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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 -
Salpeter Mass Functions of Young Populous Clusters in the LMC? T
with the help of P. Joulie and manufac- and F. Casoli Ed., IAU Symposium 146, Davies, R.D., Elliott, K.H., Meaburn, J. 1976, tured with the help of our observatory p. 182. M.N.R.A.S. 81, 89. mechanics workshops, more especially Balick, B., Boeshaar, G.O., Gull, T.R. 1980, Downes, D., Wilson, T.L., Bieging, J., Wink, J. J. Urios who also helped us at La Silla. Astrophys. J., 242, 584. 1980, Astron. Astrophys. Suppl., 40, 379. Boulesteix, J., Georgelin, Y.P., Marcelin, M., We also want to thank A. Viale for her Grabelsky, D.A., Cohen, R.S., Bronfman, L., Monnet, G., 1984, Instrumentation in As- Thaddeus, P. 1988, Astrophys. J., 331, constant help when reducing the data in tronomy, V.A. Boksenberg, D.L. Crawford 181. Marseille. Ed., Proc. SPlE 445, p. 37. Georgelin, Y.M., Georgelin, Y.P. 1976, As- Bronfman, L., Alvarez, H., Cohen, R.S., tron. Astrophys., 49, 57. References Thaddeus, P. 1989, Astrophys. J. Suppl. Henize, K.G. 1956, Astrophys. J. Suppl., 2, Amram, P., Boulesteix, J., Marcelin, M., Ser. 71, 481. 31 5. 1991, Dynamics of Galaxies and their Caswell, J.L., Haynes, R.F. 1987, Astron. As- Melnick, J. 1989, The Messenger, 57, 4. Molecular cloud distributions, F. Combes trophys., 171, 261. Salpeter Mass Functions of Young Populous Clusters in the LMC? T. RICHTLER, K.S. DE BOER, Sternwarte der Universitat Bonn, Germany R. SAGAR, Indian Institute of Astrophysics, Bangalore, India 1. The Magellanic Clouds as the Initial Mass Function (IMF) of newly vance for galaxy evolution, since it con- Laboratories for Deriving IMFs formed stars. -
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. -
Arxiv:Astro-Ph/0305472 V1 23 May 2003
Astronomy & Astrophysics manuscript no. (will be inserted by hand later) An Hα survey aiming at the detection of extraplanar diffuse ionized gas in halos of edge–on spiral galaxies ? II. The Hα survey atlas and catalog J. Rossa ??1,2 and R.–J. Dettmar1 1 Astronomisches Institut, Ruhr–Universit¨at Bochum, D–44780 Bochum, Germany e-mail: [email protected], [email protected] 2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, U.S.A. (present address) Received 14 February 2003 / Accepted 6 May 2003 Abstract. In this second paper on the investigation of extraplanar diffuse ionized gas in nearby edge–on spiral galaxies we present the actual results of the individual galaxies of our Hα imaging survey. A grand total of 74 galaxies have been studied, including the 9 galaxies of a recently studied sub–sample (Rossa & Dettmar 2000). 40.5% of all studied galaxies reveal extraplanar diffuse ionized gas, whereas in 59.5% of the survey galaxies no extraplanar diffuse ionized gas could be detected. The average distances of this extended emission above the galactic midplane range from 1–2 kpc, while individual filaments in a few galaxies reach distances of up to |z| ∼ 6 kpc. In several cases a pervasive layer of ionized gas was detected, similar to the Reynolds layer in our Milky Way, while other galaxies reveal only extended emission locally. The morphology of the diffuse ionized gas is discussed for each galaxy and is compared with observations of other important ISM constituents in the context of the disk–halo connection, in those cases where published results were available. -
7.5 X 11.5.Threelines.P65
Cambridge University Press 978-0-521-19267-5 - Observing and Cataloguing Nebulae and Star Clusters: From Herschel to Dreyer’s New General Catalogue Wolfgang Steinicke Index More information Name index The dates of birth and death, if available, for all 545 people (astronomers, telescope makers etc.) listed here are given. The data are mainly taken from the standard work Biographischer Index der Astronomie (Dick, Brüggenthies 2005). Some information has been added by the author (this especially concerns living twentieth-century astronomers). Members of the families of Dreyer, Lord Rosse and other astronomers (as mentioned in the text) are not listed. For obituaries see the references; compare also the compilations presented by Newcomb–Engelmann (Kempf 1911), Mädler (1873), Bode (1813) and Rudolf Wolf (1890). Markings: bold = portrait; underline = short biography. Abbe, Cleveland (1838–1916), 222–23, As-Sufi, Abd-al-Rahman (903–986), 164, 183, 229, 256, 271, 295, 338–42, 466 15–16, 167, 441–42, 446, 449–50, 455, 344, 346, 348, 360, 364, 367, 369, 393, Abell, George Ogden (1927–1983), 47, 475, 516 395, 395, 396–404, 406, 410, 415, 248 Austin, Edward P. (1843–1906), 6, 82, 423–24, 436, 441, 446, 448, 450, 455, Abbott, Francis Preserved (1799–1883), 335, 337, 446, 450 458–59, 461–63, 470, 477, 481, 483, 517–19 Auwers, Georg Friedrich Julius Arthur v. 505–11, 513–14, 517, 520, 526, 533, Abney, William (1843–1920), 360 (1838–1915), 7, 10, 12, 14–15, 26–27, 540–42, 548–61 Adams, John Couch (1819–1892), 122, 47, 50–51, 61, 65, 68–69, 88, 92–93, -
BR Photometry of the Globular Cluster System of NGC 3115
BR Photometry of the Globular Cluster System of NGC 3115 by S.J. Bickerton A thesis submitted in the Department of Physics in conformit?; with the requirements for the degree of Master of Science Queen's Kingston. Ontario. Canada January. 2002 @ copyright S.J. Bickerton. 2002 National Library Bibliothèque nationale 1 of Canada du Canada Acquisitions and Acquisitions et Bibliographie Services services bibliographiques 395 WeUulglon Street 395. rue Wellingtan Otiawa ON KiA ON4 OnawaON K1AûN4 canada Canada The author has granted a non- L'auteur a accordé une licence non exclusive licence diowing the exclusive pemettant à la National Librq of Canada to Bibliothèque nationale du Canada de reproduce, loan, distriiute or sel reproduire, prêter, distribuer ou copies of this thesis in microform, vendre des copies de cette thèse sous paper or electronic formats. la fonne de microfiche/film, de reproduction sur papier ou sur format électronique. The author retains ownership of the L'auteur conserve la propriété du copyright in this thesis. Neither the droit d'auteur qui protège cette thèse. thesis nor substantial extracts fiom it Ni la thèse ni des extraits substantiels may be printed or othenwise de celle-ci ne doivent être imprimés reproduced without the author's ou autrement reproduits sans son permission. autorisation. ii Abstract The lenticular galavy NGC 3113 sits in isolation in the constellation Sextans. Photometric observations of the gala~ymade with the CFHlZK detector at the Canada- France-Hawaii 3.6m telescope have provided the deepest wide field images of the galavy to date. revealing nearly its entire globular cluster system. -
2018 Publication Year 2020-10-29T13:00:40Z Acceptance
Publication Year 2018 Acceptance in OA@INAF 2020-10-29T13:00:40Z Title VEGAS-SSS. II. Comparing the globular cluster systems in NGC 3115 and NGC 1399 using VEGAS and FDS survey data. The quest for a common genetic heritage of globular cluster systems Authors CANTIELLO, Michele; D'Abrusco, Raffaele; SPAVONE, MARILENA; Paolillo, Maurizio; CAPACCIOLI, Massimo; et al. DOI 10.1051/0004-6361/201730649 Handle http://hdl.handle.net/20.500.12386/28082 Journal ASTRONOMY & ASTROPHYSICS Number 611 A&A 611, A93 (2018) / / Astronomy DOI: 10.1051 0004-6361 201730649 & c ESO 2018 Astrophysics VEGAS-SSS. II. Comparing the globular cluster systems in NGC 3115 and NGC 1399 using VEGAS and FDS survey data The quest for a common genetic heritage of globular cluster systems? Michele Cantiello1, Raffaele D’Abrusco2, Marilena Spavone3, Maurizio Paolillo4, Massimo Capaccioli4, Luca Limatola3, Aniello Grado3, Enrica Iodice3, Gabriella Raimondo1, Nicola Napolitano3, John P. Blakeslee5, Enzo Brocato6, Duncan A. Forbes7, Michael Hilker8, Steffen Mieske9, Reynier Peletier10, Glenn van de Ven11, and Pietro Schipani3 1 INAF Osservatorio Astr. di Teramo, via Maggini, 64100 Teramo, Italy e-mail: [email protected] 2 Smithsonian Astrophysical Observatory, 60 Garden Street, 02138 Cambridge, MA, USA 3 INAF Osservatorio Astr. di Capodimonte Napoli, Salita Moiariello, 80131 Napoli, Italy 4 Dip. di Fisica, Universitá di Napoli Federico II, C.U. di Monte Sant’Angelo, via Cintia, 80126 Naples, Italy 5 NRC Herzberg Astronomy & Astrophysics, Victoria, BC V9E 2E7, Canada 6 INAF Osservatorio Astronomico di Roma, via di Frascati, 33, 00040 Monteporzio Catone, Italy 7 Centre for Astrophysics & Supercomputing, Swinburne University, Hawthorn, VIC 3122, Australia 8 European Southern Observatory, Karl-Schwarzschild-Str. -
Arxiv:Astro-Ph/0609148V1 6 Sep 2006 L Ik+Hl Tcuemksi Airt Iden- to Easier It Makes Stucture Halo + Sim- Their Disk 1985)
Hi studies of the Sculptor group galaxies. VIII. The background galaxies: NGC 24 and NGC 45 Laurent Chemin1,2, Claude Carignan1, Nathalie Drouin1, and Kenneth C. Freeman3 [chemin,carignan]@astro.umontreal.ca, [email protected] ABSTRACT In order to complete our Hi survey of galaxies in the Sculptor group area, VLA observations of NGC 24 and NGC 45 are presented. These two galaxies of similar magnitude MB ∼ −17.4 lie in the background of the Sculptor group and are low surface brightness galaxies, especially NGC 45. The Hi distribution and kinematics are regular for NGC 24 while NGC 45 exhibits a kinematical twist of its major axis. A tilted-ring model shows that the position angle of the major axis changes by ∼ 25◦. A best-fit model of their mass distribution gives mass-to-light ratios for the stellar disk of 2.5 and 5.2 for NGC 24 and NGC 45 respectively. These values are higher than the ones expected from stellar population synthesis models. Despite the large dark matter contribution, the galaxy mass is still dominated by the stellar component in their very inner regions. These high mass-to-light ratios are typical of what is seen in low surface brightness galaxies and may indicate that, in those galaxies, disks are far from the maximum disk case. The halo parameters derived from the best-fit models are thus lower limits. Subject headings: galaxies: halos — galaxies: fundamental parameter (mass) — galaxies: individual (NGC 24, NGC 45) — galaxies: kinematics and dynamics galaxies: structure 1. Introduction tify the contribution of each component to the ro- tation curve. -
1983Apj. ..265 ...IA the Astrophysical Journal
IA .... The Astrophysical Journal, 265:1-17, 1983 February 1 ..265 © 1983. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1983ApJ. A DISTANCE SCALE FROM THE INFRARED MAGNITUDE/H I VELOCITY-WIDTH RELATION. IV. THE MORPHOLOGICAL TYPE DEPENDENCE AND SCATTER IN THE RELATION; THE DISTANCES TO NEARBY GROUPS Marc Aaronson Steward Observatory, University of Arizona AND Jeremy Mould Kitt Peak National Observatory1 Received 1982 February 5; accepted 1982 July 19 ABSTRACT A newly published catalog of infrared and 21 cm data for 300 galaxies in the Local Supercluster is analyzed in order to investigate empirically several properties of the Tully-Fisher relation. For this sample, we obtain the following results: 1. In the infrared, there is no significant dependence of the Tully-Fisher relation with type. A small type dependence is found in the blue; however, the spread in profile width at fixed magnitude is only about one-third as great as that found earlier by Roberts. 2. The slope of the Tully-Fisher relation is wavelength dependent, increasing in value from the blue to the infrared. The slope of the relation does appear steeper than previously indicated, though, and a small nonlinearity is identified. 3. The scatter in the Tully-Fisher relation is smaller in the infrared, where a ~ 0.45 mag, than in the optical. Distances to a number of nearby groups are calculated using the absolute calibration from Paper I. Good agreement in relative distance is found with both the Sandage-Tammann and de Vaucouleurs scales. Current disagreement over the absolute distance scale and value of the Hubble constant appears reduced to two issues: the infall velocity toward Virgo, and the distance scale for galaxies in the neighborhood of the Milky Way. -
View the Energy Map of Trinidad and Tobago, 2017 Edition
Trinidad and Tobago LNG export destinations 2015 (million m3 of LNG) Trinidad and Tobago deepwater area for development 60°W 59°W 58°W Trinidad and Tobago territorial waters ENERGY MAP OF TRINIDAD AND TOBAGO 1000 2000 m m 2017 edition GRENADA BARBADOS Trinidad and Tobago 2000m LNG to Europe A tlantic Ocean 2.91 million m3 LNG A TLANTIC Caribbean 2000m 20 Produced by Petroleum Economist, in association with 00 O CEAN EUROPE Sea m Trinidad and Tobago 2000m LNG to North America NORTH AMERICA Trinidad and Tobago 5.69 million m3 LNG LNG to Asia 3 GO TTDAA 30 TTDAA 31 TTDAA 32 BA 1.02 million m LNG TO Trinidad and Tobago OPEN OPEN OPEN 12°N LNG to MENA 3 1.90 million m LNG ASIA Trinidad and Tobago CARIBBEAN TRINIDAD AND TOBAGO 2000m LNG to Caribbean Atlantic LNG Company profile Company Profile Company profile Company Profile 3 Established by the Government of Trinidad and Tobago in August 1975, The National Gas Company of Trinidad and Tobago Limited (NGC) is an BHP Billiton is a leading global resources company with a Petroleum Business that includes exploration, development, production and marketing Shell has been in Trinidad and Tobago for over 100 years and has played a major role in the development of its oil and gas industry. Petroleum Company of Trinidad and Tobago Limited (Petrotrin) is an integrated Oil and Gas Company engaged in the full range of petroleum 3.84 million m LNG internationally investment-graded company that is strategically positioned in the midstream of the natural gas value chain. -
Ngc Catalogue Ngc Catalogue
NGC CATALOGUE NGC CATALOGUE 1 NGC CATALOGUE Object # Common Name Type Constellation Magnitude RA Dec NGC 1 - Galaxy Pegasus 12.9 00:07:16 27:42:32 NGC 2 - Galaxy Pegasus 14.2 00:07:17 27:40:43 NGC 3 - Galaxy Pisces 13.3 00:07:17 08:18:05 NGC 4 - Galaxy Pisces 15.8 00:07:24 08:22:26 NGC 5 - Galaxy Andromeda 13.3 00:07:49 35:21:46 NGC 6 NGC 20 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 7 - Galaxy Sculptor 13.9 00:08:21 -29:54:59 NGC 8 - Double Star Pegasus - 00:08:45 23:50:19 NGC 9 - Galaxy Pegasus 13.5 00:08:54 23:49:04 NGC 10 - Galaxy Sculptor 12.5 00:08:34 -33:51:28 NGC 11 - Galaxy Andromeda 13.7 00:08:42 37:26:53 NGC 12 - Galaxy Pisces 13.1 00:08:45 04:36:44 NGC 13 - Galaxy Andromeda 13.2 00:08:48 33:25:59 NGC 14 - Galaxy Pegasus 12.1 00:08:46 15:48:57 NGC 15 - Galaxy Pegasus 13.8 00:09:02 21:37:30 NGC 16 - Galaxy Pegasus 12.0 00:09:04 27:43:48 NGC 17 NGC 34 Galaxy Cetus 14.4 00:11:07 -12:06:28 NGC 18 - Double Star Pegasus - 00:09:23 27:43:56 NGC 19 - Galaxy Andromeda 13.3 00:10:41 32:58:58 NGC 20 See NGC 6 Galaxy Andromeda 13.1 00:09:33 33:18:32 NGC 21 NGC 29 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 22 - Galaxy Pegasus 13.6 00:09:48 27:49:58 NGC 23 - Galaxy Pegasus 12.0 00:09:53 25:55:26 NGC 24 - Galaxy Sculptor 11.6 00:09:56 -24:57:52 NGC 25 - Galaxy Phoenix 13.0 00:09:59 -57:01:13 NGC 26 - Galaxy Pegasus 12.9 00:10:26 25:49:56 NGC 27 - Galaxy Andromeda 13.5 00:10:33 28:59:49 NGC 28 - Galaxy Phoenix 13.8 00:10:25 -56:59:20 NGC 29 See NGC 21 Galaxy Andromeda 12.7 00:10:47 33:21:07 NGC 30 - Double Star Pegasus - 00:10:51 21:58:39 -
Arxiv:1408.6413V1 [Astro-Ph.GA] 27 Aug 2014 Ot Africa
The Abundance Properties of Nearby Late-Type Galaxies. II. The Relation between Abundance Distributions and Surface Brightness Profiles L. S. Pilyugin1 and E. K. Grebel and I. A. Zinchenko1 Astronomisches Rechen-Institut, Zentrum f¨ur Astronomie der Universit¨at Heidelberg, M¨onchhofstr. 12–14, 69120 Heidelberg, Germany [email protected], [email protected], [email protected] A. Y. Kniazev2,3 South African Astronomical Observatory, PO Box 9, 7935 Observatory, Cape Town, South Africa [email protected] Received ; accepted arXiv:1408.6413v1 [astro-ph.GA] 27 Aug 2014 1Visiting Astronomer, Main Astronomical Observatory of National Academy of Sciences of Ukraine, 27 Zabolotnogo str., 03680 Kiev, Ukraine. 2Southern African Large Telescope Foundation, PO Box 9, 7935 Observatory, Cape Town, South Africa. 3Sternberg Astronomical Institute, Lomonosov Moscow State University, Moscow 119992, Russia –2– ABSTRACT The relations between oxygen abundance and disk surface brightness (OH–SB relation) in the infrared W 1 band are examined for a nearby late-type galaxies. The oxygen abundances were presented in Paper I. The photometric character- istics of the disks are inferred here using photometric maps from the literature through bulge-disk decomposition. We find evidence that the OH – SB relation is not unique but depends on the galactocentric distance r (taken as a fraction of the optical radius R25) and on the properties of a galaxy: the disk scale length h and the morphological T -type. We suggest a general, four-dimensional OH – SB relation with the values r, h, and T as parameters. The parametric OH – SB relation reproduces the observed data better than a simple, one-parameter relation; the deviations resulting when using our parametric relation are smaller by a factor of ∼1.4 than that the simple relation.