DOCSLIB.ORG

Cvn – Objektauswahl NGC Seite 1

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Cvn – Objektauswahl NGC Seite 1 CVn – Objektauswahl NGC Seite 1 NGC 4109 NGC 4151 NGC 4220 NGC 4288 NGC 4449 NGC 4619 NGC 4707 NGC 4846 NGC 4956 NGC 4111 NGC 4156 NGC 4226 NGC 4346 NGC 4460 NGC 4625 NGC 4711 NGC 4861 NGC 4959 NGC 4117 NGC 4163 NGC 4227 NGC 4357 NGC 4485 NGC 4627 NGC 4719 NGC 4868 NGC 4963 Seite 2 NGC 4118 NGC 4229 NGC 4369 NGC 4490 NGC 4631 NGC 4736 NGC 4870 NGC 4985 NGC 4135 NGC 4183 NGC 4231 NGC 4389 NGC 4509 NGC 4655 NGC 4737 NGC 4893 NGC 4986 Seite 3 NGC 4137 NGC 4187 NGC 4232 NGC 4392 NGC 4534 NGC 4656 NGC 4741 NGC 4901 NGC 4987 NGC 4138 NGC 4190 NGC 4242 NGC 4395 NGC 4542 NGC 4657 NGC 4774 NGC 4914 NGC 4998 NGC 4143 NGC 4214 NGC 4244 NGC 4399 NGC 4583 NGC 4662 NGC 4800 NGC 4917 NGC 5002 NGC 4145 NGC 4217 NGC 4248 NGC 4400 NGC 4617 NGC 4687 NGC 4834 NGC 4932 NGC 5003 NGC 4148 NGC 4218 NGC 4258 NGC 4401 NGC 4618 NGC 4704 NGC 4837 NGC 4938 NGC 5005 Sternbild- Zur Objektauswahl: Nummer anklicken Übersicht Zur Übersichtskarte: Objekt in Aufsuchkarte anklicken Zum Detailfoto: Objekt in Übersichtskarte anklicken CVn – Objektauswahl NGC Seite 2 NGC 5009 NGC 5083 NGC 5131 NGC 5173 NGC 5229 NGC 5272 NGC 5290 NGC 5319 NGC 5349 NGC 5014 NGC 5093 NGC 5141 NGC 5187 NGC 5233 NGC 5273 NGC 5296 NGC 5320 NGC 5350 Seite 1 NGC 5021 NGC 5096 NGC 5142 NGC 5194 NGC 5238 NGC 5274 NGC 5297 NGC 5321 NGC 5351 NGC 5023 NGC 5098 NGC 5143 NGC 5195 NGC 5240 NGC 5275 NGC 5301 NGC 5325 NGC 5352 NGC 5025 NGC 5103 NGC 5145 NGC 5198 NGC 5243 NGC 5276 NGC 5303 NGC 5326 NGC 5353 Seite 3 NGC 5029 NGC 5107 NGC 5149 NGC 5199 NGC 5259 NGC 5277 NGC 5305 NGC 5336 NGC 5354 NGC 5033 NGC 5112 NGC 5154 NGC 5214 NGC 5263 NGC 5280 NGC 5311 NGC 5337 NGC 5355 NGC 5040 NGC 5117 NGC 5157 NGC 5223 NGC 5265 NGC 5282 NGC 5312 NGC 5341 NGC 5358 NGC 5055 NGC 5123 NGC 5166 NGC 5225 NGC 5267 NGC 5287 NGC 5313 NGC 5346 NGC 5361 NGC 5074 NGC 5127 NGC 5169 NGC 5228 NGC 5271 NGC 5289 NGC 5318 NGC 5347 NGC 5362 Sternbild- Zur Objektauswahl: Nummer anklicken Übersicht Zur Übersichtskarte: Objekt in Aufsuchkarte anklicken Zum Detailfoto: Objekt in Übersichtskarte anklicken CVn – Objektauswahl NGC Seite 3 NGC 5371 NGC 5403 NGC 5375 NGC 5406 Seite 1 NGC 5377 NGC 5407 Seite 2 NGC 5378 NGC 5410 NGC 5380 NGC 5421 NGC 5383 NGC 5433 NGC 5394 NGC 5439 NGC 5395 NGC 5440 NGC 5399 NGC 5444 NGC 5401 NGC 5445 Sternbild- Zur Objektauswahl: Nummer anklicken Übersicht Zur Übersichtskarte: Objekt in Aufsuchkarte anklicken Zum Detailfoto: Objekt in Übersichtskarte anklicken CVn Übersichtskarte Boo UMa Com Auswahl NGC 4109_11_17_18_35_37_38_43_83_4449_60_85_90 Aufsuchkarte Auswahl NGC 4145_4151_4156_4369 Aufsuchkarte 6 CVn 6 Auswahl NGC 4148_63_90_4214_27_29_44_4395_99_4400_01 Aufsuchkarte 6 CVn Auswahl NGC 4187 Aufsuchkarte Auswahl NGC 4217_18_20_26_31_32_42_48_58_88_4346_57_89_92 Aufsuchkarte Auswahl NGC 4509_4583_4627_4631_4656_4657_4719_4737 Aufsuchkarte Auswahl NGC 4534_4619_4662_4687_4711_4774 Aufsuchkarte Auswahl NGC 4542_4617_4707 Aufsuchkarte Auswahl NGC 4618_4625_4655_4704_4736 Aufsuchkarte Auswahl NGC 4741_4800_4837_4901_4917_5021_5029 Aufsuchkarte Auswahl NGC 4834_4932_4938_4987_4998_5009_5040 Aufsuchkarte CVn 21 Auswahl NGC 4846_4868_4870_4893_4914 Aufsuchkarte Auswahl NGC 4861_4956_4959_4986_5025_5074_5096_5098 Aufsuchkarte Auswahl NGC 4963_4985_5003_5023_5055 Aufsuchkarte Auswahl NGC 5002_5005_5014_5033 Aufsuchkarte Auswahl NGC 5083_5093_5107_5112 Aufsuchkarte Auswahl NGC 5103_5123_5145_5214 Aufsuchkarte Auswahl NGC 5117_27_31_57_66_87_5259_63_71_72_74_75_77_80_82_87_5312_18_19_21 Aufsuchkarte Auswahl NGC 5141_42_43_49_54_99_5223_28_33_40 Aufsuchkarte Auswahl NGC 5169_73_94_95_98_5229_96_97_5301_36_77_5439 Aufsuchkarte Auswahl NGC 5225_5238 Aufsuchkarte Auswahl NGC 5243_65_67_5303_05_25_41_49_51_52_61_78_80_94_95_5401_03_ 06_07 Aufsuchkarte Auswahl NGC 5273_5276 Aufsuchkarte Auswahl NGC 5289_5290 Aufsuchkarte Auswahl NGC 5311_13_20_26_37_46_50_53_54_55_58_62_71_83_5410 Aufsuchkarte Auswahl NGC 5347_5375_5421_5433 Aufsuchkarte Auswahl NGC 5399_5440_5444_5445 Aufsuchkarte Auswahl NGC 4109_4111_4117_4118_4143 Übersichtskarte Aufsuch- Auswahl karte NGC 4135_4137_4138_4183 Übersichtskarte Aufsuch- Auswahl karte NGC 4145_4151_4156 Übersichtskarte Aufsuch- Auswahl karte NGC 4148_4163 Übersichtskarte Aufsuch- Auswahl karte NGC 4187 Übersichtskarte Aufsuch- Auswahl karte NGC 4190_4214 Übersichtskarte Aufsuch- Auswahl karte NGC 4217_4226_4231_4232_4248_4258 Übersichtskarte Aufsuch- Auswahl karte NGC 4218_4220 Übersichtskarte Aufsuch- Auswahl karte NGC 4227_4229 Übersichtskarte Aufsuch- Auswahl karte NGC 4242_4288 Übersichtskarte Aufsuch- Auswahl karte NGC 4244 Übersichtskarte Aufsuch- Auswahl karte NGC 4346 Übersichtskarte Aufsuch- Auswahl karte NGC 4357 Übersichtskarte Aufsuch- Auswahl karte NGC 4369 Übersichtskarte Aufsuch- Auswahl karte NGC 4389_4392 Übersichtskarte Aufsuch- Auswahl karte NGC 4395_4399_4400_4401 Übersichtskarte Aufsuch- Auswahl karte NGC 4449_4460 Übersichtskarte Aufsuch- Auswahl karte NGC 4485_4490 Übersichtskarte Aufsuch- Auswahl karte NGC 4509 Übersichtskarte Aufsuch- Auswahl karte NGC 4534 Übersichtskarte Aufsuch- Auswahl karte NGC 4542 Übersichtskarte Aufsuch- Auswahl karte NGC 4583 Übersichtskarte Aufsuch- Auswahl karte NGC 4617 Übersichtskarte Aufsuch- Auswahl karte NGC 4618_4625_4655 Übersichtskarte Aufsuch- Auswahl karte NGC 4619 Übersichtskarte Aufsuch- Auswahl karte NGC 4627_4631_4656_4657 Übersichtskarte Aufsuch- Auswahl karte NGC 4662 Übersichtskarte Aufsuch- Auswahl karte NGC 4687_4711 Übersichtskarte Aufsuch- Auswahl karte NGC 4704 Übersichtskarte Aufsuch- Auswahl karte NGC 4707 Übersichtskarte Aufsuch- Auswahl karte NGC 4719 Übersichtskarte Aufsuch- Auswahl karte NGC 4736 Übersichtskarte Aufsuch- Auswahl karte NGC 4737 Übersichtskarte Aufsuch- Auswahl karte NGC 4741 Übersichtskarte Aufsuch- Auswahl karte NGC 4774 Übersichtskarte Aufsuch- Auswahl karte NGC 4800 Übersichtskarte Aufsuch- Auswahl karte NGC 4834 Übersichtskarte Aufsuch- Auswahl karte NGC 4837 Übersichtskarte Aufsuch- Auswahl karte NGC 4846 Übersichtskarte Aufsuch- Auswahl karte NGC 4861 Übersichtskarte Aufsuch- Auswahl karte NGC 4868_4870_4893_4914 Übersichtskarte Aufsuch- Auswahl karte NGC 4901_4917 Übersichtskarte Aufsuch- Auswahl karte NGC 4932_4938 Übersichtskarte Aufsuch- Auswahl karte NGC 4956_4986 Übersichtskarte Aufsuch- Auswahl karte NGC 4959 Übersichtskarte Aufsuch- Auswahl karte NGC 4963_4985 Übersichtskarte Aufsuch- Auswahl karte NGC 4987 Übersichtskarte Aufsuch- Auswahl karte NGC 4998 Übersichtskarte Aufsuch- Auswahl karte NGC 5002_5005_5014_5033 Übersichtskarte Aufsuch- Auswahl karte NGC 5003_5023 Übersichtskarte Aufsuch- Auswahl karte NGC 5009 Übersichtskarte Aufsuch- Auswahl karte NGC 5021_5029 Übersichtskarte Aufsuch- Auswahl karte NGC 5025 Übersichtskarte Aufsuch- Auswahl karte NGC 5040 Übersichtskarte Aufsuch- Auswahl karte NGC 5055 Übersichtskarte Aufsuch- Auswahl karte NGC 5074 Übersichtskarte Aufsuch- Auswahl karte NGC 5083_5093 Übersichtskarte Aufsuch- Auswahl karte NGC 5096_5098 Übersichtskarte Aufsuch- Auswahl karte NGC 5103_5123_5145 Übersichtskarte Aufsuch- Auswahl karte NGC 5107_5112 Übersichtskarte Aufsuch- Auswahl karte NGC 5117 Übersichtskarte Aufsuch- Auswahl karte NGC 5127_5131 Übersichtskarte Aufsuch- Auswahl karte NGC 5141_5142_5143 Übersichtskarte Aufsuch- Auswahl karte NGC 5149_5154 Übersichtskarte Aufsuch- Auswahl karte NGC 5157_5166 Übersichtskarte Aufsuch- Auswahl karte NGC 5169_5173_5194_5195_5198 Übersichtskarte Aufsuch- Auswahl karte NGC 5187 Übersichtskarte Aufsuch- Auswahl karte NGC 5199_5224_5228_5233 Übersichtskarte Aufsuch- Auswahl karte NGC 5214 Übersichtskarte Aufsuch- Auswahl karte NGC 5225_5238 Übersichtskarte Aufsuch- Auswahl karte NGC 5229 Übersichtskarte Aufsuch- Auswahl karte NGC 5240 Übersichtskarte Aufsuch- Auswahl karte NGC 5243_5267 Übersichtskarte Aufsuch- Auswahl karte NGC 5259 Übersichtskarte Aufsuch- Auswahl karte NGC 5263_5272 Übersichtskarte Aufsuch- Auswahl karte NGC 5265 Übersichtskarte Aufsuch- Auswahl karte NGC 5271_74_75_77_80_82_87 Übersichtskarte Aufsuch- Auswahl karte NGC 5273_5276 Übersichtskarte Aufsuch- Auswahl karte NGC 5289_5290 Übersichtskarte Aufsuch- Auswahl karte NGC 5296_5297 Übersichtskarte Aufsuch- Auswahl karte NGC 5301 Übersichtskarte Aufsuch- Auswahl karte NGC 5303_5305_5325 Übersichtskarte Aufsuch- Auswahl karte NGC 5311_5313_5326_5337_5346 Übersichtskarte Aufsuch- Auswahl karte NGC 5312_5318_5319_5321 Übersichtskarte Aufsuch- Auswahl karte NGC 5320 Übersichtskarte Aufsuch- Auswahl karte NGC 5336 Übersichtskarte Aufsuch- Auswahl karte NGC 5341_5349_5351 Übersichtskarte Aufsuch- Auswahl karte NGC 5347 Übersichtskarte Aufsuch- Auswahl karte NGC 5350_5353_5354_5355_5356_5371 Übersichtskarte Aufsuch- Auswahl karte NGC 5352 Übersichtskarte Aufsuch- Auswahl karte NGC 5361 Übersichtskarte Aufsuch- Auswahl karte NGC 5362_5383 Übersichtskarte Aufsuch- Auswahl karte NGC 5375 Übersichtskarte Aufsuch- Auswahl karte NGC 5377 Übersichtskarte Aufsuch- Auswahl karte NGC 5378_5380_5394_5395_5403 Übersichtskarte Aufsuch- Auswahl karte NGC 5399 Übersichtskarte Aufsuch- Auswahl karte NGC 5401 Übersichtskarte Aufsuch- Auswahl karte NGC 5406_5407 Übersichtskarte Aufsuch- Auswahl karte NGC 5410 Übersichtskarte Aufsuch- Auswahl karte NGC 5421 Übersichtskarte Aufsuch- Auswahl karte NGC 5433 Übersichtskarte Aufsuch- Auswahl karte NGC 5439 Übersichtskarte Aufsuch- Auswahl karte NGC 5440_5444_5445 Übersichtskarte Aufsuch- Auswahl karte NGC 4109_4111 Detailfoto 4.‘8 x1.‘1 m 4111 NGC 0.‘8 x0.‘7 m 4109 NGC Übersichts- p p Auswahl = 11. = 15. karte m m 7 0 NGC 4117_4118 Detailfoto 0.‘9x 0.‘5 m 4118 NGC 2.‘8 x1.‘1 m 4117 NGC Übersichts- p p Auswahl = 15.
Load more

Recommended publications
  • The HERACLES View of the H -To-HI Ratio in Galaxies
    The HERACLES View of the H2-to-HI Ratio in Galaxies Adam Leroy (NRAO, Hubble Fellow) Fabian Walter, Frank Bigiel, the HERACLES and THINGS teams The Saturday Morning Summary • Star formation rate vs. gas relation on ~kpc scales breaks apart into: A relatively universal CO-SFR relation in nearby disks Systematic environmental scalings in the CO-to-HI ratio • The CO-to-HI ratio is a strong function of radius, total gas, and stellar surface density correlated with ISM properties: dust-to-gas ratio, pressure harder to link to dynamics: gravitational instability, arms • Interpretation: the CO-to-HI ratio traces the efficiency of GMC formation Density and dust can explain much of the observed behavior heracles Fabian Walter Erik Rosolowsky MPIA UBC Frank Bigiel Eva Schinnerer UC Berkeley THINGS plus… MPIA Elias Brinks Antonio Usero Gaelle Dumas U Hertfordshire OAN, Madrid MPIA Erwin de Blok Andreas Schruba Helmut Wiesemeyer U Cape Town IRAM … MPIA Rob Kennicutt Axel Weiss Karl Schuster Cambridge MPIfR IRAM Barry Madore Carsten Kramer Karin Sandstrom Carnegie IRAM MPIA Michele Thornley Daniela Calzetti Kelly Foyle Bucknell UMass MPIA Collaborators The HERA CO-Line Extragalactic Survey First maps Leroy et al. (2009) • IRAM 30m Large Program to map CO J = 2→1 line • Instrument: HERA receiver array operating at 230 GHz • 47 galaxies: dwarfs to starbursts and massive spirals -2 • Very wide-field (~ r25) and sensitive (σ ~ 1-2 Msun pc ) NGS The HI Nearby Galaxy Survey HI Walter et al. (2008), AJ Special Issue (2008) • VLA HI maps of 34 galaxies:
    [Show full text]
  • High Resolution HI Distributions and Multi-Wavelength Analyses Of
    High Resolution H I Distributions and Multi-Wavelength Analyses of Magellanic Spirals NGC 4618 and NGC 4625 Jane F. Kaczmarek1& Eric M. Wilcots University of Wisconsin Madison, Department of Astronomy, 475 N. Charter Street, Madison WI 53706 USA [email protected], [email protected] ABSTRACT We present a detailed analysis of high resolution H I observations of the Magellanic spiral galaxies NGC 4618 and NGC 4625. While the H I disk of NGC 4625 is remarkably quiescent with a nearly uniform velocity dispersion and no evidence of H I holes, there is a dynamic interplay between star formation and the distribution of neutral hydrogen in NGC 4618. We calculate the critical density for widespread star formation in each galaxy and find that star formation proceeds even where the surface density of the atomic gas is well below the critical density necessary for global star formation. There are strong spatial correlations in NGC 4618 between UV emission, 1.4 GHz radio continuum emission, and peaks in the H I column density. Despite the apparent overlap of the outer disks of the two galaxies, we find that they are kinematically distinct, indicating that NGC 4618 and NGC 4625 are not interacting. The structure of NGC 4618 and, in particular, the nature of its outer ring, are highly suggestive of an interaction, but the timing and nature of such an interaction remain unclear. Subject headings: galaxies: neutral hydrogen { galaxies: Magellanic spirals { galaxies: individual (NGC 4618 & NGC 4625) 1. Introduction arXiv:1206.4104v1 [astro-ph.CO] 19 Jun 2012 One of the more stunning revelations about the Local Group in the past few years has been the observations of the proper motions of the Magellanic Clouds showing that they are moving at significantly higher velocities than previously thought (e.g.
    [Show full text]
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • The Metallicity-Luminosity Relationship of Dwarf Irregular Galaxies
    A&A 399, 63–76 (2003) Astronomy DOI: 10.1051/0004-6361:20021748 & c ESO 2003 Astrophysics The metallicity-luminosity relationship of dwarf irregular galaxies II. A new approach A. M. Hidalgo-G´amez1,,F.J.S´anchez-Salcedo2, and K. Olofsson1 1 Astronomiska observatoriet, Box 515, 751 20 Uppsala, Sweden e-mail: [email protected], [email protected] 2 Instituto de Astronom´ıa-UNAM, Ciudad Universitaria, Apt. Postal 70 264, C.P. 04510, Mexico City, Mexico e-mail: [email protected] Received 21 June 2001 / Accepted 21 November 2002 Abstract. The nature of a possible correlation between metallicity and luminosity for dwarf irregular galaxies, including those with the highest luminosities, has been explored using simple chemical evolutionary models. Our models depend on a set of free parameters in order to include infall and outflows of gas and covering a broad variety of physical situations. Given a fixed set of parameters, a non-linear correlation between the oxygen abundance and the luminosity may be established. This would be the case if an effective self–regulating mechanism between the accretion of mass and the wind energized by the star formation could lead to the same parameters for all the dwarf irregular galaxies. In the case that these parameters were distributed in a random manner from galaxy to galaxy, a significant scatter in the metallicity–luminosity diagram is expected. Comparing with observations, we show that only variations of the stellar mass–to–light ratio are sufficient to explain the observed scattering and, therefore, the action of a mechanism of self–regulation cannot be ruled out.
    [Show full text]
  • Flat Galaxy - Above 30 Deg
    Flat Galaxy - Above 30 Deg. DEC A B C D E F G H I J K L 1 Const. Object ID Other ID RA Dec Size (arcmin) Mag Urano. Urano. Millennium Notes 2 RFGC NGC hh mm ss dd mm ss.s Major Minor 1st Ed. 2nd Ed. 3 CVn 2245 NGC 4244 12 17 30 +37 48 31 19.4 2.1 10.2 107 54 633 Vol II Note: 4 Com 2335 NGC 4565 12 36 21 +25 59 06 15.9 1.9 10.6 149 71 677 Vol II Note: Slightly asymmetric dust lane 5 Dra 2946 NGC 5907 15 15 52 +56 19 46 12.8 1.4 11.3 50 22 568 Vol II Note: 6 Vir 2315 NGC 4517 12 32 46 +00 06 53 11.5 1.5 11.3 238 110 773 Vol II Note: Dust spots 7 Vir 2579 NGC 5170 13 29 49 -17 57 57 9.9 1.2 11.8 285 130 842 Vol II Note: Eccentric dust lane 8 UMa 2212 NGC 4157 12 11 05 +50 29 07 7.9 1.1 12.2 47 37 592 Vol II Note: 9 Vir 2449 MCG-3-33-30 13 03 17 -17 25 23 8.0 1.1 12.5 284 130 843 Vol II Note: Four knots in the centre 10 CVn 2495 NGC 5023 13 12 12 +44 02 17 7.3 0.8 12.7 75 37 609 Vol II Note: 11 Hya 2682 IC 4351 13 57 54 -29 18 57 6.1 0.8 12.9 371 148 888 Vol II Note: Dust lane.
    [Show full text]
  • Astronomy Astrophysics
    A&A 433, 79–86 (2005) Astronomy DOI: 10.1051/0004-6361:20034537 & c ESO 2005 Astrophysics Asymmetrical structure of ionization and kinematics in the Seyfert galaxy NGC 5033 E. Mediavilla1, A. Guijarro2, A. Castillo-Morales3 , J. Jiménez-Vicente3, E. Florido3, S. Arribas4,, B. García-Lorenzo1, and E. Battaner3 1 Instituto de Astrofísica de Canarias, Tenerife, Spain e-mail: [email protected] 2 Centro Astronómico Hispano Alemán, Almería, Spain e-mail: [email protected] 3 Dpto. Física Teórica y del Cosmos, Universidad de Granada, Spain 4 Space Telescope Science Institute, Baltimore, USA Received 18 October 2003 / Accepted 29 November 2004 Abstract. We present integral field spectroscopy of NGC 5033, a low luminosity Seyfert galaxy. The observations were made with INTEGRAL, a fiber based system operating at the WHT. The intensity map of the Hβ emission line represents a spi- ral or ring-like pattern of HII regions. On the contrary, the [OIII] intensity map morphology is markedly anisotropic. The strong morphological differences imply that the [OIII] emitters represent highly ionized gas illuminated by the central source. The [OIII] map morphology is compatible with a biconical structure of ionization induced by strong extinction in the galaxy disc that also obscures half of the spheroidal stellar bulge. We identify the spectrum corresponding to the Seyfert 1 nucleus from the presence of Hβ broad emission lines. This spectrum is located in a region where strong extinction is expected but exhibits the bluest spectral energy distribution. The Seyfert 1 nucleus seems to be offcenter with respect to the stellar rotation center. This result has been also found in other Seyfert galaxies and interpreted in terms of a past merger.
    [Show full text]
  • EMISSION-LINE NUCLEI at HUBBLE SPACE TELESCOPE RESOLUTION1 Joseph C
    The Astrophysical Journal, 654:125Y137, 2007 January 1 # 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE SURVEY OF NEARBY NUCLEI WITH THE SPACE TELESCOPE IMAGING SPECTROGRAPH: EMISSION-LINE NUCLEI AT HUBBLE SPACE TELESCOPE RESOLUTION1 Joseph C. Shields,2 Hans-Walter Rix,3 Marc Sarzi,4 Aaron J. Barth,5 Alexei V. Filippenko,6 Luis C. Ho,7 Daniel H. McIntosh,8 Gregory Rudnick,9,10 and Wallace L. W. Sargent11 Received 2004 August 14; accepted 2006 September 8 ABSTRACT We present results from a program of optical spectroscopy for 23 nearby galaxies with emission-line nuclei. This investigation takes advantage of the spatial resolution of the Hubble Space Telescope to study the structure and energetics of the central 10Y20 pc, and the resulting data have value for quantifying central black hole masses, star formation histories, and nebular properties. This paper provides a description of the experimental design, and new findings from the study of emission lines. The sample targets span a range of nebular spectroscopic class, from H ii to Seyfert nuclei. This data set and the resulting measurements are unique in terms of the sample size, the range of nebular class, and the investigation of physical scales extending down to parsecs. The line ratios indicative of nebular ionization show only modest variations over order-of-magnitude differences in radius, and demonstrate in a sys- tematic way that geometrical dilution of the radiation field from a central source cannot be assumed as a primary driver of ionization structure. Comparisons between large- and small-aperture measurements for the H ii/LINER tran- sition objects provide a new test that challenges conventional wisdom concerning the composite nature of these systems.
    [Show full text]
  • 121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
    221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S.
    [Show full text]
  • Stsci Newsletter: 2011 Volume 028 Issue 02
    National Aeronautics and Space Administration Interacting Galaxies UGC 1810 and UGC 1813 Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA) 2011 VOL 28 ISSUE 02 NEWSLETTER Space Telescope Science Institute We received a total of 1,007 proposals, after accounting for duplications Hubble Cycle 19 and withdrawals. Review process Proposal Selection Members of the international astronomical community review Hubble propos- als. Grouped in panels organized by science category, each panel has one or more “mirror” panels to enable transfer of proposals in order to avoid conflicts. In Cycle 19, the panels were divided into the categories of Planets, Stars, Stellar Rachel Somerville, [email protected], Claus Leitherer, [email protected], & Brett Populations and Interstellar Medium (ISM), Galaxies, Active Galactic Nuclei and Blacker, [email protected] the Inter-Galactic Medium (AGN/IGM), and Cosmology, for a total of 14 panels. One of these panels reviewed Regular Guest Observer, Archival, Theory, and Chronology SNAP proposals. The panel chairs also serve as members of the Time Allocation Committee hen the Cycle 19 Call for Proposals was released in December 2010, (TAC), which reviews Large and Archival Legacy proposals. In addition, there Hubble had already seen a full cycle of operation with the newly are three at-large TAC members, whose broad expertise allows them to review installed and repaired instruments calibrated and characterized. W proposals as needed, and to advise panels if the panelists feel they do not have The Advanced Camera for Surveys (ACS), Cosmic Origins Spectrograph (COS), the expertise to review a certain proposal. Fine Guidance Sensor (FGS), Space Telescope Imaging Spectrograph (STIS), and The process of selecting the panelists begins with the selection of the TAC Chair, Wide Field Camera 3 (WFC3) were all close to nominal operation and were avail- about six months prior to the proposal deadline.
    [Show full text]
  • Arxiv:0907.4718V1 [Astro-Ph.GA] 27 Jul 2009 Nnab Aais Hi Ihlmnste ( Luminosities High Their Objects Point-Like Galaxies
    Submitted to Astrophysical Journal A Preprint typeset using L TEX style emulateapj v. 04/03/99 ULTRALUMINOUS X-RAY SOURCE CORRELATIONS WITH STAR-FORMING REGIONS Douglas A. Swartz1 Allyn F. Tennant2, and Roberto Soria3 Submitted to Astrophysical Journal ABSTRACT Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u − g, g − r and r − i colors are used to determine whether Ultraluminous X-ray sources (ULXs) are predominantly associated with star-forming regions of their host galaxies. An empirical selection criterion is derived from colors of H ii regions in M 81 and M 101 that differentiates between the young, blue stellar component and the older disk and bulge population. This criterion is applied to a sample of 58 galaxies of Hubble type S0 and later and verified through an application of Fisher’s linear discriminant analysis. It is found that 60% (49%) of ULXs in optically-bright environments are within regions blueward of their host galaxy’s H ii regions compared to only 27% (0%) of a control sample according to the empirical (Fisher) criterion. This is an excess of 3σ above the 32% (27%) expected if the ULXs were randomly distributed within their galactic hosts. This indicates a ULX preference for young, ∼<10 Myr, OB associations. However, none of the ULX environments have the morphology and optical brightness suggestive of a massive young super star cluster though several are in extended or crowded star-forming (blue) environments that may contain clusters unresolved by Sloan imaging. Ten of the 12 ULX candidates with estimated X-ray luminosities in excess of 3×1039 ergs s−1 are equally divided among the group of ULX environments redward of H ii regions and the group of optically faint regions.
    [Show full text]
  • University of Groningen Warps in Disk Galaxies Garcнa Ruiz, Iсigo
    University of Groningen Warps in disk galaxies García Ruiz, Iñigo 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: 2001 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): García Ruiz, I. (2001). Warps in disk galaxies. s.n. 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. Downloaded from the University of Groningen/UMCG research database (Pure): http://www.rug.nl/research/portal. For technical reasons the number of authors shown on this cover page is limited to 10 maximum. Download date: 07-10-2021 4 Neutral Hydrogen and Optical Observations of Edge-on Galaxies: The data Based on a paper by I. Garc´ıa-Ruiz, R. Sancisi & K.
    [Show full text]