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VEGAS: a VST Early-Type Galaxy Survey. the Faint Substructures of NGC 4472 Stellar Halo
VEGAS: A VST Early-type GAlaxy Survey. The faint substructures of NGC 4472 stellar halo. MARILENA SPAVONE ON THE BEHALF OF THE VEGAS TEAM: M. CAPACCIOLI, M. CANTIELLO, A. GRADO, E. IODICE, F. LA BARBERA, N.R. NAPOLITANO, C. TORTORA, L. LIMATOLA, M. PAOLILLO, T. PUZIA, R. PELETIER, A.J. ROMANOWSKY, D. FORBES, G. RAIMONDO OUTLINE The VST VEGAS survey Science aims Results on NGC 4472 field Conclusions Future plans MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). An example Obj. name Morph. type u g r i IC 1459 E3 5630 1850 1700 NGC 1399 E1 8100 5320 2700 NGC 3115 S0 14800 8675 6030 Observations to date (to P94) g-BAND ~ 16% i-BAND ~ 19% r-BAND ~ 3% + FORNAX u-BAND ~ 1% MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). OT ~ 350 h @ vst over 5 years Expected SB limits: 27.5 g, 2 27.0 r and 26.2 i mag/arcsec . g band expected SB limit MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). ~ 350 h @ vst over 5 years Expected SB limits: 27.5 g, 27.0 r and 26.2 i mag/arcsec2. -
Pdf, Integral-Field Stellar and Ionized Gas Kinematics of Peculiar Virgo
The Astrophysical Journal Supplement Series, 216:9 (34pp), 2015 January doi:10.1088/0067-0049/216/1/9 C 2015. The American Astronomical Society. All rights reserved. INTEGRAL-FIELD STELLAR AND IONIZED GAS KINEMATICS OF PECULIAR VIRGO CLUSTER SPIRAL GALAXIES Juan R. Cortes´ 1,2,3,5, Jeffrey D. P. Kenney4, and Eduardo Hardy1,3,5,6 1 National Radio Astronomy Observatory Avenida Nueva Costanera 4091, Vitacura, Santiago, Chile; [email protected], [email protected] 2 Joint ALMA Observatory Alonso de Cordova´ 3107, Vitacura, Santiago, Chile 3 Departamento de Astronom´ıa, Universidad de Chile Casilla 36-D, Santiago, Chile 4 Department of Astronomy, Yale University, P.O. Box 208101, New Haven, CT 06520-8101, USA; [email protected] Received 2014 March 10; accepted 2014 November 7; published 2014 December 24 ABSTRACT We present the stellar and ionized gas kinematics of 13 bright peculiar Virgo cluster galaxies observed with the DensePak Integral Field Unit at the WIYN 3.5 m telescope in order to look for kinematic evidence that these galaxies have experienced gravitational interactions or gas stripping. Two-dimensional maps of the stellar velocity V, stellar velocity dispersion σ, and the ionized gas velocity (Hβ and/or [O iii]) are presented for the galaxies in the sample. The stellar rotation curves and velocity dispersion profiles are determined for 13 galaxies, and the ionized gas rotation curves are determined for 6 galaxies. Misalignments between the optical and kinematical major axes are found in several galaxies. While in some cases this is due to a bar, in other cases it seems to be associated with gravitational interaction or ongoing ram pressure stripping. -
Thesis University of Western Australia
Kinematic and Environmental Regulation of Atomic Gas in Galaxies Jie Li March 2019 Master Thesis University of Western Australia Supervisors: Dr. Danail Obreschkow Dr. Claudia Lagos Dr. Charlotte Welker 20/05/2019 Acknowledgments I would like to thank my supervisors Danail Obreschkow, Claudia Lagos and Charlotte Welker for their guidance and support during this project, Luca Cortese, Robert Dˇzudˇzar and Garima Chauhan for their useful suggestions, my parents for giving me financial support and love, and ICRAR for o↵ering an open and friendly environments. Abstract Recent studies of neutral atomic hydrogen (H i) in nearby galaxies find that all isolated star-forming disk-dominated galaxies, from low-mass dwarfs to massive spirals systems, are H i saturated, in that they carry roughly (within a factor 1.5) as much H i fraction as permitted before this gas becomes gravitationally unstable. By taking this H i saturation for granted, the atomic gas fraction fatm of galactic disks can be predicted as a function of a stability parameter q j/M,whereM and j are the baryonic mass and specific / angular momentum of the disk (Obreschkow et al., 2016). The (logarithmic) di↵erence ∆fq between this predictor and the observed atomic fraction can thus be seen as a physically motivated way of defining a ‘H i deficiency’. While isolated disk galaxies have ∆f 0, q ⇡ objects subject to environmental removal/suppression of H i are expected to have ∆fq > 0. Within this framework, we revisit the H i deficiencies of satellite galaxies in the Virgo cluster (from the VIVA sample), as well as in clusters of the EAGLE simulation. -
Arxiv:0807.3747V2 [Astro-Ph] 13 Sep 2008 Prlsrcuebtltl,I N,Ogigsa Formation
Draft version October 23, 2018 A Preprint typeset using LTEX style emulateapj v. 08/13/06 THE STELLAR POPULATIONS OF STRIPPED SPIRAL GALAXIES IN THE VIRGO CLUSTER Hugh H. Crowl1 and Jeffrey D.P. Kenney Department of Astronomy, Yale University, New Haven, CT 06520 Draft version October 23, 2018 ABSTRACT We present an analysis of the stellar populations of the gas-stripped outer disks of ten Virgo Clus- ter spiral galaxies, utilizing SparsePak integral field spectroscopy on the WIYN 3.5m telescope and GALEX UV photometry. The galaxies in our sample show evidence for being gas-stripped spiral galaxies, with star formation within a truncation radius, and a passive population beyond the trun- cation radius. We find that all of the galaxies with spatially truncated star formation have outer disk stellar populations consistent with star formation ending within the last 500 Myr. The synthe- sis of optical spectroscopy and GALEX observations demonstrate that star formation was relatively constant until the quenching time, after which the galaxies passively evolved. Large starbursts at the time of quenching are excluded for all galaxies, but there is evidence of a modest starburst in at least one galaxy. For approximately half of our galaxies, the timescales derived from our observations are consistent with galaxies being stripped in or near the cluster core, where simple ram-pressure estimates can explain the observed stripping. However, the other half of our sample galaxies were clearly stripped outside the cluster core. Such galaxies provide evidence that the intra-cluster medium is not static and smooth. For three of the most recently stripped galaxies, there are estimates for the stripping timescales from detailed gas stripping simulations. -
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 . -
Radial Distribution of Globular Clusters and Diffuse Hot
Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed 13 September 2018 (MN LATEX style file v2.2) The Baryonic Halos of Elliptical Galaxies: Radial Distribution of Globular Clusters and Diffuse Hot Gas Duncan A. Forbes1⋆, Trevor Ponman2 and Ewan O’Sullivan2,3, 1Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn VIC 3122, Australia 2School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT 3Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 13 September 2018 ABSTRACT For a sample of 9 well-studied giant ellipticals we compare the projected radial dis- tribution of their red and blue globular cluster (GC) subpopulations with their host galaxy stellar and X-ray surface brightness profiles. We support previous findings that the surface density distribution of red (metal-rich) GCs follows that of the host galaxy starlight. We find good agreement between the outer slope of the blue GC surface density and that of the galaxy X-ray emission. This coincidence of projected radial profiles is likely due to the fact that both blue GCs and X-ray emitting hot gas share the same gravitational potential in equilibrium. When deprojected the X-ray emitting hot gas has a radial density dependence that is the square root of that for the GC density. We further show that the energy per unit mass for blue GCs is roughly half that of the hot gas. Key words: globular clusters: general – galaxies: star clusters – galaxies: individual – galaxies: formation 1 INTRODUCTION common formation history with the stellar component of an elliptical galaxy. The globular cluster (GC) systems of most, well-studied large galaxies reveal evidence for two subpopulations in The blue GCs have been associated with elliptical colour (and by proxy in metallicity). -
Exploring the Globular Cluster Systems of the Leo II Group and Their Global Relationships
MNRAS 458, 105–126 (2016) doi:10.1093/mnras/stw185 The SLUGGS survey∗: exploring the globular cluster systems of the Leo II group and their global relationships Sreeja S. Kartha,1‹ Duncan A. Forbes,1 Adebusola B. Alabi,1 Jean P. Brodie,2 Aaron J. Romanowsky,2,3 Jay Strader,4 Lee R. Spitler,5,6 Zachary G. Jennings2 and Joel C. Roediger7 1Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn VIC 3122, Australia 2University of California Observatories, 1156 High St., Santa Cruz, CA 95064, USA 3Department of Physics and Astronomy, San Jose´ State University, One Washington Square, San Jose, CA 95192, USA 4Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA 5Macquarie University, Macquarie Park, Sydney, NSW 2113, Australia 6Australian Astronomical Observatory, PO Box 915, North Ryde, NSW 1670, Australia 7NRC Herzberg Astronomy & Astrophysics, Victoria, BC V9E 2E7, Canada Accepted 2016 January 20. Received 2016 January 20; in original form 2015 July 23 ABSTRACT We present an investigation of the globular cluster (GC) systems of NGC 3607 and NGC 3608 as part of the ongoing SLUGGS (SAGES Legacy Unifying Globulars and GalaxieS) survey. We use wide-field imaging data from the Subaru telescope in the g, r and i filters to analyse the radial density, colour and azimuthal distributions of both GC systems. With the complementary kinematic data obtained from the Keck II telescope, we measure the radial velocities of a total of 81 GCs. Our results show that the GC systems of NGC 3607 and NGC 3608 have a detectable spatial extent of ∼15 and 13 galaxy effective radii, respectively. -
WALLABY Pre-Pilot Survey: Two Dark Clouds in the Vicinity of NGC 1395
University of Texas Rio Grande Valley ScholarWorks @ UTRGV Physics and Astronomy Faculty Publications and Presentations College of Sciences 2021 WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395 O. I. Wong University of Western Australia A. R. H. Stevens B. Q. For University of Western Australia Tobias Westmeier M. Dixon See next page for additional authors Follow this and additional works at: https://scholarworks.utrgv.edu/pa_fac Part of the Astrophysics and Astronomy Commons, and the Physics Commons Recommended Citation O I Wong, A R H Stevens, B-Q For, T Westmeier, M Dixon, S-H Oh, G I G Józsa, T N Reynolds, K Lee-Waddell, J Román, L Verdes-Montenegro, H M Courtois, D Pomarède, C Murugeshan, M T Whiting, K Bekki, F Bigiel, A Bosma, B Catinella, H Dénes, A Elagali, B W Holwerda, P Kamphuis, V A Kilborn, D Kleiner, B S Koribalski, F Lelli, J P Madrid, K B W McQuinn, A Popping, J Rhee, S Roychowdhury, T C Scott, C Sengupta, K Spekkens, L Staveley-Smith, B P Wakker, WALLABY pre-pilot survey: Two dark clouds in the vicinity of NGC 1395, Monthly Notices of the Royal Astronomical Society, 2021;, stab2262, https://doi.org/10.1093/ mnras/stab2262 This Article is brought to you for free and open access by the College of Sciences at ScholarWorks @ UTRGV. It has been accepted for inclusion in Physics and Astronomy Faculty Publications and Presentations by an authorized administrator of ScholarWorks @ UTRGV. For more information, please contact [email protected], [email protected]. -
Information to Users
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 fece, 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 afreet reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are missing pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, charts) are reproduced by sectioning the original, beginning at the upper left-hand comer and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. Higher quality 6” x 9” black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. UMI A Bell & Howell Information Company 300 North Zed) Road, Ann Arbor MI 48106-1346 USA 313/761-4700 800/521-0600 A STUDY OF ATTENUATION EFFECTS IN HIGHLY INCLINED SPIRAL GALAXIES DISSERTATION Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Leslie E. -
Distances from Stellar Kinematics for Peculiar Virgo Cluster Spiral Galaxies
Distances from Stellar Kinematics for Peculiar Virgo Cluster Spiral Galaxies Juan R. Cort´es Departamento de Astronom´ıa, Universidad de Chile Casilla 36-D, Santiago, Chile [email protected] National Astronomical Observatory of Japan 2-21-1 Osawa, Mitaka, Tokyo, 181-8588 Jeffrey D. P. Kenney Department of Astronomy, Yale University P.0. Box 208101, New Haven, CT 06520-8101 [email protected] Eduardo Hardy1 National Radio Astronomy Observatory Casilla El Golf 16-10, Las Condes, Santiago, Chile [email protected] Departamento de Astronom´ıa, Universidad de Chile2 Casilla 36-D, Santiago, Chile ABSTRACT We present distance estimates for eleven peculiar Virgo cluster spiral galaxies based on mea- surements of the stellar kinematics of their central 2 kpc. Stellar circular velocities were obtained using two-integral dynamical models. Distances were obtained by comparing, at each radius, the stellar circular velocities with synthetic Hα rotation curves derived from NIR Tully-Fisher relations. The results show that most of our galaxies are located within 4 Mpc of the core arXiv:0803.3638v2 [astro-ph] 14 Apr 2008 of the cluster. Three of these galaxies, previously classified as “low rotator galaxies” or with “Truncated/Compact” Hα radial distributions, have stellar kinematics-based distances that are discrepant with HI-based distances by at least 60%, and are likely to be located within the virial radius of the cluster. These discrepancies appear due to very truncated gas distributions plus non-circular gas motions or gas motions not in the plane of the stellar disk, perhaps as the result of gravitational interactions. Our results show that environmental effects can significantly re- duce the measured HI linewidths for some disturbed cluster galaxies, thus affecting the accurate determination of distances based on gas kinematics methods. -
The I Band Tully-Fisher Relation for Cluster Galaxies: Data Presentation
Dartmouth College Dartmouth Digital Commons Open Dartmouth: Peer-reviewed articles by Dartmouth faculty Faculty Work 10-13-1997 The I Band Tully-Fisher Relation for Cluster Galaxies: Data Presentation. Riccardo Giovanelli Cornell University Martha P. Haynes Cornell University Terry Herter Cornell University Nicole P. Vogt Cornell University Gary Wegner Dartmouth College See next page for additional authors Follow this and additional works at: https://digitalcommons.dartmouth.edu/facoa Part of the Astrophysics and Astronomy Commons Dartmouth Digital Commons Citation Giovanelli, Riccardo; Haynes, Martha P.; Herter, Terry; Vogt, Nicole P.; Wegner, Gary; Salzer, John J.; da Costa, Luiz N.; and Freudling, Wolfram, "The I Band Tully-Fisher Relation for Cluster Galaxies: Data Presentation." (1997). Open Dartmouth: Peer-reviewed articles by Dartmouth faculty. 3427. https://digitalcommons.dartmouth.edu/facoa/3427 This Article is brought to you for free and open access by the Faculty Work at Dartmouth Digital Commons. It has been accepted for inclusion in Open Dartmouth: Peer-reviewed articles by Dartmouth faculty by an authorized administrator of Dartmouth Digital Commons. For more information, please contact [email protected]. Authors Riccardo Giovanelli, Martha P. Haynes, Terry Herter, Nicole P. Vogt, Gary Wegner, John J. Salzer, Luiz N. da Costa, and Wolfram Freudling This article is available at Dartmouth Digital Commons: https://digitalcommons.dartmouth.edu/facoa/3427 Version 1.1 13 October 1996 To appear in Astronomical Journal The I–Band Tully–Fisher Relation for Cluster Galaxies: Data Presentation Riccardo Giovanelli, Martha P. Haynes, Terry Herter and Nicole P. Vogt Center for Radiophysics and Space Research and National Astronomy and Ionosphere Center1, Cornell University, Ithaca, NY 14853 Gary Wegner Dept. -
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,