DOCSLIB.ORG

Annual Report 1999

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Annual Report 1999 Astronomy at the University of Canterbury Department of Physics and Astronomy and Mt John University Observatory | annual report 1999 Director: Prof. J.B. Hearnshaw Report for the period 1 January 1999 to 31 December 1999 1 Sta® Assoc. Prof. Peter Cottrell continued as Head of Department in 1999, Prof. John Hearn- shaw continued as Mt John director and Alan Gilmore as Mt John superintendent. Cottrell continued to serve on the Carter Observatory board as deputy chair in 1999, and on the organizing committees of IAU Commissions 27 (variable stars) and 29 (stellar spectra). He was also elected to the council of the Astronomical Society of Australia in July. Dr William Tobin continued on a half-time lectureship in 1999, working the ¯rst six months of the year in Christchurch and the remainder in France. Dr Karen Pollard was appointed to a temporary lectureship in astronomy for the second half of the year. Dr John Pritchard continued as a Marsden-¯nanced postdoctoral fellow until October when he left to take up a New Zealand-funded fellowship at the Niels Bohr Institute of Astronomy in Copenhagen. Other post-doctoral fellows were Michael Albrow (supported by the Marsden Fund), Karen Pollard (New Zealand Foundation for Research, Science and Technology Postdoctoral Fellow) and Ian Bond (the last being based at Mt John on a Marsden-funded fellowship with the MOA project). Stephen Barlow was promoted to technician grade 3. Hearnshaw continued as president of IAU Commission 30 (radial velocities) and Prof. Jack Baggaley as president of IAU Commission 22 (meteors and interplane- tary dust) during the year. Hearnshaw also served on the board of IAU Div. IX (optical techniques), on the IAU Working Group for the world-wide development of astronomy, and he served on the council of the Royal Astron. Soc. of N.Z. as fellows' representative. 2 Students In March, Stuart Barnes completed his MSc research with the support of the Mars- den Fund (supervisor Tobin) on the H and K lines of ¯ Pictoris and 51 Ophiuchi and was awarded an MSc with ¯rst class honours. He then commenced a PhD work- ing on the Hercules spectrograph project (supervisor Hearnshaw) with the support 1 of a University of Canterbury doctoral scholarship. At the end of the year, two students submitted PhD theses: they were Lyndon Watson (supervisor Hearnshaw) with a thesis on active-chromosphere stars with EUV emission, and Jovan Skuljan (supervisors Hearnshaw and Cottrell) on moving groups of stars in the Galaxy. In mid-1999 Daniel Pooley (supervisors Cottrell, Albrow, Pollard) took leave from his PhD research on AGB stars for the remainder of the year and travelled to Europe. The following students have continued their PhD research during the year: Ljil- jana Skuljan (supervisor Cottrell) on RCB stars; Orlon Petterson on binary cepheid variables (supervisors Cottrell and Albrow); Jennifer McSaveney (supervisors Cot- trell and Pollard) on RV Tauri stars; Glenn Bayne (supervisors Tobin, Bond, Pritchard and Pollard) on eclipsing binary stars in the Magellanic Clouds. 3 Visitors We had several astronomical visitors in 1999. Dr Frank Fekel, from Tennessee State University, came from late February until mid-April as an Erskine Fellow, and gave lectures to third-year astronomy students on variable stars. In May Drs M. Honma (Tokyo) and Y. Kanya (Kyoto) gave a joint seminar on microlensing and dark mat- ter. In June Dr Bill Sheehan (based temporarily in Timaru) gave an historical talk on the American astronomer E.E. Barnard. Prof. Brian Warner (Cape Town) also came in June and gave seminars on novae and on white dwarfs, neutron stars and black holes (the second talk was a public one arranged by the Canterbury Astronom- ical Society). Dr David Buckley from SAAO (Cape Town), a former MSc graduate of Canterbury, visited in August. Prof. Leon Mestel (Sussex UK) visited and gave a seminar on stellar magnetism in October; Prof. Michael Bessell (A.N.U., Canberra) and Peter Gillingham (AAO, Epping) visited in November as part of the feasibil- ity study for New Zealand joining the Southern African Large Telescope (SALT) project (see under miscellaneous below). Dr Penny Sackett (Groningen, Holland) gave a seminar on microlensing in November. In addition, there have been numerous visitors in November for a meeting of the PLANET group (Drs P. Sackett, Groningen; M. Dominik, Groningen; J. Menzies, SAAO; J.-P. Beaulieu, IAP, Paris; A. Gould, Ohio State Univ.; D. Depoy, Ohio State Univ.; K. Sahu, Space Telescope Science Inst.; A. Williams, Perth Observ.; J. Green- hill, Univ. Tasmania and S. Gaudi, Ohio State Univ.) organized at Canterbury by Karen Pollard and Michael Albrow, and there were also visitors at Mt John during the year for the MOA project (including Prof. Yasushi Muraki, Nagoya Univ. and Dr Mine Takeuti, Tohoku Univ., Japan). Drs Ian Gri±n (Auckland Observatory, studying near-Earth asteroids), Phil Yock (Auckland Univ., MOA project) and De- nis Sullivan (Victoria Univ. Wellington, Whole-Earth Telescope project) all visited Mt John to make observations in 1999. Dr Denis Sullivan and MSc student Tiri Sullivan (both Victoria Univ. Welling- 2 ton) made three observing runs to Mt John in 1999. All were for photoelectric photometry of pulsating degenerate stars. The visit in April was part of the Whole Earth Telescope (WET) program. In April a team from Imperial College London (Drs Wooder and Rigal) and from the Canterbury Electrical and Electronic Engineering Dept. (Drs R. Lane and P. Bones) undertook Scidar measurements of the atmospheric turbulence height distribution on the 1-metre telescope. Cottrell and Honours student Dane Kent participated in this work and as a result they investigated a possible adaptive optics system for Mt John. The height distribution of turbulence indicated most turbulence at low levels in close proximity to the ground. 4 Conferences Seven Canterbury astronomers attended the second joint RASNZ/ASA conference and associated astronomy education meeting in Sydney in July (Adams, Barnes, Bayne, Cottrell, Petterson, Pollard, Tobin). Cottrell served as co-chair of the orga- nizing committee for this joint meeting. Tobin presented there an oral paper (with Pritchard, Zainuddin and Bayne) on Magellanic Cloud eclipsing binaries. Tobin, Barnes and Pollard also gave a poster paper on ¯ Pictoris. Pollard gave an oral pa- per on selected results from the PLANET collaboration at this meeting and Albrow and Pollard presented a poster on variable star research in the PLANET collabora- tion. Petterson, Cottrell and Albrow had a poster paper on cepheids and Cottrell gave an oral presentation on New Zealand participation in SALT at a session on future options for Australasian optical/IR astronomy. Dr Jenni Adams gave an invited talk on neutrino telescopes in Antarctica. Four members of the group attended and gave papers at IAU Colloquium 176 on The impact of large-scale surveys on pulsating star research in Budapest, Hungary, in August (Albrow, Hearnshaw, Pollard, L. Skuljan). Since this meeting marked the centenary of the Konkoly Observatory as a state institution in Hungary, Hearnshaw gave an introductory historical address to mark this occasion, as well as a paper on photometry of variable stars in the Magellanic Clouds, observed in the MOA project. Pollard gave an invited review on RV Tauri stars and type II cepheids in the Magellanic Clouds, as well as a poster paper on a spectroscopic survey of RV Tauri stars in the Clouds (with T. Lloyd Evans, SAAO). Pritchard attended a meeting for the opening of the Very Large Telescope in Antofagasta, Chile in March, and gave an oral paper on Magellanic Cloud eclipsing binaries. Pollard was a speaker at a conference on women in science at the Univ. of Otago in June. Bond attended the Ninth international conference on astronomical data analysis and software in Hawaii in November. He presented there a paper on time critical analysis by image subtraction. N. Rattenbury (the Mt John MOA winter observer for 1999) gave a paper on searching for optical afterglows of GRBs at the Fifth Huntsville GRB symposium. Barnes and Bayne were participants in 3 the Harley Wood Summer School (Sydney, July) and L. Skuljan in the conference for PhD students in astronomy in Kecskemet, Hungary in August and gave a paper on RCB decline phases. Hearnshaw went to a workshop on the history of astronomy at Tihany, Lake Balaton, Hungary in August and gave a paper on the history of photographic photometry. A PLANET microlensing workshop was organized by Pollard and Albrow in the Dept. of Physics and Astronomy in November. While in Hungary, four Canterbury astronomers all witnessed a magni¯cent total eclipse of the Sun on August 11 under clear skies. William Tobin in France was also in the eclipse path, and reported that what he saw `remained grandiose even when viewed from under clouds'. 5 Instrumentation The Hercules spectrograph construction has continued during 1999 under John Hearnshaw as project leader, with the collaboration of Graeme Kershaw (mechani- cal) and Garry Nankivell (Lower Hutt) for optical fabrication. Barnes has worked on the project for his PhD thesis. The ¶echelle grating for the spectrograph was pur- chased from Spectronics Inc. (Rochester, N.Y.) and the BK7 cross-dispersing prism was received and sent to D. Cochrane (IRL, Lower Hutt) for optical ¯guring and polishing. Good progress has been made, and it is anticipated that the spectrograph will be assembled and tested in 2000. Barlow and Frost have installed an SBIG guide camera on the CCD photometer head, which will enable autoguiding. Pritchard, with the assistance of Andrew Richards, has written a Linux-based data acquisition program called MoJo for the Mt John SITe CCD camera and in- stalled this at Mt John in early August. It has been in routine use for all CCD camera operations on the 1-m telescope since that time.
Load more

Recommended publications
  • Naming the Extrasolar Planets
    Naming the extrasolar planets W. Lyra Max Planck Institute for Astronomy, K¨onigstuhl 17, 69177, Heidelberg, Germany [email protected] Abstract and OGLE-TR-182 b, which does not help educators convey the message that these planets are quite similar to Jupiter. Extrasolar planets are not named and are referred to only In stark contrast, the sentence“planet Apollo is a gas giant by their assigned scientific designation. The reason given like Jupiter” is heavily - yet invisibly - coated with Coper- by the IAU to not name the planets is that it is consid- nicanism. ered impractical as planets are expected to be common. I One reason given by the IAU for not considering naming advance some reasons as to why this logic is flawed, and sug- the extrasolar planets is that it is a task deemed impractical. gest names for the 403 extrasolar planet candidates known One source is quoted as having said “if planets are found to as of Oct 2009. The names follow a scheme of association occur very frequently in the Universe, a system of individual with the constellation that the host star pertains to, and names for planets might well rapidly be found equally im- therefore are mostly drawn from Roman-Greek mythology. practicable as it is for stars, as planet discoveries progress.” Other mythologies may also be used given that a suitable 1. This leads to a second argument. It is indeed impractical association is established. to name all stars. But some stars are named nonetheless. In fact, all other classes of astronomical bodies are named.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 # Name Mass Star Name
    exoplanet.eu_catalog # name mass star_name star_distance star_mass OGLE-2016-BLG-1469L b 13.6 OGLE-2016-BLG-1469L 4500.0 0.048 11 Com b 19.4 11 Com 110.6 2.7 11 Oph b 21 11 Oph 145.0 0.0162 11 UMi b 10.5 11 UMi 119.5 1.8 14 And b 5.33 14 And 76.4 2.2 14 Her b 4.64 14 Her 18.1 0.9 16 Cyg B b 1.68 16 Cyg B 21.4 1.01 18 Del b 10.3 18 Del 73.1 2.3 1RXS 1609 b 14 1RXS1609 145.0 0.73 1SWASP J1407 b 20 1SWASP J1407 133.0 0.9 24 Sex b 1.99 24 Sex 74.8 1.54 24 Sex c 0.86 24 Sex 74.8 1.54 2M 0103-55 (AB) b 13 2M 0103-55 (AB) 47.2 0.4 2M 0122-24 b 20 2M 0122-24 36.0 0.4 2M 0219-39 b 13.9 2M 0219-39 39.4 0.11 2M 0441+23 b 7.5 2M 0441+23 140.0 0.02 2M 0746+20 b 30 2M 0746+20 12.2 0.12 2M 1207-39 24 2M 1207-39 52.4 0.025 2M 1207-39 b 4 2M 1207-39 52.4 0.025 2M 1938+46 b 1.9 2M 1938+46 0.6 2M 2140+16 b 20 2M 2140+16 25.0 0.08 2M 2206-20 b 30 2M 2206-20 26.7 0.13 2M 2236+4751 b 12.5 2M 2236+4751 63.0 0.6 2M J2126-81 b 13.3 TYC 9486-927-1 24.8 0.4 2MASS J11193254 AB 3.7 2MASS J11193254 AB 2MASS J1450-7841 A 40 2MASS J1450-7841 A 75.0 0.04 2MASS J1450-7841 B 40 2MASS J1450-7841 B 75.0 0.04 2MASS J2250+2325 b 30 2MASS J2250+2325 41.5 30 Ari B b 9.88 30 Ari B 39.4 1.22 38 Vir b 4.51 38 Vir 1.18 4 Uma b 7.1 4 Uma 78.5 1.234 42 Dra b 3.88 42 Dra 97.3 0.98 47 Uma b 2.53 47 Uma 14.0 1.03 47 Uma c 0.54 47 Uma 14.0 1.03 47 Uma d 1.64 47 Uma 14.0 1.03 51 Eri b 9.1 51 Eri 29.4 1.75 51 Peg b 0.47 51 Peg 14.7 1.11 55 Cnc b 0.84 55 Cnc 12.3 0.905 55 Cnc c 0.1784 55 Cnc 12.3 0.905 55 Cnc d 3.86 55 Cnc 12.3 0.905 55 Cnc e 0.02547 55 Cnc 12.3 0.905 55 Cnc f 0.1479 55
    [Show full text]
  • Messenger-No117.Pdf
    ESO WELCOMES FINLANDINLAND AS ELEVENTH MEMBER STAATE CATHERINE CESARSKY, ESO DIRECTOR GENERAL n early July, Finland joined ESO as Education and Science, and exchanged which started in June 2002, and were con- the eleventh member state, following preliminary information. I was then invit- ducted satisfactorily through 2003, mak- II the completion of the formal acces- ed to Helsinki and, with Massimo ing possible a visit to Garching on 9 sion procedure. Before this event, howev- Tarenghi, we presented ESO and its scien- February 2004 by the Finnish Minister of er, Finland and ESO had been in contact tific and technological programmes and Education and Science, Ms. Tuula for a long time. Under an agreement with had a meeting with Finnish authorities, Haatainen, to sign the membership agree- Sweden, Finnish astronomers had for setting up the process towards formal ment together with myself. quite a while enjoyed access to the SEST membership. In March 2000, an interna- Before that, in early November 2003, at La Silla. Finland had also been a very tional evaluation panel, established by the ESO participated in the Helsinki Space active participant in ESO’s educational Academy of Finland, recommended Exhibition at the Kaapelitehdas Cultural activities since they began in 1993. It Finland to join ESO “anticipating further Centre with approx. 24,000 visitors. became clear, that science and technology, increase in the world-standing of ESO warmly welcomes the new mem- as well as education, were priority areas Astronomy in Finland”. In February 2002, ber country and its scientific community for the Finnish government. we were invited to hold an information that is renowned for its expertise in many Meanwhile, the optical astronomers in seminar on ESO in Helsinki as a prelude frontline areas.
    [Show full text]
  • Constelações – Volume 8
    Coleção Os Mensageiros das Estrelas: Constelações – volume 8 Constelações de Maio Organizador Paulo Henrique Colonese Autores Leonardo Pereira de Castro Rafaela Ribeiro da Silva Ilustrador Caio Lopes do Nascimento Baldi Fiocruz-COC 2021 Coleção Os Mensageiros das Estrelas: Constelações – volume 8 Constelações de Maio Organizador Paulo Henrique Colonese Autores Leonardo Pereira de Castro Rafaela Ribeiro da Silva Ilustrador Caio Lopes do Nascimento Baldi Fiocruz-COC 2021 ii Licença de Uso O conteúdo dessa obra, exceto quando indicado outra licença, está disponível sob a Licença Creative Commons, Atribuição-Não Comercial-Compartilha Igual 4.0. FUNDAÇÃO OSWALDO CRUZ Presidente Nísia Trindade Lima Diretor da Casa de Oswaldo Cruz Paulo Roberto Elian dos Santos Chefe do Museu da Vida Alessandro Machado Franco Batista TECNOLOGIAS SERVIÇO DE ITINERÂNCIA Stellarium, OBS Studio, VideoScribe, Canva CIÊNCIA MÓVEL Paulo Henrique Colonese (Coordenação) Ana Carolina de Souza Gonzalez Fernanda Marcelly de Gondra França REVISÃO CADERNO DE CONTEÚDOS Flávia Souza Lima Paulo Henrique Colonese Lais Lacerda Viana Marta Fabíola do Valle G. Mayrink APOIO ADMINISTRATIVO (Coordenação) Fábio Pimentel Paulo Henrique Colonese Rodolfo de Oliveira Zimmer MÍDIAS E DIVULGAÇÃO Julianne Gouveia CONCEPÇÃO E DESENVOLVIMENTO Melissa Raquel Faria Silva Jackson Almeida de Farias Renata Bohrer Leonardo Pereira de Castro Renata Maria B. Fontanetto (Coordenação) Luiz Gustavo Barcellos Inácio (in memoriam) Paulo Henrique Colonese (Coordenação) CAPTAÇÃO DE RECURSOS Rafaela Ribeiro da Silva Escritório de Captação da Fiocruz Willian Alves Pereira Willian Vieira de Abreu GESTÃO CULTURAL Sociedade de Promoção da Casa de Oswaldo DESIGN GRÁFICO E ILUSTRAÇÃO Cruz Caio Lopes do Nascimento Baldi Biblioteca de Educação e Divulgação Científica Iloni Seibel C756 Constelações de maio [recurso eletrônico] / Organizador: Paulo Henrique Colonese.
    [Show full text]
  • Mètodes De Detecció I Anàlisi D'exoplanetes
    MÈTODES DE DETECCIÓ I ANÀLISI D’EXOPLANETES Rubén Soussé Villa 2n de Batxillerat Tutora: Dolors Romero IES XXV Olimpíada 13/1/2011 Mètodes de detecció i anàlisi d’exoplanetes . Índex - Introducció ............................................................................................. 5 [ Marc Teòric ] 1. L’Univers ............................................................................................... 6 1.1 Les estrelles .................................................................................. 6 1.1.1 Vida de les estrelles .............................................................. 7 1.1.2 Classes espectrals .................................................................9 1.1.3 Magnitud ........................................................................... 9 1.2 Sistemes planetaris: El Sistema Solar .............................................. 10 1.2.1 Formació ......................................................................... 11 1.2.2 Planetes .......................................................................... 13 2. Planetes extrasolars ............................................................................ 19 2.1 Denominació .............................................................................. 19 2.2 Història dels exoplanetes .............................................................. 20 2.3 Mètodes per detectar-los i saber-ne les característiques ..................... 26 2.3.1 Oscil·lació Doppler ........................................................... 27 2.3.2 Trànsits
    [Show full text]
  • Patrick Moore's Practical Astronomy Series
    Patrick Moore’s Practical Astronomy Series Other Titles in this Series Navigating the Night Sky Astronomy of the Milky Way How to Identify the Stars and The Observer’s Guide to the Constellations Southern/Northern Sky Parts 1 and 2 Guilherme de Almeida hardcover set Observing and Measuring Visual Mike Inglis Double Stars Astronomy of the Milky Way Bob Argyle (Ed.) Part 1: Observer’s Guide to the Observing Meteors, Comets, Supernovae Northern Sky and other transient Phenomena Mike Inglis Neil Bone Astronomy of the Milky Way Human Vision and The Night Sky Part 2: Observer’s Guide to the How to Improve Your Observing Skills Southern Sky Michael P. Borgia Mike Inglis How to Photograph the Moon and Planets Observing Comets with Your Digital Camera Nick James and Gerald North Tony Buick Telescopes and Techniques Practical Astrophotography An Introduction to Practical Astronomy Jeffrey R. Charles Chris Kitchin Pattern Asterisms Seeing Stars A New Way to Chart the Stars The Night Sky Through Small Telescopes John Chiravalle Chris Kitchin and Robert W. Forrest Deep Sky Observing Photo-guide to the Constellations The Astronomical Tourist A Self-Teaching Guide to Finding Your Steve R. Coe Way Around the Heavens Chris Kitchin Visual Astronomy in the Suburbs A Guide to Spectacular Viewing Solar Observing Techniques Antony Cooke Chris Kitchin Visual Astronomy Under Dark Skies How to Observe the Sun Safely A New Approach to Observing Deep Space Lee Macdonald Antony Cooke The Sun in Eclipse Real Astronomy with Small Telescopes Sir Patrick Moore and Michael Maunder Step-by-Step Activities for Discovery Transit Michael K.
    [Show full text]
  • Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗
    Tracing the Outer Structure of the Sagittarius Dwarf Galaxy: Detections at Angular Distances Between 10 and 34 Degrees ∗ Mario Mateo1 e-mail: [email protected] Edward W. Olszewski2 e-mail: [email protected] Heather L. Morrison3 e-mail: [email protected] Received ; accepted ∗BasedonobservationsobtainedwiththeBlancoTelescopeatCTIO,whichisoperated by the National Optical Astronomy Observatory, under contract to AURA. 1Department of Astronomy, University of Michigan, 821 Dennison Bldg., Ann Arbor, MI 48109–1090 2Steward Observatory, 933 N. Cherry, University of Arizona, Tucson, AZ 85721-0065 3Cottrell Scholar of Research Corporation, and NSF Career Fellow; Department of Astronomy and Department of Physics, Case Western Reserve University, Cleveland OH 44106 –2– ABSTRACT We have obtained deep photometric data in 24 fields along the southeast extension of the major axis of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy, and in four fields along the northwest extension. Using star counts at the expected position of the Sgr upper main-sequence within the resulting color-magnitude diagrams (CMDs), we unambiguously detect Sgr stars in the southeast over the range 10–34◦ from the galaxy’s center. If Sgr is symmetric, this implies a true major-axis diameter of at least 68◦, or nearly 30 kpc if all portions of Sgr are equally distant from the Sun. Star counts parallel to the galaxy’s minor-axis reveal that Sgr remains quite broad far from its center. This suggests that the outer portions of Sgr resemble a stream rather than an extension of the ellipsoidal inner regions of the galaxy. The inferred V-band surface brightness (SB) profile ranges from 27.3-30.5 mag arcsec−2 over this radial range and exhibits a change in slope ∼ 20◦ from the center of Sgr.
    [Show full text]
  • Exoplanet.Eu Catalog Page 1 Star Distance Star Name Star Mass
    exoplanet.eu_catalog star_distance star_name star_mass Planet name mass 1.3 Proxima Centauri 0.120 Proxima Cen b 0.004 1.3 alpha Cen B 0.934 alf Cen B b 0.004 2.3 WISE 0855-0714 WISE 0855-0714 6.000 2.6 Lalande 21185 0.460 Lalande 21185 b 0.012 3.2 eps Eridani 0.830 eps Eridani b 3.090 3.4 Ross 128 0.168 Ross 128 b 0.004 3.6 GJ 15 A 0.375 GJ 15 A b 0.017 3.6 YZ Cet 0.130 YZ Cet d 0.004 3.6 YZ Cet 0.130 YZ Cet c 0.003 3.6 YZ Cet 0.130 YZ Cet b 0.002 3.6 eps Ind A 0.762 eps Ind A b 2.710 3.7 tau Cet 0.783 tau Cet e 0.012 3.7 tau Cet 0.783 tau Cet f 0.012 3.7 tau Cet 0.783 tau Cet h 0.006 3.7 tau Cet 0.783 tau Cet g 0.006 3.8 GJ 273 0.290 GJ 273 b 0.009 3.8 GJ 273 0.290 GJ 273 c 0.004 3.9 Kapteyn's 0.281 Kapteyn's c 0.022 3.9 Kapteyn's 0.281 Kapteyn's b 0.015 4.3 Wolf 1061 0.250 Wolf 1061 d 0.024 4.3 Wolf 1061 0.250 Wolf 1061 c 0.011 4.3 Wolf 1061 0.250 Wolf 1061 b 0.006 4.5 GJ 687 0.413 GJ 687 b 0.058 4.5 GJ 674 0.350 GJ 674 b 0.040 4.7 GJ 876 0.334 GJ 876 b 1.938 4.7 GJ 876 0.334 GJ 876 c 0.856 4.7 GJ 876 0.334 GJ 876 e 0.045 4.7 GJ 876 0.334 GJ 876 d 0.022 4.9 GJ 832 0.450 GJ 832 b 0.689 4.9 GJ 832 0.450 GJ 832 c 0.016 5.9 GJ 570 ABC 0.802 GJ 570 D 42.500 6.0 SIMP0136+0933 SIMP0136+0933 12.700 6.1 HD 20794 0.813 HD 20794 e 0.015 6.1 HD 20794 0.813 HD 20794 d 0.011 6.1 HD 20794 0.813 HD 20794 b 0.009 6.2 GJ 581 0.310 GJ 581 b 0.050 6.2 GJ 581 0.310 GJ 581 c 0.017 6.2 GJ 581 0.310 GJ 581 e 0.006 6.5 GJ 625 0.300 GJ 625 b 0.010 6.6 HD 219134 HD 219134 h 0.280 6.6 HD 219134 HD 219134 e 0.200 6.6 HD 219134 HD 219134 d 0.067 6.6 HD 219134 HD
    [Show full text]
  • OGLE 2004-BLG-254: a K3 III Galactic Bulge Giant Spatially Resolved by A
    Astronomy & Astrophysics manuscript no. 4414arti c ESO 2018 January 9, 2018 OGLE 2004–BLG–254: a K3 III Galactic Bulge Giant spatially resolved by a single microlens⋆ A. Cassan1,2,3, J.-P. Beaulieu1,3, P. Fouqu´e1,4, S. Brillant1,5, M. Dominik1,6, J. Greenhill1,7, D. Heyrovsk´y8, K. Horne1,6, U.G. Jørgensen1,9, D. Kubas1,5, H.C. Stempels6, C. Vinter1,9, M.D. Albrow1,12, D. Bennett1,13, J.A.R. Caldwell1,14,15, J.J. Calitz1,16, K. Cook1,17, C. Coutures1,18, D. Dominis1,19, J. Donatowicz1,20, K. Hill1,7, M. Hoffman1,16, S. Kane1,21, J.-B. Marquette1,3, R. Martin1,22, P. Meintjes1,16, J. Menzies1,23, V.R. Miller12, K.R. Pollard1,12, K.C. Sahu1,14, J. Wambsganss1,2, A. Williams1,22, A. Udalski10,11, M.K. Szyma´nski10,11, M. Kubiak10,11, G. Pietrzy´nski10,11,24, I. Soszy´nski10,11,24, K. Zebru´n˙ 10,11, O. Szewczyk10,11, and Ł. Wyrzykowski10,11,25 (Affiliations can be found after the references) Received ¡date¿ / Accepted ¡date¿ ABSTRACT Aims. We present an analysis of OGLE 2004–BLG–254, a high-magnification (A 60) and relatively short duration (tE 13.2 days) microlensing event in which the source star, a Bulge K-giant, has been spatially resolved◦ ≃ by a point-like lens. We seek to determine≃ the lens and source distance, and provide a measurement of the linear limb-darkening coefficients of the source star in the I and R bands. We discuss the derived values of the latter and compare them to the classical theoretical laws, and furthermore examine the cases of already published microlensed GK-giants limb-darkening measurements.
    [Show full text]
  • Cycle 12 Abstract Catalog
    Cycle 12 Abstract Catalog Generated April 04, 2003 ================================================================================ Proposal Category: GO Scientific Category: ISM AND CIRCUMSTELLAR MATTER ID: 9718 Title: SMC Extinction Curve Towards a Quiescent Molecular Cloud PI: Francois Boulanger PI Institution: Institut d'Astrophysique Spatiale The lack of 2175 A bump in the SMC extinction curve is interpreted as an absence of small carbon grains. ISO Mid-IR observations support this interpretation by showing that PAH features are absent in the spectra of SMC and LMC massive star forming regions. However, the only ISO observation of an SMC quiescent molecular cloud shows all PAH features, indicating a PAH abundance relative to large dust grains similar to that of Milky Way clouds. We identified a reddened B2III star associated with this cloud. We propose to observe it with STIS. This observation will provide the first measure of the extinction properties of SMC dust away from star forming regions. It will allow us to disentangle the effects of metallicity and massive stars on the SMC extinction curve and dust composition and to assess the relevance of the SMC bump-free extinction curve to low metallicity and/or starburst galaxies in general. ================================================================================ Proposal Category: GO Scientific Category: STELLAR POPULATIONS ID: 9719 Title: Search For Metallicity Spreads in M31 Globular Clusters PI: Terry Bridges PI Institution: Anglo-Australian Observatory Our recent deep HST photometry of the M31 halo globular cluster (GC) Mayall~II, also called G1, has revealed a red-giant branch with a clear spread that we attribute to an intrinsic metallicity dispersion of at least 0.4 dex in [Fe/H].
    [Show full text]
  • Extrasolar Planets Topics to Be Covered
    3/25/2013 Extrasolar planets Astronomy 9601 1 Topics to be covered • 12.1 Physics and sizes • 12.2 Detecting extrasolar planets • 12.3 Observations of exoplanets • 12.4 Exoplanet statistics • 12.5 Planets and Life 2 What is a planet? What is a star? • The composition of Jupiter closely resembles that of the Sun: who’s to say that Jupiter is not simply a “failed star” rather than a planet? • The discovery of low-mass binary stars would be interesting, but (perhaps) not as exciting as discovering new “true” planets. • Is there a natural boundary between planets and stars? 3 1 3/25/2013 Planets and brown dwarfs • A star of mass less than 8% Luminosity “bump” due to short- of the Sun (80x Jupiter’s lived deuterium burning mass) will never grow hot Steady luminosity due to H burning enough in its core to fuse hydrogen • This is used as the boundary between true stars and very large gas planets • Object s b el ow thi s mass are called brown dwarfs • The boundary between BD and planet is more controversial – some argue it should be based on formation – other choose 0.013 solar masses=13 Mj as the boundary, as objects below this mass will never reach even deuterium fusion 4 Nelson et al., 1986, AJ, 311, 226 5 Pulsar planets • In 1992, Wolszczan and Frail announced the discovery of a multi‐ Artist’s conception of the planet planet planetary system around the orbiting pulsar PSR B1257+12 millisecond pulsar PSR 1257+12 (an earlier announcement had been retracted).
    [Show full text]
  • Assaj V4 N2 1937-Feb
    Vol. IV. No.2. acbt Janrnai of tlJt J\,strnnlltttl!al ~l1!ietu of ~l1ntb lfriea Edited by: J. JACKSON, M.A., D.Sc., F.R.A.S. otnntents : THE NEARER STARS 49 By J. Jackson, M.A., D.Sc., F.~.A.S. LIST OF NEAREST STARS 61. REPLY TO PROF. MILNE'S REVIEW OF MY PRESIDENTIAL ADDRESS 65 By J. K. E. Halm, Ph.D., F.R.A.S. ADDENDUM TO THE REMARKS IN MY ADDRESS ON THE QUESTION OF THE ORIGIN OF ICE AGES AND MOUNTAIN BUILDING .... 68 By J. K. E. Halm, Ph.D., F.R.A.S. REVIEWS 72 OBITUARIES 74 REPORT OF COUNCIL FOR 1935-36 77 SECTIONAL REpORTS:- Comet Section 79 Variable Star Section 81 Zodiacal Light Section 82 New Telescope and a New Observing Section 86 REPORT OF CAPE CENTRE 87 REPORT OF NATAL CENTRE 90 LIST OF OFFICE BEARERS 92 Published by the Society, P.O. Box 2061, Cape Town. Price to Members and Associates-One Shilling. Price to Non-Members-Two Shillings. FEBRUARY, 1937. ~be Journal of tbt ~5tronomical ~ocidlJ of ~ontb }.frica. VOL. IV. MARCH, 1937. No.2. THE NEARER STARS. By J. JACKSON, M.A., D.Sc. (PRESIDENTIAL ADDRESS 1935-1936.) The structure of the universe is a subject to which astronomers rightly devote a large portion of their time. There are many methods of approach to the subject, direct and indirect. Before the first determination of a stellar distance, not quite a century ago, the scale had to be a purely arbitrary one. Halley's detection of the proper motion of a few stars in the early years of the eighteenth century was the first demonstration that the stars are not at an infinite distance, but it was not till more than half a century later that the general structure of the galactic system was first revealed by Herschel's star gauges, or counts of the number of stars visible in his telescope when pointed in different directions.
    [Show full text]