Stellar Populations of Early-Type Galaxies in Different Environments II
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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.................. -
Arxiv:2001.00331V2 [Astro-Ph.GA] 27 Feb 2020 Et Al
Draft version February 28, 2020 Typeset using LATEX twocolumn style in AASTeX62 The Carnegie-Irvine Galaxy Survey. IX. Classification of Bulge Types and Statistical Properties of Pseudo Bulges Hua Gao (高f),1, 2 Luis C. Ho,2, 1 Aaron J. Barth,3 and Zhao-Yu Li4 1Department of Astronomy, School of Physics, Peking University, Beijing 100871, China 2Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, China 3Department of Physics and Astronomy, University of California at Irvine, 4129 Frederick Reines Hall, Irvine, CA 92697-4575, USA 4Department of Astronomy, Shanghai Jiao Tong University, Shanghai 200240, China ABSTRACT We study the statistical properties of 320 bulges of disk galaxies in the Carnegie-Irvine Galaxy Survey, using robust structural parameters of galaxies derived from image fitting. We apply the Kormendy relation to classify classical and pseudo bulges and characterize bulge dichotomy with respect to bulge structural properties and physical properties of host galaxies. We confirm previous findings that pseudo bulges on average have smaller S´ersic indices, smaller bulge-to-total ratios, and fainter surface brightnesses when compared with classical bulges. Our sizable sample statistically shows that pseudo bulges are more intrinsically flattened than classical bulges. Pseudo bulges are most frequent (incidence & 80%) in late-type spirals (later than Sc). Our measurements support the picture in which pseudo bulges arose from star formation induced by inflowing gas, while classical bulges were born out of violent processes such as mergers and coalescence of clumps. We reveal differences with the literature that warrant attention: (1) the bimodal distribution of S´ersicindices presented by previous studies is not reproduced in our study; (2) classical and pseudo bulges have similar relative bulge sizes; and (3) the pseudo bulge fraction is considerably smaller in early-type disks compared with previous studies based on one-dimensional surface brightness profile fitting. -
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. -
Arxiv:Astro-Ph/9906499V1 30 Jun 1999
to appear in AJ Globular Cluster Systems I: V − I Color Distributions Karl Gebhardt 1,3 University of California Observatories / Lick Observatory, University of California, Santa Cruz, CA 95064 Electronic mail: [email protected] Markus Kissler-Patig 2 European Southern Observatory, Karl–Schwarzschild–Str. 2, 85748 Garching, Germany University of California Observatories / Lick Observatory, University of California, Santa Cruz, CA 95064 Electronic mail: [email protected] ABSTRACT We have compiled data for the globular cluster systems of 50 galaxies from the HST WFPC2 archive, of which 43 are type S0 or earlier. In this paper, we present the data set and derive the V − I color distributions. We derive the first four moments of the color distributions, as well as a measure for their non–unimodality. The number of globular clusters in each galaxy ranges from 18 (in NGC 2778) to 781 (NGC 5846). For those systems having more than 100 clusters, seven of sixteen (44%) show significant bimodality. Overall, roughly half of all the systems in our sample show hints of a bimodal color distribution. In general, the distributions of the faint galaxies are consistent with unimodality, whereas those of the brighter galaxies are not. We also find a number of systems with narrow color distributions—with both mean red and arXiv:astro-ph/9906499v1 30 Jun 1999 blue colors—suggesting that systems exist with only metal–rich or only metal–poor globular clusters. We discuss their possible origins. In comparing the moments of the V − I distributions with various -
1985Apjs ... 59 ...IW the Astrophysical Journal Supplement Series, 59:1-21,1985 September © 1985. the American Astronomical S
IW The Astrophysical Journal Supplement Series, 59:1-21,1985 September .... © 1985. The American Astronomical Society. All rights reserved. Printed in U.S.A. 59 ... A CATALOG OF STELLAR VELOCITY DISPERSIONS. I. 1985ApJS COMPILATION AND STANDARD GALAXIES Bradley C. Whitmore Space Telescope Science Institute Douglas B. McElroy Computer Sciences Corporation1 AND John L. Tonry California Institute of Technology Received 1984 October 23; accepted 1985 February 19 ABSTRACT A catalog of central stellar velocity dispersion measurements is presented, current through 1984 June. The catalog includes 1096 measurements of 725 galaxies. A set of 51 standard galaxies is defined which consists of galaxies with at least three reliable, concordant measurements. We suggest that future studies observe some of these standard galaxies in the course of their observations so that different studies can be normalized to the same system. We compare previous studies with the derived standards to determine relative accuracies and to compute scale factors where necessary. Subject headings: galaxies: internal motions I. INTRODUCTION be flattened by rotation. Results from Whitmore, Rubin, and The ability to make accurate measurements of stellar veloc- Ford (1984) conflict with the Kormendy and Illingworth con- ity dispersions has provided a major catalyst for the study of clusion. galactic structure and dynamics. Several important discoveries While most dispersion profiles are either flat or falling, have resulted from the use of this new tool. For example, a studies of cD galaxies at the center of rich clusters of galaxies correlation between the luminosity of an elliptical galaxy and have shown rising dispersion profiles (Dressier 1979; Carter the central stellar velocity dispersion was discovered by Faber et al 1981). -
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. -
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A&A 439, 487–496 (2005) Astronomy DOI: 10.1051/0004-6361:20042529 & c ESO 2005 Astrophysics Are radio galaxies and quiescent galaxies different? Results from the analysis of HST brightness profiles, H. R. de Ruiter1,2,P.Parma2, A. Capetti3,R.Fanti4,2, R. Morganti5, and L. Santantonio6 1 INAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, Italy 2 INAF – Istituto di Radioastronomia, via Gobetti 101, 40129 Bologna, Italy 3 INAF – Osservatorio Astronomico di Torino, Strada Osservatorio 25, 10025 Pino Torinese, Italy 4 Istituto di Fisica, Università degli Studi di Bologna, via Irnerio 46, 40126 Bologna, Italy 5 Netherlands Foundation for Research in Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands 6 Università degli Studi di Torino, via Giuria 1, 10125 Torino, Italy Received 14 December 2004 / Accepted 12 April 2005 Abstract. We present a study of the optical brightness profiles of early type galaxies, using a number of samples of radio galax- ies and optically selected elliptical galaxies. For the radio galaxy samples – B2 of Fanaroff-Riley type I and 3C of Fanaroff-Riley type II – we determined a number of parameters that describe a “Nuker-law” profile, which were compared with those already known for the optically selected objects. We find that radio active galaxies are always of the “core” type (i.e. an inner Nuker law slope γ<0.3). However, there are core-type galaxies which harbor no significant radio source and which are indistinguishable from the radio active galaxies. We do not find any radio detected galaxy with a power law profile (γ>0.5). -
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, -
Exploring the Star Formation History of Elliptical Galaxies Rogers, Ben; Ferreras, Ignacio; Peletier, Reynier F.; Silk, Joseph
University of Groningen Exploring the Star Formation History of Elliptical Galaxies Rogers, Ben; Ferreras, Ignacio; Peletier, Reynier F.; Silk, Joseph Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1111/j.1365-2966.2009.15892.x IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2010 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Rogers, B., Ferreras, I., Peletier, R. F., & Silk, J. (2010). Exploring the Star Formation History of Elliptical Galaxies: Beyond Simple Stellar Populations with a New Estimator of Line Strengths. Monthly Notices of the Royal Astronomical Society, 402(1), 447-460. https://doi.org/10.1111/j.1365-2966.2009.15892.x Copyright Other than for strictly personal use, 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), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment. Take-down policy If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
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 -
Arxiv:Astro-Ph/0702572V1 21 Feb 2007 O.Nt .Ato.Soc
Mon. Not. R. Astron. Soc. 000, 1–?? (2006) Printed 22 February 2007 (MN LATEX style file v2.2) Spatially resolved spectroscopy of early-type galaxies over a range in mass Patricia S´anchez–Bl´azquez1,2,3⋆ Duncan A. Forbes,3 Jay Strader,4 Jean Brodie,4 Robert Proctor3 ⋆† 1University of Central Lancashire, Centre for Astrophysics, Preston, PR1 2HE, UK 2Laboratoire d’Astrophysique, Ecole´ Polytechnique F´ed´erale de Lausanne (EPFL),Observatoire, 1290 Sauverny, Switzerland 3Center for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Australia 4UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA Accepted ??? December 15. Received ??? December 14; ABSTRACT Long-slit spectra have been obtained with the Keck telescope for a sample of 11 early-type galaxies covering a wide range in luminosity and hence mass. Rotation velocity and velocity dispersions, together with 19 Lick line-strength gradients have been measured, to, on average, two effective radii. Stellar population models taking into account the effect of the non-solar chemical composition have been used to derive ages, metallicities and α/Fe abundances along the radius. We find that line-strength gradients are due, mainly, to variations of the total metallicity with the radius. One galaxy out of 11 shows very strong age gradients, with a young central component, while the age gradient for the rest of the sample is very shallow or consistent with zero. We also find small variations in the [α/Fe] ratio with radius. Contrary to what is expected in simple collapse models, galaxies show both positive and negative [α/Fe] profiles.