XUV-DISK) GALAXIES in the LOCAL UNIVERSE David A
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
May, 2021 President: Andrew Edelen 618-457-3331 Secretary
MAY 2021 IO Io May, 2021 PO Box 591 Lowell, OR 97452 www.eugeneastro.org [1] M51 - The Whirlpool Galaxy and NGC 5195 Companion Mark Wetzel President: Andrew Edelen 618-457-3331 Secretary: Randy Beiderwell 541-342-4686 Board Members: Oggie Golub, Randy Beiderwell, Ken Martin, Jerry Oltion 1 MAY 2021 IO May Meeting - Thursday, May 20 7pm PLEASE NOTE THAT ALL MEETINGS ARE CURRENTLY VIRTUAL To Be Announced April Meeting We had a special double meeting this month with two short programs by Alan Gillespie and Bernie Bopp. Alan Gillespie gave a talk, "My Lunacy," about several alternative techniques that he has been using to process lunar images. After that, Bernie Bopp spoke on "Solar Nucleosynthesis, or How Does the Sun Work, Anyway?” https://youtu.be/oFqIQDeZdYs Lunar Eclipse The only Total Lunar Eclipse of 2021 will occur during the morning twilight on Wednesday May 26. Totality will only last about 18 minutes as the moon barely cruises through the edge of the Earths Umbra. This means that one limb of the Moon will be noticeably brighter than the opposite edge. Furthermore the eclipse will be happening as the sky is getting brighter from the morning dawn. However the Moon will be interestingly positioned 6 degrees West of Antares. So somebody somewhere is going to get a nice picture! Here are some times and positions: Wednesday May 26,2021 Azimuth altitude 2:45 Partial Eclipse Begins 204 20 3:23 Astronomical Twilight Begins 213 17 4:10 Totality Begins 222 12 4:16 Nautical Twilight Begins 224 11 4:19 Mid-Totality 224 11 4:28 Totality Ends 226 10 5:01 Civil Twilight Begins 232 5 5:35 Sunrise 238 1 5:45 Moonset 239 0 5:53 Partial Eclipse Ends Alan Gillespie 2 MAY 2021 IO [2] Heart Nebula Ronald Perez Do you have something for the newsletter? If you have an article, photo, meeting notes, stories, etc. -
Observing Galaxies in Lynx 01 October 2015 22:25
Observing galaxies in Lynx 01 October 2015 22:25 Context As you look towards Lynx you are looking above the galactic plane above the Perseus spiral arm of our galaxy which itself is about 7,000 light years away. The constellation contains a number of brighter galaxies 30 - 50 million light years away and is also relatively rich in galaxies which spread out in to the distance out to over 300 million light years away. The constellation is well placed from early winter to early summer. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 2683 This is a very edge on bright galaxy which I can see in my 100mm binoculars. It is a galaxy which does not seem to be part of a group. NGC 2549 By constellation Page 1 A smaller fainter version of NGC 2683. It was still easy to see with direct vision in my 10 inch reflector. NGC 2537 Near a group of three stars in a row. Quite large looking but with a low surface brightness in my 10 inch scope. NGC 2273 By constellation Page 2 Nice circular galaxy in my 14 inch scope. I could only see the bright core in the above image. NGC 2832 This was a lovely looking galaxy in my 14 inch Dark star scope. As you can see this galaxy is the central galaxy of a group. -
THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B
The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M . -
Spiral Galaxy HI Models, Rotation Curves and Kinematic Classifications
Spiral galaxy HI models, rotation curves and kinematic classifications Theresa B. V. Wiegert A thesis submitted to the Faculty of Graduate Studies of The University of Manitoba in partial fulfillment of the requirements of the degree of Doctor of Philosophy Department of Physics & Astronomy University of Manitoba Winnipeg, Canada 2010 Copyright (c) 2010 by Theresa B. V. Wiegert Abstract Although galaxy interactions cause dramatic changes, galaxies also continue to form stars and evolve when they are isolated. The dark matter (DM) halo may influence this evolu- tion since it generates the rotational behaviour of galactic disks which could affect local conditions in the gas. Therefore we study neutral hydrogen kinematics of non-interacting, nearby spiral galaxies, characterising their rotation curves (RC) which probe the DM halo; delineating kinematic classes of galaxies; and investigating relations between these classes and galaxy properties such as disk size and star formation rate (SFR). To generate the RCs, we use GalAPAGOS (by J. Fiege). My role was to test and help drive the development of this software, which employs a powerful genetic algorithm, con- straining 23 parameters while using the full 3D data cube as input. The RC is here simply described by a tanh-based function which adequately traces the global RC behaviour. Ex- tensive testing on artificial galaxies show that the kinematic properties of galaxies with inclination > 40 ◦, including edge-on galaxies, are found reliably. Using a hierarchical clustering algorithm on parametrised RCs from 79 galaxies culled from literature generates a preliminary scheme consisting of five classes. These are based on three parameters: maximum rotational velocity, turnover radius and outer slope of the RC. -
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 -
The Saga of M81: Global View of a Massive Stellar Halo in Formation
Draft version October 27, 2020 Typeset using LATEX twocolumn style in AASTeX63 The Saga of M81: Global View of a Massive Stellar Halo in Formation Adam Smercina ,1, 2 Eric F. Bell ,1 Paul A. Price,3 Colin T. Slater ,2 Richard D'Souza,1, 4 Jeremy Bailin ,5 Roelof S. de Jong ,6 In Sung Jang ,6 Antonela Monachesi ,7, 8 and David Nidever 9, 10 1Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA 2Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195-1580, USA 3Department of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USA 4Vatican Observatory, Specola Vaticana, V-00120, Vatican City State 5Department of Physics and Astronomy, University of Alabama, Box 870324, Tuscaloosa, AL 35487-0324, USA 6Leibniz-Institut f¨urAstrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 7Instituto de Investigaci´onMultidisciplinar en Ciencia y Tecnolog´ıa,Universidad de La Serena, Ra´ulBitr´an1305, La Serena, Chile 8Departamento de F´ısica y Astronom´ıa,Universidad de La Serena, Av. Juan Cisternas 1200 N, La Serena, Chile 9Department of Physics, Montana State University, P.O. Box 173840, Bozeman, MT 59717-3840 10National Optical Astronomy Observatory, 950 North Cherry Ave, Tucson, AZ 85719 (Received 31 October, 2019; Revised 31 August, 2020; Accepted 23 October, 2020) Submitted to The Astrophysical Journal ABSTRACT Recent work has shown that Milky Way-mass galaxies display an incredible range of stellar halo properties, yet the origin of this diversity is unclear. The nearby galaxy M81 | currently interacting with M82 and NGC 3077 | sheds unique light on this problem. -
NEUTRAL HYDROGEN CLOUDS in the M81/M82 GROUP KM Chynoweth
University of Massachusetts Amherst ScholarWorks@UMass Amherst Astronomy Department Faculty Publication Series Astronomy 2008 NEUTRAL HYDROGEN CLOUDS IN THE M81/M82 GROUP KM Chynoweth GI Langston Min Yun University of Massachusetts - Amherst FJ Lockman KHR Rubin See next page for additional authors Follow this and additional works at: https://scholarworks.umass.edu/astro_faculty_pubs Part of the Astrophysics and Astronomy Commons Recommended Citation Chynoweth, KM; Langston, GI; Yun, Min; Lockman, FJ; Rubin, KHR; and Scoles, SA, "NEUTRAL HYDROGEN CLOUDS IN THE M81/M82 GROUP" (2008). The Astrophysical Journal. 1129. 10.1088/0004-6256/135/6/1983 This Article is brought to you for free and open access by the Astronomy at ScholarWorks@UMass Amherst. It has been accepted for inclusion in Astronomy Department Faculty Publication Series by an authorized administrator of ScholarWorks@UMass Amherst. For more information, please contact [email protected]. Authors KM Chynoweth, GI Langston, Min Yun, FJ Lockman, KHR Rubin, and SA Scoles This article is available at ScholarWorks@UMass Amherst: https://scholarworks.umass.edu/astro_faculty_pubs/1129 Neutral Hydrogen Clouds in the M81/M82 Group Katie M. Chynoweth1 Vanderbilt University, Physics and Astronomy Department, 1807 Station B, Nashville, TN 37235 Glen I. Langston National Radio Astronomy Observatory, Green Bank, WV 24944 Min S. Yun University of Massachusetts, 710 North Pleasant Street, Amherst, MA 01002 Felix J. Lockman, K.H.R. Rubin2 and Sarah A. Scoles3 National Radio Astronomy Observatory, Green Bank, WV 24944 ABSTRACT We have observed a 3◦ ×3◦ area centered on the M81/M82 group of galaxies using the Robert C. Byrd Green Bank Telescope (GBT) in a search for analogs to the High Velocity Clouds (HVCs) of neutral hydrogen found around our galaxy. -
Astronomy Magazine Special Issue
γ ι ζ γ δ α κ β κ ε γ β ρ ε ζ υ α φ ψ ω χ α π χ φ γ ω ο ι δ κ α ξ υ λ τ μ β α σ θ ε β σ δ γ ψ λ ω σ η ν θ Aι must-have for all stargazers η δ μ NEW EDITION! ζ λ β ε η κ NGC 6664 NGC 6539 ε τ μ NGC 6712 α υ δ ζ M26 ν NGC 6649 ψ Struve 2325 ζ ξ ATLAS χ α NGC 6604 ξ ο ν ν SCUTUM M16 of the γ SERP β NGC 6605 γ V450 ξ η υ η NGC 6645 M17 φ θ M18 ζ ρ ρ1 π Barnard 92 ο χ σ M25 M24 STARS M23 ν β κ All-in-one introduction ALL NEW MAPS WITH: to the night sky 42,000 more stars (87,000 plotted down to magnitude 8.5) AND 150+ more deep-sky objects (more than 1,200 total) The Eagle Nebula (M16) combines a dark nebula and a star cluster. In 100+ this intense region of star formation, “pillars” form at the boundaries spectacular between hot and cold gas. You’ll find this object on Map 14, a celestial portion of which lies above. photos PLUS: How to observe star clusters, nebulae, and galaxies AS2-CV0610.indd 1 6/10/10 4:17 PM NEW EDITION! AtlAs Tour the night sky of the The staff of Astronomy magazine decided to This atlas presents produce its first star atlas in 2006. -
Strong Evidence for the Density-Wave Theory of Spiral Structure from a Multi-Wavelength Study of Disk Galaxies Hamed Pour-Imani University of Arkansas, Fayetteville
University of Arkansas, Fayetteville ScholarWorks@UARK Theses and Dissertations 8-2018 Strong Evidence for the Density-wave Theory of Spiral Structure from a Multi-wavelength Study of Disk Galaxies Hamed Pour-Imani University of Arkansas, Fayetteville Follow this and additional works at: http://scholarworks.uark.edu/etd Part of the Physical Processes Commons, and the Stars, Interstellar Medium and the Galaxy Commons Recommended Citation Pour-Imani, Hamed, "Strong Evidence for the Density-wave Theory of Spiral Structure from a Multi-wavelength Study of Disk Galaxies" (2018). Theses and Dissertations. 2864. http://scholarworks.uark.edu/etd/2864 This Dissertation is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. Strong Evidence for the Density-wave Theory of Spiral Structure from a Multi-wavelength Study of Disk Galaxies A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics by Hamed Pour-Imani University of Isfahan Bachelor of Science in Physics, 2004 University of Arkansas Master of Science in Physics, 2016 August 2018 University of Arkansas This dissertation is approved for recommendation to the Graduate Council. Daniel Kennefick, Ph.D. Dissertation Director Vincent Chevrier, Ph.D. Claud Lacy, Ph.D. Committee Member Committee Member Julia Kennefick, Ph.D. William Oliver, Ph.D. Committee Member Committee Member ABSTRACT The density-wave theory of spiral structure, though first proposed as long ago as the mid-1960s by C.C. -
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. -
NGC 6872 in the Constellation of Pavo 23 September 2014
Image: NGC 6872 in the constellation of Pavo 23 September 2014 of free hydrogen, which is the basis material for new stars, meaning that if it weren't for its interactions with IC 4970, NGC 6872 might not have been able to produce new bursts of star formation. Provided by NASA Credit: ESA/Hubble & NASA / Acknowledgement: Judy Schmidt This picture, taken by the NASA/ESA Hubble Space Telescope's Wide Field Planetary Camera 2 (WFPC2), shows a galaxy known as NGC 6872 in the constellation of Pavo (The Peacock). Its unusual shape is caused by its interactions with the smaller galaxy that can be seen just above NGC 6872, called IC 4970. They both lie roughly 300 million light-years away from Earth. From tip to tip, NGC 6872 measures over 500,000 light-years across, making it the second largest spiral galaxy discovered to date. In terms of size it is beaten only by NGC 262, a galaxy that measures a mind-boggling 1.3 million light-years in diameter! To put that into perspective, our own galaxy, the Milky Way, measures between 100,000 and 120,000 light-years across, making NGC 6872 about five times its size. The upper left spiral arm of NGC 6872 is visibly distorted and is populated by star-forming regions, which appear blue on this image. This may have been be caused by IC 4970 recently passing through this arm—although here, recent means 130 million years ago! Astronomers have noted that NGC 6872 seems to be relatively sparse in terms 1 / 2 APA citation: Image: NGC 6872 in the constellation of Pavo (2014, September 23) retrieved 23 September 2021 from https://phys.org/news/2014-09-image-ngc-constellation-pavo.html This document is subject to copyright. -
Cold Gas Accretion in Galaxies
Astron Astrophys Rev (2008) 15:189–223 DOI 10.1007/s00159-008-0010-0 REVIEW ARTICLE Cold gas accretion in galaxies Renzo Sancisi · Filippo Fraternali · Tom Oosterloo · Thijs van der Hulst Received: 28 January 2008 / Published online: 17 April 2008 © The Author(s) 2008 Abstract Evidence for the accretion of cold gas in galaxies has been rapidly accumulating in the past years. H I observations of galaxies and their environment have brought to light new facts and phenomena which are evidence of ongoing or recent accretion: (1) A large number of galaxies are accompanied by gas-rich dwarfs or are surrounded by H I cloud complexes, tails and filaments. This suggests ongoing minor mergers and recent arrival of external gas. It may be regarded, therefore, as direct evidence of cold gas accretion in the local universe. It is probably the same kind of phenomenon of material infall as the stellar streams observed in the halos of our galaxy and M 31. (2) Considerable amounts of extra-planar H I have been found in nearby spiral galaxies. While a large fraction of this gas is undoubtedly produced by galactic fountains, it is likely that a part of it is of extragalactic origin. Also the Milky Way has extra-planar gas complexes: the Intermediate- and High-Velocity Clouds (IVCs and HVCs). (3) Spirals are known to have extended and warped outer layers of H I. It is not clear how these have formed, and how and for how long the warps can R. Sancisi (B) Osservatorio Astronomico di Bologna, Via Ranzani 1, 40127 Bologna, Italy e-mail: [email protected] R.