INFRARED SURFACE BRIGHTNESS FLUCTUATIONS of MAGELLANIC STAR CLUSTERS1 Rosa A
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Arxiv:1612.03165V3 [Astro-Ph.HE] 12 Sep 2017 – 2 –
The second catalog of flaring gamma-ray sources from the Fermi All-sky Variability Analysis S. Abdollahi1, M. Ackermann2, M. Ajello3;4, A. Albert5, L. Baldini6, J. Ballet7, G. Barbiellini8;9, D. Bastieri10;11, J. Becerra Gonzalez12;13, R. Bellazzini14, E. Bissaldi15, R. D. Blandford16, E. D. Bloom16, R. Bonino17;18, E. Bottacini16, J. Bregeon19, P. Bruel20, R. Buehler2;21, S. Buson12;22, R. A. Cameron16, M. Caragiulo23;15, P. A. Caraveo24, E. Cavazzuti25, C. Cecchi26;27, A. Chekhtman28, C. C. Cheung29, G. Chiaro11, S. Ciprini25;26, J. Conrad30;31;32, D. Costantin11, F. Costanza15, S. Cutini25;26, F. D'Ammando33;34, F. de Palma15;35, A. Desai3, R. Desiante17;36, S. W. Digel16, N. Di Lalla6, M. Di Mauro16, L. Di Venere23;15, B. Donaggio10, P. S. Drell16, C. Favuzzi23;15, S. J. Fegan20, E. C. Ferrara12, W. B. Focke16, A. Franckowiak2, Y. Fukazawa1, S. Funk37, P. Fusco23;15, F. Gargano15, D. Gasparrini25;26, N. Giglietto23;15, M. Giomi2;59, F. Giordano23;15, M. Giroletti33, T. Glanzman16, D. Green13;12, I. A. Grenier7, J. E. Grove29, L. Guillemot38;39, S. Guiriec12;22, E. Hays12, D. Horan20, T. Jogler40, G. J´ohannesson41, A. S. Johnson16, D. Kocevski12;42, M. Kuss14, G. La Mura11, S. Larsson43;31, L. Latronico17, J. Li44, F. Longo8;9, F. Loparco23;15, M. N. Lovellette29, P. Lubrano26, J. D. Magill13, S. Maldera17, A. Manfreda6, M. Mayer2, M. N. Mazziotta15, P. F. Michelson16, W. Mitthumsiri45, T. Mizuno46, M. E. Monzani16, A. Morselli47, I. V. Moskalenko16, M. Negro17;18, E. Nuss19, T. Ohsugi46, N. Omodei16, M. Orienti33, E. -
Is the Universe Expanding?: an Historical and Philosophical Perspective for Cosmologists Starting Anew
Western Michigan University ScholarWorks at WMU Master's Theses Graduate College 6-1996 Is the Universe Expanding?: An Historical and Philosophical Perspective for Cosmologists Starting Anew David A. Vlosak Follow this and additional works at: https://scholarworks.wmich.edu/masters_theses Part of the Cosmology, Relativity, and Gravity Commons Recommended Citation Vlosak, David A., "Is the Universe Expanding?: An Historical and Philosophical Perspective for Cosmologists Starting Anew" (1996). Master's Theses. 3474. https://scholarworks.wmich.edu/masters_theses/3474 This Masters Thesis-Open Access is brought to you for free and open access by the Graduate College at ScholarWorks at WMU. It has been accepted for inclusion in Master's Theses by an authorized administrator of ScholarWorks at WMU. For more information, please contact [email protected]. IS THEUN IVERSE EXPANDING?: AN HISTORICAL AND PHILOSOPHICAL PERSPECTIVE FOR COSMOLOGISTS STAR TING ANEW by David A Vlasak A Thesis Submitted to the Faculty of The Graduate College in partial fulfillment of the requirements forthe Degree of Master of Arts Department of Philosophy Western Michigan University Kalamazoo, Michigan June 1996 IS THE UNIVERSE EXPANDING?: AN HISTORICAL AND PHILOSOPHICAL PERSPECTIVE FOR COSMOLOGISTS STARTING ANEW David A Vlasak, M.A. Western Michigan University, 1996 This study addresses the problem of how scientists ought to go about resolving the current crisis in big bang cosmology. Although this problem can be addressed by scientists themselves at the level of their own practice, this study addresses it at the meta level by using the resources offered by philosophy of science. There are two ways to resolve the current crisis. -
Expected Differences Between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition
New Views of the Magellanic Clouds fA U Symposium, Vol. 190, 1999 Y.-H. Chu, N.B. Suntzef], J.E. Hesser, and D.A. Bohlender, eds. Expected Differences between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition Ju. Frantsman Astronomical Institute, Latvian University, Raina Blvd. 19, Riga, LV-1586, LATVIA Abstract. Certain aspects of the AGB population, such as the relative number of M and N stars, the mass loss rates, and the initial masses of carbon- oxygen cores, depend on the initial heavy element abundance Z. I have calculated synthetic populations of AGB stars for different initial Z values taking into consideration the evolution of single and close binary stars. I present the results of population syntheses of AGB stars in clusters as a function of different initial chemical compositions. The relation for the tip luminosity of AGB stars versus cluster age as a function of Z is presented and is used to determine the ages for a number of clusters in the LMC and the SMC, including clusters with no previous age determinations. Population simulations show that for low heavy element abundance (Z = 0.001) few M stars are formed with respect to the number of carbon stars. However, the total number of all AGB stars in clusters is not affected by the initial chemical composition. As a result of the evolution of close binary components after the mass exchange, an increase in the range of limiting values of the thermal pulsing AGB star luminosities is expected. The difference between the maximum luminosity on the AGB of single star and the luminosity of a star after a mass exchange event in a close binary system may be as great as 1 magnitude for very young clusters. -
On the Effects of Subvirial Initial Conditions and the Birth
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 24 October 2018 (MN LATEX style file v2.2) On the Effects of Subvirial Initial Conditions and the Birth Temperature of R136 Daniel P. Caputo1⋆, Nathan de Vries1 and Simon Portegies Zwart1 1Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, the Netherlands 24 October 2018 ABSTRACT We investigate the effect of different initial virial temperatures, Q, on the dynamics of star clusters. We find that the virial temperature has a strong effect on many aspects of the resulting system, including among others: the fraction of bodies escaping from the system, the depth of the collapse of the system, and the strength of the mass segregation. These differences deem the practice of using “cold” initial conditions no longer a simple choice of convenience. The choice of initial virial temperature must be carefully considered as its impact on the remainder of the simulation can be profound. We discuss the pitfalls and aim to describe the general behavior of the collapse and the resultant system as a function of the virial temperature so that a well reasoned choice of initial virial temperature can be made. We make a correction to the previous theoretical estimate for the minimum radius, Rmin, of the cluster at the deepest (−1/3) moment of collapse to include a Q dependency, Rmin ≈ Q+N , where N is the number of particles. We use our numericalresults to infer more aboutthe initial conditions of the young cluster R136. Based on our analysis, we find that R136 was likely formed with a rather cool, but not cold, initial virial temperature (Q ≈ 0.13). -
Remerciements – Unité 1
TVO ILC SNC1D Remerciements Remerciements – Unité 1 Graphs, diagrams, illustrations, images in this course, unless otherwise specified, are ILC created, Copyright © 2018 The Ontario Educational Communications Authority. All rights reserved. Intro Video, Copyright © 2018 The Ontario Educational Communications Authority. All rights reserved. All title artwork and graphics, unless otherwise specified, Copyright © 2018The Ontario Educational Communications Authority. All rights reserved. Logo: Science Presse , Agence Science-Presse, URL: https://www.sciencepresse.qc.ca/, Accessed 14/01/2019. Logo: Curium, Curium, URL: https://curiummag.com/wp-content/uploads/2017/10/logo_ curium-web.png, Accessed 14/01/2019. Logo: Science Étonnante, David Louapre, URL: https://sciencetonnante.wordpress.com/, Accessed 20/03/2018, © 2018 HowStuffWorks, a division of InfoSpace Holdings LLC, a System1 Company. Blog, blogging and blogglers theme, djvstock/iStock/Getty Images Logo: Wordpress, WordPress.com, Automattic Inc., URL: https://wordpress.com/, Accessed 20/03/2018, © The WordPress Foundation. Logo: Wix, Wix.com, Inc., URL: https://static.wixstatic.com/ media/9ab0d1_39d56f21398048df8af89aab0cec67b8~mv1.png, Accessed 14/01/2019. Logo: Blogger, Blogger, Inc., ZyMOS, URL: https://commons.wikimedia.org/wiki/File:Blogger. svg, Accessed 20/03/2018, © Google LLC. HOME A film by Yann Arthus-Bertrand, GoodPlanet Foundation, Europacorp and Elzévir Films, URL: https://www.youtube.com/watch?v=GItD10Joaa0, Published 04/02/2009, Accessed 20/04/2018, Courtesy of the GoodPlanet -
Annual Report 1972
I I ANNUAL REPORT 1972 EUROPEAN SOUTHERN OBSERVATORY ANNUAL REPORT 1972 presented to the Council by the Director-General, Prof. Dr. A. Blaauw, in accordance with article VI, 1 (a) of the ESO Convention Organisation Europeenne pour des Recherches Astronomiques dans 1'Hkmisphtre Austral EUROPEAN SOUTHERN OBSERVATORY Frontispiece: The European Southern Observatory on La Silla mountain. In the foreground the "old camp" of small wooden cabins dating from the first period of settlement on La Silln and now gradually being replaced by more comfortable lodgings. The large dome in the centre contains the Schmidt Telescope. In the background, from left to right, the domes of the Double Astrograph, the Photo- metric (I m) Telescope, the Spectroscopic (1.>2 m) Telescope, and the 50 cm ESO and Copen- hagen Telescopes. In the far rear at right a glimpse of the Hostel and of some of the dormitories. Between the Schmidt Telescope Building and the Double Astrograph the provisional mechanical workshop building. (Viewed from the south east, from a hill between thc existing telescope park and the site for the 3.6 m Telescope.) TABLE OF CONTENTS INTRODUCTION General Developments and Special Events ........................... 5 RESEARCH ACTIVITIES Visiting Astronomers ........................................ 9 Statistics of Telescope Use .................................... 9 Research by Visiting Astronomers .............................. 14 Research by ESO Staff ...................................... 31 Joint Research with Universidad de Chile ...................... -
Cfa in the News ~ Week Ending 3 January 2010
Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis. -
Sep Temb Er 2010
Te Patiki – Palmerston North Astronomical Society Inc September 2010 September 2010 September Headliners The NEXT MEETING Spring on Titan brings will be at the Manawatu sunshine and patchy Observatory on Wednes- clouds day, September 29th, http://www.astronomy.com/asy/ at 8.00 p.m. default.aspx?c=a&id=10253 Jupiter’s Disappearing Belt Many of you who have http:// read Te Patiki over the www.oneminuteastronomer.com/2 010/09/09/jupiters-disappearing- years will no doubt realize belt/ that many of our members Possibility for White Dwarf specialize in deep-sky pho- Pulsars? http:// tography and are amongst www.universetoday.com/74300/ New Zealand’s leading white-dwarf-pulsars/ proponents of this field of In this issue: astronomy. The Big Wet before the Big Dry? There are however more The Planet Mercury has a strings to our bow than comet-like tail. astrophotography as you Google finds a new impact crater in Egypt will find out when you come along and listen to Weird water lurking inside giant planets our featured talk by one of our newer members, Awesome death spiral of a bizarre star Carl Knight, who now Above: Carl Knight with his pride and joy, a 12 lives on the rise just NW NASA to Send a Probe Into inch (30cm) Meade Cassegrain set up outside our the Sun of Bulls. observatory last year for an open night. Carl has Ancient Greeks spotted Hal- ley's comet since established himself at a dark sky site on the Carl will be speaking to us Mars moon may have rise north of Bulls heading towards Wanganui. -
Arxiv:Astro-Ph/0605132 V1 4 May 2006
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server PUBLISHED IN THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2005 DEC: APJS, 161, 304-360 Preprint typeset using LATEX style emulateapj v. 6/22/04 RESOLVED MASSIVE STAR CLUSTERS IN THE MILKY WAY AND ITS SATELLITES: BRIGHTNESS PROFILES AND A CATALOGUE OF FUNDAMENTAL PARAMETERS DEAN E. MCLAUGHLIN University of Leicester, Dept. of Physics and Astronomy, University Road, Leicester, UK LE1 7RH AND ROELAND P. VAN DER MAREL Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 Published in the Astrophysical Journal Supplement Series, 2005 Dec: ApJS, 161, 304-360 ABSTRACT We present a database of structural and dynamical properties for 153 spatially resolved star clusters in the Milky Way, the Large and Small Magellanic Clouds, and the Fornax dwarf spheroidal. This database comple- ments and extends others in the literature, such as those of Harris (1996) and Mackey & Gilmore (2003a,b,c). Our cluster sample comprises 50 “young massive clusters” in the LMC and SMC, and 103 old globular clusters between the four galaxies. The parameters we list include central and half-light averaged surface brightnesses and mass densities; core and effective radii; central potentials, concentration parameters, and tidal radii; pre- dicted central velocity dispersions and escape velocities; total luminosities, masses, and binding energies; central phase-space densities; half-mass relaxation times; and “κ-space” parameters. We use publicly available population-synthesis models to compute stellar-population properties (intrinsic B −V colors, reddenings, and V-band mass-to-light ratios) for the same 153 clusters plus another 63 globulars in the Milky Way. -
Download the 2016 Spring Deep-Sky Challenge
Deep-sky Challenge 2016 Spring Southern Star Party Explore the Local Group Bonnievale, South Africa Hello! And thanks for taking up the challenge at this SSP! The theme for this Challenge is Galaxies of the Local Group. I’ve written up some notes about galaxies & galaxy clusters (pp 3 & 4 of this document). Johan Brink Peter Harvey Late-October is prime time for galaxy viewing, and you’ll be exploring the James Smith best the sky has to offer. All the objects are visible in binoculars, just make sure you’re properly dark adapted to get the best view. Galaxy viewing starts right after sunset, when the centre of our own Milky Way is visible low in the west. The edge of our spiral disk is draped along the horizon, from Carina in the south to Cygnus in the north. As the night progresses the action turns north- and east-ward as Orion rises, drawing the Milky Way up with it. Before daybreak, the Milky Way spans from Perseus and Auriga in the north to Crux in the South. Meanwhile, the Large and Small Magellanic Clouds are in pole position for observing. The SMC is perfectly placed at the start of the evening (it culminates at 21:00 on November 30), while the LMC rises throughout the course of the night. Many hundreds of deep-sky objects are on display in the two Clouds, so come prepared! Soon after nightfall, the rich galactic fields of Sculptor and Grus are in view. Gems like Caroline’s Galaxy (NGC 253), the Black-Bottomed Galaxy (NGC 247), the Sculptor Pinwheel (NGC 300), and the String of Pearls (NGC 55) are keen to be viewed. -
Carbon Stars T. Lloyd Evans
J. Astrophys. Astr. (2010) 31, 177–211 Carbon Stars T. Lloyd Evans SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK. e-mail: [email protected] Received 2010 July 19; accepted 2010 October 18 Abstract. In this paper, the present state of knowledge of the carbon stars is discussed. Particular attention is given to issues of classification, evolution, variability, populations in our own and other galaxies, and circumstellar material. Key words. Stars: carbon—stars: evolution—stars: circumstellar matter —galaxies: magellanic clouds. 1. Introduction Carbon stars have been reviewed on several previous occasions, most recently by Wallerstein & Knapp (1998). A conference devoted to this topic was held in 1996 (Wing 2000) and two meetings on AGB stars (Le Bertre et al. 1999; Kerschbaum et al. 2007) also contain much on carbon stars. This review emphasizes develop- ments since 1997, while paying particular attention to connections with earlier work and to some of the important sources of concepts. Recent and ongoing develop- ments include surveys for carbon stars in more of the galaxies of the local group and detailed spectroscopy and infrared photometry for many of them, as well as general surveys such as 2MASS, AKARI and the Sirius near infrared survey of the Magel- lanic Clouds and several dwarf galaxies, the Spitzer-SAGE mid-infrared survey of the Magellanic Clouds and the current Herschel infrared satellite project. Detailed studies of relatively bright galactic examples continue to be made by high-resolution spectroscopy, concentrating on abundance determinations using the red spectral region, and infrared and radio observations which give information on the history of mass loss. -
407 a Abell Galaxy Cluster S 373 (AGC S 373) , 351–353 Achromat
Index A Barnard 72 , 210–211 Abell Galaxy Cluster S 373 (AGC S 373) , Barnard, E.E. , 5, 389 351–353 Barnard’s loop , 5–8 Achromat , 365 Barred-ring spiral galaxy , 235 Adaptive optics (AO) , 377, 378 Barred spiral galaxy , 146, 263, 295, 345, 354 AGC S 373. See Abell Galaxy Cluster Bean Nebulae , 303–305 S 373 (AGC S 373) Bernes 145 , 132, 138, 139 Alnitak , 11 Bernes 157 , 224–226 Alpha Centauri , 129, 151 Beta Centauri , 134, 156 Angular diameter , 364 Beta Chamaeleontis , 269, 275 Antares , 129, 169, 195, 230 Beta Crucis , 137 Anteater Nebula , 184, 222–226 Beta Orionis , 18 Antennae galaxies , 114–115 Bias frames , 393, 398 Antlia , 104, 108, 116 Binning , 391, 392, 398, 404 Apochromat , 365 Black Arrow Cluster , 73, 93, 94 Apus , 240, 248 Blue Straggler Cluster , 169, 170 Aquarius , 339, 342 Bok, B. , 151 Ara , 163, 169, 181, 230 Bok Globules , 98, 216, 269 Arcminutes (arcmins) , 288, 383, 384 Box Nebula , 132, 147, 149 Arcseconds (arcsecs) , 364, 370, 371, 397 Bug Nebula , 184, 190, 192 Arditti, D. , 382 Butterfl y Cluster , 184, 204–205 Arp 245 , 105–106 Bypass (VSNR) , 34, 38, 42–44 AstroArt , 396, 406 Autoguider , 370, 371, 376, 377, 388, 389, 396 Autoguiding , 370, 376–378, 380, 388, 389 C Caldwell Catalogue , 241 Calibration frames , 392–394, 396, B 398–399 B 257 , 198 Camera cool down , 386–387 Barnard 33 , 11–14 Campbell, C.T. , 151 Barnard 47 , 195–197 Canes Venatici , 357 Barnard 51 , 195–197 Canis Major , 4, 17, 21 S. Chadwick and I. Cooper, Imaging the Southern Sky: An Amateur Astronomer’s Guide, 407 Patrick Moore’s Practical