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Black Holes in 4 Nearby Radio Galaxies
Astrophys Space Sci (2015) 356:347–351 DOI 10.1007/s10509-014-2166-6 ORIGINAL ARTICLE Black holes in 4 nearby radio galaxies Jeremy Mould · Tony Readhead · Garret Cotter · David Batt · Mark Durré Received: 26 June 2014 / Accepted: 18 October 2014 / Published online: 4 March 2015 © Springer Science+Business Media Dordrecht 2014 Abstract We study the velocity dispersion profiles of the NGC 1326 is a ring barred S0 galaxy in the Fornax clus- nuclei of NGC 1326, 2685, 5273 and 5838 in the CO first ter with circumnuclear star formation (Buta et al. 2000). Our overtone band. There is evidence for a black hole (BH) in second galaxy is a Hubble Atlas polar ring galaxy, an S0 NGC 1326 and 5838. Gas is seen flowing out of the nuclear Seyfert 2. Schinnerer and Scoville (2002) detected four giant region of NGC 5273. We put upper limits on the nuclear molecular cloud associations within the polar ring in NGC BHs responsible for its activity and that of NGC 2685. 2685 (the Helix) with of order 107 M of molecular hy- drogen. Dust has been detected with Spitzer in our third S0 Keywords Infrared: general · Active galactic nuclei · galaxy, NGC 5273, totaling 2.5 × 105 M by Martini et al. Galaxies: elliptical · Radiosources · Black holes (2013). NGC5838 has a nuclear star cluster of 5 × 107 M (Scott and Graham 2013). 1 Introduction 2 Sample and observations Understanding activity in galactic nuclei requires high spa- tial resolution. Kormendy and Richstone (1995) have out- We have drawn our radiogalaxy sample from Brown et al. -
Fourier Dissection of Early-Type Galaxy Bars R
The Astronomical Journal, 132:1859Y1876, 2006 November # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. FOURIER DISSECTION OF EARLY-TYPE GALAXY BARS R. Buta,1 E. Laurikainen,2 H. Salo,2 D. L. Block,3 and J. H. Knapen4 Received 2006 May 4; accepted 2006 July 14 ABSTRACT This paper reports on a near-infrared survey of early-type galaxies designed to provide information on bar strengths, bulges, disks, and bar parameters in a statistically well-defined sample of S0YSa galaxies. Early-type galaxies have the advantage that their bars are relatively free of the effects of dust, star formation, and spiral structure that com- plicate bar studies in later type galaxies. We describe the survey and present results on a detailed analysis of the rela- tive Fourier intensity amplitudes of bars in 26 early-type galaxies. We also evaluate the ‘‘symmetry assumption’’ of these amplitudes with radius, used recently for bar-spiral separation in later type galaxies. The results show a wide variety of radial Fourier profiles of bars, ranging from simple symmetric profiles that can be represented in terms of a single Gaussian component to both symmetric and asymmetric profiles that can be represented by two overlapping Gaussian components. More complicated profiles than these are also found, often due to multiple barlike features including extended ovals or lenses. Based on the gravitational bar torque indicator Qb, double-Gaussian bars are stronger on average than single-Gaussian bars, at least for our small sample. We show that published numerical simulations in which the bar transfers a large amount of angular momentum to the halo can account for many of the observed profiles. -
The Stellar Content of Active Galaxies
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Mon. Not. R. Astron. Soc. 000, 000–000 (1998) The Stellar Content of Active Galaxies Roberto Cid Fernandes Jr.1‡, Thaisa Storchi Bergmann2?‡ and Henrique R. Schmitt2†‡ 1 Departamento de F´ısica, CFM - UFSC, Campus Universit´ario - Trindade, Caixa Postal: 476. CEP: 88040-900 Florian´opolis, SC, Brazil. 2 Instituto de F´ısica - UFRGS, Caixa Postal: 15051. CEP: 91501-970 Porto Alegre, RS, Brazil. 31 January 1998 ABSTRACT We present the results of a long-slit spectroscopic study of 39 active and 3 normal galaxies. Stellar absorption features, continuum colors and their radial variations are analyzed in an effort to characterize the stellar population in these galaxies and detect the presence of a featureless continuum underlying the starlight spectral component. Spatial variations of the equivalent widths of conspicuous absorption lines and contin- uum colors are detected in most galaxies. Star-forming rings, in particular, leave clear fingerprints in the equivalent widths and color profiles. We find that the stellar popu- lations in the inner regions of active galaxies present a variety of characteristics, and cannot be represented by a single starlight template. Dilution of the stellar lines by an underlying featureless continuum is detected in most broad-lined objects, but little or no dilution is found for the most of the 20 type 2 Seyferts in the sample. Color gradients are also ubiquitous. In particular, all but one of the observed Seyfert 2s are redder at the nucleus than in its immediate vicinity. -
TYPHOON Observations of NGC 1365, NGC 1068, and The
MNRAS 479, 4907–4935 (2018) doi:10.1093/mnras/sty1676 Advance Access publication 2018 June 26 Starburst–AGN mixing: TYPHOON observations of NGC 1365, NGC 1068, and the effect of spatial resolution on the AGN fraction Downloaded from https://academic.oup.com/mnras/article-abstract/479/4/4907/5045261 by Da-Collect Chifley Library ANUC user on 17 December 2018 Joshua J. D’Agostino,1,2‹ Henry Poetrodjojo,1,2 I-Ting Ho,3 Brent Groves,1,2 Lisa Kewley,1,2 Barry F. Madore,4 Jeff Rich4 and Mark Seibert4 1Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston ACT 2611, Australia 2ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) 3Max Planck Institute for Astronomy, Konigstuhl¨ 17, D-69117 Heidelberg, Germany 4Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St, Pasadena, CA 91101, USA Accepted 2018 June 22. Received 2018 June 22; in original form 2018 April 16 ABSTRACT We demonstrate a robust method of resolving the star formation and AGN contributions to emission lines using two very well known AGN systems: NGC 1365 and NGC 1068, using the high spatial resolution data from the TYPHOON/PrISM survey. We expand the previous method of calculating the AGN fraction by using theoretical-based model grids rather than empirical points. The high spatial resolution of the TYPHOON/PrISM observations shows evidence of both star formation and AGN activity occurring in the nuclei of the two galaxies. We rebin the data to the lower resolutions, typically found in other integral field spectroscopy surveys such as SAMI, MaNGA, and CALIFA. -
The 2.2 M Telescope Is Ready
blue central colour to have a redder halo, while those systems to three orders of magnitude compared to the preliminary with a relatively red central colour (ellipticals and SOs) seem to results for the Fornax cluster. By then we will have acquired an have a bluer halo colour. unprecedented set of properties of Southern Hemisphere At the bollom of the flow chart in Fig. 1 we have indicated the galaxies. The size of the sampie and the uniform approach as Possible presentation of the acquired data bases. Eventually attempted in this project should allow us to study the universe in Our final data base of 16,000 galaxies will be expanded by two an unbiased way. The 2.2 mTelescope is Ready M. Tarenghi, ESO The 2.2 m Zeiss telescope is the last telescope to have The erection of the telescope began on February 15, 1983, arrived on La Silla, thanks to a 25-year loan to ESO from the and as a result of a collaboration of qualified personnel from Max-Planck-Gesellschaft (MPG) who will receive for their Zeiss and MAN and the services of many ESO technicians, we contribution 25 % of the observing time. ESO assumed respon succeeded in obtaining the "first light" on the night of June 22, sibility for the installation of the telescope, the arrangement of 1983. Ouring the following weeks the telescope was used for necessary modifications, and construction of the building and optical, mechanical and electronic tuning. The end of the bad dome according to specifications agreed with the MPG. ESO winter weather made it possible to start using the telescope will also assume responsibility for the maintenance and opera with the photographic camera, the B & C spectrograph plus tion of the telescope. -
Monster Image of the Fornax Galaxy Cluster 25 October 2017
Monster image of the Fornax Galaxy Cluster 25 October 2017 telescope technology to observe the finer details of NGC 1316's unusual structure through a combination of imaging and modelling. The mergers that formed NGC 1316 led to an influx of gas, which fuels an exotic astrophysical object at its centre: a supermassive black hole with a mass roughly 150 million times that of the Sun. As it accretes mass from its surroundings, this cosmic monster produces immensely powerful jets of high- energy particles , that in turn give rise to the Credit: ESO characteristic lobes of emission seen at radio wavelengths, making NGC 1316 the fourth- brightest radio source in the sky. Countless galaxies vie for attention in this monster NGC 1316 has also been host to four recorded type image of the Fornax Galaxy Cluster, some Ia supernovae, which are vitally important appearing only as pinpricks of light while others astrophysical events for astronomers. Since type Ia dominate the foreground. One of these is the supernovae have a very clearly defined brightness, lenticular galaxy NGC 1316. The turbulent past of they can be used to measure the distance to the this much-studied galaxy has left it with a delicate host galaxy; in this case, 60 million light-years. structure of loops, arcs and rings that astronomers These "standard candles" are much sought-after by have now imaged in greater detail than ever before astronomers, as they are an excellent tool to with the VLT Survey Telescope. This astonishingly reliably measure the distance to remote objects. In deep image also reveals a myriad of dim objects fact, they played a key role in the groundbreaking along with faint intracluster light. -
Arxiv:1603.06895V2 [Astro-Ph.GA] 10 May 2016 Cno Ta.19)I
A Selection of Giant Radio Sources from NVSS D. D. Proctor Visiting Scientist, Lawrence Livermore National Laboratory, L-405, 7000 East Avenue, Livermore, CA, 94550; [email protected] ABSTRACT Results of the application of pattern recognition techniques to the problem of identifying Giant Radio Sources (GRS) from the data in the NVSS catalog are presented and issues affecting the process are explored. Decision-tree pat- tern recognition software was applied to training set source pairs developed from known NVSS large angular size radio galaxies. The full training set consisted of 51,195 source pairs, 48 of which were known GRS for which each lobe was primarily represented by a single catalog component. The source pairs had a maximum separation of 20′ and a minimum component area of 1.87 square arc minutes at the 1.4 mJy level. The importance of comparing resulting probabil- ity distributions of the training and application sets for cases of unknown class ratio is demonstrated. The probability of correctly ranking a randomly selected (GRS, non-GRS) pair from the best of the tested classifiers was determined to be 97.8+1.5%. The best classifiers were applied to the over 870,000 candidate pairs from the entire catalog. Images of higher ranked sources were visually screened and a table of over sixteen hundred candidates, including morphological annota- tion, is presented. These systems include doubles and triples, Wide-Angle Tail (WAT) and Narrow-Angle Tail (NAT), S- or Z-shaped systems, and core-jets and resolved cores. While some resolved lobe systems are recovered with this technique, generally it is expected that such systems would require a different approach. -
Astrophysics in 2006 3
ASTROPHYSICS IN 2006 Virginia Trimble1, Markus J. Aschwanden2, and Carl J. Hansen3 1 Department of Physics and Astronomy, University of California, Irvine, CA 92697-4575, Las Cumbres Observatory, Santa Barbara, CA: ([email protected]) 2 Lockheed Martin Advanced Technology Center, Solar and Astrophysics Laboratory, Organization ADBS, Building 252, 3251 Hanover Street, Palo Alto, CA 94304: ([email protected]) 3 JILA, Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder CO 80309: ([email protected]) Received ... : accepted ... Abstract. The fastest pulsar and the slowest nova; the oldest galaxies and the youngest stars; the weirdest life forms and the commonest dwarfs; the highest energy particles and the lowest energy photons. These were some of the extremes of Astrophysics 2006. We attempt also to bring you updates on things of which there is currently only one (habitable planets, the Sun, and the universe) and others of which there are always many, like meteors and molecules, black holes and binaries. Keywords: cosmology: general, galaxies: general, ISM: general, stars: general, Sun: gen- eral, planets and satellites: general, astrobiology CONTENTS 1. Introduction 6 1.1 Up 6 1.2 Down 9 1.3 Around 10 2. Solar Physics 12 2.1 The solar interior 12 2.1.1 From neutrinos to neutralinos 12 2.1.2 Global helioseismology 12 2.1.3 Local helioseismology 12 2.1.4 Tachocline structure 13 arXiv:0705.1730v1 [astro-ph] 11 May 2007 2.1.5 Dynamo models 14 2.2 Photosphere 15 2.2.1 Solar radius and rotation 15 2.2.2 Distribution of magnetic fields 15 2.2.3 Magnetic flux emergence rate 15 2.2.4 Photospheric motion of magnetic fields 16 2.2.5 Faculae production 16 2.2.6 The photospheric boundary of magnetic fields 17 2.2.7 Flare prediction from photospheric fields 17 c 2008 Springer Science + Business Media. -
New Type of Black Hole Detected in Massive Collision That Sent Gravitational Waves with a 'Bang'
New type of black hole detected in massive collision that sent gravitational waves with a 'bang' By Ashley Strickland, CNN Updated 1200 GMT (2000 HKT) September 2, 2020 <img alt="Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image." class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190516104725-ngc-4485-nasa-super-169.jpg"> Photos: Wonders of the universe Galaxy NGC 4485 collided with its larger galactic neighbor NGC 4490 millions of years ago, leading to the creation of new stars seen in the right side of the image. Hide Caption 98 of 195 <img alt="Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. " class="media__image" src="//cdn.cnn.com/cnnnext/dam/assets/190502151952-0502-wonders-of-the-universe-super-169.jpg"> Photos: Wonders of the universe Astronomers developed a mosaic of the distant universe, called the Hubble Legacy Field, that documents 16 years of observations from the Hubble Space Telescope. The image contains 200,000 galaxies that stretch back through 13.3 billion years of time to just 500 million years after the Big Bang. Hide Caption 99 of 195 <img alt="A ground-based telescope&amp;#39;s view of the Large Magellanic Cloud, a neighboring galaxy of our Milky Way. -
The Distance to NGC 1316 \(Fornax
A&A 552, A106 (2013) Astronomy DOI: 10.1051/0004-6361/201220756 & c ESO 2013 Astrophysics The distance to NGC 1316 (Fornax A): yet another curious case,, M. Cantiello1,A.Grado2, J. P. Blakeslee3, G. Raimondo1,G.DiRico1,L.Limatola2, E. Brocato1,4, M. Della Valle2,6, and R. Gilmozzi5 1 INAF, Osservatorio Astronomico di Teramo, via M. Maggini snc, 64100 Teramo, Italy e-mail: [email protected] 2 INAF, Osservatorio Astronomico di Capodimonte, salita Moiariello, 80131 Napoli, Italy 3 Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, Victoria BC V82 3H3, Canada 4 INAF, Osservatorio Astronomico di Roma, via Frascati 33, Monte Porzio Catone, 00040 Roma, Italy 5 European Southern Observatory, Karl–Schwarzschild–Str. 2, 85748 Garching bei München, Germany 6 International Centre for Relativistic Astrophysics, Piazzale della Repubblica 2, 65122 Pescara, Italy Received 16 November 2012 / Accepted 14 February 2013 ABSTRACT Aims. The distance of NGC 1316, the brightest galaxy in the Fornax cluster, provides an interesting test for the cosmological distance scale. First, because Fornax is the second largest cluster of galaxies within 25 Mpc after Virgo and, in contrast to Virgo, has a small line-of-sight depth; and second, because NGC 1316 is the single galaxy with the largest number of detected Type Ia supernovae (SNe Ia), giving the opportunity to test the consistency of SNe Ia distances both internally and against other distance indicators. Methods. We measure surface brightness fluctuations (SBF) in NGC 1316 from ground- and space-based imaging data. The sample provides a homogeneous set of measurements over a wide wavelength interval. -
Dissecting the Origin of the Submillimetre Emission in Nearby Galaxies with Herschel and LABOCA
MNRAS 439, 2542–2570 (2014) doi:10.1093/mnras/stu113 Advance Access publication 2014 February 17 Dissecting the origin of the submillimetre emission in nearby galaxies with Herschel and LABOCA M. Galametz,1,2‹ M. Albrecht,3 R. Kennicutt,1 G. Aniano,4 F. Bertoldi,3 D. Calzetti,5 K. V. Croxall,6 D. Dale,7 B. Draine,8 C. Engelbracht,9,10 K. Gordon,11 J. Hinz,9 Downloaded from https://academic.oup.com/mnras/article-abstract/439/3/2542/1092583 by Princeton University user on 02 May 2019 L. K. Hunt,12 A. Kirkpatrick,5 E. Murphy,13 H. Roussel,14 R. A. Skibba,15 F. Walter,16 A. Weiss17 andC.D.Wilson18 1Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK 2European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching-bei-Munchen,¨ Germany 3Argelander-Institut fur¨ Astronomie, Abteilung Radioastronomie, Auf dem Hugel¨ 71, D-53121 Bonn, Germany 4Institut d’Astrophysique Spatiale, Orsay 5Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA 6Department of Astronomy, The Ohio State University, 4051 McPherson Laboratory, 140 W 18th Ave., Columbus, OH 43210, USA 7Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82071, USA 8Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 9Steward Observatory, University of Arizona, Tucson, AZ 85721, USA 10Raytheon Company, 1151 East Hermans Road, Tucson, AZ 85756, USA 11Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 12INAF Osservatorio Astrofisico di Arcetri, -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93,