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Distances to Local Group Galaxies
View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by CERN Document Server Distances to Local Group Galaxies Alistair R. Walker Cerro Tololo Inter-American Observatory, NOAO, Casilla 603, la Serena, Chile Abstract. Distances to galaxies in the Local Group are reviewed. In particular, the distance to the Large Magellanic Cloud is found to be (m M)0 =18:52 0:10, cor- − ± responding to 50; 600 2; 400 pc. The importance of M31 as an analog of the galaxies observed at greater distances± is stressed, while the variety of star formation and chem- ical enrichment histories displayed by Local Group galaxies allows critical evaluation of the calibrations of the various distance indicators in a variety of environments. 1 Introduction The Local Group (hereafter LG) of galaxies has been comprehensively described in the monograph by Sidney van den Berg [1], with update in [2]. The zero- velocity surface has radius of a little more than 1 Mpc, therefore the small sub-group of galaxies consisting of NGC 3109, Antlia, Sextans A and Sextans B lie outside the the LG by this definition, as do galaxies in the direction of the nearby Sculptor and IC342/Maffei groups. Thus the LG consists of two large spirals (the Galaxy and M31) each with their entourage of 11 and 10 smaller galaxies respectively, the dwarf spiral M33, and 13 other galaxies classified as either irregular or spherical. We have here included NGC 147 and NGC 185 as members of the M31 sub-group [60], whether they are actually bound to M31 is not proven. -
Grant Proposals, 1991-1999
Grant Proposals, 1991-1999 Finding aid prepared by Smithsonian Institution Archives Smithsonian Institution Archives Washington, D.C. Contact us at [email protected] Table of Contents Collection Overview ........................................................................................................ 1 Administrative Information .............................................................................................. 1 Descriptive Entry.............................................................................................................. 1 Names and Subjects ...................................................................................................... 1 Container Listing ............................................................................................................. 2 Grant Proposals https://siarchives.si.edu/collections/siris_arc_251859 Collection Overview Repository: Smithsonian Institution Archives, Washington, D.C., [email protected] Title: Grant Proposals Identifier: Accession 99-171 Date: 1991-1999 Extent: 17 cu. ft. (17 record storage boxes) Creator:: Smithsonian Astrophysical Observatory. Contracts and Procurement Office Language: English Administrative Information Prefered Citation Smithsonian Institution Archives, Accession 99-171, Smithsonian Astrophysical Observatory, Contracts and Procurement Office, Grant Proposals Descriptive Entry This accession consists of records documenting Smithsonian Astrophysical Observatory projects and activities. Materials include proposals, correspondence, progress -
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. -
MC^ 2: Galaxy Imaging and Redshift Analysis of the Merging Cluster CIZA J2242. 8+ 5301
LLNL-DOC-661846-DRAFT A Preprint typeset using LTEX style emulateapj v. 8/13/10 MC2: GALAXY IMAGING AND REDSHIFT ANALYSIS OF THE MERGING CLUSTER CIZA J2242.8+5301 William A. Dawson1, M. James Jee2, Andra Stroe3, Y. Karen Ng2, Nathan Golovich2, David Wittman2, David Sobral3,4,5, M. Bruggen¨ 6, H. J. A. Rottgering¨ 3, R. J. van Weeren7 (Dated: Draft June 21, 2021) LLNL-DOC-661846-DRAFT ABSTRACT X-ray and radio observations of CIZA J2242.8+5301 suggest that it is a major cluster merger. Despite being well studied in the X-ray, and radio, little has been presented on the cluster structure and dynamics inferred from its galaxy population. We carried out a deep (i< 25) broad band imaging survey of the system with Subaru SuprimeCam (g & i bands) and the Canada France Hawaii Telescope (r band) as well as a comprehensive spectroscopic survey of the cluster area (505 redshifts) using Keck DEIMOS. We use this data to perform a comprehensive galaxy/redshift analysis of the system, which is the first step to a proper understanding the geometry and dynamics of the merger, as well as using the merger to constrain self-interacting dark matter. We find that the system is dominated by two ′+0.7 +0.13 subclusters of comparable richness with a projected separation of6.9 −0.5 (1.3−0.10 Mpc). We find that the north and south subclusters have similar redshifts of z 0.188 with a relative line-of-sight velocity difference of 69 190kms−1. We also find that north and south≈ subclusters have velocity dispersions of +100 −±1 +100 −1 +4.6 14 1160−90 kms and 1080−70 kms , respectively. -
Arxiv:1508.03622V2 [Astro-Ph.GA] 6 Nov 2015 – 2 –
Eight Ultra-faint Galaxy Candidates Discovered in Year Two of the Dark Energy Survey 1; 2;3; 4;5 6;7 6;7 8;4;5 A. Drlica-Wagner ∗, K. Bechtol y, E. S. Rykoff , E. Luque , A. Queiroz , Y.-Y. Mao , R. H. Wechsler8;4;5, J. D. Simon9, B. Santiago6;7, B. Yanny1, E. Balbinot10;7, S. Dodelson1;11, A. Fausti Neto7, D. J. James12, T. S. Li13, M. A. G. Maia7;14, J. L. Marshall13, A. Pieres6;7, K. Stringer13, A. R. Walker12, T. M. C. Abbott12, F. B. Abdalla15;16, S. Allam1, A. Benoit-L´evy15, G. M. Bernstein17, E. Bertin18;19, D. Brooks15, E. Buckley-Geer1, D. L. Burke4;5, A. Carnero Rosell7;14, M. Carrasco Kind20;21, J. Carretero22;23, M. Crocce22, L. N. da Costa7;14, S. Desai24;25, H. T. Diehl1, J. P. Dietrich24;25, P. Doel15, T. F. Eifler17;26, A. E. Evrard27;28, D. A. Finley1, B. Flaugher1, P. Fosalba22, J. Frieman1;11, E. Gaztanaga22, D. W. Gerdes28, D. Gruen29;30, R. A. Gruendl20;21, G. Gutierrez1, K. Honscheid31;32, K. Kuehn33, N. Kuropatkin1, O. Lahav15, P. Martini31;34, R. Miquel35;23, B. Nord1, R. Ogando7;14, A. A. Plazas26, K. Reil5, A. Roodman4;5, M. Sako17, E. Sanchez36, V. Scarpine1, M. Schubnell28, I. Sevilla-Noarbe36;20, R. C. Smith12, M. Soares-Santos1, F. Sobreira1;7, E. Suchyta31;32, M. E. C. Swanson21, G. Tarle28, D. Tucker1, V. Vikram37, W. Wester1, Y. Zhang28, J. Zuntz38 (The DES Collaboration) arXiv:1508.03622v2 [astro-ph.GA] 6 Nov 2015 { 2 { *[email protected] [email protected] 1Fermi National Accelerator Laboratory, P. -
Annual Report / Rapport Annuel / Jahresbericht 1996
Annual Report / Rapport annuel / Jahresbericht 1996 ✦ ✦ ✦ E U R O P E A N S O U T H E R N O B S E R V A T O R Y ES O✦ 99 COVER COUVERTURE UMSCHLAG Beta Pictoris, as observed in scattered light Beta Pictoris, observée en lumière diffusée Beta Pictoris, im Streulicht bei 1,25 µm (J- at 1.25 microns (J band) with the ESO à 1,25 microns (bande J) avec le système Band) beobachtet mit dem adaptiven opti- ADONIS adaptive optics system at the 3.6-m d’optique adaptative de l’ESO, ADONIS, au schen System ADONIS am ESO-3,6-m-Tele- telescope and the Observatoire de Grenoble télescope de 3,60 m et le coronographe de skop und dem Koronographen des Obser- coronograph. l’observatoire de Grenoble. vatoriums von Grenoble. The combination of high angular resolution La combinaison de haute résolution angu- Die Kombination von hoher Winkelauflö- (0.12 arcsec) and high dynamical range laire (0,12 arcsec) et de gamme dynamique sung (0,12 Bogensekunden) und hohem dy- (105) allows to image the disk to only 24 AU élevée (105) permet de reproduire le disque namischen Bereich (105) erlaubt es, die from the star. Inside 50 AU, the main plane jusqu’à seulement 24 UA de l’étoile. A Scheibe bis zu einem Abstand von nur 24 AE of the disk is inclined with respect to the l’intérieur de 50 UA, le plan principal du vom Stern abzubilden. Innerhalb von 50 AE outer part. Observers: J.-L. Beuzit, A.-M. -
And – Objektauswahl NGC Teil 1
And – Objektauswahl NGC Teil 1 NGC 5 NGC 49 NGC 79 NGC 97 NGC 184 NGC 233 NGC 389 NGC 531 Teil 1 NGC 11 NGC 51 NGC 80 NGC 108 NGC 205 NGC 243 NGC 393 NGC 536 NGC 13 NGC 67 NGC 81 NGC 109 NGC 206 NGC 252 NGC 404 NGC 542 Teil 2 NGC 19 NGC 68 NGC 83 NGC 112 NGC 214 NGC 258 NGC 425 NGC 551 NGC 20 NGC 69 NGC 85 NGC 140 NGC 218 NGC 260 NGC 431 NGC 561 NGC 27 NGC 70 NGC 86 NGC 149 NGC 221 NGC 262 NGC 477 NGC 562 NGC 29 NGC 71 NGC 90 NGC 160 NGC 224 NGC 272 NGC 512 NGC 573 NGC 39 NGC 72 NGC 93 NGC 169 NGC 226 NGC 280 NGC 523 NGC 590 NGC 43 NGC 74 NGC 94 NGC 181 NGC 228 NGC 304 NGC 528 NGC 591 NGC 48 NGC 76 NGC 96 NGC 183 NGC 229 NGC 317 NGC 529 NGC 605 Sternbild- Zur Objektauswahl: Nummer anklicken Übersicht Zur Übersichtskarte: Objekt in Aufsuchkarte anklicken Zum Detailfoto: Objekt in Übersichtskarte anklicken And – Objektauswahl NGC Teil 2 NGC 620 NGC 709 NGC 759 NGC 891 NGC 923 NGC 1000 NGC 7440 NGC 7836 Teil 1 NGC 662 NGC 710 NGC 797 NGC 898 NGC 933 NGC 7445 NGC 668 NGC 712 NGC 801 NGC 906 NGC 937 NGC 7446 Teil 2 NGC 679 NGC 714 NGC 812 NGC 909 NGC 946 NGC 7449 NGC 687 NGC 717 NGC 818 NGC 910 NGC 956 NGC 7618 NGC 700 NGC 721 NGC 828 NGC 911 NGC 980 NGC 7640 NGC 703 NGC 732 NGC 834 NGC 912 NGC 982 NGC 7662 NGC 704 NGC 746 NGC 841 NGC 913 NGC 995 NGC 7686 NGC 705 NGC 752 NGC 845 NGC 914 NGC 996 NGC 7707 NGC 708 NGC 753 NGC 846 NGC 920 NGC 999 NGC 7831 Sternbild- Zur Objektauswahl: Nummer anklicken Übersicht Zur Übersichtskarte: Objekt in Aufsuchkarte anklicken Zum Detailfoto: Objekt in Übersichtskarte anklicken Auswahl And SternbildübersichtAnd -
Neutral Hydrogen in Local Group Dwarf Galaxies
Neutral Hydrogen in Local Group Dwarf Galaxies Jana Grcevich Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in the Graduate School of Arts and Sciences COLUMBIA UNIVERSITY 2013 c 2013 Jana Grcevich All rights reserved ABSTRACT Neutral Hydrogen in Local Group Dwarfs Jana Grcevich The gas content of the faintest and lowest mass dwarf galaxies provide means to study the evolution of these unique objects. The evolutionary histories of low mass dwarf galaxies are interesting in their own right, but may also provide insight into fundamental cosmological problems. These include the nature of dark matter, the disagreement be- tween the number of observed Local Group dwarf galaxies and that predicted by ΛCDM, and the discrepancy between the observed census of baryonic matter in the Milky Way’s environment and theoretical predictions. This thesis explores these questions by studying the neutral hydrogen (HI) component of dwarf galaxies. First, limits on the HI mass of the ultra-faint dwarfs are presented, and the HI content of all Local Group dwarf galaxies is examined from an environmental standpoint. We find that those Local Group dwarfs within 270 kpc of a massive host galaxy are deficient in HI as compared to those at larger galactocentric distances. Ram- 4 3 pressure arguments are invoked, which suggest halo densities greater than 2-3 10− cm− × out to distances of at least 70 kpc, values which are consistent with theoretical models and suggest the halo may harbor a large fraction of the host galaxy’s baryons. We also find that accounting for the incompleteness of the dwarf galaxy count, known dwarf galaxies whose gas has been removed could have provided at most 2.1 108 M of HI gas to the Milky Way. -
Arxiv:1705.02358V2 [Hep-Ph] 24 Nov 2017
Dark Matter Self-interactions and Small Scale Structure Sean Tulin1, ∗ and Hai-Bo Yu2, y 1Department of Physics and Astronomy, York University, Toronto, Ontario M3J 1P3, Canada 2Department of Physics and Astronomy, University of California, Riverside, California 92521, USA (Dated: November 28, 2017) Abstract We review theories of dark matter (DM) beyond the collisionless paradigm, known as self-interacting dark matter (SIDM), and their observable implications for astrophysical structure in the Universe. Self- interactions are motivated, in part, due to the potential to explain long-standing (and more recent) small scale structure observations that are in tension with collisionless cold DM (CDM) predictions. Simple particle physics models for SIDM can provide a universal explanation for these observations across a wide range of mass scales spanning dwarf galaxies, low and high surface brightness spiral galaxies, and clusters of galaxies. At the same time, SIDM leaves intact the success of ΛCDM cosmology on large scales. This report covers the following topics: (1) small scale structure issues, including the core-cusp problem, the diversity problem for rotation curves, the missing satellites problem, and the too-big-to-fail problem, as well as recent progress in hydrodynamical simulations of galaxy formation; (2) N-body simulations for SIDM, including implications for density profiles, halo shapes, substructure, and the interplay between baryons and self- interactions; (3) semi-analytic Jeans-based methods that provide a complementary approach for connecting particle models with observations; (4) merging systems, such as cluster mergers (e.g., the Bullet Cluster) and minor infalls, along with recent simulation results for mergers; (5) particle physics models, including light mediator models and composite DM models; and (6) complementary probes for SIDM, including indirect and direct detection experiments, particle collider searches, and cosmological observations. -
Annual Report 2013 Cover Photo: the International LOFAR Telescope (ILT) & Big Data, Danielle Futselaar © ASTRON
Annual report 2013 Cover photo: The International LOFAR Telescope (ILT) & Big Data, Danielle Futselaar © ASTRON. Photo on this page: prototype for the Apertif phased array feed. The Westerbork Synthesis Radio Telescope (WSRT) will be upgraded with Phased Array Feeds (PAFs), which will allow scientists to perform much faster observations with the telescope with a wider field of view. More information is available on the ASTRON/ JIVE daily image: http://www.astron.nl/ dailyimage/main.php?date=20130624. 2 ASTRON Annual report 2013 Facts and figures of 2013 8 Awards or grants 163 employees 162 refereed articles Funding: € 17,420,955 Expenditure: € 17,091,022 Balance: € 329.33 25 press releases 3 ASTRON Annual report 2013 Contents Facts and figures 2013 3 Director’s report 5 ASTRON Board and Management Team 7 ASTRON in brief 8 Contribution to top sectors 11 Performance indicators 12 Astronomy Group 17 Radio Observatory 22 R&D Laboratory 30 Connected legal entities 36 NOVA Optical/ Infrared Instrumentation Group 38 Joint Institute for VLBI in Europe 41 Outreach and education 43 Appendices 58 Appendix 1: financial summary 59 Appendix 2: personnel highlights 60 Appendix 3: WSRT & LOFAR proposals in 2013 62 Appendix 4: board, committees & staff in 2013 65 Appendix 5: publications 67 4 ASTRON Annual report 2013 Report 2013 was a year in which earlier efforts began to bear fruit. In particular, the various hardware and firmware changes made to the LOFAR telescope system in 2012, resulted in science quality data being delivered to the various Key Science Projects, and in particular the EoR (Epoch of Reionisation) Team. -
Ω Cen 127 M96 = NGC 3377 116 582
INDEX OF OBJECTS Palomar 3 95 Palomar 4 95 Palomar 5 95 CLUSTERS OF GALAXIES Palomar 14 95 85 203 Abell Palomar 15 95 Abell 262 203 47 Tue 155 Abell 1060 203 Abell 1367 181 GALAXIES Abell 1795 189. 203 A0136-080 5, 315 Abell 2029 203 AM2020-5050 315 Abell 2199 203 Arp 220 432 Abell 2256 169-170 Abell 2319 203 Carina 145-147, 158-159, 247-249 Abell 2626 203 Cygnus A 208 AWM 4 167. 169 DDO 127 139, 141-142, 147-148, 152 AWM 7 169. 208 DDO 154 141 Cancer 59 Draco 5, 144-147, 149, 153-155, Canes-Venatici/Ursa Major complex 157-159, 247-249 115 ESO 415-G26 315 Centaurus 110, 168 ESO 474-G20 314 Coma 1, 15, 87, 97, 101, 112, 115, Fornax 5, 144-147, 158-159, 249, 165, 169, 181, 186-187, 283, 351 403, 408 Galaxy, The (Milky Way) 2, 16-20, DC1842-63 59-60 23-25, 33, 36, 39-41, 43-44, 46- Hercules 59 47, 49-50, 87-88, 95, 111, 119, Hickson 88 51-52 122, 127-130, 136, 197, 207, Local Group 43, 50, 100, 115, 250, 213, 237, 248-250, 289, 294-295, 253, 322, 331, 350, 362, 402, 297-298, 301, 322, 327, 331, 435, 439, 539, 541 356, 391, 397-398, 407, 411-413, MKW 4 169 433. 436, 473, 494, 496, 499, MKW 9 169 519, 525, 530-531, 535-536, 540, M96 Group 116 542, 551, 553, 555, 557 Pegasus I 59, 167 Hickson 88a 51-52 Perseus 15, 105, 186, 189, 197, IC 724 59 206-207, 313 IC 2233 416, 418 Sculptor Group 132 Magellanic Clouds 408 Virgo 97-104, 107-108, 110, 115, M31 49-50, 86-87, 127-128, 146, 162, 168, 175, 203, 216, 248, 249-250, 275, 297, 331, 334, 257, 322, 332, 350. -
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