Brightness Profiles of Early-Type Galaxies Hosting Seyfert Nuclei
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Near-Infrared Luminosity Relations and Dust Colors L
A&A 578, A47 (2015) Astronomy DOI: 10.1051/0004-6361/201525817 & c ESO 2015 Astrophysics Obscuration in active galactic nuclei: near-infrared luminosity relations and dust colors L. Burtscher1, G. Orban de Xivry1, R. I. Davies1, A. Janssen1, D. Lutz1, D. Rosario1, A. Contursi1, R. Genzel1, J. Graciá-Carpio1, M.-Y. Lin1, A. Schnorr-Müller1, A. Sternberg2, E. Sturm1, and L. Tacconi1 1 Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, Gießenbachstr., 85741 Garching, Germany e-mail: [email protected] 2 Raymond and Beverly Sackler School of Physics & Astronomy, Tel Aviv University, 69978 Ramat Aviv, Israel Received 5 February 2015 / Accepted 5 April 2015 ABSTRACT We combine two approaches to isolate the AGN luminosity at near-IR wavelengths and relate the near-IR pure AGN luminosity to other tracers of the AGN. Using integral-field spectroscopic data of an archival sample of 51 local AGNs, we estimate the fraction of non-stellar light by comparing the nuclear equivalent width of the stellar 2.3 µm CO absorption feature with the intrinsic value for each galaxy. We compare this fraction to that derived from a spectral decomposition of the integrated light in the central arcsecond and find them to be consistent with each other. Using our estimates of the near-IR AGN light, we find a strong correlation with presumably isotropic AGN tracers. We show that a significant offset exists between type 1 and type 2 sources in the sense that type 1 MIR X sources are 7 (10) times brighter in the near-IR at log LAGN = 42.5 (log LAGN = 42.5). -
On the Origin and Propagation of Ultra-High Energy Cosmic Rays (Measurements & Prediction Techniques)
Dissertation On the Origin and Propagation of Ultra-High Energy Cosmic Rays (Measurements & Prediction Techniques) Nils Nierstenhoefer Wuppertal, 2011 University of Wuppertal Supervisor/First reviewer: Prof. Dr. K.-H. Kampert Second reviewer: Prof. Dr. M. Risse Motivation & Preface It is a long known fact that cosmic rays reach Earth with tremendous energies of even above 1020 eV. Despite of decades of intensive research, it was not possible to finally reveal the origin of these par- ticles. The main obstacle in this field is their rare occurrence. This is due to a very steep energy spectrum. To make this point more clear, one roughly expects to observe less than one particle per km2 in one century exceeding energies larger than 1020 eV. To overcome the limitation of low statis- tics, larger and larger cosmic ray detectors have been deployed. Today’s largest cosmic ray detector is the Pierre Auger observatory (PAO) which was constructed in the Pampa Amarilla in Argentina. It covers an area of 3000 km2 and provides the largest set of observations of ultra-high energy cosmic rays (UHECR) in history. A second difficulty in understanding the origin of UHECR should be pointed out: Galactic and extra- galactic magnetic fields might alter the direction of even the highest energy events in a way that they do not point back to their source. In 2007 and 2008, already before the completion of the full detector, the Auger collaboration pub- lished a set of three important papers [1, 2, 3]. The first paper dealt with the correlation of the arrival directions of the highest energetic events with the distribution of active galactic nuclei (AGN) closer than 75Mpc from a catalog compiled by Veron-Cetty and Veron (VC-V) [4]. -
Lateinischer Name: Deutscher Name: Hya Hydra Wasserschlange
Lateinischer Name: Deutscher Name: Hya Hydra Wasserschlange Atlas Karte (2000.0) Kulmination um Cambridge 10, 16, Mitternacht: Star Atlas 17 12, 13, Sky Atlas Benachbarte Sternbilder: 20, 21 Ant Cnc Cen Crv Crt Leo Lib 9. Februar Lup Mon Pup Pyx Sex Vir Deklinationsbereic h: -35° ... 7° Fläche am Himmel: 1303° 2 Mythologie und Geschichte: Bei der nördlichen Wasserschlange überlagern sich zwei verschiedene Bilder aus der griechischen Mythologie. Das erste Bild zeugt von der eher harmlosen Wasserschlange aus der Geschichte des Raben : Der Rabe wurde von Apollon ausgesandt, um mit einem goldenen Becher frisches Quellwasser zu holen. Stattdessen tat sich dieser an Feigen gütlich und trug bei seiner Rückkehr die Wasserschlange in seinen Fängen, als angebliche Begründung für seine Verspätung. Um jedermann an diese Untat zu erinnern, wurden der Rabe samt Becher und Wasserschlange am Himmel zur Schau gestellt. Von einem ganz anderen Schlag war die Wasserschlange, mit der Herakles zu tun hatte: In einem Sumpf in der Nähe von Lerna, einem See und einer Stadt an der Küste von Argo, hauste ein unsagbar gefährliches und grässliches Untier. Diese Schlange soll mehrere Köpfe gehabt haben. Fünf sollen es gewesen sein, aber manche sprechen auch von sechs, neun, ja fünfzig oder hundert Köpfen, aber in jedem Falle war der Kopf in der Mitte unverwundbar. Fürchterlich war es, da diesen grässlichen Mäulern - ob die Schlange nun schlief oder wachte - ein fauliger Atem, ein Hauch entwich, dessen Gift tödlich war. Kaum schlug ein todesmutiger Mann dem Untier einen Kopf ab, wuchsen auf der Stelle zwei neue Häupter hervor, die noch furchterregender waren. Eurystheus, der König von Argos, beauftragte Herakles in seiner zweiten Aufgabe diese lernäische Wasserschlange zu töten. -
Stark Broadening of Spectral Lines in Plasmas
atoms Stark Broadening of Spectral Lines in Plasmas Edited by Eugene Oks Printed Edition of the Special Issue Published in Atoms www.mdpi.com/journal/atoms Stark Broadening of Spectral Lines in Plasmas Stark Broadening of Spectral Lines in Plasmas Special Issue Editor Eugene Oks MDPI • Basel • Beijing • Wuhan • Barcelona • Belgrade Special Issue Editor Eugene Oks Auburn University USA Editorial Office MDPI St. Alban-Anlage 66 4052 Basel, Switzerland This is a reprint of articles from the Special Issue published online in the open access journal Atoms (ISSN 2218-2004) in 2018 (available at: https://www.mdpi.com/journal/atoms/special issues/ stark broadening plasmas) For citation purposes, cite each article independently as indicated on the article page online and as indicated below: LastName, A.A.; LastName, B.B.; LastName, C.C. Article Title. Journal Name Year, Article Number, Page Range. ISBN 978-3-03897-455-0 (Pbk) ISBN 978-3-03897-456-7 (PDF) Cover image courtesy of Eugene Oks. c 2018 by the authors. Articles in this book are Open Access and distributed under the Creative Commons Attribution (CC BY) license, which allows users to download, copy and build upon published articles, as long as the author and publisher are properly credited, which ensures maximum dissemination and a wider impact of our publications. The book as a whole is distributed by MDPI under the terms and conditions of the Creative Commons license CC BY-NC-ND. Contents About the Special Issue Editor ...................................... vii Preface to ”Stark Broadening of Spectral Lines in Plasmas” ..................... ix Eugene Oks Review of Recent Advances in the Analytical Theory of Stark Broadening of Hydrogenic Spectral Lines in Plasmas: Applications to Laboratory Discharges and Astrophysical Objects Reprinted from: Atoms 2018, 6, 50, doi:10.3390/atoms6030050 ................... -
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). -
A Search for Transiting Extrasolar Planets in the Open Cluster NGC 4755
ResearchOnline@JCU This file is part of the following reference: Jayawardene, Bandupriya S. (2015) A search for transiting extrasolar planets in the open cluster NGC 4755. DAstron thesis, James Cook University. Access to this file is available from: http://researchonline.jcu.edu.au/41511/ The author has certified to JCU that they have made a reasonable effort to gain permission and acknowledge the owner of any third party copyright material included in this document. If you believe that this is not the case, please contact [email protected] and quote http://researchonline.jcu.edu.au/41511/ A SEARCH FOR TRANSITING EXTRASOLAR PLANETS IN THE OPEN CLUSTER NGC 4755 by Bandupriya S. Jayawardene A thesis submitted in satisfaction of the requirements for the degree of Doctor of Astronomy in the Faculty of Science, Technology and Engineering June 2015 James Cook University Townsville - Australia i STATEMENT OF ACCESS I the undersigned, author of this work, understand that James Cook University will make this thesis available for use within the University Library and, via the Australian Digital Thesis network, for use elsewhere. I understand that, as an unpublished work, a thesis has significant protection under the Copyright Act and; I do not wish to place any further restriction on access to this work. 2 STATEMENT OF SOURCES DECLARATION I declare that this thesis is my own work and has not been submitted in any form for another degree or diploma at any University or other institution of tertiary education. Information derived from the published or unpublished work of others has been acknowledged in the text and list of references is given. -
The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-To-Light Ratio
The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-to-Light Ratio Gene G. Byrd – University of Alabama Tarsh Freeman – Bevill State Community College Ronald J. Buta – University of Alabama Deposited 06/13/2018 Citation of published version: Byrd, G., Freeman, T., Buta, R. (2006): The Inner Resonance Ring of NGC 3081. II. Star Formation, Bar Strength, Disk Surface Mass Density, and Mass-to-Light Ratio. The Astronomical Journal, 131(3). DOI: 10.1086/499944 © 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. The Astronomical Journal, 131:1377–1393, 2006 March # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE INNER RESONANCE RING OF NGC 3081. II. STAR FORMATION, BAR STRENGTH, DISK SURFACE MASS DENSITY, AND MASS-TO-LIGHT RATIO Gene G. Byrd,1 Tarsh Freeman,2 and Ronald J. Buta1 Received 2005 July 19; accepted 2005 November 19 ABSTRACT We complement our Hubble Space Telescope (HST ) observations of the inner ring of the galaxy NGC 3081 using an analytical approach and n-body simulations. We find that a gas cloud inner (r) ring forms under a rotating bar perturbation with very strong azimuthal cloud crowding where the ring crosses the bar major axis. Thus, star forma- tion results near to and ‘‘downstream’’ of the major axis. From the dust distribution and radial velocities, the disk rotates counterclockwise (CCW) on the sky like the bar pattern speed. We explain the observed CCW color asym- metry crossing the major axis as due to the increasing age of stellar associations inside the r ring major axis. -
Mass Distribution in Galaxy Clusters
Pontificia Universidad Cat´olicade Chile Facultad de F´ısica Instituto de Astrof´ısica The Blue Straggler Star Populations in Galactic Globular Clusters by Mirko Simunovic Mu~noz Thesis presented to the Instituto de Astrof´ısica, Facultad de F´ısica, Pontificia Universidad Cat´olica de Chile to obtain the degree of Doctor in Astrophysics Thesis presented to the Combined Faculties for the Natural Sciences and for Mathematics of the Ruperto-Carola University of Heidelberg, Germany to obtain the degree of Doctor of Natural Sciences Supervisors : Prof. Dr. Thomas H. Puzia Prof. Dr. Eva K. Grebel Correctors : Prof. Dr. Marcio Catel´an Prof. Dr. Dante Minnitti Prof. Dr. Jorge Alfaro Santiago − Heidelberg 2016 Dissertation submitted to the Instituto de Astrof´ısica,Facultad de F´ısica Pontificia Universidad Cat´olicade Chile, Chile for the degree of Doctor in Astrophysics submitted to the Combined Faculties for the Natural Sciences and for Mathematics of the Ruperto-Carola University of Heidelberg, Germany for the degree of Doctor of Natural Sciences Put forward by Mirko Simunovic Mu~noz born in: Antofagasta, Chile Oral examination: October 19, 2016 The Blue Straggler Star Populations in Galactic Globular Clusters Mirko Simunovic Mu~noz Astronomisches Rechen-Institut Referees: Prof. Dr. Eva K. Grebel Prof. Dr. Thomas H. Puzia vi Abstract The puzzling existence of Blue Straggler Stars (BSSs) implies that they must form in relatively recent events, after the majority of the constituent globular cluster (GC) stellar population was formed. In this thesis we compile a large set of independent work to help understand the formation of BSSs. In Chapter2 we present new proper-motion cleaned BSS catalogs in 38 Milky Way GCs based on multi-passband and multi-epoch treasury survey data from the Hubble Space Telescope. -
OBSERVING GALAXIES in ANDROMEDA As You Look Towards
OBSERVING GALAXIES IN ANDROMEDA As you look towards Andromeda you are looking out into deep space underneath the Perseus spiral arm of our milky way. The constellation has a good density of observable galaxies. There is a group of relatively local galaxies which are less than 20 million light years away and then a big gap to the rest which are over 200 million light years away. The constellation is well place from late summer to mid-winter. M31 / M32 / M110 These galaxies are generally the first galaxies that amateur astronomers observe first. M31 is visible to the naked eye in dark skies. M31 whilst bright and large is fairly bland in appearance until you start to look a bit closer. With good conditions, the dark line of a dust lane is visible. I have to say that observing two of the globular clusters of this galaxy rank up there in my most memorable observations ever. M32 is very bright and I have seen it in binoculars as a very small bright blob. M110 can be a challenge to see with its low surface brightness. Having said that, I have seen it easily in my 80mm binoculars when the sky was transparent. NGC404 This galaxy is memorable to observe as it is close to the star Mirach and hence is known as Mirach’s ghost. It is a lovely circular low surface brightness glow that is visible with direct vision in my 10 inch reflector and was visible at low power with averted vision even with Mirach in the field of view. -
The Host Galaxy/AGN Connection. Brightness Profiles of Early-Type Galaxies Hosting Seyfert Nuclei
Astronomy & Astrophysics manuscript no. 6684 October 25, 2018 (DOI: will be inserted by hand later) The host galaxy/AGN connection⋆. Brightness profiles of early-type galaxies hosting Seyfert nuclei. Alessandro Capetti1 and Barbara Balmaverde1 INAF - Osservatorio Astronomico di Torino, Strada Osservatorio 20, I-10025 Pino Torinese, Italy e-mail: [email protected] e-mail: [email protected] Abstract. We recently presented evidence of a connection between the brightness profiles of nearby early-type galaxies and the properties of the AGN they host. The radio loudness of the AGN appears to be univocally related to the host’s brightness profile: radio-loud nuclei are only hosted by “core” galaxies while radio-quiet AGN are only found in “power-law” galaxies. We extend our analysis here to a sample of 42 nearby (Vrec < 7000 − km s 1) Seyfert galaxies hosted by early-type galaxies. From the nuclear point of view, they show a large deficit of radio emission (at a given X-ray or narrow line luminosity) with respect to radio-loud AGN, conforming with their identification as radio-quiet AGN. We used the available HST images to study their brightness profiles. Having excluded complex and highly nucleated galaxies, in the remaining 16 objects the brightness profiles can be successfully modeled with a Nuker law with a steep nuclear cusp characteristic of “power-law” galaxies (with logarithmic slope γ = 0.51 − 1.07). This result is what is expected for these radio-quiet AGN based on our previous findings, thus extending the validity of the connection between brightness profile and radio loudness to AGN of a far higher luminosity. -
Readingsample
Stellar Physics 2: Stellar Evolution and Stability Bearbeitet von Gennady S. Bisnovatyi-Kogan, A.Y. Blinov, M. Romanova 1. Auflage 2011. Buch. xxii, 494 S. Hardcover ISBN 978 3 642 14733 3 Format (B x L): 15,5 x 23,5 cm Gewicht: 1024 g Weitere Fachgebiete > Physik, Astronomie > Astronomie: Allgemeines > Astrophysik Zu Inhaltsverzeichnis schnell und portofrei erhältlich bei Die Online-Fachbuchhandlung beck-shop.de ist spezialisiert auf Fachbücher, insbesondere Recht, Steuern und Wirtschaft. Im Sortiment finden Sie alle Medien (Bücher, Zeitschriften, CDs, eBooks, etc.) aller Verlage. Ergänzt wird das Programm durch Services wie Neuerscheinungsdienst oder Zusammenstellungen von Büchern zu Sonderpreisen. Der Shop führt mehr als 8 Millionen Produkte. Chapter 8 Pre-Main Sequence Evolution As can be seen from the calculations of cloud collapse described in Sect. 7.2,stars with mass M>3Mˇ appear in the optical range immediately near to the main se- quence. Objects of lower mass exist for part of the time as optical stars with radiation due to gravitational contraction energy. Consider evolution of a star from its ap- pearance in the optical region until it reaches the main sequence, and its central temperature becomes sufficiently high to initiate a nuclear reaction converting hy- drogen into helium (see review [105]). 8.1 Hayashi Phase The pre-main sequence evolution of stars takes place at not very high temperatures, when a non-full ionization of matter and large opacity cause such stars to be almost convective. This fact was first established by Hayashi [461, 462], who took into account a convection in constructing evolutionary tracks for contracting stars in the HR diagram (see Fig. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it.