Appendix: Swift's Deep Sky Catalogs
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al. -
Large-Scale Outflows in Edge-On Seyfert Galaxies. II. Kiloparsec
Large-Scale Outflows in Edge-on Seyfert Galaxies. II. Kiloparsec-Scale Radio Continuum Emission Edward J. M. Colbert1,2, Stefi A. Baum1, Jack F. Gallimore1,2, Christopher P. O’Dea1, Jennifer A. Christensen1 Received ; accepted arXiv:astro-ph/9604022v1 3 Apr 1996 1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 2 Department of Astronomy, University of Maryland, College Park, MD 20742 –2– ABSTRACT We present deep images of the kpc-scale radio continuum emission in 14 edge-on galaxies (ten Seyfert and four starburst galaxies). Observations were taken with the VLA at 4.9 GHz (6 cm). The Seyfert galaxies were selected from a distance-limited sample of 22 objects (defined in paper I). The starburst galaxies were selected to be well-matched to the Seyferts in radio power, recessional velocity and inclination angle. All four starburst galaxies have a very bright disk component and one (NGC 3044) has a radio halo that extends several kpc out of the galaxy plane. Six of the ten Seyferts observed have large-scale (radial extent >1 kpc) radio structures extending outward from the ∼ nuclear region, indicating that large-scale outflows are quite common in Seyferts. Large-scale radio sources in Seyferts are similar in radio power and radial extent to radio halos in edge-on starburst galaxies, but their morphologies do not resemble spherical halos observed in starburst galaxies. The sources have diffuse morphologies, but, in general, they are oriented at skewed angles with respect to the galaxy minor axes. This result is most easily understood if the outflows are AGN-driven jets that are somehow diverted away from the galaxy disk on scales >1 kpc. -
Flat Galaxy - Above 30 Deg
Flat Galaxy - Above 30 Deg. DEC A B C D E F G H I J K L 1 Const. Object ID Other ID RA Dec Size (arcmin) Mag Urano. Urano. Millennium Notes 2 RFGC NGC hh mm ss dd mm ss.s Major Minor 1st Ed. 2nd Ed. 3 CVn 2245 NGC 4244 12 17 30 +37 48 31 19.4 2.1 10.2 107 54 633 Vol II Note: 4 Com 2335 NGC 4565 12 36 21 +25 59 06 15.9 1.9 10.6 149 71 677 Vol II Note: Slightly asymmetric dust lane 5 Dra 2946 NGC 5907 15 15 52 +56 19 46 12.8 1.4 11.3 50 22 568 Vol II Note: 6 Vir 2315 NGC 4517 12 32 46 +00 06 53 11.5 1.5 11.3 238 110 773 Vol II Note: Dust spots 7 Vir 2579 NGC 5170 13 29 49 -17 57 57 9.9 1.2 11.8 285 130 842 Vol II Note: Eccentric dust lane 8 UMa 2212 NGC 4157 12 11 05 +50 29 07 7.9 1.1 12.2 47 37 592 Vol II Note: 9 Vir 2449 MCG-3-33-30 13 03 17 -17 25 23 8.0 1.1 12.5 284 130 843 Vol II Note: Four knots in the centre 10 CVn 2495 NGC 5023 13 12 12 +44 02 17 7.3 0.8 12.7 75 37 609 Vol II Note: 11 Hya 2682 IC 4351 13 57 54 -29 18 57 6.1 0.8 12.9 371 148 888 Vol II Note: Dust lane. -
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. -
Structure and Star Formation in Disk Galaxies I. Sample Selection And
Mon. Not. R. Astron. Soc. 000, 1–9 (2003) Printed 31 October 2018 (MN LATEX style file v1.4) Structure and star formation in disk galaxies I. Sample selection and near infrared imaging J. H. Knapen1,2, R. S. de Jong3, S. Stedman1 and D. M. Bramich4 1University of Hertfordshire, Department of Physical Sciences, Hatfield, Herts AL10 9AB 2Isaac Newton Group of Telescopes, Apartado 321, E-38700 Santa Cruz de La Palma, Spain 3Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 4School of Physics and Astronomy, University of St. Andrews, Scotland KY16 9SS Accepted March 2003. Received ; in original form ABSTRACT We present near-infrared imaging of a sample of 57 relatively large, Northern spiral galaxies with low inclination. After describing the selection criteria and some of the basic properties of the sample, we give a detailed description of the data collection and reduction procedures. The Ks λ =2.2µm images cover most of the disk for all galaxies, with a field of view of at least 4.2 arcmin. The spatial resolution is better than an arcsec for most images. We fit bulge and exponential disk components to radial profiles of the light distribution. We then derive the basic parameters of these components, as well as the bulge/disk ratio, and explore correlations of these parameters with several galaxy parameters. Key words: galaxies: spiral – galaxies: structure – infrared: galaxies 1 INTRODUCTION only now starting to be published (e.g., 2MASS: Skrutskie et al. 1997, Jarrett et al. 2003; Seigar & James 1998a, 1998b; Near-infrared (NIR) imaging of galaxies is a better tracer Moriondo et al. -
Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V
Astronomy Letters, Vol. 27, No. 4, 2001, pp. 207–212. Translated from Pis’ma v Astronomicheskiœ Zhurnal, Vol. 27, No. 4, 2001, pp. 243–249. Original Russian Text Copyright © 2001 by Dubrovich. Formation Mechanisms of “Negative”-Intensity Spots in the Cosmic Microwave Background Radiation and Distant Objects V. K. Dubrovich* Special Astrophysical Observatory, Russian Academy of Sciences, pos. Nizhniœ Arkhyz, Stavropol kraœ, 357147 Russia Received June 2, 2000; in final form, October 2, 2000 Abstract—We consider the formation mechanisms of “negative”-intensity spots in the radio band for various astrophysical conditions. For wavelengths λ < 1.5 mm, the regions of reduced temperature (relative to the cos- mic microwave background radiation, CMBR) are shown to be produced only by high-redshift objects moving at peculiar velocities. The main processes are CMBR Thomson scattering and bremsstrahlung. We show that the effect δT/T can be ~ 10–5 in magnitude. We derive simple analytic expressions, which allow the redshifts, electron densities, and linear sizes of these regions to be estimated from observed spectral and spatial parame- ters. Additional observational methods for refining these parameters are outlined. © 2001 MAIK “Nauka/Inter- periodica”. Key words: theoretical and observational cosmology INTRODUCTION only two formation mechanisms of the “glow.” One of In the last 30 years, much attention has been given them is the Doppler distortion of external, equilibrium, to the search for and a detailed analysis of spatial fluc- and isotropic radiation (CMBR). For this to occur, the tuations in cosmic microwave background radiation object must have a peculiar velocity Vp and some non- zero opacity. -
And Ecclesiastical Cosmology
GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc. -
Radio Astronom1y G
£t,: ,/ NATIONAL RADIO ASTRONOMY OBSERVATORY QUARTERLY REPORT October 1 - December 31, 1989 RADIO ASTRONOM1Y G.. '8 tO- C~oe'' n,'evI! I E. Vi. t-Li 1 2 1990 TABLE OF CONTENTS A. TELESCOPE USAGE ... .... ...... ............ 1 B. 140-FOOT OBSERVING PROGRAMS . .... .......... ... 1 C. 12-METER TELESCOPE ....... ..... ., .... ........ 5 D. VERY LARGE ARRAY ....... 1...................8 E. SCIENTIFIC HIGHLIGHTS .... ........ 19 F. PUBLICATIONS ............. G. CENTRAL DEVELOPMENT LABORATORY ........ 20 H. GREEN BANK ELECTRONICS . .. .a.. ...... 21 I. 12-METER ELECTRONICS ...... .. 0. I. 22 J. VLA ELECTRONICS ...... 0..... ..... .... a. 24 K. AIPS .... .............. ...... ............. 26 L. VLA COMPUTER ............. .. .0. .0. ... 27 M. VERY LONG BASELINE ARRAY . .. .0 .0 .0 .0 .0 . .0 .. 27 N. PERSONNEL .. ...... .... .0.0 . .0. .0. .. e. 30 APPENDIX A: List of NRAO Preprints A. TELESCOPE USAGE The NRAO telescopes have been scheduled for research and maintenance in the following manner during the fourth quarter of 1989. 140-ft 12-m VLA Scheduled observing (hrs) 1901.75 1583.50 1565.2 Scheduled maintenance and equipment changes 132.00 107.75 259.8 Scheduled tests and calibrations 20.75 425.75 327.1 Time lost 139.25 208.25 107.0 Actual observing 1762.50 1375.25 1458.2 B. 140-FOOT OBSERVING PROGRAMS The following line programs were conducted during this quarter. No. Observer(s) Program A-95 Avery, L (Herzberg) Observations at 18.2, 18.6, and Bell, M. (Herzberg) 23.7 GHz of cyanopolyynes in carbon Feldman, P. (Herzberg) stars part II. MacLeod, J. (Herzberg) Matthews, H. (Herzberg) B-493 Bania, T. (Boston) Measurements at 8.666 GHz of 3He + Rood, R. (Virginia) emission in HII regions and planetary Wilson, T. -
Dark Matter Thermonuclear Supernova Ignition
MNRAS 000,1{21 (2019) Preprint 1 January 2020 Compiled using MNRAS LATEX style file v3.0 Dark Matter Thermonuclear Supernova Ignition Heinrich Steigerwald,1? Stefano Profumo,2 Davi Rodrigues,1 Valerio Marra1 1Center for Astrophysics and Cosmology (Cosmo-ufes) & Department of Physics, Federal University of Esp´ırito Santo, Vit´oria, ES, Brazil 2Department of Physics and Santa Cruz Institute for Particle Physics, 1156 High St, University of California, Santa Cruz, CA 95064, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT We investigate local environmental effects from dark matter (DM) on thermonuclear supernovae (SNe Ia) using publicly available archival data of 224 low-redshift events, in an attempt to shed light on the SN Ia progenitor systems. SNe Ia are explosions of carbon-oxygen (CO) white dwarfs (WDs) that have recently been shown to explode at sub-Chandrasekhar masses; the ignition mechanism remains, however, unknown. Recently, it has been shown that both weakly interacting massive particles (WIMPs) and macroscopic DM candidates such as primordial black holes (PBHs) are capable of triggering the ignition. Here, we present a method to estimate the DM density and velocity dispersion in the vicinity of SN Ia events and nearby WDs; we argue that (i) WIMP ignition is highly unlikely, and that (ii) DM in the form of PBHs distributed according to a (quasi-) log-normal mass distribution with peak log10¹m0/1gº = 24:9±0:9 and width σ = 3:3 ± 1:0 is consistent with SN Ia data, the nearby population of WDs and roughly consistent with other constraints from the literature. -
194 9 Ce Le B Rating 65 Ye Ars O F Br Inging As Tr on Omy T O No Rth Te X As 2
1949 Celebrating 65 Years of Bringing Astronomy to North Texas 2014 Contact information: Inside this issue: Info Officer (General Info) – [email protected] Website Administrator – [email protected] Page Postal Address: November Club Calendar 3 Fort Worth Astronomical Society Celestial Events 4 c/o Matt McCullar 5801 Trail Lake Drive Sky Chart 5 Fort Worth, TX 76133 Moon Phase Calendar 6 Web Site: http://www.fortworthastro.org Facebook: http://tinyurl.com/3eutb22 Lunar Occultations/Conjs 7 Twitter: http://twitter.com/ftwastro Yahoo! eGroup (members only): http://tinyurl.com/7qu5vkn Mercury/Venus Chart 8 Officers (2014-2015): Mars/Minor Planets Charts 9 President – Bruce Cowles, [email protected] Jupiter Charts 10 Vice President – Russ Boatwright, [email protected] Sec/Tres – Michelle Theisen, [email protected] Planet Vis & ISS Passes 11 Board Members: CSAC Event Update 12 2014-2016 Mike Langohr Young Astronomer News 12 Tree Oppermann ‘66 Leonids Remembered 13 2013-2015 Bill Nichols Cloudy Night Library 15 Jim Craft Cover Photo: Monthly AL Observing Club 17 Composite image taken by FWAS mem- bers: Left to right, from top to bottom— Constellation of the Month 18 Laura Cowles, Mike Ahner, Brian Wortham, Constellation Mythology 19 Shawn Kirchdorfer, Mark Wainright, Phil Stage, Patrick McMahon, Dennis Webb, Ben Prior Club Meeting Minutes 20 Hudgens, Shawn Kirchdorfer, John McCrea, and Chris Mlodnicki General Club Information 21 That’s A Fact 21 Observing Site Reminders: Be careful with fire, mind all local burn bans! Full Moon Name 21 Dark Site Usage Requirements (ALL MEMBERS): FWAS Foto Files 22 Maintain Dark-Sky Etiquette (http://tinyurl.com/75hjajy) Turn out your headlights at the gate! Sign the logbook (in camo-painted storage shed. -
Overview on Spectral Line Source Finding and Visualisation
CSIRO PUBLISHING Publications of the Astronomical Society of Australia, 2012, 29, 359–370 http://dx.doi.org/10.1071/AS12030 Overview on Spectral Line Source Finding and Visualisation B. S. Koribalski CSIRO Astronomy & Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia Email: [email protected] Abstract: Here I will outline successes and challenges for finding spectral line sources in large data cubes that are dominated by noise. This is a 3D challenge as the sources we wish to catalog are spread over several spatial pixels and spectral channels. While 2D searches can be applied, e.g. channel by channel, optimal searches take into account the 3-dimensional nature of the sources. In this overview I will focus on HI 21-cm spectral line source detection in extragalactic surveys, in particular HIPASS, the HI Parkes All-Sky Survey and WALLABY, the ASKAP HI All-Sky Survey. I use the original HIPASS data to highlight the diversity of spectral signatures of galaxies and gaseous clouds, both in emission and absorption. Among others, I report the À1 discovery of a 680 km s wide HI absorption trough in the megamaser galaxy NGC 5793. Issues such as source confusion and baseline ripples, typically encountered in single-dish HI surveys, are much reduced in interferometric HI surveys. Several large HI emission and absorption surveys are planned for the Australian Square Kilometre Array Pathfinder (ASKAP): here we focus on WALLABY, the 21-cm survey of the sky (d , þ308; z , 0.26) which will take about one year of observing time with ASKAP. -
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.