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A Dozen Colliding Wind X-Ray Binaries in the Star Cluster R 136 in the 30 Doradus Region
A dozen colliding wind X-ray binaries in the star cluster R 136 in the 30 Doradus region Simon F. Portegies Zwart?,DavidPooley,Walter,H.G.Lewin Massachusetts Institute of Technology, Cambridge, MA 02139, USA ? Hubble Fellow Subject headings: stars: early-type — tars: Wolf-Rayet — galaxies:) Magellanic Clouds — X-rays: stars — X-rays: binaries — globular clusters: individual (R136) –2– ABSTRACT We analyzed archival Chandra X-ray observations of the central portion of the 30 Doradus region in the Large Magellanic Cloud. The image contains 20 32 35 1 X-ray point sources with luminosities between 5 10 and 2 10 erg s− (0.2 × × — 3.5 keV). A dozen sources have bright WN Wolf-Rayet or spectral type O stars as optical counterparts. Nine of these are within 3:4 pc of R 136, the ∼ central star cluster of NGC 2070. We derive an empirical relation between the X-ray luminosity and the parameters for the stellar wind of the optical counterpart. The relation gives good agreement for known colliding wind binaries in the Milky Way Galaxy and for the identified X-ray sources in NGC 2070. We conclude that probably all identified X-ray sources in NGC 2070 are colliding wind binaries and that they are not associated with compact objects. This conclusion contradicts Wang (1995) who argued, using ROSAT data, that two earlier discovered X-ray sources are accreting black-hole binaries. Five early type stars in R 136 are not bright in X-rays, possibly indicating that they are either: single stars or have a low mass companion or a wide orbit. -
Annual Report 2017
Koninklijke Sterrenwacht van België Observatoire royal de Belgique Royal Observatory of Belgium Jaarverslag 2017 Rapport Annuel 2017 Annual Report 2017 Cover illustration: Above: One billion star map of our galaxy created with the optical telescope of the satellite Gaia (Credit: ESA/Gaia/DPAC). Below: Three armillary spheres designed by Jérôme de Lalande in 1775. Left: the spherical sphere; in the centre: the geocentric model of our solar system (with the Earth in the centre); right: the heliocentric model of our solar system (with the Sun in the centre). Royal Observatory of Belgium - Annual Report 2017 2 De activiteiten beschreven in dit verslag werden ondersteund door Les activités décrites dans ce rapport ont été soutenues par The activities described in this report were supported by De POD Wetenschapsbeleid De Nationale Loterij Le SPP Politique Scientifique La Loterie Nationale The Belgian Science Policy The National Lottery Het Europees Ruimtevaartagentschap De Europese Gemeenschap L’Agence Spatiale Européenne La Communauté Européenne The European Space Agency The European Community Het Fonds voor Wetenschappelijk Onderzoek – Le Fonds de la Recherche Scientifique Vlaanderen Royal Observatory of Belgium - Annual Report 2017 3 Table of contents Preface .................................................................................................................................................... 6 Reference Systems and Planetology ...................................................................................................... -
197 6Apjs. . .30. .451H the Astrophysical Journal Supplement Series, 30:451-490, 1976 April © 1976. the American Astronomical S
.451H The Astrophysical Journal Supplement Series, 30:451-490, 1976 April .30. © 1976. The American Astronomical Society. All rights reserved. Printed in U.S.A. 6ApJS. 197 EVOLVED STARS IN OPEN CLUSTERS Gretchen L. H. Harris* David Dunlap Observatory, Richmond Hill, Ontario Received 1974 September 16; revised 1975 June 18 ABSTRACT Radial-velocity observations and MK classifications have been used to study evolved stars in 25 open clusters. Published data on stars in 72 additional clusters are rediscussed and com- bined with the observations friade in this investigation to yield positions in the Hertzsprung- Russell diagram for 559 evolved stars in 97 clusters. Ages for the parent clusters were estimated from the main-sequence turnoff points, earliest spectral types, and bluest stars in the clusters themselves. The evolved stars were sorted into six age groups ranging from 4 x 106 yr to 4 x 108 yr, and the composite H-R diagram for each age group was then used to study the evolutionary tracks for stars of various masses. The observational results were found to be in reasonably good agreement with recent theoretical computations. The composite color-magnitude diagrams were found to be strikingly different from those of the rich open clusters in the Magellanic Clouds. At a given age the red giants in the Small Magellanic Cloud and the Large Magellanic Cloud clusters are brighter and bluer than their galactic counterparts. It is suggested that these effects may be accounted for by differences in metal abundance. Subject headings: clusters: open — galaxies: Magellanic Clouds — radial velocities — stars : evolution — stars : late-type — stars : spectral classification 1. -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
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. -
THE MAGELLANIC CLOUDS NEWSLETTER an Electronic Publication Dedicated to the Magellanic Clouds, and Astrophysical Phenomena Therein
THE MAGELLANIC CLOUDS NEWSLETTER An electronic publication dedicated to the Magellanic Clouds, and astrophysical phenomena therein No. 153 — 5 June 2018 http://www.astro.keele.ac.uk/MCnews Editor: Jacco van Loon Editorial Dear Colleagues, It is my pleasure to present you the 153rd issue of the Magellanic Clouds Newsletter. It features a large number of papers related to star clusters, in one way or another. But even if you are not fond of star clusters you are likely to find something of interest among the posts, which include further results from Gaia and work on massive stars but also the interstellar medium. The next issue is planned to be distributed on the 6th of August. Editorially Yours, Jacco van Loon 1 Refereed Journal Papers The VLT-FLAMES Tarantula Survey: XXVIII. Nitrogen abundances for apparently single dwarf and giant B-type stars with small projected rotational velocities P.L. Dufton1, A. Thompson1, P. A. Crowther2, C. J. Evans3, F.R.N. Schneider4, A. de Koter5, S.E. de Mink5, R. Garland1,12, N. Langer6, D.J. Lennon7, C.M. McEvoy1,13, O.H. Ram´ırez-Agudelo3, H. Sana8, S. Sim´on D´ıaz9,10, W.D. Taylor3 and J.S. Vink11 1Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK 2Department of Physics and Astronomy, Hounsfield Road, University of Sheffield, Sheffield, S3 7RH, UK 3UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK 4Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK 5Anton Pannekoek Institute -
The VLT-FLAMES Tarantula Survey? XXIX
A&A 618, A73 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833433 & c ESO 2018 Astrophysics The VLT-FLAMES Tarantula Survey? XXIX. Massive star formation in the local 30 Doradus starburst F. R. N. Schneider1, O. H. Ramírez-Agudelo2, F. Tramper3, J. M. Bestenlehner4,5, N. Castro6, H. Sana7, C. J. Evans2, C. Sabín-Sanjulián8, S. Simón-Díaz9,10, N. Langer11, L. Fossati12, G. Gräfener11, P. A. Crowther5, S. E. de Mink13, A. de Koter13,7, M. Gieles14, A. Herrero9,10, R. G. Izzard14,15, V. Kalari16, R. S. Klessen17, D. J. Lennon3, L. Mahy7, J. Maíz Apellániz18, N. Markova19, J. Th. van Loon20, J. S. Vink21, and N. R. Walborn22,?? 1 Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK e-mail: [email protected] 2 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK 3 European Space Astronomy Centre, Mission Operations Division, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain 4 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 5 Department of Physics and Astronomy, Hicks Building, Hounsfield Road, University of Sheffield, Sheffield S3 7RH, UK 6 Department of Astronomy, University of Michigan, 1085 S. University Avenue, Ann Arbor, MI 48109-1107, USA 7 Institute of Astrophysics, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium 8 Departamento de Física y Astronomía, Universidad de La Serena, Avda. Juan Cisternas 1200, Norte, La Serena, Chile 9 Instituto de Astrofísica de Canarias, 38205 La Laguna, -
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 -
Arxiv:1803.10763V1 [Astro-Ph.GA] 28 Mar 2018
Draft version October 10, 2018 Typeset using LATEX default style in AASTeX61 TRACERS OF STELLAR MASS-LOSS - II. MID-IR COLORS AND SURFACE BRIGHTNESS FLUCTUATIONS Rosa A. Gonzalez-L´ opezlira´ 1 1Instituto de Radioastronomia y Astrofisica, UNAM, Campus Morelia, Michoacan, Mexico, C.P. 58089 (Received 2017 October 20; Revised 2018 February 20; Accepted 2018 February 21) Submitted to ApJ ABSTRACT I present integrated colors and surface brightness fluctuation magnitudes in the mid-IR, derived from stellar popula- tion synthesis models that include the effects of the dusty envelopes around thermally pulsing asymptotic giant branch (TP-AGB) stars. The models are based on the Bruzual & Charlot CB∗ isochrones; they are single-burst, range in age from a few Myr to 14 Gyr, and comprise metallicities between Z = 0.0001 and Z = 0.04. I compare these models to mid-IR data of AGB stars and star clusters in the Magellanic Clouds, and study the effects of varying self-consistently the mass-loss rate, the stellar parameters, and the output spectra of the stars plus their dusty envelopes. I find that models with a higher than fiducial mass-loss rate are needed to fit the mid-IR colors of \extreme" single AGB stars in the Large Magellanic Cloud. Surface brightness fluctuation magnitudes are quite sensitive to metallicity for 4.5 µm and longer wavelengths at all stellar population ages, and powerful diagnostics of mass-loss rate in the TP-AGB for intermediater-age populations, between 100 Myr and 2-3 Gyr. Keywords: stars: AGB and post{AGB | stars: mass-loss | Magellanic Clouds | infrared: stars | stars: evolution | galaxies: stellar content arXiv:1803.10763v1 [astro-ph.GA] 28 Mar 2018 Corresponding author: Rosa A. -
Cycle 8 Approved Programs
Cycle 8 Approved Programs PI INSTITUTION COUNTRY PANEL TITLE Ajhar National Optical Astronomy Observatories United States CLUS Reconciling the SBF and SNIa Distance Scales Allen Space Telescope Science Institute United States ISM How Opaque Are Spiral Galaxies? Antonucci University of California Santa Barbara United States AGNH Optical Nuclear Hotspot in NGC 1068 Arav Institute of Geophysics and Planetary Physics United States AGNP Deep STIS Observations of BALQSO PG 0946+301 Armandroff Kitt Peak National Observatory United States FSP The Horizontal Branches of the M31 Dwarf Spheroidal Companions And V & VI Axon University of Manchester United Kingdom GSD The black hole versus bulge mass relationship in spiral galaxies Ayres University of Colorado United States CS Origins Structure and Evolution of Magnetic Activity in the Cool Half of the H-R Diagram: A STIS Survey Bagenal University of Colorado United States SS HST-Galileo Io Campaign Bailyn Yale University United States SPC High Precision Photometry of the Core of M13 Baker University of California Berkeley United States AGNP Absorption and obscuration in radio-loud quasars Baldwin Cerro Tololo Interamerican Observatory Chile AGNP High Abundances in Luminous Quasars: A Test Case Bally CASA University of Colorado Boulder United States SE Herbig-Haro Jets Irradiated by Massive OB Stars Bally University of Colorado Boulder United States YS The Structure and Kinematics of Irradiated Disks and Associated High Velocity Features in Orion Barstow University of Leicester United Kingdom HS THE -
Appendix II. Publications
Publications Gemini Staff Publications Papers in Peer-Reviewed Journals: Bergmann, M.[2]. Gemini 3D spectroscopy of BAL+IR+FeII QSOs - II. IRAS 04505-2958, an explosive QSO with hypershells and a new scenario for galaxy formation and galaxy end phase. Monthly Notices of the Royal Astronomical Society, 398:658-700. 9/2009. McDermid, Richard M.[8]. Stellar velocity profiles and line strengths out to four effective radii in the early-type galaxies NGC3379 and 821. Monthly Notices of the Royal Astronomical Society, 398:561-574. 9/2009. Levenson, N. A.[1]; Radomski, J. T.[2]; Mason, R. E.[4]. Isotropic Mid-Infrared Emission from the Central 100 pc of Active Galaxies. The Astrophysical Journal, 703:390-398. 9/2009. Radomski, J. T.[6]; Fisher, R. S.[8]. The Infrared Nuclear Emission of Seyfert Galaxies on Parsec Scales: Testing the Clumpy Torus Models. The Astrophysical Journal, 702:1127-1149. 9/2009. Leggett, S. K.[2]; Geballe, T. R.[6]. The 0.8-14.5 μm Spectra of Mid-L to Mid-T Dwarfs: Diagnostics of Effective Temperature, Grain Sedimentation, Gas Transport, and Surface Gravity. The Astrophysical Journal, 702:154-170. 9/2009. Rantakyro, F.[11]. Cyclic variability of the circumstellar disk of the Be star ζ Tauri. I. Long-term monitoring observations. Astronomy and Astrophysics, 504:929-944. 9/2009. Artigau, E.[10]; Hartung, M.[11]. A deep look into the core of young clusters. II. λ- Orionis. Astronomy and Astrophysics, 504:199-209. 9/2009. West, Michael J.[19]. The XMM Cluster Survey: forecasting cosmological and cluster scaling- relation parameter constraints. -
Florian Niederhofer1,2 Michael Hilker1 Nate Bastian3 Esteban Silva-Villa4,5
Florian Niederhofer1,2 Michael Hilker1 Nate Bastian3 Esteban Silva-Villa4,5 1- European Southern Observatory 2- Universitäts-Sternwarte München 3- John Moores University Liverpool 4- CRAQ 5- Universidad de Antioquia NGC 2100 Credit: ESO Searching for Age Spreads ! Color-magnitude diagrams of intermediate age (1-2 Gyr) massive clusters in the LMC show extended or double main sequence turn-offs (MSTO) NGC 1783, NGC 1806 and NGC 1846 (Mackey et al. 2008) ! If these features are related to an age spread of 200-500 Myr, young clusters (<1 Gyr) with similar properties should have age spreads of the same order, as well ! We searched for age spreads in a sample of eight young (< 1.1 Gyr) 4 massive (> 10 M") LMC clusters ! The data set consists of archival HST WFPC2 data from Brocato et al. 2001, Fischer et al. 1998 and the Hubble Legacy Archive RASPUTIN Workshop 13.-17. October 2014 Our Cluster Sample ! The selected clusters cover the age range from 20 Myr to ≈ 1 Gyr ! They follow the same mass-effective radius relation as the intermediate age clusters that show an extended MSTO ! Blue circles: Clusters analyzed in this study ! Blue dots surrounded by circles: Clusters already analyzed by Bastian & Silva-Villa 2013 ! Red triangles: Intermediate age (1-2 Gyr) clusters that show extended or double MS turn- offs (Goudfrooij 2009,11a) ! Black dots: Other LMC clusters RASPUTIN Workshop 13.-17. October 2014 CMDs of the Clusters NGC 2249 NGC 1831 NGC 2136 NGC 2157 NGC 1850 NGC 1847 Stars that are used for NGC 2004 NGC 2100 further analysis Red crosses: Stars that are removed as field stars Niederhofer et al.