Curriculum Vitae D. Michael Crenshaw Distinguished University
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PMAS-PPAK Integral-Field Spectroscopy of Nearby Seyfert And
PMAS-PPAK integral-field spectroscopy of nearby Seyfert and normal spiral galaxies I. The central kiloparsecs of NGC 4138 Bartakov´ a´ T.1, Jungwiert B.2,3,Sanchez´ S. F.4,5, Stoklasova´ I.2, Emsellem E.6, Ferruit P.7, Jahnke K.8, Mundell C.9, Tacconi-Garman L. E.6, Vergani D.10, Wisotzki L.11 1 Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University, Brno, Czech Republic; 2 Astronomical Institute, Academy of Science of the Czech Republic, Prague, Czech Republic; 3 Astronomical Institute of the Charles University in Prague, Czech Republic; 4 Centro de Estudios de F´ısica del Cosmos de Aragon´ (CEFCA), Teruel, Spain; 5 Centro Astronomico´ Hispano-Aleman,´ Calar Alto, Almer´ıa, Spain; 6 European Southern Observatory, Garching, Germany; 7 CRAL-Observatoire de Lyon, Saint-Genis-Laval, France; 8 Max-Planck-Institut fur Astronomie, Heidelberg, Germany; 9 Astrophysics Research Institute, Liverpool John Moores University, United Kingdom; 10 INAF-Osservatorio Astronomico di Bologna, Italy; 11 Astrophysical Institute Potsdam, Germany. email: [email protected] Project overview These peculiarities are suspected to be related to a minor merger, however they could also be related to a destroyed Ratio Ha/Hb |2.5/*| Ratio [SII]6717/[SII]6731 |1.15/2.0| We study properties of ionized gas, gas/stellar kinematics bar, or a combination of both. New studies are necessary 30 6 30 2 5.5 1.9 and stellar populations in central regions (a few inner 20 20 to understand the galaxy history and mass transfer within 1.8 5 kiloparsecs) of four pairs of nearby Seyfert (NGC 5194, 10 10 1.7 the inner kiloparsecs. -
Do Normal Galaxies Host a Black Hole? the High Energy Perspective
DO NORMAL GALAXIES HOST A BLACK HOLE? THE HIGH ENERGY PERSPECTIVE 1 Y. Terashima2 Nagoya University ABSTRACT We review ASCA results on a search for low luminosity active nuclei at the center of nearby normal galaxies. More than a dozen low-luminosity AGN have been discovered with 2–10 keV − − luminosity in the range 1040 41 ergs s 1. Their X-ray properties are in some respects similar to those of luminous Seyfert galaxies, but differ in other respects. We also present estimated black hole masses in low luminosity AGNs and a drastic activity decline in the nucleus of the radio galaxy Fornax A. These results altogether suggest that relics of the past luminous AGNs lurk in nearby normal galaxies. KEYWORDS: Galaxies; Low luminosity AGNs; LINERs; Black holes 1. Introduction The number density of quasars is peaked at a redshift of z ∼ 2 and rapidly de- creases toward smaller redshifts. In the local universe, there is no AGN emitting at huge luminosity like quasars. These facts infer that quasars evolve to supermassive black holes in nearby apparently normal galaxies (e.g. Rees 1990). The growing evidence for supermassive black holes in nearby galaxies are ob- tained from recent optical and radio observations of gas/stellar kinematics around the center of galaxies (e.g. Ho 1998a; Magorrian et al. 1998; Kormendy & Rich- stone 1995). If fueling to the supermassive black hole takes place with a small arXiv:astro-ph/9905218v1 17 May 1999 mass accretion rate, they are expected to be observed as very low luminosity AGNs compared to quasars. Recent optical spectroscopic surveys have shown that low level activity is fairly common in nearby galaxies. -
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 -