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The Local Radio-Galaxy Population at 20
Mon. Not. R. Astron. Soc. 000, 1–?? (2013) Printed 2 December 2013 (MN LATEX style file v2.2) The local radio-galaxy population at 20GHz Elaine M. Sadler1⋆, Ronald D. Ekers2, Elizabeth K. Mahony3, Tom Mauch4,5, Tara Murphy1,6 1Sydney Institute for Astronomy, School of Physics, The University of Sydney, NSW 2006, Australia 2Australia Telescope National Facility, CSIRO, PO Box 76, Epping, NSW 1710, Australia 3ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA, Dwingeloo, The Netherlands 4Oxford Astrophysics, Department of Physics, Keble Road, Oxford OX1 3RH 5SKA Africa, 3rd Floor, The Park, Park Road, Pinelands, 7405, South Africa 6School of Information Technologies, The University of Sydney, NSW 2006, Australia Accepted 0000 December 08. Received 0000 December 08; in original form 0000 December 08 ABSTRACT We have made the first detailed study of the high-frequency radio-source population in the local universe, using a sample of 202 radio sources from the Australia Telescope 20GHz (AT20G) survey identified with galaxies from the 6dF Galaxy Survey (6dFGS). The AT20G- 6dFGS galaxies have a median redshift of z=0.058 and span a wide range in radio luminosity, allowing us to make the first measurement of the local radio luminosity function at 20GHz. Our sample includes some classical FR-1 and FR-2 radio galaxies, but most of the AT20G-6dFGS galaxies host compact (FR-0) radio AGN which appear lack extended radio emission even at lower frequencies. Most of these FR-0 sources show no evidence for rela- tivistic beaming, and the FR-0 class appears to be a mixed population which includes young Compact Steep-Spectrum (CSS) and Gigahertz-Peaked Spectrum (GPS) radio galaxies. -
The MASSIVE Survey-VIII. Stellar Velocity Dispersion Profiles And
MNRAS 000,1{17 (2017) Preprint 26 October 2017 Compiled using MNRAS LATEX style file v3.0 The MASSIVE Survey - VIII. Stellar Velocity Dispersion Profiles and Environmental Dependence of Early-Type Galaxies Melanie Veale,1;2? Chung-Pei Ma,1;2? Jenny E. Greene,3 Jens Thomas,4 John P. Blakeslee,5 Jonelle L. Walsh,6 Jennifer Ito1 1Department of Astronomy, University of California, Berkeley, CA 94720, USA 2Department of Physics, University of California, Berkeley, CA 94720, USA 3Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 4Max Plank-Institute for Extraterrestrial Physics, Giessenbachstr. 1, D-85741 Garching, Germany 5Dominion Astrophysical Observatory, NRC Herzberg Astronomy & Astrophysics, Victoria BC V9E2E7, Canada 6George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We measure the radial profiles of the stellar velocity dispersions, σ¹Rº, for 90 early-type galaxies (ETGs) in the MASSIVE survey, a volume-limited integral-field spectroscopic (IFS) galaxy survey targeting all northern-sky ETGs with absolute K-band magnitude > 11 MK < −25:3 mag, or stellar mass M∗ ∼ 4 × 10 M , within 108 Mpc. Our wide-field 10700×10700 IFS data cover radii as large as 40 kpc, for which we quantify separately the inner (2 kpc) and outer (20 kpc) logarithmic slopes γinner and γouter of σ¹Rº. While γinner is mostly negative, of the 56 galaxies with sufficient radial coverage to determine γouter we find 36% to have rising outer dispersion profiles, 30% to be flat within the uncertainties, and 34% to be falling. -
CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
Publ. Astron. Soc. Japan (2018) 00(0), 1–33 1 doi: 10.1093/pasj/xxx000 CO Multi-line Imaging of Nearby Galaxies (COMING) IV. Overview of the Project Kazuo SORAI1, 2, 3, 4, 5, Nario KUNO4, 5, Kazuyuki MURAOKA6, Yusuke MIYAMOTO7, 8, Hiroyuki KANEKO7, Hiroyuki NAKANISHI9 , Naomasa NAKAI4, 5, 10, Kazuki YANAGITANI6 , Takahiro TANAKA4, Yuya SATO4, Dragan SALAK10, Michiko UMEI2 , Kana MOROKUMA-MATSUI7, 8, 11, 12, Naoko MATSUMOTO13, 14, Saeko UENO9, Hsi-An PAN15, Yuto NOMA10, Tsutomu, T. TAKEUCHI16 , Moe YODA16, Mayu KURODA6, Atsushi YASUDA4 , Yoshiyuki YAJIMA2 , Nagisa OI17, Shugo SHIBATA2, Masumichi SETA10, Yoshimasa WATANABE4, 5, 18, Shoichiro KITA4, Ryusei KOMATSUZAKI4 , Ayumi KAJIKAWA2, 3, Yu YASHIMA2, 3, Suchetha COORAY16 , Hiroyuki BAJI6 , Yoko SEGAWA2 , Takami TASHIRO2 , Miho TAKEDA6, Nozomi KISHIDA2 , Takuya HATAKEYAMA4 , Yuto TOMIYASU4 and Chey SAITA9 1Department of Physics, Faculty of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 2Department of Cosmosciences, Graduate School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 3Department of Physics, School of Science, Hokkaido University, Kita 10 Nishi 8, Kita-ku, Sapporo 060-0810, Japan 4Division of Physics, Faculty of Pure and Applied Sciences, University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 5Tomonaga Center for the History of the Universe (TCHoU), University of Tsukuba, 1-1-1 Tennodai, Tsukuba, Ibaraki 305-8571, Japan 6Department of Physical Science, Osaka Prefecture University, Gakuen 1-1, -
THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B
The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M . -
Southern Arp - AM # Order
Southern Arp - AM # Order A B C D E F G H I J 1 AM # Constellation Object Name RA DEC Mag. Size Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 AM 0003-414 Phoenix ESO 293-G034 00h06m19.9s -41d30m00s 13.7 3.2 x 1.0 386 177 430 Vol I 4 AM 0006-340 Sculptor NGC 10 00h08m34.5s -33d51m30s 13.3 2.4 x 1.2 350 159 410 Vol I 5 AM 0007-251 Sculptor NGC 24 00h09m56.5s -24d57m47s 12.4 5.8 x 1.3 305 141 366 Vol I 6 AM 0011-232 Cetus NGC 45 00h14m04.0s -23d10m55s 11.6 8.5 x 5.9 305 141 366 Vol I 7 AM 0027-333 Sculptor NGC 134 00h30m22.0s -33d14m39s 11.4 8.5 x 2.0 351 159 409 Vol I 8 AM 0029-643 Tucana ESO 079- G003 00h32m02.2s -64d15m12s 12.6 2.7 x 0.4 440 204 409 Vol I 9 AM 0031-280B Sculptor NGC 150 00h34m15.5s -27d48m13s 12 3.9 x 1.9 306 141 387 Vol I 10 AM 0031-320 Sculptor NGC 148 00h34m15.5s -31d47m10s 13.3 2 x 0.8 351 159 387 Vol I 11 AM 0033-253 Sculptor IC 1558 00h35m47.1s -25d22m28s 12.6 3.4 x 2.5 306 141 365 Vol I 12 AM 0041-502 Phoenix NGC 238 00h43m25.7s -50d10m58s 13.1 1.9 x 1.6 417 177 449 Vol I 13 AM 0045-314 Sculptor NGC 254 00h47m27.6s -31d25m18s 12.6 2.5 x 1.5 351 176 386 Vol I 14 AM 0050-312 Sculptor NGC 289 00h52m42.3s -31d12m21s 11.7 5.1 x 3.6 351 176 386 Vol I 15 AM 0052-375 Sculptor NGC 300 00h54m53.5s -37d41m04s 9 22 x 16 351 176 408 Vol I 16 AM 0106-803 Hydrus ESO 013- G012 01h07m02.2s -80d18m28s 13.6 2.8 x 0.9 460 214 509 Vol I 17 AM 0105-471 Phoenix IC 1625 01h07m42.6s -46d54m27s 12.9 1.7 x 1.2 387 191 448 Vol I 18 AM 0108-302 Sculptor NGC 418 01h10m35.6s -30d13m17s 13.1 2 x 1.7 352 176 385 Vol I 19 AM 0110-583 Hydrus NGC -
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A&A 562, A92 (2014) Astronomy DOI: 10.1051/0004-6361/201321493 & c ESO 2014 Astrophysics Li depletion in solar analogues with exoplanets Extending the sample, E. Delgado Mena1,G.Israelian2,3, J. I. González Hernández2,3,S.G.Sousa1,2,4, A. Mortier1,4,N.C.Santos1,4, V. Zh. Adibekyan1, J. Fernandes5, R. Rebolo2,3,6,S.Udry7, and M. Mayor7 1 Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Instituto de Astrofísica de Canarias, C/ Via Lactea s/n, 38200 La Laguna, Tenerife, Spain 3 Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain 4 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, 4169-007 Porto, Portugal 5 CGUC, Department of Mathematics and Astronomical Observatory, University of Coimbra, 3049 Coimbra, Portugal 6 Consejo Superior de Investigaciones Científicas, CSIC, Spain 7 Observatoire de Genève, Université de Genève, 51 ch. des Maillettes, 1290 Sauverny, Switzerland Received 18 March 2013 / Accepted 25 November 2013 ABSTRACT Aims. We want to study the effects of the formation of planets and planetary systems on the atmospheric Li abundance of planet host stars. Methods. In this work we present new determinations of lithium abundances for 326 main sequence stars with and without planets in the Teff range 5600–5900 K. The 277 stars come from the HARPS sample, the remaining targets were observed with a variety of high-resolution spectrographs. Results. We confirm significant differences in the Li distribution of solar twins (Teff = T ± 80 K, log g = log g ± 0.2and[Fe/H] = [Fe/H] ±0.2): the full sample of planet host stars (22) shows Li average values lower than “single” stars with no detected planets (60). -
Upholding the Unified Model for Active Galactic Nuclei: VLT/FORS2 Spectropolarimetry of Seyfert 2 Galaxies
MNRAS 461, 1387–1403 (2016) doi:10.1093/mnras/stw1388 Advance Access publication 2016 June 9 Upholding the unified model for active galactic nuclei: VLT/FORS2 spectropolarimetry of Seyfert 2 galaxies C. Ramos Almeida,1,2‹† M. J. Mart´ınez Gonzalez,´ 1,2 A. Asensio Ramos,1,2 J. A. Acosta-Pulido,1,2 S. F. Honig,¨ 3 A. Alonso-Herrero,4,5 C. N. Tadhunter6 and O. Gonzalez-Mart´ ´ın7 1Instituto de Astrof´ısica de Canarias, Calle V´ıa Lactea,´ s/n, E-38205 La Laguna, Tenerife, Spain 2Departamento de Astrof´ısica, Universidad de La Laguna, E-38205 La Laguna, Tenerife, Spain 3School of Physics and Astronomy, University of Southampton, Southampton SO17 1BJ, UK 4Centro de Astrobiolog´ıa (CAB, CSIC-INTA), ESAC Campus, E-28692 Villanueva de la Canada,˜ Madrid, Spain 5Department of Physics and Astronomy, University of Texas at San Antonio, One UTSA Circle, San Antonio, TX 78249, USA 6Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK 7Instituto de Radioastronom´ıa y Astrof´ısica (IRAF-UNAM), 3-72 (Xangari), 8701 Morelia, Mexico Accepted 2016 June 7. Received 2016 June 7; in original form 2015 September 2 ABSTRACT The origin of the unification model for active galactic nuclei (AGN) was the detection of broad hydrogen recombination lines in the optical polarized spectrum of the Seyfert 2 galaxy (Sy2) NGC 1068. Since then, a search for the hidden broad-line region (HBLR) of nearby Sy2s started, but polarized broad lines have only been detected in ∼30–40 per cent of the nearby Sy2s observed to date. -
Chapter 2 Spatially Resolved Spitzer Spectroscopy of the Starburst Nucleus in NGC 5253
Interstellar medium conditions in starburst galaxies Beirão, M.P.L. Citation Beirão, M. P. L. (2010, January 13). Interstellar medium conditions in starburst galaxies. Retrieved from https://hdl.handle.net/1887/14559 Version: Not Applicable (or Unknown) License: Leiden University Non-exclusive license Downloaded from: https://hdl.handle.net/1887/14559 Note: To cite this publication please use the final published version (if applicable). Chapter 2 Spatially Resolved Spitzer Spectroscopy of the Starburst Nucleus in NGC 5253 Chapter enhanced from P. Beir˜ao, B. R. Brandl, D. Devost, J. D. Smith, L. Hao & J. R. Houck, Astrophysical Journal Letters, 643, L1 (2006) We present new Spitzer Space Telescope data on the nearby, low-metallicity star- burst galaxy NGC 5253, from the Infrared Array Camera IRAC and the Infrared Spectrograph IRS1. The mid-IR luminosity profile of NGC 5253 is clearly domi- nated by an unresolved cluster near the center, which outshines the rest of the galaxy at longer wavelengths. We find that the [NeIII]/[NeII] ratio decreases from ∼ 8.5 at the center to ∼ 2.5 at a distance of ∼ 250 pc. The [S IV]/[S III] fol- lows the [Ne III]/[Ne II] ratio remarkably well, being about 4 − 5 times lower at all distances. Our spectra reveal for the first time PAH emission features at 11.3µm; their equivalent widths increase significantly with distance from the center. The good anti-correlation between the PAH strength and the product between hard- ness and luminosity of the UV radiation field suggests photo-destruction of the PAH molecules in the central region. -
The Interstellar and Circumnuclear Medium of Active Nuclei Traced by H I 21 Cm Absorption
The Astronomy and Astrophysics Review (2018) 26:4 https://doi.org/10.1007/s00159-018-0109-x REVIEW ARTICLE The interstellar and circumnuclear medium of active nuclei traced by H i 21 cm absorption Raffaella Morganti1,2 · Tom Oosterloo1,2 Received: 23 April 2018 © The Author(s) 2018 Abstract This review summarises what we have learnt in the last two decades based on H i 21 cm absorption observations about the cold interstellar medium (ISM) in the central regions of active galaxies and about the interplay between this gas and the active nucleus (AGN). Hi absorption is a powerful tracer on all scales, from the parsec-scales close to the central black hole to structures of many tens of kpc tracing interactions and mergers of galaxies. Given the strong radio continuum emission often associated with the central activity, H i absorption observations can be used to study the Hi near an active nucleus out to much higher redshifts than is possible using H i emission. In this way, Hi absorption has been used to characterise in detail the general ISM in active galaxies, to trace the fuelling of radio-loud AGN, to study the feedback occurring between the energy released by the active nucleus and the ISM, and the impact of such interactions on the evolution of galaxies and of their AGN. In the last two decades, significant progress has been made in all these areas. It is now well established that many radio loud AGN are surrounded by small, regularly rotating gas disks that contain a significant fraction of H i. -
Tracing Kinematic (Mis)Alignments in CALIFA Merging Galaxies Stellar and Ionized Gas Kinematic Orientations at Every Merger Stage
Astronomy & Astrophysics manuscript no. final_interKin_jkbb_aanda_corr c ESO 2015 June 15, 2015 Tracing kinematic (mis)alignments in CALIFA merging galaxies Stellar and ionized gas kinematic orientations at every merger stage J.K. Barrera-Ballesteros1; 2,?, B. García-Lorenzo1; 2, J. Falcón-Barroso1; 2, G. van de Ven3, M. Lyubenova3; 4, V. Wild5, J. Méndez-Abreu5, S. F. Sánchez6, I. Marquez7, J. Masegosa7, A. Monreal-Ibero8; 9, B. Ziegler10, A. del Olmo7, L. Verdes-Montenegro7, R. García-Benito7, B. Husemann11; 8, D. Mast12, C. Kehrig7, J. Iglesias-Paramo7; 13, R. A. Marino14, J. A. L. Aguerri1; 2, C. J. Walcher8, J. M. Vílchez7, D. J. Bomans15; 16, C. Cortijo-Ferrero7, R. M. González Delgado7, J. Bland-Hawthorn17, D. H. McIntosh18, Simona Bekeraite˙8, and the CALIFA Collaboration (Affiliations can be found after the references) June 15, 2015 ABSTRACT We present spatially resolved stellar and/or ionized gas kinematic properties for a sample of 103 interacting galaxies, tracing all merger stages: close companions, pairs with morphological signatures of interaction, and coalesced merger remnants. In order to distinguish kinematic properties caused by a merger event from those driven by internal processes, we compare our galaxies with a control sample of 80 non-interacting galaxies. We measure for both the stellar and the ionized gas components the major (projected) kinematic position angles (PAkin, approaching and receding) directly from the velocity distributions with no assumptions on the internal motions. This method also allow us to derive the deviations of the kinematic PAs from a straight line (δPAkin). We find that around half of the interacting objects show morpho-kinematic PA misalignments that cannot be found in the control sample. -
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This is an Open Access document downloaded from ORCA, Cardiff University's institutional repository: http://orca.cf.ac.uk/136213/ This is the author’s version of a work that was submitted to / accepted for publication. Citation for final published version: Smith, Mark D., Bureau, Martin, Davis, Timothy A., Cappellari, Michele, Liu, Lijie, Onishi, Kyoko, Iguchi, Satoru, North, Eve V. and Sarzi, Marc 2021. WISDOM project - VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas. Monthly Notices of the Royal Astronomical Society 500 , pp. 1933-1952. 10.1093/mnras/staa3274 file Publishers page: http://dx.doi.org/10.1093/mnras/staa3274 <http://dx.doi.org/10.1093/mnras/staa3274> Please note: Changes made as a result of publishing processes such as copy-editing, formatting and page numbers may not be reflected in this version. For the definitive version of this publication, please refer to the published source. You are advised to consult the publisher’s version if you wish to cite this paper. This version is being made available in accordance with publisher policies. See http://orca.cf.ac.uk/policies.html for usage policies. Copyright and moral rights for publications made available in ORCA are retained by the copyright holders. MNRAS 500, 1933–1952 (2021) doi:10.1093/mnras/staa3274 Advance Access publication 2020 October 22 WISDOM project – VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas Mark D. Smith ,1‹ Martin Bureau,1,2 Timothy A. Davis ,3 Michele Cappellari ,1 Lijie Liu,1 Kyoko Onishi ,4,5,6 Satoru Iguchi ,5,6 Eve V. -
Compact Jets Causing Large Turmoil in Galaxies Enhanced Line Widths Perpendicular to Radio Jets As Tracers of Jet-ISM Interaction?
A&A 648, A17 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039869 & c G. Venturi et al. 2021 Astrophysics MAGNUM survey: Compact jets causing large turmoil in galaxies Enhanced line widths perpendicular to radio jets as tracers of jet-ISM interaction? G. Venturi1,2, G. Cresci2, A. Marconi3,2, M. Mingozzi4, E. Nardini3,2, S. Carniani5,2, F. Mannucci2, A. Marasco2, R. Maiolino6,7,8 , M. Perna9,2, E. Treister1, J. Bland-Hawthorn10,11, and J. Gallimore12 1 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile e-mail: [email protected] 2 INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: [email protected] 3 Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Via G. Sansone 1, 50019 Sesto Fiorentino, Firenze, Italy 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy 6 Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge CB3 0HE, UK 7 Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 8 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 9 Centro de Astrobiología (CSIC-INTA), Departamento de Astrofísica Cra. de Ajalvir Km. 4, 28850 Torrejón de Ardoz, Madrid, Spain 10 Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW 2006, Australia 11 ARC Centre of Excellence for All Sky Astrophysics in Three Dimensions (ASTRO-3D), Canberra ACT2611, Australia 12 Department of Physics and Astronomy, Bucknell University, Lewisburg, PA 17837, USA Received 6 November 2020 / Accepted 13 January 2021 ABSTRACT Context.