The Globular Cluster System of NGC1316. III. Kinematic Complexity ?
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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. -
115 Abell Galaxy Cluster # 373
WINTER Medium-scope challenges 271 # # 115 Abell Galaxy Cluster # 373 Target Type RA Dec. Constellation Magnitude Size Chart AGCS 373 Galaxy cluster 03 38.5 –35 27.0 Fornax – 180 ′ 5.22 Chart 5.22 Abell Galaxy Cluster (South) 373 272 Cosmic Challenge WINTER Nestled in the southeast corner of the dim early winter western suburbs. Deep photographs reveal that NGC constellation Fornax, adjacent to the distinctive triangle 1316 contains many dust clouds and is surrounded by a formed by 6th-magnitude Chi-1 ( 1), Chi-2 ( 2), and complex envelope of faint material, several loops of Chi-3 ( 3) Fornacis, is an attractive cluster of galaxies which appear to engulf a smaller galaxy, NGC 1317, 6 ′ known as Abell Galaxy Cluster – Southern Supplement to the north. Astronomers consider this to be a case of (AGCS) 373. In addition to his research that led to the galactic cannibalism, with the larger NGC 1316 discovery of more than 80 new planetary nebulae in the devouring its smaller companion. The merger is further 1950s, George Abell also examined the overall structure signaled by strong radio emissions being telegraphed of the universe. He did so by studying and cataloging from the scene. 2,712 galaxy clusters that had been captured on the In my 8-inch reflector, NGC 1316 appears as a then-new National Geographic Society–Palomar bright, slightly oval disk with a distinctly brighter Observatory Sky Survey taken with the 48-inch Samuel nucleus. NGC 1317, about 12th magnitude and 2 ′ Oschin Schmidt camera at Palomar Observatory. In across, is visible in a 6-inch scope, although averted 1958, he published the results of his study as a paper vision may be needed to pick it out. -
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. -
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, -
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 -
Arxiv:1703.07989V1 [Astro-Ph.GA] 23 Mar 2017 Accretion of Small Satellites
Draft version March 24, 2017 Typeset using LATEX twocolumn style in AASTeX61 THE FORNAX DEEP SURVEY WITH VST. II. FORNAX A: A TWO-PHASE ASSEMBLY CAUGHT ON ACT E. Iodice,1 M. Spavone,2 M. Capaccioli,3 R. F. Peletier,4 T. Richtler,5 M. Hilker,6 S. Mieske,7 L. Limatola, A. Grado, N.R. Napolitano,8 M. Cantiello,9 R. D'Abrusco,10 M. Paolillo,11 A. Venhola,12 T. Lisker,13 G. Van de Ven,14 J. Falcon-Barroso,15 and P. Schipani16 1INAF-Astronomical Observatory of Capodimonte, via Moiariello 16, Naples, I-80131, Italy 2Astronomical Observatory of Capodimonte, via Moiariello 16, Naples, I-80131, Italy 3University of Naples \Federico II", C.U. Monte SantAngelo, Via Cinthia, 80126, Naples, Italy 4Kapteyn Astronomical Institute, University of Groningen, PO Box 72, 9700 AV Groningen, The Netherlands 5Universidad de Concepci´on,Concepci´on,Chile 6European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei Munchen, Germany 7European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile 8INAF - Astronomical Observatory of Capodimonte, via Moiariello 16, Naples, I-80131, Italy 9INAF-Astronomical Observatory of Teramo, Via Maggini, 64100, Teramo, Italy 10Smithsonian Astrophysical Observatory/Chandra X-ray centre, 02138 Cambridge (MA), US 11Univ. of Naples \Federico II", C.U. Monte SantAngelo, Via Cinthia, 80126, Naples, Italy 12Division of Astronomy, Department of Physics, University of Oulu, Oulu, Finland 13Zentrum fuer Astronomie der Universitaet Heidelberg, Germany 14Max Planck Institute for Astronomy, Heidelberg, Germany 15Instituto de Astrof´ısica de Canarias, C/ Via L´actea s/n, 38200 La Laguna, Canary Islands, Spain 16Astron. Observatory of Capodimonte, via Moiariello 16, Naples, I-80131, Italy ABSTRACT As part of the Fornax Deep Survey with the ESO VLT Survey Telescope, we present new g and r bands mosaics of the SW group of the Fornax cluster. -
Astronomy Astrophysics
A&A 415, 123–143 (2004) Astronomy DOI: 10.1051/0004-6361:20031448 & c ESO 2004 Astrophysics VLT spectroscopy of globular cluster systems? I. The photometric and spectroscopic data set??;??? T. H. Puzia1, M. Kissler-Patig2, D. Thomas3, C. Maraston3,R.P.Saglia1, R. Bender1,3, T. Richtler4, P. Goudfrooij5,andM.Hempel2 1 Sternwarte der Ludwig-Maximilians-Universit¨at, Scheinerstr. 1, 81679 M¨unchen, Germany e-mail: [email protected] 2 European Southern Observatory, 85749 Garching bei M¨unchen, Germany e-mail: [email protected] 3 Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstrasse, 85748 Garching bei M¨unchen, Germany e-mail: bender, maraston, [email protected] 4 Grupo de Astronom´ıa, Departamento de F´ısica, Casilla 160-C, Universidad de Concepci´on, Concepci´on, Chile e-mail: [email protected] 5 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] Received 14 May 2003 / Accepted 11 September 2003 Abstract. We present Lick line-index measurements of extragalactic globular clusters in seven early-type galaxies (NGC 1380, 2434, 3115, 3379, 3585, 5846, and 7192) with different morphological types (E–S0) located in field and group/cluster environ- ments. High-quality spectra were taken with the FORS2 instrument at ESO’s Very Large Telescope. 50% of our data allows an age resolution ∆t/t 0.3 and a metallicity resolution 0.25 0.4 dex, depending on the absolute metallicity.∼ Globular cluster candidates are selected≈ from deep B, V, R, I, K FORS2/ISAAC∼ − photometry with 80 100% success rate inside one effective ra- − dius. -
Neutral Hydrogen Gas Within and Around NGC 1316
This is an Open Access document downloaded from ORCA, Cardiff University's institutional repository: http://orca.cf.ac.uk/124401/ This is the author’s version of a work that was submitted to / accepted for publication. Citation for final published version: Serra, P., Maccagni, F. M., Kleiner, D., de Blok, W. J. G., van Gorkom, J. H., Hugo, B., Iodice, E., Jozsa, G. I. G., Kamphuis, P., Kraan-Korteweg, R., Loni, A., Makhathini, S., Molnar, D., Oosterloo, T., Peletier, R., Ramaila, A., Ramatsoku, M., Smirnov, O. and Smith, Matthew W. L. 2019. Neutral hydrogen gas within and around NGC 1316. Astronomy and Astrophysics 628 , A122. 10.1051/0004-6361/201936114 file Publishers page: http://dx.doi.org/10.1051/0004-6361/201936114 <http://dx.doi.org/10.1051/0004- 6361/201936114> Please note: Changes made as a result of publishing processes such as copy-editing, formatting and page numbers may not be reflected in this version. For the definitive version of this publication, please refer to the published source. You are advised to consult the publisher’s version if you wish to cite this paper. This version is being made available in accordance with publisher policies. See http://orca.cf.ac.uk/policies.html for usage policies. Copyright and moral rights for publications made available in ORCA are retained by the copyright holders. Astronomy & Astrophysics manuscript no. n1316 c ESO 2019 July 17, 2019 Neutral hydrogen gas within and around NGC 1316 P. Serra1,⋆, F. M. Maccagni1, D. Kleiner1, W. J. G. de Blok2, 3, 4, J. H. van Gorkom5, B. -
The Black Hole Mass Function Derived from Local Spiral Galaxies
PUBLISHED IN THE ASTROPHYSICAL JOURNAL, 789:124 (16PP),2014 JULY 10 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE BLACK HOLE MASS FUNCTION DERIVED FROM LOCAL SPIRAL GALAXIES BENJAMIN L. DAVIS1 , JOEL C. BERRIER1,2,5,LUCAS JOHNS3,6 ,DOUGLAS W. SHIELDS1,2, MATTHEW T. HARTLEY2,DANIEL KENNEFICK1,2, JULIA KENNEFICK1,2, MARC S. SEIGAR1,4 , AND CLAUD H.S. LACY1,2 Published in The Astrophysical Journal, 789:124 (16pp), 2014 July 10 ABSTRACT We present our determination of the nuclear supermassive black hole mass (SMBH) function for spiral galax- ies in the local universe, established from a volume-limited sample consisting of a statistically complete col- lection of the brightest spiral galaxies in the southern (δ< 0◦) hemisphere. Our SMBH mass function agrees well at the high-mass end with previous values given in the literature. At the low-mass end, inconsistencies exist in previous works that still need to be resolved, but our work is more in line with expectations based on modeling of black hole evolution. This low-mass end of the spectrum is critical to our understanding of the mass function and evolution of black holes since the epoch of maximum quasar activity. A limiting luminos- ity (redshift-independent) distance, DL = 25.4 Mpc (z =0.00572) and a limiting absolute B-band magnitude, MB = −19.12 define the sample. These limits define a sample of 140 spiral galaxies, with 128 measurable pitch angles to establish the pitch angle distribution for this sample. This pitch angle distribution function may be useful in the study of the morphology of late-type galaxies. -
Observer's Guide to Galaxies
Observer’s Guide to Galaxies By Rob Horvat (WSAAG) Mar 2020 This document has evolved from a supplement to Night-Sky Objects for Southern Observers (Night-Sky Objects for short), which became available on the web in 2009. The document has now been split into two, this one being called the Observer’s Guide to Galaxies. The maps have been designed for those interested in locating galaxies by star-hopping around the constellations. However, like Night-Sky Objects, the resource can be used to simply identify interesting galaxies to GOTO. As with Night-Sky Objects, the maps have been designed and oriented for southern observers with the limit of observation being Declination +55 degrees. Facing north, the constellations are inverted so that they are the “right way up”. Facing south, constellations have the usual map orientation. Pages are A4 in size and can be read as a pdf on a computer or tablet. Note on copyright. This document may be freely reproduced without alteration for educational or personal use. Contributed images by WSAAG members remain the property of their authors. Types of Galaxies Spiral (S) galaxies consist of a rotating disk of stars, dust and gas that surround a central bulge or concentration of stars. Bulges often house a central supermassive black hole. Most spiral galaxies have two arms that are sites of ongoing star formation. Arms are brighter than the rest of the disk because of young hot OB class stars. Approx. 2/3 of spiral galaxies have a central bar (SB galaxies). Lenticular (S0) galaxies have a rather formless disk (no obvious spiral arms) with a prominent bulge. -
CHANDRA X-RAY OBSERVATIONS of NGC 1316 (FORNAX A) Dong-Woo Kim and G
The Astrophysical Journal, 586:826–849, 2003 April 1 # 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. CHANDRA X-RAY OBSERVATIONS OF NGC 1316 (FORNAX A) Dong-Woo Kim and G. Fabbiano Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 Received 2002 June 25; accepted 2002 December 9 ABSTRACT We report the results of the Chandra ACIS subarcsecond resolution X-ray observation of the archetypal merger radio galaxy NGC 1316 (Fornax A). We confirm the presence of fine substructures in the hot inter- stellar medium (ISM). Some of these are likely to result from interaction with the radio jets, while others may be related to a complex intermingling of different phases of the ISM. We detect a low-luminosity X-ray active 39 À1 galactic nucleus (AGN) with LX ¼ 5 Â 10 ergs s (in 0.3–8 keV) and a À ¼ 1:7 power-law energy spectrum. We also detect 81 point sources within the 25th magnitude isophotal ellipse of NGC 1316 (LX in the range of 2 Â 1037 to 2 Â 1039 ergs sÀ1), with hard (kT 5 keV) X-ray spectra, typical of X-ray binaries, and a spatial radial distribution consistent with that of the optical (i.e., stellar) surface brightness. We derive the X-ray luminosity function (XLF) of these sources, correcting for the incompleteness at the faint end caused by the presence of the diffuse emission from the hot ISM in the central regions of NGC 1316 and by the widening of the Chandra point-spread functions at increasing distance from the aim point.