April 2016 BRAS Newsletter
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Mathématiques Et Espace
Atelier disciplinaire AD 5 Mathématiques et Espace Anne-Cécile DHERS, Education Nationale (mathématiques) Peggy THILLET, Education Nationale (mathématiques) Yann BARSAMIAN, Education Nationale (mathématiques) Olivier BONNETON, Sciences - U (mathématiques) Cahier d'activités Activité 1 : L'HORIZON TERRESTRE ET SPATIAL Activité 2 : DENOMBREMENT D'ETOILES DANS LE CIEL ET L'UNIVERS Activité 3 : D'HIPPARCOS A BENFORD Activité 4 : OBSERVATION STATISTIQUE DES CRATERES LUNAIRES Activité 5 : DIAMETRE DES CRATERES D'IMPACT Activité 6 : LOI DE TITIUS-BODE Activité 7 : MODELISER UNE CONSTELLATION EN 3D Crédits photo : NASA / CNES L'HORIZON TERRESTRE ET SPATIAL (3 ème / 2 nde ) __________________________________________________ OBJECTIF : Détermination de la ligne d'horizon à une altitude donnée. COMPETENCES : ● Utilisation du théorème de Pythagore ● Utilisation de Google Earth pour évaluer des distances à vol d'oiseau ● Recherche personnelle de données REALISATION : Il s'agit ici de mettre en application le théorème de Pythagore mais avec une vision terrestre dans un premier temps suite à un questionnement de l'élève puis dans un second temps de réutiliser la même démarche dans le cadre spatial de la visibilité d'un satellite. Fiche élève ____________________________________________________________________________ 1. Victor Hugo a écrit dans Les Châtiments : "Les horizons aux horizons succèdent […] : on avance toujours, on n’arrive jamais ". Face à la mer, vous voyez l'horizon à perte de vue. Mais "est-ce loin, l'horizon ?". D'après toi, jusqu'à quelle distance peux-tu voir si le temps est clair ? Réponse 1 : " Sans instrument, je peux voir jusqu'à .................. km " Réponse 2 : " Avec une paire de jumelles, je peux voir jusqu'à ............... km " 2. Nous allons maintenant calculer à l'aide du théorème de Pythagore la ligne d'horizon pour une hauteur H donnée. -
Gamma Leonis B
Gamma Leonis b The planetary system Gamma Leonis hosts at least one planet. Note that the system is a multiple star system. It hosts at least 2 stellar components. System parameters. Primary system name. Gamma Leonis. Alternative system names. N/A. Gamma-2 Leonis. Alternative star names. gamma 1 Leo, gam01 Leo, γ1 Leo, γ1 Leonis, γ Leo A, Gamma Leonis A, gamma Leo A, gam Leo A, Algieba A, Al Gieba A, HD 89484, HIP 50583 A, TYC 1423-1349-1, SAO 81298, BD+20 2467 A, WDS J10200+1950 A, STF 1424 A. Gamma Leonis's wiki: Gamma Leonis (γ Leo, γ Leonis) is a binary star system in the constellation Leo. It has the traditional name Algieba or Al Gieba . Name origin and history The name Algieba originates from the Arabic الجبهة Al-Jabhah Gamma Leonis b is an extrasolar planet located 125.5 light years away in the constellation Leo, orbiting the giant star Gamma Leonis. On November 6, 2009, a planetary companion around primary star Gamma1 Leonis has been announced. Moreover radial velocity variations would also hint two strong signals at 8.5 and 1340 days. The former periodicity is likely due to stellar pulsation, whereas the latter could be indicative of the presence of an additional planetary companion with 2.14 Jupiter masses Gamma Leonis (γ Leo / γ Leonis) is a binary star system in the constellation Leo. It also has the traditional name Algieba or Al Gieba. Name origin and history. The name "Algieba" originates from the Arabic "Al-Jabhah", meaning "the forehead". -
Homogeneous Spectroscopic Parameters for Bright Planet Host Stars from the Northern Hemisphere the Impact on Stellar and Planetary Mass (Research Note)
A&A 576, A94 (2015) Astronomy DOI: 10.1051/0004-6361/201425227 & c ESO 2015 Astrophysics Homogeneous spectroscopic parameters for bright planet host stars from the northern hemisphere The impact on stellar and planetary mass (Research Note) S. G. Sousa1,2,N.C.Santos1,2, A. Mortier1,3,M.Tsantaki1,2, V. Adibekyan1, E. Delgado Mena1,G.Israelian4,5, B. Rojas-Ayala1,andV.Neves6 1 Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal e-mail: [email protected] 2 Departamento de Física e Astronomia, Faculdade de Ciências, Universidade do Porto, Rua do Campo Alegre, 4169-007 Porto, Portugal 3 SUPA, School of Physics and Astronomy, University of St Andrews, St Andrews KY16 9SS, UK 4 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain 5 Departamento de Astrofísica, Universidade de La Laguna, 38205 La Laguna, Tenerife, Spain 6 Departamento de Física, Universidade Federal do Rio Grande do Norte, Brazil Received 27 October 2014 / Accepted 19 February 2015 ABSTRACT Aims. In this work we derive new precise and homogeneous parameters for 37 stars with planets. For this purpose, we analyze high resolution spectra obtained by the NARVAL spectrograph for a sample composed of bright planet host stars in the northern hemisphere. The new parameters are included in the SWEET-Cat online catalogue. Methods. To ensure that the catalogue is homogeneous, we use our standard spectroscopic analysis procedure, ARES+MOOG, to derive effective temperatures, surface gravities, and metallicities. These spectroscopic stellar parameters are then used as input to compute the stellar mass and radius, which are fundamental for the derivation of the planetary mass and radius. -
Exo-Mercat a Merged Exoplanet Catalog
Exo-MerCat a merged exoplanet catalog 1,2 Eleonora Alei , Riccardo Claudi1, Andrea Bignamini3, Marco Molinaro3 1 INAF – Osservatorio Astronomico di Padova 2 DFA-UNIPD – Dipartimento di Fisica e Astronomia dell’Università degli Studi di Padova 3 INAF – Osservatorio Astronomico di Trieste IVOA Interoperability meeting Paris, 12-17 May 2019 Overview • Online exoplanet catalogs: state of the art • Raw statistics with the current datasets • Known Issues: updates, errors, selection criteria • Exo-MerCat: aims, description, efficiency • Update workflow and VO resource NASA Exoplanet Archive (NASA) Exoplanets Orbit Database (ORG) Open Exoplanet Catalogue (OEC) Extrasolar Planets Encyclopaedia (EU) Yikes! Raw statistics Raw Problems Selection Criteria Aliases Coordinates Updates - Names appear in different - Human errors (plus-minus - False positives are present in formats; signs); the catalogs because of lags - Whitespaces are present; - Not updated coordinates; in the updates; - Different aliases for the same - Different epochs. - New candidates have yet to be planet; included in the database. Algieba, gamma Leonis: Proxima Centauri b (ra,dec): in NASA: gam 1 Leo in NASA: (217.428995,-62.679485) in ORG: gamma Leo A in ORG: (217.448946,-62.681353) in EU: gamma 1 Leo in EU: (217.429167,-62.679444) in OEC: Gamma Leonis in OEC: (219.990850,-60.835619) 5 Aims • Provide greater uniformity among the databases; • More effective associations among the datasets; • Identify and correct errors, to warn the catalog maintainers; Exo-MerCat • Provide a direct link with most stellar sources archives; • Provide the user with an intuitive Graphical Interface to download and filter data. 6 Icons made by https://www.flaticon.com/authors/gregor-cresnar from www.flaticon.com Description Initialization • Create a nested folder to contain all useful files; • Use various Virtual Observatory tools to download raw datasets: Exo-MerCat • wget command to access NASA/ORG database; • git commands and an *.xml reader to access the OEC database; • VO TAP service for the EU database. -
Maps for GLOBE at Night at Latitude 40 , February 23, 21 H Local Time
< 0.50 mag < 1.50 mag < 2.50 mag < 3.50 mag < 4.50 mag < 5.50 mag < 6.50 mag < 7.50 mag Maps for GLOBE at Night at latitude 40◦, February 23, 21 h local time (deep night), assuming rather transparent air. Orion’s belt is 34◦ to the right from the south, at 43◦ height. The brightest fixed star, Sirius, is at left. Jan Hollan, Ecological Institute Veronica and http://www.astro.cz/darksky < 0.50 mag < 1.50 mag < 2.50 mag < 3.50 mag < 4.50 mag < 5.50 mag < 6.50 mag < 7.50 mag Maps for GLOBE at Night at latitude 40◦, March 2, 21 h local time (deep night), assuming rather transparent air. Orion’s belt is 42◦ to the right from the south, at 40◦ height. The brightest fixed star, Sirius, is at left. Jan Hollan, Ecological Institute Veronica and http://www.astro.cz/darksky Betelgeuse Rigel Pollux Procyon Sirius Sirius Arcturus Saturn < 0.50 mag < 1.50 mag S S Betelgeuse Big Dipper Big Big Dipper Big Betelgeuse Rigel Rigel Pollux Pollux Procyon Procyon Sirius Sirius Arcturus Regulus Arcturus Regulus Denebola Denebola Saturn Saturn < 2.50 mag < 3.50 mag S S Procyon Procyon Regulus Regulus Denebola Denebola < 4.50 mag < 5.50 mag Procyon Procyon Regulus Regulus Denebola Denebola < 6.50 mag < 7.50 mag Maps for GLOBE at Night at latitude 40◦, March 23, 21 h local time (Sun at -31◦). Lines from N(E,S,W) to zenith shown (crosses each 10◦). Regulus (α Leonis) is 32◦ to the left from S, at 58◦ height. -
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. -
San Jose Astronomical Association Membership Form P.O
SJAA EPHEMERIS SJAA Activities Calendar March General Meeting Jim Van Nuland Dr. Adrian Brown March March 22, 2008 - 8 p.m. - Houge Park 1 Dark Sky weekend. Sunset 6:02 p.m., 28% moon David Smith rises 3:36 a.m. The Mars Reconnaissance Orbiter spacecraft has collected stunning 8 Dark Sky weekend. Sunset 6:09 p.m., 3% moon images on the Red planet since it arrived at Mars last year. Scientists sets 7:41 p.m. Messier Marathon at Henry Coe like Dr. Adrian Brown at the NASA Ames Research Center are poring Park. Henry Coe Park’s “Astronomy” lot has over the data to work out what Mars is telling them about its history been reserved. as a planet through the eyes of the CRISM (Compact InfraRed Imaging 9 DST starts at 2 a.m. Advance clocks 1 hour. Spectrometer for Mars) and the HiRISE (High Resolution Imaging 14 Astronomy Class at Houge Park. 7:30 p.m. Science Experiment) camera. Mark Wagner will discuss observing galaxies. 14 Houge Park star party. Sunset 7:15 p.m., 58% Dr. Brown will give an overview of MRO, and talk about Martian polar moon sets 3:41 a.m. Star party hours: 8:00 until research that is shedding light on the most active regions on Mars 11:00 p.m. today, where oceans of water are locked away in perpetuity at the polar 22 General Meeting at Houge Park. 8 p.m. Our caps. Or are they? speaker is Dr. Adrian Brown of the SETI Insti- tute. His topic is “Latest Results from the Mars The Golden State Star Party 2008 Reconnaissance Orbiter.” Bill Porte 28 Houge Park star party. -
The Skyscraper 2009 04.Indd
A Better Galaxy Guide: Early Spring M67: One of the most ancient open clusters known and Craig Cortis is a great novelty in this regard. Located 1.7° due W of mag NGC 2419: 3.25° SE of mag 6.2 66 Aurigae. Hard to find 4.3 Alpha Cancri. and see; at E end of short row of two mag 7.5 stars. Highly NGC 2775: Located 3.7° ENE of mag 3.1 Zeta Hydrae. significant and worth the effort —may be approximately (Look for “Head of Hydra” first.) 300,000 light years distant and qualify as an extragalactic NGC 2903: Easily found at 1.5° due S of mag 4.3 Lambda cluster. Named the Intergalactic Wanderer. Leonis. NGC 2683: Marks NW “crook” of coathanger-type triangle M95: One of three bright galaxies forming a compact with easy double star mag 4.2 Iota Cancri (which is SSW by triangle, along with M96 and M105. All three can be seen 4.8°) and mag 3.1 Alpha Lyncis (at 6° to the ENE). together in a low power, wide field view. M105 is at the NE tip of triangle, midway between stars 52 and 53 Leonis, mag Object Type R.A. Dec. Mag. Size 5.5 and 5.3 respectively —M95 is at W tip. Lynx NGC 3521: Located 0.5° due E of mag 6.0 62 Leonis. M65: One of a pair of bright galaxies that can be seen in NGC 2419 GC 07h 38.1m +38° 53’ 10.3 4.2’ a wide field view along with M66, which lies just E. -
The Dynamical State of the Coma Cluster with XMM-Newton?
A&A 400, 811–821 (2003) Astronomy DOI: 10.1051/0004-6361:20021911 & c ESO 2003 Astrophysics The dynamical state of the Coma cluster with XMM-Newton? D. M. Neumann1,D.H.Lumb2,G.W.Pratt1, and U. G. Briel3 1 CEA/DSM/DAPNIA Saclay, Service d’Astrophysique, L’Orme des Merisiers, Bˆat. 709, 91191 Gif-sur-Yvette, France 2 Science Payloads Technology Division, Research and Science Support Dept., ESTEC, Postbus 299 Keplerlaan 1, 2200AG Noordwijk, The Netherlands 3 Max-Planck Institut f¨ur extraterrestrische Physik, Giessenbachstr., 85740 Garching, Germany Received 19 June 2002 / Accepted 13 December 2002 Abstract. We present in this paper a substructure and spectroimaging study of the Coma cluster of galaxies based on XMM- Newton data. XMM-Newton performed a mosaic of observations of Coma to ensure a large coverage of the cluster. We add the different pointings together and fit elliptical beta-models to the data. We subtract the cluster models from the data and look for residuals, which can be interpreted as substructure. We find several significant structures: the well-known subgroup connected to NGC 4839 in the South-West of the cluster, and another substructure located between NGC 4839 and the centre of the Coma cluster. Constructing a hardness ratio image, which can be used as a temperature map, we see that in front of this new structure the temperature is significantly increased (higher or equal 10 keV). We interpret this temperature enhancement as the result of heating as this structure falls onto the Coma cluster. We furthermore reconfirm the filament-like structure South-East of the cluster centre. -
The Transfiguration in the Theology of Gregory Palamas And
Duquesne University Duquesne Scholarship Collection Electronic Theses and Dissertations Spring 2015 Deus in se et Deus pro nobis: The rT ansfiguration in the Theology of Gregory Palamas and Its Importance for Catholic Theology Cory Hayes Follow this and additional works at: https://dsc.duq.edu/etd Recommended Citation Hayes, C. (2015). Deus in se et Deus pro nobis: The rT ansfiguration in the Theology of Gregory Palamas and Its Importance for Catholic Theology (Doctoral dissertation, Duquesne University). Retrieved from https://dsc.duq.edu/etd/640 This Immediate Access is brought to you for free and open access by Duquesne Scholarship Collection. It has been accepted for inclusion in Electronic Theses and Dissertations by an authorized administrator of Duquesne Scholarship Collection. For more information, please contact [email protected]. DEUS IN SE ET DEUS PRO NOBIS: THE TRANSFIGURATION IN THE THEOLOGY OF GREGORY PALAMAS AND ITS IMPORTANCE FOR CATHOLIC THEOLOGY A Dissertation Submitted to the McAnulty Graduate School of Liberal Arts Duquesne University In partial fulfillment of the requirements for the degree of Doctor of Philosophy By Cory J. Hayes May 2015 Copyright by Cory J. Hayes 2015 DEUS IN SE ET DEUS PRO NOBIS: THE TRANSFIGURATION IN THE THEOLOGY OF GREGORY PALAMAS AND ITS IMPORTANCE FOR CATHOLIC THEOLOGY By Cory J. Hayes Approved March 31, 2015 _______________________________ ______________________________ Dr. Bogdan Bucur Dr. Radu Bordeianu Associate Professor of Theology Associate Professor of Theology (Committee Chair) (Committee Member) _______________________________ Dr. Christiaan Kappes Professor of Liturgy and Patristics Saints Cyril and Methodius Byzantine Catholic Seminary (Committee Member) ________________________________ ______________________________ Dr. James Swindal Dr. -
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 -
A Handbook of Double Stars, with a Catalogue of Twelve Hundred
The original of this bool< is in the Cornell University Library. There are no known copyright restrictions in the United States on the use of the text. http://www.archive.org/details/cu31924064295326 3 1924 064 295 326 Production Note Cornell University Library pro- duced this volume to replace the irreparably deteriorated original. It was scanned using Xerox soft- ware and equipment at 600 dots per inch resolution and com- pressed prior to storage using CCITT Group 4 compression. The digital data were used to create Cornell's replacement volume on paper that meets the ANSI Stand- ard Z39. 48-1984. The production of this volume was supported in part by the Commission on Pres- ervation and Access and the Xerox Corporation. Digital file copy- right by Cornell University Library 1991. HANDBOOK DOUBLE STARS. <-v6f'. — A HANDBOOK OF DOUBLE STARS, WITH A CATALOGUE OF TWELVE HUNDRED DOUBLE STARS AND EXTENSIVE LISTS OF MEASURES. With additional Notes bringing the Measures up to 1879, FOR THE USE OF AMATEURS. EDWD. CROSSLEY, F.R.A.S.; JOSEPH GLEDHILL, F.R.A.S., AND^^iMES Mt^'^I^SON, M.A., F.R.A.S. "The subject has already proved so extensive, and still ptomises so rich a harvest to those who are inclined to be diligent in the pursuit, that I cannot help inviting every lover of astronomy to join with me in observations that must inevitably lead to new discoveries." Sir Wm. Herschel. *' Stellae fixac, quae in ccelo conspiciuntur, sunt aut soles simplices, qualis sol noster, aut systemata ex binis vel interdum pluribus solibus peculiari nexu physico inter se junccis composita.