DOCSLIB.ORG

Studying Faint Ultra Hard X-Ray Emission from AGN in GOALS

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Studying Faint Ultra Hard X-Ray Emission from AGN in GOALS Draft version July 17, 2018 A Preprint typeset using LTEX style emulateapj v. 5/2/11 STUDYING FAINT ULTRA HARD X-RAY EMISSION FROM AGN IN GOALS LIRGS WITH SWIFT BAT Michael Koss1, Richard Mushotzky2, Wayne Baumgartner3, Sylvain Veilleux2,3, Jack Tueller3, Craig Markwardt3, and Caitlin M. Casey1 Draft version July 17, 2018 ABSTRACT We present the first analysis of the all-sky Swift BAT ultra hard X-ray (14-195 keV) data for a targeted list of objects. We find the BAT data can be studied at 3× fainter limits than in previous blind detection catalogs based on prior knowledge of source positions and using smaller energy ranges for source detection. We determine the AGN fraction in 134 nearby (z<0.05) luminous infrared galaxies (LIRGS) from the GOALS sample. We find that LIRGs have a higher detection frequency than galaxies matched in stellar mass and redshift at 14-195 keV and 24-35 keV. In agreement with work at other wavelengths, the AGN detection fraction increases strongly at high IR luminosity with half of high luminosity LIRGs (50%, 6/12, log LIR/L⊙>11.8) detected. The BAT AGN classification shows 97% (37/38) agreement with Chandra and XMM AGN classification using hardness ratios or detection of a iron K-alpha line. This confirms our statistical analysis and supports the use of the Swift BAT all-sky survey to study fainter populations of any category of sources in the ultra hard X-ray band. BAT AGN in LIRGs tend to show higher column densities with 40±9% showing 14-195 keV/2-10 keV hardness flux ratios suggestive of high or Compton-thick column densities (log NH >24 cm−2), compared to only 12±5% of non-LIRG BAT AGN. We also find that using specific energy ranges of the BAT detector can yield additional sources over total band detections with 24% (5/21) of detections in LIRGs at 24-35 keV not detected at 14-195 keV. Subject headings: galaxies: active — X-rays 1. INTRODUCTION tion of X-ray selected AGN are in LIRGs (Koss et al. The Swift BAT survey with over 500 AGN has 2011b), an ultra-hard X-ray survey of LIRGs might come revolutionized our study of the ultra hard X-ray sky to different conclusions than those derived at lower ener- (Tueller et al. 2010), but is still limited to bright gies. −11 −1 −2 The ultra hard X-rays (>15 keV) are much less sensi- (F − >10 erg s cm ) objects in a blind sur- 14 195 tive to obscuration in the line-of-sight than soft X-ray or vey. However, the stability of the instrument and the optical wavelengths and are biased only against highly Gaussian nature of the noise, along with its wide energy Compton-thick AGN (Burlon et al. 2011). This band is range, allows the detection at fainter limits for a well also free from contamination from star formation that is defined, moderate sized sample of objects. For the first significant in the soft X-rays (<5 keV). Additionally, in time, we use this property to study the AGN in luminous Compton-Thick AGN the radiation below 10 keV is al- infrared galaxies (LIRGs; log LIR/L⊙>11.0). most completely absorbed in the X-rays whereas a broad The nature of the IR (8-1000 µm) emission and its Compton reflection hump appears in the >15 keV con- relation to star formation in AGN is still not well un- tinuum (Reynolds 1998). Thus, ultra-hard X-ray obser- derstood. Past studies of samples of LIRGs have sug- vations are an important complement to lower energy gested, based primarily on optical and IR AGN indica- X-ray data. tors, that the dominant power source is star formation We use the the most sensitive all-sky ultra hard X- and AGN activity is more common in luminous sources arXiv:1302.0850v1 [astro-ph.HE] 4 Feb 2013 ray survey from the Swift BAT instrument to search (e.g. Veilleux et al. 1995). Recent studies used a vari- for AGN emission in LIRGs. Previous studies using the ety of mid-IR spectral diagnostics and X-ray observa- INTEGRAL satellite stacked emission from a large sam- tions (Ptak et al. 2003; Teng et al. 2005; Veilleux et al. ple of IRAS bright galaxies and found no AGN detection 2009; Teng & Veilleux 2010; Petric et al. 2011) to deter- (Walter & Cabral 2009). Additionally, past BAT AGN mine the AGN contribution. However, contamination catalogs generated >4.8σ sources from ”blind” detections from star formation and obscuration by dust and gas (e.g. Tueller et al. 2010). To achieve higher sensitivities, are problematic. Additionally, studies of AGN in the we identify AGN (see §2.2) based on the prior knowledge hard X-rays have shown the existence of large fraction of source positions and search in energy bands where we of AGN not showing Spitzer IRAC AGN indicators (e.g. expect the AGN emission to be brightest. We adopt a Donley et al. 2012) and some AGN are not optically de- −1 standard cosmology (Ωm=0.3, Ω =0.7, H =70 km s tected (Koss et al. 2011a, 2012). Since a significant frac- Λ 0 Mpc−1) to determine distances. [email protected] 1 Institute for Astronomy, University of Hawaii, 2680 Wood- 2. lawn Drive, Honolulu, HI 96822, USA; SAMPLE SELECTION AND DERIVED QUANTITIES 2 Astronomy Department, University of Maryland, College 2.1. Sample of LIRGs and ULIRGs Park, MD, USA 3 Astrophysics Science Division, NASA Goddard Space Flight We selected a sample of nearby LIRGs (z<0.05) in Center, Greenbelt, MD, USA the northern hemisphere (DEC>-25) from the Great Ob- 2 servatories All Sky LIRG Survey (GOALS; Armus et al. We use the distribution of SNR for 1000 random point- 2009). In this redshift range, we are sensitive to X-ray ings from the SDSS survey area to measure the signifi- 42.0 luminosities of L14−195 keV >10 erg/s. This limit ef- cance of the X-ray detections in the other samples. The fectively detects AGN since it is ten times larger than the significance distribution at 14-195 keV of the random maximum known emission from a starburst galaxy (e.g., pointings is well fit by a Gaussian centered at 0.02±0.11 M82, log L14−195 keV =40.8 erg/s). Since single tempera- SNR with σ=1.01±0.06, consistent with the expected tures and SED templates can overestimate IR luminosi- values for a Gaussian distribution of pure noise. For the ties (Casey 2012), we recomputed GOALS IR luminosi- LIRG and matched sample, the Gaussian distribution of ties based on SED fitting using IRAS data and a model noise is fit from the SNR<0 source distribution. joining a modified, single dust temperature greybody, We choose a 2.7σ cutoff SNR in the 134 LIRG sample that approximates hot-dust emission from AGN heating. to have on average less than one ’fake’ noise source based We have limited our sources to be outside the Galactic on the Gaussian distribution of noise using both whole plane (b>10◦) because of source confusion in IRAS and band 14-195 keV and 24-35 keV detections if we assume Swift, as well difficulty measuring stellar masses because the distribution is pure noise. Finally, we note that the of high levels of optical extinction. lowest SNR of any LIRG is -2.1 at 14-195 keV and -2.7 at We have also limited our sample because in the low 24-35 keV suggesting this cutoff should assure a sample resolution BAT detector, source confusion from nearby of clean individual detections. bright AGN can occur. For blind source detection, We also analyze X-ray emission using XSPEC v12.7.1 Ajello et al. (2009) estimated a confusion radius of 5.5′ for the new sources between 2.7-4.8σ. To calculate lu- at SNR=2, 3.8′ at SNR=3, and 2.8′ at SNR=4. We use a minosities and upper limits, we assume an X-ray power conservative approach and exclude all detections within law of Γ=1.9 and Galactic extinction, consistent with 15′ of BAT catalog sources. This excludes seven LIRGs the mean 14-195 keV power law for Seyfert 2s in the 70 from our study. NGC 232 and NGC 838 are in merging month blind detection catalog (Winter et al. 2009). The ′ galaxy groups with a nearby (<2 ) bright BAT-detected BAT emission is absorbed by <10% for NH <3 × 1023 AGN companion. Additionally, UGC 3608 is 5.1′ from a cm−2, but sources with larger obscurations are underesti- nearby ROSAT X-ray source, 1RXS J065711.8+462731. mated. To determine 1σ errors in luminosity, we include A 1.5 ks XRT observation suggests the majority of the error from assuming a fixed power law index (14%) the flux is coincident with this ROSAT source. IRAS as well as sky and detector noise (<37%). Finally, to F03217+4022 and UGC 02717 are near a bright BAT better understand the average properties of the sources, AGN, IRAS 03219+4031 at 8.5′ and 7′ separation re- we fit a simple X-ray power law to the average emission spectively. Finally, NGC 2524 is near a bright BAT AGN in each X-ray band. Mrk 0622 at 10.7′. This leaves our total LIRG sample with 134 objects. 2.3. X-ray Hardness Flux Ratios and Comparison Sample 2.2. Faint BAT Source Detection in the GOALS Sample The ultra hard X-ray hardness flux ratio (HRUX =14- In Swift BAT, the detector noise distribution is a 195 keV/2-10 keV) provides a measure of obscuration Gaussian function centered at zero significance.
Load more

Recommended publications
  • The HERACLES View of the H -To-HI Ratio in Galaxies
    The HERACLES View of the H2-to-HI Ratio in Galaxies Adam Leroy (NRAO, Hubble Fellow) Fabian Walter, Frank Bigiel, the HERACLES and THINGS teams The Saturday Morning Summary • Star formation rate vs. gas relation on ~kpc scales breaks apart into: A relatively universal CO-SFR relation in nearby disks Systematic environmental scalings in the CO-to-HI ratio • The CO-to-HI ratio is a strong function of radius, total gas, and stellar surface density correlated with ISM properties: dust-to-gas ratio, pressure harder to link to dynamics: gravitational instability, arms • Interpretation: the CO-to-HI ratio traces the efficiency of GMC formation Density and dust can explain much of the observed behavior heracles Fabian Walter Erik Rosolowsky MPIA UBC Frank Bigiel Eva Schinnerer UC Berkeley THINGS plus… MPIA Elias Brinks Antonio Usero Gaelle Dumas U Hertfordshire OAN, Madrid MPIA Erwin de Blok Andreas Schruba Helmut Wiesemeyer U Cape Town IRAM … MPIA Rob Kennicutt Axel Weiss Karl Schuster Cambridge MPIfR IRAM Barry Madore Carsten Kramer Karin Sandstrom Carnegie IRAM MPIA Michele Thornley Daniela Calzetti Kelly Foyle Bucknell UMass MPIA Collaborators The HERA CO-Line Extragalactic Survey First maps Leroy et al. (2009) • IRAM 30m Large Program to map CO J = 2→1 line • Instrument: HERA receiver array operating at 230 GHz • 47 galaxies: dwarfs to starbursts and massive spirals -2 • Very wide-field (~ r25) and sensitive (σ ~ 1-2 Msun pc ) NGS The HI Nearby Galaxy Survey HI Walter et al. (2008), AJ Special Issue (2008) • VLA HI maps of 34 galaxies:
    [Show full text]
  • Radio Continuum and CO Emission in Star-Forming Galaxies
    A&A 385, 412–424 (2002) Astronomy DOI: 10.1051/0004-6361:20020140 & c ESO 2002 Astrophysics Radio continuum and CO emission in star-forming galaxies M. Murgia1,A.Crapsi1,2, L. Moscadelli3, and L. Gregorini1,4 1 Istituto di Radioastronomia del CNR, Via Gobetti 101, 40129, Bologna, Italy 2 Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125, Firenze, Italy 3 Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54, 09012 Capoterra (CA), Italy 4 Dipartimento di Fisica, Universit`a di Bologna, Via B. Pichat 6/2, 40127 Bologna, Italy Received 30 October 2001 / Accepted 23 January 2002 Abstract. We combine the radio continuum images from the NRAO VLA Sky Survey with the CO-line observations from the extragalactic CO survey of the Five College Radio Astronomy Observatory to study the relationship between molecular gas and the star formation rate within the disks of 180 spiral galaxies at 4500 resolution. We find a tight correlation between these quantities. On average, the ratio between the radio continuum and the CO emission is constant, within a factor of 3, both inside the same galaxy and from galaxy to galaxy. The mean star formation efficiency deduced from the radio continuum corresponds to convert 3.5% of the available molecular gas into stars on a time scale of 108 yr and depends weakly on general galaxy properties, such as Hubble type or nuclear activity. A comparison is made with another similar analysis performed using the Hα luminosity as star formation indicator. The overall agreement we find between the two studies reinforces the use of the radio luminosity as star formation rate indicator not only on global but also on local scales.
    [Show full text]
  • Arxiv:Astro-Ph/0309446V1 16 Sep 2003 N Necocigmlclrcod(..Mk38 Eke Al
    The Neutral ISM in Starburst Galaxies ASP Conference Series, Vol. xxx, 2003 S. Aalto, S. H¨uttemeister, A. Pedlar Extragalactic water masers in bright IRAS sources A. Tarchi1,2, C. Henkel3, A.B. Peck4, N. Nagar5, L. Moscadelli2, and K.M. Menten3 1Instituto di Radioastronomia, CNR, Bologna, Italy 2Osservatorio Astronomico di Cagliari, Capoterra (CA), Italy 3MPIfR, Bonn, Germany 4Harvard-Smithsonian CfA, SMA Project, Hilo, HI, USA 5Kapteyn Astronomical Institute, Groningen, the Netherlands Abstract. We report the results of a search for 22 GHz water maser emission in IRAS-bright galaxies, using the 100-m Effelsberg telescope. In particular, we present the details of four new maser detections (IC 342, NGC 2146, NGC 3556, and Arp 299) and follow-up interferometric stud- ies. A comparison between water maser detection rates derived in the present study and those in previous similar surveys is also presented. 1. Introduction To date, there is evidence for a total of three distinct classes of extragalactic H2O masers: i) H2O megamasers (with isotropic luminosities Liso > 10 L⊙) associated with accretion disks in active galaxies (e.g. NGC 4258, Miyoshi et al. 1995) ii) H2O megamasers resulting from an interaction between the nuclear radio jet and an encroaching molecular cloud (e.g. Mrk 348, Peck et al. 2001, 2003) iii) weaker H2O masers, the ‘kilomasers’ (with Liso < 10 L⊙), often associated with prominent star forming regions in large scale galactic disks, and, thus far arXiv:astro-ph/0309446v1 16 Sep 2003 found in galaxies containing bright IRAS (Infrared Astronomical Satellite) point sources (e.g. NGC 2146, Tarchi et al.
    [Show full text]
  • Star Formation and Galaxy Evolution of the Local Universe Based on HIPASS
    Star formation and galaxy evolution of the Local Universe based on HIPASS Oiwei Ivy Wong Submitted in total fulfilment of the requirements of the Degree of Doctor of Philosophy School of Physics University of Melbourne December, 2007 Abstract This thesis investigates the star formation and galaxy evolution of the nearby Local Volume based on Neutral Hydrogen (HI) studies. A large portion of this thesis con- sists of work with the Northern extension of the HI Parkes All Sky Survey (HIPASS). HIPASS is an HI survey of the entire Southern sky up to a declination of +25.5 de- grees (including the Northern extension) using the Parkes 64-metre radio telescope. I have also produced a catalogue of the optical counterparts corresponding to the galaxies found in Northern HIPASS. From this optical catalogue, we also conclude that we did not find any isolated dark galaxies. The other half of my thesis consists of work with the SINGG and SUNGG projects. SINGG is the Survey for Ioniza- tion in Neutral Gas Galaxies and SUNGG is the Survey of Ultraviolet emission in Neutral Gas Galaxies. Both SINGG and SUNGG are selected from HIPASS and are star formation studies in the H-alpha and ultraviolet (UV), respectively. My work in the SINGG-SUNGG collaboration is mostly based on SUNGG. Using the results of SUNGG, I measured the local luminosity density and the cosmic star formation rate density (SFRD) of the Local Universe. Using far-infrared (FIR) observations from IRAS, the FIR luminosity density was also calculated. Combining the FUV luminosity density and the FIR luminosity density, the bolometric SFRD of the Lo- cal Universe was estimated.
    [Show full text]
  • RED DE ASTRONOMÍA DE COLOMBIA, RAC [email protected]
    ___________________________________________________________ RED DE ASTRONOMÍA DE COLOMBIA, RAC www.eafit.edu.co/astrocol [email protected] CIRCULAR 506 de marzo 6 de 2009. ___________________________________________________________ Dirección: Antonio Bernal González: [email protected] Edición: Gonzalo Duque-Escobar: www.galeon.com/gonzaloduquee-00/ __________________________________________________________ Las opiniones emitidas en esta circular son responsabilidad de sus autores. ________________________________________________________ Apreciados amigos de la astronomía: El proyecto "100 horas de Astronomía" propuesto a nivel global por la Unión Astronómica Internacional UAI para los días 2 al 5 de abril de 2009 y que ha sido acogido por multitud de grupos de astrónomos profesionales y aficionados del mundo en diferentes lugares, se va consolidando como pilar emblemático entre los eventos centrales previstos y en curso para celebrar el Año Internacional de la Astronomía IYA2009. Invitamos a las varias decenas de grupos de la Red de Astronomía de Colombia a que, asociados unos y otros, se preparen con actividades escalonadas y variadas de difusión y divulgación, en una programación continua que requiere relevos, para participar en la interesante propuesta de la UAI y cuyo objeto es llevar durante estas 100 horas ininterrumpidas la Astronomía a todo tipo de público. En una región se pueden hacer alianzas entre grupos de diferentes localidades vecinas, concertando voluntades para sumar fuerzas y compartir recursos en torno a este común propósito. Con ciclos de conferencias, programas de radio y televisión, películas y foros científicos, sesiones de planetario y observación astronómica, entre otras ideas, este interesante e impactante programa puede hacerse una realidad. Desde el OAM, Gonzalo Duque-Escobar http://www.manizales.unal.edu.co/oam_manizales/ __________________________________________________________ BIENVENIDA Damos la bienvenida a personas y grupos que se inscribieron por medio del servidor automático de Yahoogroups.
    [Show full text]
  • Hubble Sights Galaxy Stuck in the Middle 30 April 2018
    Hubble sights galaxy stuck in the middle 30 April 2018 from Earth in the constellation of Camelopardalis (the Giraffe). Camelopardalis contains many other interesting deep-sky objects, including the open cluster NGC 1502, the elegant Kemble's Cascade asterism, and the starburst galaxy NGC 2146. Provided by NASA Credit: ESA/Hubble & NASA, A. Fillipenko This pretty, cloud-like object may not look much like a galaxy—it lacks the well-defined arms of a spiral galaxy, or the reddish bulge of an elliptical—but it is in fact something known as a lenticular galaxy. Lenticular galaxies sit somewhere between the spiral and elliptical types; they are disk-shaped, like spirals, but they no longer form large numbers of new stars and thus contain only aging populations of stars, like ellipticals. NGC 2655's core is extremely luminous, resulting in its additional classification as a Seyfert galaxy: a type of active galaxy with strong and characteristic emission lines. This luminosity is thought to be produced as matter is dragged onto the accretion disk of a supermassive black hole sitting at the center of NGC 2655. The structure of NGC 2655's outer disk, on the other hand, appears calmer, but it is oddly shaped. The complex dynamics of the gas in the galaxy suggest that it may have had a turbulent past, including mergers and interactions with other galaxies. NGC 2655 is located about 80 million light-years 1 / 2 APA citation: Hubble sights galaxy stuck in the middle (2018, April 30) retrieved 28 September 2021 from https://phys.org/news/2018-04-hubble-sights-galaxy-stuck-middle.html This document is subject to copyright.
    [Show full text]
  • Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/Luminous Infrared Galaxies Observed with Nustar And/Or Swift/BAT
    Draft version July 26, 2021 Typeset using LATEX twocolumn style in AASTeX631 Comprehensive Broadband X-ray and Multiwavelength Study of Active Galactic Nuclei in Local 57 Ultra/luminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT Satoshi Yamada ,1 Yoshihiro Ueda ,1 Atsushi Tanimoto ,2 Masatoshi Imanishi ,3, 4 Yoshiki Toba ,1, 5 Claudio Ricci ,6, 7, 8 and George C. Privon 9 1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan 2Department of Physics, The University of Tokyo, Tokyo 113-0033, Japan 3National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan 4Department of Astronomical Science, Graduate University for Advanced Studies (SOKENDAI), 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan 5Research Center for Space and Cosmic Evolution, Ehime University, 2-5 Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan 6N´ucleo de Astronom´ıade la Facultad de Ingenier´ıa,Universidad Diego Portales, Av. Ej´ercito Libertador 441, Santiago, Chile 7Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing 100871, People's Republic of China 8George Mason University, Department of Physics & Astronomy, MS 3F3, 4400 University Drive, Fairfax, VA 22030, USA 9National Radio Astronomy Observatory, 520 Edgemont Rd, Charlottesville, VA 22903, USA (Received April 13, 2021; Revised June 11, 2021; Accepted Jul, 2021) ABSTRACT We perform a systematic X-ray spectroscopic analysis of 57 local ultra/luminous infrared galaxy systems (containing 84 individual galaxies) observed with Nuclear Spectroscopic Telescope Array and/or Swift/BAT. Combining soft X-ray data obtained with Chandra, XMM-Newton, Suzaku and/or Swift/XRT, we identify 40 hard (>10 keV) X-ray detected active galactic nuclei (AGNs) and con- strain their torus parameters with the X-ray clumpy torus model XCLUMPY (Tanimoto et al.
    [Show full text]
  • Title Spons Agency Bureau No Pub Date Contract Note
    DOCUMENT LIZSUME ED 071' C87 82 015 524 TITLE Project Musics Reader 2,Motion in the Heavens. .INSTITUTION Harvard Univ., Cambridge,Mass. Harvard Project _Physics. SPONS AGENCY Office of Education (DREW), Washington, D.C.,Bureau of Research. BUREAU NO BK-5-1038 PUB DATE 68 CONTRACT 08C-5-10-058 NOTE 233p.; Authorized InterimVersion EDRS PRICE MF -$0.65 HC-89.87 _DESCRIPTORS Astronomy; Instructional Materials;.*Motion; *Physics; Science, Fiction;. Science Materials; _Secondary Grades; *Secondary School Science; *Space; *Supplementary Reading Materials IDENTIFIER'S Harvard Project Physics ABSTRACT As a supplement to.Projpct Physics Unit 2, specially, selected articles are presented in this reader for student browsing. _Eight excerpts are given under headings:,the starry messenger, Newton_. And the principia, an appreciation of the earth, space the unconquerable, Is there intelligent life beyond the earth3,11 the life story of a galaxy, expansion of the universe, and Dyson sphere. Seven book passages. are included under. the, headings of the black cloud, roll call, a night at the observatory, Repler's celestial music, universal gravitation, a table of stars within twenty-two light years that could have habitable planets, and three poetic _fragments about astronomy. The remaining articles includea preface to the books of the ,revolutions, Kepler, Kepler on. Mars, laws of ..motion and proposition one,, garden of Epicurus, a search for life on earth at Kilometer resolution, the. boy who redeemed his father's _name, great comet of 1965, gravity experiments, unidentified flying objects, and negative mass. Illustrations for explanationpurposes . are provided. The work of Harvard. Project Physics has been .financially supported by: the Carnegie Corporation of New York, the Ford.
    [Show full text]
  • 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
    [Show full text]
  • 1987Apj. . .320. .2383 the Astrophysical Journal, 320:238-257
    .2383 The Astrophysical Journal, 320:238-257,1987 September 1 © 1987. The American Astronomical Society. AU rights reserved. Printed in U.S.A. .320. 1987ApJ. THE IRÁS BRIGHT GALAXY SAMPLE. II. THE SAMPLE AND LUMINOSITY FUNCTION B. T. Soifer, 1 D. B. Sanders,1 B. F. Madore,1,2,3 G. Neugebauer,1 G. E. Danielson,4 J. H. Elias,1 Carol J. Lonsdale,5 and W. L. Rice5 Received 1986 December 1 ; accepted 1987 February 13 ABSTRACT A complete sample of 324 extragalactic objects with 60 /mi flux densities greater than 5.4 Jy has been select- ed from the IRAS catalogs. Only one of these objects can be classified morphologically as a Seyfert nucleus; the others are all galaxies. The median distance of the galaxies in the sample is ~ 30 Mpc, and the median 10 luminosity vLv(60 /mi) is ~2 x 10 L0. This infrared selected sample is much more “infrared active” than optically selected galaxy samples. 8 12 The range in far-infrared luminosities of the galaxies in the sample is 10 LQ-2 x 10 L©. The far-infrared luminosities of the sample galaxies appear to be independent of the optical luminosities, suggesting a separate luminosity component. As previously found, a correlation exists between 60 /¿m/100 /¿m flux density ratio and far-infrared luminosity. The mass of interstellar dust required to produce the far-infrared radiation corre- 8 10 sponds to a mass of gas of 10 -10 M0 for normal gas to dust ratios. This is comparable to the mass of the interstellar medium in most galaxies.
    [Show full text]
  • A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
    TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques.
    [Show full text]
  • Red-Channel (6000-8000 {\AA}) Nuclear Spectra of 376 Local Galaxies
    Astronomy & Astrophysics manuscript no. loispectra˙rev c ESO 2018 November 2, 2018 Red-channel (6000-8000 Å) nuclear spectra of 376 local galaxies ⋆ Giuseppe Gavazzi1, Guido Consolandi1, Massimo Dotti1, Matteo Fossati2,3,1, Giulia Savorgnan4, Roberto Gualandi5, Ivan Bruni5 1 Dipartimento di Fisica G. Occhialini, Universit`adi Milano- Bicocca, Piazza della Scienza 3, I-20126 Milano, Italy e-mail: [email protected], [email protected], [email protected] 2 Universit¨ats-Sternwarte M¨unchen, Scheinerstrasse 1, D-81679 M¨unchen, Germany e-mail: [email protected] 3 Max-Planck-Institut f¨ur Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany 4 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria 3122, Australia e-mail: [email protected] 5 Osservatorio astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy e-mail: [email protected], [email protected] Received - Accepted ABSTRACT We obtained long-slit optical spectra of the nuclear regions of 376 galaxies in the local Universe using the 1.5m Cassini telescope of Bologna Observatory. Of these spectra, 164 were either never taken before by the Sloan Digital Sky Survey (SDSS), or given by the Nasa Extragalactic Database (NED). With these new spectra, we contribute investigating the occurrence of active galactic nuclei (AGNs). Nevertheless, we stress that the present sample is by no means complete, thus, it cannot be used to perform any demographic study. Following the method presented in Gavazzi et al (2011), we classify the nuclear spectra using a six bin scheme: SEY (Seyfert), sAGN (strong AGN), and wAGN (weak AGN) represent active galactic nuclei of different levels of activity; HII accounts for star-forming nuclei; RET (retired) and PAS (passive) refer to nuclei with poor or no star-formation activity.
    [Show full text]