Deep-Sky Companions: Southern Gems Stephen James O’Meara Index More Information
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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. -
IRS Form 990PF for Vertex Foundation
2949115321712 8 7. Return of Private Foundation m- or Section 4947(a)(1) Trust Treated as Private Foundation De anmem ofme Treasury > Do not enter socIal securIty numbers on this form as It may be made publIc. Mirna, Revenue Senna; D Go to www.irs.gov/Form990PF for instructions and the latest information. I pen 0 u .5 n5 EC .0" For calendaryear 2017 or taxyear beginning OCT 11 , 2017 ,and ending DEC 31 , 2017 Name of loundaIIon A Employer identification number THE VERTEX FOUNDATION, INC. 82-3101518 Number and street (or P 0 box number It mall Is not delIvered to street address) Room/sune B Telephone number 50 NORTHERN AVENUE 617-961-5104 City or town, state or provmce, country, and ZIP 0f forelgn postal code c If exemptIon applIcatIon Is pendrng. check here > D U BOSTON, MA 02210 6 Check all that apply. lnItIal return I3 lnItIal return of a former pubIIc charIty D 1. ForeIgn organIzatIons, check here DE E] FInaI return E Amended return I3 Address change III Name change 2' SELEEggggggigiTngRngML >E] H Check type of organIzatIonz SectIon 501(c)(3) exempt prIvate foundatIon q E If prIvate toundatIon status was termInated [Z] SectIon 4947(a)(1) nonexempt charItable trust C] Other taxable prIvate foundatIon C under sectIon 507(b)(1)(A), check here D I I FaIr market value of all assets at end of year J AccountIng methodi El Cash Accrual F If the foundatIon IS In a 60-month termInatIon i (from Part II, col. (c), We 16) El Other (speCIfy) under sectIon 507(b)(1)(B), check here D b $ 6 2 4 , 6 0 2 . -
The X-Ray Emission of Local Luminous Infrared Galaxies⋆
A&A 535, A93 (2011) Astronomy DOI: 10.1051/0004-6361/201117420 & c ESO 2011 Astrophysics The X-ray emission of local luminous infrared galaxies M. Pereira-Santaella1, A. Alonso-Herrero1, M. Santos-Lleo2, L. Colina1, E. Jiménez-Bailón3, A. L. Longinotti4, G. H. Rieke5,M.Ward6, and P. Esquej1 1 Departamento de Astrofísica, Centro de Astrobiología, CSIC/INTA, Carretera de Torrejón a Ajalvir, km 4, 28850 Torrejón de Ardoz, Madrid, Spain e-mail: [email protected] 2 XMM-Newton Science Operation Centre, European Space Agency, 28691 Villanueva de la Cañada, Madrid, Spain 3 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, 04510 Mexico DF, México 4 MIT Kavli Institute for Astrophysics and Space Research, 77 Massachusetts Avenue, NE80-6011, Cambridge, MA 02139, USA 5 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA 6 Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK Received 6 June 2011 / Accepted 5 September 2011 ABSTRACT We study the X-ray emission of a representative sample of 27 local luminous infrared galaxies (LIRGs). The median IR luminosity of our sample is log LIR/L = 11.2, therefore the low-luminosity end of the LIRG class is well represented. We used new XMM-Newton data as well as Chandra and XMM-Newton archive data. The soft X-ray (0.5–2 keV) emission of most of the galaxies (>80%), including LIRGs hosting a Seyfert 2 nucleus, is dominated by star-formation-related processes. These LIRGs follow the star-formation rate (SFR) versus soft X-ray luminosity correlation observed in local starbursts. -
Infrared Spectroscopy of Nearby Radio Active Elliptical Galaxies
The Astrophysical Journal Supplement Series, 203:14 (11pp), 2012 November doi:10.1088/0067-0049/203/1/14 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. INFRARED SPECTROSCOPY OF NEARBY RADIO ACTIVE ELLIPTICAL GALAXIES Jeremy Mould1,2,9, Tristan Reynolds3, Tony Readhead4, David Floyd5, Buell Jannuzi6, Garret Cotter7, Laura Ferrarese8, Keith Matthews4, David Atlee6, and Michael Brown5 1 Centre for Astrophysics and Supercomputing Swinburne University, Hawthorn, Vic 3122, Australia; [email protected] 2 ARC Centre of Excellence for All-sky Astrophysics (CAASTRO) 3 School of Physics, University of Melbourne, Melbourne, Vic 3100, Australia 4 Palomar Observatory, California Institute of Technology 249-17, Pasadena, CA 91125 5 School of Physics, Monash University, Clayton, Vic 3800, Australia 6 Steward Observatory, University of Arizona (formerly at NOAO), Tucson, AZ 85719 7 Department of Physics, University of Oxford, Denys, Oxford, Keble Road, OX13RH, UK 8 Herzberg Institute of Astrophysics Herzberg, Saanich Road, Victoria V8X4M6, Canada Received 2012 June 6; accepted 2012 September 26; published 2012 November 1 ABSTRACT In preparation for a study of their circumnuclear gas we have surveyed 60% of a complete sample of elliptical galaxies within 75 Mpc that are radio sources. Some 20% of our nuclear spectra have infrared emission lines, mostly Paschen lines, Brackett γ , and [Fe ii]. We consider the influence of radio power and black hole mass in relation to the spectra. Access to the spectra is provided here as a community resource. Key words: galaxies: elliptical and lenticular, cD – galaxies: nuclei – infrared: general – radio continuum: galaxies ∼ 1. INTRODUCTION 30% of the most massive galaxies are radio continuum sources (e.g., Fabbiano et al. -
Download And/Or Print One Copy of Any Article(S) in LJMU Research Online to Facilitate Their Private Study Or for Non-Commercial Research
LJMU Research Online Tartaglia, L, Sand, DJ, Valenti, S, Wyatt, S, Anderson, JP, Arcavi, I, Ashall, C, Botticella, MT, Cartier, R, Chen, TW, Cikota, A, Coulter, D, Valle, MD, Foley, RJ, Gal-Yam, A, Galbany, L, Gall, C, Haislip, JB, Harmanen, J, Hosseinzadeh, G, Howell, DA, Hsiao, EY, Inserra, C, Jha, SW, Kankare, E, Kilpatrick, CD, Kouprianov, VV, Kuncarayakti, H, Maccarone, TJ, Maguire, K, Mattila, S, Mazzali, PA, McCully, C, Melandri, A, Morrell, N, Phillips, MM, Pignata, G, Piro, AL, Prentice, SJ, Reichart, DE, Rojas-Bravo, C, Smartt, SJ, Smith, KW, Sollerman, J, Stritzinger, MD, Sullivan, M, Taddia, F and Young, DR The early detection and follow-up of the highly obscured Type II supernova 2016ija/DLT16am http://researchonline.ljmu.ac.uk/8049/ Article Citation (please note it is advisable to refer to the publisher’s version if you intend to cite from this work) Tartaglia, L, Sand, DJ, Valenti, S, Wyatt, S, Anderson, JP, Arcavi, I, Ashall, C, Botticella, MT, Cartier, R, Chen, TW, Cikota, A, Coulter, D, Valle, MD, Foley, RJ, Gal-Yam, A, Galbany, L, Gall, C, Haislip, JB, Harmanen, J, Hosseinzadeh, G, Howell, DA, Hsiao, EY, Inserra, C, Jha, SW, Kankare, E, LJMU has developed LJMU Research Online for users to access the research output of the University more effectively. Copyright © and Moral Rights for the papers on this site are retained by the individual authors and/or other copyright owners. Users may download and/or print one copy of any article(s) in LJMU Research Online to facilitate their private study or for non-commercial research. -
Astronomy & Astrophysics Background Galaxies As Reddening
A&A 371, 895–907 (2001) Astronomy DOI: 10.1051/0004-6361:20010467 & c ESO 2001 Astrophysics Background galaxies as reddening probes throughout the Magellanic Clouds C. M. Dutra1,3,E.Bica1,3,J.J.Clari´a2,3,A.E.Piatti2,3, and A. V. Ahumada2,3 1 Instituto de Fisica-UFRGS, CP 15051, CEP 91501-970 POA – RS, Brazil 2 Observatorio Astron´omico de C´ordoba, Laprida 854, 5000, C´ordoba, Argentina 3 Visiting Astronomer, Complejo Astron´omico El Leoncito operated under agreement between the Consejo Nacional de Investigaciones Cient´ıficas y T´ecnicas de la Rep´ublica Argentina and the National Universities of La Plata, C´ordoba and San Juan Received 3 January 2001 / Accepted 23 March 2001 Abstract. We study the spectral properties in the range 3600 A–6800˚ A˚ of the nuclear region of galaxies behind the Magellanic Clouds. The radial velocities clarified the nature of the objects as background galaxies or extended objects belonging to the Clouds. For most galaxies behind the main bodies of the LMC and SMC, radial velocities were measured for the first time. In the present sample typical LMC background galaxies are nearby (4000 <V(km s−1) < 6000), while SMC’s are considerably more distant (10 000 <V(km s−1) < 20 000). We determine the reddening in each line of sight by matching a reddening-free galaxy template with comparable stellar population. For the LMC main body we derive a combined Milky Way and internal reddening value E(B−V )MW+i =0.120.10, while for the SMC E(B−V )MW+i =0.050.05. -
THE 1000 BRIGHTEST HIPASS GALAXIES: H I PROPERTIES B
The Astronomical Journal, 128:16–46, 2004 July A # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE 1000 BRIGHTEST HIPASS GALAXIES: H i PROPERTIES B. S. Koribalski,1 L. Staveley-Smith,1 V. A. Kilborn,1, 2 S. D. Ryder,3 R. C. Kraan-Korteweg,4 E. V. Ryan-Weber,1, 5 R. D. Ekers,1 H. Jerjen,6 P. A. Henning,7 M. E. Putman,8 M. A. Zwaan,5, 9 W. J. G. de Blok,1,10 M. R. Calabretta,1 M. J. Disney,10 R. F. Minchin,10 R. Bhathal,11 P. J. Boyce,10 M. J. Drinkwater,12 K. C. Freeman,6 B. K. Gibson,2 A. J. Green,13 R. F. Haynes,1 S. Juraszek,13 M. J. Kesteven,1 P. M. Knezek,14 S. Mader,1 M. Marquarding,1 M. Meyer,5 J. R. Mould,15 T. Oosterloo,16 J. O’Brien,1,6 R. M. Price,7 E. M. Sadler,13 A. Schro¨der,17 I. M. Stewart,17 F. Stootman,11 M. Waugh,1, 5 B. E. Warren,1, 6 R. L. Webster,5 and A. E. Wright1 Received 2002 October 30; accepted 2004 April 7 ABSTRACT We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 H i brightest galaxies in the southern sky as obtained from the H i Parkes All-Sky Survey (HIPASS). The selection of the brightest sources is basedontheirHi peak flux density (Speak k116 mJy) as measured from the spatially integrated HIPASS spectrum. 7 ; 10 The derived H i masses range from 10 to 4 10 M . -
Arxiv:Astro-Ph/9808091V1 10 Aug 1998 Pc Eecp Cec Nttt,Wihi Prtdb the NAS5-26555
To appear in the Astronomical Journal (accepted 1998 August 10) WFPC2 OBSERVATIONS OF STAR CLUSTERS IN THE MAGELLANIC CLOUDS. II. THE OLDEST STAR CLUSTERS IN THE SMALL MAGELLANIC CLOUD1 Kenneth J. Mighell2 Kitt Peak National Observatory, National Optical Astronomy Observatories3, P. O. Box 26732, Tucson, AZ 85726-6732 Electronic mail: [email protected] Ata Sarajedini4 Department of Physics and Astronomy, San Francisco State University, 1600 Holloway Avenue, San Francisco, CA 94132 Electronic mail: [email protected] Rica S. French5 Middle Tennessee State University, Physics & Astronomy Department, WPS 219, P. O. Box 71, Murfreesboro, TN 37132 Electronic mail: [email protected] arXiv:astro-ph/9808091v1 10 Aug 1998 1 Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS5-26555. 2 Guest User, Canadian Astronomy Data Centre, which is operated by the Dominion Astrophysical Observatory for the National Research Council of Canada’s Herzberg Institute of Astrophysics. 3NOAO is operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement with the National Science Foundation. 4Hubble Fellow 5Based on research conducted at NOAO as part of the Research Experiences for Undergraduates program. – 2 – ABSTRACT We present our analysis of archival Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) observations in F450W ( B) and F555W ( V ) of the ∼ ∼ intermediate-age populous star clusters NGC 121, NGC 339, NGC 361, NGC 416, and Kron 3 in the Small Magellanic Cloud. -
The SBF Survey of Galaxy Distances. I. Sample Selection, Photometric
TheSBFSurveyofGalaxyDistances.I. Sample Selection, Photometric Calibration, and the Hubble Constant1 John L. Tonry2 and John P. Blakeslee2 Physics Dept. Room 6-204, MIT, Cambridge, MA 02139; Edward A. Ajhar2 Kitt Peak National Observatory, National Optical Astronomy Observatories, P.O. Box 26732 Tucson, AZ 85726; Alan Dressler Carnegie Observatories, 813 Santa Barbara St., Pasadena, CA 91101 ABSTRACT We describe a program of surface brightness fluctuation (SBF) measurements for determining galaxy distances. This paper presents the photometric calibration of our sample and of SBF in general. Basing our zero point on observations of Cepheid variable stars we find that the absolute SBF magnitude in the Kron-Cousins I band correlates well with the mean (V −I)0 color of a galaxy according to M I =(−1.74 ± 0.07) + (4.5 ± 0.25) [(V −I)0 − 1.15] for 1.0 < (V −I) < 1.3. This agrees well with theoretical estimates from stellar popula- tion models. Comparisons between SBF distances and a variety of other estimators, including Cepheid variable stars, the Planetary Nebula Luminosity Function (PNLF), Tully-Fisher (TF), Dn−σ, SNII, and SNIa, demonstrate that the calibration of SBF is universally valid and that SBF error estimates are accurate. The zero point given by Cepheids, PNLF, TF (both calibrated using Cepheids), and SNII is in units of Mpc; the zero point given by TF (referenced to a distant frame), Dn−σ, and SNIa is in terms of a Hubble expan- sion velocity expressed in km/s. Tying together these two zero points yields a Hubble constant of H0 =81±6 km/s/Mpc. -
Southern Arp - AM # Order
Southern Arp - AM # Order A B C D E F G H I J 1 AM # Constellation Object Name RA DEC Mag. Size Uranom. Uranom. Millenium 2 1st Ed. 2nd Ed. 3 AM 0003-414 Phoenix ESO 293-G034 00h06m19.9s -41d30m00s 13.7 3.2 x 1.0 386 177 430 Vol I 4 AM 0006-340 Sculptor NGC 10 00h08m34.5s -33d51m30s 13.3 2.4 x 1.2 350 159 410 Vol I 5 AM 0007-251 Sculptor NGC 24 00h09m56.5s -24d57m47s 12.4 5.8 x 1.3 305 141 366 Vol I 6 AM 0011-232 Cetus NGC 45 00h14m04.0s -23d10m55s 11.6 8.5 x 5.9 305 141 366 Vol I 7 AM 0027-333 Sculptor NGC 134 00h30m22.0s -33d14m39s 11.4 8.5 x 2.0 351 159 409 Vol I 8 AM 0029-643 Tucana ESO 079- G003 00h32m02.2s -64d15m12s 12.6 2.7 x 0.4 440 204 409 Vol I 9 AM 0031-280B Sculptor NGC 150 00h34m15.5s -27d48m13s 12 3.9 x 1.9 306 141 387 Vol I 10 AM 0031-320 Sculptor NGC 148 00h34m15.5s -31d47m10s 13.3 2 x 0.8 351 159 387 Vol I 11 AM 0033-253 Sculptor IC 1558 00h35m47.1s -25d22m28s 12.6 3.4 x 2.5 306 141 365 Vol I 12 AM 0041-502 Phoenix NGC 238 00h43m25.7s -50d10m58s 13.1 1.9 x 1.6 417 177 449 Vol I 13 AM 0045-314 Sculptor NGC 254 00h47m27.6s -31d25m18s 12.6 2.5 x 1.5 351 176 386 Vol I 14 AM 0050-312 Sculptor NGC 289 00h52m42.3s -31d12m21s 11.7 5.1 x 3.6 351 176 386 Vol I 15 AM 0052-375 Sculptor NGC 300 00h54m53.5s -37d41m04s 9 22 x 16 351 176 408 Vol I 16 AM 0106-803 Hydrus ESO 013- G012 01h07m02.2s -80d18m28s 13.6 2.8 x 0.9 460 214 509 Vol I 17 AM 0105-471 Phoenix IC 1625 01h07m42.6s -46d54m27s 12.9 1.7 x 1.2 387 191 448 Vol I 18 AM 0108-302 Sculptor NGC 418 01h10m35.6s -30d13m17s 13.1 2 x 1.7 352 176 385 Vol I 19 AM 0110-583 Hydrus NGC -
ATNF News Issue No
Galaxy Pair NGC 1512 / NGC 1510 ATNF News Issue No. 67, October 2009 ISSN 1323-6326 Questacon "astronaut" street performer and visitors at the Parkes Open Days 2009. Credit: Shaun Amy, CSIRO. Cover page image Cover Figure: Multi-wavelength color-composite image of the galaxy pair NGC 1512/1510 obtained using the Digitised Sky Survey R-band image (red), the Australia Telescope Compact Array HI distribution (green) and the Galaxy Evolution Explorer NUV -band image (blue). The Spitzer 24µm image was overlaid just in the center of the two galaxies. We note that in the outer disk the UV emission traces the regions of highest HI column density. See article (page 28) for more information. 2 ATNF News, Issue 67, October 2009 Contents From the Director ...................................................................................................................................................................................................4 CSIRO Medal Winners .........................................................................................................................................................................................5 CSIRO Astronomy and Space Science Unit Formed ........................................................................................................................6 ATNF Distinguished Visitors Program ........................................................................................................................................................6 ATNF Graduate Student Program ................................................................................................................................................................7 -
115 Abell Galaxy Cluster # 373
WINTER Medium-scope challenges 271 # # 115 Abell Galaxy Cluster # 373 Target Type RA Dec. Constellation Magnitude Size Chart AGCS 373 Galaxy cluster 03 38.5 –35 27.0 Fornax – 180 ′ 5.22 Chart 5.22 Abell Galaxy Cluster (South) 373 272 Cosmic Challenge WINTER Nestled in the southeast corner of the dim early winter western suburbs. Deep photographs reveal that NGC constellation Fornax, adjacent to the distinctive triangle 1316 contains many dust clouds and is surrounded by a formed by 6th-magnitude Chi-1 ( 1), Chi-2 ( 2), and complex envelope of faint material, several loops of Chi-3 ( 3) Fornacis, is an attractive cluster of galaxies which appear to engulf a smaller galaxy, NGC 1317, 6 ′ known as Abell Galaxy Cluster – Southern Supplement to the north. Astronomers consider this to be a case of (AGCS) 373. In addition to his research that led to the galactic cannibalism, with the larger NGC 1316 discovery of more than 80 new planetary nebulae in the devouring its smaller companion. The merger is further 1950s, George Abell also examined the overall structure signaled by strong radio emissions being telegraphed of the universe. He did so by studying and cataloging from the scene. 2,712 galaxy clusters that had been captured on the In my 8-inch reflector, NGC 1316 appears as a then-new National Geographic Society–Palomar bright, slightly oval disk with a distinctly brighter Observatory Sky Survey taken with the 48-inch Samuel nucleus. NGC 1317, about 12th magnitude and 2 ′ Oschin Schmidt camera at Palomar Observatory. In across, is visible in a 6-inch scope, although averted 1958, he published the results of his study as a paper vision may be needed to pick it out.