MAY 2010 OBSERVER a Bird’S-Eye View Inside the Observer
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Ann Arbor AAPT 2009
AnnAAPT 09 Asummerrbor meeting First Time at an AAPT Meeting? ...4 AAPT 2009 Meeting Information .....................6 Summer Meeting Bus Schedule/information ............8 Welcome to Ann Arbor ...............10 Special Events ...........................12 July 25–29 Awards/Plenaries ........................14 Committee Meetings ..................20 University of Michigan Exhibitor Information ..................21 Ann Arbor Commercial Workshops .............25 Meeting at a Glance ...................26 Session Finder ............................30 www.aapt.org Workshops .................................33 SESSION ABSTRACTS Sunday ..................................39 Monday .................................41 Tuesday .................................82 American Association of Physics Teachers Wednesday ..........................126 One Physics Ellipse College Park, MD 20740 Index of Contributors ...............144 301-209-3300, fax: 301-209-0845 Index of Advertisers .................146 [email protected], www.aapt.org Our Donors ...............................147 Map of Exhibit Hall ...................148 Welcome to Ann Arbor and the University of Michigan! This summer’s AAPT meeting offers about three dozen workshops and seven dozen sessions on a wide variety of topics; the apparatus, photo, and video contests; exhibits by numerous vendors of books and equipment; the traditional picnic and demo show; and the great book give-away. In addition (and of particular importance), 18 area committee meetings offer attendees an invaluable opportunity -
Identification of Old Tidal Dwarfs Near Early-Type Galaxies from Deep
Mon. Not. R. Astron. Soc. 000,1–11 (2013) Printed 29 October 2018 (MN LATEX style file v2.2) Identification of old tidal dwarfs near early-type galaxies from deep imaging and H I observations Pierre-Alain Duc,1? Sanjaya Paudel,1 Richard M. McDermid,2 Jean-Charles Cuillandre,3 Paolo Serra,4 Fred´ eric´ Bournaud,1 Michele Cappellari,5 Eric Emsellem6;7 1Laboratoire AIM Paris-Saclay, CEA/IRFU/SAp, CNRS/INSU, Universite´ Paris Diderot, 91191 Gif-sur-Yvette Cedex, France 2Gemini Observatory, Northern Operations Centre, 670 N. A‘ohoku Place, Hilo, HI 96720, USA 3Canada-France-Hawaii Telescope Corporation, 65-1238 Mamalahoa Hwy., Kamuela, Hawaii 96743 USA 4CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia 5Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH 6European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany 7Centre de Recherche Astrophysique de Lyon, Universite´ Lyon 1, Observatoire de Lyon, Ecole Normale Superieure´ de Lyon, CNRS, UMR 5574, 9 avenue Charles Andre,´ F-69230 Saint-Genis Laval, France Accepted for publication in MNRAS ABSTRACT It has recently been proposed that the dwarf spheroidal galaxies located in the Local Group disks of satellites (DoSs) may be tidal dwarf galaxies (TDGs) born in a major merger at least 5 Gyr ago. Whether TDGs can live that long is still poorly constrained by observations. As part of deep optical and H I surveys with the CFHT MegaCam camera and Westerbork Syn- thesis Radio Telescope made within the ATLAS3D project, and follow-up spectroscopic ob- servations with the Gemini-North telescope, we have discovered old TDG candidates around several early-type galaxies. -
Lemmings. I. the Emerlin Legacy Survey of Nearby Galaxies. 1.5-Ghz Parsec-Scale Radio Structures and Cores
MNRAS 000,1{44 (2018) Preprint 8 February 2018 Compiled using MNRAS LATEX style file v3.0 LeMMINGs. I. The eMERLIN legacy survey of nearby galaxies. 1.5-GHz parsec-scale radio structures and cores R. D. Baldi1?, D. R. A. Williams1, I. M. McHardy1, R. J. Beswick2, M. K. Argo2;3, B. T. Dullo4, J. H. Knapen5;6, E. Brinks7, T. W. B. Muxlow2, S. Aalto8, A. Alberdi9, G. J. Bendo2;10, S. Corbel11;12, R. Evans13, D. M. Fenech14, D. A. Green15, H.-R. Kl¨ockner16, E. K¨ording17, P. Kharb18, T. J. Maccarone19, I. Mart´ı-Vidal8, C. G. Mundell20, F. Panessa21, A. B. Peck22, M. A. P´erez-Torres9, D. J. Saikia18, P. Saikia17;23, F. Shankar1, R. E. Spencer2, I. R. Stevens24, P. Uttley25 and J. Westcott7 1 School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK 2 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK 3 Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 4 Departamento de Astrofisica y Ciencias de la Atmosfera, Universidad Complutense de Madrid, E-28040 Madrid, Spain 5 Instituto de Astrofisica de Canarias, Via Lactea S/N, E-38205, La Laguna, Tenerife, Spain 6 Departamento de Astrofisica, Universidad de La Laguna, E-38206, La Laguna, Tenerife, Spain 7 Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK 8 Department of Space, Earth and Environment, Chalmers University of Technology, Onsala Space Observatory, 43992 Onsala, Sweden 9 Instituto de Astrofisica de Andaluc´ıa(IAA, CSIC); Glorieta de la Astronom´ıa s/n, 18008-Granada, Spain 10 ALMA Regional Centre Node, UK 11 Laboratoire AIM (CEA/IRFU - CNRS/INSU - Universit´eParis Diderot), CEA DSM/IRFU/SAp, F-91191 Gif-sur-Yvette, France 12 Station de Radioastronomie de Nan¸cay, Observatoire de Paris, PSL Research University, CNRS, Univ. -
Cfa in the News ~ Week Ending 3 January 2010
Wolbach Library: CfA in the News ~ Week ending 3 January 2010 1. New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 2. 2009 in science and medicine, ROGER SCHLUETER, Belleville News Democrat (IL), Sunday, January 3, 2010 3. 'Science, celestial bodies have always inspired humankind', Staff Correspondent, Hindu (India), Tuesday, December 29, 2009 4. Why is Carpenter defending scientists?, The Morning Call, Morning Call (Allentown, PA), FIRST ed, pA25, Sunday, December 27, 2009 5. CORRECTIONS, OPINION BY RYAN FINLEY, ARIZONA DAILY STAR, Arizona Daily Star (AZ), FINAL ed, pA2, Saturday, December 19, 2009 6. We see a 'Super-Earth', TOM BEAL; TOM BEAL, ARIZONA DAILY STAR, Arizona Daily Star, (AZ), FINAL ed, pA1, Thursday, December 17, 2009 Record - 1 DIALOG(R) New social science research from G. Sonnert and co-researchers described, Science Letter, p40, Tuesday, January 5, 2010 TEXT: "In this paper we report on testing the 'rolen model' and 'opportunity-structure' hypotheses about the parents whom scientists mentioned as career influencers. According to the role-model hypothesis, the gender match between scientist and influencer is paramount (for example, women scientists would disproportionately often mention their mothers as career influencers)," scientists writing in the journal Social Studies of Science report (see also ). "According to the opportunity-structure hypothesis, the parent's educational level predicts his/her probability of being mentioned as a career influencer (that ism parents with higher educational levels would be more likely to be named). The examination of a sample of American scientists who had received prestigious postdoctoral fellowships resulted in rejecting the role-model hypothesis and corroborating the opportunity-structure hypothesis. -
MASSIVE Galaxies with Supermassive Black Holes
Hubble Space Telescope Cycle 23 GO Proposal 750 Homogeneous Distances and Central Profiles for MASSIVE Survey Galaxies with Supermassive Black Holes Scientific Category: UNRESOLVED STELLAR POPULATIONS AND GALAXY STRUCTURE Scientific Keywords: Black Holes, Cosmological Parameters And Distance Scale, Galaxy Centers, Galaxy Morphology And Structure Instruments: WFC3 Proprietary Period: 12 Proposal Size: Small Orbit Request Prime Parallel Cycle 23 34 0 Abstract Massive early-type galaxies are the subject of intense interest: they exhibit the most massive black holes (BHs), most extreme stellar IMFs, and most dramatic size evolution over cosmic time. Yet, their complex formation histories remain obscure. Enter MASSIVE: a volume-limited survey of the structure and dynamics of the 100 most massive early-type galaxies within ~100 Mpc. We use integral-field spectroscopy (IFS) on sub-arcsecond (with AO) and large scales for simultaneous dynamical modeling of the supermassive BH, stars, and dark matter. The goals of MASSIVE include precise constraints on BH-galaxy scaling relations, the stellar IMF, and late-time assembly of ellipticals. We have already obtained much of the needed IFS and wide-field imaging for this project; here, we propose to add the one missing ingredient: high-resolution imaging with HST. This will nail down the central profiles, greatly reducing the degeneracy between M/L and BH masses in our dynamical orbit modeling. Further, we will measure efficient, high-quality WFC3/IR SBF distances for all targets, thereby removing potentially large errors from peculiar velocities (especially in the high-density regions occupied by massive early-types) or heterogeneous distance methods. Distance errors are insidious: they affect BH masses and galaxy properties in dissimilar ways, and thus can bias both the scatter and slopes of the scaling relations. -
Lord Rosse, Robinson, South and the Discovery of Spiral Structure in 1845
Journal of Astronomical History and Heritage, 15(1), 19-29 (2012). THE M51 MYSTERY: LORD ROSSE, ROBINSON, SOUTH AND THE DISCOVERY OF SPIRAL STRUCTURE IN 1845 Wolfgang Steinicke Gottenheimerstr. 18, D-79224, Umkirch, Germany. E-mail: [email protected] Abstract: In April 1845 Lord Rosse discovered the spiral structure of M51 with his 72-inch reflector at Birr Castle. Already in March the new telescope had been pointed at the object in Canes Venatici, later nicknamed the ‘Whirlpool Nebula’. Two experienced astronomers were present: Sir James South and the Reverend Thomas Romney Robin- son. The problem is that there is no record that they noticed the spiral structure, even though it was immediately seen by Lord Rosse the next month. The solution presented here is based on evidentiary facts, highlighting the nine- teenth century astronomical praxis. Focal points are bias, fantasy and a sometimes fatal conspiracy of eye and brain. Keywords: Spiral structure, nebulae, star clusters, Lord Rosse, Birr Castle, Leviathan of Parsonstown, Whirlpool Nebula, nebular hypothesis, visual observation, drawings. 1 DISCOVERY OF M51 AND JOHN the core, surrounded by a divided ring (Figure 2); it HERSCHEL’S ‘RING NEBULA’ appears as Figure 25 in the Slough catalogue. Herschel M51 (NGC 5194) is a nearby Sbc-galaxy with a visual magnitude 8.4 and a size of 11.2 × 6.9. It was dis- covered on 13 October 1773 by Charles Messier (1730–1817) with a 3.5-inch refractor at Paris. The description, published in his famous catalogue of 1781, reads: “… very faint nebula without stars …” 1 (Messier, 1781: 247). -
Atlas Menor Was Objects to Slowly Change Over Time
C h a r t Atlas Charts s O b by j Objects e c t Constellation s Objects by Number 64 Objects by Type 71 Objects by Name 76 Messier Objects 78 Caldwell Objects 81 Orion & Stars by Name 84 Lepus, circa , Brightest Stars 86 1720 , Closest Stars 87 Mythology 88 Bimonthly Sky Charts 92 Meteor Showers 105 Sun, Moon and Planets 106 Observing Considerations 113 Expanded Glossary 115 Th e 88 Constellations, plus 126 Chart Reference BACK PAGE Introduction he night sky was charted by western civilization a few thou - N 1,370 deep sky objects and 360 double stars (two stars—one sands years ago to bring order to the random splatter of stars, often orbits the other) plotted with observing information for T and in the hopes, as a piece of the puzzle, to help “understand” every object. the forces of nature. The stars and their constellations were imbued with N Inclusion of many “famous” celestial objects, even though the beliefs of those times, which have become mythology. they are beyond the reach of a 6 to 8-inch diameter telescope. The oldest known celestial atlas is in the book, Almagest , by N Expanded glossary to define and/or explain terms and Claudius Ptolemy, a Greco-Egyptian with Roman citizenship who lived concepts. in Alexandria from 90 to 160 AD. The Almagest is the earliest surviving astronomical treatise—a 600-page tome. The star charts are in tabular N Black stars on a white background, a preferred format for star form, by constellation, and the locations of the stars are described by charts. -
00E the Construction of the Universe Symphony
The basic construction of the Universe Symphony. There are 30 asterisms (Suites) in the Universe Symphony. I divided the asterisms into 15 groups. The asterisms in the same group, lay close to each other. Asterisms!! in Constellation!Stars!Objects nearby 01 The W!!!Cassiopeia!!Segin !!!!!!!Ruchbah !!!!!!!Marj !!!!!!!Schedar !!!!!!!Caph !!!!!!!!!Sailboat Cluster !!!!!!!!!Gamma Cassiopeia Nebula !!!!!!!!!NGC 129 !!!!!!!!!M 103 !!!!!!!!!NGC 637 !!!!!!!!!NGC 654 !!!!!!!!!NGC 659 !!!!!!!!!PacMan Nebula !!!!!!!!!Owl Cluster !!!!!!!!!NGC 663 Asterisms!! in Constellation!Stars!!Objects nearby 02 Northern Fly!!Aries!!!41 Arietis !!!!!!!39 Arietis!!! !!!!!!!35 Arietis !!!!!!!!!!NGC 1056 02 Whale’s Head!!Cetus!! ! Menkar !!!!!!!Lambda Ceti! !!!!!!!Mu Ceti !!!!!!!Xi2 Ceti !!!!!!!Kaffalijidhma !!!!!!!!!!IC 302 !!!!!!!!!!NGC 990 !!!!!!!!!!NGC 1024 !!!!!!!!!!NGC 1026 !!!!!!!!!!NGC 1070 !!!!!!!!!!NGC 1085 !!!!!!!!!!NGC 1107 !!!!!!!!!!NGC 1137 !!!!!!!!!!NGC 1143 !!!!!!!!!!NGC 1144 !!!!!!!!!!NGC 1153 Asterisms!! in Constellation Stars!!Objects nearby 03 Hyades!!!Taurus! Aldebaran !!!!!! Theta 2 Tauri !!!!!! Gamma Tauri !!!!!! Delta 1 Tauri !!!!!! Epsilon Tauri !!!!!!!!!Struve’s Lost Nebula !!!!!!!!!Hind’s Variable Nebula !!!!!!!!!IC 374 03 Kids!!!Auriga! Almaaz !!!!!! Hoedus II !!!!!! Hoedus I !!!!!!!!!The Kite Cluster !!!!!!!!!IC 397 03 Pleiades!! ! Taurus! Pleione (Seven Sisters)!! ! ! Atlas !!!!!! Alcyone !!!!!! Merope !!!!!! Electra !!!!!! Celaeno !!!!!! Taygeta !!!!!! Asterope !!!!!! Maia !!!!!!!!!Maia Nebula !!!!!!!!!Merope Nebula !!!!!!!!!Merope -
Pahs in the Halo of NGC 5529
Astronomy & Astrophysics manuscript no. irwin c ESO 2018 October 25, 2018 PAHs in the Halo of NGC 5529 J. A. Irwin1, H. Kennedy1, T. Parkin1, and S. Madden2 1 Dept. of Physics, Engineering Physics, & Astronomy, Queen’s University, Kingston, Canada, K7L 3N6 e-mail: [email protected] 2 CEA/Saclay, Service d’Astrophysique, Orme des Merisiers, Bˆatiment 709, 91191 Gif-sur-Yvette cedex, France e-mail: [email protected] Received 00 month 0000; accepted 00 month 0000 ABSTRACT We present sensitive ISO λ 6.7 µm observations of the edge-on galaxy, NGC 5529, finding an extensive MIR halo around NGC 5529. The emission is dominated by PAHs in this band. The PAH halo has an exponential scale height of 3.7 kpc but can still be detected as far as ≈ 10 kpc from the plane to the limits of the high dynamic range (1770/1) data. This is the most extensive PAH halo yet detected in a normal galaxy. This halo shows substructure and the PAHs likely originate from some type of disk outflow. PAHs are long-lived in a halo environment and therefore continuous replenishment from the disk is not required (unless halo PAHs are also being destroyed or removed), consistent with the current low SFR of the galaxy. The PAHs correlate spatially with halo Hα emission, previously observed by Miller & Veilleux (2003); both components are likely excited/ionized by in-disk photons that are leaking into the halo. The presence of halo gas may be related to the environment of NGC 5529 which contains at least 17 galaxies in a small group of which NGC 5529 is the dominant member. -
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. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Nearby Supernova Host Galaxies from the CALIFA Survey: II. SN
Astronomy & Astrophysics manuscript no. IFU_P2_v10 c ESO 2018 June 17, 2018 Nearby supernova host galaxies from the CALIFA Survey: II. SN environmental metallicity L. Galbany1, 2, V. Stanishev3, A. M. Mourão3, M. Rodrigues4, 5, H. Flores5, C. J. Walcher6, S. F. Sánchez7, R. García-Benito8, D. Mast9, C. Badenes10, R. M. González Delgado8, C. Kehrig8, M. Lyubenova11, R. A. Marino12, 13 M. Mollá14, S. Meidt15, E. Pérez8, G. van de Ven15, J. M. Vílchez8 (Affiliations can be found after the references) Received December 26th / Accepted ————- ABSTRACT The metallicity of a supernova progenitor, together with its mass, is one of the main parameters that can rule their outcome. We present the second study of nearby supernova (SN) host galaxies (0.005 < z < 0.03) using Integral Field Spectroscopy (IFS) from the CALIFA survey. We analyze the metallicity of 115 galaxies, which hosted 132 SNe within and 10 SNe outside the field-of-view (FoV) of the instrument. Further 18 galaxies, which hosted only SNe outside the FoV were also studied. Using the O3N2 calibrator from Marino et al. (2013) we found no statistically significant differences between the gas-phase metallicities at the locations of the three main SN types – Ia, Ib/c and II, all having 12 + log(O/H) ≃ 8.50 within 0.02 dex. The total galaxy metallicities are also very similar and we argue that this is because our sample consists only of SNe discovered in massive galaxies (log(M/M⊙) > 10 dex) by targeted searches. We also found no evidence that the metallicity at the SN location differs from the average metallicity at the galactocentric distance of the SNe.