NGC4636 - a Rich Globular Cluster System in Anormal Elliptical Galaxy 1 1 2 4 M
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Globular Clusters - Guides to Galaxies
ESO Astrophysics Symposia Globular Clusters - Guides to Galaxies Proceedings of the Joint ESO-FONDAP Workshop on Globular Clusters held in Concepción, Chile, 6-10 March 2006 Bearbeitet von Tom Richtler, Søren Larsen 1. Auflage 2008. Buch. xx, 456 S. Hardcover ISBN 978 3 540 76960 6 Format (B x L): 15,5 x 23,5 cm Gewicht: 871 g Weitere Fachgebiete > Physik, Astronomie > Angewandte Physik > Astrophysik Zu Leseprobe schnell und portofrei erhältlich bei Die Online-Fachbuchhandlung beck-shop.de ist spezialisiert auf Fachbücher, insbesondere Recht, Steuern und Wirtschaft. Im Sortiment finden Sie alle Medien (Bücher, Zeitschriften, CDs, eBooks, etc.) aller Verlage. Ergänzt wird das Programm durch Services wie Neuerscheinungsdienst oder Zusammenstellungen von Büchern zu Sonderpreisen. Der Shop führt mehr als 8 Millionen Produkte. Contents Open Questions in the Globular Cluster – Galaxy Connection Markus Kissler-Patig ............................................ 1 Part I Detailed Studies of Individual Globular Clusters Detailed Chemical Abundances of Extragalactic Globular Clusters Rebecca Bernstein, Andrew McWilliam ............................ 11 Spectroscopic Abundances and Radial Velocities of the Galactic Globular Clusters 2MASS GC01 and 2MASS GC02: Preliminary Results J. Borissova, V.D. Ivanov, A. Stephens, D. Minniti ................ 17 Abundance Anomalies in Galactic Globular Clusters – Looking for the Stellar Culprits C. Charbonnel, N. Prantzos ...................................... 21 Globular Clusters in the Direction of the Inner Galaxy J. Alonso-Garc´ıa, M. Mateo ...................................... 25 Globular Cluster Research with Astronomical Archives Carol A. Christian .............................................. 27 Super-He-Rich Populations in Globular Clusters Chul Chung, Young-Wook Lee, Suk-Jin Yoon, Seok-Joo Joo, and Sang-Il Han ................................................ 29 Testing the BH 176 and Berkeley 29 Association with GASS/Monoceros Peter M. -
198 7Apj. . .312L. .11J the Astrophysical Journal, 312:L11-L15
.11J The Astrophysical Journal, 312:L11-L15,1987 January 1 .312L. © 1987. The American Astronomical Society. All rights reserved. Printed in U.S.A. 7ApJ. 198 INTERSTELLAR DUST IN SHAPLEY-AMES ELLIPTICAL GALAXIES M. Jura and D. W. Kim Department of Astronomy, University of California, Los Angeles AND G. R. Knapp and P. Guhathakurta Princeton University Observatory Received 1986 August 11; accepted 1986 September 30 ABSTRACT We have co-added the IRAS survey data at the positions of the brightest elliptical galaxies in the Revised Shapley-Ames Catalog to increase the sensitivity over that of the IRAS Point Source Catalog. More than half of 7 8 the galaxies (with Bj< \\ mag) are detected at 100 /xm with flux levels indicating, typically, 10 or 10 M0 of cold interstellar matter. The presence of cold gas in ellipticals thus appears to be the rule rather than the exception. Subject headings: galaxies: general — infrared: sources I. INTRODUCTION infrared emission from the elliptical galaxy in the line of sight. The traditional view of early-type galaxies is that they are Our criteria for a real detection are as follows: essentially free of interstellar matter. However, with advances 1. The optical position of the galaxy and the position of the in instrumental sensitivity, it has become possible to observe IRAS source agree to better than V. (The agreement is usually 21 cm emission (Knapp, Turner, and Cunniffe 1985; Wardle much better than T.) and Knapp 1986), optical dust patches (Sadler and Gerhard 2. The flux is at least 3 times the r.m.s. noise. -
Clustering of Local Group Distances: Publication Bias Or Correlated Measurements? VI
Draft version November 12, 2019 Typeset using LATEX default style in AASTeX63 Clustering of Local Group distances: publication bias or correlated measurements? VI. Extending to Virgo cluster distances Richard de Grijs1, 2, 3 and Giuseppe Bono4, 5 1Department of Physics & Astronomy, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia 2Research Centre for Astronomy, Astrophysics & Astrophotonics, Macquarie University, Balaclava Road, Sydney, NSW 2109, Australia 3International Space Science Institute{Beijing, 1 Nanertiao, Zhongguancun, Hai Dian District, Beijing 100190, China 4Dipartimento di Fisica, Universit`adi Roma Tor Vergata, via Della Ricerca Scientifica 1, 00133, Roma, Italy 5INAF, Rome Astronomical Observatory, via Frascati 33, 00078 Monte Porzio Catone, Italy ABSTRACT We have established an internally consistent Local Group distance framework, using the Galactic Center, the Large Magellanic Cloud, and Messier 31 (M31) as important stepping stones. At greater distances, few distance benchmarks are available. As a consequence, M87 and/or Virgo cluster dis- tances are often invoked as the next rung on the ladder to more distant objects such as the Fornax and Coma clusters. Therefore, we extensively mined the published literature for independently derived distance estimates to either M87 or the center of the Virgo cluster. Based on our newly compiled, comprehensive database of 213 such distances, published between 1929 and 2017 July, we recommend M87 an outward extension to our distance framework, (m − M)0 = 31:03 ± 0:14 mag (D = 16:07 ± 1:03 Mpc; where the uncertainty represents the Gaussian σ of the distribution), based on a subset of recent (post-1990) M87/Virgo cluster distance measurements. The most stable distance tracers employed here were derived from analysis of both primary and secondary distance indicators. -
Globular Clusters and Galactic Nuclei
Scuola di Dottorato “Vito Volterra” Dottorato di Ricerca in Astronomia– XXIV ciclo Globular Clusters and Galactic Nuclei Thesis submitted to obtain the degree of Doctor of Philosophy (“Dottore di Ricerca”) in Astronomy by Alessandra Mastrobuono Battisti Program Coordinator Thesis Advisor Prof. Roberto Capuzzo Dolcetta Prof. Roberto Capuzzo Dolcetta Anno Accademico 2010-2011 ii Abstract Dynamical evolution plays a key role in shaping the current properties of star clus- ters and star cluster systems. We present the study of stellar dynamics both from a theoretical and numerical point of view. In particular we investigate this topic on different astrophysical scales, from the study of the orbital evolution and the mutual interaction of GCs in the Galactic central region to the evolution of GCs in the larger scale galactic potential. Globular Clusters (GCs), very old and massive star clusters, are ideal objects to explore many aspects of stellar dynamics and to investigate the dynamical and evolutionary mechanisms of their host galaxy. Almost every surveyed galaxy of sufficiently large mass has an associated group of GCs, i.e. a Globular Cluster System (GCS). The first part of this Thesis is devoted to the study of the evolution of GCSs in elliptical galaxies. Basing on the hypothesis that the GCS and stellar halo in a galaxy were born at the same time and, so, with the same density distribution, a logical consequence is that the presently observed difference may be due to evolution of the GCS. Actually, in this scenario, GCSs evolve due to various mechanisms, among which dynamical friction and tidal interaction with the galactic field are the most important. -
Synapses of Active Galactic Nuclei: Comparing X-Ray and Optical Classifications Using Artificial Neural Networks?
A&A 567, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201322592 & c ESO 2014 Astrophysics Synapses of active galactic nuclei: Comparing X-ray and optical classifications using artificial neural networks? O. González-Martín1;2;??, D. Díaz-González3, J. A. Acosta-Pulido1;2, J. Masegosa4, I. E. Papadakis5;6, J. M. Rodríguez-Espinosa1;2, I. Márquez4, and L. Hernández-García4 1 Instituto de Astrofísica de Canarias (IAC), C/Vía Láctea s/n, 38205 La Laguna, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna (ULL), 38205 La Laguna, Spain 3 Shidix Technologies, 38320, La Laguna, Spain 4 Instituto de Astrofísica de Andalucía, CSIC, C/ Glorieta de la Astronomía s/n, 18005 Granada, Spain 5 Physics Department, University of Crete, PO Box 2208, 710 03 Heraklion, Crete, Greece 6 IESL, Foundation for Research and Technology, 711 10 Heraklion, Crete, Greece Received 2 September 2013 / Accepted 3 April 2014 ABSTRACT Context. Many classes of active galactic nuclei (AGN) have been defined entirely through optical wavelengths, while the X-ray spectra have been very useful to investigate their inner regions. However, optical and X-ray results show many discrepancies that have not been fully understood yet. Aims. The main purpose of the present paper is to study the synapses (i.e., connections) between X-ray and optical AGN classifications. Methods. For the first time, the newly implemented efluxer task allowed us to analyse broad band X-ray spectra of a sample of emission-line nuclei without any prior spectral fitting. Our sample comprises 162 spectra observed with XMM-Newton/pn of 90 lo- cal emission line nuclei in the Palomar sample. -
00E the Construction of the Universe Symphony
The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope -
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact Information: Department of Physics & Astronomy San
Aaron J. Romanowsky Curriculum Vitae (Rev. 1 Septembert 2021) Contact information: Department of Physics & Astronomy +1-408-924-5225 (office) San Jose´ State University +1-409-924-2917 (FAX) One Washington Square [email protected] San Jose, CA 95192 U.S.A. http://www.sjsu.edu/people/aaron.romanowsky/ University of California Observatories +1-831-459-3840 (office) 1156 High Street +1-831-426-3115 (FAX) Santa Cruz, CA 95064 [email protected] U.S.A. http://www.ucolick.org/%7Eromanow/ Main research interests: galaxy formation and dynamics – dark matter – star clusters Education: Ph.D. Astronomy, Harvard University Nov. 1999 supervisor: Christopher Kochanek, “The Structure and Dynamics of Galaxies” M.A. Astronomy, Harvard University June 1996 B.S. Physics with High Honors, June 1994 College of Creative Studies, University of California, Santa Barbara Employment: Professor, Department of Physics & Astronomy, Aug. 2020 – present San Jose´ State University Associate Professor, Department of Physics & Astronomy, Aug. 2016 – Aug. 2020 San Jose´ State University Assistant Professor, Department of Physics & Astronomy, Aug. 2012 – Aug. 2016 San Jose´ State University Research Associate, University of California Observatories, Santa Cruz Oct. 2012 – present Associate Specialist, University of California Observatories, Santa Cruz July 2007 – Sep. 2012 Researcher in Astronomy, Department of Physics, Oct. 2004 – June 2007 University of Concepcion´ Visiting Adjunct Professor, Faculty of Astronomical and May 2005 Geophysical Sciences, National University of La Plata Postdoctoral Research Fellow, School of Physics and Astronomy, June 2002 – Oct. 2004 University of Nottingham Postdoctoral Fellow, Kapteyn Astronomical Institute, Oct. 1999 – May 2002 Rijksuniversiteit Groningen Research Fellow, Harvard-Smithsonian Center for Astrophysics June 1994 – Oct. -
Caldwell Catalogue - Wikipedia, the Free Encyclopedia
Caldwell catalogue - Wikipedia, the free encyclopedia Log in / create account Article Discussion Read Edit View history Caldwell catalogue From Wikipedia, the free encyclopedia Main page Contents The Caldwell Catalogue is an astronomical catalog of 109 bright star clusters, nebulae, and galaxies for observation by amateur astronomers. The list was compiled Featured content by Sir Patrick Caldwell-Moore, better known as Patrick Moore, as a complement to the Messier Catalogue. Current events The Messier Catalogue is used frequently by amateur astronomers as a list of interesting deep-sky objects for observations, but Moore noted that the list did not include Random article many of the sky's brightest deep-sky objects, including the Hyades, the Double Cluster (NGC 869 and NGC 884), and NGC 253. Moreover, Moore observed that the Donate to Wikipedia Messier Catalogue, which was compiled based on observations in the Northern Hemisphere, excluded bright deep-sky objects visible in the Southern Hemisphere such [1][2] Interaction as Omega Centauri, Centaurus A, the Jewel Box, and 47 Tucanae. He quickly compiled a list of 109 objects (to match the number of objects in the Messier [3] Help Catalogue) and published it in Sky & Telescope in December 1995. About Wikipedia Since its publication, the catalogue has grown in popularity and usage within the amateur astronomical community. Small compilation errors in the original 1995 version Community portal of the list have since been corrected. Unusually, Moore used one of his surnames to name the list, and the catalogue adopts "C" numbers to rename objects with more Recent changes common designations.[4] Contact Wikipedia As stated above, the list was compiled from objects already identified by professional astronomers and commonly observed by amateur astronomers. -
The Unusual X-Ray Morphology of NGC 4636
TheThe unusualunusual X-rayX-ray morphologymorphology ofof NGCNGC 4636:4636: cavities,cavities, off-centeroff-center outburstsoutbursts andand shocksshocks revealedrevealed byby deepdeep ChandraChandra observationsobservations AAlleessssaannddrroo BBaallddii Smithsonian Astrophysical Observatory In collaboration with: W. Forman (SAO), C. Jones (SAO), P. Nulsen (SAO), R. Kraft (SAO), L. David (SAO), E. Churazov (MPA-Garching) NGCNGC 46364636 •One of the most X-ray luminous ‘normal’ elliptical galaxies: LX ~ 2 x 1041 ergs s-1 •Located in the outskirts of the Virgo Cluster, at a distance of 15 Mpc Optical Soft X-rays (Tonry et al. 2001) •Already studied in the X-ray wavelengths by Chandra & XMM- Newton (e.g. Jones et al. 2002, O’ Sullivan et al. 2005) Radio contours X-ray Optical Radio Eight Years of Science with Chandra - Huntsville, AL Oct 23-25 2007 ChandraChandra datadata preparationpreparation • ACIS-I (2 observations: 150 ks) and ACIS-S (1 observation: 52 ks) data reprocessed with CIAO 3.4 applying: • Newest ACIS gain maps • Time-dependent ACIS gain correction • ACIS CTI correction, etc. • Removal of high background flaring period: • ACIS-I: Tclean = 149 ks • ACIS-S: Tclean = 37 ks Eight Years of Science with Chandra - Huntsville, AL Oct 23-25 2007 NGCNGC 46364636:: globalglobal X-rayX-ray propertiesproperties •The temperature profile shows Temperature evidence of a cooling core; several substructures are detected as well. •The density and pressure profiles show a strong central peak and a ‘plateau’ located at 2 kpc < r < 4.5 kpc from -
ALABAMA University Libraries
THE UNIVERSITY OF ALABAMA University Libraries The X-Ray-Faint Early-Type Galaxy NGC 4697 Jimmy A. Irwin – University of Michigan Craig L. Sarazin – University of Virginia Joel N. Bregman – University of Michigan Deposited 09/14/2018 Citation of published version: Irwin, J., Sarazin, C., Bregman, J. (2000): The X-Ray-Faint Early-Type Galaxy NGC 4697. The Astrophysical Journal Letters, 544(2). DOI: 10.1086/317196 © 2000. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE ASTROPHYSICAL JOURNAL, 544:293È301, 2000 November 20 ( 2000. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE X-RAYÈFAINT EARLY-TYPE GALAXY NGC 4697 JIMMY A. IRWIN,1,2 CRAIG L. SARAZIN,3 AND JOEL N. BREGMAN1 Received 2000 March 7; accepted 2000 June 27 ABSTRACT We analyze archival ROSAT HRI, ROSAT PSPC, and ASCA data of the X-rayÈfaint early-type galaxy NGC 4697. The joint ROSAT PSPC]ASCA spectrum is Ðtted by a two-component thermal model, a MEKAL model withkT \ 0.26`0.04 keV with low metallicity and a bremsstrahlung \ `3.0 MEKAL ~0.03 model withkTBREM 5.2~1.6 keV. A similar model was found to Ðt the spectra of another faint early- type galaxy (NGC 4382) and the bulge of M31. We interpret this soft emission as a combination of emission from a soft component of low-mass X-ray binaries (LMXBs) and from a low-temperature inter- stellar medium, although the relative contributions of the two components could not be determined. Twelve point sources were identiÐed within 4@ of NGC 4697, of which 11 are most likely LMXBs associ- ated with the galaxy. -
MIPS 24160 M Photometry for the Herschelspire Local Galaxies
Mon. Not. R. Astron. Soc. 423, 197–212 (2012) doi:10.1111/j.1365-2966.2012.20784.x MIPS 24–160 µm photometry for the Herschel-SPIRE Local Galaxies Guaranteed Time Programs G. J. Bendo,1,2 F. Galliano3 andS.C.Madden3 1UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL 2Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2AZ 3Laboratoire AIM, CEA, Universite´ Paris Diderot, IRFU/Service d’Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France Accepted 2012 February 20. Received 2012 January 23; in original form 2011 November 14 ABSTRACT We provide an overview of ancillary 24-, 70- and 160-µm data from the Multiband Imaging Photometer for Spitzer (MIPS) that are intended to complement the 70–500 µm Herschel Space Observatory photometry data for nearby galaxies obtained by the Herschel-SPIRE Local Galaxies Guaranteed Time Programs and the Herschel Virgo Cluster Survey. The MIPS data can be used to extend the photometry to wavebands that are not observed in these Herschel surveys and to check the photometry in cases where Herschel performs observations at the same wavelengths. Additionally, we measured globally integrated 24–160 µm flux densities for the galaxies in the sample that can be used for the construction of spectral energy distributions. Using MIPS photometry published by other references, we have confirmed that we are obtaining accurate photometry for these galaxies. Key words: catalogues – galaxies: photometry – infrared: galaxies. (SEDs) of the dust emission and to map the distribution of cold 1 INTRODUCTION dust within these galaxies. -
The Caldwell Catalogue+Photos
The Caldwell Catalogue was compiled in 1995 by Sir Patrick Moore. He has said he started it for fun because he had some spare time after finishing writing up his latest observations of Mars. He looked at some nebulae, including the ones Charles Messier had not listed in his catalogue. Messier was only interested in listing those objects which he thought could be confused for the comets, he also only listed objects viewable from where he observed from in the Northern hemisphere. Moore's catalogue extends into the Southern hemisphere. Having completed it in a few hours, he sent it off to the Sky & Telescope magazine thinking it would amuse them. They published it in December 1995. Since then, the list has grown in popularity and use throughout the amateur astronomy community. Obviously Moore couldn't use 'M' as a prefix for the objects, so seeing as his surname is actually Caldwell-Moore he used C, and thus also known as the Caldwell catalogue. http://www.12dstring.me.uk/caldwelllistform.php Caldwell NGC Type Distance Apparent Picture Number Number Magnitude C1 NGC 188 Open Cluster 4.8 kly +8.1 C2 NGC 40 Planetary Nebula 3.5 kly +11.4 C3 NGC 4236 Galaxy 7000 kly +9.7 C4 NGC 7023 Open Cluster 1.4 kly +7.0 C5 NGC 0 Galaxy 13000 kly +9.2 C6 NGC 6543 Planetary Nebula 3 kly +8.1 C7 NGC 2403 Galaxy 14000 kly +8.4 C8 NGC 559 Open Cluster 3.7 kly +9.5 C9 NGC 0 Nebula 2.8 kly +0.0 C10 NGC 663 Open Cluster 7.2 kly +7.1 C11 NGC 7635 Nebula 7.1 kly +11.0 C12 NGC 6946 Galaxy 18000 kly +8.9 C13 NGC 457 Open Cluster 9 kly +6.4 C14 NGC 869 Open Cluster