Evolutionary Status and Internal Structure of Μ
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FY08 Technical Papers by GSMTPO Staff
AURA/NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation July 23, 2008 Revised as Complete and Submitted December 23, 2008 NGC 660, ~13 Mpc from the Earth, is a peculiar, polar ring galaxy that resulted from two galaxies colliding. It consists of a nearly edge-on disk and a strongly warped outer disk. Image Credit: T.A. Rector/University of Alaska, Anchorage NATIONAL OPTICAL ASTRONOMY OBSERVATORY NOAO ANNUAL REPORT FY 2008 Submitted to the National Science Foundation December 23, 2008 TABLE OF CONTENTS EXECUTIVE SUMMARY ............................................................................................................................. 1 1 SCIENTIFIC ACTIVITIES AND FINDINGS ..................................................................................... 2 1.1 Cerro Tololo Inter-American Observatory...................................................................................... 2 The Once and Future Supernova η Carinae...................................................................................................... 2 A Stellar Merger and a Missing White Dwarf.................................................................................................. 3 Imaging the COSMOS...................................................................................................................................... 3 The Hubble Constant from a Gravitational Lens.............................................................................................. 4 A New Dwarf Nova in the Period Gap............................................................................................................ -
Disertaciones Astronómicas Boletín Número 55 De Efemérides Astronómicas 28 De Octubre De 2020
Disertaciones astronómicas Boletín Número 55 de efemérides astronómicas 28 de octubre de 2020 Realiza Luis Fernando Ocampo O. ([email protected]). Noticias de la semana. Osiris–Rex y el astroide Bennu. Imagen 1: Estas imágenes muestran los cuatro sitios de recolección de muestras candidatos en el asteroide Bennu: Nightingale, Kingfisher, Osprey y Sandpiper. Imagen: NASA / / Goddard / Universidad de Arizona. La misión OSIRIS-REx de la NASA está realizó un almacenamiento temprano el martes 27 de octubre de la gran muestra que recolectó la semana pasada de la superficie del asteroide Bennu para proteger y devolver la mayor cantidad posible de muestra. Su capacidad es hasta 2 kg. El 22 de octubre, el equipo de la misión OSIRIS-REx recibió imágenes que mostraban que la cabeza recolectora de la nave espacial rebosaba de material recolectado de la superficie de Bennu, muy por encima del requisito de la misión de dos onzas (60 gramos), y que algunas de estas partículas parecían estar escapar lentamente del cabezal de recolección, llamado Mecanismo de adquisición de muestras Touch-And-Go (TAGSAM). Una solapa de mylar en el TAGSAM permite que el material entre fácilmente en el cabezal del colector y debe sellar para cerrar una vez que las partículas pasan. Sin embargo, las rocas más grandes que no pasaron completamente a través de la solapa hacia el TAGSAM parecen haber abierto esta solapa, lo que permitió que se filtraran fragmentos de la muestra. Debido a que el primer evento de recolección de muestras fue tan exitoso, la Dirección de Misiones Científicas de la NASA le ha dado al equipo de la misión el visto bueno para acelerar el almacenamiento de muestras, originalmente programado para el 2 de noviembre, en la Cápsula de Retorno de Muestras (SRC) de la nave espacial para minimizar una mayor pérdida de muestras. -
Visual Double Star Measurements with an Alt-Azimuth Telescope
Vol. 4 No. 2 Spring 2008 Journal of Double Star Observations Page 59 Visual Double Star Measurements with an Alt-Azimuth Telescope Thomas G. Frey California Polytechnic State University San Luis Obispo, CA 93407 Abstract: An alt-az mounted Newtonian telescope was used to determine the separation and position angle of seven known and five neglected double stars. The problem of field rotation was solved by modifying the usual observing technique. Separation and position angle determinations are described, and the standard deviations and mean errors for these measurements are presented. The direction of future studies is outlined. techniques were accurate and precise, additional Introduction measurements on neglected double stars listed in the Professional astronomers have carried out visual Washington Double Star Catalogue were made. double star measurements for over 200 years. These scientists measured the separation between double Double Star Observation: Equatorial vs. stars in arc seconds, and the position angle in degrees Alt-Az Mounts that defined the orientation of pairs with respect to Most observers involved in double star measure- celestial north. Over time, the orbital motion of each ments, including Argyle (p.x) and Teague (p.112), star can create a change in the observed separation recommend the use of equatorial mounted telescopes. and position angle if the pair proves to be binary in Such telescopes have drive motors that are oriented so nature. A binary star revolves around a common the right ascension axis rotates around the north center of mass. celestial pole, canceling out the Earth’s rotation and Today’s amateur astronomers continue to evaluate the image in the eyepiece remains stationary. -
M17 CEN1.Pdf
The Origin of Hard X-rays in M 17's Remarkable O4+O4 Binary M 17, the closest Giant H ii Region (d ≈ 2 kpc), is a superior laboratory for the study of young massive stars. Producing the second-brightest H ii region in the sky (after the Orion Nebula), the OB cluster NGC 6618 has nearly 10,000 members extending up to masses M ≈ 60M (spectral type O4 V) in the central binary. It is a scaled-up, edge-on version of the Orion Molecular Cloud: a blister nebula on the edge of one of the Galaxy's most massive giant molecular clouds. With an age of ∼ 0:5 Myr (Hanson et al. 1997, ApJ 489, 698) and no evolved stars, M 17 is one of the few massive star-forming regions whose massive stars are luminous enough to produce a prominent X-ray outflow (Townsley et al. 2003, ApJ 593, 874) and yet is unlikely to have hosted any supernovae. Co-I's Townsley and Garmire have amassed 320 ks of Chandra ACIS-I time on NGC 6618, through a combination of GO and ACIS GTO programs, to study M 17 and its enormous X-ray champagne flow. The ACIS data reveal that the massive O4 stars in NGC 6618 are a pair of remarkable hard, variable X-ray sources separated by 1:800 (Broos et al. 2007, ApJS 169, 353; Fig. 1A). The stars are seen through AV ≈ 10 mag and no spatially resolved near-infrared photometry or spectroscopy of the visual pair is published. The pair is known historically as Kleinmann's Anonymous Star (Kleinmann 1973, ApL, 14, 39); Chini et al. -
List of Easy Double Stars for Winter and Spring = Easy = Not Too Difficult = Difficult but Possible
List of Easy Double Stars for Winter and Spring = easy = not too difficult = difficult but possible 1. Sigma Cassiopeiae (STF 3049). 23 hr 59.0 min +55 deg 45 min This system is tight but very beautiful. Use a high magnification (150x or more). Primary: 5.2, yellow or white Seconary: 7.2 (3.0″), blue 2. Eta Cassiopeiae (Achird, STF 60). 00 hr 49.1 min +57 deg 49 min This is a multiple system with many stars, but I will restrict myself to the brightest one here. Primary: 3.5, yellow. Secondary: 7.4 (13.2″), purple or brown 3. 65 Piscium (STF 61). 00 hr 49.9 min +27 deg 43 min Primary: 6.3, yellow Secondary: 6.3 (4.1″), yellow 4. Psi-1 Piscium (STF 88). 01 hr 05.7 min +21 deg 28 min This double forms a T-shaped asterism with Psi-2, Psi-3 and Chi Piscium. Psi-1 is the uppermost of the four. Primary: 5.3, yellow or white Secondary: 5.5 (29.7), yellow or white 5. Zeta Piscium (STF 100). 01 hr 13.7 min +07 deg 35 min Primary: 5.2, white or yellow Secondary: 6.3, white or lilac (or blue) 6. Gamma Arietis (Mesarthim, STF 180). 01 hr 53.5 min +19 deg 18 min “The Ram’s Eyes” Primary: 4.5, white Secondary: 4.6 (7.5″), white 7. Lambda Arietis (H 5 12). 01 hr 57.9 min +23 deg 36 min Primary: 4.8, white or yellow Secondary: 6.7 (37.1″), silver-white or blue 8. -
Anexo Ii: Catálogos De Espectros Estelares
ANEXO II: CATÁLOGOS DE ESPECTROS ESTELARES Base de datos de espectros estelares del enfoque híbrido I 1 (continuación) 2 (continuación) Catálogo G. H. Jacoby & D. A. Hunter & C. A. Christian 3 4 (continuación) 5 (continuación) Catálogo A.J. Pickles 1988 6 7 (continuación) Catálogo Silva 1992 8 Num Name Sp Type Vr Teff log g 1 HD000245 G2V -93.73 5433. 3.50 2 HD000358 B8IVmnp.. -33.90 14007. 3.77 3 HD000400 F8IV -15.13 6146. 4.09 4 HD000693 F5V 14.79 6156. 4.13 5 HD001227 G8II-III -0.03 5063. 2.65 6 HD001835 G3V -2.46 5777. 4.45 7 HD002665 G5IIIwe -382.34 5004. 2.27 8 HD002665 G5IIIwe -382.57 5004. 2.27 9 HD002796 Fw -61.36 4920. 1.39 10 HD003268 F7V -23.40 6130. 4.01 11 HD003546 G5III... -84.14 4769. 2.22 12 HD003567 F5V -47.62 5991. 3.96 13 HD003628 G2V -27.09 5701. 4.06 14 HD003712 K0II-IIIva -4.49 4608. 2.20 15 HD003712 K0II-IIIva -4.45 4608. 2.20 16 HD004306 G0 -61.71 4933. 1.96 17 HD004306 G0 -61.71 4933. 1.96 18 HD004307 G2V -10.36 5806. 4.04 19 HD004395 G5 -0.75 5471. 3.32 20 HD004614 G0V... 8.29 5890. 4.40 21 HD005234 K2III -23.56 4385. 1.58 22 HD005395 G8III-IV -48.08 4708. 2.42 23 HD005448 A5V 9.60 8029. 3.90 24 HD005516 G8III-IV -25.49 4940. 2.70 25 HD005600 F8 3.70 6631. 3.98 26 HD005916 G8III-IV -68.17 4874. -
Arxiv:2006.10868V2 [Astro-Ph.SR] 9 Apr 2021 Spain and Institut D’Estudis Espacials De Catalunya (IEEC), C/Gran Capit`A2-4, E-08034 2 Serenelli, Weiss, Aerts Et Al
Noname manuscript No. (will be inserted by the editor) Weighing stars from birth to death: mass determination methods across the HRD Aldo Serenelli · Achim Weiss · Conny Aerts · George C. Angelou · David Baroch · Nate Bastian · Paul G. Beck · Maria Bergemann · Joachim M. Bestenlehner · Ian Czekala · Nancy Elias-Rosa · Ana Escorza · Vincent Van Eylen · Diane K. Feuillet · Davide Gandolfi · Mark Gieles · L´eoGirardi · Yveline Lebreton · Nicolas Lodieu · Marie Martig · Marcelo M. Miller Bertolami · Joey S.G. Mombarg · Juan Carlos Morales · Andr´esMoya · Benard Nsamba · KreˇsimirPavlovski · May G. Pedersen · Ignasi Ribas · Fabian R.N. Schneider · Victor Silva Aguirre · Keivan G. Stassun · Eline Tolstoy · Pier-Emmanuel Tremblay · Konstanze Zwintz Received: date / Accepted: date A. Serenelli Institute of Space Sciences (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E- 08193, Spain and Institut d'Estudis Espacials de Catalunya (IEEC), Carrer Gran Capita 2, Barcelona, E-08034, Spain E-mail: [email protected] A. Weiss Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany C. Aerts Institute of Astronomy, Department of Physics & Astronomy, KU Leuven, Celestijnenlaan 200 D, 3001 Leuven, Belgium and Department of Astrophysics, IMAPP, Radboud University Nijmegen, Heyendaalseweg 135, 6525 AJ Nijmegen, the Netherlands G.C. Angelou Max Planck Institute for Astrophysics, Karl Schwarzschild Str. 1, Garching bei M¨unchen, D-85741, Germany D. Baroch J. C. Morales I. Ribas Institute of· Space Sciences· (ICE, CSIC), Carrer de Can Magrans S/N, Bellaterra, E-08193, arXiv:2006.10868v2 [astro-ph.SR] 9 Apr 2021 Spain and Institut d'Estudis Espacials de Catalunya (IEEC), C/Gran Capit`a2-4, E-08034 2 Serenelli, Weiss, Aerts et al. -
Sr.No LLPIN/Fllpinname of the Entity Date of Registration 1 AAB
Sr.No LLPIN/FLLPINName of the entity Date of Registration 1 AAB-9711 VEGA LIVINGS LLP 1/1/2014 2 AAB-9712 DALE DAIRY PRODUCTS LLP 1/1/2014 3 AAB-9713 VSD HOLDINGS & ADVISORY LLP 1/1/2014 4 AAB-9714 SHARPERSUN INDUSTRIES LLP 1/1/2014 5 AAB-9715 XL PAPER CORE LLP 1/1/2014 6 AAB-9716 ZEE RPM PROPERTIES LLP 1/1/2014 7 AAB-9717 MAHAWAJRESHWARI AGRO HI TECH LLP 1/1/2014 8 AAB-9718 TRAILOKYA AGRI TECH LLP 1/1/2014 9 AAB-9719 VIDHYASHRI AGRI HI TECH LLP 1/1/2014 10 AAB-9720 CRYSTAL CLEAR VISION CENTRE LLP 1/1/2014 11 AAB-9721 SPECTASYS INFRA SERVICES LLP 1/1/2014 12 AAB-9722 INDE GLOBAL CONSULTING LLP 1/1/2014 13 AAB-9723 BLUE HEAVEN DEVELOPERS LLP 1/1/2014 14 AAB-9724 VAICHAL DEVELOPERS LLP 1/1/2014 15 AAB-9725 RURBAN INFRASTRUCTURE AND DEVELOPMENT CORPORATION LLP 1/1/2014 16 AAB-9726 EDGE REALTORS LLP 1/1/2014 17 AAB-9727 TRINETRA BUSINESS ADVISORS INDIA LLP 1/1/2014 18 AAB-9728 REBEL FASHION STUDIO LLP 1/1/2014 19 AAB-9729 ADPHLOX MEDIA LLP 1/1/2014 20 AAB-9730 JALAN STUDIOS LLP 1/1/2014 21 AAB-9731 NILMADHAV CONSTRUCTIONS LLP 1/1/2014 22 AAB-9732 KAPASHERA DEVELOPERS LLP 1/1/2014 23 AAB-9733 JUST TECHNICAL SOLUTIONS LLP 1/1/2014 24 AAB-9734 SHUBHAM PRINTS LLP 1/1/2014 25 AAB-9735 NBN FOODS LLP 1/1/2014 26 AAB-9736 ZYPSON ENGINEERING SERVICES LLP 1/1/2014 27 AAB-9737 BUILDCON PROMOTERS LLP 1/1/2014 28 AAB-9738 KNOSPE & CO. -
Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 Through 2009
Vol. 6 No. 3 July 1, 2010 Journal of Double Star Observations Page 180 Double and Multiple Star Measurements in the Northern Sky with a 10” Newtonian and a Fast CCD Camera in 2006 through 2009 Rainer Anton Altenholz/Kiel, Germany e-mail: rainer.anton”at”ki.comcity.de Abstract: Using a 10” Newtonian and a fast CCD camera, recordings of double and multiple stars were made at high frame rates with a notebook computer. From superpositions of “lucky images”, measurements of 139 systems were obtained and compared with literature data. B/w and color images of some noteworthy systems are also presented. mented double stars, as will be described in the next Introduction section. Generally, I used a red filter to cope with By using the technique of “lucky imaging”, seeing chromatic aberration of the Barlow lens, as well as to effects can strongly be reduced, and not only the reso- reduce the atmospheric spectrum. For systems with lution of a given telescope can be pushed to its limits, pronounced color contrast, I also made recordings but also the accuracy of position measurements can be with near-IR, green and blue filters in order to pro- better than this by about one order of magnitude. This duce composite images. This setup was the same as I has already been demonstrated in earlier papers in used with telescopes under the southern sky, and as I this journal [1-3]. Standard deviations of separation have described previously [1-3]. Exposure times varied measurements of less than +/- 0.05 msec were rou- between 0.5 msec and 100 msec, depending on the tinely obtained with telescopes of 40 or 50 cm aper- star brightness, and on the seeing. -
Supernova Star Maps
Supernova Star Maps Which Stars in the Night Sky Will Go Su pernova? About the Activity Allow visitors to experience finding stars in the night sky that will eventually go supernova. Topics Covered Observation of stars that will one day go supernova Materials Needed • Copies of this month's Star Map for your visitors- print the Supernova Information Sheet on the back. • (Optional) Telescopes A S A Participants N t i d Activities are appropriate for families Cre with children over the age of 9, the general public, and school groups ages 9 and up. Any number of visitors may participate. Location and Timing This activity is perfect for a star party outdoors and can take a few minutes, up to 20 minutes, depending on the Included in This Packet Page length of the discussion about the Detailed Activity Description 2 questions on the Supernova Helpful Hints 5 Information Sheet. Discussion can start Supernova Information Sheet 6 while it is still light. Star Maps handouts 7 Background Information There is an Excel spreadsheet on the Supernova Star Maps Resource Page that lists all these stars with all their particulars. Search for Supernova Star Maps here: http://nightsky.jpl.nasa.gov/download-search.cfm © 2008 Astronomical Society of the Pacific www.astrosociety.org Copies for educational purposes are permitted. Additional astronomy activities can be found here: http://nightsky.jpl.nasa.gov Star Maps: Stars likely to go Supernova! Leader’s Role Participants’ Role (Anticipated) Materials: Star Map with Supernova Information sheet on back Objective: Allow visitors to experience finding stars in the night sky that will eventually go supernova. -
Proquest Dissertations
Low-mass star formation and the initial mass function in young clusters Item Type text; Dissertation-Reproduction (electronic) Authors Luhman, Kevin Lee, 1971- Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 01/10/2021 22:31:04 Link to Item http://hdl.handle.net/10150/288884 INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand comer and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. -
High Energy Astrophysics Program (Heap)
HIGH ENERGY ASTROPHYSICS PROGRAM (HEAP) NASA CONTRACT NAS 5 - 32490 Final Technical Report April 1, 1998 through September 30, 1998 UNIVERSITIES SPACE RESEARCH ASSOCIATION (USRA) David V. Holdridge Project Manager TABLE OF CONTENTS Task 93-01-00 - HEASARC Corcoran, Michael ......................................................................... 03 Drake, Stephen ............................................................................... 05 McGlynn, Thomas A ..................................................................... 08 Task 93-02-00 - ROSAT-GOF Snowden, Stephen ........................................................................... 9 Task 93-03-00 - ASCA-GOF Gotthelf, Eric ................................................................................. 11 Mukai, Koji ................................................................................... 13 Task 93-04-00 - XTE-GOF Boyd, Padi ..................................................................................... 16 Cannizzo, John .............................................................................. 18 Lochner, James .............................................................................. 20 Smale, Alan ................................................................................... 21 TASK 93-09-00 - RMT/BATSE Barthelmy, Scott ............................................................................ 24 TASK 93-10-00 - TGRS/WIND Palmer, David ................................................................................ 26 Task 93-11-00-