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I. Is There an Accretion Mode Dichotomy in Radio-Loud AGN?
MNRAS 440, 269–297 (2014) doi:10.1093/mnras/stu263 Advance Access publication 2014 March 10 An X-ray survey of the 2 Jy sample – I. Is there an accretion mode dichotomy in radio-loud AGN? B. Mingo,1,2‹ M. J. Hardcastle,1 J. H. Croston,3 D. Dicken,4 D. A. Evans,5 R. Morganti6,7 and C. Tadhunter8 1School of Physics, Astronomy & Mathematics, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK 2Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH, UK 3School of Physics and Astronomy, University of Southampton, Southampton SO17 1SJ, UK 4Institut d’Astrophysique Spatiale, Universite´ Paris Sud, F-91405 Orsay, France 5Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 6ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, NL-7990 AA Dwingeloo, the Netherlands 7Kapteyn Astronomical Institute, University of Groningen, PO Box 800, NL-9700 AV Groningen, the Netherlands 8Department of Physics and Astronomy, University of Sheffield, Hounsfield Road, Sheffield S3 7RH, UK Accepted 2014 February 6. Received 2014 February 6; in original form 2013 May 31 ABSTRACT We carry out a systematic study of the X-ray emission from the active nuclei of the 0.02 <z< 0.7 2 Jy sample, using Chandra and XMM–Newton observations. We combine our results with those from mid-infrared, optical emission-line and radio observations, and add them to those of the 3CRR sources. We show that the low-excitation objects in our samples show signs of radiatively inefficient accretion. We study the effect of the jet-related emission on the various luminosities, confirming that it is the main source of soft X-ray emission for our sources. -
ATNF News Issue No
Galaxy Pair NGC 1512 / NGC 1510 ATNF News Issue No. 67, October 2009 ISSN 1323-6326 Questacon "astronaut" street performer and visitors at the Parkes Open Days 2009. Credit: Shaun Amy, CSIRO. Cover page image Cover Figure: Multi-wavelength color-composite image of the galaxy pair NGC 1512/1510 obtained using the Digitised Sky Survey R-band image (red), the Australia Telescope Compact Array HI distribution (green) and the Galaxy Evolution Explorer NUV -band image (blue). The Spitzer 24µm image was overlaid just in the center of the two galaxies. We note that in the outer disk the UV emission traces the regions of highest HI column density. See article (page 28) for more information. 2 ATNF News, Issue 67, October 2009 Contents From the Director ...................................................................................................................................................................................................4 CSIRO Medal Winners .........................................................................................................................................................................................5 CSIRO Astronomy and Space Science Unit Formed ........................................................................................................................6 ATNF Distinguished Visitors Program ........................................................................................................................................................6 ATNF Graduate Student Program ................................................................................................................................................................7 -
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). -
Where Are Compton-Thick Radio Galaxies? a Hard X-Ray View of Three Candidates
MNRAS 000, 000–000 (0000) Preprint 11 September 2018 Compiled using MNRAS LATEX style file v3.0 Where are Compton-thick radio galaxies? A hard X-ray view of three candidates F. Ursini,1 ? L. Bassani,1 F. Panessa,2 A. Bazzano,2 A. J. Bird,3 A. Malizia,1 and P. Ubertini2 1 INAF-IASF Bologna, Via Gobetti 101, I-40129 Bologna, Italy. 2 INAF/Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere, 00133 Roma, Italy. 3 School of Physics and Astronomy, University of Southampton, SO17 1BJ, UK. Released Xxxx Xxxxx XX ABSTRACT We present a broad-band X-ray spectral analysis of the radio-loud active galactic nuclei NGC 612, 4C 73.08 and 3C 452, exploiting archival data from NuSTAR, XMM-Newton, Swift and INTEGRAL. These Compton-thick candidates are the most absorbed sources among the hard X-ray selected radio galaxies studied in Panessa et al.(2016). We find an X-ray absorbing column density in every case below 1:5 × 1024 cm−2, and no evidence for a strong reflection continuum or iron K α line. Therefore, none of these sources is properly Compton-thick. We review other Compton-thick radio galaxies reported in the literature, arguing that we currently lack strong evidences for heavily absorbed radio-loud AGNs. Key words: galaxies: active – galaxies: Seyfert – X-rays: galaxies – X-rays: individual: NGC 612, 4C 73.08, 3C 452 1 INTRODUCTION 2000). A number of local CT AGNs have been detected thanks to recent hard X-ray surveys with INTEGRAL (Sazonov et al. 2008; A significant fraction of active galactic nuclei (AGNs) are known Malizia et al. -
RESEARCH PROGRAMS 140-Foot Telescope
VS/G LI NATIONAL RADIO ASTRONOMY OBSERVATORY Charlottesville, Virginia r Quarterly Report October 1, 1981 - December 31, 1981 RESEARCH PROGRAMS 140-foot Telescope Hours Scheduled observing 1955.75 Scheduled maintenance and equipment changes 179.25 Scheduled tests and calibration 1.00 Time lost due to: equipment failure 34.75 power 9.50 weather 133.25 interference 0.00 The following line programs were conducted during this quarter. No. Observer (s) Program T-156 I. Kazes (Meudon, France) Observations to study giant molecular B. Turner clouds at the main 18 cm OH line frequencies. T-145 B. Turner Search within the 13-16 GHz range for new molecular species. S-233 L. Buxton (Illinois) Observations at 20.9 and 24.4 GHz to E. Campbell (Illinois) search for the HCN dimer (HCN) 2 . W. Flygare (Illinois) P. Jewell (Illinois) M. Schenewerk (Illinois) L. Snyder (Illinois) B-381 R. Brown Observations at 5-cm to confirm and extend the detection of recombination line emission from 3C 245 and a search for this type of emission from other QSOs. S-246 M. Bell (NRC, Canada) Search at 5 cm for recombination lines E. Seaquist (Toronto) in compact extragalactic sources. No. Observer(s) Program M-176 L. Avery (NRC, Canada) Observations at 18.2 GHz of the J=241 N. Broten (NRC, Canada) transition of HC3N, generally toward J. MacLeod (NRC, Canada) dark clouds. H. Matthews (NRC, Canada T. Oka (Chicago) The following continuum programs were conducted during this quarter. No. Observer (s) Program C-194 M. Condon (unaffiliated) Survey at 14.5 cm of extragalactic J. -
Sample Program of Study
Sample Program of Study - Nurse Anesthetist Program 126 Credits* (Specialty coursework in BOLD) Year One – Preclinical Year Summer Cr Fall Cr Spring Cr NAN 543 Principles of Anesthesia I 3 NAN 718 Prof Aspects NA I 1 NAN 544 Principles of Anes II 2 NGC 501 Conceptual Foundations 3 NGC 527 Eval and Gen Evidence for HC II 3 NAN 544L Principles of Anes II Lab 1 NGC 518 Health Promotion 3 NGC 527L Eval and Gen Evidence II Lab 1 NAN 672 Pharm Anesth/Adj Drugs 3 NGC 520 Scientific Communications 2 NGC 634 Organizational Leadership 3 NAN 719 Prof Aspects NA II 1 NGC 625 Pathophysiology for APN I 3 NGC 575 Adv Helth Assessmnt (CRNA) 2 NGC 502 Informatics 3 NGC 612 Pharmacotherapeutics 4 NGC 509 Ethics* 3 NGC 626 Pathophysiology for APN II 3 NGC 526 Eval and Gen Evidence for HC I 4 Total Credits 14 Total Credits 17 Total Credits 17 Year Two – Clinical Year I Summer Fall Spring NAN 598 Intro to NA Clin Prac (1 d/wk) 2 NAN 545 Principles of Anes III 3 NAN 546 Principles of Anes IV 3 NAN 601 NA Clin Pract I (3 d/wk) 6 NAN 602 NA Clin Pract II (4 d/wk) 8 NAN 603 NA Clin Pract III (4 d/wk) 8 NGC 632 Interpreting HC Policy 3 NAN 711 Current Top Anes 1 NAN 712 Current Top Anes II 1 NGC 692 Grantsmanship 1 NGC 701 State of the Science 3 NAN 721 Anes Crisis Res Mgt I 1 NGC 638 Program Evaluation 3 Total Credits 12 Total Credits 15 Total Credits 16 Year Three – Clinical Year II Summer Fall Spring NAN 604 NA Clin Pract IV (4 d/wk) 6 NAN 605 NA Clin Pract V (4 d/wk) 6 NAN 547 Principles of Anes V 3 NGC 725 DNP Advanced Clinical Prac I 2 NAN 713 Current Top Anes III 1 NAN 606 NA Clin Pract VI (4 d/wk) 8 NGC 798 DNP Capstone Course I 1 NAN 722 Anes Crisis Res Mgt II 1 NAN 714 Current Top Anes IV 1 NGC 533 Teaching in Nursing 3 NGC 726 DNP Advanced Clinical Prac II 2 NGC 799 DNP Capstone Course II 1 Total Credits 9 Total Credits 14 Total Credits 12 *Effective for all students matriculating Spring 2015 and thereafter, N509 is not a required course and the total credits will be 123. -
Publications 2019 16 Jul 2021
Publications 2019 16 Jul 2021 1 *Acciari, V.A.; Ansoldi, S.; Antonelli, L.A.; Engels, A.A.; Baack, D.; Babić, A.; Banerjee, B.; Barres de Almeida, U.; Barrio, J.A.; Becerra González, J. and 297 coauthors "Observation of inverse Compton emission from a long γ-ray burst". Nature, 575, 459-463 (2019). https://doi.org/10.1038/s41586-019-1754-6 (C) 2 *Agarwal, D.; Lorimer, D.R.; Fialkov, A.; Bannister, K.W.; Shannon, R.M.; Farah, W.l; Bhandari, S.; Macquart, J.-P.; Flynn, C.; Pignata, G.; and 12 coauthors "A fast radio burst in the direction of the Virgo Cluster". MNRAS, 490, 1-8 (2019). https://doi.org/10.1093/mnras/stz2574 (A) 3 Agliozzo, C.; Mehner, A.; Phillips, N.M.; Leto, P.; Groh, J.H.; Noriega-Crespo, A.; Buemi, C.; Cavallaro, F.; Cerrigone, L.; Ingallinera, A.; and 4 coauthors "A massive nebula around the luminous blue variable star RMC 143 revealed by ALMA". A&A, 626, 126, (2019). https://doi.org/10.1051/0004-6361/201935239 (C) 4 *Allison, J.R.; Mahony, E.K.; Moss, V.A.; Sadler, E.M.; Whiting, M.T.; Allison, R.F.; Bland-Hawthorn, J.; Curran, S.J.; Emonts, B.H.C.; Lagos, C.D.P.; and 6 coauthors "PKS B1740-517: an ALMA view of the cold gas feeding a distant interacting young radio galaxy". MNRAS, 482, 2934-2949 (2019). https://doi.org/10.1093/mnras/sty2852 (A) 5 *Alsaberi, R.Z.E.; Barnes, L.A.; Filipović, M.D.; Maxted, N.I.; Sano, H.; Rowell, G.; Bozzetto, L.M.; Gurovich, S.; Urošević, D.; Onić, D.; and 12 coauthors "Radio emission from interstellar shocks: Young type Ia supernova remnants and the case of N 103B in the Large Magellanic Cloud". -
Annual Report 1979
ANNUAL REPORT 1979 EUROPEAN SOUTHERN OBSERVATORY Cover Photograph This image is the result 0/ computer analysis through the ESO image-processing system 0/ the interaeting pair 0/galaxies ES0273-JG04. The spiral arms are disturbed by tidal/orces. One 0/ the two spirals exhibits Sey/ert characteristics. The original pfate obtained at the prime/ocus 0/ the 3.6 m telescope by S. Laustsen has been digitized with the new PDS machine in Geneva. ANNUAL REPORT 1979 presented to the Council by the Director-General, Prof. Dr. L. Woltjer Organisation Europeenne pour des Recherehes Astronomiques dans I'Hemisphere Austral EUROPEAN SOUTHERN OBSERVATORY TABLE OF CONTENTS INTRODUCTION ............................................ 5 RESEARCH................................................. 7 Schmidt Telescope; Sky Survey and Atlas Laboratory .................. 8 Joint Research with Chilean Institutes 9 Conferences and Workshops .................................... 9 FACILITIES Telescopes 11 Instrumentation 12 Image Processing ............................................. 13 Buildings and Grounds 15 FINANCIAL AND ORGANIZATIONAL MATTERS ................ 17 APPENDIXES AppendixI-UseofTeiescopes 22 Appendix II - Programmes 33 Appendix III - Publications ..................................... 47 Appendix IV - Members of Council, Committees and Working Groups for 1980. ................................................... 55 3 INTRODUCTION Several instruments were completed during ihe year, while others progressed weIl. Completed and sent to La Silla for installation -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Are All Radio Galaxies Genuine Ellipticals??
A&A 375, 791–796 (2001) Astronomy DOI: 10.1051/0004-6361:20010902 & c ESO 2001 Astrophysics Are all radio galaxies genuine ellipticals?? M. P. V´eron-Cetty1 and P. V´eron1 Observatoire de Haute Provence, CNRS, 04870 Saint-Michel l’Observatoire, France e-mail: [email protected] Received 16 January 2001 / Accepted 11 June 2001 Abstract. Classical double radio sources are believed to be powered by a strong relativistic jet due to the presence of a rapidly spinning black hole in the center of a giant E galaxy formed by the merging of two galaxies. If this is true, no radio source should have been found in spiral or S0 galaxies. A number of radio S0s have been reported, but most of them are probably misclassified Es. However, our own observations confirm that NGC 612 is an S0 although it is associated with the FR II radio source PKS 0131−36. We conclude that S0s can be classical radio sources, but that such occurences are extremely rare. Key words. galaxies: elliptical and lenticular, cD – galaxies: individual: NGC 612 – radio continuum: galaxies 1. Introduction S0 light profiles can be separated into two components: (1) a bulge component characterized by an E-like surface Most classical double radio sources (FR Is and FR IIs; brightness distribution, and (2) a disk component with an Fanaroff & Riley 1974) are associated with giant ellipti- exponential light distribution of the form: cal (E) galaxies. It has been suggested that these radio −r/ro sources are the result of the presence in the nucleus of the I = Io × e galaxies of a rapidly spinning black hole and that these black holes are due to the merging of two galaxies imply- where ro is the scale length of the exponential disk ing that S0s and spirals cannot be the host of a double (Freeman 1970). -
Biennial Report 2004 2005 Published in Spain by the ISAAC NEWTON GROUP of TELESCOPES (ING) ISSN 1575–8966 Legal License: TF–1142 /99
I SAAC N EWTON G ROUP OF T ELESCOPES Biennial Report 2004 2005 Published in Spain by the ISAAC NEWTON GROUP OF TELESCOPES (ING) ISSN 1575–8966 Legal license: TF–1142 /99 Apartado de correos, 321 E-38700 Santa Cruz de La Palma; Canary Islands; Spain Tel: +34 922 425 400 Fax: +34 922 425 401 URL: http://www.ing.iac.es/; http://www.ast.cam.ac.uk/ING/ (UK mirror) Editor and designer: Javier Méndez ([email protected]) Preprinting: Gráficas El Time. Tel: +34 922 416 651 Printing: Gráficas Sabater. Tel: +34 922 623 555 Front cover: IC1396 or the Elephant Trunk Nebula. Image obtained as part of the Isaac Newton Telescope Photometric Hα Survey of the Northen Galactic Plane, and it was prepared by Nick Wright, University College London. Inset: Photograph of laser test on the William Herschel Telescope as part of GLAS preparatory study. Credit: Javier Méndez. Other picture credits: Nik Szymanek (WHT, p. 4); Nik Szymanek (INT, p. 4); Nik Szymanek (JKT, p. 4); Nik Szymanek (ING, p. 5); Jens Moser (WHT, back); Jens Moser (INT, back); Nik Szymanek (JKT, back). The ING Biennial Report is available online at http://www.ing.iac.es/PR/AR/ or at http://www.ast.cam.ac.uk/ING/PR/AR/. ISAAC NEWTON GROUP OF TELESCOPES Biennial Report of the PPARC-NWO-IAC ING Board 2004 – 2005 ISAAC NEWTON GROUP William Herschel Telescope Isaac Newton Telescope Jacobus Kapteyn Telescope 4 • ING BIENNIAL R EPORT 2004–2005 OF TELESCOPES The Isaac Newton Group of Telescopes (ING) consists of the 4.2- metre William Herschel Telescope (WHT), the 2.5-metre Isaac Newton Telescope (INT) and the 1.0-metre Jacobus Kapteyn Telescope (JKT). -
The Properties of the Young Stellar Populations in Powerful Radio Galaxies at Low and Intermediate Redshifts Holt, J.; Tadhunter, C
University of Groningen The properties of the young stellar populations in powerful radio galaxies at low and intermediate redshifts Holt, J.; Tadhunter, C. N.; Delgado, R. M. Gonzalez; Inskip, K. J.; Rodriguez, J.; Emonts, B. H. C.; Morganti, R.; Wills, K. A. Published in: Monthly Notices of the Royal Astronomical Society DOI: 10.1111/j.1365-2966.2007.12140.x IMPORTANT NOTE: You are advised to consult the publisher's version (publisher's PDF) if you wish to cite from it. Please check the document version below. Document Version Publisher's PDF, also known as Version of record Publication date: 2007 Link to publication in University of Groningen/UMCG research database Citation for published version (APA): Holt, J., Tadhunter, C. N., Delgado, R. M. G., Inskip, K. J., Rodriguez, J., Emonts, B. H. C., Morganti, R., & Wills, K. A. (2007). The properties of the young stellar populations in powerful radio galaxies at low and intermediate redshifts. Monthly Notices of the Royal Astronomical Society, 381(2), 611-639. https://doi.org/10.1111/j.1365-2966.2007.12140.x Copyright Other than for strictly personal use, it is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), unless the work is under an open content license (like Creative Commons). The publication may also be distributed here under the terms of Article 25fa of the Dutch Copyright Act, indicated by the “Taverne” license. More information can be found on the University of Groningen website: https://www.rug.nl/library/open-access/self-archiving-pure/taverne- amendment.