Andromeda - Daughter of Cassiopeia
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BRAS Newsletter August 2013
www.brastro.org August 2013 Next meeting Aug 12th 7:00PM at the HRPO Dark Site Observing Dates: Primary on Aug. 3rd, Secondary on Aug. 10th Photo credit: Saturn taken on 20” OGS + Orion Starshoot - Ben Toman 1 What's in this issue: PRESIDENT'S MESSAGE....................................................................................................................3 NOTES FROM THE VICE PRESIDENT ............................................................................................4 MESSAGE FROM THE HRPO …....................................................................................................5 MONTHLY OBSERVING NOTES ....................................................................................................6 OUTREACH CHAIRPERSON’S NOTES .........................................................................................13 MEMBERSHIP APPLICATION .......................................................................................................14 2 PRESIDENT'S MESSAGE Hi Everyone, I hope you’ve been having a great Summer so far and had luck beating the heat as much as possible. The weather sure hasn’t been cooperative for observing, though! First I have a pretty cool announcement. Thanks to the efforts of club member Walt Cooney, there are 5 newly named asteroids in the sky. (53256) Sinitiere - Named for former BRAS Treasurer Bob Sinitiere (74439) Brenden - Named for founding member Craig Brenden (85878) Guzik - Named for LSU professor T. Greg Guzik (101722) Pursell - Named for founding member Wally Pursell -
Observing List
day month year Epoch 2000 local clock time: 23.98 Observing List for 23 7 2019 RA DEC alt az Constellation object mag A mag B Separation description hr min deg min 20 50 Andromeda Gamma Andromedae (*266) 2.3 5.5 9.8 yellow & blue green double star 2 3.9 42 19 28 69 Andromeda Pi Andromedae 4.4 8.6 35.9 bright white & faint blue 0 36.9 33 43 30 55 Andromeda STF 79 (Struve) 6 7 7.8 bluish pair 1 0.1 44 42 16 52 Andromeda 59 Andromedae 6.5 7 16.6 neat pair, both greenish blue 2 10.9 39 2 45 67 Andromeda NGC 7662 (The Blue Snowball) planetary nebula, fairly bright & slightly elongated 23 25.9 42 32.1 31 60 Andromeda M31 (Andromeda Galaxy) large sprial arm galaxy like the Milky Way 0 42.7 41 16 31 61 Andromeda M32 satellite galaxy of Andromeda Galaxy 0 42.7 40 52 32 60 Andromeda M110 (NGC205) satellite galaxy of Andromeda Galaxy 0 40.4 41 41 17 55 Andromeda NGC752 large open cluster of 60 stars 1 57.8 37 41 17 48 Andromeda NGC891 edge on galaxy, needle-like in appearance 2 22.6 42 21 45 69 Andromeda NGC7640 elongated galaxy with mottled halo 23 22.1 40 51 46 57 Andromeda NGC7686 open cluster of 20 stars 23 30.2 49 8 30 121 Aquarius 55 Aquarii, Zeta 4.3 4.5 2.1 close, elegant pair of yellow stars 22 28.8 0 -1 12 120 Aquarius 94 Aquarii 5.3 7.3 12.7 pale rose & emerald 23 19.1 -13 28 32 152 Aquarius M72 globular cluster 20 53.5 -12 32 31 151 Aquarius M73 Y-shaped asterism of 4 stars 20 59 -12 38 16 117 Aquarius NGC7606 Galaxy 23 19.1 -8 29 32 149 Aquarius NGC7009 Saturn Neb planetary nebula, large & bright pale green oval 21 4.2 -11 21.8 38 135 -
INVESTIGATING ACTIVE GALACTIC NUCLEI with LOW FREQUENCY RADIO OBSERVATIONS By
INVESTIGATING ACTIVE GALACTIC NUCLEI WITH LOW FREQUENCY RADIO OBSERVATIONS by MATTHEW LAZELL A thesis submitted to The University of Birmingham for the degree of DOCTOR OF PHILOSOPHY School of Physics & Astronomy College of Engineering and Physical Sciences The University of Birmingham March 2015 University of Birmingham Research Archive e-theses repository This unpublished thesis/dissertation is copyright of the author and/or third parties. The intellectual property rights of the author or third parties in respect of this work are as defined by The Copyright Designs and Patents Act 1988 or as modified by any successor legislation. Any use made of information contained in this thesis/dissertation must be in accordance with that legislation and must be properly acknowledged. Further distribution or reproduction in any format is prohibited without the permission of the copyright holder. Abstract Low frequency radio astronomy allows us to look at some of the fainter and older synchrotron emission from the relativistic plasma associated with active galactic nuclei in galaxies and clusters. In this thesis, we use the Giant Metrewave Radio Telescope to explore the impact that active galactic nuclei have on their surroundings. We present deep, high quality, 150–610 MHz radio observations for a sample of fifteen predominantly cool-core galaxy clusters. We in- vestigate a selection of these in detail, uncovering interesting radio features and using our multi-frequency data to derive various radio properties. For well-known clusters such as MS0735, our low noise images enable us to see in improved detail the radio lobes working against the intracluster medium, whilst deriving the energies and timescales of this event. -
Constraining Gas Motions in the Intra-Cluster Medium
Noname manuscript No. (will be inserted by the editor) Constraining Gas Motions in the Intra-Cluster Medium Aurora Simionescu · John ZuHone · Irina Zhuravleva · Eugene Churazov · Massimo Gaspari · Daisuke Nagai · Norbert Werner · Elke Roediger · Rebecca Canning · Dominique Eckert · Liyi Gu · Frits Paerels Received: date / Accepted: date Aurora Simionescu SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands; E-mail: [email protected] Institute of Space and Astronautical Science (ISAS), JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210, Japan John ZuHone Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA Irina Zhuravleva Department of Astronomy & Astrophysics, University of Chicago, 5640 S Ellis Ave, Chicago, IL 60637, USA Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, 452 Lomita Mall, Stanford, CA 94305-4085, USA Department of Physics, Stanford University, 382 Via Pueblo Mall, Stanford, CA 94305-4085, USA Eugene Churazov Max Planck Institute for Astrophysics, Karl-Schwarzschild-Strasse 1, D-85741 Garching, Germany Space Research Institute (IKI), Profsoyuznaya 84/32, Moscow 117997, Russia Massimo Gaspari Einstein and Spitzer Fellow, Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, NJ 08544-1001, USA Daisuke Nagai Department of Physics, Yale University, PO Box 208101, New Haven, CT, USA Yale Center for Astronomy and Astrophysics, PO Box 208101, New Haven, CT, USA Norbert Werner MTA-E¨otv¨osLor´andUniversity Lend¨uletHot Universe Research Group, H-1117 P´azm´any P´eters´eta´ny1/A, Budapest, Hungary Department of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk Univer- sity, Kotl´arsk´a2, Brno, 61137, Czech Republic School of Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi-Hiroshima 739-8526, arXiv:1902.00024v1 [astro-ph.CO] 31 Jan 2019 Japan 2 Aurora Simionescu et al. -
Extra-Nuclear Starbursts: Young Luminous Hinge Clumps In
Extra-Nuclear Starbursts: Young Luminous Hinge Clumps in Interacting Galaxies Beverly J. Smith1, Roberto Soria2, Curtis Struck3, Mark L. Giroux1, Douglas A. Swartz4, and Mihoko Yukita5 ABSTRACT Hinge clumps are luminous knots of star formation near the base of tidal features in some interacting galaxies. We use archival Hubble Space Telescope UV/optical/IR images and Chandra X-ray maps along with GALEX UV, Spitzer IR, and ground-based optical/near-IR images to investigate the star forming properties in a sample of 12 hinge clumps in five interacting galaxies. 1 The most extreme of these hinge clumps have star formation rates of 1 9 M yr− , comparable to or larger than the ‘overlap’ region of intense star formation between− the⊙ two disks of the colliding galaxy system the Antennae. In the HST images, we have found remarkably large and luminous sources at the centers of these hinge clumps. These objects are much larger and more luminous than typical ‘super-star clusters’ in interacting galaxies, and are sometimes embedded in a linear ridge of fainter star clusters, consistent with star formation along a narrow caustic. These central sources have diameters of 70 pc, compared to 3 pc in ‘ordinary’ super-star clusters. ∼ ∼ Their absolute I magnitudes range from MI 12.2 to 16.5, thus if they are individual star clusters they would lie near the top of the ‘super∼ − star cluster’− luminosity function of star clusters. These sources may not be individual star clusters, but instead may be tightly packed groups of clusters that are blended together in the HST images. -
10. Scientific Programme 10.1
10. SCIENTIFIC PROGRAMME 10.1. OVERVIEW (a) Invited Discourses Plenary Hall B 18:00-19:30 ID1 “The Zoo of Galaxies” Karen Masters, University of Portsmouth, UK Monday, 20 August ID2 “Supernovae, the Accelerating Cosmos, and Dark Energy” Brian Schmidt, ANU, Australia Wednesday, 22 August ID3 “The Herschel View of Star Formation” Philippe André, CEA Saclay, France Wednesday, 29 August ID4 “Past, Present and Future of Chinese Astronomy” Cheng Fang, Nanjing University, China Nanjing Thursday, 30 August (b) Plenary Symposium Review Talks Plenary Hall B (B) 8:30-10:00 Or Rooms 309A+B (3) IAUS 288 Astrophysics from Antarctica John Storey (3) Mon. 20 IAUS 289 The Cosmic Distance Scale: Past, Present and Future Wendy Freedman (3) Mon. 27 IAUS 290 Probing General Relativity using Accreting Black Holes Andy Fabian (B) Wed. 22 IAUS 291 Pulsars are Cool – seriously Scott Ransom (3) Thu. 23 Magnetars: neutron stars with magnetic storms Nanda Rea (3) Thu. 23 Probing Gravitation with Pulsars Michael Kremer (3) Thu. 23 IAUS 292 From Gas to Stars over Cosmic Time Mordacai-Mark Mac Low (B) Tue. 21 IAUS 293 The Kepler Mission: NASA’s ExoEarth Census Natalie Batalha (3) Tue. 28 IAUS 294 The Origin and Evolution of Cosmic Magnetism Bryan Gaensler (B) Wed. 29 IAUS 295 Black Holes in Galaxies John Kormendy (B) Thu. 30 (c) Symposia - Week 1 IAUS 288 Astrophysics from Antartica IAUS 290 Accretion on all scales IAUS 291 Neutron Stars and Pulsars IAUS 292 Molecular gas, Dust, and Star Formation in Galaxies (d) Symposia –Week 2 IAUS 289 Advancing the Physics of Cosmic -
Chapter 1 Inventory of the Local Universe
Chapter 1 Inventory of the Local Universe 1 CHAPTER 1. INVENTORY OF THE LOCAL UNIVERSE 1.1 The major types of galaxies: Hubble-Sandage system Hubble-Sandage Tuning Fork: Kormendy & Bender, ApJ 464, L119 (1996), revised for ellipticals. Other classification schemes: e.g. de Vaucouleurs (1959), van den Bergh (1960/66), Yerkes (Morgan, 1957 ff) 2 CHAPTER 1. INVENTORY OF THE LOCAL UNIVERSE Primary classification criteria of commonly used Hubble-Sandage system: Bulge-to-disk ratio (S0/Sa: 5 to 0.3, Sb: 1 to 0.1, Sc/Irr: 0.2 to 0) Opening angle of spiral arms (Sa: 0 to 10, Sb: 5 to 20, Sc: 10 to 30 degrees) Bars Physical parameters varying along the Hubble-Sandage system: Stellar mass M increases from irregulars (108M ) to ellipticals (1012M ) Specific Angular Momentum J=M of baryons increases from ellipticals to spirals Mean age increases from irregulars through spirals to ellipticals (B-V increases from 0.3 to 1.0, mass-to-light M=LB ratio increases from about 2 to 10) Mean stellar density of spheroids increases with decreasing spheroid luminosity Mean surface brightness of disks increases with luminosity cold gas content increases along Hubble sequence (fraction of baryonic mass: 0 in E/S0, 0.1 to 0.3 in Sa to Sc, up to 0.9 in Irr) hot gas content only significant in massive E (few percent of baryonic mass) 3 CHAPTER 1. INVENTORY OF THE LOCAL UNIVERSE Examples for Normal Galaxies: Elliptical (E) Galaxies: The ellipticals M 84 (right) and M 86 (middle) in the Virgo cluster (NOAO). -
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. -
Measuring the Scatter in the Cluster Optical Richness-Mass Relation with Machine Learning
MEASURING THE SCATTER IN THE CLUSTER OPTICAL RICHNESS-MASS RELATION WITH MACHINE LEARNING A Dissertation by STEVEN ALVARO BOADA Submitted to the Office of Graduate and Professional Studies of Texas A&M University in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY Chair of Committee, Casey J. Papovich Committee Members, Wolfgang Bangerth Louis Strigari Nicholas Suntzeff Head of Department, Peter McIntyre August 2016 Major Subject: Physics Copyright 2016 Steven Alvaro Boada ABSTRACT The distribution of massive clusters of galaxies depends strongly on the total cos- mic mass density, the mass variance, and the dark energy equation of state. As such, measures of galaxy clusters can provide constraints on these parameters and even test models of gravity, but only if observations of clusters can lead to accurate estimates of their total masses. Here, we carry out a study to investigate the ability of a blind spectroscopic survey to recover accurate galaxy cluster masses through their line- of-sight velocity dispersions (LOSVD) using probability based and machine learning methods. We focus on the Hobby Eberly Telescope Dark Energy Experiment (HET- DEX), which will employ new Visible Integral-Field Replicable Unit Spectrographs (VIRUS), over 420 degree2 on the sky with a 1/4.5 fill factor. VIRUS covers the blue/optical portion of the spectrum (3500 − 5500 A),˚ allowing surveys to measure redshifts for a large sample of galaxies out to z < 0:5 based on their absorption or emission (e.g., [O II], Mg II, Ne V) features. We use a detailed mock galaxy catalog from a semi-analytic model to simulate surveys observed with VIRUS, including: (1) Survey, a blind, HETDEX-like survey with an incomplete but uniform spectroscopic selection function; and (2) Targeted, a survey which targets clusters directly, ob- taining spectra of all galaxies in a VIRUS-sized field. -
Nov-EH-SAS.Pdf
▲ In the News - 21/Borisov Dark Matter - First All Female Space Walk SAS Facebook Page Astro Quiz - comets Members’ Gallery For Sale - 12” Meade AFC - Glenn Burgess Sky Map - November Southern Astronomical Society - Brisbane South - Logan -Gold Coast - Tweed Heads - www.sas.org.au ▲ From the Editor’s Desk 2 Welcome to the November edition of Event Horizon. Meetings: There’ll be supper available ($1per serve) from 6:30pm prior to the meeting at 7:30pm. Tea & coffee is provided free of charge. In the News: Comet 21/Borisov Dark Matters: First All Female Space Walk Astronomy 2020 Australia: Now available for purchase at the next meeting for $22 each. Normally $29 elsewhere. Please bring the right CONTENTS money. 3 About SAS Members’ Gallery: Ray Suckling, Klaus Schlussler, Tony Kim, John McLennan, Mark Boothman, David Bainbridge, Noeleen Lowndes, Mike Geisel, Greg Bock. 4 Presidential Musings For Sale: Glenn Burgess has a great Meade telescope for sale. 5 In the News: Comet 21/Borisov Free download: Beyond Earth: A Chronicle of Deep Space Exploration 7 Dark Matters: First All Female Space Walk Astro Quiz: This month, it’s all about comets. 8 SAS Facebook Page news World science Festival - https://www.worldsciencefestival.com/video/video-library/ 9 Astro Quiz November - comets Get the latest videos on all sorts of science including the wide and varied field of astronomy. 10 Members’ Gallery SAS club t-shirt - Pricing has been sourced for new SAS polo shirts and beanies. Details at the meeting. Interested? - please see Brendan Junge. 21 For Sale - Glenn Burgess Tracy Travis. -
Disk Mass and Disk Heating in the Spiral Galaxy NGC 3223?
A&A 576, A57 (2015) Astronomy DOI: 10.1051/0004-6361/201425279 & c ESO 2015 Astrophysics Disk mass and disk heating in the spiral galaxy NGC 3223? G. Gentile1;2, C. Tydtgat1;3, M. Baes1, G. De Geyter1, M. Koleva1, G. W. Angus2, W. J. G. de Blok4;5;6, W. Saftly1, and S. Viaene1 1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281, 9000 Gent, Belgium e-mail: [email protected] 2 Department of Physics and Astrophysics, Vrije Universiteit Brussel, Pleinlaan 2, 1050 Brussels, Belgium 3 Department of Solid State Sciences, Krijgslaan 281, 9000 Gent, Belgium 4 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands 5 Astrophysics, Cosmology and Gravity Centre, Department of Astronomy, University of Cape Town, Private Bag X3, 7701 Rondebosch, South Africa 6 Kapteyn Astronomical Institute, University of Groningen, PO Box 800, 9700 AV Groningen, The Netherlands Received 5 November 2014 / Accepted 11 February 2015 ABSTRACT We present the stellar and gaseous kinematics of an Sb galaxy, NGC 3223, with the aim of determining the vertical and radial stellar velocity dispersion as a function of radius, which can help to constrain disk heating theories. Together with the observed NIR photometry, the vertical velocity dispersion is also used to determine the stellar mass-to-light (M=L) ratio, typically one of the largest uncertainties when deriving the dark matter distribution from the observed rotation curve. We find a vertical-to-radial velocity dispersion ratio of σz/σR = 1:21 ± 0:14, significantly higher than expectations from known correlations, and a weakly-constrained Ks-band stellar M=L ratio in the range 0.5–1.7, which is at the high end of (but consistent with) the predictions of stellar population synthesis models. -
A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques.