CO Multi-Line Imaging of Nearby Galaxies (COMING) IV. Overview Of
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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 -
Radio Sources in Low-Luminosity Active Galactic Nuclei
A&A 392, 53–82 (2002) Astronomy DOI: 10.1051/0004-6361:20020874 & c ESO 2002 Astrophysics Radio sources in low-luminosity active galactic nuclei III. “AGNs” in a distance-limited sample of “LLAGNs” N. M. Nagar1, H. Falcke2,A.S.Wilson3, and J. S. Ulvestad4 1 Arcetri Observatory, Largo E. Fermi 5, Florence 50125, Italy 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany e-mail: [email protected] 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 4 National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA e-mail: [email protected] Received 23 January 2002 / Accepted 6 June 2002 Abstract. This paper presents the results of a high resolution radio imaging survey of all known (96) low-luminosity active galactic nuclei (LLAGNs) at D ≤ 19 Mpc. We first report new 2 cm (150 mas resolution using the VLA) and 6 cm (2 mas resolution using the VLBA) radio observations of the previously unobserved nuclei in our samples and then present results on the complete survey. We find that almost half of all LINERs and low-luminosity Seyferts have flat-spectrum radio cores when observed at 150 mas resolution. Higher (2 mas) resolution observations of a flux-limited subsample have provided a 100% (16 of 16) detection rate of pc-scale radio cores, with implied brightness temperatures ∼>108 K. The five LLAGNs with the highest core radio fluxes also have pc-scale “jets”. -
The Radio Properties of a Complete Sample of Bright Galaxies
Aust. J. Phys., 1982,35,321-50 The Radio Properties of a Complete Sample of Bright Galaxies J. I. Harnett School of Physics, University of Sydney, Sydney, N.S.W. 2006. Abstract Results are given for the radio continuum properties of an optically complete sample of 294 bright galaxies, 147 of which have been detected. Data were obtained with the 408 MHz Molonglo Radio Telescope. The radio luminosity functions for all galaxies and for spiral galaxies alone are derived and the radio emission for different galaxy types is investigated. Spectral indices of 73 galaxies which had been detected at other frequencies were derived; the mean index of a reliable subsample is <ex) = -0,71. 1. Introduction There have been many extensive surveys of continuum radio emission from bright galaxies. The earliest comprehensive survey of high sensitivity was that of Cameron (1971a, 1971b) using the Molonglo Cross Radio Telescope at 408 MHz. Cameron observed two optically complete samples south of b = + 18° and defined the radio luminosity function with reasonable statistics at radio powers of ~ 1022 W HZ-I. In the past decade the optical properties of galaxies have been revised so that the selection of an optically complete sample is more reliable. In addition, between 1970 and 1978 the sensitivity of the 408 MHz Molonglo Cross was improved by more than a magnitude, permitting more detections and more accurate measurements of weak' radio emission. Before observations at 408 MHz with the Molonglo Cross ceased in 1978, a new survey was made to improve Cameron's results and provide the best possible data base for subsequent investigations at different frequencies. -
Guide Du Ciel Profond
Guide du ciel profond Olivier PETIT 8 mai 2004 2 Introduction hjjdfhgf ghjfghfd fg hdfjgdf gfdhfdk dfkgfd fghfkg fdkg fhdkg fkg kfghfhk Table des mati`eres I Objets par constellation 21 1 Androm`ede (And) Andromeda 23 1.1 Messier 31 (La grande Galaxie d'Androm`ede) . 25 1.2 Messier 32 . 27 1.3 Messier 110 . 29 1.4 NGC 404 . 31 1.5 NGC 752 . 33 1.6 NGC 891 . 35 1.7 NGC 7640 . 37 1.8 NGC 7662 (La boule de neige bleue) . 39 2 La Machine pneumatique (Ant) Antlia 41 2.1 NGC 2997 . 43 3 le Verseau (Aqr) Aquarius 45 3.1 Messier 2 . 47 3.2 Messier 72 . 49 3.3 Messier 73 . 51 3.4 NGC 7009 (La n¶ebuleuse Saturne) . 53 3.5 NGC 7293 (La n¶ebuleuse de l'h¶elice) . 56 3.6 NGC 7492 . 58 3.7 NGC 7606 . 60 3.8 Cederblad 211 (N¶ebuleuse de R Aquarii) . 62 4 l'Aigle (Aql) Aquila 63 4.1 NGC 6709 . 65 4.2 NGC 6741 . 67 4.3 NGC 6751 (La n¶ebuleuse de l’œil flou) . 69 4.4 NGC 6760 . 71 4.5 NGC 6781 (Le nid de l'Aigle ) . 73 TABLE DES MATIERES` 5 4.6 NGC 6790 . 75 4.7 NGC 6804 . 77 4.8 Barnard 142-143 (La tani`ere noire) . 79 5 le B¶elier (Ari) Aries 81 5.1 NGC 772 . 83 6 le Cocher (Aur) Auriga 85 6.1 Messier 36 . 87 6.2 Messier 37 . 89 6.3 Messier 38 . -
The Extragalactic Distance Scale
The Extragalactic Distance Scale Published in "Stellar astrophysics for the local group" : VIII Canary Islands Winter School of Astrophysics. Edited by A. Aparicio, A. Herrero, and F. Sanchez. Cambridge ; New York : Cambridge University Press, 1998 Calibration of the Extragalactic Distance Scale By BARRY F. MADORE1, WENDY L. FREEDMAN2 1NASA/IPAC Extragalactic Database, Infrared Processing & Analysis Center, California Institute of Technology, Jet Propulsion Laboratory, Pasadena, CA 91125, USA 2Observatories, Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena CA 91101, USA The calibration and use of Cepheids as primary distance indicators is reviewed in the context of the extragalactic distance scale. Comparison is made with the independently calibrated Population II distance scale and found to be consistent at the 10% level. The combined use of ground-based facilities and the Hubble Space Telescope now allow for the application of the Cepheid Period-Luminosity relation out to distances in excess of 20 Mpc. Calibration of secondary distance indicators and the direct determination of distances to galaxies in the field as well as in the Virgo and Fornax clusters allows for multiple paths to the determination of the absolute rate of the expansion of the Universe parameterized by the Hubble constant. At this point in the reduction and analysis of Key Project galaxies H0 = 72km/ sec/Mpc ± 2 (random) ± 12 [systematic]. Table of Contents INTRODUCTION TO THE LECTURES CEPHEIDS BRIEF SUMMARY OF THE OBSERVED PROPERTIES OF CEPHEID -
Breaking the Radio – Gamma-Ray Connection in Arp 220
MNRAS 000, 000{000 (0000) Preprint 16 January 2019 Compiled using MNRAS LATEX style file v3.0 Breaking the Radio { Gamma-Ray Connection in Arp 220 Tova M. Yoast-Hull? and Norman Murrayy Canadian Institute for Theoretical Astrophysics, University of Toronto, ON, M5S 3H8, Canada 16 January 2019 ABSTRACT Recent analyses of the γ-ray spectrum from the ultra-luminous infrared galaxy Arp 220 have revealed a discrepancy in the cosmic ray energy injection rates derived from the γ-rays versus the radio emission. While the observed radio emission is consistent with the star formation rate inferred from infrared observations, a significantly higher cosmic ray population is necessary to accurately model the measured γ-ray flux. To resolve this discrepancy between the radio and γ-ray observations, we find that we must increase the cosmic ray energy injection rate and account for an infrared optical depth greater than unity. Raising the energy injection rate naturally raises the total γ-ray flux but also raises the radio flux unless there is also an increase in the energy loss rate for cosmic ray leptons. A optically thick medium results in an increase in energy losses via inverse Compton for cosmic ray leptons and preserves agreement with submillimeter, millimeter, and infrared wavelength observations. Key words: cosmic rays { galaxies: individual (Arp 220) { galaxies: starburst { gamma rays: galaxies { radiative transfer { radio continuum: galaxies 1 INTRODUCTION collide with the ISM to produce neutral pions that subse- quently decay into γ-rays. Over the past decade, eight star-forming galaxies (mostly gi- In our current understanding, the correlation between ant spirals) have been detected in γ-rays by Fermi, including radio and FIR emission seen in star-forming galaxies requires M31 (NGC 0224), NGC 0253, NGC 1068, NGC 2146, M82 two additional conditions to hold. -
As101 Galaxy V2
Reminder 1. “Runaway Universe” assignment, with an in-class essay next week 2. Final Exam on 05/09 - Mandatory Presence; no make up - Closed online searches - Open book and open notes 3. Misc? This presentation on galaxy deviates from the textbook materials It is built with the next week’s presentation in mind Hubble’s Classification of Galaxies (Tuning Fork) http://en.wikipedia.org/wiki/Galaxy_morphological_classification MWG is SBb - Hubble Classification is improved upon by de Vaucouleurs We will see some examples of each type Let’s begin with our galactic neighbors The Whirlpool Galaxy M51 (M51a) (And companion M51b) Grand-design galaxy Self-sustaining star forming regions along spiral arm M51b: Lencular? (SB0) Amorphous? Irregular? Our Big Neighbors: M33 and M31 (Barred Spirals) http://tehgeektive.com/2012/06/12/what-happens-when-two-galaxies-collide-video/ Our Big Neighbors: M33 and M31 (Barred Spirals) http://apod.nasa.gov/apod/ap121220.html Triangulum Galaxy (Pinwheel) (M33, NGC 598) http://apod.nasa.gov/apod/ap080124.html Andromeda Galaxy (M31, NGC224) M32, a small elliptical dwarf, is above M110, a spheroidal dwarf, is below http:// annesastronomynews.com/annes-picture-of-the-day- the-andromeda-galaxy/ Andromeda - M31 - Barred Spiral http://apod.nasa.gov/apod/ap130202.html/ http://apod.nasa.gov/apod/ap120518.html Herschel Space Observatory (better than Spitzer) GALEX Bar can be seen! Hot Blue stars (O and B stars) Warm dust à will have star formation (now quiescent) Shows some ring structure – collision with M32? All about Andromeda -
Black Hole Mass Scaling Relations for Spiral Galaxies. I. MBH–M*,Sph Benjamin L
The Astrophysical Journal, 873:85 (26pp), 2019 March 1 https://doi.org/10.3847/1538-4357/aaf3b8 © 2019. The American Astronomical Society. All rights reserved. Black Hole Mass Scaling Relations for Spiral Galaxies. I. MBH–M*,sph Benjamin L. Davis1 , Alister W. Graham1 , and Ewan Cameron2 1 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia; [email protected] 2 Oxford Big Data Institute, University of Oxford, Oxford OX3 7LF, UK Received 2018 May 18; revised 2018 October 19; accepted 2018 November 13; published 2019 March 6 Abstract ( )–( ) The supermassive black hole mass, MBH bulge stellar mass, M*,sph relation is, obviously, derived using two quantities. We endeavor to provide accurate values for the latter via detailed multicomponent galaxy decompositions for the current full sample of 43 spiral galaxies having directly measured MBH values; 35 of these galaxies have been alleged to contain pseudobulges, 21 have water maser measurements, and three appear bulgeless. This more than doubles the previous sample size of spiral galaxies with a finessed image analysis. We have analyzed near-infrared images, accounting for not only the bulge, disk (exponential, truncated, or inclined), and bar but also spiral arms and rings and additional central components (active galactic nuclei (AGNs),etc.). A symmetric Bayesian analysis finds = +0.35 / 10 +( ± ) υ log (MMBH ☉) (2.44-0.31) log{M*,sph [u(1.15´ 10 M☉ )]} 7.24 0.12 ,with a stellar mass-to-light ratio term. The level of scatter equals that about the MBH–σ* relation. The nonlinear slope rules out the idea that many mergers, coupled with the central limit theorem, produced this scaling relation, and it corroborates previous observational studies and simulations, which have reported a near-quadratic slope at the low-mass end of the MBH– M ,sph diagram. -
The Applicability of Far-Infrared Fine-Structure Lines As Star Formation
A&A 568, A62 (2014) Astronomy DOI: 10.1051/0004-6361/201322489 & c ESO 2014 Astrophysics The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types? Ilse De Looze1, Diane Cormier2, Vianney Lebouteiller3, Suzanne Madden3, Maarten Baes1, George J. Bendo4, Médéric Boquien5, Alessandro Boselli6, David L. Clements7, Luca Cortese8;9, Asantha Cooray10;11, Maud Galametz8, Frédéric Galliano3, Javier Graciá-Carpio12, Kate Isaak13, Oskar Ł. Karczewski14, Tara J. Parkin15, Eric W. Pellegrini16, Aurélie Rémy-Ruyer3, Luigi Spinoglio17, Matthew W. L. Smith18, and Eckhard Sturm12 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Gent, Belgium e-mail: [email protected] 2 Zentrum für Astronomie der Universität Heidelberg, Institut für Theoretische Astrophysik, Albert-Ueberle Str. 2, 69120 Heidelberg, Germany 3 Laboratoire AIM, CEA, Université Paris VII, IRFU/Service d0Astrophysique, Bat. 709, 91191 Gif-sur-Yvette, France 4 UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Oxford Road, Manchester M13 9PL, UK 5 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 6 Laboratoire d0Astrophysique de Marseille − LAM, Université Aix-Marseille & CNRS, UMR7326, 38 rue F. Joliot-Curie, 13388 Marseille CEDEX 13, France 7 Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, UK 8 European Southern Observatory, Karl -
Accretion Disk Versus Jet Orientation in H2O Megamaser Galaxies F
A&A 624, A42 (2019) Astronomy https://doi.org/10.1051/0004-6361/201834600 & c F. Kamali et al. 2019 Astrophysics Accretion disk versus jet orientation in H2O megamaser galaxies F. Kamali1;?, C. Henkel1,2, S. Koyama3,1, C. Y. Kuo4, J. J. Condon5, A. Brunthaler1, M. J. Reid6, J. E. Greene7, K. M. Menten1, C. M. V. Impellizzeri5,8, J. A. Braatz5, E. Litzinger9,10, and M. Kadler9 1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: [email protected], [email protected] 2 Astron. Dept., King Abdulaziz University, PO Box 80203, Jeddah 21589, Saudi Arabia 3 Academia Sinica Institute of Astronomy and Astrophysics, PO Box 23-141, Taipei 10617, Taiwan 4 Physics Department, National Sun Yat-Sen University, No. 70, Lien-Hai Rd, Kaosiung City 80424, Taiwan 5 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA 6 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 7 Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 8 Joint ALMA Office, Alonso de Córdova 3107, Vitacura, Santiago, Chile 9 Institut für Theoretische Physik und Astrophysik, Universität Würzburg, Campus Hubland Nord, Emil-Fischer-Str. 31, 97074 Würzburg, Germany 10 Dr. Remeis-Observatory, Erlangen Centre for Astroparticle, Physics, University of Erlangen-Nuremberg, Sternwartstr. 7, 96049 Bamberg, Germany Received 7 November 2018 / Accepted 11 February 2019 ABSTRACT Context. An essential part of the paradigm describing active galactic nuclei is the alignment between the radio jet and the associated rotation axis of the sub-pc accretion disks. -
The Stellar Populacons of IC 10 and NGC 1569 Observed with Keck
The Stellar Populaons of IC 10 and NGC 1569 observed with Keck LGSAO and HST William D. Vacca (USRA‐SOFIA) Chris Sheehy James Graham (UC Berkeley) Nate McCrady (UCLA) Properes of IC 10 • Small irregular starburst (BCD) galaxy on outskirts of Local Group – R ~ 1 kpc 9 – M ~ 1‐2 x 10 M • Low metallicity (Z ~ 0.2‐0.3 Z~ ZSMC) • Brief, galaxy‐wide burst of SF occurred within last 10 Myr – Numerous HII regions – Large Hα and FIR luminosity ‐1 • Highest SFR of any LG dwarf (> 0.7 M yr ) – Large populaon of W‐R stars (NWR > 24; SMC has ~ 8) • Highest surface density of W‐Rs in LG ( ~ 8 kpc‐2; MW ~ 2.5 kpc‐2) • Anomalously high WC/WN rao ( ~ 1‐2) for its Z (10x too large!) • Have WN stars been missed in surveys? • b = −3.3° – Uncertain reddening: AV = 1.2 – 6.0 mag – Uncertain distance: D = 0.5 – 3.0 Mpc • Ideal extragalacc target for NIR observaons with LGSAO – Nearby, relavely large AV (foreground and internal), high ρ★ – Bright p‐lt guide stars available N IC 10 HST/ACS/WFC F435W, F606W, F814W 1” ≈ 4 pc WR Object: [MAC92] 24 • Brightest W‐R candidate in HST/WFPC2 F555W IC10 • Lies within prominent H II region HL 111c • Lies at center of a young stellar cluster (Hunter 2001) • Uncertain spectral type 5’’ – Weak, broad He II 4686 emission (Massey & Holmes 2002) – WN+OB? • Three components (A, B, C) • Cluster itself? Crowther et al. (2003) Observaons • NIR Data: • Opcal Data: – NIRC2/Keck II/LGSAO H and K’ – HST/ACS/WFC F814W – 0.01”pixel‐1 – 0.05”pixel‐1 – Final FOV = 12.2” x 12.2” – texp = 1080 s – texp = 1200 s (H); 1500 s (K’) – FWHM = 0.08” – FWHM = 0.048” (H); 0.051” (K’) – Strehl ~ 18% (H); 32% (K’) ACS WFC / NIRC2 Comparison HST/ACS/WFC F814W Keck II/NIRC2/LGSAO K’ IC 10 IHK’ N E 12.2” x 12.2” 47 pc x 47 pc Vacca, Sheehy, & Graham (2007) CMD of IC 10 [MAC92] 24 Region Opcal Data: • PSF fing (Anderson & King 2006) • 690 stars found in F814W • [F814W]Lim ~ 25.25 • σ < 0.04 mag for [F814W] < 23.0 NIR Data: • MTF‐fing method (Sheehy et al. -
Physical Conditions of the Molecular Gas in Metal-Poor Galaxies? L
A&A 606, A99 (2017) Astronomy DOI: 10.1051/0004-6361/201731000 & c ESO 2017 Astrophysics Physical conditions of the molecular gas in metal-poor galaxies? L. K. Hunt1, A. Weiß2, C. Henkel2; 3, F. Combes4, S. García-Burillo5, V. Casasola1, P. Caselli6, A. Lundgren9, R. Maiolino7, K. M. Menten2, and L. Testi1; 8 1 INAF–Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy e-mail: [email protected] 2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany 3 Astronomy Department, King Abdulaziz University, PO Box 80203, Jeddah, Saudia Arabia 4 Observatoire de Paris, LERMA, Collège de France, CNRS, PSL, Sorbonne University UPMC, 75014 Paris, France 5 Observatorio Astronómico Nacional (OAN)-Observatorio de Madrid, Alfonso XII, 3, 28014 Madrid, Spain 6 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany 7 Cavendish Laboratory, University of Cambridge, 19 J.J. Thomson Avenue, Cambridge CB3 0HE, UK 8 ESO, Karl Schwarzschild str. 2, 85748 Garching bei München, Germany 9 Vittja 64, 74793 Alunda, Sweden Received 18 April 2017 / Accepted 8 August 2017 ABSTRACT Studying the molecular component of the interstellar medium (ISM) in metal-poor galaxies has been challenging because of the faint- ness of carbon monoxide emission, the most common proxy of H2. Here we present new detections of molecular gas at low metal- licities, and assess the physical conditions in the gas through various CO transitions for 8 galaxies. For one, NGC 1140 (Z=Z ∼ 0.3), two detections of 13CO isotopologues and atomic carbon, [Ci](1–0) and an upper limit for HCN(1–0) are also reported.