DECEMBER 2014 Introduction the Purpose of the Observer’S Challenge Is to Encourage the Pursuit of Visual Observing
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CONSTELLATION TRIANGULUM, the TRIANGLE Triangulum Is a Small Constellation in the Northern Sky
CONSTELLATION TRIANGULUM, THE TRIANGLE Triangulum is a small constellation in the northern sky. Its name is Latin for "triangle", derived from its three brightest stars, which form a long and narrow triangle. Known to the ancient Babylonians and Greeks, Triangulum was one of the 48 constellations listed by the 2nd century astronomer Ptolemy. The celestial cartographers Johann Bayer and John Flamsteed catalogued the constellation's stars, giving six of them Bayer designations. The white stars Beta and Gamma Trianguli, of apparent magnitudes 3.00 and 4.00, respectively, form the base of the triangle and the yellow-white Alpha Trianguli, of magnitude 3.41, the apex. Iota Trianguli is a notable double star system, and there are three star systems with planets located in Triangulum. The constellation contains several galaxies, the brightest and nearest of which is the Triangulum Galaxy or Messier 33—a member of the Local Group. The first quasar ever observed, 3C 48, also lies within Triangulum's boundaries. HISTORY AND MYTHOLOGY In the Babylonian star catalogues, Triangulum, together with Gamma Andromedae, formed the constellation known as MULAPIN "The Plough". It is notable as the first constellation presented on (and giving its name to) a pair of tablets containing canonical star lists that were compiled around 1000 BC, the MUL.APIN. The Plough was the first constellation of the "Way of Enlil"—that is, the northernmost quarter of the Sun's path, which corresponds to the 45 days on either side of summer solstice. Its first appearance in the pre-dawn sky (heliacal rising) in February marked the time to begin spring ploughing in Mesopotamia. -
Making a Sky Atlas
Appendix A Making a Sky Atlas Although a number of very advanced sky atlases are now available in print, none is likely to be ideal for any given task. Published atlases will probably have too few or too many guide stars, too few or too many deep-sky objects plotted in them, wrong- size charts, etc. I found that with MegaStar I could design and make, specifically for my survey, a “just right” personalized atlas. My atlas consists of 108 charts, each about twenty square degrees in size, with guide stars down to magnitude 8.9. I used only the northernmost 78 charts, since I observed the sky only down to –35°. On the charts I plotted only the objects I wanted to observe. In addition I made enlargements of small, overcrowded areas (“quad charts”) as well as separate large-scale charts for the Virgo Galaxy Cluster, the latter with guide stars down to magnitude 11.4. I put the charts in plastic sheet protectors in a three-ring binder, taking them out and plac- ing them on my telescope mount’s clipboard as needed. To find an object I would use the 35 mm finder (except in the Virgo Cluster, where I used the 60 mm as the finder) to point the ensemble of telescopes at the indicated spot among the guide stars. If the object was not seen in the 35 mm, as it usually was not, I would then look in the larger telescopes. If the object was not immediately visible even in the primary telescope – a not uncommon occur- rence due to inexact initial pointing – I would then scan around for it. -
Arxiv:1911.08543V1 [Astro-Ph.GA] 19 Nov 2019 Tions (Diemand Et Al
MNRAS 000,1{ ?? (2018) Preprint 21 November 2019 Compiled using MNRAS LATEX style file v3.0 The Smallest Scale of Hierarchy Survey (SSH). I. Survey Description. F. Annibali,1? G. Beccari,2 M. Bellazzini,1 M. Tosi,1 F. Cusano,1 D. Paris,5 M. Cignoni,3 L. Ciotti,4 C. Nipoti4 E. Sacchi.6 1INAF - Osservatorio di Astrofisica e Scienza dello Spazio, Via Piero Gobetti, 93/3, I-40129 - Bologna, Italy 2ESO, Karl-Schwarzschild Strasse 2, D-80 Garching, Germany 3Dipartimento di Fisica, Universit`adi Pisa, Largo Bruno Pontecorvo 3, I-56127 Pisa, Italy 4Dipartimento di Fisica e Astronomia, Universit`adi Bologna, via Piero Gobetti 93/2, I-40129 - Bologna, Italy 5INAF-Osservatorio Astronomico di Roma, Via Frascati 33, I-00078 Monte Porzio, Italy 6Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA Accepted XXX. Received YYY; in original form ZZZ ABSTRACT The Smallest Scale of Hierarchy (SSH) survey is an ongoing strategic large program at the Large Binocular Telescope, aimed at the detection of faint stellar streams and satellites around 45 late-type dwarf galaxies located in the Local Universe within '10 Mpc. SSH exploits the wide-field, deep photometry provided by the Large Binocular Cameras in the two wide filters g and r. This paper describes the survey, its goals, and the observational and data reduction strategies. We present preliminary scientific results for five representative cases (UGC 12613, NGC 2366, UGC 685, NGC 5477 and UGC 4426) covering the whole distance range spanned by the SSH targets. We reach a surface brightness limit as faint as µ(r) ∼ 31 mag arcsec−2 both for targets closer than 4−5 Mpc, which are resolved into individual stars, and for more distant targets through the diffuse light. -
Star Formation Histories of the LEGUS Dwarf Galaxies. III. the Nonbursty
Draft version November 13, 2019 Preprint typeset using LATEX style emulateapj v. 12/16/11 STAR FORMATION HISTORIES OF THE LEGUS DWARF GALAXIES (III): THE NON-BURSTY NATURE OF 23 STAR FORMING DWARF GALAXIES M. Cignoni2,3,4, E. Sacchi5, M. Tosi4, A. Aloisi5, D. O. Cook6,7, D. Calzetti8, J. C. Lee7, E. Sabbi5, D. A. Thilker14 ,A. Adamo9 , D. A. Dale10, B. G. Elmegreen11, J.S. Gallagher III15, E. K. Grebel12, K. E. Johnson16, M. Messa9, L. J. Smith13 and L. Ubeda5 Draft version November 13, 2019 ABSTRACT We derive the recent star formation histories of 23 active dwarf galaxies using HST observations from the Legacy Extragalactic UV Survey (LEGUS). We apply a color-magnitude diagram fitting technique using two independent sets of stellar models, PARSEC-COLIBRI and MIST. Despite the non-negligible recent activity, none of the 23 star forming dwarfs show enhancements in the last 100 Myr larger than three times the 100-Myr-average. The unweighted mean of the individual SFHs in the last 100 Myr is also consistent with a rather constant activity, irrespective of the atomic gas fraction. We confirm previous results that for dwarf galaxies the CMD-based average star formation rates (SFRs) are generally higher than the FUV-based SFR. For half of the sample, the 60-Myr-average CMD-based SFR is more than two times the FUV SFR. In contrast, we find remarkable agreement between the 10-Myr-average CMD-based SFR and the Hα-based SFR. Finally, using core helium burning stars of intermediate mass we study the pattern of star formation spatial progression over the past 60 Myr, and speculate on the possible triggers and connections of the star formation activity with the environment in which these galaxies live. -
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. -
The Westerbork Hydrogen Accretion in Local Galaxies \(HALOGAS\)
A&A 526, A118 (2011) Astronomy DOI: 10.1051/0004-6361/201015938 & c ESO 2011 Astrophysics The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) survey I. Survey description and pilot observations G. Heald1, G. Józsa1, P. Serra1, L. Zschaechner2,R.Rand2, F. Fraternali3, T. Oosterloo1,4, R. Walterbos5, E. Jütte6, and G. Gentile7 1 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2, 7990 AA Dwingeloo, The Netherlands e-mail: [email protected] 2 University of New Mexico, 800 Yale Blvd, Albuquerque, NM, USA 3 Astronomy Department, Bologna University, via Ranzani 1, 40127 Bologna, Italy 4 Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, The Netherlands 5 Department of Astronomy, New Mexico State University, PO Box 30001, MSC 4500, Las Cruces, NM 88003, USA 6 Astronomisches Institut der Ruhr-Universität Bochum, Universitätsstr. 150, 44780 Bochum, Germany 7 Sterrenkundig Observatorium, Ghent University, Krijgslaan 281, S9, 9000 Ghent, Belgium Received 15 October 2010 / Accepted 27 November 2010 ABSTRACT We introduce a new, very deep neutral hydrogen (H i) survey being performed with the Westerbork Synthesis Radio Telescope (WSRT). The Westerbork Hydrogen Accretion in LOcal GAlaxieS (HALOGAS) Survey is producing an archive of some of the most sensitive H i observations available, on the angular scales which are most useful for studying faint, diffuse gas in and around nearby galaxies. The survey data are being used to perform careful modeling of the galaxies, characterizing their gas content, mor- phology, and kinematics, with the primary goal of revealing the global characteristics of cold gas accretion onto spiral galaxies in the local Universe. In this paper, we describe the survey sample selection, the data acquisition, reduction, and analysis, and present the data products obtained during our pilot program, which consists of UGC 2082, NGC 672, NGC 925, and NGC 4565. -
The Search for Failed Supernovae with the Large Binocular Telescope: a New Candidate and the Failed SN Fraction with 11 Yr of Data
The search for failed supernovae with the Large Binocular Telescope: a new candidate and the failed SN fraction with 11 yr of data J. M. M. Neustadt1, C. S. Kochanek1,2, K. Z. Stanek1, C. Basinger1, T. Jayasinghe1, C. T . Garling1, S. M. Adams1, and J. Gerke1 1Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210, USA 2Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, 191 W. Woodruff Avenue, Columbus, OH 43210, USA Abstract We present updated results of the Large Binocular Telescope Search for Failed Supernovae. This search monitors luminous stars in 27 nearby galaxies with a current baseline of 11 yr of data. We re-discover the failed supernova (SN) candidate N6946-BH1 as well as a new candidate, M101-OC1. M101-OC1 is a blue supergiant that rapidly disappears in optical wavelengths with no evidence for significant obscuration by warm dust. While we consider other options, a good explanation for the fading of M101-OC1 is a failed SN, but follow-up observations are needed to confirm this. Assuming only one clearly detected failed SN, we find ¸0.23 a failed SN fraction 5 = 0.16−0.12 at 90 per cent confidence. We also report on a collection of stars that show slow (∼decade), large amplitude (Δ!/!¡ 3) luminosity changes. 1 1 Introduction The life of every massive star (>8 M ) ends with the collapse of its core, which is sometimes followed by the violent ejection of its envelope and the production of a luminous core-collapse supernova (ccSN). -
Arxiv:1903.02375V1
Star Formation in Nearby Dwarf Galaxies* S. S. Kaisin1, ** and I. D. Karachentsev 1Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, 369167 Russia (Received July 20, 2018; Revised December 12, 2018; Accepted December 12, 2018) We report the measured Hα fluxes and images of 66 nearby objects observed with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. Three of these objectsIC2233, UGC4704, and NGC3432are late-type spiral galaxies, six objects are distant globular clusters of the M31 galaxy, and the remaining ones are dwarf galaxies. We used the measured Hα fluxes to estimate the integrated and specific star- formation rates and analyzed some of the main features of star formation in dwarf galaxies and late-type spirals based on a sample of more than 500 Local-volume galaxies. Keywords: galaxies, dwarf – galaxies, star formation 1. INTRODUCTION Over the last decade observations of nearby galaxies aimed at determining their star-formation rate (SFR) from Hα emission flux have been carried out at the Special Astrophysical Observatory of the Russian Academy of Sciences. The Hα survey targets are Local-Volume (LV) galaxies located within 11 Mpc. The results of our previous observations are reported in a series of 9 papers references to which can be found in the last paper of this series [1]. Mass sky surveys made at optical wavelengths and in the H I 21 cm line gave rise to a rapid increase of the number of galaxies in the LV. Their number in the ”Updated Nearby Galaxy Catalog” (UNGC) [2] reached 869, and more than 80% of the sample are made up of dwarf galaxies with ∗ stellar masses log(M /M⊙) < 9.0. -
Cv Noah Brosch 2009.Pdf
CURRICULUM VITAE Noah Brosch March 23, 2009 1 Personal information ² Name: Noah Brosch, PhD, Id. card No. 068692060. ² Faculty of Exact Sciences, School of Physics and Astronomy Phones [972]-3-640-7413, Fax [972]-3-640-8179. ² Home Address: 6, Olesh Matsui St., Nataniya 42201 Phone numbers [972]-9-885-6689/6690 (home), [972]-54-752-912 (mo- bile). ² Date and place of birth: Jan. 27, 1948, Romania. ² Date of arrival in Israel: 1963. ² Zahal military service: 31.8.1966 - 10.11.1971. ID number 987945. ² Nationality: Israeli. ² Familial status: Married, with two daughters. 1.1 Education 1971-1974 Tel Aviv University Physics BSc, 1975 1974-1976 Tel Aviv University Physics MSc, 1977 1976-1980 Tel Aviv University Astronomy | 1980-1983 University of Leiden Astronomy PhD, 1983 The Netherlands MSc thesis: The spectrum of the Be star MWC342 in 1974-1975 Supervisor: Prof. E. M. Leibowitz, Tel Aviv University 1 PhD thesis: Galaxies in low density regions of the Universe Supervisors: ² Prof. Dr. J. Mayo Greenberg, University of Leiden ² Prof. Dr. W. W. Shane, University of Nijmegen 1.2 Academic and Professional Experience Period Institution Department Rank 1974-1976 Tel Aviv Municipality Popular University Lecturer 1974-1976 Tel Aviv University Physics and Astron. Teaching Assistant 1976-1979 Museum Haaretz Lasky Planetarium Director 1980-1983 University of Leiden Lab. Astrophys. Research Assistant 1982-1992 Tel Aviv University Wise Observatory Technical Director 1987-1988 Tel Aviv University Physics and Astron. Research Associate 1988-1999 Tel Aviv University Physics and Astron. Senior Research Associate 1990- Tel Aviv University Physics and Astron. TAUVEX Principal Investigator 1997-1998 STScI RPO Sabbatical Visitor 1999- Tel Aviv University Physics and Astron. -
Cloud Download
ATLAS OF GALAXIES USEFUL FOR MEASURING THE COSMOLOGICAL DISTANCE SCALE .0 o NASA SP-496 ATLAS OF GALAXIES USEFUL FOR MEASURING THE COSMOLOGICAL DISTANCE SCALE Allan Sandage Space Telescope Science Institute Baltimore, Maryland and Department of Physics and Astronomy, The Johns Hopkins University Baltimore, Maryland and John Bedke Computer Sciences Corporation Space Telescope Science Institute Baltimore, Maryland Scientific and Technical Information Division 1988 National Aeronautics and Space Administration Washington, DC Library of Congress Cataloging-in-Publication Data Sandage, Allan. Atlas of galaxies useful for measuring the cosomological distance scale. (NASA SP ; 496) Bibliography: p. 1. Cosmological distances--Measurement. 2. GalaxiesrAtlases. 3. Hubble Space Telescope. I. Bedke, John. II. Title. 111. Series. QB991.C66S36 1988 523.1'1 88 600056 For sale b_ the Superintendent of tX_uments. U S Go_ernment Printing Office. Washington. DC 20402 PREFACE A critical first step in determining distances to galaxies is to measure some property (e.g., size or luminosity) of primary objects such as stars of specific types, H II regions, and supernovae remnants that are resolved out of the general galaxy stellar content. Very few galaxies are suitable for study at such high resolution because of intense disk background light, excessive crowding by contaminating images, internal obscuration due to dust, high inclination angles, or great distance. Nevertheless, these few galaxies with accurately measurable primary distances are required to calibrate secondary distance indicators which have greater range. If telescope time is to be optimized, it is important to know which galaxies are suitable for specific resolution studies. No atlas of galaxy photographs at a scale adequate for resolution of stellar content exists that is complete for the bright galaxy sample [e.g.; for the Shapley-Ames (1932) list, augmented with listings in the Second Reference Catalog (RC2) (de Vaucouleurs, de Vaucouleurs, and Corwin, 1977); and the Uppsala Nilson (1973) catalogs]. -
November 2009
Deepsky BeautBeautiesiesiesies:::: November 2009 All objects in this article can be observed underneath a dark sky with telescopes Than we aim our scopes at the cluster with a maximum of 8 inch (20 cm). Most NGC 752 , the golf ball of the Golf Putter. objects can already be observed with The irregular shaped open star cluster smaller scopes or binoculars stands out nicely from its background. Apart from a few stars, the cluster exists namely out of sixty faint stars. Within NGC Wintertime has started and announces the 752 there are a lot of double stars and start of a new observing season. The condensations of stars. NNE of the cluster nights will last longer and starts earlier, so the double star Struve 14 is located. The we have more time for observing the cluster is best observed with binoculars. nightly sky. This month we will highlight You can capture the three objects (Struve some nice objects in the constellations 14, STAR 14 and NGC 752) in one field of Andromeda, Triangulum and Perseus. view. Let’s start with a nice optical double star in The last gem in Andromeda that we will Andromeda: Struve 14 . This is a wide pair discuss this month is the beautiful Blue southwest of the open cluster NGC 752. Snowball , NGC 7662. Small telescopes Both stars have a beautiful golden colour. reveal a star with a fuzzy glow around it. A The main star is located at a distance of 15cm telescope with a magnification of 360 light years from earth, its companion about 100x will show a round nebula with at 1.200 light years. -
The WSRT HALOGAS Survey Main Results and Public Data Release George Heald and the HALOGAS Team
The WSRT HALOGAS Survey Main Results and Public Data Release George Heald and the HALOGAS team CSIRO ASTRONOMY AND SPACE SCIENCE Outline • Recap of science case and galaxy sample • HALOGAS observations and ancillary data • Results and publications • Main outcomes • Public data releases • DR1 (12 February 2019) - WSRT HI cubes and moment maps • DR2 (31 May 2019) - Ancillary data • Timeline for final publications, and moving forward ... 2 | George Heald | HALOGAS Results and Data Release Motivation Motivation for HALOGAS project was similar to the MHONGOOSE science case • How common are thick HI disks and what are their properties? • What is the origin of thick disks, and how are they related to star formation and/or the gas accretion process? • How much cool neutral hydrogen surrounds spiral galaxies, in what form is it typically found, and what is its contribution to the gas accretion process? • Is accreting neutral hydrogen a substantial contributor to the gas mass budget in the star formation process? 3 | George Heald | HALOGAS Results and Data Release HALOGAS team past & present George Heald, Björn Adebahr, Nadya Ben Bekhti, Bob Benjamin, Erwin de Blok, Ralf-Jürgen Dettmar, Lars Flöer, Filippo Fraternali, Gianfranco Gentile, Mark Gorski, Noelia Herrera-Ruiz, Gyula Jozsa, Eva Jütte, Peter Kamphuis, Antonino Marasco, Tom Oosterloo, Maria Patterson, Nick Pingel, Rich Rand, Renzo Sancisi, Paolo Serra, Carlos Vargas, Rene Walterbos, Benjamin Winkel, Cat Wu, Laura Zschaechner 2010 (Dwingeloo, The Netherlands) 2011 (Bochum, Germany) 4 | George