DOCSLIB.ORG

The Galaxies of the Local Group Sidney Van Den Bergh Index More Information

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

Cambridge University Press 978-0-521-03743-3 - The Galaxies of the Local Group Sidney van den Bergh Index More information Object Index 30 Doradus, 49, 88, 99, 100, 101, 108, 110, 112–116, DDO 155, 263 121, 124, 131, 134, 135, 139 DDO 187, 263, 279 47 Tucanae, see NGC 104 DDO 210, 5, 7, 194–195, 280, 288 287.5 + 22.5 + 240, 139, 161 DDO 216, 5, 6, 7, 174, 192–194, 280 AE And, 37 DDO 221, 174, 188–191, 280 AF And, see M31V19 DEM 71, 132 Alpha UMi, see Polaris DEM L316, 133 AM 1013-394A, 270, 272 Draco dwarf, 5, 58, 137, 185, 231, 249–252, 256, 259, And I, 5, 234, 235, 236, 237, 242, 280 262, 280 And II, 5, 7, 234, 236, 237, 238, 240, 242, 280 And III, 5, 234, 236, 237, 238, 240, 242, 280 EGB 0419 + 72, 270 And IV, 234 EGB 0427 + 63, see UGC-A92 And V, 5, 7, 237–240, 242, 280 Eridanus, 58, 64, 229 And VI, 5, 7, 240, 241, 242, 280 ESO 121-SC03, 103, 104, 124, 125, 161, 162 And VII, 5, 7, 241, 242, 280 ESO 249-010, 264 Andromeda galaxy, see M31 ESO 439-26, 55 Antlia dwarf, 265–267, 270, 272 Eta Carinae, 37 Aquarius dwarf, see DDO 210 AqrDIG, see DDO 210 F8D1, 2 Arches cluster, see G0.121+0.017 Fornax clusters 1–6, 222, 223, 224 Arp 2, 58, 64, 161, 226, 227, 228, 230, 232 Fornax dwarf 5, 94, 167, 219–226, 231, 256, 259, 260, Arp 220, 113 262, 280 B 327, 24 G 1, 27, 32, 34, 35, 45 BD +40◦ 147, 164 G 105, 35 BD +40◦ 148, 12 G 185, 31 Berkeley 17, 54 G 219, 27, 32 Berkeley 21, 56 G 280, 32 G0.7-0.0, see Sgr B2 C1,20 G0.121 + 0.017, 48 C 107, see vdB0 G1.1-0.1, 49 Camelopardalis dwarf, 241, 242 G359.87 + 0.18, 67 Carina dwarf, 5, 245–247, 256, 259, 278, 280 Galaxy, 5, 6, 32, 33, 34, 36, 39, 42, 43, 45, 46–71, 76, Cassiopeia 1, 263, 272 79, 117, 136, 149, 167, 179, 220, 232, 242, 244, Cassiopeia A, 131, 160 260, 273, 276, 277, 280, 284, 285, 288, 289, 290 Cassiopeia dwarf, see And VII GR 8, see DDO 155 Centaurus A, see NGC 5128 Complex C, 273 HD 5980, 151, 152 Constellations I–IX, 108, 109, 124, 131 HD 17072, 97 Crab nebula, 132 HDE 269582, 124 CS 22893-052, 54 HDE 269599, 124 Cygnus Loop, 132 He 2-436, 231 Hodge 11, 104, 106 DDO 69, 5, 202–204, 280, 290 Hubble 282, see G280 DDO 70, see Sextans B HV 829, 143 DDO 75, see Sextans A HV 837, 150 325 © Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-03743-3 - The Galaxies of the Local Group Sidney van den Bergh Index More information 326 Object Index HV 883, 118 M 33, 5, 6, 7, 20, 23, 29, 38, 72–91, 106, 139, 140, HV 905, 96, 100 170, 172, 176, 178, 179, 190, 191, 198, 236, 274, HV 966, 123 275, 280, 284, 290 HV 1157, 150 M 33 C 39, 82 HV 2274, 99 M 33 S 135, 82 HV 5637, 123 M 33 X-7, 90 HV 5756, 119 M 33 X-8, 76 HV 12842, 123 M 54, 226, 227, 228, 230 M 81, 57, 83, 91, 273 IC 10, 2, 5, 6, 174, 177–181, 190, 280 M 82, 273 IC 10 No. 113, 181 M 83, 79 IC 342, 2, 263, 271, 277, 279 M 87, 163, 165 IC 443, 132 M 92, 32, 54, 223, 251, 257 IC 1613, 4, 5, 6, 7, 126, 180–187, 189, 190, 191, 194, Maffei 1, 263, 271, 279 280, 282 Maffei 2, 279 IC 1613 V39, 183, 187 Magellanic Bridge, 138, 162, 273, 291 IC 1613 Sandage 3, 8, 186 Magellanic Stream, 137, 138, 139, 140, 248, 273, 291 Mayall II, see G1 IC 4499, 58, 64 see IC 5152, 2, 264, 272, 279 Mayall IV, G 219 Milky Way, see Galaxy K 58, 34 Mu Leonis, 51, 53, 55, 71 K 280, 34 N Aquilae 1918, 39 K 648, 68 NGC 45, 264 KMK 80, 130 NGC 55, 263, 264, 272 NGC 59, 264 Large Magellanic Cloud, 5, 6, 21, 22, 39, 41, 79, 81, NGC 104, 26, 52, 82, 146, 231 82, 84, 91–141, 142, 150, 155, 160, 161, 162, 179, NGC 121, 115, 143, 144, 145, 149, 154, 155, 162 182, 183, 186, 190, 191, 215, 218, 277, 278, 280, NGC 147, 5, 6, 205, 210, 213–218, 234, 260, 280, 290 284, 290, 291 NGC 147:I, 216 LMC 4, 109, 136, 139 NGC 147:III, 216 LMC N 49, 131, 132, 137 NGC 152, 154 LMC N 63A, 131, 132 NGC 185, 5, 6, 167, 205, 209–218, 234, 236, 260, LMC N 113, 128 280, 283, 290 LMC N 132D, 131, 160 NGC 185:III, 212 LMC N 157B, 133 NGC 185:IV, 212 LMC novae 1926–1997, 101, 120, 122 NGC 185:V, 212 LMC SL 663, 103, 125 NGC 205, 5, 6, 29, 167, 205–209, 213, 236, 260, 280, see Leo A, DDO 69 283, 284, 290 Leo I, 5, 234, 243–245, 256, 259, 260, 262, 277, 280, NGC 205:III, 207, 208 288, 290 NGC 205:V, 207, 208 Leo II, 5, 234, 235, 253–256, 259, 262, 280 NGC 206, 20, 36 LGS 1, 198 NGC 221, see M32 LGS 2, 198, 263 NGC 224, see M31 LGS 3, 5, 7, 195, 196, 198–199, 203, 260, 280 NGC 247, 264 LMC, see Large Magellanic Cloud NGC 253, 264 NGC 300, 264 M 5, 26, 32 NGC 330, 148 M 15, 68, 82 NGC 339, 155 M 31, 5, 6, 7, 9–45, 49, 61, 69, 74, 76, 82, 88, 91, NGC 404, 279 92, 27, 140, 164, 165, 166, 167, 168, 170, 172, NGC 411, 154 176, 178, 179, 181, 190, 191, 192, 205, 210, NGC 416, 149 236, 242, 244, 260, 274, 275, 276, 277, 280, NGC 592, 89 284, 285, 288, 289 NGC 598, see M33 M 31-290, 42 NGC 604, 73, 86, 88, 89, 174 M 31-372, 42 NGC 891, 46 M 31 V 15, 37 NGC 1049, 222 M 31 V 19, 37 NGC 1399, 15 M 31 V 40, 20 NGC 1466, 97, 104, 106, 115, 119 M31VA1,37 NGC 1560, 263, 272 M 32, 5, 6, 17, 19, 76, 163–169, 205, 213, 280, NGC 1569, 178, 263, 272 283, 291 NGC 1754, 104, 106, 107 © Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-03743-3 - The Galaxies of the Local Group Sidney van den Bergh Index More information Object Index 327 NGC 1774, 129 Palomar 12, 58, 64, 161, 225, 226, 228, 232 NGC 1786, 104, 119 Pegasus dwarf, see DDO 216 NGC 1818, 102, 129 Pegasus II, see And VI NGC 1835, 35, 45, 104, 106, 107, 115 Phoenix dwarf, 5, 7, 195, 196, 200–203, 260, NGC 1841, 104, 105, 119 280 NGC 1846, 102 Pisces dwarf, see LGS 3 NGC 1866, 82, 102, 140 Pleiades, 97 NGC 1898, 104, 105, 106, 107 Polaris, 96 NGC 1916, 104, 106, 107 NGC 1951, 129 R 40, 151 NGC 1978, 106, 108 R 49, 124 NGC 2005, 104, 106, 107, 129 R 71, 124 NGC 2019, 104, 106, 107, 129 R 110, 124 NGC 2121, 103, 125 R 127, 124, 133 NGC 2155, 103, 125 R 136, 49, 113, 115, 140, 179 NGC 2157, 99, 102, 106 R 136a-608, 115 NGC 2210, 104, 119 R 143, 124, 133 NGC 2257, 97, 104, 119 Regulus, 243 NGC 2403, 83 Reticulum cluster, 104, 119 NGC 2419, 51, 62, 63, 64, 70, 106, 223, 228, 229, Ruprecht 106, 54, 58, 64, 161 251, 290 RW UMi 1956, 68 NGC 2420, 98, 145 NGC 2506, 98, 145 S 119, 133 NGC 3031, see M81 S Andromedae, 12, 38, 50, 69 NGC 3034, see M82 S Doradus, 37, 124 NGC 3077, 208, 273 SagDIG, 5, 194, 199, 280 NGC 3109, 265, 266, 269, 270, 272, 279 Sagittarius A, 14, 47, 49, 50, 67, 69 NGC 3603, 114 Sagittarius dwarf, 5, 31, 52, 58, 59, 161, 167, 174, NGC 4486B, 13, 163 225–233, 256, 262, 280, 283 NGC 5128, 32, 33, 41, 91 Sculptor 314, 248 NGC 5139, 35, 45, 227, 257 Sculptor DIG, 264 NGC 5236, see M83 Sculptor dwarf, 5, 58, 219, 220, 225, 231, 247–250, NGC 5237, 263 256, 259, 260, 262, 280 NGC 5253, 79 Sextans A, 268–272, 279 NGC 5291, 283 Sextans B, 267–268, 270, 272, 279 NGC 6171, 26 Sextans dwarf, 5, 255–256, 259, 262, 280, 282 NGC 6287, 52 Sgr A, see Sagittarius A NGC 6397, 97 Sgr B2, 48, 51 NGC 6522, 47 Sk -69◦ 202, 130 NGC 6528, 52 Small Magellanic Cloud, 5, 6, 56, 99, 117, 118, 127, NGC 6553, 52 135, 136, 137, 138, 140, 142–162, 178, 179, 185, NGC 6715, see M54 186, 187, 190, 191, 209, 215, 218, 273, 277, 280, NGC 6791, 54, 55, 71 284, 290, 291 NGC 6822, 4, 5, 6, 7, 127, 170–176, 179, 180, 181, SMC, see Small Magellanic Cloud 184, 188, 190, 191, 194, 265, 280 SMC 98-1, 149 NGC 6822 Ho 12, 175 SMC K3, 149, 155 NGC 6822 V, VI, VII, 170, 173, 175, 284 SMC L1, 149, 155 NGC 6946, 2 SMC L11, 155 NGC 6949, 279 SMC L113, 149, 155 NGC 7006, 223, 235 SMC N19, 159 NGC 7078, see M15 SMC N24, 159 NGC 7793, 264 SMC novae 1897–1994, 147, 150 SN 1885A, see S Andromedae OB 184, 36 SN 1987A, 96, 99, 100, 115, 129–131, 132 Omega Centauri, see NGC 5139 SNR 0045-73.4, 159 SNR 0045-73.5, 159 P Cygni, 37 SNR 0101-724, 159 Palomar 1, 58, 64 SNR 0101-7226, 159 Palomar 2, 225, 226, 232 SNR 0104-72.3, 159 Palomar 3, 267 SNR 0102.2-7219, 159, 160 Palomar 3, 58, 64, 229 SNR 0540-693, 132, 133 Palomar 4, 58, 64, 229 SNR 1E102-7219, 159 © Cambridge University Press www.cambridge.org Cambridge University Press 978-0-521-03743-3 - The Galaxies of the Local Group Sidney van den Bergh Index More information 328 Object Index SNR 2E0053.2-7242, 160 Ursa Minor dwarf, 5, 58, 137, 185, 231, 256, 257–259, SNR DEM S128, 160 262, 280 Terzan 7, 58, 64, 161, 226, 227, 228, 229, 230, 232 vdB 0, 20, 32 Terzan 8, 226, 227, 228, 229, 230 Virgo cluster, 39, 41, 42 Triangulum galaxy, see M33 Tucana dwarf, 5, 7, 252, 253, 260, 280 W 49, 46 W Mensae, see HV 966 UGC-A86, 263, 272 WLM, see DDO 221 UGC-A92, 270–271 Wolf–Lundmark–Melotte, see DDO 221 UKS 2323-326, 263, 264, 272 Wray 16-423, 231 © Cambridge University Press www.cambridge.org.
Recommended publications
  • The Parkes H I Survey of the Magellanic System

    The Parkes H I Survey of the Magellanic System

    A&A 432, 45–67 (2005) Astronomy DOI: 10.1051/0004-6361:20040321 & c ESO 2005 Astrophysics The Parkes H I Survey of the Magellanic System C. Brüns1,J.Kerp1, L. Staveley-Smith2, U. Mebold1,M.E.Putman3,R.F.Haynes2, P. M. W. Kalberla1,E.Muller4, and M. D. Filipovic2,5 1 Radioastronomisches Institut, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany e-mail: [email protected] 2 Australia Telescope National Facility, CSIRO, PO Box 76, Epping NSW 1710, Australia 3 Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA 4 Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00612, USA 5 University of Western Sydney, Locked Bag 1797, Penrith South, DC, NSW 1797, Australia Received 24 February 2004 / Accepted 27 October 2004 Abstract. We present the first fully and uniformly sampled, spatially complete H survey of the entire Magellanic System with high velocity resolution (∆v = 1.0kms−1), performed with the Parkes Telescope. Approximately 24 percent of the southern skywascoveredbythissurveyona≈5 grid with an angular resolution of HPBW = 14.1. A fully automated data-reduction scheme was developed for this survey to handle the large number of H spectra (1.5 × 106). The individual Hanning smoothed and polarization averaged spectra have an rms brightness temperature noise of σ = 0.12 K. The final data-cubes have an rms noise of σrms ≈ 0.05 K and an effective angular resolution of ≈16 . In this paper we describe the survey parameters, the data- reduction and the general distribution of the H gas. The Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) are associated with huge gaseous features – the = Magellanic Bridge, the Interface Region, the Magellanic Stream, and the Leading Arm – with a total H mass of M(H ) 8 2 4.87 × 10 M d/55 kpc ,ifallH gas is at the same distance of 55 kpc.
  • VMC – the VISTA Survey of the Magellanic System Metallicity Of

    VMC – the VISTA Survey of the Magellanic System Metallicity Of

    Dr Maria‐Rosa Cioni VMC – the VISTA survey of the Magellanic System (Gal-Exgal survey) Metallicity of stellar populaons Moon of stellar populaons ESO spectroscopic survey workshop ESO-Garching, Germany, 9-10 March 2009 The VISTA survey of the Magellanic System ESO Public Survey 2009-2014 The most sensive near‐IR survey across the LMC, SMC, The team Bridge and part of the Stream M. Cioni, K. Bekki, G. Clemenni, W. de Blok, J. Emerson, C. Evans, R. de Grijs, B. Gibson, L. Girardi, M. Groenewegen, 4m Telescope V. Ivanov, M. Marconi, C. Mastropietro, B. Moore, R. Napiwotzki, T. Naylor, J. Oliveira, V. Ripepi, J. van Loon, M. Wilkinson, P. Wood 1.5 deg2 FOV United Kingdom, Italy, Belgium, Chile, France, Switzerland, South Africa, Australia http://star.herts.ac.uk/~mcioni/vmc/ 0. Observe the Magellanic System 2 ≈180 deg 3 filters ‐ YJKs 15 epochs (12 in KS and 3 in YJ; once simultaneous colours) S/N=10 at: Y=21.9, J=21.4, Ks=20.3 (Ks≈19 single epoch) Seeing 0.8 arcsec – average Spaal resoluon 0.34 pix/arcsec (0.51 arcsec instrument PSF) Service mode observing 1840 hours / 240 nights http://star.herts.ac.uk/~mcioni/vmc/ I. Derive the spaally resolved SFH Synthec diagram of a typical LMC stellar field as expected from VMC data. This field covers 1 VISTA detector! Accuracy: metallicity S/N=10 0.1 dex and age 20% in 0.1 deg2 Kerber et al 2009 http://star.herts.ac.uk/~mcioni/vmc/ II. Trace the 3D structure as a funcon of me The LMC is a few kpc thick and the SMC up to 20 kpc RR Lyrae stars are excellent distance indicators in the near‐IR First applicaon to the LMC bar to derive the LMC distance (Szewczyk et al 2008) – 0.2 kpc accuracy The structure of the Magellanic System will be measured using Cepheid variables, the red clump luminosity, the p of the red giant brach, etc.
  • We Had a Great Time on the Trip. We Had Some Representatives from the Vandenberg and Santa Barbara Clubs Along with Us for the Trip

    We Had a Great Time on the Trip. We Had Some Representatives from the Vandenberg and Santa Barbara Clubs Along with Us for the Trip

    We had a great time on the trip. We had some representatives from the Vandenberg and Santa Barbara clubs along with us for the trip. The most notable thing on the trip up was a stop in La Canada Flintridge to refuel the bus and get a bite to eat. I pulled out my PST Coronado and did a little impromptu public Sun Gazing. The Sun was pretty active with a number of platform prominences as well as the ever-present flame types. A distinct sunspot group in a very disturbed area of the Sun with a bright spot had me wondering if there was a flare in progress (There wasn’t.) The patrons at the tables outside didn’t seem to object to seeing the Sun either. I had a little bit of a scare when we first got up to the gate as a couple of people who were going to meet us there were nowhere to be seen. Fortunately one of them was already on the grounds and the other showed up while we were in the Museum. Relief! As it turned out we all went on the tour of the grounds. Our tour guide Greg gave us a tour starting outside the 60” Dome. He talked about the various Solar Telescopes -the old Snow telescope which was always a non-performer because of the design of the building- too many air currents. He talked about the rivalry over the 60 and 150 ft tower solar instruments (looks like UCLA won this one over USC.) And we got a good look at the 150 ft tower.
  • Astronomy & Astrophysics Background Galaxies As Reddening

    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.
  • Arxiv:Astro-Ph/9808091V1 10 Aug 1998 Pc Eecp Cec Nttt,Wihi Prtdb the NAS5-26555

    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.
  • RATIOS and STAR FORMATION EFFICIENCIES in SUPERGIANT H Ii REGIONS

    RATIOS and STAR FORMATION EFFICIENCIES in SUPERGIANT H Ii REGIONS

    The Astrophysical Journal, 788:167 (7pp), 2014 June 20 doi:10.1088/0004-637X/788/2/167 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. ENHANCEMENT OF CO(3–2)/CO(1–0) RATIOS AND STAR FORMATION EFFICIENCIES IN SUPERGIANT H ii REGIONS Rie E. Miura1,2, Kotaro Kohno3,4, Tomoka Tosaki5, Daniel Espada1,6,7, Akihiko Hirota8, Shinya Komugi1, Sachiko K. Okumura9, Nario Kuno7,8, Kazuyuki Muraoka10, Sachiko Onodera10, Kouichiro Nakanishi1,6,7, Tsuyoshi Sawada1,6, Hiroyuki Kaneko11, Tetsuhiro Minamidani8, Kosuke Fujii1,2, and Ryohei Kawabe1,6 1 National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; [email protected] 2 Department of Astronomy, The University of Tokyo, Hongo, Bunkyo-ku, Tokyo 133-0033, Japan 3 Institute of Astronomy, School of Science, The University of Tokyo, Osawa, Mitaka, Tokyo 181-0015, Japan 4 Research Center for Early Universe, School of Science, The University of Tokyo, Hongo, Bunkyo, Tokyo 113-0033, Japan 5 Joetsu University of Education, Yamayashiki-machi, Joetsu, Niigata 943-8512, Japan 6 Joint ALMA Observatory, Alonso de Cordova 3107, Vitacura 763-0355, Santiago, Chile 7 Department of Astronomical Science, The Graduate University for Advanced Studies (Sokendai), 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan 8 Nobeyama Radio Observatory, Minamimaki, Minamisaku, Nagano 384-1805, Japan 9 Department of Mathematical and Physical Sciences, Faculty of Science, Japan Woman’s University, Mejirodai 2-8-1, Bunkyo, Tokyo 112-8681, Japan 10 Osaka Prefecture University,
  • Expected Differences Between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition

    Expected Differences Between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition

    New Views of the Magellanic Clouds fA U Symposium, Vol. 190, 1999 Y.-H. Chu, N.B. Suntzef], J.E. Hesser, and D.A. Bohlender, eds. Expected Differences between AGB Stars in the LMC and the SMC Due to Differences in Chemical Composition Ju. Frantsman Astronomical Institute, Latvian University, Raina Blvd. 19, Riga, LV-1586, LATVIA Abstract. Certain aspects of the AGB population, such as the relative number of M and N stars, the mass loss rates, and the initial masses of carbon- oxygen cores, depend on the initial heavy element abundance Z. I have calculated synthetic populations of AGB stars for different initial Z values taking into consideration the evolution of single and close binary stars. I present the results of population syntheses of AGB stars in clusters as a function of different initial chemical compositions. The relation for the tip luminosity of AGB stars versus cluster age as a function of Z is presented and is used to determine the ages for a number of clusters in the LMC and the SMC, including clusters with no previous age determinations. Population simulations show that for low heavy element abundance (Z = 0.001) few M stars are formed with respect to the number of carbon stars. However, the total number of all AGB stars in clusters is not affected by the initial chemical composition. As a result of the evolution of close binary components after the mass exchange, an increase in the range of limiting values of the thermal pulsing AGB star luminosities is expected. The difference between the maximum luminosity on the AGB of single star and the luminosity of a star after a mass exchange event in a close binary system may be as great as 1 magnitude for very young clusters.
  • Annual Report 2017

    Annual Report 2017

    Koninklijke Sterrenwacht van België Observatoire royal de Belgique Royal Observatory of Belgium Jaarverslag 2017 Rapport Annuel 2017 Annual Report 2017 Cover illustration: Above: One billion star map of our galaxy created with the optical telescope of the satellite Gaia (Credit: ESA/Gaia/DPAC). Below: Three armillary spheres designed by Jérôme de Lalande in 1775. Left: the spherical sphere; in the centre: the geocentric model of our solar system (with the Earth in the centre); right: the heliocentric model of our solar system (with the Sun in the centre). Royal Observatory of Belgium - Annual Report 2017 2 De activiteiten beschreven in dit verslag werden ondersteund door Les activités décrites dans ce rapport ont été soutenues par The activities described in this report were supported by De POD Wetenschapsbeleid De Nationale Loterij Le SPP Politique Scientifique La Loterie Nationale The Belgian Science Policy The National Lottery Het Europees Ruimtevaartagentschap De Europese Gemeenschap L’Agence Spatiale Européenne La Communauté Européenne The European Space Agency The European Community Het Fonds voor Wetenschappelijk Onderzoek – Le Fonds de la Recherche Scientifique Vlaanderen Royal Observatory of Belgium - Annual Report 2017 3 Table of contents Preface .................................................................................................................................................... 6 Reference Systems and Planetology ......................................................................................................
  • From Luminous Hot Stars to Starburst Galaxies

    From Luminous Hot Stars to Starburst Galaxies

    9780521791342pre CUP/CONT July 9, 2008 11:48 Page-i FROM LUMINOUS HOT STARS TO STARBURST GALAXIES Luminous hot stars represent the extreme upper mass end of normal stellar evolution. Before exploding as supernovae, they live out their lives of only a few million years with prodigious outputs of radiation and stellar winds which dramatically affect both their evolution and environments. A detailed introduction to the topic, this book connects the astrophysics of mas- sive stars with the extremes of galaxy evolution represented by starburst phenomena. A thorough discussion of the physical and wind parameters of massive stars is pre- sented, together with considerations of their birth, evolution, and death. Hll galaxies, their connection to starburst galaxies, and the contribution of starburst phenomena to galaxy evolution through superwinds, are explored. The book concludes with the wider cosmological implications, including Population III stars, Lyman break galaxies, and gamma-ray bursts, for each of which massive stars are believed to play a crucial role. This book is ideal for graduate students and researchers in astrophysics who are interested in massive stars and their role in the evolution of galaxies. Peter S. Conti is an Emeritus Professor at the Joint Institute for Laboratory Astro- physics (JILA) and theAstrophysics and Planetary Sciences Department at the University of Colorado. Paul A. Crowther is a Professor of Astrophysics in the Department of Physics and Astronomy at the University of Sheffield. Claus Leitherer is an Astronomer with the Space Telescope Science Institute, Baltimore. 9780521791342pre CUP/CONT July 9, 2008 11:48 Page-ii Cambridge Astrophysics Series Series editors: Andrew King, Douglas Lin, Stephen Maran, Jim Pringle and Martin Ward Titles available in the series 10.
  • Science in the Urantia Papers

    Science in the Urantia Papers

    Science ¾ Scientific Validation of the UB z By Denver Pearson z By Phil Calabrese ¾ Seraphic Velocities ¾ Astronomy The Scientific Integrity of the Urantia Book by Denver Pearson As scientifically minded readers first peruse the Urantia Book, it soon occurs to them that many of its statements on the natural sciences conflict with currently held data and theories. In the minds of many this gives rise to doubts about the truthfulness of those statements. Wisdom would lead us to realize that nothing short of perfection is perfect, and anything touched by human hands has fingerprints. This should be our guiding thoughts as we contemplate the accuracy of the scientific content of the Urantia Papers. Several years ago, at the first scientific symposium, it was implied by one of the speakers that the revelation contains errors. This implication is alarming. More recently, at the second symposium held in Oklahoma, an interesting publication named "The Science Content of The Urantia Book" was made available (this document is obtainable from the Brotherhood of Man Library). In this publication is an article entitled "Time Bombs" in which the author suggests that the revelators planted certain inaccurate scientific statements in the book in order to prevent it from becoming a fetish. He states "...the revelators incorporated safeguards in the papers that would form The Urantia Book to diminish the tendency to regard it as an object of worship. What safeguards did they use? Suppose they decided to make sure that mortals reading it understood that some cosmological statements in the book would be found to be inaccurate".
  • Remerciements – Unité 1

    Remerciements – Unité 1

    TVO ILC SNC1D Remerciements Remerciements – Unité 1 Graphs, diagrams, illustrations, images in this course, unless otherwise specified, are ILC created, Copyright © 2018 The Ontario Educational Communications Authority. All rights reserved. Intro Video, Copyright © 2018 The Ontario Educational Communications Authority. All rights reserved. All title artwork and graphics, unless otherwise specified, Copyright © 2018The Ontario Educational Communications Authority. All rights reserved. Logo: Science Presse , Agence Science-Presse, URL: https://www.sciencepresse.qc.ca/, Accessed 14/01/2019. Logo: Curium, Curium, URL: https://curiummag.com/wp-content/uploads/2017/10/logo_ curium-web.png, Accessed 14/01/2019. Logo: Science Étonnante, David Louapre, URL: https://sciencetonnante.wordpress.com/, Accessed 20/03/2018, © 2018 HowStuffWorks, a division of InfoSpace Holdings LLC, a System1 Company. Blog, blogging and blogglers theme, djvstock/iStock/Getty Images Logo: Wordpress, WordPress.com, Automattic Inc., URL: https://wordpress.com/, Accessed 20/03/2018, © The WordPress Foundation. Logo: Wix, Wix.com, Inc., URL: https://static.wixstatic.com/ media/9ab0d1_39d56f21398048df8af89aab0cec67b8~mv1.png, Accessed 14/01/2019. Logo: Blogger, Blogger, Inc., ZyMOS, URL: https://commons.wikimedia.org/wiki/File:Blogger. svg, Accessed 20/03/2018, © Google LLC. HOME A film by Yann Arthus-Bertrand, GoodPlanet Foundation, Europacorp and Elzévir Films, URL: https://www.youtube.com/watch?v=GItD10Joaa0, Published 04/02/2009, Accessed 20/04/2018, Courtesy of the GoodPlanet
  • And Ecclesiastical Cosmology

    And Ecclesiastical Cosmology

    GSJ: VOLUME 6, ISSUE 3, MARCH 2018 101 GSJ: Volume 6, Issue 3, March 2018, Online: ISSN 2320-9186 www.globalscientificjournal.com DEMOLITION HUBBLE'S LAW, BIG BANG THE BASIS OF "MODERN" AND ECCLESIASTICAL COSMOLOGY Author: Weitter Duckss (Slavko Sedic) Zadar Croatia Pусскй Croatian „If two objects are represented by ball bearings and space-time by the stretching of a rubber sheet, the Doppler effect is caused by the rolling of ball bearings over the rubber sheet in order to achieve a particular motion. A cosmological red shift occurs when ball bearings get stuck on the sheet, which is stretched.“ Wikipedia OK, let's check that on our local group of galaxies (the table from my article „Where did the blue spectral shift inside the universe come from?“) galaxies, local groups Redshift km/s Blueshift km/s Sextans B (4.44 ± 0.23 Mly) 300 ± 0 Sextans A 324 ± 2 NGC 3109 403 ± 1 Tucana Dwarf 130 ± ? Leo I 285 ± 2 NGC 6822 -57 ± 2 Andromeda Galaxy -301 ± 1 Leo II (about 690,000 ly) 79 ± 1 Phoenix Dwarf 60 ± 30 SagDIG -79 ± 1 Aquarius Dwarf -141 ± 2 Wolf–Lundmark–Melotte -122 ± 2 Pisces Dwarf -287 ± 0 Antlia Dwarf 362 ± 0 Leo A 0.000067 (z) Pegasus Dwarf Spheroidal -354 ± 3 IC 10 -348 ± 1 NGC 185 -202 ± 3 Canes Venatici I ~ 31 GSJ© 2018 www.globalscientificjournal.com GSJ: VOLUME 6, ISSUE 3, MARCH 2018 102 Andromeda III -351 ± 9 Andromeda II -188 ± 3 Triangulum Galaxy -179 ± 3 Messier 110 -241 ± 3 NGC 147 (2.53 ± 0.11 Mly) -193 ± 3 Small Magellanic Cloud 0.000527 Large Magellanic Cloud - - M32 -200 ± 6 NGC 205 -241 ± 3 IC 1613 -234 ± 1 Carina Dwarf 230 ± 60 Sextans Dwarf 224 ± 2 Ursa Minor Dwarf (200 ± 30 kly) -247 ± 1 Draco Dwarf -292 ± 21 Cassiopeia Dwarf -307 ± 2 Ursa Major II Dwarf - 116 Leo IV 130 Leo V ( 585 kly) 173 Leo T -60 Bootes II -120 Pegasus Dwarf -183 ± 0 Sculptor Dwarf 110 ± 1 Etc.