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Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
An Optical Spectroscopic Survey of the 3CR
A&A 560, A81 (2013) Astronomy DOI: 10.1051/0004-6361/201322842 & c ESO 2013 Astrophysics An optical spectroscopic survey of the 3CR sample of radio galaxies with z < 0.3 V. Implications for the unified model for FR IIs Ranieri D. Baldi1, Alessandro Capetti2, Sara Buttiglione3, Marco Chiaberge4,5,6, and Annalisa Celotti1,7,8 1 SISSA-ISAS, via Bonomea 265, 34136 Trieste, Italy e-mail: [email protected] 2 INAF − Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese, Italy 3 INAF − Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy 4 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 5 INAF − Istituto di Radio Astronomia, via P. Gobetti 101, 40129 Bologna, Italy 6 Center for Astrophysical Sciences, Johns Hopkins University, 3400 N. Charles Street Baltimore, MD 21218, USA 7 INAF − Osservatorio Astronomico di Brera, via E. Bianchi 46, 23807 Merate, Italy 8 INFN − Sezione di Trieste, via Valerio 2, 34127 Trieste, Italy Received 14 October 2013 / Accepted 30 October 2013 ABSTRACT We explore the implications of our optical spectroscopic survey of 3CR radio sources with z < 0.3 for the unified model (UM) for radio-loud AGN, focusing on objects with a “edge-brightened” (FR II) radio morphology. The sample contains 33 high ionization galaxies (HIGs) and 18 broad line objects (BLOs). According to the UM, HIGs, the narrow line sources, are the nuclearly obscured counterparts of BLOs. The fraction of HIGs indicates a covering factor of the circumnuclear matter of 65% that corresponds, adopting a torus geometry, to an opening angle of 50◦ ± 5. -
Lick Observatory Records: Photographs UA.036.Ser.07
http://oac.cdlib.org/findaid/ark:/13030/c81z4932 Online items available Lick Observatory Records: Photographs UA.036.Ser.07 Kate Dundon, Alix Norton, Maureen Carey, Christine Turk, Alex Moore University of California, Santa Cruz 2016 1156 High Street Santa Cruz 95064 [email protected] URL: http://guides.library.ucsc.edu/speccoll Lick Observatory Records: UA.036.Ser.07 1 Photographs UA.036.Ser.07 Contributing Institution: University of California, Santa Cruz Title: Lick Observatory Records: Photographs Creator: Lick Observatory Identifier/Call Number: UA.036.Ser.07 Physical Description: 101.62 Linear Feet127 boxes Date (inclusive): circa 1870-2002 Language of Material: English . https://n2t.net/ark:/38305/f19c6wg4 Conditions Governing Access Collection is open for research. Conditions Governing Use Property rights for this collection reside with the University of California. Literary rights, including copyright, are retained by the creators and their heirs. The publication or use of any work protected by copyright beyond that allowed by fair use for research or educational purposes requires written permission from the copyright owner. Responsibility for obtaining permissions, and for any use rests exclusively with the user. Preferred Citation Lick Observatory Records: Photographs. UA36 Ser.7. Special Collections and Archives, University Library, University of California, Santa Cruz. Alternative Format Available Images from this collection are available through UCSC Library Digital Collections. Historical note These photographs were produced or collected by Lick observatory staff and faculty, as well as UCSC Library personnel. Many of the early photographs of the major instruments and Observatory buildings were taken by Henry E. Matthews, who served as secretary to the Lick Trust during the planning and construction of the Observatory. -
The Jets in Radio Galaxies
The jets in radio galaxies Martin John Hardcastle Churchill College September 1996 A dissertation submitted in candidature for the degree of Doctor of Philosophy in the University of Cambridge i `Glaucon: ª...But how did you mean the study of astronomy to be reformed, so as to serve our pur- poses?º Socrates: ªIn this way. These intricate traceries on the sky are, no doubt, the loveliest and most perfect of material things, but still part of the visibleworld, and therefore they fall far short of the true realities Ð the real relativevelocities,in theworld of purenumber and all geometrical ®gures, of the movements which carry round the bodies involved in them. These, you will agree, can be conceived by reason and thought, not by the eye.º Glaucon: ªExactly.º Socrates: ªAccordingly, we must use the embroidered heaven as a model to illustrateour study of these realities, just as one might use diagrams exquisitely drawn by some consummate artist like Daedalus. An expert in geometry, meeting with such designs, would admire their ®nished workmanship, but he wouldthink it absurd to studythem in all earnest with the expectation of ®nding in their proportionsthe exact ratio of any one number to another...º ' Ð Plato (429±347 BC), The Republic, trans. F.M. Cornford. ii Contents 1 Introduction 1 1.1 Thisthesis...................................... ... 1 1.2 Abriefhistory................................... .... 2 1.3 Synchrotronphysics........ ........... ........... ...... 4 1.4 Currentobservationalknowledgeintheradio . ............. 5 1.4.1 Jets ........................................ 6 1.4.2 Coresornuclei ................................. 6 1.4.3 Hotspots ..................................... 7 1.4.4 Largescalestructure . .... 7 1.4.5 Theradiosourcemenagerie . .... 8 1.4.6 Observationaltrends . -
Extragalactic Radio Jets
Annual Reviews www.annualreviews.org/aronline Ann. Rev. Astron.Astrophys. 1984. 22 : 319-58 Copyright© 1984 by AnnualReviews Inc. All rights reserved EXTRAGALACTIC RADIO JETS Alan H. Bridle National Radio AstronomyObservatory, 1 Charlottesville, Virginia 22901 Richard A. Perley National Radio Astronomy Observatory, Socorro, New Mexico 87801 1. INTRODUCTION Powerful extended extragalactic radio sources pose two vexing astro- physical problems [reviewed in (147) and (157)]. First, from what energy reservoir do they draw their large radio luminosities (as muchas 10a8 W between 10 MHzand 100 GHz)?Second, how does the active center in the parent galaxy or QSOsupply as muchas 10~4 J in relativistic particles and fields to radio "lobes" up to several hundredkiloparsecs outside the optical object? Newaperture synthesis arrays (68, 250) and new image-processing algorithms (66, 101, 202, 231) have recently allowed radio imaging subarcsecond resolution with high sensitivity and high dynamicrange; as a result, the complexityof the brighter sources has been revealed clearly for the first time. Manycontain radio jets, i.e. narrow radio features between compact central "cores" and more extended "lobe" emission. This review examinesthe systematic properties of such jets and the dues they give to the by PURDUE UNIVERSITY LIBRARY on 01/16/07. For personal use only. physics of energy transfer in extragalactic sources. Wedo not directly consider the jet production mechanism,which is intimately related to the Annu. Rev. Astro. Astrophys. 1984.22:319-358. Downloaded from arjournals.annualreviews.org first problemnoted above--for reviews, see (207) and (251). 1. i Why "’Jets"? Baade & Minkowski(3) first used the term jet in an extragalactic context, describing the train of optical knots extending ,-~ 20" from the nucleus of M87; the knots resemble a fluid jet breaking into droplets. -
January 2010 Malama
SIERRA CLUB Cherish the Earth JOURNAL OF THE SIERRA CLUB, HAWAI`I CHAPTER A Quarterly Newsletter January - March 2010 Planting Native! Bold Policy Proposals Hey Mr. Green! Nate’s Adventures! National Ocean Policy Task Force Guest Entering the new year, Looking for ways to columnist what bold and realistic save the environment? Long-time Sierra Club Rick policy proposals can we Check out our advice volunteer Dave Raney Barbosa promote in order to column on short, easy describes the mission of SAVE A TREE! writes ensure a greener tips that you can use to the National Ocean about the Hawai`i? Learn about help save the Policy Task and some Receive your Malama the issues the Sierra Club environment. This Join Nate Yuen as he of the current electronically by going distribution, care, and is advocating month suggests how to describes a recent hike recommendations to cultural use of the native be green and save some along Wailuku River. being proposed. www.hi.sierraclub.org Ho`awa. Page 5 green! Click the link below Pages 8 - 9 Pages 10 - 11 “Email My Newsletter” Page 3 Page 6 private homes. Sandy areas -- where children build sand castles and Preserving sunbathers get “tan” -- are increasingly scarce and usually quite crowded. Sandy Hawai`i coastlines are dynamic. Beaches erode or accrete depending upon their location on the coast, their Beaches proximity to various things such as piers, sandwalls, the impact of storms, etc. Anyone who buys beachfront A Proposal to Protect Hawai’i’s property is made aware of the fact that Beaches for Our Keiki boundaries between private property and the public easement may shift over by Robert D. -
Lowellobserver
THE ISSUE 105 FALL 2015 LOWELL OBSERVER THE QUARTERLY NEWSLETTER OF LOWELL OBSERVATORY HOME OF PLUTO Just 15 minutes after its closest approach to Pluto on July 14, 2015, NASA’s New Horizons spacecraft looked back toward the Sun and captured a near- sunset view of the rugged, icy mountains and flat ice plains extending to Pluto’s horizon. (NASA/JHUAPL/SwRI) IN THIS SPECIAL EXTENDED ISSUE 2 Director’s Update 2 Trustee’s Update 3 Bound for Chile! New Horizons Unveils Pluto’s Secrets By Will Grundy Astronomers can normally study memes. Importantly, the focus remained distant objects only through their light, so almost entirely on the science, not hare- a unique appeal of solar system science is brained conspiracy theories or umbrage the possibility to send spacecraft to study at off-the-cuff remarks of team members. bodies in ways that could only be done Pluto, the real star of the show, up-close. Such spacecraft exploration isn’t certainly rose to the occasion, revealing 4 Education On Board SOFIA cheap, and competition is fierce over which incredible complexities and stark beauty. missions should be flown. The opportunity But much about the encounter was 5 Pluto Occultation Team to participate in one is a rare and cherished attributable to the hard-working team 6 Lowell Hosts Pluto Palooza opportunity for a planetary scientist like who delivered Pluto to the world. How myself. That’s especially so for a first-ever was this done, and what was it like being encounter with a previously unexplored involved? The key was practice. -
Arxiv:1804.09969V1
Research in Astron. Astrophys. Vol.0 (20xx) No.0, 000–000 Research in http://www.raa-journal.org http://www.iop.org/journals/raa Astronomy and (LATEX: sample.tex; printed on November 9, 2018; 22:51) Astrophysics The pc-scale radio structure of MIR-observed radio galaxies Ye Yuan1,2,3, Minfeng Gu1,2 and Yongjun Chen1,4 1 Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China; [email protected] 2 Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, 200030, China 3 Uinversity of Chinese Academy of Sciences,19A Yuquan Road, Beijing 10049, China 4 Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, 2 West Beijing Road, Nanjing, JiangSu 210008, China Abstract We investigated the relationship between the accretion process and jet proper- ties by ultilizing the VLBA and mid-infrared (MIR) data for a sample of 45 3CRR radio galaxies selected with a flux density at 178 MHz > 16.4 Jy, 5 GHz VLA core flux den- sity 7 mJy, and MIR observations. The pc-scale radio structure at 5 GHz are presented by using≥ our VLBA observations for 21 sources in February, 2016, the analysis on the archival data for 16 objects, and directly taking the measurements for 8 radio galaxies available in literatures. The accretion mode is constrained from the Eddington ratio with a dividing value of 0.01, which is estimated from the MIR-based bolometric luminosity and the black hole masses. While most FRII radio galaxies have higher Eddington ratio than FRIs, we found that there is indeed no single correspondence between the FR morphol- ogy and accretion mode with eight FRIIs at low accretion and two FRIs at high accretion rate. -
Radio Galaxies Dominate the High-Energy Diffuse Gamma-Ray
FERMILAB-PUB-16-128-A Prepared for submission to JCAP Radio Galaxies Dominate the High-Energy Diffuse Gamma-Ray Background Dan Hoopera;b;c Tim Lindend and Alejandro Lopeze;a aFermi National Accelerator Laboratory, Center for Particle Astrophysics, Batavia, IL 60510 bUniversity of Chicago, Department of Astronomy and Astrophysics, Chicago, IL 60637 cUniversity of Chicago, Kavli Institute for Cosmological Physics, Chicago, IL 60637 dOhio State University, Center for Cosmology and AstroParticle Physcis (CCAPP), Colum- bus, OH 43210 eMichigan Center for Theoretical Physics, Department of Physics, University of Michigan, Ann Arbor, MI 48109 E-mail: [email protected], [email protected], [email protected] Abstract. It has been suggested that unresolved radio galaxies and radio quasars (sometimes referred to as misaligned active galactic nuclei) could be responsible for a significant fraction of the observed diffuse gamma-ray background. In this study, we use the latest data from the Fermi Gamma-Ray Space Telescope to characterize the gamma-ray emission from a sample of 51 radio galaxies. In addition to those sources that had previously been detected using Fermi data, we report here the first statistically significant detection of gamma-ray emission from the radio galaxies 3C 212, 3C 411, and B3 0309+411B. Combining this information with the radio fluxes, radio luminosity function, and redshift distribution of this source class, we +25:4 find that radio galaxies dominate the diffuse gamma-ray background, generating 77:2−9:4 % of this emission at energies above 1 GeV. We discuss the implications of this result and point out that it provides support for∼ scenarios in which IceCube's high-energy astrophysical arXiv:1604.08505v2 [astro-ph.HE] 8 Aug 2016 neutrinos also originate from the same population of radio galaxies. -
A CHANDRA OBSERVATION of 3C 288— REHEATING the COOL CORE of a 3 Kev CLUSTER from a NUCLEAR OUTBURST at Z = 0.246
A CHANDRA OBSERVATION OF 3C 288— REHEATING THE COOL CORE OF A 3 keV CLUSTER FROM A NUCLEAR OUTBURST at z = 0.246 The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Lal, D. V., R. P. Kraft, W. R. Forman, M. J. Hardcastle, C. Jones, P. E. J. Nulsen, D. A. Evans, J. H. Croston, and J. C. Lee. “ A CHANDRA OBSERVATION OF 3C 288—REHEATING THE COOL CORE OF A 3 keV CLUSTER FROM A NUCLEAR OUTBURST at z = 0.246 .” The Astrophysical Journal 722, no. 2 (October 4, 2010): 1735–1743. © 2010 The American Astronomical Society As Published http://dx.doi.org/10.1088/0004-637x/722/2/1735 Publisher IOP Publishing Version Final published version Citable link http://hdl.handle.net/1721.1/95820 Terms of Use Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. The Astrophysical Journal, 722:1735–1743, 2010 October 20 doi:10.1088/0004-637X/722/2/1735 C 2010. The American Astronomical Society. All rights reserved. Printed in the U.S.A. A CHANDRA OBSERVATION OF 3C 288—REHEATING THE COOL CORE OF A 3 keV CLUSTER FROM A NUCLEAR OUTBURST at z = 0.246 D. V. Lal1, R. P. Kraft1, W. R. Forman1, M. J. Hardcastle2, C. Jones1,P.E.J.Nulsen1,D.A.Evans1,3, J. H. Croston4, and J. C. Lee1 1 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA 2 School of Physics, Astronomy, and Mathematics, University of Hertfordshire, Hatfield, AL 10 9AB, UK 3 MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue, Cambridge, MA 02139, USA 4 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1SJ, UK Received 2010 April 27; accepted 2010 August 25; published 2010 October 4 ABSTRACT We present results from a 42 ks Chandra/ACIS-S observation of the transitional FR I/FR II radio galaxy 3C 288 at z = 0.246. -
National Radio Astronomy Observatory Observing
NATIONAL RADIO ASTRONOMY OBSERVATORY OBSERVING SUMMARY-1989 STATISTICS February 1990 Cover The Radio Galaxy Fornax A The cover photograph is a superposition of the VLA radio emission (shown as red) from the radio galaxy Fornax A and the visible light in the vicinity of NGC 1316 (shown as blue-white). The two main radio emitting lobes are produced by relativistic electrons in magnetic fields which have been transported hundreds of thousands of light years outward from the elliptical galaxy NGC 1316 which lies between the two regions. The energy for the relativistic flow apparently was provided by the gravitational capture of small galaxies by NGC 1316. The shock waves and trails of the infallen galaxies produce the features in the radio lobes seen as filaments and rings. The small galaxy near NGC 1316 may soon be captured. Observation details: Observers: E. Fomalont (NRAO), R. Ekers (Australia Telescope), K. Ebneter and W. Van Breugel (U. California) Frequency of 1.384 GHz; five hours of D-configuration and five hours of C-configuration Resolution of 15"; field of view is 60' x 40' NATIONAL RADIO ASTRONOMY OBSERVATORY OBSERVING SUMMARY 1989 STATISTICS FEBRUARY 1990 SOME HIGHLIGHTS OF THE 1989 RESEARCH PROGRAM A second Einstein Ring has been identified from new A-configuration VLA observations of MG1652+138, the second candidate for an Einstein ring gravitational lens system to be selected from the MIT-Green Bank 5 GHz survey. Optical images and spectra established the redshift of a faint blue quasar between the two radio sources, while the VLA results have both detected the quasar core at its optical location and improved the ring image quality. -
B Gg Revisited: the Environments of Low-Excitation Radio Galaxies And
Astronomy & Astrophysics manuscript no. 0605 December 17, 2018 (DOI: will be inserted by hand later) Research Note Bgg revisited: The environments of low-excitation radio galaxies and unified models Martin J. Hardcastle Department of Physics, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK ([email protected]) Version of December 17, 2018 Abstract. Recent measurements of the galaxy clustering environments around intermediate-redshift radio sources have suggested a systematic environmental difference between radio galaxies and radio-loud quasars, in contradic- tion to the predictions of simple unified models for the two classes of object. I show that the apparent difference arises mainly as a result of the properties of low-excitation radio galaxies included in the radio-galaxy sam- ple, which tend to lie in significantly richer environments. The environmental properties of high-excitation radio galaxies and quasars are statistically consistent in the redshift range 0.15 <z< 0.4, as unified models would predict. Key words. galaxies: active – galaxies: quasars: general – galaxies: clusters: general – radio continuum: galaxies 1. Introduction achive good statistics at high redshifts (Barr et al. 2003), at lower redshifts simple Bgg determinations seem likely In unified models for powerful radio galaxies and radio- to be able to provide a statistical measure of the environ- loud quasars (Scheuer 1987, Barthel 1987, 1989) isotropic ments of different classes of source. properties of the two classes of objects, such as their Recently Harvanek et al. (2001: hereafter HESR) have clustering environments, should be statistically identical. carried out a large systematic study of the clustering However, the classical unified models work best at high properties of 3CR (Spinrad et al.