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Distribuição De Matéria De Sistemas Estelares Esferoidais: Propriedades Dinâmicas, Intrínsecas E Observáveis
Universidade Federal do Rio Grande - FURG Instituto de Matemática, Estatística e Física - IMEF Grupo de Astrofísica Teórica e Computacional - GATC Distribuição de Matéria de Sistemas Estelares Esferoidais: Propriedades Dinâmicas, Intrínsecas e Observáveis. Graciana Brum João Rio GrandeRS, 7 de novembro de 2013 Universidade Federal do Rio Grande - FURG Instituto de Matemática, Estatística e Física - IMEF Grupo de Astrofísica Teórica e Computacional - GATC Distribuição de Matéria de Sistemas Estelares Esferoidais: Propriedades Dinâmicas, Intrínsecas e Observáveis. Discente: Graciana Brum João Orientador: Prof. Dr. Fabricio Ferrari Trabalho de Conclusão de Curso apresentado ao curso de Física Bacharelado da Universidade Federal do Rio Grande como requisito parcial para obtenção do tíitulo de bacharel em Física. Rio Grande RS, 7 de novembro de 2013 Sumário 1 Introdução. 4 1.1 Galáxias..........................................5 1.1.1 Galáxias Espirais.................................6 1.1.2 Galáxias Espirais Barradas............................6 1.1.3 Galáxias Irregulares................................7 1.1.4 Galáxias Elípticas.................................7 1.2 Pers de Brilho......................................7 1.3 Fotometria e Massa....................................9 1.3.1 Relação Massa-Luminosidade........................... 11 1.3.2 Distribuição de Brilho supercial......................... 11 1.4 Dinâmica de Galáxias................................... 11 2 Teoria Potencial 13 2.1 Propriedades Dinâmicas, Intrínsecas e Observáveis.................. -
The Cheshire Cat Gravitational Lens: the Formation of a Massive Fossil Group
THE UNIVERSITY OF ALABAMA University Libraries The Cheshire Cat Gravitational Lens: The Formation of a Massive Fossil Group Jimmy A. Irwin – University of Alabama et al. Deposited 09/10/2018 Citation of published version: Irwin, J., et al. (2015): The Cheshire Cat Gravitational Lens: The Formation of a Massive Fossil Group. The Astrophysical Journal, 806(2). http://dx.doi.org/10.1088/0004- 637X/806/2/268 © 2015. The American Astronomical Society. All rights reserved. The Astrophysical Journal, 806:268 (14pp), 2015 June 20 doi:10.1088/0004-637X/806/2/268 © 2015. The American Astronomical Society. All rights reserved. THE CHESHIRE CAT GRAVITATIONAL LENS: THE FORMATION OF A MASSIVE FOSSIL GROUP Jimmy A. Irwin1, Renato Dupke1,2,3,4, Eleazar R. Carrasco5, W. Peter Maksym1, Lucas Johnson1, and Raymond E. White III1 1 Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487, USA; [email protected] 2 Department of Astronomy, University of Michigan, 500 Church St., Ann Arbor, MI 48109, USA 3 Observatório Nacional, Rua Gal. José Cristino 77, São Cristóvão, CEP20921-400 Rio de Janeiro RJ, Brazil 4 Eureka Scientific Inc., 2452 Delmer St. Suite 100, Oakland, CA 94602, USA 5 Gemini Observatory/AURA, Southern Operations Center, AURA, Casilla 603, La Serena, Chile Received 2014 July 4; accepted 2015 April 28; published 2015 June 23 ABSTRACT The Cheshire Cat is a relatively poor group of galaxies dominated by two luminous elliptical galaxies surrounded by at least four arcs from gravitationally lensed background galaxies that give the system a humorous appearance. Our combined optical/X-ray study of this system reveals that it is experiencing a line of sight merger between two groups with a roughly equal mass ratio with a relative velocity of ∼1350 km s−1. -
Copyright by Marcel Peter Bergmann 2002 the Dissertation Committee for Marcel Peter Bergmann Certifies That This Is the Approved Version of the Following Dissertation
Copyright by Marcel Peter Bergmann 2002 The Dissertation Committee for Marcel Peter Bergmann certifies that this is the approved version of the following dissertation: Galaxy Evolution: The Relationship Between Structure, Star Formation, and Environment Committee: Gary Hill, Supervisor J. Craig Wheeler, Supervisor Inger Jørgensen Karl Gebhardt Chris Sneden Ralf Bender Galaxy Evolution: The Relationship Between Structure, Star Formation, and Environment by Marcel Peter Bergmann, B.S., M.A. DISSERTATION Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of DOCTOR OF PHILOSOPHY THE UNIVERSITY OF TEXAS AT AUSTIN December 2002 Dedicated to Peter, Margot, Marianne, and Ernest Bergmann who taught me the equal importance of hard work and creativity in science, and in life. Acknowledgments I enjoyed my time during grad school, and have many people to thank. First and foremost, I am deeply grateful to my advisors Inger Jørgensen and Gary Hill for mentoring me in the ways of research and the forging of a scientific career. Their never-wavering support was invaluable as I struggled through the process of writing papers and this dissertation. I would also like to thank Craig Wheeler, my faculty supervisor, for many good suggestions regarding writing and the job hunt. Karl Gebhardt, though not formally one of my supervisors, has been a great teacher and collaborator since his arrival in Texas two years ago. I look forward to many years of continued collaboration with all of these great scientists. I also discovered during graduate school that I am a social person, and rely greatly on social interaction with others to maintain my spirit and sanity. -
Revealing Hidden Substructures in the $ M {BH} $-$\Sigma $ Diagram
Draft version November 14, 2019 A Typeset using L TEX twocolumn style in AASTeX63 Revealing Hidden Substructures in the MBH –σ Diagram, and Refining the Bend in the L–σ Relation Nandini Sahu,1,2 Alister W. Graham2 And Benjamin L. Davis2 — 1OzGrav-Swinburne, Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia 2Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia (Accepted 2019 October 22, by The Astrophysical Journal) ABSTRACT Using 145 early- and late-type galaxies (ETGs and LTGs) with directly-measured super-massive black hole masses, MBH , we build upon our previous discoveries that: (i) LTGs, most of which have been 2.16±0.32 alleged to contain a pseudobulge, follow the relation MBH ∝ M∗,sph ; and (ii) the ETG relation 1.27±0.07 1.9±0.2 MBH ∝ M∗,sph is an artifact of ETGs with/without disks following parallel MBH ∝ M∗,sph relations which are offset by an order of magnitude in the MBH -direction. Here, we searched for substructure in the MBH –(central velocity dispersion, σ) diagram using our recently published, multi- component, galaxy decompositions; investigating divisions based on the presence of a depleted stellar core (major dry-merger), a disk (minor wet/dry-merger, gas accretion), or a bar (evolved unstable 5.75±0.34 disk). The S´ersic and core-S´ersic galaxies define two distinct relations: MBH ∝ σ and MBH ∝ 8.64±1.10 σ , with ∆rms|BH = 0.55 and 0.46 dex, respectively. We also report on the consistency with the slopes and bends in the galaxy luminosity (L)–σ relation due to S´ersic and core-S´ersic ETGs, and LTGs which all have S´ersic light-profiles. -
VERGINE (Virgo) Aspetto, Posizione, Composizione
VERGINE (virgo) Aspetto, posizione, composizione. Questa nota costellazione è la seconda più grande. Al suo interno gli antichi di Roma identificavano Astrea, la divinità della giustizia, a cui veniva associata la vicina costellazione della bilancia. La costellazione zodiacale viene attraversata dal Sole durante il 23 settembre. Al suo interno troviamo un interessante ammasso di galassie, questi si estendono fino ala Coma Berenices. Questo ammasso dista circa 65 milioni di a.l. e ospita fino a 3000 galassie. alfa Virginis (Spica), mag. 1.0, è una stella bianco-azzurra distante 260 a.l. È una binaria a eclissi che varia di circo 1/10 di magnitudine con un periodo di 4 giorni. beta Vir, mag. 3.6, una stella gialla distante 33 a.l. gamma Vir (Porrima), distante 36 a.l., è una celebre stella doppia. Nel suo insieme appare come una stella di mag. 2.8, ma con un piccolo telescopio sono visibili le due componenti bianco-gialle, entrambe di mag. 3.6, che orbitano l’una intorno all’altra con un periodo di 172 anni. Attualmente si stanno avvicinando; intorno al 2000 per separarle ci vorrà un telescopio da 75 mm; intorno al 2008 saranno troppo vicine per poter essere separate con un telescopio per dilettanti. delta Vir, mag. 3.4, è una gigante rossa distante 180 a.l. epsilon Vir (Vindemiatrix), mag. 2.8, è una gigante gialla distante 100 a.l. theta Vir, distante 140 a.l., è una stella doppia, visibile con un piccolo telescopio, con componenti bianco-azzurre di mag. 4.4 e 8.6. -
X-Ray Luminosities for a Magnitude-Limited Sample of Early-Type Galaxies from the ROSAT All-Sky Survey
Mon. Not. R. Astron. Soc. 302, 209±221 (1999) X-ray luminosities for a magnitude-limited sample of early-type galaxies from the ROSAT All-Sky Survey J. Beuing,1* S. DoÈbereiner,2 H. BoÈhringer2 and R. Bender1 1UniversitaÈts-Sternwarte MuÈnchen, Scheinerstrasse 1, D-81679 MuÈnchen, Germany 2Max-Planck-Institut fuÈr Extraterrestrische Physik, D-85740 Garching bei MuÈnchen, Germany Accepted 1998 August 3. Received 1998 June 1; in original form 1997 December 30 Downloaded from https://academic.oup.com/mnras/article/302/2/209/968033 by guest on 30 September 2021 ABSTRACT For a magnitude-limited optical sample (BT # 13:5 mag) of early-type galaxies, we have derived X-ray luminosities from the ROSATAll-Sky Survey. The results are 101 detections and 192 useful upper limits in the range from 1036 to 1044 erg s1. For most of the galaxies no X-ray data have been available until now. On the basis of this sample with its full sky coverage, we ®nd no galaxy with an unusually low ¯ux from discrete emitters. Below log LB < 9:2L( the X-ray emission is compatible with being entirely due to discrete sources. Above log LB < 11:2L( no galaxy with only discrete emission is found. We further con®rm earlier ®ndings that Lx is strongly correlated with LB. Over the entire data range the slope is found to be 2:23 60:12. We also ®nd a luminosity dependence of this correlation. Below 1 log Lx 40:5 erg s it is consistent with a slope of 1, as expected from discrete emission. -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
X-Ray Constraints on the Local Supermassive Black Hole
Draft version November 11, 2018 A Preprint typeset using LTEX style emulateapj v. 5/2/11 X-RAY CONSTRAINTS ON THE LOCAL SUPERMASSIVE BLACK HOLE OCCUPATION FRACTION Brendan P. Miller,1,2 Elena Gallo,1 Jenny E. Greene,3 Brandon C. Kelly,4 Tommaso Treu,4 Jong-Hak Woo5, & Vivienne Baldassare1 Draft version November 11, 2018 ABSTRACT Distinct seed formation mechanisms are imprinted upon the fraction of dwarf galaxies currently containing a central supermassive black hole. Seeding by Pop III remnants is expected to produce a higher occupation fraction than is generated with direct gas collapse precursors. Chandra observations of nearby early-type galaxies can directly detect even low-level supermassive black hole activity, and the active fraction immediately provides a firm lower limit to the occupation fraction. Here, we use the volume-limited AMUSE surveys of ∼200 optically-selected early-type galaxies to characterize simultaneously, for the first time, the occupation fraction and the scaling of LX with Mstar, accounting for intrinsic scatter, measurement uncertainties, and X-ray limits. For early-type galaxies with Mstar < 10 10 M⊙, we obtain a lower limit to the occupation fraction of >20% (at 95% confidence), but full occupation cannot be excluded. The preferred dependence of log LX upon log Mstar has a slope of ∼0.7–0.8, consistent with the “downsizing” trend previously identified from the AMUSE dataset, and a uniform Eddington efficiency is disfavored at ∼2σ. We provide guidelines for the future precision with which these parameters may be refined with larger or more sensitive samples. Subject headings: black hole physics — galaxies: nuclei 1. -
Facultad De Ciencias Atronomicas Y Geofisicas
Universidad Nacional de La Plata Facultad de ciencias Atronomicas y Geofisicas Tesis Doctoral Estudio de enanas ultra-compactas y c´umulos globulares en el c´umulo de Antlia Juan Pablo CASO Tesis presentada para optar por el t´ıtulo de Doctor en Astronom´ıa 3 de diciembre de 2015 Directora: Dra. Lilia Bassino (Universidad Nacional de La Plata) Co-Director: Dr. Thomas Richtler (Universidad de Concepci´on, Chile) Agradecimientos A mi familia, quienes siempre me apoyaron desde que decid´ıestudiar esta carrera, y en especial a mis padres, que han sido el motor de todos mis logros. A mis amigos, que han hecho el camino m´as ameno, compartiedo infinidad de momentos. A Lilia y Tom, por ense˜narme, y guiarme en mi Doctorado. Su ejemplo y dedicaci´on fueron fundamentales para que haya podido llegar hasta aqu´ı. v UNIVERSIDAD NACIONAL DE LA PLATA Facultad de Ciencias Astron´omicas y Geof´ısicas Resumen Estudio de enanas ultra-compactas y c´umulos globulares en el c´umulo de Antlia por Juan Pablo Caso En la presente Tesis se intenta aportar evidencias que ayuden a dilucidar el origen de las enanas ultra-compactas (UCDs). Las mismas fueron descu- biertas hace poco m´as de una d´ecada, y presentan propiedades que podr´ıan relacionarlas tanto con los c´umulos globulares (CGs), como con galaxias de baja masa. Esto ha resultado en un abanico de hip´otesis sobre su origen, que incluyen ser los miembros m´as brillantes de los sistemas de CGs, los resultantes de la fusi´on de varios c´umulos estelares masivos durante eventos de formaci´on estelar particularmente intensos, o los remanentes de galaxias enanas nucleadas, desmembradas por las fuerzas tidales de galaxias vecinas masivas. -
Globular Cluster System Erosion in Elliptical Galaxies
A&A 507, 183–193 (2009) Astronomy DOI: 10.1051/0004-6361/200912255 & c ESO 2009 Astrophysics Globular cluster system erosion in elliptical galaxies R. Capuzzo-Dolcetta and A. Mastrobuono-Battisti Dep. of Physics, Sapienza, University of Roma, P.le A. Moro 5, 00185, Roma, Italy e-mail: [roberto.capuzzodolcetta;alessandra.mastrobuonobattisti]@uniroma1.it Received 2 April 2009 / Accepted 5 August 2009 ABSTRACT Context. We analyse data of 8 elliptical galaxies to study the difference between the radial distributions of their globular cluster systems (GCSs) and their galactic stellar component. In all galaxies studied, the GCS density profile is significantly flatter towards the galactic centre than that of the stars. Aims. A flatter profile of the radial distribution of the GCS with respect to that of the galactic stellar component is a difference with astrophysical relevance. A quantitative comparative analysis of the profiles may provide insight into both galaxy and globular cluster formation and evolution. If the difference is caused by erosion of the GCS, the missing GCs in the galactic central region may have merged around the galactic centre and formed, or at least increased in mass, the galactic nucleus. Observational support to this are the correlations between the galaxy integrated absolute magnitude and the number of globular clusters lost and that between the central massive black hole mass and the total mass of globular clusters lost. Methods. We fitted both the stellar and globular cluster system radial profiles of a set of galaxies observed at high resolution. We found that the GCS profile is less sharply peaked at the galactic centre than the stellar one. -
190 Index of Names
Index of names Ancora Leonis 389 NGC 3664, Arp 005 Andriscus Centauri 879 IC 3290 Anemodes Ceti 85 NGC 0864 Name CMG Identification Angelica Canum Venaticorum 659 NGC 5377 Accola Leonis 367 NGC 3489 Angulatus Ursae Majoris 247 NGC 2654 Acer Leonis 411 NGC 3832 Angulosus Virginis 450 NGC 4123, Mrk 1466 Acritobrachius Camelopardalis 833 IC 0356, Arp 213 Angusticlavia Ceti 102 NGC 1032 Actenista Apodis 891 IC 4633 Anomalus Piscis 804 NGC 7603, Arp 092, Mrk 0530 Actuosus Arietis 95 NGC 0972 Ansatus Antliae 303 NGC 3084 Aculeatus Canum Venaticorum 460 NGC 4183 Antarctica Mensae 865 IC 2051 Aculeus Piscium 9 NGC 0100 Antenna Australis Corvi 437 NGC 4039, Caldwell 61, Antennae, Arp 244 Acutifolium Canum Venaticorum 650 NGC 5297 Antenna Borealis Corvi 436 NGC 4038, Caldwell 60, Antennae, Arp 244 Adelus Ursae Majoris 668 NGC 5473 Anthemodes Cassiopeiae 34 NGC 0278 Adversus Comae Berenices 484 NGC 4298 Anticampe Centauri 550 NGC 4622 Aeluropus Lyncis 231 NGC 2445, Arp 143 Antirrhopus Virginis 532 NGC 4550 Aeola Canum Venaticorum 469 NGC 4220 Anulifera Carinae 226 NGC 2381 Aequanimus Draconis 705 NGC 5905 Anulus Grahamianus Volantis 955 ESO 034-IG011, AM0644-741, Graham's Ring Aequilibrata Eridani 122 NGC 1172 Aphenges Virginis 654 NGC 5334, IC 4338 Affinis Canum Venaticorum 449 NGC 4111 Apostrophus Fornac 159 NGC 1406 Agiton Aquarii 812 NGC 7721 Aquilops Gruis 911 IC 5267 Aglaea Comae Berenices 489 NGC 4314 Araneosus Camelopardalis 223 NGC 2336 Agrius Virginis 975 MCG -01-30-033, Arp 248, Wild's Triplet Aratrum Leonis 323 NGC 3239, Arp 263 Ahenea -
GALEX UV COLOR RELATIONS for NEARBY EARLY-TYPE GALAXIES Jose´ Donas,1 Jean-Michel Deharveng,1 R
The Astrophysical Journal Supplement Series, 173:597Y606, 2007 December # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALEX UV COLOR RELATIONS FOR NEARBY EARLY-TYPE GALAXIES Jose´ Donas,1 Jean-Michel Deharveng,1 R. Michael Rich,2 Sukyoung K. Yi,3 Young-Wook Lee,3 Alessandro Boselli,1 Armando Gil de Paz,4 Samuel Boissier,1 Ste´phane Charlot,5 Samir Salim,2 Luciana Bianchi,6 Tom A. Barlow,7 Karl Forster,7 Peter G. Friedman,7 Timothy M. Heckman,8 Barry F. Madore,9 D. Christopher Martin,7 Bruno Milliard,1 Patrick Morrissey,7 Susan G. Neff,10 David Schiminovich,11 Mark Seibert,7 Todd Small,7 Alex S. Szalay,8 Barry Y. Welsh,12 and Ted K. Wyder7 Received 2006 May 4; accepted 2006 July 20 ABSTRACT We use GALEX/optical photometry to construct color-color relationships for early-type galaxies sorted by mor- phological type. We have matched objects in the GALEX GR1 public release and the first IR1.1 internal release, with the RC3 early-type galaxies having a morphological type À5:5 T < À1:5, with mean error on T < 1:5 and mean error on (B À V )T < 0:05. After visual inspection of each match, we are left with 130 galaxies with reliable GALEX pipeline photometry in the far-UVand near-UV bands. This sample is divided into ellipticals (À5:5 T < À3:5) and lenticulars (À3:5 T < À1:5). After correction for Galactic extinction, the color-color diagrams FUV À NUV versus (B À V )Tc are plotted for the two subsamples.