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AS/NZS ISO 6709:2011 ISO 6709:2008 ISO 6709:2008 Cor.1 (2009) AS/NZS ISO 6709:2011 AS/NZS ISO 6709:2011
AS/NZS ISO 6709:2011 ISO 6709:2008 ISO 6709:2008 Cor.1 (2009) AS/NZS ISO 6709:2011AS/NZS ISO Australian/New Zealand Standard™ Standard representation of geographic point location by coordinates AS/NZS ISO 6709:2011 This Joint Australian/New Zealand Standard was prepared by Joint Technical Committee IT-004, Geographical Information/Geomatics. It was approved on behalf of the Council of Standards Australia on 15 November 2011 and on behalf of the Council of Standards New Zealand on 14 November 2011. This Standard was published on 23 December 2011. The following are represented on Committee IT-004: ANZLIC—The Spatial Information Council Australasian Fire and Emergency Service Authorities Council Australian Antarctic Division Australian Hydrographic Office Australian Map Circle CSIRO Exploration and Mining Department of Lands, NSW Department of Primary Industries and Water, Tas. Geoscience Australia Land Information New Zealand Mercury Project Solutions Office of Spatial Data Management The University of Melbourne Keeping Standards up-to-date Standards are living documents which reflect progress in science, technology and systems. To maintain their currency, all Standards are periodically reviewed, and new editions are published. Between editions, amendments may be issued. Standards may also be withdrawn. It is important that readers assure themselves they are using a current Standard, which should include any amendments which may have been published since the Standard was purchased. Detailed information about joint Australian/New Zealand Standards can be found by visiting the Standards Web Shop at www.saiglobal.com.au or Standards New Zealand web site at www.standards.co.nz and looking up the relevant Standard in the on-line catalogue. -
International Standard
International Standard INTERNATIONAL ORGANIZATION FOR STANDARDIZATlON.ME~YHAPO~HAR OPI-AHH3AWlR fl0 CTAH~APTM3Al&lM.ORGANISATION INTERNATIONALE DE NORMALISATION Standard representation of latitude, longitude and altitude for geographic Point locations Reprksen ta tion normalis6e des latitude, longitude et altitude pbur Ia localisa tion des poin ts gkographiques First edition - 1983-05-15i Teh STANDARD PREVIEW (standards.iteh.ai) ISO 6709:1983 https://standards.iteh.ai/catalog/standards/sist/40603644-5feb-4b20-87de- d0a2bddb21d5/iso-6709-1983 UDC 681.3.04 : 528.28 Ref. No. ISO 67094983 (E) Descriptors : data processing, information interchange, geographic coordinates, representation of data. Price based on 3 pages Foreword ISO (the International Organization for Standardization) is a worldwide federation of national Standards bodies (ISO member bedies). The work of developing International Standards is carried out through ISO technical committees. Every member body interested in a subject for which a technical committee has been authorized has the right to be represented on that committee. International organizations, governmental and non-governmental, in liaison with ISO, also take part in the work. Draft International Standards adopted by the technical committees are circulated to the member bodies for approval before their acceptance as International Standards by the ISO Council. International Standard ISO 6709 was developediTeh Sby TTechnicalAN DCommitteeAR DISO/TC PR 97,E VIEW Information processing s ystems, and was circulated to the member bodies in November 1981. (standards.iteh.ai) lt has been approved by the member bodies of the following IcountriesSO 6709 :1: 983 https://standards.iteh.ai/catalog/standards/sist/40603644-5feb-4b20-87de- Belgium France d0a2bddRomaniab21d5/is o-6709-1983 Canada Germany, F. -
QUICK REFERENCE GUIDE Latitude, Longitude and Associated Metadata
QUICK REFERENCE GUIDE Latitude, Longitude and Associated Metadata The Property Profile Form (PPF) requests the property name, address, city, state and zip. From these address fields, ACRES interfaces with Google Maps and extracts the latitude and longitude (lat/long) for the property location. ACRES sets the remaining property geographic information to default values. The data (known collectively as “metadata”) are required by EPA Data Standards. Should an ACRES user need to be update the metadata, the Edit Fields link on the PPF provides the ability to change the information. Before the metadata were populated by ACRES, the data were entered manually. There may still be the need to do so, for example some properties do not have a specific street address (e.g. a rural property located on a state highway) or an ACRES user may have an exact lat/long that is to be used. This Quick Reference Guide covers how to find latitude and longitude, define the metadata, fill out the associated fields in a Property Work Package, and convert latitude and longitude to decimal degree format. This explains how the metadata were determined prior to September 2011 (when the Google Maps interface was added to ACRES). Definitions Below are definitions of the six data elements for latitude and longitude data that are collected in a Property Work Package. The definitions below are based on text from the EPA Data Standard. Latitude: Is the measure of the angular distance on a meridian north or south of the equator. Latitudinal lines run horizontal around the earth in parallel concentric lines from the equator to each of the poles. -
Equatorial and Cartesian Coordinates • Consider the Unit Sphere (“Unit”: I.E
Coordinate Transforms Equatorial and Cartesian Coordinates • Consider the unit sphere (“unit”: i.e. declination the distance from the center of the (δ) sphere to its surface is r = 1) • Then the equatorial coordinates Equator can be transformed into Cartesian coordinates: right ascension (α) – x = cos(α) cos(δ) – y = sin(α) cos(δ) z x – z = sin(δ) y • It can be much easier to use Cartesian coordinates for some manipulations of geometry in the sky Equatorial and Cartesian Coordinates • Consider the unit sphere (“unit”: i.e. the distance y x = Rcosα from the center of the y = Rsinα α R sphere to its surface is r = 1) x Right • Then the equatorial Ascension (α) coordinates can be transformed into Cartesian coordinates: declination (δ) – x = cos(α)cos(δ) z r = 1 – y = sin(α)cos(δ) δ R = rcosδ R – z = sin(δ) z = rsinδ Precession • Because the Earth is not a perfect sphere, it wobbles as it spins around its axis • This effect is known as precession • The equatorial coordinate system relies on the idea that the Earth rotates such that only Right Ascension, and not declination, is a time-dependent coordinate The effects of Precession • Currently, the star Polaris is the North Star (it lies roughly above the Earth’s North Pole at δ = 90oN) • But, over the course of about 26,000 years a variety of different points in the sky will truly be at δ = 90oN • The declination coordinate is time-dependent albeit on very long timescales • A precise astronomical coordinate system must account for this effect Equatorial coordinates and equinoxes • To account -
Earth-Centred Universe
Earth-centred Universe The fixed stars appear on the celestial sphere Earth rotates in one sidereal day The solar day is longer by about 4 minutes → scattered sunlight obscures the stars by day The constellations are historical → learn to recognise: Ursa Major, Ursa Minor, Cassiopeia, Pegasus, Auriga, Gemini, Orion, Taurus Sun’s Motion in the Sky The Sun moves West to East against the background of Stars Stars Stars stars Us Us Us Sun Sun Sun z z z Start 1 sidereal day later 1 solar day later Compared to the stars, the Sun takes on average 3 min 56.5 sec extra to go round once The Sun does not travel quite at a constant speed, making the actual length of a solar day vary throughout the year Pleiades Stars near the Sun Sun Above the atmosphere: stars seen near the Sun by the SOHO probe Shield Sun in Taurus Image: Hyades http://sohowww.nascom.nasa.g ov//data/realtime/javagif/gifs/20 070525_0042_c3.gif Constellations Figures courtesy: K & K From The Beauty of the Heavens by C. F. Blunt (1842) The Celestial Sphere The celestial sphere rotates anti-clockwise looking north → Its fixed points are the north celestial pole and the south celestial pole All the stars on the celestial equator are above the Earth’s equator How high in the sky is the pole star? It is as high as your latitude on the Earth Motion of the Sky (animated ) Courtesy: K & K Pole Star above the Horizon To north celestial pole Zenith The latitude of Northern horizon Aberdeen is the angle at 57º the centre of the Earth A Earth shown in the diagram as 57° 57º Equator Centre The pole star is the same angle above the northern horizon as your latitude. -
Appendix: Derivations
Paleomagnetism: Chapter 11 224 APPENDIX: DERIVATIONS This appendix provides details of derivations referred to throughout the text. The derivations are devel- oped here so that the main topics within the chapters are not interrupted by the sometimes lengthy math- ematical developments. DERIVATION OF MAGNETIC DIPOLE EQUATIONS In this section, a derivation is provided of the basic equations describing the magnetic field produced by a magnetic dipole. The geometry is shown in Figure A.1 and is identical to the geometry of Figure 1.3 for a geocentric axial dipole. The derivation is developed by using spherical coordinates: r, θ, and φ. An addi- tional polar angle, p, is the colatitude and is defined as π – θ. After each quantity is derived in spherical coordinates, the resulting equation is altered to provide the results in the convenient forms (e.g., horizontal component, Hh) that are usually encountered in paleomagnetism. H ^r H H h I = H p r = –Hr H v M Figure A.1 Geocentric axial dipole. The large arrow is the magnetic dipole moment, M ; θ is the polar angle from the positive pole of the magnetic dipole; p is the magnetic colatitude; λ is the geo- graphic latitude; r is the radial distance from the magnetic dipole; H is the magnetic field produced by the magnetic dipole; rˆ is the unit vector in the direction of r. The inset figure in the upper right corner is a magnified version of the stippled region. Inclination, I, is the vertical angle (dip) between the horizontal and H. The magnetic field vector H can be broken into (1) vertical compo- nent, Hv =–Hr, and (2) horizontal component, Hh = Hθ . -
AS/NZS ISO 6709:2008 Standard Representation of Latitude, Longitude
AS/NZS ISO 6709:2008 ISO 6709:1983 AS/NZS ISO 6709:2008 Australian/New Zealand Standard™ Standard representation of latitude, longitude and altitude for geographic point locations AS/NZS ISO 6709:2008 This Joint Australian/New Zealand Standard was prepared by Joint Technical Committee IT-004, Geographical Information/Geomatics. It was approved on behalf of the Council of Standards Australia on 25 July 2008 and on behalf of the Council of Standards New Zealand on 21 July 2008. This Standard was published on 16 September 2008. The following are represented on Committee IT-004: ACT Planning and Land Authority ANZLIC - the Spatial Information Council Australian Antarctic Division Australian Bureau of Statistics Australian Hydrographic Office Australian Key Centre In Land Information Studies Australian Map Circle Australian Spatial Information Business Association CSIRO Exploration & Mining Department for Administrative and Information Services (SA) Department of Defence (Australia) Department of Lands NSW Department of Natural Resources and Water (Qld) Department of Planning and Infrastructure (NT) Department of Primary Industries and Water Tasmania Department of Sustainability and Environment (Victoria) Geoscience Australia InterGovernmental Committee on Surveying and Mapping Land Information New Zealand Office of Spatial Data Management Western Australian Land Information System Keeping Standards up-to-date Standards are living documents which reflect progress in science, technology and systems. To maintain their currency, all Standards are periodically reviewed, and new editions are published. Between editions, amendments may be issued. Standards may also be withdrawn. It is important that readers assure themselves they are using a current Standard, which should include any amendments which may have been published since the Standard was purchased. -
Rotational Motion of Electric Machines
Rotational Motion of Electric Machines • An electric machine rotates about a fixed axis, called the shaft, so its rotation is restricted to one angular dimension. • Relative to a given end of the machine’s shaft, the direction of counterclockwise (CCW) rotation is often assumed to be positive. • Therefore, for rotation about a fixed shaft, all the concepts are scalars. 17 Angular Position, Velocity and Acceleration • Angular position – The angle at which an object is oriented, measured from some arbitrary reference point – Unit: rad or deg – Analogy of the linear concept • Angular acceleration =d/dt of distance along a line. – The rate of change in angular • Angular velocity =d/dt velocity with respect to time – The rate of change in angular – Unit: rad/s2 position with respect to time • and >0 if the rotation is CCW – Unit: rad/s or r/min (revolutions • >0 if the absolute angular per minute or rpm for short) velocity is increasing in the CCW – Analogy of the concept of direction or decreasing in the velocity on a straight line. CW direction 18 Moment of Inertia (or Inertia) • Inertia depends on the mass and shape of the object (unit: kgm2) • A complex shape can be broken up into 2 or more of simple shapes Definition Two useful formulas mL2 m J J() RRRR22 12 3 1212 m 22 JRR()12 2 19 Torque and Change in Speed • Torque is equal to the product of the force and the perpendicular distance between the axis of rotation and the point of application of the force. T=Fr (Nm) T=0 T T=Fr • Newton’s Law of Rotation: Describes the relationship between the total torque applied to an object and its resulting angular acceleration. -
The Sundial Cities
The Sundial Cities Joel Van Cranenbroeck, Belgium Keywords: Engineering survey;Implementation of plans;Positioning;Spatial planning;Urban renewal; SUMMARY When observing in our modern cities the sun shade gliding along the large surfaces of buildings and towers, an observer can notice that after all the local time could be deduced from the position of the sun. The highest building in the world - the Burj Dubai - is de facto the largest sundial ever designed. The principles of sundials can be understood most easily from an ancient model of the Sun's motion. Science has established that the Earth rotates on its axis, and revolves in an elliptic orbit about the Sun; however, meticulous astronomical observations and physics experiments were required to establish this. For navigational and sundial purposes, it is an excellent approximation to assume that the Sun revolves around a stationary Earth on the celestial sphere, which rotates every 23 hours and 56 minutes about its celestial axis, the line connecting the celestial poles. Since the celestial axis is aligned with the axis about which the Earth rotates, its angle with the local horizontal equals the local geographical latitude. Unlike the fixed stars, the Sun changes its position on the celestial sphere, being at positive declination in summer, at negative declination in winter, and having exactly zero declination (i.e., being on the celestial equator) at the equinoxes. The path of the Sun on the celestial sphere is known as the ecliptic, which passes through the twelve constellations of the zodiac in the course of a year. This model of the Sun's motion helps to understand the principles of sundials. -
3.- the Geographic Position of a Celestial Body
Chapter 3 Copyright © 1997-2004 Henning Umland All Rights Reserved Geographic Position and Time Geographic terms In celestial navigation, the earth is regarded as a sphere. Although this is an approximation, the geometry of the sphere is applied successfully, and the errors caused by the flattening of the earth are usually negligible (chapter 9). A circle on the surface of the earth whose plane passes through the center of the earth is called a great circle . Thus, a great circle has the greatest possible diameter of all circles on the surface of the earth. Any circle on the surface of the earth whose plane does not pass through the earth's center is called a small circle . The equator is the only great circle whose plane is perpendicular to the polar axis , the axis of rotation. Further, the equator is the only parallel of latitude being a great circle. Any other parallel of latitude is a small circle whose plane is parallel to the plane of the equator. A meridian is a great circle going through the geographic poles , the points where the polar axis intersects the earth's surface. The upper branch of a meridian is the half from pole to pole passing through a given point, e. g., the observer's position. The lower branch is the opposite half. The Greenwich meridian , the meridian passing through the center of the transit instrument at the Royal Greenwich Observatory , was adopted as the prime meridian at the International Meridian Conference in 1884. Its upper branch is the reference for measuring longitudes (0°...+180° east and 0°...–180° west), its lower branch (180°) is the basis for the International Dateline (Fig. -
Astro110-01 Lecture 7 the Copernican Revolution
Astro110-01 Lecture 7 The Copernican Revolution or the revolutionaries: Nicolas Copernicus (1473-1543) Tycho Brahe (1546-1601) Johannes Kepler (1571-1630) Galileo Galilei (1564-1642) Isaac Newton (1642-1727) who toppled Aristotle’s cosmos 2/2/09 Astro 110-01 Lecture 7 1 Recall: The Greek Geocentric Model of the heavenly spheres (around 400 BC) • Earth is a sphere that rests in the center • The Moon, Sun, and the planets each have their own spheres • The outermost sphere holds the stars • Most famous players: Aristotle and Plato 2/2/09 Aristotle Plato Astro 110-01 Lecture 7 2 But this made it difficult to explain the apparent retrograde motion of planets… Over a period of 10 weeks, Mars appears to stop, back up, then go forward again. Mars Retrograde Motion 2/2/09 Astro 110-01 Lecture 7 3 A way around the problem • Plato had decreed that in the heavens only circular motion was possible. • So, astronomers concocted the scheme of having the planets move in circles, called epicycles, that were themselves centered on other circles, called deferents • If an observation of a planet did not quite fit the existing system of deferents and epicycles, another epicycle could be added to improve the accuracy • This ancient system of astronomy was codified by the Alexandrian Greek astronomer Ptolemy (A.D. 100–170), in a book translated into Arabic and called Almagest. • Almagest remained the principal textbook of astronomy for 1400 years until Copernicus 2/2/09 Astro 110-01 Lecture 7 4 So how does the Ptolemaic model explain retrograde motion? Planets really do go backward in this model. -
1 the Equatorial Coordinate System
General Astronomy (29:61) Fall 2013 Lecture 3 Notes , August 30, 2013 1 The Equatorial Coordinate System We can define a coordinate system fixed with respect to the stars. Just like we can specify the latitude and longitude of a place on Earth, we can specify the coordinates of a star relative to a coordinate system fixed with respect to the stars. Look at Figure 1.5 of the textbook for a definition of this coordinate system. The Equatorial Coordinate System is similar in concept to longitude and latitude. • Right Ascension ! longitude. The symbol for Right Ascension is α. The units of Right Ascension are hours, minutes, and seconds, just like time • Declination ! latitude. The symbol for Declination is δ. Declination = 0◦ cor- responds to the Celestial Equator, δ = 90◦ corresponds to the North Celestial Pole. Let's look at the Equatorial Coordinates of some objects you should have seen last night. • Arcturus: RA= 14h16m, Dec= +19◦110 (see Appendix A) • Vega: RA= 18h37m, Dec= +38◦470 (see Appendix A) • Venus: RA= 13h02m, Dec= −6◦370 • Saturn: RA= 14h21m, Dec= −11◦410 −! Hand out SC1 charts. Find these objects on them. Now find the constellation of Orion, and read off the Right Ascension and Decli- nation of the middle star in the belt. Next week in lab, you will have the chance to use the computer program Stellar- ium to display the sky and find coordinates of objects (stars, planets). 1.1 Further Remarks on the Equatorial Coordinate System The Equatorial Coordinate System is fundamentally established by the rotation axis of the Earth.