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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. -
VEGAS: a VST Early-Type Galaxy Survey. the Faint Substructures of NGC 4472 Stellar Halo
VEGAS: A VST Early-type GAlaxy Survey. The faint substructures of NGC 4472 stellar halo. MARILENA SPAVONE ON THE BEHALF OF THE VEGAS TEAM: M. CAPACCIOLI, M. CANTIELLO, A. GRADO, E. IODICE, F. LA BARBERA, N.R. NAPOLITANO, C. TORTORA, L. LIMATOLA, M. PAOLILLO, T. PUZIA, R. PELETIER, A.J. ROMANOWSKY, D. FORBES, G. RAIMONDO OUTLINE The VST VEGAS survey Science aims Results on NGC 4472 field Conclusions Future plans MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). An example Obj. name Morph. type u g r i IC 1459 E3 5630 1850 1700 NGC 1399 E1 8100 5320 2700 NGC 3115 S0 14800 8675 6030 Observations to date (to P94) g-BAND ~ 16% i-BAND ~ 19% r-BAND ~ 3% + FORNAX u-BAND ~ 1% MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). OT ~ 350 h @ vst over 5 years Expected SB limits: 27.5 g, 2 27.0 r and 26.2 i mag/arcsec . g band expected SB limit MARILENA SPAVONE STELLAR HALOS 2015 ESO-GARCHING, 23-27 FEBRUARY THE VEGAS SURVEY Multiband u, g, r, i survey of ~ 110 galaxies with vrad < 4000 km/s in all environments (field to clusters). ~ 350 h @ vst over 5 years Expected SB limits: 27.5 g, 27.0 r and 26.2 i mag/arcsec2. -
The SBF Survey of Galaxy Distances. I. Sample Selection, Photometric
TheSBFSurveyofGalaxyDistances.I. Sample Selection, Photometric Calibration, and the Hubble Constant1 John L. Tonry2 and John P. Blakeslee2 Physics Dept. Room 6-204, MIT, Cambridge, MA 02139; Edward A. Ajhar2 Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732 Tucson, AZ 85726; Alan Dressler Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101 ABSTRACT We describe a program of surface brightness fluctuation (SBF) measurements for determining galaxy distances. This paper presents the photometric calibration of our sample and of SBF in general. Basing our zero point on observations of Cepheid variable stars we find that the absolute SBF magnitude in the Kron-Cousins I band correlates well with the mean (V −I)0 color of a galaxy according to M I =(−1.74 ± 0.07) + (4.5 ± 0.25) [(V −I)0 − 1.15] for 1.0 < (V −I) < 1.3. This agrees well with theoretical estimates from stellar popula- tion models. Comparisons between SBF distances and a variety of other estimators, including Cepheid variable stars, the Planetary Nebula Luminosity Function (PNLF), Tully-Fisher (TF), Dn−σ, SNII, and SNIa, demonstrate that the calibration of SBF is universally valid and that SBF error estimates are accurate. The zero point given by Cepheids, PNLF, TF (both calibrated using Cepheids), and SNII is in units of Mpc; the zero point given by TF (referenced to a distant frame), Dn−σ, and SNIa is in terms of a Hubble expan- sion velocity expressed in km/s. Tying together these two zero points yields a Hubble constant of H0 =81±6 km/s/Mpc. -
Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei Davide Lena
Rochester Institute of Technology RIT Scholar Works Theses Thesis/Dissertation Collections 4-2015 Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei Davide Lena Follow this and additional works at: http://scholarworks.rit.edu/theses Recommended Citation Lena, Davide, "Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei" (2015). Thesis. Rochester Institute of Technology. Accessed from This Dissertation is brought to you for free and open access by the Thesis/Dissertation Collections at RIT Scholar Works. It has been accepted for inclusion in Theses by an authorized administrator of RIT Scholar Works. For more information, please contact [email protected]. Aspects of Supermassive Black Hole Growth in Nearby Active Galactic Nuclei A Search for Recoiling Supermassive Black Holes Gas Kinematics in the Circumnuclear Region of Two Seyfert Galaxies Davide Lena A dissertation submitted in partial fulfillment of the requirements for the degree of Ph.D. in Astrophysical Sciences and Technology in the College of Science, School of Physics and Astronomy Rochester Institute of Technology © D. Lena April, 2015 Cover image: flux map for the [NII]λ6583 emission line in the nuclear region of the Seyfert galaxy NGC 1386. The map was derived from integral field observations performed with the Gemini Multi Object Spectrograph on the Gemini-South Observatory. Certificate of Approval Astrophysical Sciences and Technologies R·I·T College of Science Rochester, NY, USA The Ph.D. Dissertation of DAVIDE LENA has been approved by the undersigned members of the dissertation committee as satisfactory for the degree of Doctor of Philosophy in Astrophysical Sciences and Technology. -
Compact Jets Causing Large Turmoil in Galaxies Enhanced Line Widths Perpendicular to Radio Jets As Tracers of Jet-ISM Interaction?
A&A 648, A17 (2021) Astronomy https://doi.org/10.1051/0004-6361/202039869 & c G. Venturi et al. 2021 Astrophysics MAGNUM survey: Compact jets causing large turmoil in galaxies Enhanced line widths perpendicular to radio jets as tracers of jet-ISM interaction? G. Venturi1,2, G. Cresci2, A. Marconi3,2, M. Mingozzi4, E. Nardini3,2, S. Carniani5,2, F. Mannucci2, A. Marasco2, R. Maiolino6,7,8 , M. Perna9,2, E. Treister1, J. Bland-Hawthorn10,11, and J. Gallimore12 1 Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile e-mail: [email protected] 2 INAF-Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: [email protected] 3 Dipartimento di Fisica e Astronomia, Università degli Studi di Firenze, Via G. Sansone 1, 50019 Sesto Fiorentino, Firenze, Italy 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 Scuola Normale Superiore, Piazza dei Cavalieri 7, 56126 Pisa, Italy 6 Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Ave., Cambridge CB3 0HE, UK 7 Kavli Institute for Cosmology, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 8 Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK 9 Centro de Astrobiología (CSIC-INTA), Departamento de Astrofísica Cra. de Ajalvir Km. 4, 28850 Torrejón de Ardoz, Madrid, Spain 10 Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, NSW 2006, Australia 11 ARC Centre of Excellence for All Sky Astrophysics in Three Dimensions (ASTRO-3D), Canberra ACT2611, Australia 12 Department of Physics and Astronomy, Bucknell University, Lewisburg, PA 17837, USA Received 6 November 2020 / Accepted 13 January 2021 ABSTRACT Context. -
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 -
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. -
Giacomo Venturi Phd Student at University of Florence / INAF - Arcetri Astrophysical Observatory Visitor at Kavli Institute for Cosmology, Cambridge
The Laws of Star Formation: From the Cosmic Dawn to the Present Universe July 4, 2018 Outflows versus star formation in nearby AGN from the MAGNUM survey Giacomo Venturi PhD student at University of Florence / INAF - Arcetri Astrophysical Observatory Visitor at Kavli Institute for Cosmology, Cambridge A. Marconi (P.I.), M. Mingozzi, S. Carniani, R. Maiolino, G. Cresci, E. Nardini et al. Galaxy evolution: the need for outflows Stellar (SN) feedback accounts for the lack of low-mass galaxies Feedback damps/quenches star formation! acting through outflows/jets! driven by SNe or AGN AGN feedback accounts for the lack of massive galaxies Silk & Mamon 2012 G. Venturi Outflows vs star formation in nearby AGN from the MAGNUM survey "2 Detecting outflows Ionized outflows traced by broad wings in [OIII] in luminous AGN at z ~ 1–3 Brusa+2016 peak of AGN activity [OIII] velocity Star Formation (Hα) [OIII] wing map Star Formation (Hα) Cresci+15a Carniani+16 Bongiorno+07 … but low-resolution, very difficult to measure outflow physical properties and study feedback in detail G. Venturi! Outflows vs star formation in nearby AGN from the MAGNUM survey ! "3 MAGNUM survey Study in detail outflows and feedback in nearby (D < 50 Mpc) Seyfert galaxies with VLT/MUSE FOV covers 1 to 15 kpc with resolution: 15 pc (@4Mpc) to 115 pc (@30Mpc) VLT/MUSE FOV 1'⨉1' Centaurus A Circinus IC 5063 NGC 1068 NGC 1365 NGC 1386 NGC 2992 NGC 4945 NGC 5643 NGC 6810 G. Venturi! Outflows vs star formation in nearby AGN from the MAGNUM survey ! "4 Part 1: NGC 1365 Detailed study of ionized gas in the central kpcs of NGC 1365:! AGN vs star formation, mapping the outflow properties! from optical (MUSE) and X-ray (Chandra) data! (Venturi et al., subm.) G. -
Nuclear Activity in Circumnuclear Ring Galaxies
International Journal of Astronomy and Astrophysics, 2016, 6, 219-235 Published Online September 2016 in SciRes. http://www.scirp.org/journal/ijaa http://dx.doi.org/10.4236/ijaa.2016.63018 Nuclear Activity in Circumnuclear Ring Galaxies María P. Agüero1, Rubén J. Díaz2,3, Horacio Dottori4 1Observatorio Astronómico de Córdoba, UNCand CONICET, Córdoba, Argentina 2ICATE, CONICET, San Juan, Argentina 3Gemini Observatory, La Serena, Chile 4Instituto de Física, UFRGS, Porto Alegre, Brazil Received 23 May 2016; accepted 26 July 2016; published 29 July 2016 Copyright © 2016 by authors and Scientific Research Publishing Inc. This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/ Abstract We have analyzed the frequency and properties of the nuclear activity in a sample of galaxies with circumnuclear rings and spirals (CNRs), compiled from published data. From the properties of this sample a typical circumnuclear ring can be characterized as having a median radius of 0.7 kpc (mean 0.8 kpc, rms 0.4 kpc), located at a spiral Sa/Sb galaxy (75% of the hosts), with a bar (44% weak, 37% strong bars). The sample includes 73 emission line rings, 12 dust rings and 9 stellar rings. The sample was compared with a carefully matched control sample of galaxies with very similar global properties but without detected circumnuclear rings. We discuss the relevance of the results in regard to the AGN feeding processes and present the following results: 1) bright companion galaxies seem