 Asteroid Belt 186 16 Jupiter 483 41 Saturn 886 76 Uranus 1,784 153 Neptune 2,794 240 Pluto 3,674 316 Oort Cloud 186,000 16,000 This chart demonstrates a few important facts about the distance between planets. First, the sweet spot for speculatively habitable worlds is generally between 6 and 12 lm. Closer to 6 gives you swelteringly hot worlds like Venus, and towards 12 you get cold, mostly airless planets like Mars. If the universe the characters are occupying adheres more closely to a realistic, hard science premise, then even these aren’t serious options, and life is limited to a narrow band of 7 to 9 lm, with 8 lm being ideal. Second, the further you get from the Sun, the more spread out planets become. The space between the Sun and Saturn is slightly less than the distance between Saturn and Uranus, the next planet out. Third, a solar system can be really, really big. If a voyager could cover 1 lm per hour, it would take almost two weeks to travel to Pluto from the Sun. Then there’s the Oort Cloud, the massive expanse of ice, dust and rocks that surrounds the solar system. At 1 lm per hour, it would take about 21 months reach the inner fringe of the Oort Cloud, and you wouldn’t reach the other side for almost 90 years. The conclusion to all of this is that mere Thrust won’t cut it for any setting where interstellar travel is a factor. For adventures on that scale, the light-year scale, players need some way to break the speed limit that light imposes. Interstellar Travel: Workarounds Before we get into the nitty-gritty of moving at speeds approaching or exceeding the speed of light, it’s worth mentioning that not all settings benefit from establishing hard rules on interstellar travel.
Recommended publications
  • A Revised View of the Canis Major Stellar Overdensity with Decam And
    MNRAS 501, 1690–1700 (2021) doi:10.1093/mnras/staa2655 Advance Access publication 2020 October 14 A revised view of the Canis Major stellar overdensity with DECam and Gaia: new evidence of a stellar warp of blue stars Downloaded from https://academic.oup.com/mnras/article/501/2/1690/5923573 by Consejo Superior de Investigaciones Cientificas (CSIC) user on 15 March 2021 Julio A. Carballo-Bello ,1‹ David Mart´ınez-Delgado,2 Jesus´ M. Corral-Santana ,3 Emilio J. Alfaro,2 Camila Navarrete,3,4 A. Katherina Vivas 5 and Marcio´ Catelan 4,6 1Instituto de Alta Investigacion,´ Universidad de Tarapaca,´ Casilla 7D, Arica, Chile 2Instituto de Astrof´ısica de Andaluc´ıa, CSIC, E-18080 Granada, Spain 3European Southern Observatory, Alonso de Cordova´ 3107, Casilla 19001, Santiago, Chile 4Millennium Institute of Astrophysics, Santiago, Chile 5Cerro Tololo Inter-American Observatory, NSF’s National Optical-Infrared Astronomy Research Laboratory, Casilla 603, La Serena, Chile 6Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Universidad Catolica´ de Chile, Av. Vicuna˜ Mackenna 4860, 782-0436 Macul, Santiago, Chile Accepted 2020 August 27. Received 2020 July 16; in original form 2020 February 24 ABSTRACT We present the Dark Energy Camera (DECam) imaging combined with Gaia Data Release 2 (DR2) data to study the Canis Major overdensity. The presence of the so-called Blue Plume stars in a low-pollution area of the colour–magnitude diagram allows us to derive the distance and proper motions of this stellar feature along the line of sight of its hypothetical core. The stellar overdensity extends on a large area of the sky at low Galactic latitudes, below the plane, and in the range 230◦ <<255◦.
    [Show full text]
  • Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects
    Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Porto Alegre 2017 Juliana Crestani Ribeiro de Souza Spatial Distribution of Galactic Globular Clusters: Distance Uncertainties and Dynamical Effects Dissertação elaborada sob orientação do Prof. Dr. Eduardo Luis Damiani Bica, co- orientação do Prof. Dr. Charles José Bon- ato e apresentada ao Instituto de Física da Universidade Federal do Rio Grande do Sul em preenchimento do requisito par- cial para obtenção do título de Mestre em Física. Porto Alegre 2017 Acknowledgements To my parents, who supported me and made this possible, in a time and place where being in a university was just a distant dream. To my dearest friends Elisabeth, Robert, Augusto, and Natália - who so many times helped me go from "I give up" to "I’ll try once more". To my cats Kira, Fen, and Demi - who lazily join me in bed at the end of the day, and make everything worthwhile. "But, first of all, it will be necessary to explain what is our idea of a cluster of stars, and by what means we have obtained it. For an instance, I shall take the phenomenon which presents itself in many clusters: It is that of a number of lucid spots, of equal lustre, scattered over a circular space, in such a manner as to appear gradually more compressed towards the middle; and which compression, in the clusters to which I allude, is generally carried so far, as, by imperceptible degrees, to end in a luminous center, of a resolvable blaze of light." William Herschel, 1789 Abstract We provide a sample of 170 Galactic Globular Clusters (GCs) and analyse its spatial distribution properties.
    [Show full text]
  • Annual Report 2005
    Max Planck Institute t für Astron itu o st m n ie -I k H c e n id la e l P b - e x r a g M M g for Astronomy a r x e b P l la e n id The Max Planck Society c e k H In y s m titu no Heidelberg-Königstuhl te for Astro The Max Planck Society for the Promotion of Sciences was founded in 1948. It operates at present 88 Institutes and other facilities dedicated to basic and applied research. With an annual budget of around 1.4 billion € in the year 2005, the Max Planck Society has about 12 400 employees, of which 4300 are scientists. In addition, annually about 11000 junior and visiting scientists are working at the Institutes of the Max Planck Society. The goal of the Max Planck Society is to promote centers of excellence at the fore- front of the international scientific research. To this end, the Institutes of the Society are equipped with adequate tools and put into the hands of outstanding scientists, who Annual Report have a high degree of autonomy in their scientific work. 2005 Max-Planck-Gesellschaft zur Förderung der Wissenschaften e.V. 2005 Public Relations Office Hofgartenstr. 8 80539 München Tel.: 089/2108-1275 or -1277 Annual Report Fax: 089/2108-1207 Internet: www.mpg.de Max Planck Institute for Astronomie K 4242 K 4243 Dossenheim B 3 D o s s E 35 e n h e N i eckar A5 m e r L a n d L 531 s t r M a a ß nn e he im B e e r r S t tr a a - K 9700 ß B e e n z - S t r a ß e Ziegelhausen Wieblingen Handschuhsheim K 9702 St eu b A656 e n s t B 37 r a E 35 ß e B e In de A5 r r N l kar ec i c M Ne k K 9702 n e a Ruprecht-Karls- ß lierb rh
    [Show full text]
  • Carbon Stars T. Lloyd Evans
    J. Astrophys. Astr. (2010) 31, 177–211 Carbon Stars T. Lloyd Evans SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK. e-mail: [email protected] Received 2010 July 19; accepted 2010 October 18 Abstract. In this paper, the present state of knowledge of the carbon stars is discussed. Particular attention is given to issues of classification, evolution, variability, populations in our own and other galaxies, and circumstellar material. Key words. Stars: carbon—stars: evolution—stars: circumstellar matter —galaxies: magellanic clouds. 1. Introduction Carbon stars have been reviewed on several previous occasions, most recently by Wallerstein & Knapp (1998). A conference devoted to this topic was held in 1996 (Wing 2000) and two meetings on AGB stars (Le Bertre et al. 1999; Kerschbaum et al. 2007) also contain much on carbon stars. This review emphasizes develop- ments since 1997, while paying particular attention to connections with earlier work and to some of the important sources of concepts. Recent and ongoing develop- ments include surveys for carbon stars in more of the galaxies of the local group and detailed spectroscopy and infrared photometry for many of them, as well as general surveys such as 2MASS, AKARI and the Sirius near infrared survey of the Magel- lanic Clouds and several dwarf galaxies, the Spitzer-SAGE mid-infrared survey of the Magellanic Clouds and the current Herschel infrared satellite project. Detailed studies of relatively bright galactic examples continue to be made by high-resolution spectroscopy, concentrating on abundance determinations using the red spectral region, and infrared and radio observations which give information on the history of mass loss.
    [Show full text]
  • Die Lokale Gruppe
    Die „lokale Gruppe“ Vortrag im Rahmen des Seminars „Entstehung und Entwicklung der Galaxis“ Vortrag imVortrag Rahmen im des Rahmen Seminars „Entstehung des Seminars und Entwicklung „Entstehung der Galaxis“ und Entwicklung der Galaxis“ Marius Halosar 31.5.2013 Übersicht • Definitionen • Struktur • Mitglieder der verschiedenen Untergruppen • Satellitenscheiben (DoS) • Umgebung und Dynamik der lokalen Gruppe • Morphologie und Eigenschaften von Zwerggalaxien • Populationsboxen • Vorstellung ausgewählter Mitglieder • Nachschlag Lokale Gruppe: Definitionen und Allgemeines • Der Begriff „Lokale Gruppe“ (LG) stammt aus dem Buch von Edwin HUBBLE „the realm of the Nebulae“ (E. Hubble, 1936), in dem er bereits die Mitgliedschaft von 12 Galaxien postulierte. • Eine Gruppe ist eine Ansammlung von 20 – 60 Galaxien mit einer Ausdehnung 7 13 von bis zu 10 Lj, enthält ca. 10 MO. Ihre Mitglieder sind gravitativ gebunden. • Galaxienhaufen bestehen aus bis zu 1000 Galaxien, die sich zu Superhaufen zusammenschließen. Ihre Abgrenzung zu den Gruppen ist nicht ganz eindeutig. • Die LG ist eine Galaxiengruppe, die Bestandteil des Virgo – Galaxienhaufens ist und der Andromeda (M 31) und die Milchstraße (MS) als dominante Komponenten angehören. Diese beiden enthalten 80% der Leuchtkraft der LG. • Die LG enthält 75 Galaxien und hat eine Ausdehnung von 1.8 – 2.4 Mpc. • Da die meisten Zwerggalaxien nur sehr geringe Oberflächenhelligkeiten aufweisen, wurden viele von ihnen erst kürzlich entdeckt. Es ist zu erwarten, dass durch verfeinerte Technik insbesondere in niedrigen galakt. Breiten in naher Zukunft noch weitere gefunden werden. 12 • Gesamtmasse beträgt ca. 2.10 MO • Geschwindigkeitsdispersion innerhalb der LG beträgt σ = 61 8 km/s • In einer Galaxie ist die Verteilungsfunktion des Phasenraums innerhalb des Alters des Universums inkompressibel.
    [Show full text]
  • Determination of Stellar Parameters Through the Use of All Available Flux Data and Model Spectral Energy Distributions
    University of Kentucky UKnowledge Theses and Dissertations--Physics and Astronomy Physics and Astronomy 2017 Determination of Stellar Parameters through the Use of All Available Flux Data and Model Spectral Energy Distributions Gemunu Ekanayake University of Kentucky, [email protected] Digital Object Identifier: https://doi.org/10.13023/ETD.2017.170 Right click to open a feedback form in a new tab to let us know how this document benefits ou.y Recommended Citation Ekanayake, Gemunu, "Determination of Stellar Parameters through the Use of All Available Flux Data and Model Spectral Energy Distributions" (2017). Theses and Dissertations--Physics and Astronomy. 44. https://uknowledge.uky.edu/physastron_etds/44 This Doctoral Dissertation is brought to you for free and open access by the Physics and Astronomy at UKnowledge. It has been accepted for inclusion in Theses and Dissertations--Physics and Astronomy by an authorized administrator of UKnowledge. For more information, please contact [email protected]. STUDENT AGREEMENT: I represent that my thesis or dissertation and abstract are my original work. Proper attribution has been given to all outside sources. I understand that I am solely responsible for obtaining any needed copyright permissions. I have obtained needed written permission statement(s) from the owner(s) of each third-party copyrighted matter to be included in my work, allowing electronic distribution (if such use is not permitted by the fair use doctrine) which will be submitted to UKnowledge as Additional File. I hereby grant to The University of Kentucky and its agents the irrevocable, non-exclusive, and royalty-free license to archive and make accessible my work in whole or in part in all forms of media, now or hereafter known.
    [Show full text]
  • Young Stars Raining Through the Galactic Halo: the Nature and Orbit of Price-Whelan 1 Michele Bellazzini, Rodrigo Ibata, Nicolas F
    Young stars raining through the galactic halo: the nature and orbit of price-whelan 1 Michele Bellazzini, Rodrigo Ibata, Nicolas F. Martin, Khyati Malhan, Antonino Marasco, Benoit Famaey To cite this version: Michele Bellazzini, Rodrigo Ibata, Nicolas F. Martin, Khyati Malhan, Antonino Marasco, et al.. Young stars raining through the galactic halo: the nature and orbit of price-whelan 1. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2019, 490 (2), pp.2588-2598. 10.1093/mnras/stz2788. hal-03095291 HAL Id: hal-03095291 https://hal.archives-ouvertes.fr/hal-03095291 Submitted on 4 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. MNRAS 490, 2588–2598 (2019) doi:10.1093/mnras/stz2788 Advance Access publication 2019 October 04 Young stars raining through the galactic halo: the nature and orbit of price-whelan 1 Michele Bellazzini ,1‹ Rodrigo A. Ibata,2 Nicolas Martin,2,3 Khyati Malhan,4 Antonino Marasco 5,6 and Benoit Famaey 2 1INAF - Osservatorio di Astrofisica e Scienza dello
    [Show full text]
  • Annual Report 2007 ESO
    ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2007 ESO European Organisation for Astronomical Research in the Southern Hemisphere Annual Report 2007 presented to the Council by the Director General Prof. Tim de Zeeuw ESO is the pre-eminent intergovernmental science and technology organisation in the field of ground-based astronomy. It is supported by 13 countries: Belgium, the Czech Republic, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Spain, Sweden, Switzerland and the United Kingdom. Further coun- tries have expressed interest in member- ship. Created in 1962, ESO provides state-of- the-art research facilities to European as- tronomers. In pursuit of this task, ESO’s activities cover a wide spectrum including the design and construction of world- class ground-based observational facili- ties for the member-state scientists, large telescope projects, design of inno- vative scientific instruments, developing new and advanced technologies, further- La Silla. ing European cooperation and carrying out European educational programmes. One of the most exciting features of the In 2007, about 1900 proposals were VLT is the possibility to use it as a giant made for the use of ESO telescopes and ESO operates the La Silla Paranal Ob- optical interferometer (VLT Interferometer more than 700 peer-reviewed papers servatory at several sites in the Atacama or VLTI). This is done by combining the based on data from ESO telescopes were Desert region of Chile. The first site is light from several of the telescopes, al- published. La Silla, a 2 400 m high mountain 600 km lowing astronomers to observe up to north of Santiago de Chile.
    [Show full text]
  • Searching for RR Lyrae Stars in the Canis Major Overdensity C
    Stellar Populations as Building Blocks of Galaxies Proceedings IAU Symposium No. 241, 2006 c 2007 International Astronomical Union A. Vazdekis & R. F. Peletier, eds. doi:10.1017/S1743921307008459 Searching for RR Lyrae stars in the Canis Major overdensity C. Mateu1,2,K.Vivas1,R.Zinn3 and L. Miller3 1Centro de Investigaciones de Astronom´ıa (CIDA), M´erida, Venezuela 2Facultad de Ciencias, Universidad Central de Venezuela, Caracas, Venezuela 3Astronomy Department, Yale University, New Haven, USA. Abstract. The Canis Major overdensity (CMa) was initially proposed to be the remnant of a tidally disrupting dSph galaxy. Since its nature is still subject of debate, the goal of the present work was to conduct a large-scale RR Lyrae survey in CMa, in order to see if there is an overdensity of these stars. The survey spans a total area of ∼ 34 sq. deg. with observations in V and R filters, made with the 1.0m J¨urgen Stock Schmidt telescope at the National Astronomical Observatory of Venezuela. Current results in a subregion, including spectroscopic observations, show that the small number of RR Lyrae stars found can be accounted for by the halo and thick disk components of our Galaxy. Keywords. Galaxy: structure, Galaxy: stellar content, stars: variables: RR Lyrae 1. Introduction The nature of the so-called Canis Major (CMa) overdensity has been the center of a lively debate ever since its discovery (Martin et al. 2004, Momany et al. 2004). It was originally proposed to be the remant core of a tidally disrupting dSph galaxy, and even though further observational evidence gathered in CMa has supported this view, it also has opened other possibilities for explaining its nature without invoking an origin external to our Galaxy.
    [Show full text]
  • Dwarf Cosmology with the Stromlo Missing Satellites Survey
    Hindawi Publishing Corporation Advances in Astronomy Volume 2010, Article ID 434390, 9 pages doi:10.1155/2010/434390 Review Article Dwarf Cosmology with the Stromlo Missing Satellites Survey Helmut Jerjen Research School of Astronomy & Astrophysics, Mt Stromlo Observatory Australian National University, Cotter Road, Weston ACT 2611, Australia Correspondence should be addressed to Helmut Jerjen, [email protected] Received 11 May 2009; Accepted 30 July 2009 Academic Editor: Regina Schulte-Ladbeck Copyright © 2010 Helmut Jerjen. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The standard Lambda Cold Dark Matter model is considered to be a triumph of theoretical astrophysics but observations of the Milky Way and its system of satellite galaxies irresistibly signal that theory is incomplete on galactic and subgalactic scales. The Stromlo Missing Satellites (SMS) Survey is a critical endeavor to investigate at what level predictions of CDM cosmology are consistent with the observed matter distribution in the Milky Way halo. It will be the deepest, most extended search for optically elusive satellite galaxies to date, covering 20 000 square degrees of sky. The international SMS Survey collaboration will exploit 150 TB of CCD images in six filters acquired by the new SkyMapper telescope of the Australian National University over the next five years, expecting on completion photometric limits 0.5–1.0 mag fainter than the Sloan Digital Sky Survey. The primary objective of the program is to characterise the baryonic and dark matter components of a complete sample of MW satellites in the Southern hemisphere to provide stringent observational constraints for improving our understanding of how the Milky Way formed and what physical processes governed galaxy formation and evolution in general.
    [Show full text]
  • Towards Advanced Astronomical Imaging: New Techniques of Data Reduction and Their Applications
    Jagiellonian University Doctoral Thesis Towards advanced astronomical imaging: new techniques of data reduction and their applications Author: Supervisor: Aleksander Kurek Dr hab. Agnieszka Pollo A thesis submitted in fulllment of the requirements for the degree of Doctor of Philosophy in the Faculty of Physics, Astronomy and Applied Computer Science 30 marca 2017 ii I’ve seen things you people wouldn’t believe. Attack ships on re o the shoulder of Orion. I watched C-beams glitter in the dark near the Tannhäuser Gate Roy Batty iii Abstract Goal The main goal of this thesis is to present new advanced methods of data acquisition and reduction developed in order to increase the photometric eciency and angular resolution of astronomical imaging. Methods I present an overview of the techniques I developed during my PhD studies. They include: (1) increasing the precision of bad pix- els removal, (2) impulse noise removal, (3) precise photometry and high angular resolution imaging of extremely faint sources, (4) ef- cient exposure times planning and (5) superresolved imaging of extended distant sources. Results It was shown that (1) is is possible to interpolate over bad pixels in the CCD ∼4× more eciently than it is done by standard meth- ods. A review of impulse noise removal techniques demonstrated (2) that the standard method (Laplacian Edge Detection) is in most cases the most ecient one, however, there are exceptions – mainly astrometric applications. Our evolutionary algorithm-based meth- ods were shown to be able to: (3) recover the surface prole of sources which are only ∼2-3 % stronger than their background; and (4) nd an optimal way to divide the available observing time to multiple exposures, so that the average photometric error of a dense eld photometry was lowered by 0.05 mag.
    [Show full text]
  • February 2019 BRAS Newsletter
    Monthly Meeting February 11th at 7PM at HRPO (Monthly meetings are on 2nd Mondays, Highland Road Park Observatory). Speaker: Chris Desselles on Astrophotography What's In This Issue? President’s Message Secretary's Summary Outreach Report Astrophotography Group Asteroid and Comet News Light Pollution Committee Report Recent BRAS Forum Entries Messages from the HRPO Science Academy International Astronomy Day Friday Night Lecture Series Globe at Night Adult Astronomy Courses Nano Days Observing Notes – Canis Major – The Great Dog & Mythology Like this newsletter? See PAST ISSUES online back to 2009 Visit us on Facebook – Baton Rouge Astronomical Society Newsletter of the Baton Rouge Astronomical Society February 2019 © 2019 President’s Message The highlight of January was the Total Lunar Eclipse 20/21 January 2019. There was a great turn out at HRPO, and it was a lot of fun. If any of the members wish to volunteer at HRPO, please speak to Chris Kersey, BRAS Liaison for BREC, to fill out the paperwork. MONTHLY SPEAKERS: One of the club’s needs is speakers for our monthly meetings if you are willing to give a talk or know of a great speaker let us know. UPCOMING BRAS MEETINGS: Light Pollution Committee - HRPO, Wednesday, February 6, 6:15 P.M. Business Meeting – HRPO, Wednesday, February 6, 7 P.M. Monthly Meeting – HRPO, Monday, February 11, 7 P.M. VOLUNTEERS: While BRAS members are not required to volunteer, if we do grow our volunteer core in 2019 we can do more fun activities without wearing out our great volunteers. Volunteering is an excellent opportunity to share what you know while increasing your skills.
    [Show full text]