DOCSLIB.ORG

Observing Galaxies in Perseus 11 October 2015 20:33

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Observing Galaxies in Perseus 11 October 2015 20:33 Observing galaxies in Perseus 11 October 2015 20:33 Context As you look towards Perseus you are looking just below the galactic plane under the Perseus spiral arm of our galaxy which itself is about 7,000 light years away. The Perseus-Pisces supercluster wall of galaxies starts in this constellation. It stretches from RA 3h +40 in Perseus to 23h + 10 in Pegasus and is around 200 million light years away. Apart from NGC 1023 the galaxies in this constellation are on the faint side. The constellation is well placed from late summer to early winter. Relatively bright galaxies This section covers the galaxies that were visible with direct vision in my 16 inch or smaller scopes. This list will therefore grow over time as I have not yet viewed all the galaxies in good conditions at maximum altitude in my 16 inch scope! NGC 1023 MAG 9 This is the brightest galaxy in this constellation. It is a fine galaxy to observe and sits in a triangle of stars. I have seen this in my 25 x 100 mm binoculars. It is 36 million light years away and is the lead member of a group of about ten galaxies. NGC 1275 MAG 11 - ABEL 426 This galaxy sits at the heart of the Perseus supercluster 230 million light years away. There are loads of galaxies in this field. I have only managed to see NGC 1272 with my 14 inch scope. By constellation Page 1 NGC 1169 MAG 11 The bright core of this galaxy stands out well in the sparse field of view. NGC 1138 MAG 11 Relatively small galaxy. It was possible to hold it in view with direct vision in my 16 inch scope. By constellation Page 2 Other special galaxies and galaxy groups of note I have set out below a selection of observed galaxies and galaxy groups of note in the constellation. NGC 1161 and NGC 1160 These galaxies form a pair although I was only able to see NGC 1161 in my 10 inch scope. Full list of observed galaxies in Perseus ref1 SIZE SHAPE Visual mag Comments MLY Surf INSTRUMENT scale brtness NGC 1023 medium oval 1 9.4 Nice small galaxy 36 12.8 25 x 100B NGC 1169 small oval 1 11.3 Sparse FOV. Bright core 104 13.8 Skywatcher 10 inch NGC 1275 very small circular 1 11.9 Nice oval galaxy 234 13.1 Darkstar 14 inch NGC 1138 very small circular 1 12.8 Quite obvious with AV 105 12.6 Meade 16 inch NGC 1161 very small circular <0.5 11.0 Hazy evening. This galaxy was faint, 86 12.8 Skywatcher 10 inch By constellation Page 3 NGC 1161 very small circular <0.5 11.0 Hazy evening. This galaxy was faint, 86 12.8 Skywatcher 10 inch only visible with averted vision. No sign of NGC 1160 NGC 1058 small circular <0.5 11.2 Large low sbr irregular galaxy 21 13.4 Skywatcher 10 inch NGC 1003 medium oval <0.5 11.4 Large oval shaped glow 26 13.8 Darkstar 14 inch NGC 1272 very small circular <0.5 11.8 Nice oval galaxy 179 13.2 Darkstar 14 inch NGC 1122 very small circular <0.5 12.1 Very small faint glow! 161 12.9 Skywatcher 10 inch NGC 1106 very small circular <0.5 12.3 Very small round faint galaxy 187 13.4 Skywatcher 10 inch NGC 1167 very small circular <0.5 12.4 Small faint object 218 14.3 Darkstar 14 inch NGC 1129 small circular <0.5 12.5 Oval low sbr - visible with AV only 232 15.2 Meade 16 inch NGC 1175 very small oval <0.5 12.9 Fairly tough and small but reasonably 247 12.9 Skywatcher 10 inch visible with averted vision. Nice star filed to the North of the galaxy. TARGET LIST AT 11 October 2015 Unseen Burnhams galaxies NGC 1270 m12.7 - Third brightest galaxy in Perseus supercluster. NGC 1465 m14.5 - Edge on galaxy with bright core Prepared by Mark Stuart Thornbury UK October 2015 By constellation Page 4 Prepared by Mark Stuart Thornbury UK October 2015 By constellation Page 5 .
Load more

Recommended publications
  • 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.
    [Show full text]
  • 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.
    [Show full text]
  • A Dissertation Entitled Star Cluster Populations in the Spiral Galaxy
    A Dissertation entitled Star Cluster Populations in the Spiral Galaxy M101 by Lesley A. Simanton Submitted to the Graduate Faculty as partial fulfillment of the requirements for the Doctor of Philosophy Degree in Physics Dr. Rupali Chandar, Committee Chair Dr. John-David Smith, Committee Member Dr. Steven Federman, Committee Member Dr. Bo Gao, Committee Member Dr. Bradley Whitmore, Committee Member Dr. Patricia R. Komuniecki, Dean College of Graduate Studies The University of Toledo August 2015 Copyright 2015, Lesley A. Simanton This document is copyrighted material. Under copyright law, no parts of this document may be reproduced without the expressed permission of the author. An Abstract of Star Cluster Populations in the Spiral Galaxy M101 by Lesley A. Simanton Submitted to the Graduate Faculty as partial fulfillment of the requirements for the Doctor of Philosophy Degree in Physics The University of Toledo August 2015 Most stars form in groups and clusters. Stars clusters range in age from very young (< 3 Myr, embedded in gas clouds) to some of the most ancient objects in the universe (> 13 Gyr), providing clues to the formation and evolution of their host galaxies. Our knowledge of the diversity of star cluster populations has expanded over the last few decades, especially by being able to examine star clusters outside of the Milky Way (MW). In this dissertation, we continue this expansion of extragalactic star cluster studies by examining the star cluster system of the nearby spiral galaxy M101. We utilize photometry from Hubble Space T elescope images to assess luminosity, color, size, and spatial distributions of old star clusters, and spectroscopy from the Gemini- North telescope to determine ages, metallicities, and velocities of a subset of both young and old clusters in M101.
    [Show full text]
  • Messier Plus Marathon Text
    Messier Plus Marathon Object List by Wally Brown & Bob Buckner with additional objects by Mike Roos Object Data - Saguaro Astronomy Club Score is most numbered objects in a single night. Tiebreaker is count of un-numbered objects Observer Name Date Address Marathon Obects __________ Tiebreaker Objects ________ SEQ OBJECT TYPE CON R.A. DEC. RISE TRANSIT SET MAG SIZE NOTES TIME M 53 GLOCL COM 1312.9 +1810 7:21 14:17 21:12 7.7 13.0' NGC 5024, !B,vC,iR,vvmbM,st 12.. NGC 5272, !!,eB,vL,vsmbM,st 11.., Lord Rosse-sev dark 1 M 3 GLOCL CVN 1342.2 +2822 7:11 14:46 22:20 6.3 18.0' marks within 5' of center 2 M 5 GLOCL SER 1518.5 +0205 10:17 16:22 22:27 5.7 23.0' NGC 5904, !!,vB,L,eCM,eRi, st mags 11...;superb cluster M 94 GALXY CVN 1250.9 +4107 5:12 13:55 22:37 8.1 14.4'x12.1' NGC 4736, vB,L,iR,vsvmbM,BN,r NGC 6121, Cl,8 or 10 B* in line,rrr, Look for central bar M 4 GLOCL SCO 1623.6 -2631 12:56 17:27 21:58 5.4 36.0' structure M 80 GLOCL SCO 1617.0 -2258 12:36 17:21 22:06 7.3 10.0' NGC 6093, st 14..., Extremely rich and compressed M 62 GLOCL OPH 1701.2 -3006 13:49 18:05 22:21 6.4 15.0' NGC 6266, vB,L,gmbM,rrr, Asymmetrical M 19 GLOCL OPH 1702.6 -2615 13:34 18:06 22:38 6.8 17.0' NGC 6273, vB,L,R,vCM,rrr, One of the most oblate GC 3 M 107 GLOCL OPH 1632.5 -1303 12:17 17:36 22:55 7.8 13.0' NGC 6171, L,vRi,vmC,R,rrr, H VI 40 M 106 GALXY CVN 1218.9 +4718 3:46 13:23 22:59 8.3 18.6'x7.2' NGC 4258, !,vB,vL,vmE0,sbMBN, H V 43 M 63 GALXY CVN 1315.8 +4201 5:31 14:19 23:08 8.5 12.6'x7.2' NGC 5055, BN, vsvB stell.
    [Show full text]
  • Winter Constellations
    Winter Constellations *Orion *Canis Major *Monoceros *Canis Minor *Gemini *Auriga *Taurus *Eradinus *Lepus *Monoceros *Cancer *Lynx *Ursa Major *Ursa Minor *Draco *Camelopardalis *Cassiopeia *Cepheus *Andromeda *Perseus *Lacerta *Pegasus *Triangulum *Aries *Pisces *Cetus *Leo (rising) *Hydra (rising) *Canes Venatici (rising) Orion--Myth: Orion, the great ​ ​ hunter. In one myth, Orion boasted he would kill all the wild animals on the earth. But, the earth goddess Gaia, who was the protector of all animals, produced a gigantic scorpion, whose body was so heavily encased that Orion was unable to pierce through the armour, and was himself stung to death. His companion Artemis was greatly saddened and arranged for Orion to be immortalised among the stars. Scorpius, the scorpion, was placed on the opposite side of the sky so that Orion would never be hurt by it again. To this day, Orion is never seen in the sky at the same time as Scorpius. DSO’s ● ***M42 “Orion Nebula” (Neb) with Trapezium A stellar ​ ​ ​ nursery where new stars are being born, perhaps a thousand stars. These are immense clouds of interstellar gas and dust collapse inward to form stars, mainly of ionized hydrogen which gives off the red glow so dominant, and also ionized greenish oxygen gas. The youngest stars may be less than 300,000 years old, even as young as 10,000 years old (compared to the Sun, 4.6 billion years old). 1300 ly. ​ ​ 1 ● *M43--(Neb) “De Marin’s Nebula” The star-forming ​ “comma-shaped” region connected to the Orion Nebula. ● *M78--(Neb) Hard to see. A star-forming region connected to the ​ Orion Nebula.
    [Show full text]
  • 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”.
    [Show full text]
  • X-Ray and Gamma-Ray Variability of NGC 1275
    galaxies Article X-ray and Gamma-ray Variability of NGC 1275 Varsha Chitnis 1,*,† , Amit Shukla 2,*,† , K. P. Singh 3 , Jayashree Roy 4 , Sudip Bhattacharyya 5, Sunil Chandra 6 and Gordon Stewart 7 1 Department of High Energy Physics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India 2 Discipline of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Khandwa Road, Simrol, Indore 453552, India 3 Indian Institute of Science Education and Research Mohali, Knowledge City, Sector 81, SAS Nagar, Manauli 140306, India; [email protected] 4 Inter-University Centre for Astronomy and Astrophysics, Ganeshkhind, Pune 411 007, India; [email protected] 5 Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Homi Bhabha Road, Mumbai 400005, India; [email protected] 6 Centre for Space Research, North-West University, Potchefstroom 2520, South Africa; [email protected] 7 Department of Physics and Astronomy, The University of Leicester, University Road, Leicester LE1 7RH, UK; [email protected] * Correspondence: [email protected] (V.C.); [email protected] (A.S.) † These authors contributed equally to this work. Received: 30 June 2020; Accepted: 24 August 2020; Published: 28 August 2020 Abstract: Gamma-ray emission from the bright radio source 3C 84, associated with the Perseus cluster, is ascribed to the radio galaxy NGC 1275 residing at the centre of the cluster. Study of the correlated X-ray/gamma-ray emission from this active galaxy, and investigation of the possible disk-jet connection, are hampered because the X-ray emission, particularly in the soft X-ray band (2–10 keV), is overwhelmed by the cluster emission.
    [Show full text]
  • 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.
    [Show full text]
  • A Basic Requirement for Studying the Heavens Is Determining Where In
    Abasic requirement for studying the heavens is determining where in the sky things are. To specify sky positions, astronomers have developed several coordinate systems. Each uses a coordinate grid projected on to the celestial sphere, in analogy to the geographic coordinate system used on the surface of the Earth. The coordinate systems differ only in their choice of the fundamental plane, which divides the sky into two equal hemispheres along a great circle (the fundamental plane of the geographic system is the Earth's equator) . Each coordinate system is named for its choice of fundamental plane. The equatorial coordinate system is probably the most widely used celestial coordinate system. It is also the one most closely related to the geographic coordinate system, because they use the same fun­ damental plane and the same poles. The projection of the Earth's equator onto the celestial sphere is called the celestial equator. Similarly, projecting the geographic poles on to the celest ial sphere defines the north and south celestial poles. However, there is an important difference between the equatorial and geographic coordinate systems: the geographic system is fixed to the Earth; it rotates as the Earth does . The equatorial system is fixed to the stars, so it appears to rotate across the sky with the stars, but of course it's really the Earth rotating under the fixed sky. The latitudinal (latitude-like) angle of the equatorial system is called declination (Dec for short) . It measures the angle of an object above or below the celestial equator. The longitud inal angle is called the right ascension (RA for short).
    [Show full text]
  • 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.
    [Show full text]
  • Herschel Observations of Extended Atomic Gas in the Core of the Perseus Cluster R
    University of Kentucky UKnowledge Physics and Astronomy Faculty Publications Physics and Astronomy 2012 Herschel Observations of Extended Atomic Gas in the Core of the Perseus Cluster R. Mittal Rochester Institute of Technology J. B. R. Oonk Netherlands Institute for Radio Astronomy, Netherlands Gary J. Ferland University of Kentucky, [email protected] A. C. Edge Durham University, UK C. P. O'Dea Rochester Institute of Technology See next page for additional authors Right click to open a feedback form in a new tab to let us know how this document benefits oy u. Follow this and additional works at: https://uknowledge.uky.edu/physastron_facpub Part of the Astrophysics and Astronomy Commons, and the Physics Commons Repository Citation Mittal, R.; Oonk, J. B. R.; Ferland, Gary J.; Edge, A. C.; O'Dea, C. P.; Baum, S. A.; Whelan, J. T.; Johnstone, R. M.; Combes, F.; Salomé, P.; Fabian, A. C.; Tremblay, G. R.; Donahue, M.; and H., Russell H., "Herschel Observations of Extended Atomic Gas in the Core of the Perseus Cluster" (2012). Physics and Astronomy Faculty Publications. 29. https://uknowledge.uky.edu/physastron_facpub/29 This Article is brought to you for free and open access by the Physics and Astronomy at UKnowledge. It has been accepted for inclusion in Physics and Astronomy Faculty Publications by an authorized administrator of UKnowledge. For more information, please contact [email protected]. Authors R. Mittal, J. B. R. Oonk, Gary J. Ferland, A. C. Edge, C. P. O'Dea, S. A. Baum, J. T. Whelan, R. M. Johnstone, F. Combes, P. Salomé, A. C.
    [Show full text]
  • 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.
    [Show full text]