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A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques. -
ARRAKIS: Atlas of Resonance Rings As Known in The
Astronomy & Astrophysics manuscript no. arrakis˙v12 c ESO 2018 September 28, 2018 ARRAKIS: atlas of resonance rings as known in the S4G⋆,⋆⋆ S. Comer´on1,2,3, H. Salo1, E. Laurikainen1,2, J. H. Knapen4,5, R. J. Buta6, M. Herrera-Endoqui1, J. Laine1, B. W. Holwerda7, K. Sheth8, M. W. Regan9, J. L. Hinz10, J. C. Mu˜noz-Mateos11, A. Gil de Paz12, K. Men´endez-Delmestre13 , M. Seibert14, T. Mizusawa8,15, T. Kim8,11,14,16, S. Erroz-Ferrer4,5, D. A. Gadotti10, E. Athanassoula17, A. Bosma17, and L.C.Ho14,18 1 University of Oulu, Astronomy Division, Department of Physics, P.O. Box 3000, FIN-90014, Finland e-mail: [email protected] 2 Finnish Centre of Astronomy with ESO (FINCA), University of Turku, V¨ais¨al¨antie 20, FI-21500, Piikki¨o, Finland 3 Korea Astronomy and Space Science Institute, 776, Daedeokdae-ro, Yuseong-gu, Daejeon 305-348, Republic of Korea 4 Instituto de Astrof´ısica de Canarias, E-38205 La Laguna, Tenerife, Spain 5 Departamento de Astrof´ısica, Universidad de La Laguna, E-38200, La Laguna, Tenerife, Spain 6 Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487 7 European Space Agency, ESTEC, Keplerlaan 1, 2200 AG, Noorwijk, the Netherlands 8 National Radio Astronomy Observatory/NAASC, 520 Edgemont Road, Charlottesville, VA 22903, USA 9 Space Telescope Science Institute, 3700 San Antonio Drive, Baltimore, MD 21218, USA 10 European Southern Observatory, Casilla 19001, Santiago 19, Chile 11 MMTO, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 12 Departamento de Astrof´ısica, -
Integral Field Spectroscopy of the Nearby Spiral Galaxy NGC 5668
Mem. S.A.It. Suppl. Vol. 14, 271 Memorie della c SAIt 2010 Supplementi Integral Field Spectroscopy of the nearby spiral galaxy NGC 5668 R.A. Marino1, A. Gil de Paz1, A. Castillo-Morales1, J.C. Munoz-Mateos˜ 1, and S.F. Sanchez´ 2 1 Departamento de Astrof´ısica y CC. de la Atmosfera,´ Universidad Complutense de Madrid, Madrid 28040, Spain 2 Centro Astronomico´ H´ıspano Aleman,´ Calar Alto, CSIC-MPG, C/Jesus´ Durban´ Remon´ 2-2, E-04004 Almeria, Spain Abstract. We analyze the full bi-dimensional spectral cube of the nearby spiral galaxy NGC 5668, which was obtained as a mosaic of 6 pointings, covering a total area of 2 × 3 arcmin2, obtained with the PPAK Integral Field Unit at the Calar Alto (CAHA) obser- vatory 3.5 m telescope. From these data we derive maps of the attenuation of the ionized gas (from the Hα / Hβ Balmer decrement), electron density (from the [SII]6717Å/ [SII]6731Å ratio), and chemical abundances, of both oxygen (using either the Te based method when possible or strong line methods such as the R23), and nitrogen. In addition to these maps, we also extract the spectra of individual HII regions by adding the flux over several PPAK fibers to increase the signal-to-noise ratio of the spectra and reduce the uncertainties in the properties derived. Along with the study of the ionized gas we also embark in the analysis of the absorption-line spectrum dominating the bulge and inter-arm regions. The spectra of these regions are compared with the predictions of evolutionary synthesis models for evolved stellar populations. -
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 -
The Crab Nebula Imaged by the Hubble Space Telescope in 1999 and 2000
Astronomers’ Observing Guides Other titles in this series The Moon and How to Observe It Peter Grego Double & Multiple Stars, and How to Observe Them James Mullaney Saturn and How to Observe it Julius Benton Jupiter and How to Observe it John McAnally Star Clusters and How to Observe Them Mark Allison Nebulae and How to Observe Them Steven Coe Galaxies and How to Observe Them Wolfgang Steinicke and Richard Jakiel Related titles Field Guide to the Deep Sky Objects Mike Inglis Deep Sky Observing Steven R. Coe The Deep-Sky Observer’s Year Grant Privett and Paul Parsons The Practical Astronomer’s Deep-Sky Companion Jess K. Gilmour Observing the Caldwell Objects David Ratledge Choosing and Using a Schmidt-Cassegrain Telescope Rod Mollise Martin Mobberley Supernovae and How to Observe Them with 167 Illustrations Martin Mobberley [email protected] Library of Congress Control Number: 2006928727 ISBN-10: 0-387-35257-0 e-ISBN-10: 0-387-46269-4 ISBN-13: 978-0387-35257-2 e-ISBN-13: 978-0387-46269-1 Printed on acid-free paper. © 2007 Springer Science+Business Media, LLC All rights reserved. This work may not be translated or copied in whole or in part without the written permission of the publisher (Springer Science+Business Media, LLC, 233 Spring Street, New York, NY 10013, USA), except for brief excerpts in connection with reviews or scholarly analysis. Use in connection with any form of information storage and retrieval, electronic adaptation, computer software, or by similar or dissimilar methodology now known or hereafter developed is forbidden. The use in this publication of trade names, trademarks, service marks, and similar terms, even if they are not identified as such, is not to be taken as an expression of opinion as to whether or not they are subject to proprietary rights. -
TABLE 1 Explanation of CVRHS Symbols A
TABLE 1 Explanation of CVRHS Symbols a Symbol Description 1 2 General Terms ETG An early-type galaxy, collectively referring to a galaxy in the range of types E to Sa ITG An intermediate-type galaxy, taken to be in the range Sab to Sbc LTG A late-type galaxy, collectively referring to a galaxy in the range of types Sc to Im ETS An early-type spiral, taken to be in the range S0/a to Sa ITS An intermediate-type spiral, taken to be in the range Sab to Sbc LTS A late-type spiral, taken to be in the range Sc to Scd XLTS An extreme late-type spiral, taken to be in the range Sd to Sm classical bulge A galaxy bulge that likely formed from early mergers of smaller galaxies (Kormendy & Kennicutt 2004; Athanassoula 2005) pseudobulge A galaxy bulge made of disk material that has secularly collected into the central regions of a barred galaxy (Kormendy 2012) PDG A pure disk galaxy, a galaxy lacking a classical bulge and often also lacking a pseudobulge Stage stage The characteristic of galaxy morphology that recognizes development of structure, the widespread distribution of star formation, and the relative importance of a bulge component along a sequence that correlates well with basic characteristics such as integrated color, average surface brightness, and HI mass-to-blue luminosity ratio Elliptical Galaxies E galaxy A galaxy having a smoothly declining brightness distribution with little or no evidence of a disk component and no inflections (such as lenses) in the luminosity distribution (examples: NGC 1052, 3193, 4472) En An elliptical galaxy -
A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im. -
Diffuse Neutral Hydrogen in the HI Parkes All Sky Survey
Astronomy & Astrophysics manuscript no. popping˙rhipass c ESO 2018 December 2, 2018 Diffuse neutral hydrogen in the H i Parkes All Sky Survey A. Popping12 and R. Braun3 1 Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, the Netherlands 2 International Centre for Radio Astronomy Research, The University of Western Australia, 35 Stirling Hwy, Crawley, WA 6009, Australia 3 CSIRO Astronomy and Space Science, P.O. Box 76, Epping, NSW 1710, Australia ABSTRACT Context. Observations of neutral hydrogen can provide a wealth of information about the distribution and kinematics of galaxies. To learn more about large scale structures and accretion processes, the extended environment of galaxies must also be observed. Numerical simulations predict a cosmic web of extended structures and gaseous filaments. Aims. To detect H i beyond the ionisation edge of galaxy disks, column density sensitivities have to be achieved that probe the regime of Lyman 19 2 limit systems. Typically H i observations are limited to a brightness sensitivity of NHI 10 cm− but this has to be improved by at least an order of magnitude. ∼ Methods. In this paper, reprocessed data is presented that was originally observed for the H i Parkes All Sky Survey (HIPASS). HIPASS provides complete coverage of the region that has been observed for the Westerbork Virgo Filament H i Survey (WVFS), presented in accompanying papers, and thus is an excellent product for data comparison. The region of interest extends from 8 to 17 hours in right ascension and from 1 − to 10 degrees in declination. Although the original HIPASS product already has good flux sensitivity, the sensitivity and noise characteristics can be significantly improved with a different processing method. -
PROGRESS REPORT Period: 2010-2013
CAMPUS MONCLOA CAMPUS OF INTERNATIONAL EXCELLENCE Universities Complutense and Technical University Madrid PROGRESS REPORT Period: 2010-2013 www.campusmoncloa.es Project Data: MONCLOA CAMPUS: THE POWER OF DIVERSITY (Ref.: CEI09-0019) Type of CIE: Global X Acronym: CEI Moncloa Campus Coordinating University: Universidad Complutense de Madrid Partner / Promotor Universities: COMPLUTENSE UNIVERSITY OF MADRID (UCM) and TECHNICAL UNIVERSITY OF MADRID (UPM) Other CIE institutional promotors: Agencia Estatal de Meteorología (AEMET) Ayuntamiento de Madrid Central Lechera Asturiana (CAPSA) Centre for Energy, Environment and Technology Research (CIEMAT) Madrid Autonomous Community Spanish National Research Council (CSIC) Fundación Juan José López Ibor Fundación madri+d para el Conocimiento Fundación para la Investigación Biomédica del Hospital Gregorio Marañón (FIBHGM) Hospital Universitario 12 de Octubre (H12O) Global Forecasters, S.L. Hospital Clínico San Carlos (HCSC) Indra Instituto de Salud Carlos III (ISCIII) Instituto del Patrimonio Cultural de España (IPCE) Instituto Geológico y Minero de España (IGME) Instituto Nacional de Investigación y Tecnología Agraria y Alimentaria (INIA) Instituto Tecnológico PET Parque Científico de Madrid (PCM) Patrimonio Nacional (PN) University of Colorado Denver 2 Progress Report: Nº 3 (2013) Period: 2010-June 2013 Coordinators from Partner /Promotor Institutions: J. Francisco Tirado Fernández, Vice-Chancellor for Research, UCM Roberto Prieto López, Vice-Chancellor for Research, UPM Tel: 91 394 71 90 E-mail: [email protected] Project web page: http://www.campusmoncloa.es/ CEI CAMPUS MONCLOA Table of contents 1. Brief Summarry for Publication __________________________________________ 5 2. Qualitative and Quantitative Description _________________________________ 10 INTRODUCTION _________________________________________________________ 11 Table I. Description of project actions ___________________________________________ 15 3. Governance of the project ____________________________________________ 191 4. -
Recent Results from the Spitzer Space Telescope: a New View of the Infrared Universe
RECENT RESULTS FROM THE SPITZER SPACE TELESCOPE: A NEW VIEW OF THE INFRARED UNIVERSE Giovanni G. Fazio Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA Abstract The Spitzer Space Telescope, NASA’s Great Observatory for infrared explo- ration, was launched on August 25, 2003, and is returning excellent scientific data. Combining the intrinsic sensitivity obtained with a cooled telescope in space and the imaging and spectroscopic power of modern array detectors, huge gains have been achieved in exploring the infrared universe. This paper de- scribes the Spitzer Space Telescope and its focal-plane instruments and summa- rizes some of the spectacular images and new scientific results that have been obtained. Keywords: infrared – galaxy classification – interstellar dust – star formation – interacting galaxies – active galactic nuclei – planetary nebula 1. Introduction Infrared astronomy, which covers the wavelength region from 1 to 1000 m, is concerned primarily with the study of relatively cold objects in the universe with temperatures ranging from a few degrees Kelvin to about 2000 K. One principal source of infrared radiation in the interstellar medium is dust, which absorbs optical and ultraviolet radiation and reradiates at infrared wavelengths. Infrared observations can also penetrate dust-enshrouded sources, which are invisible to optical and ultraviolet radiation. Observations of the early universe at infrared wavelengths have the advantage of seeing galaxies whose optical light has been redshifted into the infrared. However, when using ground-based telescopes, most of the infrared spec- trum in invisible because of atmospheric absorption (Figure 1). Only a few windows from 1 to 30 m wavelength are available. -
Integral Field Spectroscopy of the Nearby Spiral Galaxy NGC 5668
Highlights of Spanish Astrophysics VI, Proceedings of the IX Scientific Meeting of the Spanish Astronomical Society held on September 13 - 17, 2010, in Madrid, Spain. M. R. Zapatero Osorio et al. (eds.) Integral field spectroscopy of the nearby spiral galaxy NGC 5668 R. A. Marino12, A. Gil de Paz1, A. Castillo-Morales1, J. C. Mu~noz-Mateos1, and S. F. S´anchez2 1 Departamento de Astrof´ısicay CC. de la Atm´osfera,Universidad Complutense de Madrid, Madrid 28040, Spain 2 Centro Astron´omico Hispano Alem´an,Calar Alto, CSIC-MPG, C/Jes´usDurb´anRem´on 2-2, E-04004 Almeria, Spain Abstract We analyze the full bi-dimensional spectral cube of the nearby spiral galaxy NGC 5668, which was obtained as a mosaic of 6 pointings, covering a total area of 2 × 3 arcmin2, obtained with the PPAK Integral Field Unit at the Calar Alto (CAHA) observatory 3.5 m telescope. From these data we the bidimensional spatial distribution maps of the attenuation of the ionized gas (from the Hα=Hβ Balmer decrement), and chemical abundances of oxygen (using strong line methods such as the R23). In addition to these maps, we also extract the spectra of individual HII regions by adding the flux over several PPAK fibers to increase the signal-to-noise ratio of the spectra and reduce the uncertainties in the properties derived. The spectra of these regions are compared with the predictions of evolutionary synthesis models for evolved stellar populations. Both the measurements of spectroscopic indices and the full spectra will be used. Finally, given that most of the properties of the stars, gas, and dust in galaxies vary with radius the spectra of concentric annuli are also extracted and analyzed.