Structure, Properties and Formation Histories of S0 Galaxies
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Stellar Tidal Streams As Cosmological Diagnostics: Comparing Data and Simulations at Low Galactic Scales
RUPRECHT-KARLS-UNIVERSITÄT HEIDELBERG DOCTORAL THESIS Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Author: Referees: Gustavo MORALES Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL Astronomisches Rechen-Institut Heidelberg Graduate School of Fundamental Physics Department of Physics and Astronomy 14th May, 2018 ii DISSERTATION submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg, Germany for the degree of DOCTOR OF NATURAL SCIENCES Put forward by GUSTAVO MORALES born in Copiapo ORAL EXAMINATION ON JULY 26, 2018 iii Stellar Tidal Streams as Cosmological Diagnostics: Comparing data and simulations at low galactic scales Referees: Prof. Dr. Eva K. GREBEL Prof. Dr. Volker SPRINGEL iv NOTE: Some parts of the written contents of this thesis have been adapted from a paper submitted as a co-authored scientific publication to the Astronomy & Astrophysics Journal: Morales et al. (2018). v NOTE: Some parts of this thesis have been adapted from a paper accepted for publi- cation in the Astronomy & Astrophysics Journal: Morales, G. et al. (2018). “Systematic search for tidal features around nearby galaxies: I. Enhanced SDSS imaging of the Local Volume". arXiv:1804.03330. DOI: 10.1051/0004-6361/201732271 vii Abstract In hierarchical models of galaxy formation, stellar tidal streams are expected around most galaxies. Although these features may provide useful diagnostics of the LCDM model, their observational properties remain poorly constrained. Statistical analysis of the counts and properties of such features is of interest for a direct comparison against results from numeri- cal simulations. In this work, we aim to study systematically the frequency of occurrence and other observational properties of tidal features around nearby galaxies. -
THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B
The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M . -
Reddening Map and Recent Star Formation in the Magellanic Clouds with the Earlier Studies (E.G., Besla Et Al
Astronomy & Astrophysics manuscript no. joshi c ESO 2019 June 19, 2019 Reddening map and recent star formation in the Magellanic Clouds based on OGLE IV Cepheids Y. C. Joshi1⋆⋆⋆, A. Panchal1 1Aryabhatta Research Institute of Observational Sciences (ARIES), Manora peak, Nainital 263002, India Received: 05 November 2018; accepted 11 June 2019 Abstract Context. The reddening maps of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) are constructed using the Cepheid Period-Luminosity (P-L) relations. Aims. We examine reddening distribution across the LMC and SMC through largest data on Classical Cepheids provided by the OGLE Phase IV survey. We also investigate the age and spatio-temporal distributions of Cepheids to understand the recent star formation history in the LMC and SMC. Methods. The V and I band photometric data of 2476 fundamental mode (FU) and 1775 first overtone mode (FO) Cepheids in the LMC and 2753 FU and 1793 FO Cepheids in the SMC are analyzed for their P-L relations. We convert period of FO Cepheids to corresponding period of FU Cepheids before combining the two modes of Cepheids. Both galaxies are divided into small segments and combined FU and FO P-L diagrams are drawn in two bands for each segment. The reddening analysis is performed on 133 segments covering a total area of about 154.6 deg2 in the LMC and 136 segments covering a total area of about 31.3 deg2 in the SMC. By comparing with well calibrated P-L relations of these two galaxies, we determine reddening E(V − I) in each segment and equivalent reddening E(B − V) assuming the normal extinction law. -
ATNF News Issue No
Galaxy Pair NGC 1512 / NGC 1510 ATNF News Issue No. 67, October 2009 ISSN 1323-6326 Questacon "astronaut" street performer and visitors at the Parkes Open Days 2009. Credit: Shaun Amy, CSIRO. Cover page image Cover Figure: Multi-wavelength color-composite image of the galaxy pair NGC 1512/1510 obtained using the Digitised Sky Survey R-band image (red), the Australia Telescope Compact Array HI distribution (green) and the Galaxy Evolution Explorer NUV -band image (blue). The Spitzer 24µm image was overlaid just in the center of the two galaxies. We note that in the outer disk the UV emission traces the regions of highest HI column density. See article (page 28) for more information. 2 ATNF News, Issue 67, October 2009 Contents From the Director ...................................................................................................................................................................................................4 CSIRO Medal Winners .........................................................................................................................................................................................5 CSIRO Astronomy and Space Science Unit Formed ........................................................................................................................6 ATNF Distinguished Visitors Program ........................................................................................................................................................6 ATNF Graduate Student Program ................................................................................................................................................................7 -
Experiencing Hubble
PRESCOTT ASTRONOMY CLUB PRESENTS EXPERIENCING HUBBLE John Carter August 7, 2019 GET OUT LOOK UP • When Galaxies Collide https://www.youtube.com/watch?v=HP3x7TgvgR8 • How Hubble Images Get Color https://www.youtube.com/watch? time_continue=3&v=WSG0MnmUsEY Experiencing Hubble Sagittarius Star Cloud 1. 12,000 stars 2. ½ percent of full Moon area. 3. Not one star in the image can be seen by the naked eye. 4. Color of star reflects its surface temperature. Eagle Nebula. M 16 1. Messier 16 is a conspicuous region of active star formation, appearing in the constellation Serpens Cauda. This giant cloud of interstellar gas and dust is commonly known as the Eagle Nebula, and has already created a cluster of young stars. The nebula is also referred to the Star Queen Nebula and as IC 4703; the cluster is NGC 6611. With an overall visual magnitude of 6.4, and an apparent diameter of 7', the Eagle Nebula's star cluster is best seen with low power telescopes. The brightest star in the cluster has an apparent magnitude of +8.24, easily visible with good binoculars. A 4" scope reveals about 20 stars in an uneven background of fainter stars and nebulosity; three nebulous concentrations can be glimpsed under good conditions. Under very good conditions, suggestions of dark obscuring matter can be seen to the north of the cluster. In an 8" telescope at low power, M 16 is an impressive object. The nebula extends much farther out, to a diameter of over 30'. It is filled with dark regions and globules, including a peculiar dark column and a luminous rim around the cluster. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
Classification of Galaxies Using Fractal Dimensions
UNLV Retrospective Theses & Dissertations 1-1-1999 Classification of galaxies using fractal dimensions Sandip G Thanki University of Nevada, Las Vegas Follow this and additional works at: https://digitalscholarship.unlv.edu/rtds Repository Citation Thanki, Sandip G, "Classification of galaxies using fractal dimensions" (1999). UNLV Retrospective Theses & Dissertations. 1050. http://dx.doi.org/10.25669/8msa-x9b8 This Thesis is protected by copyright and/or related rights. It has been brought to you by Digital Scholarship@UNLV with permission from the rights-holder(s). You are free to use this Thesis in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Thesis has been accepted for inclusion in UNLV Retrospective Theses & Dissertations by an authorized administrator of Digital Scholarship@UNLV. For more information, please contact [email protected]. INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter face, while others may be from any type of computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely affect reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. -
An Ultra-Deep Survey of Low Surface Brightness Galaxies in Virgo
' $ An Ultra-Deep Survey of Low Surface Brightness Galaxies in Virgo Elizabeth Helen (Lesa) Moore, BSc(Hons) Department of Physics Macquarie University May 2008 This thesis is presented for the degree of Master of Philosophy in Physics & % iii Dedicated to all the sentient beings living in galaxies in the Virgo Cluster iv CONTENTS Synopsis : :::::::::::::::::::::::::::::::::::::: xvii Statement by Candidate :::::::::::::::::::::::::::::: xviii Acknowledgements ::::::::::::::::::::::::::::::::: xix 1. Introduction ::::::::::::::::::::::::::::::::::: 1 2. Low Surface Brightness (LSB) Galaxies :::::::::::::::::::: 5 2.1 Surface Brightness and LSB Galaxies De¯ned . 6 2.2 Physical Properties and Morphology . 8 2.3 Cluster and Field Distribution of LSB Dwarfs . 14 2.4 Galaxies, Cosmology and Clustering . 16 3. Galaxies and the Virgo Cluster :::::::::::::::::::::::: 19 3.1 Importance of the Virgo Cluster . 19 3.2 Galaxy Classi¯cation . 20 3.3 Virgo Galaxy Surveys and Catalogues . 24 3.4 Properties of the Virgo Cluster . 37 3.4.1 Velocity Distribution in the Direction of the Virgo Cluster . 37 3.4.2 Distance and 3D Structure . 38 vi Contents 3.4.3 Galaxy Population . 42 3.4.4 The Intra-Cluster Medium . 45 3.4.5 E®ects of the Cluster Environment . 47 4. Virgo Cluster Membership and the Luminosity Function :::::::::: 53 4.1 The Schechter Luminosity Function . 54 4.2 The Dwarf-to-Giant Ratio (DGR) . 58 4.3 Galaxy Detection . 59 4.4 Survey Completeness . 62 4.5 Virgo Cluster Membership . 63 4.5.1 Radial Velocities . 64 4.5.2 Morphology . 65 4.5.3 Concentration Parameters . 66 4.5.4 Scale Length Limits . 68 4.5.5 The Rines-Geller Threshold . -
Dwarf Galaxies
Europeon South.rn Ob.ervotory• ESO ML.2B~/~1 ~~t.· MAIN LIBRAKY ESO Libraries ,::;,q'-:;' ..-",("• .:: 114 ML l •I ~ -." "." I_I The First ESO/ESA Workshop on the Need for Coordinated Space and Ground-based Observations - DWARF GALAXIES Geneva, 12-13 May 1980 Report Edited by M. Tarenghi and K. Kjar - iii - INTRODUCTION The Space Telescope as a joint undertaking between NASA and ESA will provide the European community of astronomers with the opportunity to be active partners in a venture that, properly planned and performed, will mean a great leap forward in the science of astronomy and cosmology in our understanding of the universe. The European share, however,.of at least 15% of the observing time with this instrumentation, if spread over all the European astrono mers, does not give a large amount of observing time to each individual scientist. Also, only well-planned co ordinated ground-based observations can guarantee success in interpreting the data and, indeed, in obtaining observ ing time on the Space Telescope. For these reasons, care ful planning and cooperation between different European groups in preparing Space Telescope observing proposals would be very essential. For these reasons, ESO and ESA have initiated a series of workshops on "The Need for Coordinated Space and Ground based Observations", each of which will be centred on a specific subject. The present workshop is the first in this series and the subject we have chosen is "Dwarf Galaxies". It was our belief that the dwarf galaxies would be objects eminently suited for exploration with the Space Telescope, and I think this is amply confirmed in these proceedings of the workshop. -
Spiral Galaxies Like the Milky Way and Andromeda Edge on and Face On
Spiral galaxies like the Milky Way and Andromeda Edge on and face on L of Milky Way ~ few x 10 10 Lsun SDSS image by D. Hogg The Sombrero galaxy 12 kpc 40,000 light years Cartoon of the edge‐on Milky Way galaxy Palomar 5 M5 M13 M15 Images of globular clusters (GCs) (Sloan Digital Sky Survey) Leo I Dwarf Galaxy A galaxy that has 1/10 or fewer the number of stars in a Milky Way sized galaxy Dwarf galaxies Halo of dark maer 250 kpc 800,000 LY Large Magellanic cloud Wei‐Hao Wan, UH image credit (Giant) ellipcal galaxies This type of galaxy is oen found at the centers of galaxy clusters Ellipcal galaxies have relavely less gas, dust, and star formaon than spiral galaxies. They look redder because the ages of their stars are on average older than the stars in a spiral galaxy It is believed that a 2 billion solar mass black hole lives at the center of M87. Electrons accelerang along the strong magnec field near the black hole produce this jet of light and charged parcles. Irregular galaxies forming lots of stars and/or interacng with other galaxies Large Magellanic Cloud – luminosity ~ 1/10 luminosity of the Milky Way The Mice Galaxies Many galaxies live in clusters or groups Hickson Group 87 Image taken at Gemini South Abell Cluster S0740 Image was obtained with the Hubble Space Telescope Map of the Local Group Of Galaxies A dozens of dwarf galaxies and 2 giant spirals (the Milky Way and Andromeda) NGC 205 image credit: www.noao.edu ~ 1/40 Milky Way luminosity Image credit: David W. -
Secular Evolution and the Formation of Pseudobulges in Disk Galaxies
5 Aug 2004 22:35 AR AR222-AA42-15.tex AR222-AA42-15.sgm LaTeX2e(2002/01/18) P1: IKH 10.1146/annurev.astro.42.053102.134024 Annu. Rev. Astron. Astrophys. 2004. 42:603–83 doi: 10.1146/annurev.astro.42.053102.134024 Copyright c 2004 by Annual Reviews. All rights reserved First published! online as a Review in Advance on June 2, 2004 SECULAR EVOLUTION AND THE FORMATION OF PSEUDOBULGES IN DISK GALAXIES John Kormendy Department of Astronomy, University of Texas, Austin, Texas 78712; email: [email protected] Robert C. Kennicutt, Jr. Department of Astronomy, Steward Observatory, University of Arizona, Tucson, Arizona 85721; email: [email protected] KeyWords galaxy dynamics, galaxy structure, galaxy evolution I Abstract The Universe is in transition. At early times, galactic evolution was dominated by hierarchical clustering and merging, processes that are violent and rapid. In the far future, evolution will mostly be secular—the slow rearrangement of energy and mass that results from interactions involving collective phenomena such as bars, oval disks, spiral structure, and triaxial dark halos. Both processes are important now. This review discusses internal secular evolution, concentrating on one important con- sequence, the buildup of dense central components in disk galaxies that look like classical, merger-built bulges but that were made slowly out of disk gas. We call these pseudobulges. We begin with an “existence proof”—a review of how bars rearrange disk gas into outer rings, inner rings, and stuff dumped onto the center. The results of numerical sim- ulations correspond closely to the morphology of barred galaxies. -
Astronomy C SSSS 2018
Astronomy C SSSS 2018 Galaxies and Stellar Evolution Written by Anna1234 School _______________________________________________________________________ Team # _______________________________________________________________________ Names _______________________________________________________________________ _______________________________________________________________________ 1 Instructions: 1. There are pictures of a number of galaxies in this test. However, as the DSO list for 2019 hasn’t been released yet, the questions asked will not require any knowledge of the galaxies themselves. 2. No partial credit will be given. Math questions will have a range of acceptable answers 3. Tiebreaker questions are in the following order: a. Section A: #2, 6, 16; Section B: #1, 5, 9; Section C: #5b, 11, 14 4. Constants that will be used throughout the test: a. 1 Parsec = 3.1 x 1016 meters b. Mass of the sun = 1.989 x 1030 kg c. Hubble’s Constant = 65 km/s/Mpc d. Absolute Magnitude of Type 1a supernova = -19.3 2 Section A: Pseudo-DSOs M87 M87 has an active galactic nucleus (AGN). 1. Briefly explain what an AGN is and what is thought to cause it. 2. In 1999, a relativistic jet of matter beaming out from the center of this galaxy was measured to be moving much faster than the speed of light. What is the name of this phenomenon? 3. The M in “M87” signifies which classification catalog? Pinwheel Galaxy 4. Using Hubble’s Classification Scheme, classify this galaxy 5. The pinwheel galaxy is known for having a high number of HII regions... a. HII regions are also known as what 2 different categories of nebulas.? b. HII regions are ionized by stars of which spectral class? 6.