Lopsidedness in Early Type Disk Galaxies
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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. -
The ACS Virgo Cluster Survey. VI. Isophotal Analysis and Surface Brightness Profiles 3 at Odds with Previous Claims in Lauer Et Al
Rochester Institute of Technology RIT Scholar Works Articles 2006 The CA S Virgo Cluster Survey. VI. Isophotal Analysis and the Structure of Early-Type Galaxies Laura Ferrarese National Research Council of Canada Patrick Côté National Research Council of Canada Andrés Jordán European Southern Observatory Eric W. Peng National Research Council of Canada John P. Blakeslee The Johns Hopkins University See next page for additional authors Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation Laura Ferrarese et al 2006 ApJS 164 334 https://doi.org/10.1086/501350 This Article is brought to you for free and open access by RIT Scholar Works. It has been accepted for inclusion in Articles by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Authors Laura Ferrarese, Patrick Côté, Andrés Jordán, Eric W. Peng, John P. Blakeslee, Slawomir Piatek, Simona Mei, David Merritt, Miloš Milosavljević, John L. Tonry, and Michael J. West This article is available at RIT Scholar Works: http://scholarworks.rit.edu/article/1182 Accepted by The Astrophysical Journal Supplements Preprint typeset using LATEX style emulateapj v. 10/10/03 THE ACS VIRGO CLUSTER SURVEY. VI. ISOPHOTAL ANALYSIS AND THE STRUCTURE OF EARLY-TYPE GALAXIES1 Laura Ferrarese2, Patrick Cotˆ e´2, Andres´ Jordan´ 3,4, Eric W. Peng2, John P. Blakeslee5,6, Slawomir Piatek7, Simona Mei5, David Merritt8, Miloˇs Milosavljevic´9,10, John L. Tonry11, & Michael J. West12 Accepted by The Astrophysical Journal Supplements ABSTRACT We present a detailed analysis of the morphology, isophotal parameters and surface brightness profiles for 100 early-type members of the Virgo Cluster, from dwarfs (MB = −15.1 mag) to giants (MB = −21.8 mag). -
Line-Of-Sight Velocity Distributions of Low-Luminosity Elliptical Galaxies
Mon. Not. R. Astron. Soc. 326, 473–489 (2001) Line-of-sight velocity distributions of low-luminosity elliptical galaxies C. Halliday,1P† Roger L. Davies,1 Harald Kuntschner,1 M. Birkinshaw,2 Ralf Bender,3 R. P. Saglia3 and Glenn Baggley1 1Department of Physics, University of Durham, Science Labs, South Road, Durham DH1 3LE 2H.H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 1TL 3Universita¨ts-Sternwarte, Scheinerstr. 1, D-81679 Mu¨nchen, Germany Accepted 2001 March 7. Received 2000 December 21; in original form 2000 December 21 ABSTRACT The shape of the line-of-sight velocity distribution (LOSVD) is measured for a sample of 14 elliptical galaxies, predominantly low-luminosity ellipticals. The sample is dominated by galaxies in the Virgo cluster but also contains ellipticals in nearby groups and low-density environments. The parametrization of the LOSVD given by Gerhard and van der Marel & Franx is adopted, which measures the asymmetrical and symmetrical deviations of the LOSVD from a Gaussian by the amplitudes h3 and h4 of the Gauss–Hermite series. Rotation, velocity dispersion, h3 and h4 are determined as a function of radius for both major and minor axes. Non-Gaussian LOSVDs are found for all galaxies along the major axes. Deviations from a Gaussian LOSVD along the minor axis are of much lower amplitude if present at all. Central decreases in velocity dispersion are found for three galaxies. Two galaxies have kinematically decoupled cores: NGC 4458 and the well-known case of NGC 3608. Key words: galaxies: elliptical and lenticular, cD – galaxies: formation – galaxies: kinematics and dynamics. -
On the Origin of the Colour-Magnitude Relation in The
Draft version October 29, 2018 A Preprint typeset using L TEX style emulateapj v. 04/03/99 ON THE ORIGIN OF THE COLOR-MAGNITUDE RELATION IN THE VIRGO CLUSTER Alexandre Vazdekis 1,2, Harald Kuntschner 1, Roger. L. Davies 1 1 Department of Physics, University of Durham, Durham DH1 3LE, U.K; [email protected], [email protected], [email protected] 2 Instituto de Astrof´ısica de Canarias, E-38200 La Laguna, Tenerife, Spain N. Arimoto 3, O. Nakamura 3 3 Institute of Astronomy, University of Tokyo, Osawa 2-21-1, Mitaka, Tokyo 181-0015, Japan; [email protected], [email protected] R. F. Peletier 4 4 School of Physics and Astronomy, University of Nottingham, Nottingham, NG7 2RD, U.K; [email protected] To appear in The Astrophysical Journal Letters, 2001 April 20 (551, number 2) ABSTRACT We explore the origin of the color-magnitude relation (CMR) of early type galaxies in the Virgo cluster using spectra of very high S/N ratio for six elliptical galaxies selected along the CMR. The data are analysed using a new evolutionary stellar population synthesis model to generate galaxy spectra at the resolution given by their velocity dispersions. In particular we use a new age indicator that is virtually free of the effects of metallicity. We find that the luminosity weighted mean ages of Virgo ellipticals are greater than ∼ 8 Gyr, and show no clear trend with galaxy luminosity. We also find a positive correlation of metallicity with luminosity, color and velocity dispersion. -
Spatially Resolved Spectroscopy of Early-Type Galaxies Over a Range In
Mon. Not. R. Astron. Soc. 000, 1–?? (2006) Printed 8 October 2018 (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. -
19 90MNRAS.2 42P. .24C Mon. Not. R. Astr. Soc. (1990) 242
Mon. Not. R. astr. Soc. (1990) 242, Short Communication, 24p-27p .24C 42P. Further evidence of continuity between elliptical and disc galaxies* 90MNRAS.2 19 Massimo Capaccioli Osservatorio Astronómico, Vicolo Osservatorio 5,1-35122 Padova, Italy Nicola Caon Dipartimento di Astronomía, Università di Padova, Vicolo Osservatorio 5,1-35122, Italy Roberto Rampazzo Osservatorio Astronómico di Brera, Via Brera 28,1-20121 Milano, Italy Accepted 1989 October 23. Received 1989 October 20; in original form 1989 July 28 SUMMARY The behaviour of the isophotes of the E galaxies in a new photometric sample of 33 early-type galaxies belonging to the Virgo cluster (Caon) is compared to that of the SO galaxies. Almost all objects flatter than b/a - 0.3 are found to exhibit ‘pointed’ (or ‘lemon-shaped’) isophotes irrespective of their Hubble class, while almost none do if rounder than the same limit. This observation is used to support the incipient scenario (Bender et al.) in which a large fraction ( - 1/2) of E galaxies - the so-called ‘disky ellipticals’ - populates one end of a disc-to-bulge sequence including SO and spiral galaxies. 1 INTRODUCTION 1987,1989a,b; Capaccioli etal. 1989; Carter 1987). Indirect About 15 years ago the first rotation curves for E galaxies evidence that a significant fraction of E galaxies may share (Bertola & Capaccioli 1975; Illingworth 1977) broke down the same structural properties of SO bulges has been already the classical picture in which all galaxies (and galaxy com- contained in Michard’s (1985) observation of the similarity ponents) were seen as rotationally supported oblate between the ellipticity profiles of flat Es and edge-on lenticu- spheroids. -
DSO List V2 Current
7000 DSO List (sorted by name) 7000 DSO List (sorted by name) - from SAC 7.7 database NAME OTHER TYPE CON MAG S.B. SIZE RA DEC U2K Class ns bs Dist SAC NOTES M 1 NGC 1952 SN Rem TAU 8.4 11 8' 05 34.5 +22 01 135 6.3k Crab Nebula; filaments;pulsar 16m;3C144 M 2 NGC 7089 Glob CL AQR 6.5 11 11.7' 21 33.5 -00 49 255 II 36k Lord Rosse-Dark area near core;* mags 13... M 3 NGC 5272 Glob CL CVN 6.3 11 18.6' 13 42.2 +28 23 110 VI 31k Lord Rosse-sev dark marks within 5' of center M 4 NGC 6121 Glob CL SCO 5.4 12 26.3' 16 23.6 -26 32 336 IX 7k Look for central bar structure M 5 NGC 5904 Glob CL SER 5.7 11 19.9' 15 18.6 +02 05 244 V 23k st mags 11...;superb cluster M 6 NGC 6405 Opn CL SCO 4.2 10 20' 17 40.3 -32 15 377 III 2 p 80 6.2 2k Butterfly cluster;51 members to 10.5 mag incl var* BM Sco M 7 NGC 6475 Opn CL SCO 3.3 12 80' 17 53.9 -34 48 377 II 2 r 80 5.6 1k 80 members to 10th mag; Ptolemy's cluster M 8 NGC 6523 CL+Neb SGR 5 13 45' 18 03.7 -24 23 339 E 6.5k Lagoon Nebula;NGC 6530 invl;dark lane crosses M 9 NGC 6333 Glob CL OPH 7.9 11 5.5' 17 19.2 -18 31 337 VIII 26k Dark neb B64 prominent to west M 10 NGC 6254 Glob CL OPH 6.6 12 12.2' 16 57.1 -04 06 247 VII 13k Lord Rosse reported dark lane in cluster M 11 NGC 6705 Opn CL SCT 5.8 9 14' 18 51.1 -06 16 295 I 2 r 500 8 6k 500 stars to 14th mag;Wild duck cluster M 12 NGC 6218 Glob CL OPH 6.1 12 14.5' 16 47.2 -01 57 246 IX 18k Somewhat loose structure M 13 NGC 6205 Glob CL HER 5.8 12 23.2' 16 41.7 +36 28 114 V 22k Hercules cluster;Messier said nebula, no stars M 14 NGC 6402 Glob CL OPH 7.6 12 6.7' 17 37.6 -03 15 248 VIII 27k Many vF stars 14.. -
2016 Publication Year 2020-05-22T09:39:01Z
Publication Year 2016 Acceptance in OA@INAF 2020-05-22T09:39:01Z Title Deep Photometry of Galaxies in the VEGAS Survey: The Case of NGC 4472 Authors SPAVONE, MARILENA DOI 10.1007/978-3-319-19330-4_26 Handle http://hdl.handle.net/20.500.12386/25065 Series ASTROPHYSICS AND SPACE SCIENCE PROCEEDINGS Number 42 Deep photometry of galaxies in the VEGAS survey: the case of NGC 4472 Marilena Spavone on behalf of the VEGAS team⋆ Abstract The VST-VEGAS project is aimed at resolution data and the need of studying nearby, observing and studying a rich sample of nearby and thus large, objects. We present a detailed study early-type galaxies in order to systematically char- of the surface photometry of the elliptical galaxy acterize their properties over a wide baseline of NGC4472 and of smaller ETGs in its field, per- sizes and out to the faint outskirts where data are formed by using new g and i bands images to con- rather scarce so far. The external regions of galax- strain the formation history of this nearby giant ies more easily retain signatures about the for- galaxy, and to investigate the presence of very faint mation and evolution mechanisms which shaped substructures in its surroundings. them, as their relaxation time are longer, and they are more weakly influenced by processes such as mergers, secular evolution, central black hole ac- tivity, and supernova feedback on the ISM, which 1 The VEGAS survey tend to level age and metallicity gradients. The collection of a wide photometric dataset of a large number of galaxies in various environmental con- The VST Elliptical GAlaxies Survey (VEGAS) is ditions, may help to shed light on these questions.