Metallicity Relation in the Magellanic Clouds Clusters , ,
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Arxiv:Astro-Ph/9808091V1 10 Aug 1998 Pc Eecp Cec Nttt,Wihi Prtdb the NAS5-26555
To appear in the Astronomical Journal (accepted 1998 August 10) WFPC2 OBSERVATIONS OF STAR CLUSTERS IN THE MAGELLANIC CLOUDS. II. THE OLDEST STAR CLUSTERS IN THE SMALL MAGELLANIC CLOUD1 Kenneth J. Mighell2 Kitt Peak National Observatory, National Optical Astronomy Observatories3, P. O. Box 26732, Tucson, AZ 85726-6732 Electronic mail: [email protected] Ata Sarajedini4 Department of Physics and Astronomy, San Francisco State University, 1600 Holloway Avenue, San Francisco, CA 94132 Electronic mail: [email protected] Rica S. French5 Middle Tennessee State University, Physics & Astronomy Department, WPS 219, P. O. Box 71, Murfreesboro, TN 37132 Electronic mail: [email protected] arXiv:astro-ph/9808091v1 10 Aug 1998 1 Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS5-26555. 2 Guest User, Canadian Astronomy Data Centre, which is operated by the Dominion Astrophysical Observatory for the National Research Council of Canada’s Herzberg Institute of Astrophysics. 3NOAO is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. 4Hubble Fellow 5Based on research conducted at NOAO as part of the Research Experiences for Undergraduates program. – 2 – ABSTRACT We present our analysis of archival Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) observations in F450W ( B) and F555W ( V ) of the ∼ ∼ intermediate-age populous star clusters NGC 121, NGC 339, NGC 361, NGC 416, and Kron 3 in the Small Magellanic Cloud. -
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. -
Multiplicity of the Red Supergiant Population in the Young Massive Cluster NGC 330
UvA-DARE (Digital Academic Repository) Multiplicity of the red supergiant population in the young massive cluster NGC 330 Patrick, L.R.; Lennon, D.J.; Evans, C.J.; Sana, H.; Bodensteiner, J.; Britavskiy, N.; Dorda, R.; Herrero, A.; Negueruela, I.; de Koter, A. DOI 10.1051/0004-6361/201936741 Publication date 2020 Document Version Final published version Published in Astronomy & Astrophysics Link to publication Citation for published version (APA): Patrick, L. R., Lennon, D. J., Evans, C. J., Sana, H., Bodensteiner, J., Britavskiy, N., Dorda, R., Herrero, A., Negueruela, I., & de Koter, A. (2020). Multiplicity of the red supergiant population in the young massive cluster NGC 330. Astronomy & Astrophysics, 635, [A29]. https://doi.org/10.1051/0004-6361/201936741 General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulations If you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: https://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. UvA-DARE is a service provided by the library of the University of Amsterdam (https://dare.uva.nl) Download date:25 Sep 2021 A&A 635, A29 (2020) Astronomy https://doi.org/10.1051/0004-6361/201936741 & c ESO 2020 Astrophysics Multiplicity of the red supergiant population in the young massive cluster NGC 330?,?? L. -
Stars and Galaxies
Stars and Galaxies STUDENT PAGE Se e i n g i n to t h e Pa S t A galaxy is a gravitationally bound system of stars, gas, and dust. Gal- We can’t travel into the past, but we axies range in diameter from a few thousand to a few hundred thou- can get a glimpse of it. Every sand light-years. Each galaxy contains billions (10 9) or trillions (1012) time we look at the Moon, for of stars. In this activity, you will apply concepts of scale to grasp the example, we see it as it was a distances between stars and galaxies. You will use this understanding little more than a second ago. to elaborate on the question, Do galaxies collide? That’s because sunlight reflected from the Moon’s surface takes a little more EX P LORE than a second to reach Earth. We see On a clear, dark night, you can see hundreds of bright stars. The next table the Sun as it looked about eight minutes shows some of the brightest stars with their diameters and distances from ago, and the other stars as they were a the Sun. Use a calculator to determine the scaled distance to each star few years to a few centuries ago. (how many times you could fit the star between itself and the Sun). Hint: And then there’s M31, the Androm- you first need to convert light-years and solar diameters into meters. One eda galaxy — the most distant object light-year equals 9.46 x 1015 meters, and the Sun’s diameter is 1.4 x 109 that’s readily visible to human eyes. -
Hints for Multiple Populations in Intermediate-Age Clusters of the Small Magellanic Cloud Submitted to AJ ABSTRACT We Report On
Draft version September 19, 2018 Typeset using LATEX default style in AASTeX62 Hints for multiple populations in intermediate-age clusters of the Small Magellanic Cloud Andres´ E. Piatti1, 2 1Consejo Nacional de Investigaciones Cient´ıficas y T´ecnicas, Av. Rivadavia 1917, C1033AAJ,Buenos Aires, Argentina 2Observatorio Astron´omico de C´ordoba, Laprida 854, 5000, C´ordoba, Argentina Submitted to AJ ABSTRACT We report on the magnitude of the intrinsic [Fe/H] spread in the Small Magellanic Cloud (SMC) intermediate-age massive clusters NGC 339, 361, Lindsay 1 and 113, respectively. In order to measure the cluster metallicity dispersions, we used accurate Str¨omgrenphotometry of carefully selected cluster red giant branch (RGB) stars. We determined the Fe-abundance spreads by employing a maximum likelihood approach. The spreads obtained using the more accurate photometry of the brighter RGB stars resulted to be marginal (∼ 0.05±0.03 dex) for NGC 339 and NGC 361, while for Lindsay 1 and Lindsay 113 we obtained metallicity spreads of 0.00±0.04 dex. From these results, we speculated with the possibility that NGC 361 is added to the group of four SMC clusters with observational evidence of multiple populations (MPs). Furthermore, in the context of the present debate about the existence of Fe-abundance inhomogeneities among old clusters with MPs, these outcomes put new constrains to recent theoretical speculations for making this phenomenon visible. Keywords: techniques: photometric | galaxies: individual: SMC | Magellanic Clouds. 1. INTRODUCTION 5 Four intermediate-age (5-8 Gyr) massive (& 10 M ) clusters of the Small Magellanic Cloud (SMC) have been found to harbour multiple stellar populations (Kron 3, Lindsay 1, NGC 339 and 416 Hollyhead et al. -
NGC 602: Taken Under the “Wing” of the Small Magellanic Cloud
National Aeronautics and Space Administration NGC 602 www.nasa.gov NGC 602: Taken Under the “Wing” of the Small Magellanic Cloud The Small Magellanic Cloud (SMC) is one of the closest galaxies to the Milky Way. In this composite image the Chandra data is shown in purple, optical data from Hubble is shown in red, green and blue and infrared data from Spitzer is shown in red. Chandra observations of the SMC have resulted in the first detection of X-ray emission from young stars with masses similar to our Sun outside our Milky Way galaxy. The Small Magellanic Cloud (SMC) is one of the Milky Way’s region known as NGC 602, which contains a collection of at least closest galactic neighbors. Even though it is a small, or so-called three star clusters. One of them, NGC 602a, is similar in age, dwarf galaxy, the SMC is so bright that it is visible to the unaided mass, and size to the famous Orion Nebula Cluster. Researchers eye from the Southern Hemisphere and near the equator. have studied NGC 602a to see if young stars—that is, those only a few million years old—have different properties when they have Modern astronomers are also interested in studying the SMC low levels of metals, like the ones found in NGC 602a. (and its cousin, the Large Magellanic Cloud), but for very different reasons. The SMC is one of the Milky Way’s closest galactic Using Chandra, astronomers discovered extended X-ray emission, neighbors. Because the SMC is so close and bright, it offers an from the two most densely populated regions in NGC 602a. -
Large Magellanic Cloud, One of Our Busy Galactic Neighbors
The Large Magellanic Cloud, One of Our Busy Galactic Neighbors www.nasa.gov Our Busy Galactic Neighbors also contain fewer metals or elements heavier than hydrogen and helium. Such an environment is thought to slow the growth The cold dust that builds blazing stars is revealed in this image of stars. Star formation in the universe peaked around 10 billion that combines infrared observations from the European Space years ago, even though galaxies contained lesser abundances Agency’s Herschel Space Observatory and NASA’s Spitzer of metallic dust. Previously, astronomers only had a general Space Telescope. The image maps the dust in the galaxy known sense of the rate of star formation in the Magellanic Clouds, as the Large Magellanic Cloud, which, with the Small Magellanic but the new images enable them to study the process in more Cloud, are the two closest sizable neighbors to our own Milky detail. Way Galaxy. Herschel is a European The Large Magellanic Cloud looks like a fiery, circular explosion Space Agency in the combined Herschel–Spitzer infrared data. Ribbons of dust cornerstone mission, ripple through the galaxy, with significant fields of star formation with science instruments noticeable in the center, center-left and top right. The brightest provided by consortia center-left region is called 30 Doradus, or the Tarantula Nebula, of European institutes for its appearance in visible light. and with important participation by NASA. NASA’s Herschel Project Office is based at NASA’s Jet Propulsion Laboratory, Pasadena, Calif. JPL contributed mission-enabling technology for two of Herschel’s three science instruments. -
1. INTRODUCTION Formed Via the Accretion And/Or Merger of Dwarf Satellite Galaxies (Searle & Zinn 1978;Coü Te Et Al
THE ASTRONOMICAL JOURNAL, 122:220È231, 2001 July ( 2001. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE LINE-OF-SIGHT DEPTH OF POPULOUS CLUSTERS IN THE SMALL MAGELLANIC CLOUD HUGH H. CROWL1 AND ATA SARAJEDINI2,3 Department of Astronomy, Wesleyan University, Middletown, CT 06459-0123; hugh=astro.yale.edu; ata=astro.uÑ.edu ANDRE S E. PIATTI ObservatorioAstroo mico, Universidad Nacional de Cordoba, Laprida 854, Co rdoba, 5000, Argentina;andres=mail.oac.uncor.edu DOUG GEISLER Grupo de Astronomia, Departmento de Fisica, Universidad deConcepcio n, Casilla 160-C, Concepcio n, Chile; doug=kukita.cfm.udec.cl EDUARDO BICA Departamento de Astronomia, Instituto de Fisica, UFRGS, CP 15051, 91501-970, Porto Alegre, RS, Brazil; bica=if.ufrgs.br JUAN J. CLARIA ObservatorioAstroo mico, Laprida 854, Co rdoba, 5000, Argentina; claria=mail.oac.uncor.edu AND JOA8 O F. C. SANTOS,JR. Departamento de Fisica, ICEx, Universidade Federal de Minas Gerais, CP 702, 30123-970 Belo Horizonte, MG, Brazil; jsantos=Ðsica.ufmg.br Received 2000 November 14; accepted 2001 March 11 ABSTRACT We present an analysis of age, metal abundance, and positional data on populous clusters in the Small Magellanic Cloud (SMC) with the ultimate aim of determining the line-of-sight (LOS) depth of the SMC by using these clusters as proxies. Our data set contains 12 objects and is limited to clusters with the highest-quality data for which the ages and abundances are best known and can be placed on an inter- nally consistent scale. We have analyzed the variation of the clustersÏ properties with position on the sky and with line-of-sight depth. -
Star Clusters As Witnesses of the Evolutionary History of the Small Magellanic Cloud
JENAM, Symposium 5: Star Clusters – Witnesses of Cosmic History Star Clusters as Witnesses of the Evolutionary History of the Small Magellanic Cloud Eva K. Grebel Astronomisches Rechen-Institut 11.0Z9.2e00n8 trum für AstrGroebnel,o JEmNAMie Sy mdp.e 5:r S MUC nStairv Celusrtesrsität Heidelbe0 rg My collaborators: ! PhD student Katharina Glatt ! PhD student Andrea Kayser (both University of Basel & University of Heidelberg) ! Andreas Koch (U Basel & UCLA / OCIW) ! Jay Gallagher, D. Harbeck (U Wisc) ! Elena Sabbi (U Heidelberg & STScI) ! Antonella Nota, Marco Sirianni (STScI) ! Monica Tosi, Gisella Clementini (U Bologna) ! Andrew Cole (U Tasmania) ! Gary Da Costa (ANU) 11.09.2008 Grebel, JENAM Symp. 5: SMC Star Clusters 1 NGC 416 (OGLE) Tracers of the Age-Metallicity Relation: ! Star clusters: ! Easily identifiable. ! Chronometers of intense star formation events. ! Single-age, single-metallicity fossils of local conditions. ! Star clusters in the SMC: ! Clusters formed (and survived) for most of its lifetime " Closely spaced set of age tracers! " Unique property of the SMC. # Milky Way: No comparable set of intermediate-age, populous clusters. # LMC: Age gap at intermediate ages. 11.09.2008 Grebel, JENAM Symp. 5: SMC Star Clusters 2 Cluster-based Age-Metallicity Relation: Photometry Spectroscopy After Da Costa 2002 An inhomogeneous sample: ! Photometric and spectroscopic metallicities from different techniques ! Photometric ages from ground-/space-based data of differing depth 11.09.2008 Grebel, JENAM Symp. 5: SMC Star Clusters 3 Getting Homogeneous Ages and Metallicities: PhD thesis Katharina Glatt ! HST / ACS program to obtain deep CMDs (PI: Gallagher) $ GO 10396, 29 orbits, executed 2005 – 2006. $ 6 populous intermediate-age clusters, 1 globular cluster: NGC 419, Lindsay 38, NGC 416, 339, Kron 3, Lindsay 1, NGC 121. -
A Study of Be Stars in the Magellanic Clouds 3
A Mon. Not. R. Astron. Soc. 000, 1–10 (2013) Printed 27 November 2017 (MN LTEX style file v2.2) A study of Be stars in the Magellanic Clouds S. Iqbal1⋆ and S. C. Keller1† 1Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia. Received 2013 August ABSTRACT We present the results of a photometric survey for Be stars in eleven young clusters in the Large Magellanic Cloud and fourteen young clusters in the Small Magellanic Cloud. B stars with hydrogen in emission are identified on the basis of their R-Hα colour. We find that Be star fraction in clusters decreases with cluster age, and also decreases with the metallicity. Key words: early-type stars: emission-line, Be galaxies: Magellanic Clouds 1 INTRODUCTION pare the predictions of evolutionary models for early-type stars for NGC 2004 and the N 11 region on the LMC, and The transient nature of emission lines, especially those of NGC 330 and NGC 346 in the SMC. They find that their the Balmer series of hydrogen, exhibited in the spectra of nitrogen abundances are inconsistent with those predicted some B-type stars is known as the ‘Be phenomenon’. These for stars that spend most of the main-sequence lifetimes ro- spectral changes are attributed to a disk of gaseous material tating close to their critical velocity. In particular, they find surrounding the central star, the origins of which are still similar estimated nitrogen enrichment for Be and B type unclear. While recent observational data has allowed for the stars, and postulate that either Be stars rotate faster than elimination of some theoretical models (such as the wind B stars, but not at critical velocity, or that Be stars only compressed disc models of Bjorkman & Cassinelli 1993), no spend a short period (less than 10 %) of their main-sequence satisfactory mechanism for injecting material into the disk life times rotating close to critical velocity. -
Arxiv:1904.01028V2 [Astro-Ph.GA] 22 Nov 2019
MNRAS 000,1{7 (2019) Preprint 26 November 2019 Compiled using MNRAS LATEX style file v3.0 Satellites of Satellites: The Case for Carina and Fornax Stephen A. Pardy1, Elena D'Onghia1;2?, Julio Navarro3, Robert Grand4, Facundo A. G´omez5;6, Federico Marinacci7,Rudiger¨ Pakmor4, Christine Simpson8, Volker Springel4 1Department of Astronomy, University of Wisconsin, 475 North Charter Street, Madison, WI 53706, USA 2Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA 3Senior CIfAR Fellow. Department of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, Canada 4Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. 1, D-85748, Garching, Germany 5Instituto de Investigaci´on Multidisciplinar en Ciencia y Tecnolog´ıa, Universidad de La Serena, Ra´ulBitr´an 1305, La Serena, Chile 6Departamento de F´ısica y Astronom´ıa, Universidad de La Serena, Av. Juan Cisternas 1200 Norte, La Serena, Chile 7Department of Physics & Astronomy, University of Bologna, via Gobetti 93/2, 40129 Bologna, Italy 8Department of Astronomy & Astrophysics, University of Chicago, Chicago, IL 60637, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We use the Auriga cosmological simulations of Milky Way (MW)-mass galaxies and their surroundings to study the satellite populations of dwarf galaxies in ΛCDM. As expected from prior work, the number of satellites above a fixed stellar mass is a strong function of the mass of the primary dwarf. For galaxies as luminous as the Large Magellanic Cloud (LMC), and for halos as massive as expected for the LMC (determined by its rotation speed), the simulations predict about ∼ 3 satellites with 5 stellar masses exceeding M∗ > 10 M . -
The “Local Group” of Galaxies
The “Local Group” of Galaxies Two large spiral galaxies • Milky Way & Andromeda (Messier 31 or M31) • Distance between them: D = 700 kpc = 2.3 x 106 light yrs Each large spiral galaxy has several smaller satellite galaxies in orbit around it • Milky Way: Large Magellanic Cloud (LMC), Small Magellanic Cloud (SMC), Sagittarius dwarf, etc • Andromeda: Messier 32 (M32), NGC 205, NGC 147, etc You are here i>clicker Quiz #19 Which of the following statements about the EPOCH OF CONFINEMENT is TRUE? A. At this instant, quarks became bound in sets of three to produce protons and neutrons, while matter and radiation continued to interact strongly B. The Universe was matter dominated at this epoch C. Protons and electrons formed stable hydrogen atoms for the first time at this epoch, and the matter in the Universe became mostly transparent to radiation D. This epoch was immediately followed by Inflation A Star is Born! • Giant molecular clouds: consist of mostly H2 plus a small amount of other, more complex molecules • Dense cores can begin to collapse under their own gravitational attraction • As a cloud core collapses, the density and temperature of the gas increase → more blackbody radiation • Opacity — the gas is not transparent to the radiation, and the radiation interacts with the gas particles exerting an outward pressure known as radiation pressure • The intense radiation from hot, young stars ionizes the gaseous interstellar medium surrounding it — this is known as an HII region Young star cluster: NGC 3603 Proto-stars • Gravitational collapse