IRS Observations of Seyfert 1.8 and 1.9 Galaxies: a Comparison with Seyfert 1 and Seyfert 2 R
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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. -
Expanding Space, Quasars and St. Augustine's Fireworks
Universe 2015, 1, 307-356; doi:10.3390/universe1030307 OPEN ACCESS universe ISSN 2218-1997 www.mdpi.com/journal/universe Article Expanding Space, Quasars and St. Augustine’s Fireworks Olga I. Chashchina 1;2 and Zurab K. Silagadze 2;3;* 1 École Polytechnique, 91128 Palaiseau, France; E-Mail: [email protected] 2 Department of physics, Novosibirsk State University, Novosibirsk 630 090, Russia 3 Budker Institute of Nuclear Physics SB RAS and Novosibirsk State University, Novosibirsk 630 090, Russia * Author to whom correspondence should be addressed; E-Mail: [email protected]. Academic Editors: Lorenzo Iorio and Elias C. Vagenas Received: 5 May 2015 / Accepted: 14 September 2015 / Published: 1 October 2015 Abstract: An attempt is made to explain time non-dilation allegedly observed in quasar light curves. The explanation is based on the assumption that quasar black holes are, in some sense, foreign for our Friedmann-Robertson-Walker universe and do not participate in the Hubble flow. Although at first sight such a weird explanation requires unreasonably fine-tuned Big Bang initial conditions, we find a natural justification for it using the Milne cosmological model as an inspiration. Keywords: quasar light curves; expanding space; Milne cosmological model; Hubble flow; St. Augustine’s objects PACS classifications: 98.80.-k, 98.54.-h You’d think capricious Hebe, feeding the eagle of Zeus, had raised a thunder-foaming goblet, unable to restrain her mirth, and tipped it on the earth. F.I.Tyutchev. A Spring Storm, 1828. Translated by F.Jude [1]. 1. Introduction “Quasar light curves do not show the effects of time dilation”—this result of the paper [2] seems incredible. -
Arxiv:Astro-Ph/0411644V1 23 Nov 2004
Deconstructing NGC 7130 N. A. Levenson1, K. A. Weaver2,3, T. M. Heckman3, H. Awaki4, and Y. Terashima5 ABSTRACT Observations of the Seyfert 2 and starburst galaxy NGC 7130 with the Chan- dra X-ray Observatory illustrate that both of these phenomena contribute sig- nificantly to the galaxy’s detectable X-ray emission. The active galactic nucleus 24 −2 (AGN) is strongly obscured, buried beneath column density NH > 10 cm , and it is most evident in a prominent Fe Kα emission line with equivalent width greater than 1 keV. The AGN accounts for most (60%) of the observed X-rays at energy E > 2 keV, with the remainder due to spatially extended star for- mation. The soft X-ray emission is strong and predominantly thermal, on both small and large scales. We attribute the thermal emission to stellar processes. In total, the AGN is responsible for only one-third of the observed 0.5–10 keV luminosity of 3 × 1041 erg s−1 of this galaxy, and less than half of its bolometric luminosity. Starburst/AGN composite galaxies like NGC 7130 are truly common, and similar examples may contribute significantly to the high-energy cosmic X- ray background while remaining hidden at lower energies, especially if they are distant. Subject headings: Galaxies: individual (NGC 7130) — galaxies: Seyfert — X- rays: galaxies 1. Introduction arXiv:astro-ph/0411644v1 23 Nov 2004 Accretion onto supermassive black holes powers active galactic nuclei (AGNs), but star formation also may be fundamentally related to the central black holes and their activity. 1Department of Physics -
Deep Silicate Absorption Features in Compton-Thick Active Galactic Nuclei Predominantly Arise Due to Dust in the Host Galaxy
The Astrophysical Journal, 755:5 (8pp), 2012 August 10 doi:10.1088/0004-637X/755/1/5 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. DEEP SILICATE ABSORPTION FEATURES IN COMPTON-THICK ACTIVE GALACTIC NUCLEI PREDOMINANTLY ARISE DUE TO DUST IN THE HOST GALAXY A. D. Goulding1, D. M. Alexander2,F.E.Bauer3, W. R. Forman1, R. C. Hickox4, C. Jones1, J. R. Mullaney2,5, and M. Trichas1 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA; [email protected] 2 Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK 3 Departamento de Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile, Casilla 306, Santiago 22, Chile 4 Department of Physics and Astronomy, Dartmouth College, Hanover, NH 03755, USA 5 Laboratoire AIM, CEA/DSM-CNRS-Universite Paris Diderot, Irfu/Service Astrophysique, CEA-Saclay, Orme des Merisiers, 91191 Gif-sur-Yvette Cedex, France Received 2012 February 3; accepted 2012 May 31; published 2012 July 19 ABSTRACT We explore the origin of mid-infrared (mid-IR) dust extinction in all 20 nearby (z<0.05) bona fide Compton-thick 24 −2 (NH > 1.5×10 cm ) active galactic nuclei (AGNs) with hard energy (E>10 keV) X-ray spectral measurements. We accurately measure the silicate absorption features at λ ∼ 9.7 μm in archival low-resolution (R ∼ 57–127) Spitzer Infrared Spectrograph spectroscopy, and show that only a minority (≈45%) of nearby Compton-thick AGNs have strong Si-absorption features (S9.7 = ln(fint/f obs) 0.5) which would indicate significant dust attenuation. -
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. -