DOCSLIB.ORG

FY1991 Q1 Oct-Dec NO

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
FY1991 Q1 Oct-Dec NO National Optical Astronomy Observatories National Optical Astronomy Observatories Quarterly Report October - December 1990 TABLE OF CONTENTS I. INTRODUCTION 1 II. SCIENTIFIC HIGHLIGHTS 1 A. Cosmis Voids 1 B. Chiron 2 C. Surface Dynamics 2 D. South Pole Observations 3 E. Effect of Active Regions on Intermediate-Degree Solar Oscillations 3 F. Resolved Images of High Redshift QSOs: A First Look 4 G. Astrophysical Jets: More Robust than Previously Thought? 4 H. Sub-Arcsecond Structure of R Aquarii: An Accretion Disk Revealed 5 III. PERSONNEL 6 A. Visiting Scientists 6 B. New Hires 6 C. Terminations 6 D. Change in Status 6 IV. INSTRUMENTATION, NEW PROJECTS, AND OBSERVATORY ACTIVITIES . 7 A. 8-M Project 7 B. Advanced Optical Telescope Technology Program (AOTT) 8 C. Global Oscillation Network Group (GONG) 9 D. WIYN Project 10 E. Instrumentation Projects 11 F. Observatory Activities 16 V. PROGRAM SUPPORT 17 A. Director's Office 17 B. Central Administrative Services 19 C. Central Computer Services 19 D. Central Facilities Operations 20 E. Engineering and Technical Services 21 F. Publications and Information Resources 21 Appendices Appendix A Telescope Usage Statistics Appendix B Observational Programs Appendix C NOAO Annual Safety Report I. INTRODUCTION This quarterly report covers scientific highlights for the period of October through December 1990, as well as personnel changes for the period. The report also discusses progress on the 8-m telescopes, GONG, WIYN, and instrumentation projects. The appendices list telescope usage statistics and observational programs. II. SCIENTIFIC HIGHLIGHTS A. Cosmic Voids The observed smoothness of the cosmic background radiation leads one to expect that at a sufficiently large scale the universe should be homogenous. To test this expectation the space distribution of galaxies must be determined over the largest possible sky areas and, if redshifts are used as distance indicators, they must be determined for the faintest possible galaxies. However, properly done, this is such an enormous task that available surveys have been necessarily limited to finite sky areas and to galaxies brighter than convenient limits. A prime example is the on-going survey being carried out by Harvard Smithsonian Center for Astrophysics (CfA) astronomers J.P. Huchra, M. Geller, and collaborators. In this survey, galaxies brighter than about magnitude 15.5 are surveyed in sky areas consisting of strips a few degrees wide in declination but extending over a wide range of right ascension. This survey has shown extensive sheet-like concentrations of galaxies including the so- called "Great Wall." Since the sky strips are not necessarily contiguous and only relatively bright galaxies are observed, the CfA survey is not ideal for the study of what appears to be extensive voids surrounded by concentrations of galaxies. A survey adapted to the study of possible voids was undertaken by R.P. Kirshner (Harvard U.), A. Oemler (Yale U.), P.L. Schechter (Massachusetts Inst, of Tech.), and S.A. Shectman (Carnegie Obs.). Galaxies brighter than about magnitude 17 located within a set of small sample regions near the galactic north pole were included. The extremely large number of galaxies in the extensive sky area that had to be surveyed in order to delineate a possible void, made it necessary to limit the study to such sample regions. Observations obtained in 1987 with the Palomar 5-m telescope and with the KPNO 4-m telescope resulted in the finding of an apparent void toward the constellation of Bootes. With a 106 Mpc3 volume, the so-called Bootes void is a statistically significant low density region for normal galaxies. A similar survey has now been completed in the southern hemisphere. With spectroscopic observations obtained with the Las Campanas 2.5-m telescope and photometric observations obtained with the CTIO 1.5-m telescope, Kirshner, Oemler, Schechter, and Shectman have found evidence of a possible void toward the constellation of Phoenix. This survey included 150 galaxies brighter than magnitude 17.6. Again, numerous sample regions were selected. These spread over a 25 degree diameter area. The observed galaxies show a significant low density region between redshifts 11,600 and 15,400 km/sec. The apparent Phoenix void is, however, not as clearly defined as the one in Bo5tes. A search for the galaxies that might have been missed in the 25 degree area covered by the sample region shows, at a redshift of 14,500 km/sec, a clustering of galaxies. Also, three compact bright galaxies within the region have radial velocities that place them within the suspected void. Independent surveys by other investigators show that additional galaxies, near the periphery of the apparent low-density region, have radial velocities within the range mentioned earlier. Prudently, Kirshner, Oemler, Schechter, and Shectman consider the possibility that the Phoenix "void" may be spurious, but conclude that it probably is an underdense region. So far, existing surveys of distant galaxies show no evidence of homogeneity in the universe. The smoothness of the cosmic background radiation remains a challenging fact for observational cosmologists. B. Chiron In February 1988, when observing at Mauna Kea, astronomers D.J. Tholen, W.K. Hartmann, and D.P. Cruikshank (U. of Hawaii) found that asteroid No. 2060 (Chiron) was 0.7 magnitudes brighter than expected from predictions based on its position in space and its well-known rotational brightness variations. Chiron's bright outburst was found to persist past 31 October when Lowell Observatory astronomers S.J. Bus and E. Boswell, in collaboration with L. French (Massachusetts Inst, of Tech.), observed it with the CTIO 0.9-m telescope. On this occasion, Chiron's rotational light variations showed an unexpected decrease in amplitude. As it turned out, this was the first indication that Chiron was surrounded by a coma. Chiron's orbit with a semi-major axis of 13.7 A.U. places it, even at perihelion, well beyond Jupiter: far away from the asteroid belt. This unique orbit for an asteroid caused numerous speculations about Chiron's origin. Was it perhaps an escaped satellite from one of the outer major planets, or possibly a comet captured by the gravitational attraction of those planets? At first, Chiron's brightness outburst resembled frequently observed episodic cometary activity at large heliocentric distances. This led astronomer K. Meech (U. of Hawaii) to include Chiron in a program of comet observations to be carried out at CTIO in collaboration with KPNO astronomer M. Belton. An aim of the program was to search for a coma surrounding Chiron. Formation of a comet-like coma as Chiron approaches its perihelion could explain its unusual brightness outburst. Observations were made in January 1989 with the CTIO 0.9-m telescope and continued in April 1989 with the KPNO 4-m telescope. On 10 April a 5 arcsec coma surrounding Chiron was detected in KPNO direct CCD images. By its reflectivity, the coma could explain the brightness outburst and why its rotational light variations had been partly masked during the earlier CTIO observations. Further analysis of the observations suggests that the coma is caused by dust particles gravitationally bound to Chiron rather than ejected into space, as in comets. This would explain why its brightness outburst has lasted much longer than those typical of comets. Drs. Meech and Belton suggest that the dust particles may be thrown outward by gas escaping from regions of activity on Chiron's surface. Although its origin remains unknown, Chiron certainly will be carefully monitored as it approaches its 1996 perihelion. C. Surface Dynamics G. Simon, A. Title (Lockheed), and N. Weiss (U. of Cambridge), have been working on the modeling of mesogranules and exploders on the solar surface. Correlation tracking of high-resolution observations reveals a horizontal flow field containing both the supergranulation pattern and a much smaller pattern corresponding to mesogranulation. Exploding granules (exploders) occur preferentially near the centers of mesogranules. This raises the question, Are mesogranules just collections of exploders? Radial outflow in exploders and mesogranules can be modeled by superposing gaussian source functions. Simon, Title, and Weiss use this model to explore the relationship between mesogranules and exploders. Although they demonstrate that there is mathematical equivalence between mesogranules and exploders distributed normally about the mesogranules center, their results indicate that the observed mesogranular velocity pattern is not consistent with a flow pattern generated by exploders dropped randomly on the solar surface. Detailed comparison with observations suggests that the averaged mesogranular velocity is produced by a combination of a persistent outflow from a source together with exploders distributed randomly about its center. Similar analysis shows that supergranules are not the result of random occurrences of mesogranules. D. South Pole Observations The high-degree helioseismometer was shipped to the South Pole in mid-September with the goal of obtaining observations of solar oscillations uninterrupted by the day-night cycle. A field party consisting of T. Duvall (NASA), J. Harvey, S. Jefferies (Bartol), D. Neff, and M. Pomerantz (Bartol) departed from the United States on 22 October and arrived at the South Pole on 31 October. Since the camera system has 2 arcsec pixels, they were particularly interested in getting observations of high-degree oscillations at a time of high solar activity. The polar solar observatory site was activated in early November and, after the equipment arrived, the instrument was set up. An initial problem with the high speed guider was located and fixed. First observations were made on 9 November. After a few days of observing, the weather became cloudy and unusually windy. Two storms produced massive snow drifts around the instrument. However, starting on 23 November relatively good weather prevailed for two weeks and a large amount of data was obtained. Measurements of seeing quality were also obtained during this period.
Load more

Recommended publications
  • Milan Dimitrijevic Avgust.Qxd
    1. M. Platiša, M. Popović, M. Dimitrijević, N. Konjević: 1975, Z. Fur Natur- forsch. 30a, 212 [A 1].* 1. Griem, H. R.: 1975, Stark Broadening, Adv. Atom. Molec. Phys. 11, 331. 2. Platiša, M., Popović, M. V., Konjević, N.: 1975, Stark broadening of O II and O III lines, Astron. Astrophys. 45, 325. 3. Konjević, N., Wiese, W. L.: 1976, Experimental Stark widths and shifts for non-hydrogenic spectral lines of ionized atoms, J. Phys. Chem. Ref. Data 5, 259. 4. Hey, J. D.: 1977, On the Stark broadening of isolated lines of F (II) and Cl (III) by plasmas, JQSRT 18, 649. 5. Hey, J. D.: 1977, Estimates of Stark broadening of some Ar III and Ar IV lines, JQSRT 17, 729. 6. Hey, J. D.: Breger, P.: 1980, Stark broadening of isolated lines emitted by singly - ionized tin, JQSRT 23, 311. 7. Hey, J. D.: Breger, P.: 1981, Stark broadening of isolated ion lines by plas- mas: Application of theory, in Spectral Line Shapes I, ed. B. Wende, W. de Gruyter, 201. 8. Сыркин, М. И.: 1981, Расчеты электронного уширения спектральных линий в теории оптических свойств плазмы, Опт. Спектроск. 51, 778. 9. Wiese, W. L., Konjević, N.: 1982, Regularities and similarities in plasma broadened spectral line widths (Stark widths), JQSRT 28, 185. 10. Konjević, N., Pittman, T. P.: 1986, Stark broadening of spectral lines of ho- mologous, doubly ionized inert gases, JQSRT 35, 473. 11. Konjević, N., Pittman, T. P.: 1987, Stark broadening of spectral lines of ho- mologous, doubly - ionized inert gases, JQSRT 37, 311. 12. Бабин, С.
    [Show full text]
  • GTO Keypad Manual, V5.001
    ASTRO-PHYSICS GTO KEYPAD Version v5.xxx Please read the manual even if you are familiar with previous keypad versions Flash RAM Updates Keypad Java updates can be accomplished through the Internet. Check our web site www.astro-physics.com/software-updates/ November 11, 2020 ASTRO-PHYSICS KEYPAD MANUAL FOR MACH2GTO Version 5.xxx November 11, 2020 ABOUT THIS MANUAL 4 REQUIREMENTS 5 What Mount Control Box Do I Need? 5 Can I Upgrade My Present Keypad? 5 GTO KEYPAD 6 Layout and Buttons of the Keypad 6 Vacuum Fluorescent Display 6 N-S-E-W Directional Buttons 6 STOP Button 6 <PREV and NEXT> Buttons 7 Number Buttons 7 GOTO Button 7 ± Button 7 MENU / ESC Button 7 RECAL and NEXT> Buttons Pressed Simultaneously 7 ENT Button 7 Retractable Hanger 7 Keypad Protector 8 Keypad Care and Warranty 8 Warranty 8 Keypad Battery for 512K Memory Boards 8 Cleaning Red Keypad Display 8 Temperature Ratings 8 Environmental Recommendation 8 GETTING STARTED – DO THIS AT HOME, IF POSSIBLE 9 Set Up your Mount and Cable Connections 9 Gather Basic Information 9 Enter Your Location, Time and Date 9 Set Up Your Mount in the Field 10 Polar Alignment 10 Mach2GTO Daytime Alignment Routine 10 KEYPAD START UP SEQUENCE FOR NEW SETUPS OR SETUP IN NEW LOCATION 11 Assemble Your Mount 11 Startup Sequence 11 Location 11 Select Existing Location 11 Set Up New Location 11 Date and Time 12 Additional Information 12 KEYPAD START UP SEQUENCE FOR MOUNTS USED AT THE SAME LOCATION WITHOUT A COMPUTER 13 KEYPAD START UP SEQUENCE FOR COMPUTER CONTROLLED MOUNTS 14 1 OBJECTS MENU – HAVE SOME FUN!
    [Show full text]
  • Optical Astronomy Observatories
    NATIONAL OPTICAL ASTRONOMY OBSERVATORIES NATIONAL OPTICAL ASTRONOMY OBSERVATORIES FY 1994 PROVISIONAL PROGRAM PLAN June 25, 1993 TABLE OF CONTENTS I. INTRODUCTION AND PLAN OVERVIEW 1 II. SCIENTIFIC PROGRAM 3 A. Cerro Tololo Inter-American Observatory 3 B. Kitt Peak National Observatory 9 C. National Solar Observatory 16 III. US Gemini Project Office 22 IV. MAJOR PROJECTS 23 A. Global Oscillation Network Group (GONG) 23 B. 3.5-m Mirror Project 25 C. WIYN 26 D. SOAR 27 E. Other Telescopes at CTIO 28 V. INSTRUMENTATION 29 A. Cerro Tololo Inter-American Observatory 29 B. Kitt Peak National Observatory 31 1. KPNO O/UV 31 2. KPNO Infrared 34 C. National Solar Observatory 38 1. Sacramento Peak 38 2. Kitt Peak 40 D. Central Computer Services 44 VI. TELESCOPE OPERATIONS AND USER SUPPORT 45 A. Cerro Tololo Inter-American Observatory 45 B. Kitt Peak National Observatory 45 C. National Solar Observatory 46 VII. OPERATIONS AND FACILITIES MAINTENANCE 46 A. Cerro Tololo 47 B. Kitt Peak 48 C. NSO/Sacramento Peak 48 D. NOAO Tucson Headquarters 49 VIII. SCIENTIFIC STAFF AND SUPPORT 50 A. CTIO 50 B. KPNO 50 C. NSO 51 IX. PROGRAM SUPPORT 51 A. NOAO Director's Office 51 B. Central Administrative Services 52 C. Central Computer Services 52 D. Central Facilities Operations 53 E. Engineering and Technical Services 53 F. Publications and Information Resources 53 X. RESEARCH EXPERIENCES FOR UNDERGRADUATES PROGRAM 54 XI. BUDGET 55 A. Cerro Tololo Inter-American Observatory 56 B. Kitt Peak National Observatory 56 C. National Solar Observatory 57 D. Global Oscillation Network Group 58 E.
    [Show full text]
  • II. Relative Ages and Distances for Six Ancient Globular Clusters
    Mon. Not. R. Astron. Soc. 000, 1{?? (2002) Printed 7 April 2018 (MN LATEX style file v2.2) Exploring the nature and synchronicity of early cluster formation in the Large Magellanic Cloud: II. Relative ages and distances for six ancient globular clusters R. Wagner-Kaiser1, Dougal Mackey2, Ata Sarajedini1;3, Brian Chaboyer4, Roger E. Cohen5, Soung-Chul Yang6, Jeffrey D. Cummings7, Doug Geisler8, Aaron J. Grocholski9 1University of Florida, Department of Astronomy, 211 Bryant Space Science Center, Gainesville, FL, 32611 USA 2Australian National University, Research School of Astronomy & Astrophysics, Canberra, ACT 2611, Australia 3Florida Atlantic University, Department of Physics, 777 Glades Rd, Boca Raton, FL, 33431 USA 4Dartmouth College, Department of Physics and Astronomy, Hanover, NH, 03755, USA 5Space Telescope Science Institute, Baltimore, MD 21218, USA 6Korea Astronomy and Space Science Institute (KASI), Daejeon 305-348, Korea 7Center for Astrophysical Sciences, Johns Hopkins University, Baltimore MD 21218 8Departamento de Astronomia, Universidad de Concepcion, Casilla 160-C, Concepcion, Chile 9Department of Physics and Astronomy, Swarthmore College, Swarthmore, PA 19081, USA ABSTRACT We analyze Hubble Space Telescope observations of six globular clusters in the Large Magellanic Cloud from program GO-14164 in Cycle 23. These are the deepest available observations of the LMC globular cluster population; their uniformity facilitates a precise comparison with globular clusters in the Milky Way. Measuring the magnitude of the main sequence turnoff point relative to template Galactic globular clusters allows the relative ages of the clusters to be determined with a mean precision of 8.4%, and down to 6% for individual objects. We find that the mean age of our LMC cluster ensemble is identical to the mean age of the oldest metal-poor clusters in the Milky Way halo to 0.2 ± 0.4 Gyr.
    [Show full text]
  • Properties of Stellar Generations in Globular Clusters and Relations With
    Astronomy & Astrophysics manuscript no. carretta c ESO 2018 November 9, 2018 Properties of stellar generations in Globular Clusters and relations with global parameters ⋆ E. Carretta1, A. Bragaglia1, R.G. Gratton2, A. Recio-Blanco3, S. Lucatello2,4, V. D’Orazi2, and S. Cassisi5 1 INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy 2 INAF-Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 3 Laboratoire Cassiop´ee UMR 6202, Universit`ede Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d’Azur, BP 4229, 06304 Nice Cedex 4, France 4 Excellence Cluster Universe, Technische Universit¨at M¨unchen, Boltzmannstr. 2, D-85748, Garching, Germany 5 INAF-Osservatorio Astronomico di Collurania, via M. Maggini, I-64100 Teramo, Italy Received .....; accepted ..... ABSTRACT We revise the scenario of the formation of Galactic globular clusters (GCs) by adding the observed detailed chemical composition of their different stellar generations to the set of their global parameters. We exploit the unprecedented set of homogeneous abundances of more than 1200 red giants in 19 clusters, as well as additional data from literature, to give a new definition of bona fide globular clusters, as the stellar aggregates showing the presence of the Na-O anticorrelation. We propose a classification of GCs according to their kinematics and location in the Galaxy in three populations: disk/bulge, inner halo, and outer halo. We find that the luminosity function of globular clusters is fairly independent of their population, suggesting that it is imprinted by the formation mechanism, and only marginally affected by the ensuing evolution. We show that a large fraction of the primordial population should have been lost by the proto-GCs.
    [Show full text]
  • CCD Double Star Measurements - Personal Observations: #Report 1
    Vol. 8 No. 3 July 1, 2012 Journal of Double Star Observations Page 193 CCD Double Star Measurements - Personal Observations: #Report 1 Giuseppe Micello Bologna Emilia Romagna - Italy EMAIL: [email protected] Abstract: This report submits CCD measurements of 49 pairs, observed in the period No- vember 2011 – January 2012. Possible new pairs, not cataloged in the Washington Double Star Catalog, are suggested. Orionis (precise coordinate from the Aladin Sky At- Introduction las: 05:19:06.14 +02:34:27.0, Figure 3) and new pair Between November 2011 and January 2012, I in system STF 721/GUI 7/BU 557 (precise coordinate made measurements of 49 double and multiple stars. from the Aladin Sky Atlas: 05:29:39.01 +03:06:47.5, For these measurements, I used a Schmidt- Figure 4). Cassegrain 235/2350 and a Maksutov-Cassegrain In this system, GUI 7AD is a neglected double 150/1800 on equatorial mount and the optical train star and we have only one measurement, dating back composed of a CCD camera, Imaging Source to 1904. DMK21AU, and an IR Cut Filter on Flip Mirror. The method is the same that I reported in a pre- Acknowledgements vious papers [1, 2] where I used Reduc by Florent This research has made use of the catalogs pre- Losse for data reduction,. sent in The Aladin Sky Atlas. Astrometric measurements and references to im- I thank Florent Losse for excellent software Re- ages and notes, are included in Table 1. duc. This paper also includes new possible pairs not I thank the Washington Double Star Catalog and cataloged in the Washington Double Star Catalog [3].
    [Show full text]
  • Binocular Challenges
    This page intentionally left blank Cosmic Challenge Listing more than 500 sky targets, both near and far, in 187 challenges, this observing guide will test novice astronomers and advanced veterans alike. Its unique mix of Solar System and deep-sky targets will have observers hunting for the Apollo lunar landing sites, searching for satellites orbiting the outermost planets, and exploring hundreds of star clusters, nebulae, distant galaxies, and quasars. Each target object is accompanied by a rating indicating how difficult the object is to find, an in-depth visual description, an illustration showing how the object realistically looks, and a detailed finder chart to help you find each challenge quickly and effectively. The guide introduces objects often overlooked in other observing guides and features targets visible in a variety of conditions, from the inner city to the dark countryside. Challenges are provided for viewing by the naked eye, through binoculars, to the largest backyard telescopes. Philip S. Harrington is the author of eight previous books for the amateur astronomer, including Touring the Universe through Binoculars, Star Ware, and Star Watch. He is also a contributing editor for Astronomy magazine, where he has authored the magazine’s monthly “Binocular Universe” column and “Phil Harrington’s Challenge Objects,” a quarterly online column on Astronomy.com. He is an Adjunct Professor at Dowling College and Suffolk County Community College, New York, where he teaches courses in stellar and planetary astronomy. Cosmic Challenge The Ultimate Observing List for Amateurs PHILIP S. HARRINGTON CAMBRIDGE UNIVERSITY PRESS Cambridge, New York, Melbourne, Madrid, Cape Town, Singapore, Sao˜ Paulo, Delhi, Dubai, Tokyo, Mexico City Cambridge University Press The Edinburgh Building, Cambridge CB2 8RU, UK Published in the United States of America by Cambridge University Press, New York www.cambridge.org Information on this title: www.cambridge.org/9780521899369 C P.
    [Show full text]
  • On the Application of Stark Broadening Data Determined with a Semiclassical Perturbation Approach
    Atoms 2014, 2, 357-377; doi:10.3390/atoms2030357 OPEN ACCESS atoms ISSN 2218-2004 www.mdpi.com/journal/atoms Article On the Application of Stark Broadening Data Determined with a Semiclassical Perturbation Approach Milan S. Dimitrijević 1,2,* and Sylvie Sahal-Bréchot 2 1 Astronomical Observatory, Volgina 7, 11060 Belgrade, Serbia 2 Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique, Observatoire de Paris, UMR CNRS 8112, UPMC, 5 Place Jules Janssen, 92195 Meudon Cedex, France; E-Mail: [email protected] (S.S.-B.) * Author to whom correspondence should be addressed; E-Mail: [email protected]; Tel.: +381-64-297-8021; Fax: +381-11-2419-553. Received: 5 May 2014; in revised form: 20 June 2014 / Accepted: 16 July 2014 / Published: 7 August 2014 Abstract: The significance of Stark broadening data for problems in astrophysics, physics, as well as for technological plasmas is discussed and applications of Stark broadening parameters calculated using a semiclassical perturbation method are analyzed. Keywords: Stark broadening; isolated lines; impact approximation 1. Introduction Stark broadening parameters of neutral atom and ion lines are of interest for a number of problems in astrophysical, laboratory, laser produced, fusion or technological plasma investigations. Especially the development of space astronomy has enabled the collection of a huge amount of spectroscopic data of all kinds of celestial objects within various spectral ranges. Consequently, the atomic data for trace elements, which had not been
    [Show full text]
  • 1.4 the Magellanic Clouds
    The copyright of this thesis vests in the author. No quotation from it or information derived from it is to be published without full acknowledgementTown of the source. The thesis is to be used for private study or non- commercial research purposes only. Cape Published by the University ofof Cape Town (UCT) in terms of the non-exclusive license granted to UCT by the author. University THE STRUCTURE OF THE LARGE MAGELLANIC CLOUD By Oyirwoth Patrick Abedigamba Town A dissertation submitted in partial fulfillmentCape of the requirements for the degree M.Sc. in the Departmentof of Astronomy, as part of the National Astrophysics and Space Science Programme UNIVERSITY OF CAPE TOWN AUGUST 2010 University Supervisors: Honorary. Prof. Michael Feast1,2 Prof. Patricia Whitelock2,1 1Astronomy Department, University of Cape Town 2South African Astronomical Observatory Key words Large Magellanic Cloud, RR Lyrae stars, Optical Gravitational Lensing Experiment, Fourier parameters, metallicity [Fe/H]. Town Cape of University i Abstract This work gives an account of the study of the metallicity [Fe/H] distribution (gradient) in the oldest population in the Large Magellanic Cloud (LMC), by making use of the available RR Lyrae data from the Optical Gravitational Lensing Experiment III (OGLE III). RR Lyrae stars are amongst the oldest objects in the universe and they have a range in element (metal) abundances. Measuring the distribution of metallicities of RR Lyrae stars in a galaxy gives one clues to the origin of galaxies. It is known that the pulsation periods of RR Lyraes is broadly correlated with their metallicity. This fact has been used for investigating the metallicity distribution of RR Lyrae stars in the LMC.
    [Show full text]
  • Ngc Catalogue Ngc Catalogue
    NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39
    [Show full text]
  • ANDREA KUNDER an Der Sternwarte 16 14482 Potsdam, Germany B: [email protected] Curriculum Vitae : +49-331-58395304 M
    Leibniz Institut für Astrophysik ANDREA KUNDER An der Sternwarte 16 14482 Potsdam, Germany B: [email protected] Curriculum Vitae : +49-331-58395304 m: www.aip.de/∼akunder EDUCATION June 2009 Dartmouth College; Hanover, NH PhD in Physics & Astronomy Advisor: Dr. Brian C. Chaboyer Thesis: RR Lyrae stars as tracers of stellar populations in the Galactic bulge and satellite galaxies May 2003 Willamette University; Salem, OR Bachlelors of Arts in Chemistry and German; GPA: 3.73/4.00 2000 - 2001 Ludwig-Maximillians Universität München; Munich, Germany Immersion program in language, culture, and history. 2002 Columbia University’s Biosphere 2; Oracle, AZ Universe Semester; Researched RR Lyrae stars with local telescopes. CURRENT EMPLOYMENT Independent Postdoctoral Fellow, Leibniz Institut für Astrophysik, Potsdam (AIP) PI of a Deutsche Forschungsgemeinschaft (DFG) fully-funded grant to research the Galactic bulge RESEARCH INTERESTS The formation and evolution of Local Group galaxies and the Milky Way through detailed chemical and dynamical studies of individual stars; RR Lyrae stars and distance indicators; Globular clusters and resolved stellar populations. HONORS/AWARDS • 2016 “Eigene Stelle" Deutsche Forschungsgemeinschaft Science Grant (269,650 Euros) • 2013 NOAO Science Excellence Award • 2013 NOAO DECam Installation, Commissioning and Scientific Verification Team Award • 2009 The Dartmouth College Arts and Sciences Graduate Student Research Presentation Award • 2007 Honorable Mention Chambliss Award (AAS) • Mary L. Collins Graduate Scholarship
    [Show full text]
  • Constellations* - Andromeda, Aries, Auriga, Cassiopeia, Gemini, Orion, Pegasus
    Contact information: Inside this issue: Info Officer (General Info) – [email protected] Website Administrator – [email protected] Page December Club Calendar 3 Postal Address: Fort Worth Astronomical Society Celestial Events 4 c/o Matt McCullar Interesting Objects 4 5801 Trail Lake Drive Young Astronomer News 5 Fort Worth, TX 76133 Good To Know 5 Web Site: http://www.fortworthastro.org (or .com) 6 Facebook: http://tinyurl.com/3eutb22 Cloudy Night Library Twitter: http://twitter.com/ftwastro Monthly AL Observing Club 8 Yahoo! eGroup (members only): http://tinyurl.com/7qu5vkn Buzz Aldrin & FWAS Mbr Photos 9 Officers (2015-2016): TSNF Photography Contest 10 President – Bruce Cowles, [email protected] 2016 TSP Registration Notice 11 Vice President – Si Simonson, [email protected] Constellation of the Month 12 Sec/Tres – Michelle Theisen, [email protected] Constellation Mythology 13 Board Members: Monthly Sky Chart 14 2014-2016 15 Mike Langohr Monthly Planet Visibility Tree Oppermann ISS Visible Passes for DFW 15 2015-2017 Moon Phase Calendar 16 Matt Reed 1st/Last Crescent/Ephem 17 Phil Stage Conjunctions:Lunar/Planet 18 Minor Planets/Comets 19-21 Cover Photo: Mercury/Venus Data 22 The Flaming Star was captured and pro- cessed as one shot color from 3RF. It Jupiter Data 23 was taken with an Esprit 150, Canon 6D Fundraising/Donation Info 24 and an EQ8 mount. Photo by FWAS member, Jerry Gardner. General Meeting Minutes 25 That’s A Fact 26 Observing Site Reminders: Full Moon Name 26 Be careful with fire, mind all local burn bans! FWAS Fotos 27 Dark Site Usage Requirements (ALL MEMBERS): Maintain Dark-Sky Etiquette (http://tinyurl.com/75hjajy) Turn out your headlights at the gate! Edito r: Sign the logbook (in camo-painted storage shed.
    [Show full text]