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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. -
Planetary Nebula IC 5148 and Its Ionized Halo? D
A&A 620, A84 (2018) Astronomy https://doi.org/10.1051/0004-6361/201833981 & © ESO 2018 Astrophysics Planetary nebula IC 5148 and its ionized halo? D. Barría1, S. Kimeswenger1,2, W. Kausch2, and D. S. Goldman3 1 Instituto de Astronomía, Universidad Católica del Norte, Av. Angamos 0610, Antofagasta, Chile e-mail: [email protected] 2 Institut für Astro- und Teilchenphysik, Leopold–Franzens Universität Innsbruck, Technikerstr. 25, 6020 Innsbruck, Austria 3 Astrodon Imaging, 407 Tyrolean Court. Roseville, California, 95661, USA Received 29 July 2018 / Accepted 2 October 2018 ABSTRACT Context. Many round or roundish planetary nebulae (PNe) show multiple shells and halo structures during their evolutionary stage near the maximum temperature of their central star. Controversial debate is ongoing if these structures are recombination halos, as suggested by hydrodynamic modeling efforts, or ionized material. Recently, we discovered a halo with somewhat unusual structures around the sparsely studied PN IC 5148 and present for the first time spectroscopy going out to the halo of such a PN. Aims. We investigate the spatial distribution of material and its ionization state from the center of the nebula up to the very outskirts of the halo. Methods. We obtained long-slit low resolution spectroscopy (FORS2 at VLT) of the nebula in two position angles, which we used to investigate the nebular structure and its halo in the optical range from 450 to 880 nm. In addition we used medium resolution spectra taken with X-shooter at VLT ranging from 320 nm to 2.4 µm to derive atmospheric parameters for the central star. We obtained the distance and position in the Galaxy from various methods combined with Gaia DR2 data. -
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. -
Radar Images Provide Details on Halloween Asteroid 4 November 2015
Radar images provide details on Halloween asteroid 4 November 2015 California, to transmit high-power microwaves toward the asteroid. The signal bounced off the asteroid, and its radar echoes were received by the National Radio Astronomy Observatory's (NRAO) 100-meter (330-foot) Green Bank Telescope in West Virginia. The radar images achieve a spatial resolution as fine as 13 feet (4 meters) per pixel. The radar images were taken as the asteroid flew past Earth on October 31 at 1 p.m. EDT at about 1.3 lunar distances (300,000 miles, or 480,000 kilometers) from Earth. Asteroid 2015 TB145 is spherical in shape and approximately 2,000 feet (600 meters) in diameter. "The radar images of asteroid 2015 TB145 show Asteroid 2015 TB145 is depicted in eight individual radar portions of the surface not seen previously and images collected on Oct. 31, 2015 between 5:55 a.m. PDT (8:55 a.m. EDT) and 6:08 a.m. PDT (9:08 a.m. reveal pronounced concavities, bright spots that EDT). At the time the radar images were taken, the might be boulders, and other complex features that asteroid was between 440,000 miles (710,000 could be ridges," said Lance Benner of NASA's Jet kilometers) and about 430,000 miles (690,000 Propulsion Laboratory in Pasadena, California, who kilometers) distant. Asteroid 2015 TB145 safely flew past leads NASA's asteroid radar research program. Earth on Oct. 31, at 10:00 a.m. PDT (1 p.m. EDT) at "The images look distinctly different from the about 1.3 lunar distances (300,000 miles, 480,000 Arecibo radar images obtained on October 30 and kilometers). -
Professor Catriona Macleod
RRR | Cover 2015 v2 11/9/16 10:17 AM Page 1 C M Y CM MY CY CMY K Composite RRR 2015 | Features 11/12/16 1:36 PM Page 1 C M Y CM MY CY CMY K RHODES UNIVERSITY RESEARCH REPORT A publication of the Rhodes University Research Office, compiled and edited by Tarryn Gillitt, Busi Goba, Patricia Jacob, Jill Macgregor and Jaine Roberts Design & Layout: Sally Dore Research Office Director: Jaine Roberts [email protected] Tel: +27 (46) 603 8756/7572 www.ru.ac.za Cover: Rhodes University researchers Pam Maseko, Nomalanga Mkhize, Heila Lotz-Sisitka, Ruth Simbao, Anthea Garman and Catriona Macleod Cover Photos: Paul Greenway/www.3pphotography.com RESEARCH REPORT 2015 Composite RRR 2015 | Features 11/12/16 1:36 PM Page 2 C M Y CM MY CY CMY K CONTENTS 01 FOREWORD Dr Sizwe Mabizela, Vice-Chancellor 03 INTRODUCTION Dr Peter Clayton, Deputy Vice-Chancellor: Research & Development 05 TOP 30 RESEARCHERS 06 PHD GRADUATES 11 VICE-CHANCELLOR’S BOOK AWARD Professor Anthea Garman 13 VICE-CHANCELLOR’S DISTINGUISHED SENIOR RESEARCH AWARD Professor Catriona Macleod 15 VICE-CHANCELLOR’S DISTINGUISHED RESEARCH AWARD Dr Adrienne Edkins 17 SARChI CHAIRS Professor Heila Lotz-Sisitka, Professor Ruth Simbao and Dr Adrienne Edkins 23 AFRICAN LANGUAGES, SCHOOL OF LANGUAGES AND LITERATURE Associate Professor Pamela Maseko 25 DEPARTMENT OF HISTORY Dr Nomalanga Mkhize RESEARCH REPORT 2015 Composite RRR 2015 | Features 11/12/16 1:34 PM Page 3 C M Y CM MY CY CMY K RHODES RESEARCH 2015 RESEARCH REPORT DEPARTMENT PUBLICATIONS AFFILIATES, INSTITUTES AND 28 Publications from the Vice-Chancellorate -
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. -
407 a Abell Galaxy Cluster S 373 (AGC S 373) , 351–353 Achromat
Index A Barnard 72 , 210–211 Abell Galaxy Cluster S 373 (AGC S 373) , Barnard, E.E. , 5, 389 351–353 Barnard’s loop , 5–8 Achromat , 365 Barred-ring spiral galaxy , 235 Adaptive optics (AO) , 377, 378 Barred spiral galaxy , 146, 263, 295, 345, 354 AGC S 373. See Abell Galaxy Cluster Bean Nebulae , 303–305 S 373 (AGC S 373) Bernes 145 , 132, 138, 139 Alnitak , 11 Bernes 157 , 224–226 Alpha Centauri , 129, 151 Beta Centauri , 134, 156 Angular diameter , 364 Beta Chamaeleontis , 269, 275 Antares , 129, 169, 195, 230 Beta Crucis , 137 Anteater Nebula , 184, 222–226 Beta Orionis , 18 Antennae galaxies , 114–115 Bias frames , 393, 398 Antlia , 104, 108, 116 Binning , 391, 392, 398, 404 Apochromat , 365 Black Arrow Cluster , 73, 93, 94 Apus , 240, 248 Blue Straggler Cluster , 169, 170 Aquarius , 339, 342 Bok, B. , 151 Ara , 163, 169, 181, 230 Bok Globules , 98, 216, 269 Arcminutes (arcmins) , 288, 383, 384 Box Nebula , 132, 147, 149 Arcseconds (arcsecs) , 364, 370, 371, 397 Bug Nebula , 184, 190, 192 Arditti, D. , 382 Butterfl y Cluster , 184, 204–205 Arp 245 , 105–106 Bypass (VSNR) , 34, 38, 42–44 AstroArt , 396, 406 Autoguider , 370, 371, 376, 377, 388, 389, 396 Autoguiding , 370, 376–378, 380, 388, 389 C Caldwell Catalogue , 241 Calibration frames , 392–394, 396, B 398–399 B 257 , 198 Camera cool down , 386–387 Barnard 33 , 11–14 Campbell, C.T. , 151 Barnard 47 , 195–197 Canes Venatici , 357 Barnard 51 , 195–197 Canis Major , 4, 17, 21 S. Chadwick and I. Cooper, Imaging the Southern Sky: An Amateur Astronomer’s Guide, 407 Patrick Moore’s Practical -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
Probing the Physics of Narrow Line Regions in Active Galaxies II: the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7)
Probing the Physics of Narrow Line Regions in Active Galaxies II: The Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) Michael A. Dopita1,2, Prajval Shastri3, Rebecca Davies1, Lisa Kewley1,4, Elise Hampton1, Julia Scharw¨achter5, Ralph Sutherland1, Preeti Kharb3, Jessy Jose3, Harish Bhatt3, S. Ramya 3, Chichuan Jin6, Julie Banfield7, Ingyin Zaw8, St´ephanie Juneau9, Bethan James10 & Shweta Srivastava11 [email protected] ABSTRACT Here we describe the Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7) and present results on 64 galaxies drawn from the first data release. The S7 uses the Wide Field Spectrograph (WiFeS) mounted on the ANU 2.3m telescope located at the Siding Spring Observatory to deliver an integral field of 38×25 arcsec at a spectral resolution of R = 7000 in the red (530−710nm), and R = 3000 in the blue (340 − 560nm). From these data cubes we have extracted the Narrow Line Region (NLR) spectra from a 4 arc sec aperture centred on the nucleus. We also determine the Hβ and [O III] λ5007 fluxes in the narrow lines, the nuclear reddening, the reddening-corrected relative intensities of the observed emission lines, and the Hβ and [O III] λ5007 luminosities determined 1RSAA, Australian National University, Cotter Road, Weston Creek, ACT 2611, Australia 2Astronomy Department, King Abdulaziz University, P.O. Box 80203, Jeddah, Saudi Arabia 3Indian Institute of Astrophysics, Koramangala 2B Block, Bangalore 560034, India 4Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI, USA 5LERMA, Observatoire de Paris, CNRS, UMR 8112, 61 Avenue de l’Observatoire, 75014, Paris, France 6Qian Xuesen Laboratory for Space Technology, Beijing, China 7CSIRO Astronomy & Space Science, P.O. -
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A&A 598, A63 (2017) Astronomy DOI: 10.1051/0004-6361/201629584 & c ESO 2017 Astrophysics Large Halloween asteroid at lunar distance?,?? T. G. Müller1, A. Marciniak2, M. Butkiewicz-B˛ak2, R. Duffard3, D. Oszkiewicz2, H. U. Käufl4, R. Szakáts5, T. Santana-Ros2, C. Kiss5, and P. Santos-Sanz3 1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Giessenbachstraße, 85741 Garching, Germany e-mail: [email protected] 2 Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Słoneczna 36, 60-286 Poznan,´ Poland 3 Instituto de Astrofísica de Andalucía (CSIC) C/ Camino Bajo de Huétor, 50, 18008 Granada, Spain 4 ESO, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 5 Konkoly Observatory, Research Center for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly Thege 15-17, 1121 Budapest, Hungary Received 25 August 2016 / Accepted 20 October 2016 ABSTRACT The near-Earth asteroid (NEA) 2015 TB145 had a very close encounter with Earth at 1.3 lunar distances on October 31, 2015. We obtained 3-band mid-infrared observations of this asteroid with the ESO VLT-VISIR instrument covering approximately four hours in total. We also monitored the visual lightcurve during the close-encounter phase. The NEA has a (most likely) rotation period of 2:939 ± 0:005 h and the visual lightcurve shows a peak-to-peak amplitude of approximately 0:12 ± 0:02 mag. A second rotation period of 4:779 ± 0:012 h, with an amplitude of the Fourier fit of 0:10 ± 0:02 mag, also seems compatible with the available lightcurve measurements. We estimate a V − R colour of 0:56 ± 0:05 mag from different entries in the MPC database. -
Integral Field Unit Spectroscopy of 10 Early Type Galactic Nuclei: I-Principal
Mon. Not. R. Astron. Soc. 000, 1–?? (2002) Printed 10 October 2018 (MN LaTEX style file v2.2) Integral field unit spectroscopy of 10 early type galactic nuclei: I - Principal component analysis Tomography and nuclear activity T.V. Ricci,1? J.E. Steiner,1 R.B. Menezes1 1Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, 05508-900, São Paulo, Brazil Released 2002 Xxxxx XX ABSTRACT Most massive galaxies show emission lines that can be characterized as LINERs. To what extent this emission is related to AGNs or to stellar processes is still an open question. In this paper, we analysed a sample of such galaxies to study the central re- gion in terms of nuclear and circumnuclear emission lines, as well as the stellar compo- nent properties. For this reason, we selected 10 massive (σ >200 km s−1) nearby (d < 31 Mpc) galaxies and observed them with the IFU/GMOS (integral field unit/Gemini Multi-Object Spectrograph) spectrograph on the Gemini South Telescope. The data were analysed with principal component analysis (PCA) Tomography to assess the main properties of the objects. Two spectral regions were analysed: a yellow region (5100-5800 Å), adequate to show the properties of the stellar component, and a red region (6250-6800 Å), adequate to analyse the gaseous component. We found that all objects previously known to present emission lines have a central AGN-type emitting source. They also show gaseous and stellar kinematics typical of discs. Such discs may be co-aligned (NGC 1380 and ESO 208 G-21), in counter-rotation (IC 1459 and NGC 7097) or misaligned (IC 5181 and NGC 4546).