Parsec-Scale Dust Distributions in Seyfert Galaxies
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Kinematics of Nearby Active Galactic Nucleus Host Ngc 7582
KINEMATICS OF NEARBY ACTIVE GALACTIC NUCLEUS HOST NGC 7582 Item Type Electronic Thesis; text Authors Walla, Emily Citation Walla, Emily. (2020). KINEMATICS OF NEARBY ACTIVE GALACTIC NUCLEUS HOST NGC 7582 (Bachelor's thesis, University of Arizona, Tucson, USA). Publisher The University of Arizona. Rights Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. Download date 07/10/2021 08:31:34 Item License http://rightsstatements.org/vocab/InC/1.0/ Link to Item http://hdl.handle.net/10150/651409 KINEMATICS OF NEARBY ACTIVE GALACTIC NUCLEUS HOST NGC 7582 By EMILY CATHERINE WALLA ____________________ A Thesis Submitted to The Honors College In Partial Fulfillment of the Bachelor’s degree With Honors in Astronomy THE UNIVERSITY OF ARIZONA MAY 2020 Approved by: ______________________ Dr. Stephanie Juneau NSF National Optical-Infrared Astronomy Research Lab, The Astro Data Lab Dr. Susan Ridgway, NSF National Optical-Infrared Astronomy Research Laboratory, served as a secondary advisor for this project. She provided extensive scientific background for the project. Madison Walder, undergraduate student in the University of Arizona Class of Spring 2020, worked on a project adjacent to mine and as such, provided some small modifications to the code eventually used to complete my project. Leah Fulmer, PhD candidate at the University of Washington, worked with Stephanie Juneau before me and completed some initial analyses and wrote code that was foundational in the first year of the project but was ultimately not implemented in the project’s final form. -
Stellar Populations of Bulges of Disc Galaxies in Clusters
Astronomical Science Stellar Populations of Bulges of Disc Galaxies in Clusters Lorenzo Morelli1, 5 brightness radial profile of large bulges is assembly. We present a photometric and Emanuela Pompei 2 well described by the de Vaucouleurs spectroscopic study of the bulge-domi- Alessandro Pizzella1 law, although this law can be drastically nated region of a sample of spiral galax- Jairo Méndez-Abreu1, 3 changed taking into account the small- ies in clusters. Our aim is to estimate the Enrico Maria Corsini1 scale inner structures, smoothed by the age and metallicity of the stellar popula- Lodovico Coccato 4 seeing in ground-based observations. tion and the efficiency and timescale of Roberto Saglia 4 Some bulges are rotationally-flattened the last episode of star formation in order Marc Sarzi 6 oblate spheroids with little or no anisot- to disentangle early rapid assembly from Francesco Bertola1 ropy. But, the intrinsic shape of a large late slow growth of bulges. fraction of early-type bulges is triaxial, as shown by the isophotal misalignment 1 Dipartimento di Astronomia, Università with respect to their host discs and non- Sample, photometry, and spectroscopy di Padova, Italy circular gas motions. The bulk of their 2 ESO stellar population formed between red- In order to simplify the interpretation of 3 INAF-Osservatorio Astronomico di shifts 3 and 5 (~ 12 Gyr ago) over a short the results, we selected a sample of disc Padova, Italy timescale. The enrichment of the inter- galaxies, which do not show any mor- 4 Max-Planck-Institut für Extraterres- stellar medium is strongly related to the phological signature of having undergone trische Physik, Garching, Germany time delay between type II and type Ia a recent interaction event. -
Lopsided Spiral Galaxies: Evidence for Gas Accretion
A&A 438, 507–520 (2005) Astronomy DOI: 10.1051/0004-6361:20052631 & c ESO 2005 Astrophysics Lopsided spiral galaxies: evidence for gas accretion F. Bournaud1, F. Combes1,C.J.Jog2, and I. Puerari3 1 Observatoire de Paris, LERMA, 61 Av. de l’Observatoire, 75014 Paris, France e-mail: [email protected] 2 Department of Physics, Indian Institute of Science, Bangalore 560012, India 3 Instituto Nacional de Astrofísica, Optica y Electrónica, Calle Luis Enrique Erro 1, 72840 Tonantzintla, Puebla, Mexico Received 3 January 2005 / Accepted 15 March 2005 Abstract. We quantify the degree of lopsidedness for a sample of 149 galaxies observed in the near-infrared from the OSUBGS sample, and try to explain the physical origin of the observed disk lopsidedness. We confirm previous studies, but for a larger sample, that a large fraction of galaxies have significant lopsidedness in their stellar disks, measured as the Fourier amplitude of the m = 1 component normalised to the average or m = 0 component in the surface density. Late-type galaxies are found to be more lopsided, while the presence of m = 2 spiral arms and bars is correlated with disk lopsidedness. We also show that the m = 1 amplitude is uncorrelated with the presence of companions. Numerical simulations were carried out to study the generation of m = 1viadifferent processes: galaxy tidal encounters, galaxy mergers, and external gas accretion with subsequent star formation. These simulations show that galaxy interactions and mergers can trigger strong lopsidedness, but do not explain several independent statistical properties of observed galaxies. To explain all the observational results, it is required that a large fraction of lopsidedness results from cosmological accretion of gas on galactic disks, which can create strongly lopsided disks when this accretion is asymmetrical enough. -
Presentazione Standard Di Powerpoint
Challenges to the AGN Unified Model Stefano Bianchi The X-ray view of Black Hole activity in the local Universe – Zurich – February 18th 2016 The Geometry of Absorption The absorber: The Unification Model view NLR The absorber must break the symmetry of the polarization angles: a “torus” is the most BLR natural configuration BLR Torus The size of the torus was postulated to be on the parsec scale (Krolik & Begelman, 1986, 1988) Large enough to obscure the BLR Small enough not to obscure the NLR From Galactic to Sub-Pc Scale: Absorption at Different Scales The presence of nonspherically symmetric absorbers at the origin of the type 1/type 2 dichotomy remains a valid scenario, but several new observations and models suggest that multiple absorbers are present, on quite different physical scales Absorption within the Sublimation Radius Absorption from pc-scale Tori Absorption by Gas in the Host Galaxy Absorption within the Sublimation Radius X-ray absorption variability is common in AGN: the circumnuclear X-ray absorber (or, at least, one component of it) must be clumpy and located at subparsec distance Risaliti et al. 2007 NH variations on scales from months to NGC 7582 hours are found in a growing number of sources: NGC 1365 (Risaliti et al. 2005, 2007, 2009), NGC 4388 (Elvis et al. 2004), NGC 4151 (Puccetti et al. 2007), NGC 7582 (Bianchi et al. 2009), Mrk 766 (Risaliti et al. 2011) 23 -2 DNH~10 cm See also the exceptional case of DT~20 hours NGC1068! (Marinucci’s talk) Bianchi et al. 2009 NGC 1365 shows absorption variability down to ∼10 hours: absorption is 3 −1 4 due to clouds with velocity >10 km s , at distances of ~10 rg. -
Seyfert 1 Mutation of the Classical Seyfert 2 Nucleus NGC 7582
Seyfert 1 mutation of the classical Seyfert 2 nucleus NGC 75821 Itziar Aretxaga Instituto Nacional de Astrof´ısica, Optica´ y Electr´onica, Apdo. Postal 25 y 216, 72000 Puebla, Pue., Mexico E-mail: [email protected] B. Joguet European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile Institut d’Astrophysique de Paris, 98 bis Boulevard Arago, F-75014 Paris, France E-mail:[email protected] D. Kunth Institut d’Astrophysique de Paris, 98 bis Boulevard Arago, F-75014 Paris, France E-mail: [email protected] J. Melnick European Southern Observatory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile E-mail: [email protected] arXiv:astro-ph/9905147v1 12 May 1999 and R. J. Terlevich2 Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, U.K. E-mail: [email protected] 1 Based on observations collected at the European Southern Observatory at La Silla (Chile) 2Visiting Professor at INAOE, Puebla, Mexico –2– Received ; accepted Submitted to Astrophysical Journal Letters –3– ABSTRACT We report the transition towards a type 1 Seyfert experienced by the classical type 2 Seyfert nucleus in NGC 7582. The transition, found at most 20 days from its maximum peak, presents a unique opportunity to study these rare events in detail. At maximum the Hα line width is of about 12000 km s−1. We examine three scenarios that could potentially explain the transition: capture of a star by a supermassive black hole, a reddening change in the surrounding torus, and the radiative onset of a type IIn supernova exploding in a compact nuclear/circumnuclear starburst. -
The Iso Handbook
THE ISO HANDBOOK Volume I: ISO – Mission & Satellite Overview Martin F. Kessler1,2, Thomas G. M¨uller1,4, Kieron Leech 1, Christophe Arviset1, Pedro Garc´ıa-Lario1, Leo Metcalfe1, Andy M. T. Pollock1,3, Timo Prusti1,2 and Alberto Salama1 SAI-2000-035/Dc, Version 2.0 November, 2003 1 ISO Data Centre, Science Operations and Data Systems Division Research and Scientific Support Department of ESA, Villafranca del Castillo, P.O. Box 50727, E-28080 Madrid, Spain 2 ESTEC, Science Operations and Data Systems Division Research and Scientific Support Department of ESA, Keplerlaan 1, Postbus 299, 2200 AG Noordwijk, The Netherlands 3 Computer & Scientific Co. Ltd., 230 Graham Road, Sheffield S10 3GS, England 4 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany ii Document Information Document: The ISO Handbook Volume: I Title: ISO - Mission & Satellite Overview Reference Number: SAI/2000-035/Dc Issue: Version 2.0 Issue Date: November 2003 Authors: M.F. Kessler, T. M¨uller, K. Leech et al. Editors: T. M¨uller, J. Blommaert & P. Garc´ıa-Lario Web-Editor: J. Matagne Document History The ISO Handbook, Volume I: ISO – Mission & Satellite Overview is mainly based on the following documents: • The ISO Handbook, Volume I: ISO – Mission Overview, Kessler M.F., M¨uller T.G., Arviset C. et al., earlier versions, SAI-2000-035/Dc. • The ISO Handbook, Volume II: ISO – The Satellite and its Data, K. Leech & A.M.T. Pollock, earlier versions, SAI-99-082/Dc. • The following ESA Bulletin articles: The ISO Mission – A Scientific Overview, M.F. Kessler, A. -
The Nuclear Regions of NGC 7582 from [Ne II] Spectroscopy at 12.8 Μm – an Estimate of the Black Hole Mass
A&A 460, 449–457 (2006) Astronomy DOI: 10.1051/0004-6361:20053385 & c ESO 2006 Astrophysics The nuclear regions of NGC 7582 from [Ne II] spectroscopy at 12.8 µm – an estimate of the black hole mass M. Wold1,M.Lacy2,H.U.Käufl1, and R. Siebenmorgen1 1 European Southern Observatory, Karl-Schwarzschild str. 2, 85748 Garching bei München, Germany e-mail: [email protected] 2 Spitzer Science Center, California Institute of Technology, Caltech, MC 220-6, Pasadena, CA 91125, USA Received 9 May 2005 / Accepted 10 August 2006 ABSTRACT We present a high-resolution (R ≈ 16 000) spectrum and a narrow-band image centered on the [Ne ii]12.8 µm line of the central kpc region of the starburst/Seyfert 2 galaxy NGC 7582. The galaxy has a rotating circum-nuclear starburst disk, shown at great detail at a diffraction-limited resolution of 0. 4(≈40 pc). The high spatial resolution allows us to probe the dynamics of the [Ne ii]gasin the nuclear regions, and to estimate the mass of the central black hole. We construct models of gas disks rotating in the combined 7 gravitational potential from the stellar bulge and a central black hole, and derive a black hole mass of 5.5 × 10 M with a 95% 7 confidence interval of [3.6, 8.1] × 10 M. The black hole mass combined with stellar velocity dispersion measurements from the literature shows that the galaxy is consistent with the local MBH-σ∗ relation. This is the first time that a black hole mass in a galaxy except our own Milky Way system has been estimated from gas dynamics in the mid-infrared. -
Download PDF of Abstracts
15th HEAD Naples, FL – April, 2016 Meeting Program Session Table of Contents 100 – AGN I Analysis Poster Session 206 – Early Results from the Astro-H 101 – Galaxy Clusters 116 – Missions & Instruments Poster Mission 102 – Dissertation Prize Talk: Accretion Session 207 – Stellar Compact II driven outflows across the black hole mass 117 – Solar and Stellar Poster Session 300 – The Physics of Accretion Disks – A scale, Ashley King (KIPAC/Stanford 118 – Supernovae and Supernova Joint HEAD/LAD Session University) Remnants Poster Session 301 – Gravitational Waves 103 – Time Domain Astronomy 119 – WDs & CVs Poster Session 302 – Missions & Instruments 104 – Feedback from Accreting Binaries in 120 – XRBs and Population Surveys Poster 303 – Mid-Career Prize Talk: In the Ring Cosmological Scales Session with Circinus X-1: A Three-Round Struggle 105 – Stellar Compact I 200 – Solar Wind Charge Exchange: to Reveal its Secrets, Sebastian Heinz 106 – AGNs Poster Session Measurements and Models (Univ. of Wisconsin) 107 – Astroparticles, Cosmic Rays, and 201 – TeraGauss, Gigatons, and 304 – Science of X-ray Polarimetry in the Neutrinos Poster Session MegaKelvin: Theory and Observations of 21st Century 108 – Cosmic Backgrounds and Deep Accretion Column Physics 305 – Making the Multimessenger – EM Surveys Poster Session 202 – The Structure of the Inner Accretion Connection 109 – Galactic Black Holes Poster Session Flow of Stellar-Mass and Supermassive 306 – SNR/GRB/Gravitational Waves 110 – Galaxies and ISM Poster Session Black Holes 400 – AGN II 111 – Galaxy -
Radio Emission of the Nuclei of Barred Spiral Galaxies
RADIO EMISSION OF THE NUCLEI OF BARRED SPIRAL GALAXIES By H. M. TOVMASSIAN* [Manuscript received May 27, 1966] Summary The results of radio observations of 98 barred galaxies at 11, 21, and 75 cm are presented. The observations were carried out with the 210 ft radio telescope of the Australian National Radio Astronomy Observatory and with the Mills Oross of the Sydney University Molonglo Radio Observatory. Radio emission originating within 1· 5 minutes of arc of the centre of corresponding galaxies was detected in 21 cases. It is concluded that the central parts of galaxies (possibly their nuclei) are responsible for the radio emission. Spectral indices of detected sources were determined. Radio indices show that radio emissivity of the majority of the investi gated galaxies is higher than that of normal galaxies. I. INTRODUCTION For some years after the discovery of radio galaxies, collisions between galaxies were accepted by many as the cause of the intense radio emission (Baade and Minkowski 1954; Shklowski 1954; and others). Ambartsumian (1956a) was the first to reject the idea of random collisions as an explanation of the observed phenomena. He came to this conclusion by considering certain observational data, particularly that a collision is an extremely rare event among the superluminous galaxies to which the radio galaxies belong. Subsequently he proposed and developed (Ambartsumian 1956b, 1958, 1962) a theory stressing the importance of the activity of the nuclei in the formation and evolution of galaxies. Some forms of nuclear activ ity result in powerful radio emission. Nowadays the hypothesis of nuclear activity is widely accepted and there is much observational evidence in favour of it. -
Cold Molecular Gas and PAH Emission in the Nuclear and Circumnuclear Regions of Seyfert Galaxies.', Astronomy Astrophysics., 639
Durham Research Online Deposited in DRO: 06 August 2020 Version of attached le: Published Version Peer-review status of attached le: Peer-reviewed Citation for published item: Alonso-Herrero, A. and Pereira-Santaella, M. and Rigopoulou, D. and Garc¡a-Bernete,I. and Garc¡a-Burillo, S. and Dom¡nguez-Fern¡andez,A. J. and Combes, F. and Davies, R. I. and D¡az-Santos, T. and Esparza-Arredondo, D. and Gonz¡alez-Mart¡n,O. and Hern¡an-Caballero, A. and Hicks, E. K. S. and H¤onig,S. F. and Levenson, N. A. and Ramos Almeida, C. and Roche, P. F. and Rosario, D. (2020) 'Cold molecular gas and PAH emission in the nuclear and circumnuclear regions of Seyfert galaxies.', Astronomy astrophysics., 639 . A43. Further information on publisher's website: https://doi.org/10.1051/0004-6361/202037642 Publisher's copyright statement: Alonso-Herrero, A., Pereira-Santaella, M., Rigopoulou, D., Garc¡a-Bernete,I., Garc¡a-Burillo,S., Dom¡nguez-Fern¡andez,A. J., Combes, F., Davies, R. I., D¡az-Santos, T., Esparza-Arredondo, D., Gonz¡alez-Mart¡n, O., Hern¡an-Caballero,A., Hicks, E. K. S., H¤onig,S. F., Levenson, N. A., Ramos Almeida, C., Roche, P. F. Rosario, D. (2020). Cold molecular gas and PAH emission in the nuclear and circumnuclear regions of Seyfert galaxies. Astronomy Astrophysics 639: A43, reproduced with permission, c ESO. Additional information: Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. -
H-Alpha Imaging of Early-Type (Sa-Sab) Spiral Galaxies I
Hα Imaging of Early-Type(Sa-Sab) Spiral Galaxies I1 Salman Hameed2, Nick Devereux2 Astronomy Department, New Mexico State University, Las Cruces, NM 88003 ABSTRACT Hα and continuum images are presented for 27 nearby early-type(Sa-Sab) spiral galaxies. Contrary to popular perception, the images reveal copious massive star formation in some of these galaxies. A determination of the Hα morphology and a measure of the Hα luminosity suggests that early-type spirals can be classified into two broad categories based on the luminosity of largest H II region in the disk. The first category includes galaxies for which the 39 −1 individual H II regions have LHα < 10 ergs . Most of the category 1 galaxies appear to be morphologically undisturbed, but show a wide diversity in nuclear Hα properties. The second category includes galaxies which have at least one 39 −1 H II region in the disk with LHα ≥ 10 ergs . All category 2 galaxies show either prominent dust lanes or other morphological peculiarities such as tidal tails which suggests that the anomalously luminous H II regions in category 2 galaxies may have formed as a result of a recent interaction. The observations, which are part of an on-going Hα survey, reveal early-type spirals to be a heterogeneous class of galaxies that are evolving in the current epoch. We have also identified some systematic differences between the classifications of spiral galaxies in the Second General Catalog (RC2) and the Revised Shapley- Ames Catalog (RSA) which may be traced to subtle variations in the application of the criteria used for classifying spiral galaxies. -
Astronomy Magazine 2020 Index
Astronomy Magazine 2020 Index SUBJECT A AAVSO (American Association of Variable Star Observers), Spectroscopic Database (AVSpec), 2:15 Abell 21 (Medusa Nebula), 2:56, 59 Abell 85 (galaxy), 4:11 Abell 2384 (galaxy cluster), 9:12 Abell 3574 (galaxy cluster), 6:73 active galactic nuclei (AGNs). See black holes Aerojet Rocketdyne, 9:7 airglow, 6:73 al-Amal spaceprobe, 11:9 Aldebaran (Alpha Tauri) (star), binocular observation of, 1:62 Alnasl (Gamma Sagittarii) (optical double star), 8:68 Alpha Canum Venaticorum (Cor Caroli) (star), 4:66 Alpha Centauri A (star), 7:34–35 Alpha Centauri B (star), 7:34–35 Alpha Centauri (star system), 7:34 Alpha Orionis. See Betelgeuse (Alpha Orionis) Alpha Scorpii (Antares) (star), 7:68, 10:11 Alpha Tauri (Aldebaran) (star), binocular observation of, 1:62 amateur astronomy AAVSO Spectroscopic Database (AVSpec), 2:15 beginner’s guides, 3:66, 12:58 brown dwarfs discovered by citizen scientists, 12:13 discovery and observation of exoplanets, 6:54–57 mindful observation, 11:14 Planetary Society awards, 5:13 satellite tracking, 2:62 women in astronomy clubs, 8:66, 9:64 Amateur Telescope Makers of Boston (ATMoB), 8:66 American Association of Variable Star Observers (AAVSO), Spectroscopic Database (AVSpec), 2:15 Andromeda Galaxy (M31) binocular observations of, 12:60 consumption of dwarf galaxies, 2:11 images of, 3:72, 6:31 satellite galaxies, 11:62 Antares (Alpha Scorpii) (star), 7:68, 10:11 Antennae galaxies (NGC 4038 and NGC 4039), 3:28 Apollo missions commemorative postage stamps, 11:54–55 extravehicular activity