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Cosmicflows-3: Cosmography of the Local Void
Draft version May 22, 2019 Preprint typeset using LATEX style AASTeX6 v. 1.0 COSMICFLOWS-3: COSMOGRAPHY OF THE LOCAL VOID R. Brent Tully, Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA Daniel Pomarede` Institut de Recherche sur les Lois Fondamentales de l'Univers, CEA, Universite' Paris-Saclay, 91191 Gif-sur-Yvette, France Romain Graziani University of Lyon, UCB Lyon 1, CNRS/IN2P3, IPN Lyon, France Hel´ ene` M. Courtois University of Lyon, UCB Lyon 1, CNRS/IN2P3, IPN Lyon, France Yehuda Hoffman Racah Institute of Physics, Hebrew University, Jerusalem, 91904 Israel Edward J. Shaya University of Maryland, Astronomy Department, College Park, MD 20743, USA ABSTRACT Cosmicflows-3 distances and inferred peculiar velocities of galaxies have permitted the reconstruction of the structure of over and under densities within the volume extending to 0:05c. This study focuses on the under dense regions, particularly the Local Void that lies largely in the zone of obscuration and consequently has received limited attention. Major over dense structures that bound the Local Void are the Perseus-Pisces and Norma-Pavo-Indus filaments sepa- rated by 8,500 km s−1. The void network of the universe is interconnected and void passages are found from the Local Void to the adjacent very large Hercules and Sculptor voids. Minor filaments course through voids. A particularly interesting example connects the Virgo and Perseus clusters, with several substantial galaxies found along the chain in the depths of the Local Void. The Local Void has a substantial dynamical effect, causing a deviant motion of the Local Group of 200 − 250 km s−1. -
John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C
VITA NAME: John J. Cowan Date of Birth: April 3, 1948 Place of Birth: Washington, D.C. EDUCATION: 1970 B.A. George Washington University, Washington, D.C. 1972 M.S. Case Institute of Technology, Cleveland, OH 1976 Ph.D. University of Maryland, College Park, MD PROFESSIONAL EXPERIENCE: 2002–present David Ross Boyd Professor, University of Oklahoma, 2002–2002 Research Fellow, University of Texas, Austin, TX 1998–2002 Samuel Roberts Noble Foundation Presidential Professor, University of Oklahoma, Norman, OK 1997–1998 Big XIIFaculty Fellow,University ofOklahoma 1991–1992 Visiting Professor, Department of Astronomy, Columbia University, New York, NY 1989–present Professor, Department of Physics and Astronomy, University of Oklahoma, Norman, OK 1988–1994 Consultant and Participating Guest, Lawrence Livermore National Laboratory, Livermore, CA 1987–1988 Visiting Research Associate, Harvard-Smithsonian Center for Astrophysics, Harvard University, Cambridge, MA 1984–1989 Associate Professor, University of Oklahoma 1979–1984 Assistant Professor, University of Oklahoma 1976–1979 Postdoctoral Research Fellow, Harvard-Smithsonian Center for Astrophysics, Harvard University PROFESSIONAL AND HONORARY SOCIETIES: American Astronomical Society International Astronomical Union Phi Beta Kappa RESEARCH INTERESTS: Stellar evolution, supernovae, nucleosynthesis and abundances Radio observations of supernovae and galaxies JOHN J. COWAN Page 2 PUBLICATIONS J. J. Cowan and W. K. Rose, “Production of 17O and 18O by Means of the Hot CNO Tri-Cycle,” Astrophys. J. (Letters) 201, L45 (1975) J. J. Cowan, M. Kafatos, and W. K. Rose, “Sources of Excitation of the Interstellar Gas and Galactic Structure,” Astrophys. J. 195, 47 (1975) M. F. A’Hearn and J. J. Cowan, “Molecular Production Rates in Comet Kohoutek,” As- tron. -
Radio Sources in Low-Luminosity Active Galactic Nuclei
A&A 392, 53–82 (2002) Astronomy DOI: 10.1051/0004-6361:20020874 & c ESO 2002 Astrophysics Radio sources in low-luminosity active galactic nuclei III. “AGNs” in a distance-limited sample of “LLAGNs” N. M. Nagar1, H. Falcke2,A.S.Wilson3, and J. S. Ulvestad4 1 Arcetri Observatory, Largo E. Fermi 5, Florence 50125, Italy 2 Max-Planck-Institut f¨ur Radioastronomie, Auf dem H¨ugel 69, 53121 Bonn, Germany e-mail: [email protected] 3 Department of Astronomy, University of Maryland, College Park, MD 20742, USA Adjunct Astronomer, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA e-mail: [email protected] 4 National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA e-mail: [email protected] Received 23 January 2002 / Accepted 6 June 2002 Abstract. This paper presents the results of a high resolution radio imaging survey of all known (96) low-luminosity active galactic nuclei (LLAGNs) at D ≤ 19 Mpc. We first report new 2 cm (150 mas resolution using the VLA) and 6 cm (2 mas resolution using the VLBA) radio observations of the previously unobserved nuclei in our samples and then present results on the complete survey. We find that almost half of all LINERs and low-luminosity Seyferts have flat-spectrum radio cores when observed at 150 mas resolution. Higher (2 mas) resolution observations of a flux-limited subsample have provided a 100% (16 of 16) detection rate of pc-scale radio cores, with implied brightness temperatures ∼>108 K. The five LLAGNs with the highest core radio fluxes also have pc-scale “jets”. -
9905625.PDF (3.665Mb)
INFORMATION TO USERS This manuscript has been reproduced from the microfilm master. UMI films the text directly from the original or copy submitted. Thus, some thesis and dissertation copies are in typewriter free, while others may be from any type o f computer printer. The quality of this reproduction is dependent upon the quality of the copy submitted. Broken or indistinct print, colored or poor quality illustrations and photographs, print bleedthrough, substandard margins, and improper alignment can adversely afreet reproduction. In the unlikely event that the author did not send UMI a complete manuscript and there are m is^ g pages, these will be noted. Also, if unauthorized copyright material had to be removed, a note will indicate the deletion. Oversize materials (e.g., m ^ s, drawings, charts) are reproduced by sectioning the orignal, begnning at the upper left-hand comer and continuing from left to right in equal sections with small overlaps. Each original is also photographed in one exposure and is included in reduced form at the back of the book. Photographs included in the original manuscript have been reproduced xerographically in this copy. KGgher quality 6” x 9” black and white photographic prints are available for any photographs or illustrations appearing in this copy for an additional charge. Contact UMI directly to order. UMI A Bell & Howell Infoimation Compaiy 300 North Zeeb Road, Ann Arbor MI 48106-1346 USA 313/761-4700 800/521-0600 UNIVERSITY OF OKLAHOMA GRADUATE COLLEGE “ ‘TIS SOMETHING, NOTHING”, A SEARCH FOR RADIO SUPERNOVAE A DISSERTATION SUBMITTED TO THE GRADUATE FACULTY in partial fulfillment of the requirements for the degree of DOCTOR OF PHILOSOPHY By CHRISTOPHER R. -
Rotation Curves of High-Resolution LSB and SPARC Galaxies with Fuzzy and Multistate (Ultralight Boson) Scalar field Dark Matter
MNRAS 475, 1447–1468 (2018) doi:10.1093/mnras/stx3208 Advance Access publication 2017 December 12 Rotation curves of high-resolution LSB and SPARC galaxies with fuzzy and multistate (ultralight boson) scalar field dark matter T. Bernal,1‹† L. M. Fernandez-Hern´ andez,´ 1 T. Matos2‡ andM.A.Rodr´ıguez-Meza1‡ 1Departamento de F´ısica, Instituto Nacional de Investigaciones Nucleares, AP 18-1027, Ciudad de Mexico´ 11801, Mexico 2Departamento de F´ısica, Centro de Investigacion´ y de Estudios Avanzados del IPN, AP 14-740, Ciudad de Mexico´ 07000, Mexico Accepted 2017 December 8. Received 2017 December 8; in original form 2017 January 4 ABSTRACT Cold dark matter (CDM) has shown to be an excellent candidate for the dark matter (DM) of the Universe at large scales; however, it presents some challenges at the galactic level. The scalar field dark matter (SFDM), also called fuzzy, wave, Bose–Einstein condensate, or ultralight axion DM, is identical to CDM at cosmological scales but different at the galactic ones. SFDM forms core haloes, it has a natural cut-off in its matter power spectrum, and it predicts well-formed galaxies at high redshifts. In this work we reproduce the rotation curves of high- resolution low surface brightness (LSB) and SPARC galaxies with two SFDM profiles: (1) the soliton+NFW profile in the fuzzy DM (FDM) model, arising empirically from cosmological simulations of real, non-interacting scalar field (SF) at zero temperature, and (2) the multistate SFDM (mSFDM) profile, an exact solution to the Einstein–Klein–Gordon equations for a real, self-interacting SF, with finite temperature into the SF potential, introducing several quantum states as a realistic model for an SFDM halo. -
Why Gravity Cannot Be Quantized Canonically, and What We Can We Do About It
WHY GRAVITY CANNOT BE QUANTIZED CANONICALLY, AND WHAT WE CAN WE DO ABOUT IT Philip D. Mannheim Department of Physics University of Connecticut Presentation at Miami 2013, Fort Lauderdale December 2013 1 GHOST PROBLEMS, UNITARITY OF FOURTH-ORDER THEORIES AND PT QUANTUM MECHANICS 1. P. D. Mannheim and A. Davidson, Fourth order theories without ghosts, January 2000 (arXiv:0001115 [hep-th]). 2. P. D. Mannheim and A. Davidson, Dirac quantization of the Pais-Uhlenbeck fourth order oscillator, Phys. Rev. A 71, 042110 (2005). (0408104 [hep-th]). 3. P. D. Mannheim, Solution to the ghost problem in fourth order derivative theories, Found. Phys. 37, 532 (2007). (arXiv:0608154 [hep-th]). 4. C. M. Bender and P. D. Mannheim, No-ghost theorem for the fourth-order derivative Pais-Uhlenbeck oscillator model, Phys. Rev. Lett. 100, 110402 (2008). (arXiv:0706.0207 [hep-th]). 5. C. M. Bender and P. D. Mannheim, Giving up the ghost, Jour. Phys. A 41, 304018 (2008). (arXiv:0807.2607 [hep-th]) 6. C. M. Bender and P. D. Mannheim, Exactly solvable PT-symmetric Hamiltonian having no Hermitian counterpart, Phys. Rev. D 78, 025022 (2008). (arXiv:0804.4190 [hep-th]) 7. C. M. Bender and P. D. Mannheim, PT symmetry and necessary and sufficient conditions for the reality of energy eigenvalues, Phys. Lett. A 374, 1616 (2010). (arXiv:0902.1365 [hep-th]) 8. P. D. Mannheim, PT symmetry as a necessary and sufficient condition for unitary time evolution, Phil. Trans. Roy. Soc. A. 371, 20120060 (2013). (arXiv:0912.2635 [hep-th]) 9. C. M. Bender and P. D. Mannheim, PT symmetry in relativistic quantum mechanics, Phys. -
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. -
2014 Observers Challenge List
2014 TMSP Observer's Challenge Atlas page #s # Object Object Type Common Name RA, DEC Const Mag Mag.2 Size Sep. U2000 PSA 18h31m25s 1 IC 1287 Bright Nebula Scutum 20'.0 295 67 -10°47'45" 18h31m25s SAO 161569 Double Star 5.77 9.31 12.3” -10°47'45" Near center of IC 1287 18h33m28s NGC 6649 Open Cluster 8.9m Integrated 5' -10°24'10" Can be seen in 3/4d FOV with above. Brightest star is 13.2m. Approx 50 stars visible in Binos 18h28m 2 NGC 6633 Open Cluster Ophiuchus 4.6m integrated 27' 205 65 Visible in Binos and is about the size of a full Moon, brightest star is 7.6m +06°34' 17h46m18s 2x diameter of a full Moon. Try to view this cluster with your naked eye, binos, and a small scope. 3 IC 4665 Open Cluster Ophiuchus 4.2m Integrated 60' 203 65 +05º 43' Also check out “Tweedle-dee and Tweedle-dum to the east (IC 4756 and NGC 6633) A loose open cluster with a faint concentration of stars in a rich field, contains about 15-20 stars. 19h53m27s Brightest star is 9.8m, 5 stars 9-11m, remainder about 12-13m. This is a challenge obJect to 4 Harvard 20 Open Cluster Sagitta 7.7m integrated 6' 162 64 +18°19'12" improve your observation skills. Can you locate the miniature coathanger close by at 19h 37m 27s +19d? Constellation star Corona 5 Corona Borealis 55 Trace the 7 stars making up this constellation, observe and list the colors of each star asterism Borealis 15H 32' 55” Theta Corona Borealis Double Star 4.2m 6.6m .97” 55 Theta requires about 200x +31° 21' 32” The direction our Sun travels in our galaxy. -
Meteor 36. Évf. 11. Sz. (2006. November)
meteor Tartalom A Magyar Csillagászati Egyesület lapja Magyar-amerikai felfedezésű Journal of the Hungarian Astronomical exobolygó! 3 Association MCSE 1946-2006 5 H-1461 Budapest, Pf. 219., Hungary A lámák földjén 7 TeL/fax: (1) 279-0429 (hétköznap 8-20 ó.) Csillagászati hírek 13 E-mail: [email protected] Honlap: meteor.mcse.hu, www.mcse.hu A Besztercebányai Csillagvizsgáló 19 hirek.csillagaszat.hu A csillagos ég szépsége határtalan 21 Távcsőkészítés HU ISSN 0133-249X Egy új távcső születése 22 Főszerkesztő: Mizser Attila Számítástechnika Szerkesztők: Csaba György Gábor, Az XEphem 25 dr. Kiss László, dr. Kolláth Zoltán, Képmelléklet 34 Sárneczky Krisztián, Taracsák Gábor Csillagászattörténet és Tepliczky István Két közép-európai csillagvizsgáló A Meteor előfizetési díja 2006-ra évfordulójára 57 (nem tagok számára) 5500 Ft Róka Gedeon síremléke a Fiumei úti Egy szám ára: 460 Ft temetőben 62 Kiadványunkat az MCSE tagjai Programajánlat 64 illetményként kapják! Jelenségnaptár (december) 65 Tagnyilvántartás: Tepliczky István Tel.: (1) 464-1357, E-mail: [email protected] Megfigyelések Felelős kiadó: az MCSE elnöke Az egyesületi tagság formái (2006) Nap • rendes tagsági díj (közületek Észlelések (szeptember) 28 számára is!) (illetmény: Meteor + Hold Meteor csili, évkönyv 2006) 5400 Ft A három nővér 29 • rendes tagsági díj Csillagfedések 31 szomszédos országok 6500 Ft Meteorok nem szomszédos országok 9500 Ft 2005. július-augusztusi észlelések 35 • örökös tagdíj 135 000 Ft Üstökösök Az MCSE bankszámla-száma: A Nagy Becsapódás megfigyelése a 62900177-16700448 CARA észlelőhálózattal 38 Az MCSE adószáma: 19009162-2-43 Változócsillagok Az MCSE a beküldött anyagokat non-profit Észlelések (augusztus-szeptember) 44 céllal megjelentetheti az MCSE írott és Mélyég elektronikus fórumain, hacsak a szerző Észlelések (szeptember) 51 írásban másként nem rendelkezik. -
Perseus Perseus
Lateinischer Name: Deutscher Name: Per Perseus Perseus Atlas (2000.0) Karte Cambridge Star Kulmination um 2, 3 Atlas Mitternacht: Benachbarte 1, 4, Sky Atlas Sternbilder: 5 And Ari Aur Cam Cas 7. November Tau Tri Deklinationsbereich: 30° ... 59° Fläche am Himmel: 615° 2 Mythologie und Geschichte: Akrisios war der König von Argos und hatte eine hübsche Tochter namens Danae. Das Orakel von Delphi prophezeite ihm, sein Enkelsohn werde ihn einst töten. Aus Furcht vor diesem Orakelspruch ließ Akrisios seine Tochter Danae in einen Turm einschließen, damit sie keinen Mann empfangen könne. Akrisios konnte natürlich nicht wissen, dass Zeus selbst sich der liebreizenden Danae nähern wollte. Zeus tat dies auch und nahm dazu die Form eines goldenen Regens an, der durch die Wände, Fugen, Ritzen und Fenster drang. Danae gebar einen Sohn, welcher "Der aus fließendem Gold entstandene" oder auch "Der Goldgeborene" genannt wurde - eben den Perseus. Akrisios blieb dies natürlich nicht lange verborgen und er ließ seine Tochter und sein Enkelkind in einen Kasten einnageln, der dann ins Meer geworfen wurde. Danae und Perseus trieben lange Zeit auf dem Meer, bis sie schließlich an der Küste der steinigen Insel Seriphos strandeten und aus ihrem Gefängnis befreit wurden. Auf dieser Insel herrschte Polydektes, der bald jahrelang um die schöne Danae warb, jedoch vergebens. Entweder um Danae doch noch zur Ehe zu zwingen oder um Perseus aus dem Weg zu schaffen, schickte er den inzwischen zum Jüngling herangewachsenen Sohn der Danae aus, eine tödliche Aufgabe zu erledigen. Er solle das Haupt der Medusa zu holen. Die Medusa war eine der Gorgonen, eine der drei Töchter des Phorkys, die mit Schlangenhaaren ausgestattet waren und einen versteinernden Blick werfen konnten. -
A Search For" Dwarf" Seyfert Nuclei. VII. a Catalog of Central Stellar
TO APPEAR IN The Astrophysical Journal Supplement Series. Preprint typeset using LATEX style emulateapj v. 26/01/00 A SEARCH FOR “DWARF” SEYFERT NUCLEI. VII. A CATALOG OF CENTRAL STELLAR VELOCITY DISPERSIONS OF NEARBY GALAXIES LUIS C. HO The Observatories of the Carnegie Institution of Washington, 813 Santa Barbara St., Pasadena, CA 91101 JENNY E. GREENE1 Department of Astrophysical Sciences, Princeton University, Princeton, NJ ALEXEI V. FILIPPENKO Department of Astronomy, University of California, Berkeley, CA 94720-3411 AND WALLACE L. W. SARGENT Palomar Observatory, California Institute of Technology, MS 105-24, Pasadena, CA 91125 To appear in The Astrophysical Journal Supplement Series. ABSTRACT We present new central stellar velocity dispersion measurements for 428 galaxies in the Palomar spectroscopic survey of bright, northern galaxies. Of these, 142 have no previously published measurements, most being rela- −1 tively late-type systems with low velocity dispersions (∼<100kms ). We provide updates to a number of literature dispersions with large uncertainties. Our measurements are based on a direct pixel-fitting technique that can ac- commodate composite stellar populations by calculating an optimal linear combination of input stellar templates. The original Palomar survey data were taken under conditions that are not ideally suited for deriving stellar veloc- ity dispersions for galaxies with a wide range of Hubble types. We describe an effective strategy to circumvent this complication and demonstrate that we can still obtain reliable velocity dispersions for this sample of well-studied nearby galaxies. Subject headings: galaxies: active — galaxies: kinematics and dynamics — galaxies: nuclei — galaxies: Seyfert — galaxies: starburst — surveys 1. INTRODUCTION tors, apertures, observing strategies, and analysis techniques. -
The Stellar Halos of Massive Elliptical Galaxies. Ii
The Astrophysical Journal, 776:64 (12pp), 2013 October 20 doi:10.1088/0004-637X/776/2/64 C 2013. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE STELLAR HALOS OF MASSIVE ELLIPTICAL GALAXIES. II. DETAILED ABUNDANCE RATIOS AT LARGE RADIUS Jenny E. Greene1,3, Jeremy D. Murphy1,4, Genevieve J. Graves1, James E. Gunn1, Sudhir Raskutti1, Julia M. Comerford2,4, and Karl Gebhardt2 1 Department of Astrophysics, Princeton University, Princeton, NJ 08540, USA 2 Department of Astronomy, UT Austin, 1 University Station C1400, Austin, TX 71712, USA Received 2013 June 24; accepted 2013 August 6; published 2013 September 26 ABSTRACT We study the radial dependence in stellar populations of 33 nearby early-type galaxies with central stellar velocity −1 dispersions σ∗ 150 km s . We measure stellar population properties in composite spectra, and use ratios of these composites to highlight the largest spectral changes as a function of radius. Based on stellar population modeling, the typical star at 2Re is old (∼10 Gyr), relatively metal-poor ([Fe/H] ≈−0.5), and α-enhanced ([Mg/Fe] ≈ 0.3). The stars were made rapidly at z ≈ 1.5–2 in shallow potential wells. Declining radial gradients in [C/Fe], which follow [Fe/H], also arise from rapid star formation timescales due to declining carbon yields from low-metallicity massive stars. In contrast, [N/Fe] remains high at large radius. Stars at large radius have different abundance ratio patterns from stars in the center of any present-day galaxy, but are similar to average Milky Way thick disk stars.