A Radio and Infrared Investigation of Seyfert Galaxies in the Local Universe
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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. -
Arxiv:1705.04776V1 [Astro-Ph.HE] 13 May 2017 Aaua M
White Paper on East Asian Vision for mm/submm VLBI: Toward Black Hole Astrophysics down to Angular Resolution of 1 RS Editors Asada, K.1, Kino, M.2,3, Honma, M.3, Hirota, T.3, Lu, R.-S.4,5, Inoue, M.1, Sohn, B.-W.2,6, Shen, Z.-Q.4, and Ho, P. T. P.1,7 Authors Akiyama, K.3,8, Algaba, J-C.2, An, T.4, Bower, G.1, Byun, D-Y.2, Dodson, R.9, Doi, A.10, Edwards, P.G.11, Fujisawa, K.12, Gu, M-F.4, Hada, K.3, Hagiwara, Y.13, Jaroenjittichai, P.15, Jung, T.2,6, Kawashima, T.3, Koyama, S.1,5, Lee, S-S.2, Matsushita, S.1, Nagai, H.3, Nakamura, M.1, Niinuma, K.12, Phillips, C.11, Park, J-H.15, Pu, H-Y.1, Ro, H-W.2,6, Stevens, J.11, Trippe, S.15, Wajima, K.2, Zhao, G-Y.2 1 Institute of Astronomy and Astrophysics, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan 2 Korea Astronomy and Space Science Institute, Daedukudae-ro 776, Yuseong-gu, Daejeon 34055, Republic of Korea 3 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan 4 Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China 5 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, D-53121 Bonn, Germany 6 University of Science and Technology, 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea 7 East Asian Observatory, 660 N. -
The Bright Galaxies NGC 1068 (M 77), NGC 2146, NGC 3079, NGC 4826 (M 64), and NGC 7469 F
A&A 493, 525–538 (2009) Astronomy DOI: 10.1051/0004-6361:200810655 & c ESO 2009 Astrophysics CI and CO in nearby galaxy centers The bright galaxies NGC 1068 (M 77), NGC 2146, NGC 3079, NGC 4826 (M 64), and NGC 7469 F. P. Israel Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands e-mail: [email protected] Received 22 July 2008 / Accepted 5 November 2008 ABSTRACT Aims. We study the physical properties and amount of molecular gas in the central regions of galaxies with active nuclei. Methods. Maps and measurements of the J = 1−0, J = 2−1, J = 3−2, J = 4−3 12CO, the J = 1−0, J = 2−1, and J = 3−2 13CO lines in the central arcminute squared of NGC 1068, NGC 2146, NGC 3079, NGC 4826, and NGC 7469, as well as 492 GHz CI maps in three of these are used to model the molecular gas clouds in these galaxies. Results. Bright CO concentrations were detected and mapped in all five objects. In all cases, the observed lines could be fitted with two distinct gas components. The physical condition of the molecular gas is found to differ from galaxy to galaxy. Rather high kinetic temperatures of 125−150 K occur in NGC 2146 and NGC 3079. Very high densities of 0.3−1.0 × 105 cm−3 occur in NGC 2146, NGC 3079, and NGC 7469. The CO to H2 conversion factor X is typically an order of magnitude less than the “standard” value in the solar neighborhood. -
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. -
A Basic Requirement for Studying the Heavens Is Determining Where In
Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short). -
Resolving the Nuclear Obscuring Disk in the Compton-Thick Seyfert Galaxy Ngc 5643 with Alma
Draft version May 11, 2018 Typeset using LATEX twocolumn style in AASTeX61 RESOLVING THE NUCLEAR OBSCURING DISK IN THE COMPTON-THICK SEYFERT GALAXY NGC 5643 WITH ALMA A. Alonso-Herrero,1, 2 M. Pereira-Santaella,2 S. Garc´ıa-Burillo,3 R. I. Davies,4 F. Combes,5 D. Asmus,6, 7 A. Bunker,2 T. D´ıaz-Santos,8 P. Gandhi,7 O. Gonzalez-Mart´ ´ın,9 A. Hernan-Caballero,´ 10 E. Hicks,11 S. Honig,¨ 7 A. Labiano,12 N. A. Levenson,13 C. Packham,14 C. Ramos Almeida,15, 16 C. Ricci,17, 18, 19 D. Rigopoulou,2 D. Rosario,20 E. Sani,6 and M. J. Ward20 1Centro de Astrobiolog´ıa(CAB, CSIC-INTA), ESAC Campus, E-28692 Villanueva de la Ca~nada,Madrid, Spain 2Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, United Kingdom 3Observatorio de Madrid, OAN-IGN, Alfonso XII, 3, E-28014 Madrid, Spain 4Max Planck Institut fuer extraterrestrische Physik Postfach 1312, 85741 Garching bei Muenchen, Germany 5LERMA, Obs. de Paris, PSL Research Univ., Coll´egede France, CNRS, Sorbonne Univ., UPMC, Paris, France 6European Southern Observatory, Casilla 19001, Santiago 19, Chile 7Department of Physics & Astronomy, University of Southampton, Hampshire SO17 1BJ, Southampton, United Kingdom 8N´ucleo de Astronom´ıade la Facultad de Ingenier´ıa,Universidad Diego Portales, Av. Ej´ercito Libertador 441, Santiago, Chile 9Instituto de Radioastronom´ıay Astrof´ısica (IRyA-UNAM), 3-72 (Xangari), 8701, Morelia, Mexico 10Departamento de Astrof´ısica y CC. de la Atm´osfera, Facultad de CC. F´ısicas, Universidad Complutense de Madrid, E-28040 Madrid, Spain 11Department -
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 -
ESO Annual Report 2004 ESO Annual Report 2004 Presented to the Council by the Director General Dr
ESO Annual Report 2004 ESO Annual Report 2004 presented to the Council by the Director General Dr. Catherine Cesarsky View of La Silla from the 3.6-m telescope. ESO is the foremost intergovernmental European Science and Technology organi- sation in the field of ground-based as- trophysics. It is supported by eleven coun- tries: Belgium, Denmark, France, Finland, Germany, Italy, the Netherlands, Portugal, Sweden, Switzerland and the United Kingdom. Created in 1962, ESO provides state-of- the-art research facilities to European astronomers and astrophysicists. In pur- suit of this task, ESO’s activities cover a wide spectrum including the design and construction of world-class ground-based observational facilities for the member- state scientists, large telescope projects, design of innovative scientific instruments, developing new and advanced techno- logies, furthering European co-operation and carrying out European educational programmes. ESO operates at three sites in the Ataca- ma desert region of Chile. The first site The VLT is a most unusual telescope, is at La Silla, a mountain 600 km north of based on the latest technology. It is not Santiago de Chile, at 2 400 m altitude. just one, but an array of 4 telescopes, It is equipped with several optical tele- each with a main mirror of 8.2-m diame- scopes with mirror diameters of up to ter. With one such telescope, images 3.6-metres. The 3.5-m New Technology of celestial objects as faint as magnitude Telescope (NTT) was the first in the 30 have been obtained in a one-hour ex- world to have a computer-controlled main posure. -
Outflows in the Seyfert 2 Galaxy NGC 5643 Traced By
Publications of the Astronomical Society of Australia (2018), 35, e040, 8 pages doi:10.1017/pasa.2018.31 Research Paper Outflows in the Seyfert 2 galaxy NGC 5643 traced by the [S III] emission Rogemar A. Riffel1,C.Hekatelyne1 and Izabel C. Freitas1,2 1Departamento de Física, CCNE, Universidade Federal de Santa Maria, Santa Maria, 97105-900 RS, Brazil and 2Colégio Politécnico, Universidade Federal de Santa Maria, Santa Maria, 97105-900 RS, Brazil Abstract We use Gemini Multi-Object Spectrograph Integral Field Unit observations of the inner 285 × 400 pc2 region of the Seyfert 2 galaxy NGC 5643 to map the [S III]λ9069 emission line flux distribution and kinematics, as well as the stellar kinematics, derived by fitting the Ca IIλλλ8498,8542,8662 triplet, at a spatial resolution of 45 pc. The stellar velocity field shows regular rotation, with a projected velocity of − ◦ − 100 km s 1 and kinematic major axis along a position angle of –36 . A ring of low stellar velocity dispersion values (∼70 km s 1), attributed to young/intermediate age stellar populations, is seen surrounding the nucleus with a radius of 50 pc. We found that the [S III] flux distribu- tion shows an elongated structure along the east–west direction and its kinematics is dominated by outflows within a bi-cone at an ionised − gas outflow rate of 0.3 M yr 1. In addition, velocity slices across the [S III]λ9069 emission line reveal a kinematic component attributed to rotation of gas in the plane of the galaxy. Keywords: galaxies: active – galaxies: individual (NGC 5643) – galaxies: kinematics – galaxies: Seyfert (Received April 10, 2018; revised 7 July 2018; accepted August 16, 2018) 1. -
SPIRIT Target Lists
JANUARY and FEBRUARY deep sky objects JANUARY FEBRUARY OBJECT RA (2000) DECL (2000) OBJECT RA (2000) DECL (2000) Category 1 (west of meridian) Category 1 (west of meridian) NGC 1532 04h 12m 04s -32° 52' 23" NGC 1792 05h 05m 14s -37° 58' 47" NGC 1566 04h 20m 00s -54° 56' 18" NGC 1532 04h 12m 04s -32° 52' 23" NGC 1546 04h 14m 37s -56° 03' 37" NGC 1672 04h 45m 43s -59° 14' 52" NGC 1313 03h 18m 16s -66° 29' 43" NGC 1313 03h 18m 15s -66° 29' 51" NGC 1365 03h 33m 37s -36° 08' 27" NGC 1566 04h 20m 01s -54° 56' 14" NGC 1097 02h 46m 19s -30° 16' 32" NGC 1546 04h 14m 37s -56° 03' 37" NGC 1232 03h 09m 45s -20° 34' 45" NGC 1433 03h 42m 01s -47° 13' 19" NGC 1068 02h 42m 40s -00° 00' 48" NGC 1792 05h 05m 14s -37° 58' 47" NGC 300 00h 54m 54s -37° 40' 57" NGC 2217 06h 21m 40s -27° 14' 03" Category 1 (east of meridian) Category 1 (east of meridian) NGC 1637 04h 41m 28s -02° 51' 28" NGC 2442 07h 36m 24s -69° 31' 50" NGC 1808 05h 07m 42s -37° 30' 48" NGC 2280 06h 44m 49s -27° 38' 20" NGC 1792 05h 05m 14s -37° 58' 47" NGC 2292 06h 47m 39s -26° 44' 47" NGC 1617 04h 31m 40s -54° 36' 07" NGC 2325 07h 02m 40s -28° 41' 52" NGC 1672 04h 45m 43s -59° 14' 52" NGC 3059 09h 50m 08s -73° 55' 17" NGC 1964 05h 33m 22s -21° 56' 43" NGC 2559 08h 17m 06s -27° 27' 25" NGC 2196 06h 12m 10s -21° 48' 22" NGC 2566 08h 18m 46s -25° 30' 02" NGC 2217 06h 21m 40s -27° 14' 03" NGC 2613 08h 33m 23s -22° 58' 22" NGC 2442 07h 36m 20s -69° 31' 29" Category 2 Category 2 M 42 05h 35m 17s -05° 23' 25" M 42 05h 35m 17s -05° 23' 25" NGC 2070 05h 38m 38s -69° 05' 39" NGC 2070 05h 38m 38s -69°