The Search for Multiple Populations in Magellanic Cloud Clusters II: the Detection of Multiple Populations in Three Intermediate-Age SMC Clusters?
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Astronomy & Astrophysics Background Galaxies As Reddening
A&A 371, 895–907 (2001) Astronomy DOI: 10.1051/0004-6361:20010467 & c ESO 2001 Astrophysics Background galaxies as reddening probes throughout the Magellanic Clouds C. M. Dutra1,3,E.Bica1,3,J.J.Clari´a2,3,A.E.Piatti2,3, and A. V. Ahumada2,3 1 Instituto de Fisica-UFRGS, CP 15051, CEP 91501-970 POA – RS, Brazil 2 Observatorio Astron´omico de C´ordoba, Laprida 854, 5000, C´ordoba, Argentina 3 Visiting Astronomer, Complejo Astron´omico El Leoncito operated under agreement between the Consejo Nacional de Investigaciones Cient´ıficas y T´ecnicas de la Rep´ublica Argentina and the National Universities of La Plata, C´ordoba and San Juan Received 3 January 2001 / Accepted 23 March 2001 Abstract. We study the spectral properties in the range 3600 A–6800˚ A˚ of the nuclear region of galaxies behind the Magellanic Clouds. The radial velocities clarified the nature of the objects as background galaxies or extended objects belonging to the Clouds. For most galaxies behind the main bodies of the LMC and SMC, radial velocities were measured for the first time. In the present sample typical LMC background galaxies are nearby (4000 <V(km s−1) < 6000), while SMC’s are considerably more distant (10 000 <V(km s−1) < 20 000). We determine the reddening in each line of sight by matching a reddening-free galaxy template with comparable stellar population. For the LMC main body we derive a combined Milky Way and internal reddening value E(B−V )MW+i =0.120.10, while for the SMC E(B−V )MW+i =0.050.05. -
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. -
Publications OFTHK Astronomical Socik-N-Οκτπκ Pacific 101: 570-572, June 1989
Publications OFTHK Astronomical SociK-n-οκτπκ Pacific 101: 570-572, June 1989 A SURVEY FOR RR LYRAE VARIABLES IN FIVE SMALL MAGELLANIC CLOUD CLUSTERS ALISTAIR R. WALKER Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatories* Casilla 603, La Serena, Chile Received 1989 March 15 ABSTRACT Results are presented of a search for RR Lyrae variables in the SMC clusters NGC 121, Lindsay 1, Kron 3, Kron 7, and Kron 44. The techniques used rediscovered the four RR Lyraes in NGC 121, but no variables were found in the other clusters. It is concluded that RR Lyraes do not occur in SMC clusters younger than — 11 Gyr. Key words: star clusters-Magellanic Clouds-variable stars: RR Lyrae stars 1. Introduction Lindsay 1 but did not find any variables; however, the The Small Magellanic Cloud (SMC) contains a number majority of his plates were exposed in times of rather poor of populous clusters in the age range 3-12 Gyr, unlike seeing. A survey of several MC clusters for RR Lyraes was either the Galaxy or the Large Magellanic Cloud (LMC). made, using the Yale 1-m telescope and an image-tube Olszewski (1986) and Olszewski, Schommer, and camera, by Graham and Nemec (1984). They found many Aaronson (1987, henceforth OSA) point out that it should variables in old LMC clusters but none in the two SMC be possible to determine the age of the youngest cluster clusters blinked, NGC 339 and NGC 416. RR Lyraes by a suitable survey for the variables in the Since these surveys, color-magnitude diagrams candidate clusters. -
SCYON Issue 77
edited by Giovanni Carraro, Martin Netopil, and Ernst Paunzen https://www.univie.ac.at/scyon/ email: [email protected] The official Newsletter of the IAU Commission H4. SCYON Issue No. 77 September 30th, 2018 Dear Colleagues, This editorial is dedicated to an announcement by Amanda Karakas, the new President of the IAU Commission H4, which you can find on the next page. The current SCYON issue includes numerous paper abstracts, which cover a broad range in star cluster research. We also want to congratulate Maria Tiongco, who recently finished her PhD at the Indiana University. We wish her all the best for the future career! Furthermore, save the date for an upcoming conference in Bologna and register for one which takes place soon in Heidelberg. The SCYON editor team: Giovanni Carraro, Martin Netopil, and Ernst Paunzen CONTENTS About the Newsletter Abstracts of refereed papers . 3 SCYON publishes abstracts from any Star Forming Regions ..................3 area in astronomy, which are relevant to Galactic Open Clusters .................5 research on star clusters. We welcome all Galactic Globular Clusters .............8 kinds of submitted contributions (abstracts Clusters in the Magellanic clouds .......9 of refereed papers or conference proceedings, The most distant clusters .............11 PhD summaries, and general announcements Dynamical evolution - Simulations . 13 of e.g. conferences, databases, tools, etc.) Miscellaneous .........................16 Proceedings abstracts ....................17 The mission of this newsletter is to help Ph.D. (dissertation) summaries ...........18 all the researchers in the field with a quick Conferences and Announcements .........19 and efficient link to the scientific activity in the field. We encourage everybody to contribute to the new releases! New abstracts can be submitted at any time using the webform on the SCYON homepage. -
Properties of Stellar Generations in Globular Clusters and Relations With
Astronomy & Astrophysics manuscript no. carretta c ESO 2018 November 9, 2018 Properties of stellar generations in Globular Clusters and relations with global parameters ⋆ E. Carretta1, A. Bragaglia1, R.G. Gratton2, A. Recio-Blanco3, S. Lucatello2,4, V. D’Orazi2, and S. Cassisi5 1 INAF-Osservatorio Astronomico di Bologna, via Ranzani 1, I-40127 Bologna, Italy 2 INAF-Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 3 Laboratoire Cassiop´ee UMR 6202, Universit`ede Nice Sophia-Antipolis, CNRS, Observatoire de la Cote d’Azur, BP 4229, 06304 Nice Cedex 4, France 4 Excellence Cluster Universe, Technische Universit¨at M¨unchen, Boltzmannstr. 2, D-85748, Garching, Germany 5 INAF-Osservatorio Astronomico di Collurania, via M. Maggini, I-64100 Teramo, Italy Received .....; accepted ..... ABSTRACT We revise the scenario of the formation of Galactic globular clusters (GCs) by adding the observed detailed chemical composition of their different stellar generations to the set of their global parameters. We exploit the unprecedented set of homogeneous abundances of more than 1200 red giants in 19 clusters, as well as additional data from literature, to give a new definition of bona fide globular clusters, as the stellar aggregates showing the presence of the Na-O anticorrelation. We propose a classification of GCs according to their kinematics and location in the Galaxy in three populations: disk/bulge, inner halo, and outer halo. We find that the luminosity function of globular clusters is fairly independent of their population, suggesting that it is imprinted by the formation mechanism, and only marginally affected by the ensuing evolution. We show that a large fraction of the primordial population should have been lost by the proto-GCs. -
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. -
108 Afocal Procedure, 105 Age of Globular Clusters, 25, 28–29 O
Index Index Achromats, 70, 73, 79 Apochromats (APO), 70, Averted vision Adhafera, 44 73, 79 technique, 96, 98, Adobe Photoshop Aquarius, 43, 99 112 (software), 108 Aquila, 10, 36, 45, 65 Afocal procedure, 105 Arches cluster, 23 B1620-26, 37 Age Archinal, Brent, 63, 64, Barkhatova (Bar) of globular clusters, 89, 195 catalogue, 196 25, 28–29 Arcturus, 43 Barlow lens, 78–79, 110 of open clusters, Aricebo radio telescope, Barnard’s Galaxy, 49 15–16 33 Basel (Bas) catalogue, 196 of star complexes, 41 Aries, 45 Bayer classification of stellar associations, Arp 2, 51 system, 93 39, 41–42 Arp catalogue, 197 Be16, 63 of the universe, 28 Arp-Madore (AM)-1, 33 Beehive Cluster, 13, 60, Aldebaran, 43 Arp-Madore (AM)-2, 148 Alessi, 22, 61 48, 65 Bergeron 1, 22 Alessi catalogue, 196 Arp-Madore (AM) Bergeron, J., 22 Algenubi, 44 catalogue, 197 Berkeley 11, 124f, 125 Algieba, 44 Asterisms, 43–45, Berkeley 17, 15 Algol (Demon Star), 65, 94 Berkeley 19, 130 21 Astronomy (magazine), Berkeley 29, 18 Alnilam, 5–6 89 Berkeley 42, 171–173 Alnitak, 5–6 Astronomy Now Berkeley (Be) catalogue, Alpha Centauri, 25 (magazine), 89 196 Alpha Orionis, 93 Astrophotography, 94, Beta Pictoris, 42 Alpha Persei, 40 101, 102–103 Beta Piscium, 44 Altair, 44 Astroplanner (software), Betelgeuse, 93 Alterf, 44 90 Big Bang, 5, 29 Altitude-Azimuth Astro-Snap (software), Big Dipper, 19, 43 (Alt-Az) mount, 107 Binary millisecond 75–76 AstroStack (software), pulsars, 30 Andromeda Galaxy, 36, 108 Binary stars, 8, 52 39, 41, 48, 52, 61 AstroVideo (software), in globular clusters, ANR 1947 -
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 -
Ca II Triplet Spectroscopy of Giants in SMC Star Clusters: Abundances, Velocities and the Age-Metallicity Relation
Ca II Triplet Spectroscopy of Giants in SMC Star Clusters: Abundances, Velocities and the Age-Metallicity Relation G. S. Da Costa Mount Stromlo and Siding Spring Observatories, The Australian National University, Private Bag, Weston Creek Post Office, ACT 2611, Australia Electronic mail: [email protected] and D. Hatzidimitriou Physics Department, University of Crete, P.O. Box 2208, Heraklion 710 03, Crete, Greece Electronic mail: [email protected] ABSTRACT We have obtained spectra at the Ca II triplet of individual red giants in seven SMC star clusters whose ages range from ∼4 to 12 Gyr. The spectra have been used to determine mean abundances for six of the star clusters to a typical precision of 0.12 dex. When combined with existing data for other objects, the resulting SMC age-metallicity relation is generally consistent with that for a simple model of chemical evolution, scaled to the present-day SMC mean abundance and gas mass fraction. Two of the clusters (Lindsay 113 and NGC 339), however, have abundances that are ∼0.5 dex lower than that expected from the mean age-metallicity relation. It is suggested that the formation of these clusters, which have ages of ∼5 Gyr, may have involved the infall of unenriched gas, perhaps from the Magellanic Stream. The spectra also yield radial velocities for the seven clusters. The resulting velocity dispersion is −1 arXiv:astro-ph/9802008v1 2 Feb 1998 16 ± 4 km s , consistent with those of the SMC planetary nebula and carbon star populations. Subject headings: galaxies: abundances — galaxies: individual (SMC) — galaxies: kinematics and dynamics — galaxies: star clusters — Magellanic Clouds Accepted for Publication in The Astronomical Journal – 2 – 1. -
NGC 6535: the Lowest Mass Milky Way Globular Cluster with a Na-O Anti-Correlation??,?? Cluster Mass and Age in the Multiple Population Context
A&A 607, A44 (2017) Astronomy DOI: 10.1051/0004-6361/201731526 & c ESO 2017 Astrophysics NGC 6535: the lowest mass Milky Way globular cluster with a Na-O anti-correlation??,?? Cluster mass and age in the multiple population context A. Bragaglia1, E. Carretta1, V. D’Orazi2; 3; 4, A. Sollima1, P. Donati1, R. G. Gratton2, and S. Lucatello2 1 INAF–Osservatorio Astronomico di Bologna, via Gobetti 93/3, 40129 Bologna, Italy e-mail: [email protected] 2 INAF–Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, Italy 3 Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Melbourne, VIC 3800, Australia 4 Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109, Australia Received 7 July 2017 / Accepted 1 August 2017 ABSTRACT To understand globular clusters (GCs) we need to comprehend how their formation process was able to produce their abundance distribution of light elements. In particular, we seek to figure out which stars imprinted the peculiar chemical signature of GCs. One of the best ways is to study the light-element anti-correlations in a large sample of GCs that are analysed homogeneously. As part of our spectroscopic survey of GCs with FLAMES, we present here the results of our study of about 30 red giant member stars in the low-mass, low-metallicity Milky Way cluster NGC 6535. We measured the metallicity (finding [Fe/H] = −1:95, rms = 0.04 dex in our homogeneous scale) and other elements of the cluster and, in particular, we concentrate here on O and Na abundances. -
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. 144 — 5 December 2016 http://www.astro.keele.ac.uk/MCnews Editor: Jacco van Loon 10 5 MB 0 Y -5 -10 10 0 -10 -20 -30 XMB Figure 1: The Magellanic Bridges as traced by young main sequence stars (in red) and old RR Lyræ stars (in blue). These Gaia data release 1 results have been submitted by Belokurov et al. ( http://arxiv.org/abs/1611.04614 ) Editorial Dear Colleagues, It is my pleasure to present you the 144th issue of the Magellanic Clouds Newsletter. Please also see the announcement of Nature Astronomy if you hadn’t noticed it before. This is a newly launched journal that may be of interest to you. The next issue is planned to be distributed on the 1st of February 2017. I wish you all a Merry Christmas and a Happy New Year! Editorially Yours, Jacco van Loon 1 Refereed Journal Papers Multiple populations in the old and massive Small Magellanic Cloud globular cluster NGC 121 Emanuele Dalessandro1,2, Emilio Lapenna2, Alessio Mucciarelli2, Livia Origlia1, Francesco R. Ferraro2 and Barbara Lanzoni2 1INAF – Bologna Observatory, Italy 2Department of Physics and Astronomy – Bologna University, Italy We used a combination of optical and near-UV Hubble Space Telescope photometry and FLAMES/ESO-VLT high- resolution spectroscopy to characterize the stellar content of the old and massive globular cluster (GC) NGC 121 in the Small Magellanic Cloud (SMC). We report on the detection of multiple stellar populations, the first case in the SMC stellar cluster system.