Nexstar 8 & 11 GPS Star List
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Li-Rich K Giants, Dust Excess, and Binarity?,?? A
Astronomy & Astrophysics manuscript no. SBcorr c ESO 2020 July 13, 2020 Li-rich K giants, dust excess, and binarity?;?? A. Jorissen1, H. Van Winckel2, L. Siess1, A. Escorza1;2, D. Pourbaix1, and S. Van Eck1 1 Institut d’Astronomie et d’Astrophysique, Universite´ Libre de Bruxelles, ULB, CP. 226, Boulevard du Triomphe, 1050 Brussels, Belgium e-mail: [email protected] 2 Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D bus 2401, B-3001 Leuven, Belgium Received ...; accepted ... ABSTRACT The origin of the Li-rich K giants is still highly debated. Here, we investigate the incidence of binarity among this family from a nine- year radial-velocity monitoring of a sample of 11 Li-rich K giants using the HERMES spectrograph attached to the 1.2m Mercator telescope. A sample of 13 non-Li-rich giants (8 of them being surrounded by dust according to IRAS, WISE, and ISO data) was monitored alongside. When compared to the binary frequency in a reference sample of 190 K giants (containing 17.4% of definite spectroscopic binaries – SB – and 6.3% of possible spectroscopic binaries – SB?), the binary frequency appears normal among the Li-rich giants (2/11 definite binaries plus 2 possible binaries, or 18.2% SB + 18.2% SB?), after taking account of the small sample size through the hypergeometric probability distribution. Therefore, there appears to be no causal relationship between Li enrichment and binarity. Moreover, there is no correlation between Li enrichment and the presence of circumstellar dust, and the only correlation that could be found between Li enrichment and rapid rotation is that the most Li-enriched K giants appear to be fast-rotating stars. -
Ioptron AZ Mount Pro Altazimuth Mount Instruction
® iOptron® AZ Mount ProTM Altazimuth Mount Instruction Manual Product #8900, #8903 and #8920 This product is a precision instrument. Please read the included QSG before assembling the mount. Please read the entire Instruction Manual before operating the mount. If you have any questions please contact us at [email protected] WARNING! NEVER USE A TELESCOPE TO LOOK AT THE SUN WITHOUT A PROPER FILTER! Looking at or near the Sun will cause instant and irreversible damage to your eye. Children should always have adult supervision while observing. 2 Table of Content Table of Content ......................................................................................................................................... 3 1. AZ Mount ProTM Altazimuth Mount Overview...................................................................................... 5 2. AZ Mount ProTM Mount Assembly ........................................................................................................ 6 2.1. Parts List .......................................................................................................................................... 6 2.2. Identification of Parts ....................................................................................................................... 7 2.3. Go2Nova® 8407 Hand Controller .................................................................................................... 8 2.3.1. Key Description ....................................................................................................................... -
Astrometric and Photometric Measurements of Binary Stars with Adaptive Optics: Observations from 2002
A Mon. Not. R. Astron. Soc. 000, 1–9 (2010) Printed 12 September 2018 (MN L TEX style file v2.2) Astrometric and photometric measurements of binary stars with adaptive optics: observations from 2002 Lewis C. Roberts, Jr.1 ⋆ 1 Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena CA 91109, USA ABSTRACT The adaptive optics system at the 3.6 m AEOS telescope was used to measure the astrometry and differential magnitude in I -band of 56 binary stars in 2002. The astrometric measurements will be of use for future orbital determination, and the photometric measurements will be of use in estimating the spectral types of the com- ponent stars. Two candidate companions were detected, but neither is likely to be gravitationally bound. Nine systems had not been observed in over 40 years. Eight of these are shown to share common proper motion, while HD 182352 is shown to be a background star. One of the two components of the HD 114378 (α Com) is shown to be a variable star of unknown type. In addition, 86 stars were unresolved and the full-width half maxima of the images are presented. Key words: binaries: visual, instrumentation: adaptive optics, astrometry, tech- niques: photometric Accepted to MNRAS used, but ranges from 3-5 magnitudes (Mason 1994). Also, in most cases true images are not created, but instead an au- tocorrelation, which can lead to quadrant ambiguity where ◦ 1 INTRODUCTION the position of the companion is off by 180 (Bagnuolo et al. 1992). It is also difficult to extract the photometry from Speckle interferometry has been the dominant technique speckle interferograms, especially with the commonly used for observing visual binary stars for the last several intensified detectors (Roberts 1998). -
LIST of PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute
LIST OF PUBLICATIONS Aryabhatta Research Institute of Observational Sciences ARIES (An Autonomous Scientific Research Institute of Department of Science and Technology, Govt. of India) Manora Peak, Naini Tal - 263 129, India (1955−2020) ABBREVIATIONS AA: Astronomy and Astrophysics AASS: Astronomy and Astrophysics Supplement Series ACTA: Acta Astronomica AJ: Astronomical Journal ANG: Annals de Geophysique Ap. J.: Astrophysical Journal ASP: Astronomical Society of Pacific ASR: Advances in Space Research ASS: Astrophysics and Space Science AE: Atmospheric Environment ASL: Atmospheric Science Letters BA: Baltic Astronomy BAC: Bulletin Astronomical Institute of Czechoslovakia BASI: Bulletin of the Astronomical Society of India BIVS: Bulletin of the Indian Vacuum Society BNIS: Bulletin of National Institute of Sciences CJAA: Chinese Journal of Astronomy and Astrophysics CS: Current Science EPS: Earth Planets Space GRL : Geophysical Research Letters IAU: International Astronomical Union IBVS: Information Bulletin on Variable Stars IJHS: Indian Journal of History of Science IJPAP: Indian Journal of Pure and Applied Physics IJRSP: Indian Journal of Radio and Space Physics INSA: Indian National Science Academy JAA: Journal of Astrophysics and Astronomy JAMC: Journal of Applied Meterology and Climatology JATP: Journal of Atmospheric and Terrestrial Physics JBAA: Journal of British Astronomical Association JCAP: Journal of Cosmology and Astroparticle Physics JESS : Jr. of Earth System Science JGR : Journal of Geophysical Research JIGR: Journal of Indian -
(Formerly Streettracks Index Shares
SECURITIES AND EXCHANGE COMMISSION FORM NPORT-EX Filing Date: 2019-08-29 | Period of Report: 2019-06-30 SEC Accession No. 0001752724-19-105395 (HTML Version on secdatabase.com) FILER SPDR INDEX SHARES FUNDS (Formerly streetTRACKS Mailing Address Business Address ONE LINCOLN STREET ONE LINCOLN STREET Index Shares Funds) BOSTON MA 02111 BOSTON MA 02111 617-664-7037 CIK:1168164| IRS No.: 421537593 | State of Incorp.:MA | Fiscal Year End: 0930 Type: NPORT-EX | Act: 40 | File No.: 811-21145 | Film No.: 191063710 Copyright © 2021 www.secdatabase.com. All Rights Reserved. Please Consider the Environment Before Printing This Document Quarterly Report June 30, 2019 SPDR® Index Shares Funds The information contained in this report is intended for the general information of shareholders of the Trust. This report is not authorized for distribution to prospective investors unless preceded or accompanied by a current Trust prospectus which contains important information concerning the Trust. You may obtain a current prospectus and SAI from the Distributor by calling 1-866-787-2257 or visiting www.spdrs.com. Please read the prospectus carefully before you invest. Copyright © 2021 www.secdatabase.com. All Rights Reserved. Please Consider the Environment Before Printing This Document TABLE OF CONTENTS (Unaudited) Schedules of Investments (Unaudited) SPDR STOXX Europe 50 ETF (FEU) 1 SPDR EURO STOXX 50 ETF (FEZ) 3 SPDR EURO STOXX Small Cap ETF (SMEZ) 5 SPDR S&P Emerging Asia Pacific ETF (GMF) 8 SPDR S&P China ETF (GXC) 19 SPDR Portfolio Emerging Markets -
HAT-P-39B–HAT-P-41B: THREE HIGHLY INFLATED TRANSITING HOT JUPITERS∗
The Astronomical Journal, 144:139 (18pp), 2012 November doi:10.1088/0004-6256/144/5/139 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. HAT-P-39b–HAT-P-41b: THREE HIGHLY INFLATED TRANSITING HOT JUPITERS∗ J. D. Hartman1,G.A.´ Bakos1,15,B.Beky´ 2, G. Torres2, D. W. Latham2,Z.Csubry1, K. Penev1, A. Shporer3,4, B. J. Fulton3, L. A. Buchhave5,6,J.A.Johnson7, A. W. Howard8, G. W. Marcy8,D.A.Fischer9,G.Kovacs´ 10,11, R. W. Noyes2, G. A. Esquerdo2, M. Everett2, T. Szklenar´ 2,S.N.Quinn2,12, A. Bieryla2,R.P.Knox13,P.Hinz13, D. D. Sasselov2,G.Fur˝ esz´ 2, R. P. Stefanik2,J.Laz´ ar´ 14, I. Papp14,andP.Sari´ 14 1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA; [email protected] 2 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA 3 LCOGT, 6740 Cortona Drive, Santa Barbara, CA, USA 4 Department of Physics, Broida Hall, UC Santa Barbara, CA, USA 5 Niels Bohr Institute, University of Copenhagen, DK-2100, Denmark 6 Centre for Star and Planet Formation, Natural History Museum of Denmark, DK-1350 Copenhagen, Denmark 7 Department of Astrophysics, California Institute of Technology, MC 249-17, Pasadena, CA, USA 8 Department of Astronomy, University of California, Berkeley, CA, USA 9 Astronomy Department, Yale University, New Haven, CT, USA 10 Konkoly Observatory, Budapest, Hungary 11 Department of Physics and Astrophysics, University of North Dakota, Grand Forks, ND, USA 12 Department of Physics and Astronomy, Georgia State University, Atlanta, GA, USA 13 Steward Observatory, University of Arizona, Tucson, AZ, USA 14 Hungarian Astronomical Association, Budapest, Hungary Received 2012 July 13; accepted 2012 August 30; published 2012 October 9 ABSTRACT We report the discovery of three new transiting extrasolar planets orbiting moderately bright (V = 11.1, 11.7, and 12.4) F stars. -
Xtrackers (Ie) Plc
XTRACKERS (IE) PLC (An umbrella fund with variable share capital and segregated liability between funds) Condensed Interim Unaudited Report for the financial period ended 30 June 2020 XTRACKERS (IE) PLC CONTENTS Page General Information 1 Investment Manager's Report 14 Portfolio of Investments Xtrackers EUR Credit 12.5 Swap UCITS ETF 23 Xtrackers Portfolio Income UCITS ETF 25 Xtrackers MSCI Nordic UCITS ETF 26 Xtrackers Germany Mittelstand & MidCap UCITS ETF 30 Xtrackers MSCI North America High Dividend Yield UCITS ETF 34 Xtrackers MSCI AC World UCITS ETF 40 Xtrackers MSCI USA UCITS ETF 74 Xtrackers S&P 500 Equal Weight UCITS ETF 89 Xtrackers MSCI World UCITS ETF 101 Xtrackers FTSE Developed Europe ex UK Real Estate UCITS ETF 135 Xtrackers MSCI World Minimum Volatility UCITS ETF 137 Xtrackers MSCI World Momentum UCITS ETF 145 Xtrackers MSCI World Quality UCITS ETF 154 Xtrackers MSCI World Value UCITS ETF 162 Xtrackers MSCI GCC Select Swap UCITS ETF 172 Xtrackers FTSE All-World ex UK UCITS ETF 175 Xtrackers S&P 500 UCITS ETF 207 Xtrackers Russell 2000 UCITS ETF 220 Xtrackers Russell Midcap UCITS ETF 257 Xtrackers JPX-Nikkei 400 UCITS ETF 274 Xtrackers USD Corporate Bond UCITS ETF 285 Xtrackers MSCI World Financials UCITS ETF 321 Xtrackers MSCI World Health Care UCITS ETF 326 Xtrackers MSCI World Consumer Staples UCITS ETF 330 Xtrackers MSCI World Energy UCITS ETF 333 Xtrackers MSCI World Information Technology UCITS ETF 335 Xtrackers MSCI World Consumer Discretionary UCITS ETF 339 Xtrackers MSCI World Industrials UCITS ETF 344 Xtrackers -
Downloads/ Astero2007.Pdf) and by Aerts Et Al (2010)
This work is protected by copyright and other intellectual property rights and duplication or sale of all or part is not permitted, except that material may be duplicated by you for research, private study, criticism/review or educational purposes. Electronic or print copies are for your own personal, non- commercial use and shall not be passed to any other individual. No quotation may be published without proper acknowledgement. For any other use, or to quote extensively from the work, permission must be obtained from the copyright holder/s. i Fundamental Properties of Solar-Type Eclipsing Binary Stars, and Kinematic Biases of Exoplanet Host Stars Richard J. Hutcheon Submitted in accordance with the requirements for the degree of Doctor of Philosophy. Research Institute: School of Environmental and Physical Sciences and Applied Mathematics. University of Keele June 2015 ii iii Abstract This thesis is in three parts: 1) a kinematical study of exoplanet host stars, 2) a study of the detached eclipsing binary V1094 Tau and 3) and observations of other eclipsing binaries. Part I investigates kinematical biases between two methods of detecting exoplanets; the ground based transit and radial velocity methods. Distances of the host stars from each method lie in almost non-overlapping groups. Samples of host stars from each group are selected. They are compared by means of matching comparison samples of stars not known to have exoplanets. The detection methods are found to introduce a negligible bias into the metallicities of the host stars but the ground based transit method introduces a median age bias of about -2 Gyr. -
Algol Türü Örten Çift Yildizlarin Işikölçüm Ve Tayf Gözlemleri
XVI. Ulusal Astronomi Kongresi ve V. Ulusal Öğrenci Astronomi Kongresi-2008, Çanakkale ALGOL TÜRÜ ÖRTEN ÇİFT YILDIZLARIN IŞIKÖLÇÜM VE TAYF GÖZLEMLERİ C. İBANOĞLU, S. EVREN, G. TAŞ, Ö. ÇAKIRLI, Z. BOZKURT, M. AFŞAR, E.SİPAHİ, H. A. DAL, O. ÖZDARCAN, D. Z. ÇAMURDAN, M. ÇAMURDAN Ege Üniversitesi, Astronomi ve Uzay Bilimleri Bölümü, 35100 Bornova İzmir Özet: Hipparcos uydusu ile keşfedilen 13 örten çift yıldızın ışıkölçüm ve tayf gözlemleri yapılmıştır. Örten çift olduğu daha önceden bilinen zonklayan yıldız bileşenli HD 172189 ve kuvvetli salma çizgileri gösteren disk yapılı AW Peg yıldızı da listeye alınmıştır. AW Peg’in ışıkölçüm verileri daha önce elde edildiğinden yalnızca tayf gözlemleri yapılmıştır. Seçilen yıldızlardan 14’ünün ışıkölçüm ve tayf gözlemleri iki yıl gibi kısa bir sürede bitirilmiştir. CP Psc sönük olduğundan tayfı alınamamıştır. Işıkölçüm gözlemleri Ege Üniversitesi Gözlemevi’nin 48, 40 ve 35 cm’lik teleskopları ile yapılmıştır. Üç kanallı hızlı ışıkölçeri, CCD kameralar ve UBV süzgeçleri kullanılmıştır. Tayf gözlemler Catania Astrofizik Gözlemevi’nin 91 cm, TÜBİTAK TUG’un 150 ve David Dunlap Gözlemevi’nin 188 cm’lik teleskopları ile yapılmıştır. UBV ışıkölçümleri standart düzeneğe dönüştürülmüş, renk- renk diyagramları ve yıldızlararası ortamın etkisinden bağımsız geniş-band Q-parametresi kullanılarak E(B-V) ve baş yıldızın etkin sıcaklığı Te belirlenmiştir. Bu sıcaklık yıldızın tayfı ile karşılaştırılmıştır. Işık eğrilerinin analizinde temel öğe olan baş yıldızın etkin sıcaklığı duyarlı olarak bulunduktan sonra ışık eğrileri ve dikine hız verileri ortak olarak analiz edilmiş, bileşen yıldızların temel öğeleri kütle, yarıçap, sıcaklık ve ışıtmaları bulumuştur. Yıldızların bulunan salt öğeleri kuramsal modellerle karşılaştırılmış, evrim durumları ortaya çıkartılmıştır. Bileşenlerin ışınımsal özellikleri ve yıldızlararası kızıllaşma değerleri kullanılarak uzaklıklar hesaplanmıştır. -
On Mautner-Type Probability of Capture of Intergalactic Meteor Particles by Habitable Exoplanets
Article On Mautner-Type Probability of Capture of Intergalactic Meteor Particles by Habitable Exoplanets Andjelka B. Kovaˇcevi´c Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, 11000 Belgrade, Serbia; [email protected] Received: 28 June 2019; Accepted: 10 July 2019; Published: 9 August 2019 First Version Published: 15 July 2019 (doi:10.3390/sci1020041) Second Version Published: 9 August 2019 (doi:10.3390/sci1020047) Abstract: Both macro and microprojectiles (e.g., interplanetary, interstellar and even intergalactic material) are seen as important vehicles for the exchange of potential (bio)material within our solar system as well as between stellar systems in our Galaxy. Accordingly, this requires estimates of the impact probabilities for different source populations of projectiles, including for intergalactic meteor particles which have received relatively little attention since considered as rare events (discrete occurrences that are statistically improbable due to their very infrequent appearance). We employ the simple but yet comprehensive model of intergalactic microprojectile capture by the gravity of exoplanets which enables us to estimate the map of collisional probabilities for an available sample of exoplanets in habitable zones around host stars. The model includes a dynamical description of the capture adopted from Mautner model of interstellar exchange of microparticles and changed for our purposes. We use statistical and information metrics to calculate probability map of intergalactic meteorite particle capture. Moreover, by calculating the entropy index map we measure the concentration of these rare events. We further adopted a model from immigration theory, to show that the transient distribution of birth/death/immigration of material for the simplest case has a high value. -
October 29, 2018 Alpha Daily Summary
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Radial Velocity Variations in Red Giant Stars: Pulsations, Spots and Planets
RADIAL VELOCITY VARIATIONS IN RED GIANT STARS: PULSATIONS, SPOTS AND PLANETS RADIAL VELOCITY VARIATIONS IN RED GIANT STARS: PULSATIONS, SPOTS AND PLANETS Proefschrift ter verkrijging van de graad van Doctor aan de Universiteit Leiden, op gezag van de Rector Magnificus prof. mr. P. F. van der Heijden, volgens besluit van het College voor Promoties te verdedigen op 18 september 2007 klokke 13:45 uur door Saskia Hekker geboren te Heeze in 1978 Promotiecommissie Promotor: Prof. dr. A. Quirrenbach Sterrewacht Leiden Landessternwarte Heidelberg Promotor: Prof. dr. C. Aerts Katholieke Universiteit Leuven Radboud Universiteit Nijmegen Co-promotor: Dr. I. A. G. Snellen Sterrewacht Leiden Overige leden: Prof. dr. E. F. van Dishoeck Sterrewacht Leiden Prof. dr. K. H. Kuijken Sterrewacht Leiden Prof. dr. P. T. de Zeeuw Sterrewacht Leiden Dr. M. Hogerheijde Sterrewacht Leiden Dr. J. Lub Sterrewacht Leiden Dit proefschrift is tot stand gekomen met steun van No pain, no gain Contents 1 Introduction 1 1.1 Redgiantstars................................... 2 1.2 Observations ................................... 4 1.2.1 Iodinecell................................. 4 1.2.2 SimultaneousThAr............................ 4 1.3 Oscillations .................................... 5 1.3.1 Excitationmechanism .......................... 9 1.3.2 Asymptoticrelation. 10 1.3.3 Scalingrelations ............................. 10 1.4 Starspots...................................... 11 1.5 Sub-stellarcompanions . ... 12 1.6 Why can oscillations, spots and companions be observed as