DOCSLIB.ORG

Analysis of Star Identification Algorithms Due to Uncompensated

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Analysis of Star Identification Algorithms Due to Uncompensated Utah State University DigitalCommons@USU All Graduate Theses and Dissertations Graduate Studies 5-2013 Analysis of Star Identification Algorithms due ot Uncompensated Spatial Distortion Steven Paul Brätt Utah State University Follow this and additional works at: https://digitalcommons.usu.edu/etd Part of the Mechanical Engineering Commons Recommended Citation Brätt, Steven Paul, "Analysis of Star Identification Algorithms due ot Uncompensated Spatial Distortion" (2013). All Graduate Theses and Dissertations. 1714. https://digitalcommons.usu.edu/etd/1714 This Thesis is brought to you for free and open access by the Graduate Studies at DigitalCommons@USU. It has been accepted for inclusion in All Graduate Theses and Dissertations by an authorized administrator of DigitalCommons@USU. For more information, please contact [email protected]. ANALYSIS OF STAR IDENTIFICATION ALGORITHMS DUE TO UNCOMPENSATED SPATIAL DISTORTION by Steven P. Brätt A thesis submitted in partial fulfillment of the requirements for the degree of MASTER OF SCIENCE in Mechanical Engineering Approved: Dr. R. Rees Fullmer Dr. Charles M. Swenson Major Professor Committee Member Dr. David Geller Dr. Mark R. McLellan Committee Member Vice President for Research and Dean of the School of Graduate Studies UTAH STATE UNIVERSITY Logan, Utah 2013 ii Copyright © Steven Paul Brätt 2013 All Rights Reserved iii ABSTRACT Analysis of Star Identification Algorithms due to Uncompensated Spatial Distortion by Steven Paul Brätt, Master of Science Utah State University, 2013 Major Professor: Dr. Rees Fullmer Department: Mechanical and Aerospace Engineering With the evolution of spacecraft systems, we see the growing need for smaller, more affordable, and robust spacecrafts that can be jettisoned with ease and sent to sites to perform a myriad of operations that a larger craft would prohibit, or that can be quickly manipulated from performing one task into another. The developing requirements have led to the creation of CubeSats. The question then remains, how to navigate the expanse of space with such a minute spacecraft? A solution to this is using the stars themselves as a means of navigation. This can be accomplished by measuring the angular separation between illuminated pixels in a camera image and associating the pixels with a corresponding star. Once identified, the spacecraft can obtain a quaternion solution to pinpoint its position and facing. A series of star identification algorithms called Lost in Space Algorithms (LISAs) are used to identify these pixels as stars in an image and assess the accuracy and probability of error associated with each algorithm. This is done by creating various images from a simulated camera program, using MATLAB as the program interface, along with images of actual stars in the night sky containing uncompensated error data taken with an Aptina camera. It is shown how suitable these algorithms are for use in space navigation, what constraints and impediments each have, and if low quality imagers can be used to determine attitude using these LISA’s. (221 pages) iv PUBLIC ABSTRACT Analysis of Star Identification Algorithms due to Uncompensated Spatial Distortion by Steven Paul Brätt, Master of Science Utah State University, 2013 Major Professor: Dr. Rees Fullmer Department: Mechanical and Aerospace Engineering With the evolution of spacecraft systems, we see the growing need for smaller, more affordable, and robust spacecrafts that can be jettisoned with ease and sent to sites to perform a myriad of operations that a larger craft would prohibit, or that can be quickly manipulated from performing one task into another. The developing requirements have led to the creation of Nano-Satellites, or CubeSats. The question then remains, how to navigate the expanse of space with such a minute spacecraft? A solution to this is using the stars themselves as a means of navigation. This can be accomplished by measuring the distance between stars in a camera image and determining the stars’ identities. Once identified, the spacecraft can obtain its position and facing. A series of star identification algorithms called Lost in Space Algorithms (LISAs) are used to recognize the stars in an image and assess the accuracy and error associated with each algorithm. This is done by creating various images from a simulated camera, using a program called MATLAB, along with images of actual stars with uncompensated errors. It is shown how suitable these algorithms are for use in space navigation, what constraints and impediments each have, and if low quality cameras using these algorithms can solve the Lost in Space problem. (221 pages) v ACKNOWLEDGMENTS There have been many people who have made a great impact on my life and have helped me achieve my goals and pushed me to excel. To my wonderful professor, Dr. Rees Fullmer, I’d like to thank you for your constant support and input as I’ve worked to complete this thesis and finish my master’s program. You have helped me improve dramatically in my abilities as a researcher and engineer. I’d like to thank your wife who was kind enough to let you spend so much of your time helping me. To David Fowler, a good friend and great co-worker; thank you for your help and friendship as we worked together on both our research theses. You’ve helped me understand much more than you know. I would like to say a special word of gratitude to my marvelous parents, Glenn and Odile, and my family who were always there to encourage me to pursue my dreams and ambitions. Thank you for your love, your prayers, and for the person you have helped me to become. Steven Paul Brätt vi CONTENTS Page ABSTRACT .................................................................................................................................................. iii PUBLIC ABSTRACT ....................................................................................................................................iv ACKNOWLEDGMENTS ............................................................................................................................... v LIST OF TABLES .......................................................................................................................................... x LIST OF FIGURES ........................................................................................................................................xi NOMENCLATURE ................................................................................................................................... xvii CHAPTER 1. INTRODUCTION ..................................................................................................................... 1 I. Overview ............................................................................................................................ 1 II. Star Cameras ....................................................................................................................... 1 III. Star Fields and Identification .............................................................................................. 2 IV. Commercial Cameras .......................................................................................................... 3 V. Thesis Statement and Objectives ........................................................................................ 4 A. Thesis Statement ...................................................................................................4 B. Objectives .............................................................................................................4 2. STAR CATALOGS AND IDENTIFICATION METHODS EXAMINED .............................. 6 I. Star Catalogs ....................................................................................................................... 6 A. Star Databases ......................................................................................................7 1. Henry Draper Database ..........................................................................7 2. PPM Database ........................................................................................7 3. Hipparcos-Tycho Databases ..................................................................7 B. Main Identification Catalog ..................................................................................8 II. Star Identification Algorithms Reviewed ........................................................................... 9 A. Gotlieb ..................................................................................................................9 B. Groth ................................................................................................................... 10 C. Kosik .................................................................................................................. 10 D. Anderson ............................................................................................................ 11 E. Renken ................................................................................................................ 11 F. Liebe ................................................................................................................... 12 G. Baldini ................................................................................................................ 13 H. Scholl .................................................................................................................. 14 I. Ketchum ............................................................................................................
Load more

Recommended publications
  • Appendix A: Scientific Notation
    Appendix A: Scientific Notation Since in astronomy we often have to deal with large numbers, writing a lot of zeros is not only cumbersome, but also inefficient and difficult to count. Scientists use the system of scientific notation, where the number of zeros is short handed to a superscript. For example, 10 has one zero and is written as 101 in scientific notation. Similarly, 100 is 102, 100 is 103. So we have: 103 equals a thousand, 106 equals a million, 109 is called a billion (U.S. usage), and 1012 a trillion. Now the U.S. federal government budget is in the trillions of dollars, ordinary people really cannot grasp the magnitude of the number. In the metric system, the prefix kilo- stands for 1,000, e.g., a kilogram. For a million, the prefix mega- is used, e.g. megaton (1,000,000 or 106 ton). A billion hertz (a unit of frequency) is gigahertz, although I have not heard of the use of a giga-meter. More rarely still is the use of tera (1012). For small numbers, the practice is similar. 0.1 is 10À1, 0.01 is 10À2, and 0.001 is 10À3. The prefix of milli- refers to 10À3, e.g. as in millimeter, whereas a micro- second is 10À6 ¼ 0.000001 s. It is now trendy to talk about nano-technology, which refers to solid-state device with sizes on the scale of 10À9 m, or about 10 times the size of an atom. With this kind of shorthand convenience, one can really go overboard.
    [Show full text]
  • Astrometry and Optics During the Past 2000 Years
    1 Astrometry and optics during the past 2000 years Erik Høg Niels Bohr Institute, Copenhagen, Denmark 2011.05.03: Collection of reports from November 2008 ABSTRACT: The satellite missions Hipparcos and Gaia by the European Space Agency will together bring a decrease of astrometric errors by a factor 10000, four orders of magnitude, more than was achieved during the preceding 500 years. This modern development of astrometry was at first obtained by photoelectric astrometry. An experiment with this technique in 1925 led to the Hipparcos satellite mission in the years 1989-93 as described in the following reports Nos. 1 and 10. The report No. 11 is about the subsequent period of space astrometry with CCDs in a scanning satellite. This period began in 1992 with my proposal of a mission called Roemer, which led to the Gaia mission due for launch in 2013. My contributions to the history of astrometry and optics are based on 50 years of work in the field of astrometry but the reports cover spans of time within the past 2000 years, e.g., 400 years of astrometry, 650 years of optics, and the “miraculous” approval of the Hipparcos satellite mission during a few months of 1980. 2011.05.03: Collection of reports from November 2008. The following contains overview with summary and link to the reports Nos. 1-9 from 2008 and Nos. 10-13 from 2011. The reports are collected in two big file, see details on p.8. CONTENTS of Nos. 1-9 from 2008 No. Title Overview with links to all reports 2 1 Bengt Strömgren and modern astrometry: 5 Development of photoelectric astrometry including the Hipparcos mission 1A Bengt Strömgren and modern astrometry ..
    [Show full text]
  • The Ancient Star Catalog
    Vol. 12 2002 Sept ISSN 1041­5440 DIO The International Journal of Scientific History The Ancient Star Catalog Novel Evidence at the Southern Limit (still) points to Hipparchan authorship Instruments & Coordinate Systems New Star Identifications 2 2002 Sept DIO 12 2002 Sept DIO 12 3 Table of Contents Page: 1 The Southern Limit of the Ancient Star Catalog by KEITH A. PICKERING 3 z z1 The Southern Limits of the Ancient Star Catalog 2 On the Clarity of Visibility Tests by DENNIS DUKE 28 z and the Commentary of Hipparchos 3 The Measurement Method of the Almagest Stars by DENNIS DUKE 35 z 4 The Instruments Used by Hipparchos by KEITH A. PICKERING 51 by KEITH A. PICKERING1 z 5 A Reidentification of some entries in the Ancient Star Catalog z by KEITH A. PICKERING 59 A Full speed ahead into the fog A1 The Ancient Star Catalog (ASC) appears in books 7 and 8 of Claudius Ptolemy's classic work Mathematike Syntaxis, commonly known as the Almagest. For centuries, Instructions for authors wellinformed astronomers have suspected that the catalog was plagiarized from an earlier star catalog2 by the great 2nd century BC astronomer Hipparchos of Nicaea, who worked See our requirements on the inside back cover. Contributors should send (expendable primarily on the island of Rhodes. In the 20th century, these suspicions were strongly photocopies of) papers to one of the following DIO referees — and then inquire of him by confirmed by numerical analyses put forward by Robert R. Newton and Dennis Rawlins. phone in 40 days: A2 On 15 January 2000, at the 195th meeting of the American Astronomical Society Robert Headland [polar research & exploration], Scott Polar Research Institute, University in Atlanta, Brad Schaefer (then at Yale, later Univ of Texas [later yet: Louisiana State of Cambridge, Lensfield Road, Cambridge, England CB2 1ER.
    [Show full text]
  • High-Accuracy Guide Star Catalogue Generation with a Machine Learning Classification Algorithm
    sensors Article High-Accuracy Guide Star Catalogue Generation with a Machine Learning Classification Algorithm Jianming Zhang , Junxiang Lian *, Zhaoxiang Yi , Shuwang Yang and Ying Shan MOE Key Laboratory of TianQin Mission, TianQin Research Center for Gravitational Physics & School of Physics and Astronomy, Frontiers Science Center for TianQin, CNSA Research Center for Gravitational Waves, Sun Yat-Sen University (Zhuhai Campus), Zhuhai 519082, China; [email protected] (J.Z.); [email protected] (Z.Y.); [email protected] (S.Y.); [email protected] (Y.S.) * Correspondence: [email protected]; Tel.: +86-0756-3668932 Abstract: In order to detect gravitational waves and characterise their sources, three laser links were constructed with three identical satellites, such that interferometric measurements for scientific experiments can be carried out. The attitude of the spacecraft in the initial phase of laser link docking is provided by a star sensor (SSR) onboard the satellite. If the attitude measurement capacity of the SSR is improved, the efficiency of establishing laser linking can be elevated. An important technology for satellite attitude determination using SSRs is star identification. At present, a guide star catalogue (GSC) is the only basis for realising this. Hence, a method for improving the GSC, in terms of storage, completeness, and uniformity, is studied in this paper. First, the relationship between star numbers in the field of view (FOV) of a staring SSR, together with the noise equivalent angle (NEA) of the SSR—which determines the accuracy of the SSR—is discussed. Then, according to the relationship between the number of stars (NOS) in the FOV, the brightness of the stars, and the size of the FOV, two constraints are used to select stars in the SAO GSC.
    [Show full text]
  • The Dating of the Almagest Star Catalogue. Statistical and Geometrical Methods
    chapter 7 The dating of the Almagest star catalogue. Statistical and geometrical methods 1. measurements of most stars’ coordinates have always THE CATALOGUE’S INFORMATIVE KERNEL been based on the so-called reference stars, whose CONSISTS OF THE WELL-MEASURED number is rather small as compared to the total num- NAMED STARS ber of the stars in the catalogue. Let us begin by reiterating a number of consider- The analysis of the Almagest star catalogue related ations voiced in the preceding chapters, which will in Chapters 2-6 had the objective of reducing latitu- serve as a foundation of our dating method. dinal discrepancies in star coordinates by compen- Unfortunately, we do not know which reference sating the systematic error as discovered in the cata- star set was used by the author of the Almagest. All logue. we do know is that it must have included Regulus As a result, we have proven that the Almagest com- and Spica, since the measurement of their coordi- piler’s claim about the precision margin of his meas- nates is discussed in separate dedicated sections of urements being less than 10' is justified – insofar as the Almagest. However, it would make sense to as- the latitudes of most stars from celestial area A are sume that the compiler of the catalogue was at his concerned, at least. We believe this circumstance to most accurate when he measured the coordinates of be of paramount importance. named stars. As it was stated above, there are twelve However, we can only date the Almagest catalogue such stars in the Almagest: Arcturus, Regulus, Spica, by considering fast and a priori precisely measurable Previndemiatrix, Cappella, Lyra = Vega, Procyon, stars.
    [Show full text]
  • Stars and Their Spectra: an Introduction to the Spectral Sequence Second Edition James B
    Cambridge University Press 978-0-521-89954-3 - Stars and Their Spectra: An Introduction to the Spectral Sequence Second Edition James B. Kaler Index More information Star index Stars are arranged by the Latin genitive of their constellation of residence, with other star names interspersed alphabetically. Within a constellation, Bayer Greek letters are given first, followed by Roman letters, Flamsteed numbers, variable stars arranged in traditional order (see Section 1.11), and then other names that take on genitive form. Stellar spectra are indicated by an asterisk. The best-known proper names have priority over their Greek-letter names. Spectra of the Sun and of nebulae are included as well. Abell 21 nucleus, see a Aurigae, see Capella Abell 78 nucleus, 327* ε Aurigae, 178, 186 Achernar, 9, 243, 264, 274 z Aurigae, 177, 186 Acrux, see Alpha Crucis Z Aurigae, 186, 269* Adhara, see Epsilon Canis Majoris AB Aurigae, 255 Albireo, 26 Alcor, 26, 177, 241, 243, 272* Barnard’s Star, 129–130, 131 Aldebaran, 9, 27, 80*, 163, 165 Betelgeuse, 2, 9, 16, 18, 20, 73, 74*, 79, Algol, 20, 26, 176–177, 271*, 333, 366 80*, 88, 104–105, 106*, 110*, 113, Altair, 9, 236, 241, 250 115, 118, 122, 187, 216, 264 a Andromedae, 273, 273* image of, 114 b Andromedae, 164 BDþ284211, 285* g Andromedae, 26 Bl 253* u Andromedae A, 218* a Boo¨tis, see Arcturus u Andromedae B, 109* g Boo¨tis, 243 Z Andromedae, 337 Z Boo¨tis, 185 Antares, 10, 73, 104–105, 113, 115, 118, l Boo¨tis, 254, 280, 314 122, 174* s Boo¨tis, 218* 53 Aquarii A, 195 53 Aquarii B, 195 T Camelopardalis,
    [Show full text]
  • ASTRONOMY and ASTROPHYSICS a Comparison of the SAO
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE Astron. Astrophys. 359, 1195–1200 (2000) ASTRONOMYprovided by SEDICI - Repositorio de la UNLP AND ASTROPHYSICS A comparison of the SAO-Hipparcos reference frames E.F. Arias?, R.G. Cionco, R.B. Orellana?, and H. Vucetich? Facultad de Ciencias Astronomicas´ y Geof´ısicas (FCAG), Paseo del Bosque S/N, Universidad Nacional de La Plata, 1900, Argentina Received 6 December 1999 / Accepted 10 May 2000 Abstract. The reference systems defined by the SAO and Hip- the IAU recommendations (Bergeron 1992) on the definition of parcos catalogues are compared using vector spherical harmonic the system. The origin of the system is at the barycentre of the analysis. The differences between astrometric data in both cat- Solar System; the principal plane is close to the mean equator at alogues have been grouped into different data sets and separate J2000.0. The shift of the Earth’s mean pole at J2000.0 relative harmonic analysis performed on them. The Fourier coefficients to the ICRS celestial pole is 18:0 0:1 mas in the direction 12h yield estimates of systematic errors in SAO catalogue. and 5:3 0:1 mas in the direction± 18h. As required by the IAU, and for± the sake of continuity with the previous conventional Key words: astrometry – reference systems – catalogs system, the direction of the ICRS pole is consistent with that of the FK5 system within the uncertainty of the latter; assuming that the error in the precession rate is absorbed by the proper mo- tions of stars, the uncertainty of the FK5 pole position relative to 1.
    [Show full text]
  • 1910Ap J 31 8B on a GREAT NEBULOUS REGION
    8B 31 J 1910Ap ON A GREAT NEBULOUS REGION AND ON THE QUES- TION OF ABSORBING MATTER IN SPACE AND THE TRANSPARENCY OF THE NEBULAE By E. E. BARNARD While photographing the region of the great nebula of p Ophiuchi (which I had found with the Willard lens) at the Lick Observatory in 1893, the plates with the small lantern lens (ii inches diameter, also attached to the Willard mounting) showed a remarkable nebula involving the 4.5 magnitude star v Scorpii (Plate I). It had not been noticed on the Willard lens photograph, where it was very faint and near the edge of the plate. The discovery of this object therefore is due to the small lantern lens. Roughly this nebula is bounded by the figure formed by the follow- ing places (for 1855.0) : a S f j i5h 59m —180 2o/ 16 4 —18 o and 16 10 —21 00 16 16 —18 50 In its fainter portions it involves to the southeast the stars B. D. i9?4357, —19?4359, and — i9?436i. The last two are in a dense nebulous mass in which on the north following side close to the stars are a thin dark lane and a narrow strip of brighter nebulosity. These two stars are joined to —19?4357, which is itself nebulous, by a thin thread of nebulosity which is well shown in Plate II A. North and following these objects are dark regions where there are apparently very few stars. The extensions of this great nebula reach to, and in a feeble manner connect with, the great nebula of p Ophiuchi.
    [Show full text]
  • Three Editions of the Star Catalogue of Tycho Brahe*
    A&A 516, A28 (2010) Astronomy DOI: 10.1051/0004-6361/201014002 & c ESO 2010 Astrophysics Three editions of the star catalogue of Tycho Brahe Machine-readable versions and comparison with the modern Hipparcos Catalogue F. Verbunt1 andR.H.vanGent2,3 1 Astronomical Institute, Utrecht University, PO Box 80 000, 3508 TA Utrecht, The Netherlands e-mail: [email protected] 2 URU-Explokart, Faculty of Geosciences, Utrecht University, PO Box 80 115, 3508 TC Utrecht, The Netherlands 3 Institute for the History and Foundations of Science, PO Box 80 000, 3508 TA Utrecht, The Netherlands Received 6 January 2010 / Accepted 3 February 2010 ABSTRACT Tycho Brahe completed his catalogue with the positions and magnitudes of 1004 fixed stars in 1598. This catalogue circulated in manuscript form. Brahe edited a shorter version with 777 stars, printed in 1602, and Kepler edited the full catalogue of 1004 stars, printed in 1627. We provide machine-readable versions of the three versions of the catalogue, describe the differences between them and briefly discuss their accuracy on the basis of comparison with modern data from the Hipparcos Catalogue. We also compare our results with earlier analyses by Dreyer (1916, Tychonis Brahe Dani Scripta Astronomica, Vol. II) and Rawlins (1993, DIO, 3, 1), finding good overall agreement. The magnitudes given by Brahe correlate well with modern values, his longitudes and latitudes have error distributions with widths of 2, with excess numbers of stars with larger errors (as compared to Gaussian distributions), in particular for the faintest stars. Errors in positions larger than 10, which comprise about 15% of the entries, are likely due to computing or copying errors.
    [Show full text]
  • The Night Sky This Month
    The Night Sky (April 2020) BST (Universal Time plus one hour) is used this month. Northern Horizon Eastern Western Horizon Horizon 23:00 BST at beginning of the month 22:00 BST in middle of month 21:00 BST at end of month Southern Horizon The General Weather Pattern Surprisingly rainfall is not particularly high in April, but of course heavy rain showers do occur, often with hail and thunder. Expect it to be cloudy. Temperatures usually rise steadily, but clear evenings can still be cold with very cold mornings. Wear multiple layers of clothes, with a warm hat, socks and shoes to maintain body heat. As always, an energy snack and a flask containing a warm non-alcoholic drink might well be welcome at some time. Should you be interested in obtaining a detailed weather forecast for observing in the Usk area, log on to https://www.meteoblue.com/en/weather/forecast/seeing/usk_united-kingdom_2635052 other locations are available. Earth (E) As the Earth moves from the vernal equinox in March, the days are still opening out rapidly. The Moon no longer raises high in the mid-night sky as it does in the winter, but relocates at lower latitudes for the summer. The Sun, of course, does the converse. Artificial Satellites or Probes Should you be interested in observing the International Space Station or other space craft, carefully log on to http://www.heavens-above.com to acquire up-to-date information for your observing site. Sun Conditions apply as to the use of this matter. © D J Thomas 2020 (N Busby 2019) The Sun is becoming better placed for observing as it climbs to more northerly latitudes, and, it is worth reminding members that sunlight contains radiation across the spectrum that is harmful to our eyes and that the projection method should be used.
    [Show full text]
  • Yes, Aboriginal Australians Can and Did Discover the Variability of Betelgeuse
    Journal of Astronomical History and Heritage, 21(1), 7‒12 (2018). YES, ABORIGINAL AUSTRALIANS CAN AND DID DISCOVER THE VARIABILITY OF BETELGEUSE Bradley E. Schaefer Department of Physics and Astronomy, Louisiana State University, Baton Rouge, Louisiana, 70803, USA Email: [email protected] Abstract: Recently, a widely publicized claim has been made that the Aboriginal Australians discovered the variability of the red star Betelgeuse in the modern Orion, plus the variability of two other prominent red stars: Aldebaran and Antares. This result has excited the usual healthy skepticism, with questions about whether any untrained peoples can discover the variability and whether such a discovery is likely to be placed into lore and transmitted for long periods of time. Here, I am offering an independent evaluation, based on broad experience with naked-eye sky viewing and astro-history. I find that it is easy for inexperienced observers to detect the variability of Betelgeuse over its range in brightness from V = 0.0 to V = 1.3, for example in noticing from season-to-season that the star varies from significantly brighter than Procyon to being greatly fainter than Procyon. Further, indigenous peoples in the Southern Hemisphere inevitably kept watch on the prominent red star, so it is inevitable that the variability of Betelgeuse was discovered many times over during the last 65 millennia. The processes of placing this discovery into a cultural context (in this case, put into morality stories) and the faithful transmission for many millennia is confidently known for the Aboriginal Australians in particular. So this shows that the whole claim for a changing Betelgeuse in the Aboriginal Australian lore is both plausible and likely.
    [Show full text]
  • A History of Star Catalogues
    A History of Star Catalogues © Rick Thurmond 2003 Abstract Throughout the history of astronomy there have been a large number of catalogues of stars. The different catalogues reflect different interests in the sky throughout history, as well as changes in technology. A star catalogue is a major undertaking, and likely needs strong justification as well as the latest instrumentation. In this paper I will describe a representative sample of star catalogues through history and try to explain the reasons for conducting them and the technology used. Along the way I explain some relevent terms in italicized sections. While the story of any one catalogue can be the subject of a whole book (and several are) it is interesting to survey the history and note the trends in star catalogues. 1 Contents Abstract 1 1. Origin of Star Names 4 2. Hipparchus 4 • Precession 4 3. Almagest 5 4. Ulugh Beg 6 5. Brahe and Kepler 8 6. Bayer 9 7. Hevelius 9 • Coordinate Systems 14 8. Flamsteed 15 • Mural Arc 17 9. Lacaille 18 10. Piazzi 18 11. Baily 19 12. Fundamental Catalogues 19 12.1. FK3-FK5 20 13. Berliner Durchmusterung 20 • Meridian Telescopes 21 13.1. Sudlich Durchmusterung 21 13.2. Cordoba Durchmusterung 22 13.3. Cape Photographic Durchmusterung 22 14. Carte du Ciel 23 2 15. Greenwich Catalogues 24 16. AGK 25 16.1. AGK3 26 17. Yale Bright Star Catalog 27 18. Preliminary General Catalogue 28 18.1. Albany Zone Catalogues 30 18.2. San Luis Catalogue 31 18.3. Albany Catalogue 33 19. Henry Draper Catalogue 33 19.1.
    [Show full text]