Cycle 14 Approved Programs
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RADIAL VELOCITIES in the ZODIACAL DUST CLOUD
A SURVEY OF RADIAL VELOCITIES in the ZODIACAL DUST CLOUD Brian Harold May Astrophysics Group Department of Physics Imperial College London Thesis submitted for the Degree of Doctor of Philosophy to Imperial College of Science, Technology and Medicine London · 2007 · 2 Abstract This thesis documents the building of a pressure-scanned Fabry-Perot Spectrometer, equipped with a photomultiplier and pulse-counting electronics, and its deployment at the Observatorio del Teide at Izaña in Tenerife, at an altitude of 7,700 feet (2567 m), for the purpose of recording high-resolution spectra of the Zodiacal Light. The aim was to achieve the first systematic mapping of the MgI absorption line in the Night Sky, as a function of position in heliocentric coordinates, covering especially the plane of the ecliptic, for a wide variety of elongations from the Sun. More than 250 scans of both morning and evening Zodiacal Light were obtained, in two observing periods – September-October 1971, and April 1972. The scans, as expected, showed profiles modified by components variously Doppler-shifted with respect to the unshifted shape seen in daylight. Unexpectedly, MgI emission was also discovered. These observations covered for the first time a span of elongations from 25º East, through 180º (the Gegenschein), to 27º West, and recorded average shifts of up to six tenths of an angstrom, corresponding to a maximum radial velocity relative to the Earth of about 40 km/s. The set of spectra obtained is in this thesis compared with predictions made from a number of different models of a dust cloud, assuming various distributions of dust density as a function of position and particle size, and differing assumptions about their speed and direction. -
Pos(INTEGRAL 2010)091
A candidate former companion star to the Magnetar CXOU J164710.2-455216 in the massive Galactic cluster Westerlund 1 PoS(INTEGRAL 2010)091 P.J. Kavanagh 1 School of Physical Sciences and NCPST, Dublin City University Glasnevin, Dublin 9, Ireland E-mail: [email protected] E.J.A. Meurs School of Cosmic Physics, DIAS, and School of Physical Sciences, DCU Glasnevin, Dublin 9, Ireland E-mail: [email protected] L. Norci School of Physical Sciences and NCPST, Dublin City University Glasnevin, Dublin 9, Ireland E-mail: [email protected] Besides carrying the distinction of being the most massive young star cluster in our Galaxy, Westerlund 1 contains the notable Magnetar CXOU J164710.2-455216. While this is the only collapsed stellar remnant known for this cluster, a further ~10² Supernovae may have occurred on the basis of the cluster Initial Mass Function, possibly all leaving Black Holes. We identify a candidate former companion to the Magnetar in view of its high proper motion directed away from the Magnetar region, viz. the Luminous Blue Variable W243. We discuss the properties of W243 and how they pertain to the former Magnetar companion hypothesis. Binary evolution arguments are employed to derive a progenitor mass for the Magnetar of 24-25 M Sun , just within the progenitor mass range for Neutron Star birth. We also draw attention to another candidate to be member of a former massive binary. 8th INTEGRAL Workshop “The Restless Gamma-ray Universe” Dublin, Ireland September 27-30, 2010 1 Speaker Copyright owned by the author(s) under the terms of the Creative Commons Attribution-NonCommercial-ShareAlike Licence. -
1 Director's Message
1 Director’s Message Markus Kissler-Patig 3 Weighing the Black Hole in M101 ULX-1 Stephen Justham and Jifeng Liu 8 World’s Most Powerful Planet Finder Turns its Eye to the Sky: First Light with the Gemini Planet Imager Bruce Macintosh and Peter Michaud 12 Science Highlights Nancy A. Levenson 15 Operations Corner: Update and 2013 Review Andy Adamson 20 Instrumentation Development: Update and 2013 Review Scot Kleinman ON THE COVER: GeminiFocus January 2014 The cover of this issue GeminiFocus is a quarterly publication of Gemini Observatory features first light images from the Gemini 670 N. A‘ohoku Place, Hilo, Hawai‘i 96720 USA Planet Imager that Phone: (808) 974-2500 Fax: (808) 974-2589 were released at the Online viewing address: January 2014 meeting www.gemini.edu/geminifocus of the American Managing Editor: Peter Michaud Astronomical Society Science Editor: Nancy A. Levenson held in Washington, D.C. Associate Editor: Stephen James O’Meara See the press release Designer: Eve Furchgott / Blue Heron Multimedia that accompanied the images starting on Any opinions, findings, and conclusions or recommendations page 8 of this issue. expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. Markus Kissler-Patig Director’s Message 2013: A Successful Year for Gemini! As 2013 comes to an end, we can look back at 12 very successful months for Gemini despite strong budget constraints. Indeed, 2013 was the first stage of our three-year transition to a reduced opera- tions budget, and it was marked by a roughly 20 percent cut in contributions from Gemini’s partner countries. -
Disks in Nearby Planetary Systems with JWST and ALMA
Disks in Nearby Planetary Systems with JWST and ALMA Meredith A. MacGregor NSF Postdoctoral Fellow Carnegie Department of Terrestrial Magnetism 233rd AAS Meeting ExoPAG 19 January 6, 2019 MacGregor Circumstellar Disk Evolution molecular cloud 0 Myr main sequence star + planets (?) + debris disk (?) Star Formation > 10 Myr pre-main sequence star + protoplanetary disk Planet Formation 1-10 Myr MacGregor Debris Disks: Observables First extrasolar debris disk detected as “excess” infrared emission by IRAS (Aumann et al. 1984) SPHERE/VLT Herschel ALMA VLA Boccaletti et al (2015), Matthews et al. (2015), MacGregor et al. (2013), MacGregor et al. (2016a) Now, resolved at wavelengthsfrom from Herschel optical DUNES (scattered light) to millimeter and radio (thermal emission) MacGregor Planet-Disk Interactions Planets orbiting a star can gravitationally perturb an outer debris disk Expect to see a variety of structures: warps, clumps, eccentricities, central offsets, sharp edges, etc. Goal: Probe for wide separation planets using debris disk structure HD 15115 β Pictoris Kuiper Belt Asymmetry Warp Resonance Kalas et al. (2007) Lagrange et al. (2010) Jewitt et al. (2009) MacGregor Debris Disks Before ALMA Epsilon Eridani HD 95086 Tau Ceti Beta PictorisHR 4796A HD 107146 AU Mic Greaves+ (2014) Su+ (2015) Lawler+ (2014) Vandenbussche+ (2010) Koerner+ (1998) Hughes+ (2011) Matthews+ (2015) 49 Ceti HD 181327 HD 21997 Fomalhaut HD 10647 (q1 Eri) Eta Corvi HR 8799 Roberge+ (2013) Lebreton+ (2012) Moor+ (2015) Acke+ (2012) Liseau+ (2010) Lebreton+ (2016) -
Super Stellar Clusters with a Bimodal Hydrodynamic Solution: an Approximate Analytic Approach
A&A 471, 579–583 (2007) Astronomy DOI: 10.1051/0004-6361:20077282 & c ESO 2007 Astrophysics Super stellar clusters with a bimodal hydrodynamic solution: an approximate analytic approach R. Wünsch1, S. Silich2, J. Palouš1, and G. Tenorio-Tagle2 1 Astronomical Institute, Academy of Sciences of the Czech Republic, v.v.i., Bocníˇ II 1401, 141 31 Prague, Czech Republic e-mail: [email protected] 2 Instituto Nacional de Astrofísica Optica y Electrónica, AP 51, 72000 Puebla, Mexico Received 12 February 2007 / Accepted 22 May 2007 ABSTRACT Aims. We look for a simple analytic model to distinguish between stellar clusters undergoing a bimodal hydrodynamic solution from those able to drive only a stationary wind. Clusters in the bimodal regime undergo strong radiative cooling within their densest inner regions, which results in the accumulation of the matter injected by supernovae and stellar winds and eventually in the formation of further stellar generations, while their outer regions sustain a stationary wind. Methods. The analytic formulae are derived from the basic hydrodynamic equations. Our main assumption, that the density at the star cluster surface scales almost linearly with that at the stagnation radius, is based on results from semi-analytic and full numerical calculations. Results. The analytic formulation allows for the determination of the threshold mechanical luminosity that separates clusters evolving in either of the two solutions. It is possible to fix the stagnation radius by simple analytic expressions and thus to determine the fractions of the deposited matter that clusters evolving in the bimodal regime blow out as a wind or recycle into further stellar generations. -
Arxiv:2005.00801V2 [Astro-Ph.GA] 15 May 2020
Noname manuscript No. (will be inserted by the editor) The Physics of Star Cluster Formation and Evolution Martin G. H. Krause · Stella S. R. Offner · Corinne Charbonnel · Mark Gieles · Ralf S. Klessen · Enrique V´azquez-Semadeni · Javier Ballesteros-Paredes Philipp Girichidis · J. M. Diederik Kruijssen · Jacob L. Ward · Hans Zinnecker Received: 31 Jan 2020 / Accepted: date Martin G. H. Krause Centre for Astrophysics Research, School of Physics, Astronomy and Mathematics, University of Hertfordshire, College Lane, Hatfield, Hertfordshire AL10 9AB, UK E-mail: [email protected] Stella S. R. Offner Department of Astronomy, The University of Texas, Austin TX, 78712, U.S.A. Corinne Charbonnel Department of Astronomy, University of Geneva, Chemin de Pegase 51, 1290 Versoix, Switzer- land; IRAP, CNRS & Univ. of Toulouse, 14, av.E.Belin, 31400 Toulouse, France Mark Gieles Institut de Ci`enciesdel Cosmos (ICCUB-IEEC), Universitat de Barcelona, Mart´ıi Franqu`es 1, 08028 Barcelona, Spain; ICREA, Pg. Lluis Companys 23, 08010 Barcelona, Spain Ralf S. Klessen Universit¨at Heidelberg, Zentrum f¨ur Astronomie, Institut f¨ur Theoretische Astrophysik, Albert-Ueberle-Str. 2, 69120 Heidelberg, Germany Enrique V´azquez-Semadeni Instituto de Radioastronom´ıay Astrof´ısica,Universidad Nacional Aut´onomade M´ex´ıco,Cam- pus Morelia, Apdo. Postal 3-72, Morelia 58089, M´exico Javier Ballesteros-Paredes Instituto de Radioastronom´ıay Astrof´ısica,Universidad Nacional Aut´onomade M´ex´ıco,Cam- pus Morelia, Apdo. Postal 3-72, Morelia 58089, M´exico Philipp Girichidis Leibniz-Institut f¨urAstrophysik (AIP), An der Sternwarte 16, 14482 Potsdam, Germany J. M. Diederik Kruijssen Astronomisches Rechen-Institut, Zentrum f¨ur Astronomie der Universit¨at Heidelberg, M¨onchhofstraße 12-14, 69120 Heidelberg, Germany Jacob L. -
A Super-Star Cluster in NGC 253: Mid-Infrared Properties
THE ASTROPHYSICAL JOURNAL, 518:183È189, 1999 June 10 ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. A SUPERÈSTAR CLUSTER IN NGC 253: MID-INFRARED PROPERTIES ERIC KETO,JOSEPH L. HORA, AND G. G. FAZIO Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 WILLIAM HOFFMANN Steward Observatory, University of Arizona, Tucson, AZ 85721 AND LYNNE DEUTSCH Astronomy Department, Boston University, 725 Commonwealth Avenue, Boston, MA 02215 Received 1998 February 26; accepted 1999 January 12 ABSTRACT We observed the nearby starburst galaxy NGC 253 in the mid-infrared to obtain a three-dimensional data set with arcsecond angular resolution and 0.2 km spectral resolution. The observations show the major spectral features in the upper half of the mid-IR window: the 11.3 km polycyclic aromatic hydro- carbon (PAH) line and the 12.8 km [Ne II] line as well as the broad silicate absorption feature at 9.7 km. We use the [Ne II] line to determine the emission measure of the ionized gas, and in combination with radio observations to predict the thermal and nonthermal contributions to the radio continuum. The amount of ionized gas is related to the rate of star formation. Based on the mid-IR spectra, we identify three major components in the nucleus of NGC 243: an AGN in the center of the galaxy, a superÈstar cluster also seen in optical images, and a larger scale di†use envelope composed of an older population of supernova remnants and lower mass stars. Subject headings: galaxies: individual (NGC 253) È galaxies: starburst È galaxies: star clusters 1. -
Signatures of Giant Planets on the Solar System Kuiper Belt Dust Disk and Implications for Extrasolar Planet in Epsilon Eridani
Lunar and Planetary Science XXX 1698.pdf SIGNATURES OF GIANT PLANETS ON THE SOLAR SYSTEM KUIPER BELT DUST DISK AND IMPLICATIONS FOR EXTRASOLAR PLANET IN EPSILON ERIDANI. J.-C. Liou1 and H. A. Zook2, 1GB Tech/Lockheed Martin, C104 Lockheed Martin, 2400 NASA Rd. One, Houston, TX 77058, 2SN2, NASA Johnson Space Center, Houston, TX 77052. Summary: One method to detect extrasolar Dust disks in Beta Pictoris, Epsilon Eridani, planetary systems is to deduce the perturbations of and other systems are analogues to our Solar Sys- planets on the observed circumstellar dust disks. tem’s Kuiper Belt dust disk. Therefore, it is of Our Solar System, with its known configuration of great interest to understanding how the Kuiper planets, provide an excellent example to study how Belt IDP distribution is affected by the giant plan- the distribution of dust particles is affected by the ets in our Solar System. We have numerically existence of different planets. Numerical simula- simulated the orbital evolution of Kuiper Belt tions of the orbital evolution of dust particles from IDPs, including gravitational perturbations from 7 Kuiper Belt objects show that the four giant plan- planets (Mercury and Pluto are not included due to ets, especially Neptune and Jupiter, impose distinct their small masses), solar radiation pressure, and and dramatic signatures on the overall distribution PR and solar wind drag. Dust particles range from of Kuiper belt dust particles. The signatures are 3 to 23 micrometers in diameter. For a given size, very similar to those observed in Epsilon Eridani. 100 IDPs are included in the simulations. -
Extrasolar Systems Shed Light on Our
NEWS FEATURE NEWS FEATURE Extrasolar systems shed light on our own Amazing as the discoveries of planets, comets, and asteroid belts around other stars are, it’s their potential to shed light on our Solar System’s origins that is exciting astronomers. Nadia Drake broader sense, we’re trying to understand Science Writer if our own world—and our own Solar Sys- tem—is ‘normal,’” says David Grinspoon, Chair of Astrobiology at the US Library of A planet smaller than Mercury circles a star astronomers can use the Solar System’s ar- Congress in Washington, DC, “or, in some 210 light-years away. Around another star, chitecture to predict the presence of un- extraordinary way, abnormal.” two planets live so close together that each seen objects in these systems, and use the periodically rises in the other’s sky. Other systems to learn more about the celestial Chasing Comets alien skies are home to two suns that rise events that gave birth to and shaped our One stellar system with a recently identified and set, casting double shadows over their Solar System. kinship to ours is that of Vega. This famil- double-sunned worlds. Planets so dense “We definitely learn more about the Solar iar star burns brightly in the northern sky, they might have diamond rinds, worlds System’s past and future by observing other where it forms a summertime triangle with whose year is shorter than an Earthday, oth- stellar systems,” says astronomer Kate Su stars Deneb and Altair. Just 25 light-years ers that orbit their star backward—the cos- of the University of Arizona, Tucson, AZ. -
Spectral Classification of Stars
29:50 Astronomy Lab #6 Stars, Galaxies, and the Universe Name Partner(s) Date Grade Category Max Points Points Received On Time 5 Printed Copy 5 Lab Work 90 Total 100 Spectral Classification of Stars 1. Introduction Scientists across all fields use classification systems to help them sub-divide the vast universe of objects and phenomena into smaller groups, making them easier to study. In biology, life can be categorized by cellular properties. Animals are separated from plants, cats separated from dogs, oak trees separated from pine trees, etc. This framework allows biologists to better understand how processes are FIGURE 1: SPECTRUM OF VEGA interconnected and quickly predict characteristics of newly discovered species. In Astronomy, the stellar classification system allows scientists to understand the p r o p e r t i e s o f s t a r s . E a r l y astronomers began to realize that the extensive number of stars exhibited patterns related to the starʼs color and temperature. This classification was good, but had limitations (especially for studying distant stars). By the early 1900ʼs, a classification system based on the observed stellar spectra was developed and is still used today. A STELLAR SPECTRUM is a measurement of a 1 Spectral Classification of Stars starʼs brightness across of range of wavelengths (or frequencies). It is in a sense a “fingerprint” for the star, containing features that reveal the chemical composition, age, and temperature. This measurement is made by “breaking up” the light from the star into individual wavelengths, much like how a prism or a raindrop separates the sunlight into a rainbow. -
1411 (Created: Wednesday, June 24, 2020 at 12:00:37 AM Eastern Standard Time) - Overview
JWST Proposal 1411 (Created: Wednesday, June 24, 2020 at 12:00:37 AM Eastern Standard Time) - Overview 1411 - Coronagraphy of the Debris Disk Archetype Beta Pictoris Cycle: 1, Proposal Category: GTO INVESTIGATORS Name Institution E-Mail Dr. Christopher C. Stark (PI) Space Telescope Science Institute [email protected] Dr. Laurent Pueyo (CoI) Space Telescope Science Institute [email protected] Dr. Marshall Perrin (CoI) Space Telescope Science Institute [email protected] Dr. Remi Soummer (CoI) Space Telescope Science Institute [email protected] Dr. Matt Mountain (CoI) Space Telescope Science Institute [email protected] Abhijith Rajan (CoI) Space Telescope Science Institute [email protected] Dr. Mark Clampin (CoI) NASA Goddard Space Flight Center [email protected] OBSERVATIONS Folder Observation Label Observing Template Science Target Beta Pic with MIRI coronagraphs 1 Beta Pic - 2300 Lyot R MIRI Coronagraphic Imaging (1) BETA-PIC oll 1 2 Beta Pic - 1550 4QPM MIRI Coronagraphic Imaging (1) BETA-PIC Roll 1 3 Beta Pic - 1550 4QPM MIRI Coronagraphic Imaging (1) BETA-PIC Roll 2 4 Beta Pic - 2300 Lyot R MIRI Coronagraphic Imaging (1) BETA-PIC oll 2 5 Alpha Pic - 2300 Lyot MIRI Coronagraphic Imaging (2) ALPHA-PIC PSF 6 Alpha Pic - 1550 4QP MIRI Coronagraphic Imaging (2) ALPHA-PIC M PSF Beta Pic with NIRCam Coronagraphs 7 Alpha Pic - LW PSF NIRCam Coronagraphic Imaging (2) ALPHA-PIC 1 JWST Proposal 1411 (Created: Wednesday, June 24, 2020 at 12:00:37 AM Eastern Standard Time) - Overview Folder Observation Label Observing Template Science Target 8 Alpha Pic - SW PSF NIRCam Coronagraphic Imaging (2) ALPHA-PIC 10 Beta Pic - SW Roll 1 NIRCam Coronagraphic Imaging (1) BETA-PIC 11 Beta Pic - SW Roll 2 NIRCam Coronagraphic Imaging (1) BETA-PIC 12 Beta Pic - LW Roll 2 NIRCam Coronagraphic Imaging (1) BETA-PIC 13 Beta Pic - LW Roll 1 NIRCam Coronagraphic Imaging (1) BETA-PIC ABSTRACT The famous debris disk around Beta Pic was the first circumstellar disk to be spatially resolved. -
A1 F2015 Review Copy.Key
Review Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015 Quotes & Cartoon of the Day “One may wonder, What came before? If space-time did not exist then, how could everything appear from nothing? . Explaining this initial singularity—where and when it all began—still remains the most intractable problem of modern cosmology. — Andrei Linde “But who shall dwell in these worlds if they be inhabited? ... Are we or they Lords of the World? ... And how are all things made for man?” — Johannes Kepler “Our sun is one of 100 billion stars in our galaxy. Our galaxy is one of billions of galaxies populating the universe. It would be the height of presumption to think that we are the only living things in that enormous immensity.” — Wernher von Braun Astronomy 1 - Elementary Astronomy LA Mission College Levine F2015 Announcements • Observing Project & Extra Credit Due • Midterm graded & gradebook updated to drop lowest • remainder of grading (hopefully) updated this weekend • Final 12/15 at 10-12 AM! Astronomy 1 - Elementary Astronomy LA Mission College Levine F2015 Last Class • Debrief Midterm • Debrief LT • Cosmology & Fate of the Universe • Exoplanets (time permitting) Astronomy 1 - Elementary Astronomy LA Mission College Levine F2015 This Class • Review/Debrief Midterm • Exoplanets (time permitting) Astronomy 1 - Elementary Astronomy LA Mission College Levine F2015 About the Final Astronomy 1 — Elementary Astronomy LA Mission College Spring F2015 About the Final • Similar format to Midterms • Similar length • a little longer,