Active Galactic Nuclei and Their Neighbours
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The X-Ray Emission of Local Luminous Infrared Galaxies⋆
A&A 535, A93 (2011) Astronomy DOI: 10.1051/0004-6361/201117420 & c ESO 2011 Astrophysics The X-ray emission of local luminous infrared galaxies M. Pereira-Santaella1, A. Alonso-Herrero1, M. Santos-Lleo2, L. Colina1, E. Jiménez-Bailón3, A. L. Longinotti4, G. H. Rieke5,M.Ward6, and P. Esquej1 1 Departamento de Astrofísica, Centro de Astrobiología, CSIC/INTA, Carretera de Torrejón a Ajalvir, km 4, 28850 Torrejón de Ardoz, Madrid, Spain e-mail: [email protected] 2 XMM-Newton Science Operation Centre, European Space Agency, 28691 Villanueva de la Cañada, Madrid, Spain 3 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 Mexico DF, México 4 MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue, NE80-6011, Cambridge, MA 02139, USA 5 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 6 Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK Received 6 June 2011 / Accepted 5 September 2011 ABSTRACT We study the X-ray emission of a representative sample of 27 local luminous infrared galaxies (LIRGs). The median IR luminosity of our sample is log LIR/L = 11.2, therefore the low-luminosity end of the LIRG class is well represented. We used new XMM-Newton data as well as Chandra and XMM-Newton archive data. The soft X-ray (0.5–2 keV) emission of most of the galaxies (>80%), including LIRGs hosting a Seyfert 2 nucleus, is dominated by star-formation-related processes. These LIRGs follow the star-formation rate (SFR) versus soft X-ray luminosity correlation observed in local starbursts. -
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. -
The Bright Galaxies NGC 1068 (M 77), NGC 2146, NGC 3079, NGC 4826 (M 64), and NGC 7469 F
A&A 493, 525–538 (2009) Astronomy DOI: 10.1051/0004-6361:200810655 & c ESO 2009 Astrophysics CI and CO in nearby galaxy centers The bright galaxies NGC 1068 (M 77), NGC 2146, NGC 3079, NGC 4826 (M 64), and NGC 7469 F. P. Israel Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] Received 22 July 2008 / Accepted 5 November 2008 ABSTRACT Aims. We study the physical properties and amount of molecular gas in the central regions of galaxies with active nuclei. Methods. Maps and measurements of the J = 1−0, J = 2−1, J = 3−2, J = 4−3 12CO, the J = 1−0, J = 2−1, and J = 3−2 13CO lines in the central arcminute squared of NGC 1068, NGC 2146, NGC 3079, NGC 4826, and NGC 7469, as well as 492 GHz CI maps in three of these are used to model the molecular gas clouds in these galaxies. Results. Bright CO concentrations were detected and mapped in all five objects. In all cases, the observed lines could be fitted with two distinct gas components. The physical condition of the molecular gas is found to differ from galaxy to galaxy. Rather high kinetic temperatures of 125−150 K occur in NGC 2146 and NGC 3079. Very high densities of 0.3−1.0 × 105 cm−3 occur in NGC 2146, NGC 3079, and NGC 7469. The CO to H2 conversion factor X is typically an order of magnitude less than the “standard” value in the solar neighborhood. -
Multi-Wavelength Campaign on NGC 7469: Deciphering Variability of the Ionised Outflows
Multi-wavelength campaign on NGC 7469: deciphering variability of the ionised outflows Missagh Mehdipour SRON Netherlands Institute for Space Research Jelle Kaastra, Ehud Behar, Gerard Kriss, Massimo Cappi, Pierre-Olivier Petrucci, Nahum Arav, Shai Kaspi, Uria Peretz, Elisa Costantini! Chandra Workshop 2016! R.G. Detmers et al.: Multiwavelength campaign on Mrk 509 3 Table 1. Spline continuum parameters. Ionised Wavelength Flux (Å) (photons m−2 s−1 Å−1) outflows 5.00 0 5.95 0.7 ± 0.6 in AGN 7.07 13.95 ± 0.09 8.41 14.28 ± 0.06 10.00 15.10 ± 0.04 11.89 15.92 ± 0.09 14.14 17.27 ± 0.09 16.82 19.36 ± 0.16 20.00 21.31 ± 0.11 X-ray 23.78 25.15 ± 0.08 Mrk 509 - XMM RGS 28.28 27.83 ± 0.11 Detmers+11 33.64 33.62 ± 0.19 40.00 9.80 ± 0.18 Fig. 1. The fluxed stacked RGS spectrum in the 7 - 38 Å range. account for the separate outflow velocities observed. All mod- The strongest lines are indicated and the O i ISM edge can be els take a wide range of ionization states into account. These clearly seen around 23 Å. models are described in more detail in Sect. 3.2. We also in- UV cluded eleven broad and narrow emission lines, which are mod- Mrk 509 - HST COS eled with a Gaussian line profile. Radiative recombination con- fitting package to fit the spectrum.Kriss+11 We updated the wavelengths tinua (RRCs) are also included using an ad-hoc model that takes of some important transitions for our study (see Appendix A). -
Observing Galaxies in Pegasus 01 October 2015 23:07
Observing galaxies in Pegasus 01 October 2015 23:07 Context As you look towards Pegasus you are looking below the galactic plane under the Orion spiral arm of our galaxy. The Perseus-Pisces supercluster wall of galaxies runs through this constellation. It stretches from RA 3h +40 in Perseus to 23h +10 in Pegasus and is around 200 million light years away. It includes the Pegasus I group noted later this document. The constellation is well placed from mid summer to late autumn. Pegasus is a rich constellation for galaxy observing. I have observed 80 galaxies in this constellation. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 7331 MAG 9 This is the stand out galaxy of the constellation. It is similar to our milky way. Around it are a number of fainter NGC galaxies. I have seen the brightest one, NGC 7335 in my 10 inch scope with averted vision. I have seen NGC 7331 in my 25 x 100mm binoculars. NGC 7814 - Mag 10 ? Not on observed list ? This is a very lovely oval shaped galaxy. By constellation Page 1 NGC 7332 MAG 11 / NGC 7339 MAG 12 These galaxies are an isolated bound pair about 67 million light years away. NGC 7339 is the fainter of the two galaxies at the eyepiece. I have seen NGC 7332 in my 25 x 100mm binoculars. -
How Supernovae Became the Basis of Observational Cosmology
Journal of Astronomical History and Heritage, 19(2), 203–215 (2016). HOW SUPERNOVAE BECAME THE BASIS OF OBSERVATIONAL COSMOLOGY Maria Victorovna Pruzhinskaya Laboratoire de Physique Corpusculaire, Université Clermont Auvergne, Université Blaise Pascal, CNRS/IN2P3, Clermont-Ferrand, France; and Sternberg Astronomical Institute of Lomonosov Moscow State University, 119991, Moscow, Universitetsky prospect 13, Russia. Email: [email protected] and Sergey Mikhailovich Lisakov Laboratoire Lagrange, UMR7293, Université Nice Sophia-Antipolis, Observatoire de la Côte d’Azur, Boulevard de l'Observatoire, CS 34229, Nice, France. Email: [email protected] Abstract: This paper is dedicated to the discovery of one of the most important relationships in supernova cosmology—the relation between the peak luminosity of Type Ia supernovae and their luminosity decline rate after maximum light. The history of this relationship is quite long and interesting. The relationship was independently discovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. Using a limited sample of Type I supernovae they were able to show that the brighter the supernova is, the slower its luminosity declines after maximum. Only with the appearance of CCD cameras could Mark Phillips re-inspect this relationship on a new level of accuracy using a better sample of supernovae. His investigations confirmed the idea proposed earlier by Rust and Pskovskii. Keywords: supernovae, Pskovskii, Rust 1 INTRODUCTION However, from the moment that Albert Einstein (1879–1955; Whittaker, 1955) introduced into the In 1998–1999 astronomers discovered the accel- equations of the General Theory of Relativity a erating expansion of the Universe through the cosmological constant until the discovery of the observations of very far standard candles (for accelerating expansion of the Universe, nearly a review see Lipunov and Chernin, 2012). -
Modelling Ionised and Photodissociated Regions
Modelling ionised and photodissociated regions Magda Vasta Thesis submitted for the Degree of Doctor of Philosophy of University College London Department of Physics & Astronomy UNIVERSITY COLLEGE LONDON March 2010 I, Magda Vasta, confirm that the work presented in this thesis is my own. Where information has been derived from other sources, I confirm that this has been indicated in the thesis. To my parents, my brother and my husband, who always supported and encouraged me no matter what. I tell people I am too stupid to know what is impossible. I have ridiculously large dreams, and half the time they come true. — Thomas D. ACKNOWLEDGEMENTS Some people come into our lives and quickly go. Some stay for a while and leave footprints on our hearts. And we are never, ever the same. I made it, I still cannot believe it, but I finally made it. However, it would have been almost impossible to reach this target without the constant scientific support from some people. My first big THANKS go to my supervisor Serena Viti. Thanks for being the supportive person you are, for giving me the possibility to be independent in my research, but being always present when I needed you. Thanks for all the times that you did not talk to me in Italian, for encouraging me to not give up and for being the lovely person you are. Thanks to Mike Barlow for the amazing scientific suggestions and for tolerating ALL my silly questions (most of them grammatically incorrect!). Thanks to Barbara Ercolano for her patience when answering my emails “HELP, PLEASE!!” about MOCASSIN. -
Astrophysics in 2006 3
ASTROPHYSICS IN 2006 Virginia Trimble1, Markus J. Aschwanden2, and Carl J. Hansen3 1 Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, Las Cumbres Observatory, Santa Barbara, CA: ([email protected]) 2 Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Organization ADBS, Building 252, 3251 Hanover Street, Palo Alto, CA 94304: ([email protected]) 3 JILA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder CO 80309: ([email protected]) Received ... : accepted ... Abstract. The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords: cosmology: general, galaxies: general, ISM: general, stars: general, Sun: gen- eral, planets and satellites: general, astrobiology CONTENTS 1. Introduction 6 1.1 Up 6 1.2 Down 9 1.3 Around 10 2. Solar Physics 12 2.1 The solar interior 12 2.1.1 From neutrinos to neutralinos 12 2.1.2 Global helioseismology 12 2.1.3 Local helioseismology 12 2.1.4 Tachocline structure 13 arXiv:0705.1730v1 [astro-ph] 11 May 2007 2.1.5 Dynamo models 14 2.2 Photosphere 15 2.2.1 Solar radius and rotation 15 2.2.2 Distribution of magnetic fields 15 2.2.3 Magnetic flux emergence rate 15 2.2.4 Photospheric motion of magnetic fields 16 2.2.5 Faculae production 16 2.2.6 The photospheric boundary of magnetic fields 17 2.2.7 Flare prediction from photospheric fields 17 c 2008 Springer Science + Business Media. -
An Atlas of Calcium Triplet Spectra of Active Galaxies 3
Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 1 December 2018 (MN LATEX style file v2.2) An atlas of Calcium triplet spectra of active galaxies A. Garcia-Rissmann1⋆, L. R. Vega1,2†, N. V. Asari1‡, R. Cid Fernandes1§, H. Schmitt3,4¶, R. M. Gonz´alez Delgado5k, T. Storchi-Bergmann6⋆⋆ 1 Depto. de F´ısica - CFM - Universidade Federal de Santa Catarina, C.P. 476, 88040-900, Florian´opolis, SC, Brazil 2 Observatorio Astron´omico de C´ordoba, Laprida 854, 5000, C´ordoba, Argentina 3 Remote Sensing Division, Code 7210, Naval Research Laboratory, 4555 Overlook Avenue, SW, Washington, DC 20375 4 Interferometric Inc., 14120 Parke Long Court, 103, Chantilly, VA20151 5 Instituto de Astrof´ısica de Andaluc´ıa (CSIC), P.O. Box 3004, 18080 Granada, Spain 6 Instituto de F´ısica, Universidade Federal do Rio Grande do Sul, C.P. 15001, 91501-970, Porto Alegre, RS, Brazil 1 December 2018 ABSTRACT We present a spectroscopic atlas of active galactic nuclei covering the region around the λλ8498, 8542, 8662 Calcium triplet (CaT). The sample comprises 78 ob- jects, divided into 43 Seyfert 2s, 26 Seyfert 1s, 3 Starburst and 6 normal galaxies. The spectra pertain to the inner ∼ 300 pc in radius, and thus sample the central kine- matics and stellar populations of active galaxies. The data are used to measure stellar velocity dispersions (σ⋆) both with cross-correlation and direct fitting methods. These measurements are found to be in good agreement with each-other and with those in previous studies for objects in common. The CaT equivalent width is also measured. -
Observed CN and HCN Intensity Ratios Exhibit Subtle Variations in Extreme Galaxy Environments
MNRAS 000,1–12 (2021) Preprint 19 April 2021 Compiled using MNRAS LATEX style file v3.0 Observed CN and HCN intensity ratios exhibit subtle variations in extreme galaxy environments B. Ledger,1¢ C. D. Wilson,1 T. Michiyama,2 D. Iono,3,4 S. Aalto,5 T. Saito,6 A. Bemis,7 R. Aladro8 1Department of Physics and Astronomy, McMaster University, 1280 Main St. W., Hamilton, Ontario L8S 4M1, Canada 2Kavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871, P.R.China 3National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588 4Department of Astronomical Science, The Graduate University for Advanced Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 5Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Observatory, SE-439 92 Onsala, Sweden 6Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany 7Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands 8Max-Planck-Institut fur Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We use both new and archival ALMA data of three energy lines each of CN and HCN to explore intensity ratios in dense gas in NGC 3256, NGC 7469, and IRAS 13120-5453. The HCN (3-2)/HCN (1-0) intensity ratio varies in NGC 3256 and NGC 7469, with superlinear trends of 1.53 ± 0.07 and 1.55 ± 0.05, respectively. We find an offset to higher HCN (3-2)/HCN (1-0) intensity ratios (∼ 0.8) in IRAS 13120-5453 compared to NGC 3256 (∼ 0.3 − 0.4) and NGC 7469 (∼ 0.3 − 0.5). -
CI and CO in Nearby Galaxy Centers
Astronomy & Astrophysics manuscript no. brightgal c ESO 2018 October 22, 2018 CI and CO in nearby galaxy centers The bright galaxies NGC 1068 (M 77), NGC 2146, NGC 3079, NGC 4826 (M 64), and NGC 7469 F.P. Israel1 Sterrewacht Leiden, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands Received ????; accepted ???? ABSTRACT Aims. We study the physical properties and amount of molecular gas in the central regions of galaxies with active nuclei. Methods. Maps and measurements of the J=1–0, J=2–1, J=3–2, J=4–3 12CO, the J=1–0, J=2–1, and J=3–2 13CO lines in the central arcminute squared of NGC 1068, NGC 2146, NGC 3079, NGC 4826, and NGC 7469, as well as 492 GHz CI maps in three of these are used to model the molecular gas clouds in these galaxies. Results. Bright CO concentrations were detected and mapped in all five objects. In all cases, the observed lines could be fitted with two distinct gas components. The physical condition of the molecular gas is found to differ from galaxy to galaxy. Rather high kinetic temperatures of 125-150 K occur in NGC 2146 and NGC 3079. Very high densities of 5 −3 0.3−1.0 × 10 cm occur in NGC 2146, NGC 3079, and NGC 7469. The CO to H2 conversion factor X is typically an order of magnitude less than the ‘standard’ value in the Solar Neighborhood. The molecular gas is constrained within 8 radii between 0.9 and 1.5 kpc from the nuclei. -
Space Research, Education, and Related Activities in the Space Sciences"
ANNUAL PROGRESS REPORT FOR -.x t_" "SPACE RESEARCH, EDUCATION, AND RELATED ACTIVITIES IN THE SPACE SCIENCES" Cooperative Agreement #NCC 5 - 356 For the period October 1, 2000 - September 30, 2001 Submitted To: Mr. Harold Coleman Grants Officer, Mail Code 210.G NASA/Goddard Space Flight Center Greenbelt, MD 20771 From: Universities Space Research Association The American City Building, Suite 212 Columbia, MD 21044-3498 Dr. David Black, PI Mr. David Holdridge " 'x,, Program Director INTRODUCTION: The Universities Space Research Association received an award of Cooperative Agreement #NCC 5 - 356 on September 29, 1998. The mission of this activity, know as the Cooperative Program in Space Sciences (CPSS), is to conduct space science research and leading-edge instrumentation and technology development, enable research by the space sciences communities, and to expedite the effective dissemination of space science research, technology, data, and information to the educational community and the general public. To fulfill this mission, USRA recruits and maintains a staff of scientific researchers, operates a series of guest investigator facilities, organizes scientific meetings and workshops, and encourages various interactions with students and university faculty members. ACCOMPLISHMENTS: Scientific Research and Instrument Development: As an indication of scientific research accomplishments, USRA scientists working under this Cooperative Agreement submitted 34 PI-level research and education proposals during the year. Indicative of the high level of community action, a majority of these submitted proposals were made in conjunction with a university-based collaborator. There was a good success rate. What follows are abstracts from independent scientific proposal awards received during the year to USRA staff Principal Investigators: Corbet, R.; Astrophysics Data Program/RXTE," "'Monitoring and Discovering X-ray Pulsars in the SMC (and the Galaxy) with RXTE." Our continuing RXTR monitoring program of the SMC has been extremely successful.