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Science Goals and Selection Criteria
University of Groningen The ATLAS(3D) project Cappellari, Michele; Emsellem, Eric; Krajnovic, Davor; McDermid, Richard M.; Scott, Nicholas; Kleijn, G. A. Verdoes; Young, Lisa M.; Alatalo, Katherine; Bacon, R.; Blitz, Leo Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1111/j.1365-2966.2010.18174.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: 2011 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Cappellari, M., Emsellem, E., Krajnovic, D., McDermid, R. M., Scott, N., Kleijn, G. A. V., Young, L. M., Alatalo, K., Bacon, R., Blitz, L., Bois, M., Bournaud, F., Bureau, M., Davies, R. L., Davis, T. A., de Zeeuw, P. T., Duc, P-A., Khochfar, S., Kuntschner, H., ... Weijmans, A-M. (2011). The ATLAS(3D) project: I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria. Monthly Notices of the Royal Astronomical Society, 413(2), 813-836. https://doi.org/10.1111/j.1365- 2966.2010.18174.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. -
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. -
1. Introduction
THE ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, 122:109È150, 1999 May ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. GALAXY STRUCTURAL PARAMETERS: STAR FORMATION RATE AND EVOLUTION WITH REDSHIFT M. TAKAMIYA1,2 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637; and Gemini 8 m Telescopes Project, 670 North Aohoku Place, Hilo, HI 96720 Received 1998 August 4; accepted 1998 December 21 ABSTRACT The evolution of the structure of galaxies as a function of redshift is investigated using two param- eters: the metric radius of the galaxy(Rg) and the power at high spatial frequencies in the disk of the galaxy (s). A direct comparison is made between nearby (z D 0) and distant(0.2 [ z [ 1) galaxies by following a Ðxed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broad- band images at D4500A observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between D3000 and D9000A (Williams et al.). The radius is measured from the intensity proÐle of the galaxy using the formulation of Petrosian, and it is argued to be a metric radius that should not depend very strongly on the angular resolution and limiting surface brightness level of the imaging data. It is found that the metric radii of nearby and distant galaxies are comparable to each other. -
Age and Interstellar Absorption in Young Star-Formation Regions In
ISSN 1063-7729, Astronomy Reports, 2008, Vol. 52, No. 9, pp. 714–728. c Pleiades Publishing, Ltd., 2008. Original Russian Text c A.S. Gusev, V.I. Myakutin, A.E. Piskunov, F.K. Sakhibov, M.S. Khramtsova, 2008, published in Astronomicheski˘ı Zhurnal, 2008, Vol. 85, No. 9, pp. 794–809. Age and Interstellar Absorption in Young Star-Formation Regions in the Galaxies NGC 1068, NGC 4449, NGC 4490, NGC 4631, and NGC 4656/57 Derived from Multicolor Photometry A. S. Gusev1, V.I.Myakutin2, A.E.Piskunov2,F.K.Sakhibov3, 4,andM.S.Khramtsova5 1Sternberg Astronomical Institute, Universitetski ˘ı pr. 13, Moscow, 119991, Russia 2Institute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 109017 Russia 3Giessen–Friedberg University for Applied Studies, Friedberg, Germany 4Institute of Astrophysics, Academy of Sciences of Tajikistan, ul. Bukhoro 22, Dushanbe, 734670 Tajikistan 5Ural State University, pr. Lenina 51, Yekaterinburg, 620083 Received October 3, 2007; in final form, October, 26, 2007 Abstract—We have compared the results of multicolor UBVR and Hα photometry for 169 young star-formation complexes in five galaxies using a grid of evolutionary models for young star clusters. The ages and interstellar absorptions are estimated for 102 star-formation complexes with the standard m uncertainties σt =0.30 dex and σAV =0.45 . The accuracies of these parameters were verified using numerical simulations. PACS num b e r s : 98.52.Nr, 98.62.Ai, 97.10.Bt DOI: 10.1134/S1063772908090035 1. INTRODUCTION several evolutionary models, instead considering a set The evolution of galaxies depends on their history of models encompassing the entire interval of the of star formation, i.e., the history of variations of IMF and SFR. -
April Constellations of the Month
April Constellations of the Month Leo Small Scope Objects: Name R.A. Decl. Details M65! A large, bright Sa/Sb spiral galaxy. 7.8 x 1.6 arc minutes, magnitude 10.2. Very 11hr 18.9m +13° 05’ (NGC 3623) high surface brighness showing good detail in medium sized ‘scopes. M66! Another bright Sb galaxy, only 21 arc minutes from M65. Slightly brighter at mag. 11hr 20.2m +12° 59’ (NGC 3627) 9.7, measuring 8.0 x 2.5 arc minutes. M95 An easy SBb barred spiral, 4 x 3 arc minutes in size. Magnitude 10.5, with 10hr 44.0m +11° 42’ a bright central core. The bar and outer ring of material will require larger (NGC 3351) aperature and dark skies. M96 Another bright Sb spiral, about 42 arc minutes east of M95, but larger and 10hr 46.8m +11° 49’ (NGC 3368) brighter. 6 x 4 arc minutes, magnitude 10.1. Located about 48 arc minutes NNE of M96. This small elliptical galaxy measures M105 only 2 x 2.1 arc minutes, but at mag. 10.3 has very high surface brightness. 10hr 47.8m +12° 35’ (NGC 3379) Look for NGC 3384! (110NGC) and NGC 3389 (mag 11.0 and 12.2) which form a small triangle with M105. NGC 3384! 10hr 48.3m +12° 38’ See comment for M105. The brightest galaxy in Leo, this Sb/Sc spiral galaxy shines at mag. 9.5. Look for NGC 2903!! 09hr 32.2m +21° 30’ a hazy patch 11 x 4.7 arc minutes in size 1.5° south of l Leonis. -
Probing the Birth of Super Star Clusters
Probing the Birth of Super Star Clusters Kelsey Johnson With help from: Alan Aversa, Crystal Brogan, Rosie Chen, Jeremy Darling, Miller Goss, Remy Indebetouw, Amanda Kepley, Chip Kobulnicky, Amy Reines, Bill Vacca, David Whelan NOAO Summer Program 1995 Remy Regina Indebetouw Jorgenson Angelle Tanner Seth Redfield Reed Riddle Kelsey Johnson Amy Winebarger Super Star Clusters: Cluster formaon in the Extreme • Plausibly proto‐globular clusters • Formaon common in early universe • Impact on the ISM & IGM 1) What physical conditions are required to form these clusters? 2) Does this extreme environment affect affect the SF process itself? Strategy: Look for sources with similar SEDs to Ultracompact HII regions Compact, “inverted spectrum” sources Very dense HII regions non-thermal Sn free-free optically-thick free-free 100 1 l (cm) Wood & Churchwell 1989 II ZW 40 NGC 4490 NGC 4449 Aversa et al.sub Image credit: Michael Gariepy/ Kepley et al. in prep, Beck et et al. Adam Block/NOAO/AURA/NSF Reines et al. 08 NGC 2537 NGC 5253 NGC 3125 Aversa et al. sub Turner et al. 00 Aversa et al. sub Image Credit: Sloan Digital Sky Survey Image credit: Angel Lopez-Sanchez Haro 3 IC 4662 NGC 4214 Beck et al. 00 Image Credit: NASA and Hubble Heritage Team (STScI) Johnson et al. 03 Johnson et al. 04 Natal Clusters are rare! (i.e. short‐lived) Recent radio survey of nearby “star-forming” galaxies: Only 9/28 have detected thermal sources Aversa, Johnson, et al.submitted Henize 2-10 ACS optical, Vacca et al. in prep NICMOS Pa a, Reines et al. -
SUPERMASSIVE BLACK HOLES and THEIR HOST SPHEROIDS III. the MBH − Nsph CORRELATION
The Astrophysical Journal, 821:88 (8pp), 2016 April 20 doi:10.3847/0004-637X/821/2/88 © 2016. The American Astronomical Society. All rights reserved. SUPERMASSIVE BLACK HOLES AND THEIR HOST SPHEROIDS. III. THE MBH–nsph CORRELATION Giulia A. D. Savorgnan Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia; [email protected] Received 2015 December 6; accepted 2016 March 6; published 2016 April 13 ABSTRACT The Sérsic R1 n model is the best approximation known to date for describing the light distribution of stellar spheroidal and disk components, with the Sérsic index n providing a direct measure of the central radial concentration of stars. The Sérsic index of a galaxy’s spheroidal component, nsph, has been shown to tightly correlate with the mass of the central supermassive black hole, MBH.TheMnBH– sph correlation is also expected from other two well known scaling relations involving the spheroid luminosity, Lsph:theLsph–n sph and the MLBH– sph. Obtaining an accurate estimate of the spheroid Sérsic index requires a careful modeling of a galaxy’s light distribution and some studies have failed to recover a statistically significant MnBH– sph correlation. With the aim of re-investigating the MnBH– sph and other black hole mass scaling relations, we performed a detailed (i.e., bulge, disks, bars, spiral arms, rings, halo, nucleus, etc.) decomposition of 66 galaxies, with directly measured black hole masses, that had been imaged at 3.6 μm with Spitzer.Inthispaper,the third of this series, we present an analysis of the Lsph–n sph and MnBH– sph diagrams. -
A Nuclear Molecular Outflow in the Seyfert Galaxy NGC 3227
Astronomy & Astrophysics manuscript no. ALMANGC3227_final c ESO 2019 June 18, 2019 A nuclear molecular outflow in the Seyfert galaxy NGC 3227 A. Alonso-Herrero1, S. García-Burillo2, M. Pereira-Santaella3, R. I. Davies4, F. Combes5, M. Vestergaard6; 7, S. I. Raimundo6, A. Bunker3, T. Díaz-Santos8, P. Gandhi9, I. García-Bernete10, E. K. S. Hicks11, S. F. Hönig8, L. K. Hunt12, M. Imanishi13; 14, T. Izumi13, N. A. Levenson15, W. Maciejewski16, C. Packham17; 13, C. Ramos Almeida18; 19, C. Ricci8; 20, D. Rigopoulou3, P. F. Roche3, D. Rosario21, M. Schartmann22; 4, A. Usero2, and M. J. Ward21 1 Centro de Astrobiología (CAB, CSIC-INTA), ESAC Campus, E-28692 Villanueva de la Cañada, Madrid, Spain e-mail: [email protected] 2 Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, E-28014 Madrid, Spain 3 Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK 4 Max Planck Institut für extraterrestrische Physik Postfach 1312, D-85741 Garching bei München, Germany 5 LERMA, Obs. de Paris, PSL Research Univ., Collége de France, CNRS, Sorbonne Univ., UPMC, Paris, France 6 DARK, The Niels Bohr Institute, University of Copenhagen, Vibenshuset, Lyngbyvej 2, DK-2100 Copenhagen O., Denmark 7 Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, Arizona, USA 8 Núcleo de Astronomía de la Facultad de Ingeniería, Universidad Diego Portales, Av. Ejército Libertador 441, Santiago, Chile 9 Department of Physics & Astronomy, University of Southampton, Hampshire SO17 1BJ, Southampton, UK 10 Instituto de Física de Cantabria, CSIC-Universidad de Cantabria, E-39005 Santander, Spain 11 Department of Physics & Astronomy, University of Alaska Anchorage, AK 99508-4664, USA 12 INAF-Osservatorio Astrofisico di Arcetri, Largo E. -
The ACS Virgo Cluster Survey. VI. Isophotal Analysis and The
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 Patrick Cote Andres Jordan Follow this and additional works at: http://scholarworks.rit.edu/article Recommended Citation Astrophysical Journal Supplement Series 164 (2006) 334-434 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]. 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). Each galaxy has been imaged in two filters, closely resembling the Sloan g and z passbands, using the Advanced Camera for Surveys on board the Hubble Space Telescope. Dust and complex morphological structures are common. Dust is detected in as many as 18, prefer- entially bright, galaxies. The incidence rate in the 26 galaxies brighter than BT = 12.15 mag, which form a magnitude limited sample, is 42%. -
Astronomy 2008 Index
Astronomy Magazine Article Title Index 10 rising stars of astronomy, 8:60–8:63 1.5 million galaxies revealed, 3:41–3:43 185 million years before the dinosaurs’ demise, did an asteroid nearly end life on Earth?, 4:34–4:39 A Aligned aurorae, 8:27 All about the Veil Nebula, 6:56–6:61 Amateur astronomy’s greatest generation, 8:68–8:71 Amateurs see fireballs from U.S. satellite kill, 7:24 Another Earth, 6:13 Another super-Earth discovered, 9:21 Antares gang, The, 7:18 Antimatter traced, 5:23 Are big-planet systems uncommon?, 10:23 Are super-sized Earths the new frontier?, 11:26–11:31 Are these space rocks from Mercury?, 11:32–11:37 Are we done yet?, 4:14 Are we looking for life in the right places?, 7:28–7:33 Ask the aliens, 3:12 Asteroid sleuths find the dino killer, 1:20 Astro-humiliation, 10:14 Astroimaging over ancient Greece, 12:64–12:69 Astronaut rescue rocket revs up, 11:22 Astronomers spy a giant particle accelerator in the sky, 5:21 Astronomers unearth a star’s death secrets, 10:18 Astronomers witness alien star flip-out, 6:27 Astronomy magazine’s first 35 years, 8:supplement Astronomy’s guide to Go-to telescopes, 10:supplement Auroral storm trigger confirmed, 11:18 B Backstage at Astronomy, 8:76–8:82 Basking in the Sun, 5:16 Biggest planet’s 5 deepest mysteries, The, 1:38–1:43 Binary pulsar test affirms relativity, 10:21 Binocular Telescope snaps first image, 6:21 Black hole sets a record, 2:20 Black holes wind up galaxy arms, 9:19 Brightest starburst galaxy discovered, 12:23 C Calling all space probes, 10:64–10:65 Calling on Cassiopeia, 11:76 Canada to launch new asteroid hunter, 11:19 Canada’s handy robot, 1:24 Cannibal next door, The, 3:38 Capture images of our local star, 4:66–4:67 Cassini confirms Titan lakes, 12:27 Cassini scopes Saturn’s two-toned moon, 1:25 Cassini “tastes” Enceladus’ plumes, 7:26 Cepheus’ fall delights, 10:85 Choose the dome that’s right for you, 5:70–5:71 Clearing the air about seeing vs. -
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. -
Imaging Linear Polarimetry of Galaxies Members of Interacting Pairs R
Tracing the evolution of galaxies in the Leo cloud: a photometric and kinematic characterization A. Marino1, R. Rampazzo2, P. Mazzei2, H. Plana3, L. Bianchi4, M. Rosado5, D. Bettoni2, G. Galletta1, L.M. Buson2, P. Ambrocio-Cruz6, F. Gabbasov5 1 Dipartimento di Fisica e Astronomia G. Galilei, Università di Padova (Italy) 2INAF - Osservatorio Astronomico di Padova (Italy) 3LATO, Univesidade Estadual de S. Cruz, Bahia (Brazil) 4Dept. of Physics and Astronomy, Johns Hopkins University, Baltimore (USA) 5IInstituto de Astronomía, UNAM (México) 6Universidad Autonóma del Estado de Hidalgo (México) Introduction Groups contain a large fraction (50-60%) of the galaxies in the Local Universe (e.g. Eke et al. 2004, MNRAS, 348, 866; Tago et al. 2008, A&A, 479, 927). Furthermore, the fraction of star forming galaxies in groups lies in between clusters (<30%) and field (>30%). This fact suggests the presence of pre-processing mechanisms, acting on galaxies during the formation/virialization of groups, partly quenching star formation well before a group eventually fall into a cluster (e.g. Zabludoff & Mulchay 1998, ApJ, 498, L5; Bai et al. 2010, ApJ, 713, 637 and reference therein). The impact of the pre-processing operated by the group environments is still under debate, and several mechanisms, from merging to strangulation (e.g. Kawata & Mulchaey 2008, ApJ, 672, L103) have been proposed. During the group gravitational collapse, such mechanisms transform field, i.e. gas rich, mostly late-type galaxies, into cluster-like galaxies, i.e. gas poor, mostly early-type galaxies. We present here a UV-optical and kinematical analysis of two groups: USGC U268 and USGC U376 (U268 and U376 hereafter, Ramella et al.