Sirius Astronomer) Or Editor Don Saito, [email protected]

Total Page:16

File Type:pdf, Size:1020Kb

Sirius Astronomer) Or Editor Don Saito, Donsaito@Yahoo.Com April 2015 Free to members, subscriptions $12 for 12 issues Volume 42, Number 4 NASA’s Dawn spacecraft arrived at dwarf planet Ceres on March 6, revealing the surface of the larg- est unexplored body in the inner Solar System for the first time. These images were taken from 40,000 kilometers (25,000 miles) from Ceres on February 25th. Over the course of the next year we will learn much more about this fascinating and important member of our solar system! (Image credit: NASA/JPL-Caltech/UCLA/MPS/DLR/IDA) OCA CLUB MEETING STAR PARTIES COMING UP The free and open club meeng will The Black Star Canyon site will open on The next session of the Beginners be held April 10 at 7:30 PM in the Ir‐ April 11. The Anza site will be open on April Class will be held at the Heritage Mu‐ vine Lecture Hall of the Hashinger Sci‐ 18 Members are encouraged to check the seum of Orange County at 3101 West ence Center at Chapman University in website calendar for the latest updates on Harvard Street in Santa Ana on April Orange. This month’s speaker is Dr. star pares and other events. 3. The following class will be held Brendan Bowler of Caltech, who will May 1. discuss Imaging Extrasolar Planets. Please check the website calendar for the outreach events this month! Volunteers are GOTO SIG: TBA NEXT MEETINGS: May 8, June 12 always welcome! Astro‐Imagers SIG: Apr. 14, May 12 Remote Telescopes: TBA You are also reminded to check the web Astrophysics SIG: Apr. 17, May 15 site frequently for updates to the calendar Dark Sky Group: TBA of events and other club news. The Cold Never Bothered Me Anyway By Ethan Siegel For those of us in the northern hemisphere, winter brings long, cold nights, which are often excellent for sky watchers (so long as there's a way to keep warm!) But there's often an add- ed bonus that comes along when conditions are just right: the polar lights, or the Aurora Borealis around the North Pole. Here on our world, a brilliant green light often appears for observers at high northern latitudes, with occasional, dimmer reds and even blues lighting up a clear night. We had always assumed that there was some connection be- tween particles emitted from the Sun and the aurorae, as par- ticularly intense displays were observed around three days after a solar storm occurred in the direction of Earth. Presuma- bly, particles originating from the Sun—ionized electrons and atomic nuclei like protons and alpha particles—make up the vast majority of the solar wind and get funneled by the Earth's magnetic field into a circle around its magnetic poles. They're energetic enough to knock electrons off atoms and molecules at various layers in the upper atmosphere—particles like mo- lecular nitrogen, oxygen and atomic hydrogen. And when the Auroral overlays from the IMAGE spacecraft. Image credit: electrons fall back either onto the atoms or to lower energy NASA Earth Observatory (Goddard Space Flight Center) / levels, they emit light of varying but particular wavelengths— Blue Marble team. oxygen producing the most common green signature, with less common states of oxygen and hydrogen producing red and the occasional blue from nitrogen. But it wasn't until the 2000s that this picture was directly confirmed! NASA's Imager for Magnetopause-to-Aurora Global Ex- ploration (IMAGE) satellite (which ceased operations in December 2005) was able to find out how the magnetosphere responded to solar wind changes, how the plasmas were energized, transported and (in some cases) lost, and many more properties of our magnetosphere. Planets without significant magnetic fields such as Venus and Mars have much smaller, weaker aurorae than we do, and gas giant planets like Saturn have aurorae that primarily shine in the ultraviolet rather than the visible. Nevertheless, the aurorae are a spectacular sight in the evening, particularly for observers in Alaska, Canada and the Scandinavian countries. But when a solar storm comes our way, keep your eyes towards the north at night; the views will be well worth braving the cold! 2 Western Amateur Astronomers Board Meeting Notes by Tim Hogle, WAA Vice President and OCA Representative Once again I would like to report on the activities of the WAA over the last year or so. We had a very productive board meeting on February 7, this time at the Chabot Space and Science Center and Observatory overlooking Oakland and the SF Bay Area. As you will recall, WAA is an umbrella organization whose members are astronomy clubs. It exists for the main purpose of collaboration between member clubs, promoting amateur astronomy, providing awards to individuals for outstanding contribution to the hobby, and hosting or sponsoring the occasional astronomy conference. Eight member clubs were represented at this meeting, including one, Tri-Valley Stargazers (based in Stockton), which has not been active in WAA for many years. We welcome them back. The other clubs, OCA, Los Angeles Astronomical Society, Mt. Diablo Astro- nomical Society and Mt. Diablo Observatory Association, China Peak Astronomical Society, East Bay Astronomical Society, and Chabot Telescope Makers’ Workshop are regulars at this winter meeting. WAA’s most noteworthy regular action at the winter meetings is selection of a recipient for the highly prestigious G. Bruce Blair award, given to a living individual who has made outstanding contributions to amateur astronomy. This year’s award is to be present- ed to Timothy J. Thompson, a retired JPL scientist and president emeritus of LAAS who is being so honored, not only for his four dec- ades of service to LAAS, but for initiation of the docent training program at Mt. Wilson Observatory, leading public outreach there and at Griffith Observatory for many years, as a prolific speaker for astronomy clubs, civic groups, and private functions, both as an ama- teur astronomer and JPL space scientist. As in the last several years, the award will be presented at the Riverside Telescope Makers conference on Memorial Day weekend. The Blair medal itself is quite an involved production effort, which has been done personally by former WAA president Jack Borde. This task, which involves deep chemical etching on a bronze plate using an AutoCad digitized rendering of the original artwork, cut- ting out the medal itself from the plate, lathe turning, edge knurling, engraving with the recipient’s name and finally being gold plated and presented in a hand-crafted wood display case. This task has now been turned over to the Telescope Makers’ Workshop, which has a combination of professional contacts and in-house expertise for all but production of the case. Any woodworkers out there in- terested in donating some time to this last task? Let me know. Two new issues of our New Pacific Stargazer newsletter were issued during this last year. The goal of quarterly issues was not possi- ble, but the semiannual publication has worked well. The Fall 2014 and all other issues can be found from links at the WAA’s web site, http://www.waa.av.org.. We are still looking for material for publication in future issues and are happy to accept articles of as- tronomical interest from individual club members. Contact me (see back page of the Sirius Astronomer) or editor Don Saito, [email protected]. Republication from other sources, such as this one, is okay as well, and will reach a more geographically wide audience. Speaking of which, the SA could really benefit from additional material from OCA members. This august publication is rou- tinely dominated by only a few repeating authors, and would be of greatly enhanced benefit to members with the addition of material from the rest of you. Surely in a club of nearly 800 members there are a few thoughts, personal projects, ideas, insights or reports from astronomically-related trips that could be offered from this audience. Give it some thought and send something in. But I digress. Another continuing effort within WAA is to get a new, updated web page on line. I can’t offer excuses why this has taken so long (at least two years in the works), but I can say we have universal agreement on getting this launched as soon as possi- ble, hopefully before RTMC. WAA will have an information booth at RTMC again this year, probably near the snack bar. Stop by and say hello. For more info about WAA, log on to the web site. 3 AstroSpace Update April 2015 Gathered by Don Lynn from NASA and other sources Solar System visitor – Astronomers have measured the motion of a nearby star and found that it passed through the Oort Cloud of comets that surrounds our Solar System just 70,000 years ago. The star, known as Scholz’s Star, is now 20 light-years away, but at closest approach it was 0.8 light-years. The star is a small dim red dwarf star, so was only about magnitude 11 when nearest. The star has a binary companion, which is a brown dwarf that is even dimmer. There seems to be no evidence that the close passage disturbed the Oort Cloud enough to cause a noticeable increase in comets. Unusual exoplanet – Astronomers have discovered an unusual planet in Kepler (planet finding space telescope) data, which has an elongated orbit. This causes its temperature to change dramatically during each orbit. Its year is 52 Earth days, and during this time the temperature ranges from 900-1800°F (500-1000°C). The planet, dubbed Kepler-432b, is one of the densest and most massive planets known.
Recommended publications
  • 12 Strong Gravitational Lenses
    12 Strong Gravitational Lenses Phil Marshall, MaruˇsaBradaˇc,George Chartas, Gregory Dobler, Ard´ısEl´ıasd´ottir,´ Emilio Falco, Chris Fassnacht, James Jee, Charles Keeton, Masamune Oguri, Anthony Tyson LSST will contain more strong gravitational lensing events than any other survey preceding it, and will monitor them all at a cadence of a few days to a few weeks. Concurrent space-based optical or perhaps ground-based surveys may provide higher resolution imaging: the biggest advances in strong lensing science made with LSST will be in those areas that benefit most from the large volume and the high accuracy, multi-filter time series. In this chapter we propose an array of science projects that fit this bill. We first provide a brief introduction to the basic physics of gravitational lensing, focusing on the formation of multiple images: the strong lensing regime. Further description of lensing phenomena will be provided as they arise throughout the chapter. We then make some predictions for the properties of samples of lenses of various kinds we can expect to discover with LSST: their numbers and distributions in redshift, image separation, and so on. This is important, since the principal step forward provided by LSST will be one of lens sample size, and the extent to which new lensing science projects will be enabled depends very much on the samples generated. From § 12.3 onwards we introduce the proposed LSST science projects. This is by no means an exhaustive list, but should serve as a good starting point for investigators looking to exploit the strong lensing phenomenon with LSST.
    [Show full text]
  • Magellanic Type Galaxies Throughout the Universe Eric M
    The Magellanic System: Stars, Gas, and Galaxies Proceedings IAU Symposium No. 256, 2008 c 2009 International Astronomical Union Jacco Th. van Loon & Joana M. Oliveira, eds. doi:10.1017/S1743921308028871 Magellanic type galaxies throughout the Universe Eric M. Wilcots Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53706 USA email: [email protected] Abstract. The Magellanic Clouds are often characterized as “irregular” galaxies, a term that implies an overall lack of organized structure. While this may be a fitting description of the Small Cloud, the Large Magellanic Cloud, contrary to popular opinion, should not be considered an irregular galaxy. It is characterized by a distinctive morphology of having an offset stellar bar and single spiral arm. Such morphology is relatively common in galaxies of similar mass throughout the local Universe, although explaining the origin of these features has proven challenging. Through a number of recent studies we are beginning to get a better grasp on what it means to be a Magellanic spiral. One key result of these works is that we now recognize that the most unique aspect of the Magellanic Clouds is not their structure, but, rather, their proximity to a larger spiral such as the Milky Way. Keywords. galaxies: dwarf, galaxies: evolution, galaxies: interactions, Magellanic Clouds, galax- ies: structure 1. Introduction While the Small Magellanic Cloud can properly be thought of as an irregular galaxy, the Large Magellanic Cloud shares a number of key morphological properties with a population of galaxies classified as Barred Magellanic Spirals (SBm). These properties include a stellar bar, the center of which may or may not be coincident with the dynamical center of the galaxy, a single, looping spiral arm, and often a large star-forming complex at one end of the bar.
    [Show full text]
  • Arxiv:Astro-Ph/0407438V1 20 Jul 2004
    The Nature of Nearby Counterparts to Intermediate Redshift Luminous Compact Blue Galaxies I. Optical/H I Properties and Dynamical Masses C. A. Garland1 Institute for Astronomy, University of Hawai‘i, 2680 Woodlawn Drive, Honolulu, HI 96822 [email protected] D. J. Pisano2 CSIRO Australia Telescope National Facility, P.O. Box 76, Epping, NSW 1710, Australia [email protected] J. P. Williams Institute for Astronomy, University of Hawai‘i, 2680 Woodlawn Drive, Honolulu, HI 96822 [email protected] R. Guzm´an Department of Astronomy, University of Florida, 211 Bryant Space Science Center, P.O. Box 112055, Gainesville, FL 32611-2055 [email protected] arXiv:astro-ph/0407438v1 20 Jul 2004 and F. J. Castander Institut d’Estudis Espacials De Catalunya/CSIC, Gran Capit`a2-4, E-08034 Barcelona, Spain [email protected] ABSTRACT 1Present address: Natural Sciences Department, Castleton State College, Castleton, VT 05735 2Bolton Fellow & NSF MPS Distinguished International Postdoctoral Research Fellow –2– We present single-dish H I spectra obtained with the Green Bank Telescope, along with optical photometric properties from the Sloan Digital Sky Survey, of 20 nearby (D . 70 Mpc) Luminous Compact Blue Galaxies (LCBGs). These ∼L⋆, blue, high surface brightness, starbursting galaxies were selected with the same criteria used to define LCBGs at higher redshifts. We find these galaxies 8 9 −1 are gas-rich, with MHI ranging from 5×10 to 8×10 M⊙, and MHI LB ranging −1 from 0.2 to 2 M⊙ L⊙ , consistent with a variety of morphological types of galax- ies. We find the dynamical masses (measured within R25) span a wide range, 9 11 from 3×10 to 1×10 M⊙.
    [Show full text]
  • Ultra-Luminous X-Ray Sources in Nearby Galaxies from ROSAT HRI Observations I. Data Analysis
    Submitted to ApJ Supplement Ultra-luminous X-ray Sources in nearby galaxies from ROSAT HRI observations I. data analysis Ji-Feng Liu and Joel N. Bregman Astronomy Department, University of Michigan, MI 48109 ABSTRACT X-ray observations have revealed in other galaxies a class of extra-nuclear X-ray point sources with X-ray luminosities of 1039–1041 erg/sec, exceeding the Eddington luminosity for stellar mass X-ray binaries. These ultra-luminous X- ray sources (ULXs) may be powered by intermediate mass black hole of a few thousand M⊙ or stellar mass black holes with special radiation processes. In this ′ paper, we present a survey of ULXs in 313 nearby galaxies with D25>1 within 40 Mpc with 467 ROSAT HRI archival observations. The HRI observations are reduced with uniform procedures, refined by simulations that help define the point source detection algorithm employed in this survey. A sample of 562 38 43 extragalactic X-ray point sources with LX = 10 –10 erg/sec is extracted from 173 survey galaxies, including 106 ULX candidates within the D25 isophotes of 63 galaxies and 110 ULX candidates between 1–2 D25 of 64 galaxies, from × which a clean sample of 109 ULXs is constructed to minimize the contamination from foreground or background objects. The strong connection between ULXs and star formation is confirmed based on the striking preference of ULXs to arXiv:astro-ph/0501309v1 14 Jan 2005 occur in late-type galaxies, especially in star forming regions such as spiral arms. ULXs are variable on time scales over days to years, and exhibit a variety of long term variability patterns.
    [Show full text]
  • A Blind HI Survey in the Canes Venatici Region
    Mon. Not. R. Astron. Soc. 400, 743–765 (2009) doi:10.1111/j.1365-2966.2009.14662.x A blind H I survey in the Canes Venatici region K. Kovac,ˇ 1,2 T. A. Oosterloo1,3 and J. M. van der Hulst1 1Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, the Netherlands 2Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerland 3Netherlands Foundation for Research in Astronomy, Postbus 2, 7990 AA Dwingeloo, the Netherlands Accepted 2009 February 18. Received 2009 February 2; in original form 2008 June 23 ABSTRACT We have carried out a blind H I survey using the Westerbork Synthesis Radio Telescope to make 6 8 an inventory of objects with small H I masses (between 10 and 10 M) and to constrain the low-mass end of the H I mass function. The survey has been conducted in a part of the volume containing the nearby Canes Venatici groups of galaxies. The surveyed region covers an area on the sky of about 86 deg2 and a range in velocity from about −450 to about 1330 km s−1. We find 70 sources in the survey by applying an automated searching algorithm. Two of the detections have not been catalogued previously, but they can be assigned an optical counterpart, based on visual inspection of the second-generation Digital Sky Survey images. Only one of the H I detections is without an optical counterpart. This object is detected in the vicinity of NGC 4822, and it has been already detected in previous H I studies. 19 of the objects have been detected for the first time in the 21-cm emission line in this survey.
    [Show full text]
  • Magellanic Type Galaxies Throughout the Universe Eric M
    The Magellanic System: Stars, Gas, and Galaxies Proceedings IAU Symposium No. 256, 2008 c 2009 International Astronomical Union Jacco Th. van Loon & Joana M. Oliveira, eds. doi:10.1017/S1743921308028871 Magellanic type galaxies throughout the Universe Eric M. Wilcots Department of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI 53706 USA email: [email protected] Abstract. The Magellanic Clouds are often characterized as “irregular” galaxies, a term that implies an overall lack of organized structure. While this may be a fitting description of the Small Cloud, the Large Magellanic Cloud, contrary to popular opinion, should not be considered an irregular galaxy. It is characterized by a distinctive morphology of having an offset stellar bar and single spiral arm. Such morphology is relatively common in galaxies of similar mass throughout the local Universe, although explaining the origin of these features has proven challenging. Through a number of recent studies we are beginning to get a better grasp on what it means to be a Magellanic spiral. One key result of these works is that we now recognize that the most unique aspect of the Magellanic Clouds is not their structure, but, rather, their proximity to a larger spiral such as the Milky Way. Keywords. galaxies: dwarf, galaxies: evolution, galaxies: interactions, Magellanic Clouds, galax- ies: structure 1. Introduction While the Small Magellanic Cloud can properly be thought of as an irregular galaxy, the Large Magellanic Cloud shares a number of key morphological properties with a population of galaxies classified as Barred Magellanic Spirals (SBm). These properties include a stellar bar, the center of which may or may not be coincident with the dynamical center of the galaxy, a single, looping spiral arm, and often a large star-forming complex at one end of the bar.
    [Show full text]
  • NRAO Newsletter
    NRAONRAO NewsletterNewsletter The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. July 2002 www.nrao.edu/news/newsletters Number 92 DIRECTOR’S OFFICE California at Berkeley as a Miller Fellow. Two years later, he returned to Caltech where he held various research and teaching positions until 1986. Fred K.Y. Lo to Become NRAO In 1986, Lo accepted the position of Professor of Director Astronomy at the University of Illinois at Urbana- Champaign, and served as the chairman of that university's Associated Universities, astronomy department from 1995 to 1997. Lo accepted his Inc. (AUI), the not-for-profit current position at the Academia Sinica in 1997. He also corporation that operates accepted the post of Professor of Physics at the National the National Radio Astronomy Taiwan University in 1998. Observatory (NRAO) under Lo is an accomplished radio astronomer with very wide a cooperative agreement research interests. His studies range from star formation in with the National Science different environments such as dwarf galaxies, starbursts in Foundation, announces the nearby and very distant galaxies, to the determination of the appointment of Fred K.Y. Lo structure of Sagittarius A - the compact radio source at the as the director of the NRAO, center of the Milky Way Galaxy. He has been intimately effective September 1, 2002. involved in the construction and scientific use of all the mil- Lo is currently a Distinguished Research Fellow and the limeter-wave and sub-millimeter-wave interferometer arrays Director of the Institute of Astronomy and Astrophysics of in the United States, and he made the first millimeter-wave the Academia Sinica, located in Taipei.
    [Show full text]
  • A Blind HI Survey in the Canes Venatici Region
    Research Collection Journal Article A blind HI survey in the Canes Venatici region Author(s): Kovač, K.; Oosterloo, T. A.; Hulst, J. M. van der Publication Date: 2009 Permanent Link: https://doi.org/10.3929/ethz-b-000016701 Originally published in: Monthly Notices of the Royal Astronomical Society 400(2), http://doi.org/10.1111/ j.1365-2966.2009.14662.x Rights / License: In Copyright - Non-Commercial Use Permitted This page was generated automatically upon download from the ETH Zurich Research Collection. For more information please consult the Terms of use. ETH Library Mon. Not. R. Astron. Soc. 400, 743–765 (2009) doi:10.1111/j.1365-2966.2009.14662.x A blind H I survey in the Canes Venatici region K. Kovac,ˇ 1,2 T. A. Oosterloo1,3 and J. M. van der Hulst1 1Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, the Netherlands 2Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerland 3Netherlands Foundation for Research in Astronomy, Postbus 2, 7990 AA Dwingeloo, the Netherlands Accepted 2009 February 18. Received 2009 February 2; in original form 2008 June 23 ABSTRACT We have carried out a blind H I survey using the Westerbork Synthesis Radio Telescope to make 6 8 an inventory of objects with small H I masses (between 10 and 10 M) and to constrain the low-mass end of the H I mass function. The survey has been conducted in a part of the volume containing the nearby Canes Venatici groups of galaxies. The surveyed region covers an area on the sky of about 86 deg2 and a range in velocity from about −450 to about 1330 km s−1.
    [Show full text]
  • Scuola Internazionale Superiore Di Studi Avanzati - Trieste
    Scuola Internazionale Superiore di Studi Avanzati - Trieste Scuola Internazionale Superiore di Studi Avanzati Area of Physics Ph.D. in Astrophysics The nature of Dark Matter from properties of galaxies Advisor: Candidate: Prof. P. Salucci E. V. Karukes Thesis submitted in partial fulfillment of the requirements for the degree of Doctor Philosophiae Academic Year 2015/2016 SISSA - Via Bonomea 265 - 34136 TRIESTE - ITALY Acknowledgements I would like to express my special appreciation and thanks to my advisor Paolo Salucci. I appreciate all his contributions of time, ideas and discussions during these 3 years of my PhD. His advices on both research as well as on my career have been invaluable. I am thankful also to SISSA for useful lectures and to all professors of the Astrophysical sector, in particular to Alessandro Bressan, Luigi Danese and Andrea Lapi for fruitful discussions. I also thank all my friends and colleagues at SISSA Alessio, Mauro, Elena, Guillaume, Bruno, Xiao, Federico, Marco, Andrei and Lasma, who made more enjoyable the long working days and the short weekends. Then, I would like to thank Gor, Elias and Francesca for their strong and tasty coffee, that many times helped me to be productive until late. A special thank goes to my two supportive officemates Claudia and Serena for the infinite discussions about everything. I cannot forget about my friends from Rostov Polina, Roma, Vanya, Ilya and many others for all the enjoyable time we had spend together and I hope we will spend in the future. A special acknowledgement goes to my best mate of many years Nastya with whom we should write a book about all our adventures together.
    [Show full text]
  • TABLE 1 Explanation of CVRHS Symbols A
    TABLE 1 Explanation of CVRHS Symbols a Symbol Description 1 2 General Terms ETG An early-type galaxy, collectively referring to a galaxy in the range of types E to Sa ITG An intermediate-type galaxy, taken to be in the range Sab to Sbc LTG A late-type galaxy, collectively referring to a galaxy in the range of types Sc to Im ETS An early-type spiral, taken to be in the range S0/a to Sa ITS An intermediate-type spiral, taken to be in the range Sab to Sbc LTS A late-type spiral, taken to be in the range Sc to Scd XLTS An extreme late-type spiral, taken to be in the range Sd to Sm classical bulge A galaxy bulge that likely formed from early mergers of smaller galaxies (Kormendy & Kennicutt 2004; Athanassoula 2005) pseudobulge A galaxy bulge made of disk material that has secularly collected into the central regions of a barred galaxy (Kormendy 2012) PDG A pure disk galaxy, a galaxy lacking a classical bulge and often also lacking a pseudobulge Stage stage The characteristic of galaxy morphology that recognizes development of structure, the widespread distribution of star formation, and the relative importance of a bulge component along a sequence that correlates well with basic characteristics such as integrated color, average surface brightness, and HI mass-to-blue luminosity ratio Elliptical Galaxies E galaxy A galaxy having a smoothly declining brightness distribution with little or no evidence of a disk component and no inflections (such as lenses) in the luminosity distribution (examples: NGC 1052, 3193, 4472) En An elliptical galaxy
    [Show full text]
  • A Classical Morphological Analysis of Galaxies in the Spitzer Survey Of
    Accepted for publication in the Astrophysical Journal Supplement Series A Preprint typeset using LTEX style emulateapj v. 03/07/07 A CLASSICAL MORPHOLOGICAL ANALYSIS OF GALAXIES IN THE SPITZER SURVEY OF STELLAR STRUCTURE IN GALAXIES (S4G) Ronald J. Buta1, Kartik Sheth2, E. Athanassoula3, A. Bosma3, Johan H. Knapen4,5, Eija Laurikainen6,7, Heikki Salo6, Debra Elmegreen8, Luis C. Ho9,10,11, Dennis Zaritsky12, Helene Courtois13,14, Joannah L. Hinz12, Juan-Carlos Munoz-Mateos˜ 2,15, Taehyun Kim2,15,16, Michael W. Regan17, Dimitri A. Gadotti15, Armando Gil de Paz18, Jarkko Laine6, Kar´ın Menendez-Delmestre´ 19, Sebastien´ Comeron´ 6,7, Santiago Erroz Ferrer4,5, Mark Seibert20, Trisha Mizusawa2,21, Benne Holwerda22, Barry F. Madore20 Accepted for publication in the Astrophysical Journal Supplement Series ABSTRACT The Spitzer Survey of Stellar Structure in Galaxies (S4G) is the largest available database of deep, homogeneous middle-infrared (mid-IR) images of galaxies of all types. The survey, which includes 2352 nearby galaxies, reveals galaxy morphology only minimally affected by interstellar extinction. This paper presents an atlas and classifications of S4G galaxies in the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system. The CVRHS system follows the precepts of classical de Vaucouleurs (1959) morphology, modified to include recognition of other features such as inner, outer, and nuclear lenses, nuclear rings, bars, and disks, spheroidal galaxies, X patterns and box/peanut structures, OLR subclass outer rings and pseudorings, bar ansae and barlenses, parallel sequence late-types, thick disks, and embedded disks in 3D early-type systems. We show that our CVRHS classifications are internally consistent, and that nearly half of the S4G sample consists of extreme late-type systems (mostly bulgeless, pure disk galaxies) in the range Scd-Im.
    [Show full text]
  • The Large Magellanic Cloud Stellar Content with SMASH: I. Assessing the Stability of the Magellanic Spiral Arms
    Astronomy & Astrophysics manuscript no. 38392corr c ESO 2020 June 22, 2020 Letter to the Editor The Large Magellanic Cloud stellar content with SMASH: I. Assessing the stability of the Magellanic spiral arms T. Ruiz-Lara1; 2, C. Gallart1; 2, M. Monelli1; 2, D. Nidever3; 4, A. Dorta1; 2, Y. Choi3; 5, K. Olsen4, G. Besla6, E.J. Bernard7, S. Cassisi8; 9, P. Massana10, N.E.D. Noël10, I. Pérez11; 12, V. Rusakov13, M.-R. L. Cioni14, S. R. Majewski15, R.P. van der Marel5; 16, D. Martínez-Delgado17, A. Monachesi18; 19, L. Monteagudo20; 1; 2, R.R. Muñoz21, G.S. Stringfellow22, F. Surot1; 2, A. K. Vivas23, A.R. Walker23, and D. Zaritsky5 1 Instituto de Astrofísica de Canarias, Calle Vía Láctea s/n, E-38205 La Laguna, Tenerife, Spain e-mail: [email protected] 2 Departamento de Astrofísica, Universidad de La Laguna, E-38200 La Laguna, Tenerife, Spain 3 Department of Physics, Montana State University, P.O. Box 173840, Bozeman, MT 59717-3840 4 NSF’s National Optical-Infrared Astronomy Research Laboratory, 950 North Cherry Ave, Tucson, AZ 85719 5 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 6 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 7 Université Côte d’Azur, OCA, CNRS, Lagrange, France 8 INAF – Astronomical Observatory of Abruzzo, via M. Maggini, sn, 64100 Teramo, Italy 9 INFN, Sezione di Pisa, Largo Pontecorvo 3, 56127 Pisa, Italy 10 Department of Physics, University of Surrey, Guildford, GU2 7XH, UK 11 Departamento de Física Teórica y del Cosmos, Universidad de
    [Show full text]