Monthly Notices of the Everglades Astronomical
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Jurnal Fizik Malaysia Volume 39 Issue 1 (2018) pgs 10017-10028 Z. Zainal Abidin Study of A1367 Cluster by Curve Fitting Variations Zamri Zainal Abidina, Zainol Abidin Ibrahima, Low Wei Yewa, Muhammad Mustaqim Mezana, Danial Ahmad Ariffin Leea, and Christine Jordanb aRadio Cosmology Laboratory Department of Physics, Faculty of Science, University of Malaya, 50603 Kuala Lumpur, Malaysia. bThe School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL (Received: 17.12.2017 ; Published: 23.7.2018) Abstract. We investigate the possible gain spectrum of the A1367 cluster or more commonly known as the Leo cluster using different polynomial fitting techniques in DRAWSPEC. For one of the aspects of the research on the possible mass of dark matter in the Leo cluster, the mass of neutral hydrogen ( ) is to be determined using gain analysis in the DRAWSPEC programme, prior to using the virialized mass of the Leo cluster to determine the mass of dark matter in the cluster. This investigation is significant because by using different polynomial fittings, one set of data could yield different gain, thus providing different , ultimately affecting the calculation of mass of dark matter in a cluster. In this paper, we present a comparison between different gain spectrum and using different polynomial fittings and we conclude that the result yields different by using different curve fitting techniques. Keywords: galaxy cluster-curve fitting-neutral hydrogen mass-gain spectrum- DRAWSPEC I. INTRODUCTION When determining the mass of all the observable matter in a galaxy cluster, interstellar matter plays a role in contributing to the mass [1]. Among the interstellar matters taken into consideration, neutral hydrogen (HI) is chosen due to the fact that starlight is not required to give off 21cm line emission and is generally abundant in clusters [2]. -
Extended Ionized Gas out of Galaxies in the Leo Cluster (Abell 1367)
Extended Ionized Gas out of Galaxies in the Leo Cluster (Abell 1367) YAGI, Masafumi, YOSHIDA, Michitoshi, KOMIYAMA, Yutaka, KASHIKAWA, Nobunari (NAOJ) GAVAZZI, Giuseppe OKAMURA, Sadanori (University of Milano-Bicocca) (Hosei University) In clusters of galaxies, the relative motion of member galaxies to the hot gas of the cluster produces a ram pressure. The ram pressure strips gas from galaxies, and sometimes the gas stripped out of the galaxy gets ionized by some mechanism to be detected as an Hα emitting cloud. We observed a part of the Virgo cluster and the Coma cluster, in Hα narrow-band, and B, and R broad-bands of the Subaru Suprime-Cam to study such intergalactic ionized gas (e.g., [1,2]). We then executed a systematic survey of the Leo cluster (Abell 1367) with an Hα filter for redshift z=0.022 of the Suprime-Cam [3]. By the survey, we detected six new extended ionized gas clouds in addition to three galaxies with known gas tails (CGCG 097-073, CGCG 097-079, CGCG 097- 087; [4]), and one of the new clouds was confirmed to have much longer tail by a follow-up observation [5]. Remarkable objects compared to the previous studies were the clouds which show no relation to the galaxies; “Orphan clouds” (Figure 1 top). Other clouds known so far show the connection to the galaxy from which the gas came from (parent galaxies). Meanwhile, no parent candidates are found at least within 85 kpc from the orphan clouds, and any member galaxies around the region show no sign of stripping toward the orphans. -
8603517.PDF (12.42Mb)
Umversify Microfilins International 1.0 12.5 12.0 LI 1.8 1.25 1.4 1.6 MICROCOPY RESOLUTION TEST CHART NATIONAL BUREAU OF STANDARDS STANDARD REFERENCE MATERIAL 1010a (ANSI and ISO TEST CHART No. 2) University Microfilms Inc. 300 N. Zeeb Road, Ann Arbor, MI 48106 INFORMATION TO USERS This reproduction was made from a copy of a manuscript sent to us for publication and microfilming. While the most advanced technology has been used to pho tograph and reproduce this manuscript, the quality of the reproduction is heavily dependent upon the quality of the material submitted. Pages in any manuscript may have indistinct print. In all cases the best available copy has been filmed. The following explanation of techniques is provided to help clarify notations which may appear on this reproduction. 1. Manuscripts may not always be complete. When it is not possible to obtain missing pages, a note appears to indicate this. 2. When copyrighted materials are removed from the manuscript, a note ap pears to indicate this. 3. Oversize materials (maps, drawings, and charts) are photographed by sec tioning the original, beginning at the upper left hand comer and continu ing from left to right in equal sections with small overlaps. Each oversize page is also filmed as one exposure and is available, for an additional charge, as a standard 35mm slide or in black and white paper format.* 4. Most photographs reproduce acceptably on positive microfilm or micro fiche but lack clarify on xerographic copies made from the microfilm. For an additional charge, all photographs are available in black and white standard 35mm slide format. -
Ricardo Ogando Observatório Nacional
Galaxy Clusters Hunters Ricardo Ogando Observatório Nacional South American Workshop on Cosmology in the LSST Era matter distribution in space 2 South American Workshop on Cosmology in the LSST Era "São Paulo" 3 SouthThierry American Workshop Cohen on Cosmology in the LSST Era 90's revolutions First large 2D galaxy surveys APOD 4 South American Workshop on Cosmology in the LSST Era Detailing the structures with spectra ● CfA2 ○ Geller & Huchra 1989 ● SSRS2 ○ da Costa et al. 1994 Reticon 5 South American Workshop on Cosmology in the LSST Era More observations and simulations ● 2dFGRS and SDSS ○ large samples ○ clustering versus physical properties ■ luminosity ■ color ■ stellar mass 6 South American Workshop on Cosmology in the LSST Era Springel et al. 2006 how to detect a galaxy cluster? 7 South American Workshop on Cosmology in the LSST Era Galaxy Cluster optical samples ● Abell (1958) 2,712 rich clusters z ≤ 0.2 8 South American Workshop on Cosmology in the LSST Era Leo Cluster. Galaxy Cluster optical samples 9 South American Workshop on Cosmology in the LSST Era Leo Cluster. Waid Observatory Coma Cluster HST ACS 10 South American Workshop on Cosmology in the LSST Era 11 South American Workshop on Cosmology in the LSST Era SZ X-ray effect Coma cluster Copyright: Planck image: ESA/ LFI & HFI Consortia; ROSAT image: Max-Planck-Institut für extraterrestrische Physik; DSS image: (Abell NASA, ESA, and the Digitized Sky Survey 2. Acknowledgment: Davide De Martin (ESA/Hubble) 1656) 12 South American Workshop on Cosmology in the LSST Era Weak lensing Science News Emily Conover 13 South American Workshop on Cosmology in the LSST Era August 25, 2017 160403 1743 677 14 15 16 South American Workshop on Cosmology in the LSST Era SDSS galaxy cluster Samples (all reportedly very pure and complete*) Authors Publication # clusters z max Miller et al. -
Orders of Magnitude (Length) - Wikipedia
03/08/2018 Orders of magnitude (length) - Wikipedia Orders of magnitude (length) The following are examples of orders of magnitude for different lengths. Contents Overview Detailed list Subatomic Atomic to cellular Cellular to human scale Human to astronomical scale Astronomical less than 10 yoctometres 10 yoctometres 100 yoctometres 1 zeptometre 10 zeptometres 100 zeptometres 1 attometre 10 attometres 100 attometres 1 femtometre 10 femtometres 100 femtometres 1 picometre 10 picometres 100 picometres 1 nanometre 10 nanometres 100 nanometres 1 micrometre 10 micrometres 100 micrometres 1 millimetre 1 centimetre 1 decimetre Conversions Wavelengths Human-defined scales and structures Nature Astronomical 1 metre Conversions https://en.wikipedia.org/wiki/Orders_of_magnitude_(length) 1/44 03/08/2018 Orders of magnitude (length) - Wikipedia Human-defined scales and structures Sports Nature Astronomical 1 decametre Conversions Human-defined scales and structures Sports Nature Astronomical 1 hectometre Conversions Human-defined scales and structures Sports Nature Astronomical 1 kilometre Conversions Human-defined scales and structures Geographical Astronomical 10 kilometres Conversions Sports Human-defined scales and structures Geographical Astronomical 100 kilometres Conversions Human-defined scales and structures Geographical Astronomical 1 megametre Conversions Human-defined scales and structures Sports Geographical Astronomical 10 megametres Conversions Human-defined scales and structures Geographical Astronomical 100 megametres 1 gigametre -
Arxiv:2007.04414V1 [Astro-Ph.CO] 8 Jul 2020 Bution of Matter on Large Scales Is Inferred from Tion)
Key words: large scale structure of universe | galaxies: distances and redshifts Draft version July 10, 2020 Typeset using LATEX preprint2 style in AASTeX62 Cosmicflows-3: The South Pole Wall Daniel Pomarede,` 1 R. Brent Tully,2 Romain Graziani,3 Hel´ ene` M. Courtois,4 Yehuda Hoffman,5 and Jer´ emy´ Lezmy4 1Institut de Recherche sur les Lois Fondamentales de l'Univers, CEA Universit´eParis-Saclay, 91191 Gif-sur-Yvette, France 2Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822, USA 3Laboratoire de Physique de Clermont, Universit Clermont Auvergne, Aubire, France 4University of Lyon, UCB Lyon 1, CNRS/IN2P3, IUF, IP2I Lyon, France 5Racah Institute of Physics, Hebrew University, Jerusalem, 91904 Israel ABSTRACT Velocity and density field reconstructions of the volume of the universe within 0:05c derived from the Cosmicflows-3 catalog of galaxy distances has revealed the presence of a filamentary structure extending across ∼ 0:11c. The structure, at a characteristic redshift of 12,000 km s−1, has a density peak coincident with the celestial South Pole. This structure, the largest contiguous feature in the local volume and comparable to the Sloan Great Wall at half the distance, is given the name the South Pole Wall. 1. INTRODUCTION ble of measurements: to a first approximation The South Pole Wall rivals the Sloan Great Vpec = Vobs − H0d. Although uncertainties with Wall in extent, at a distance a factor two individual galaxies are large, the analysis bene- closer. The iconic structures that have trans- fits from the long range correlated nature of the formed our understanding of large scale struc- cosmic flow, allowing the reconstruction of the ture have come from the observed distribution 3D velocity field from noisy, finite and incom- of galaxies assembled from redshift surveys: the plete data (Zaroubi et al. -
2013Auguststarstuff
Volume 23, Number 8 August 2013 Size Does Matter, But containing more than 3,000 In This Issue So Does Dark Energy galaxies. There are millions of giant clusters like this in our Page One By Dr. Ethan Siegel observable universe, and the gravitational forces at play are Size Does Matter, But Here in our own galactic absolutely tremendous: there So Does Dark Energy backyard, the Milky Way are literally quadrillions of contains some 200-400 billion times the mass of our Sun in Inside Stuff stars, and that's not even the these systems. biggest galaxy in our own local 4 Treasurers Report group. Andromeda (M31) is The largest superclusters even bigger and more massive line up along filaments, forming 4 Equipment List than we are, made up of a great cosmic web of structure around a trillion stars! When with huge intergalactic voids in 4 Meeting Agenda you throw in the Triangulum between the galaxy-rich regions. These galaxy filaments 5 Astro-Imaging SIG Galaxy (M33), the Large and Small Magellanic Clouds, and span anywhere from hundreds 6 FAAC Meeting the dozens of dwarf galaxies of millions of light-years all the Minutes - July 25, and hundreds of globular way up to more than a billion 2013 clusters gravitationally bound light years in length. The CfA2 Great Wall, the Sloan Great 7 HJRO Update to us and our nearest neighbors, our local group sure Wall, and most recently, the does seem impressive. Huge-LQG (Large Quasar Group) are the largest known Yet that's just chicken feed ones, with the Huge-LQG -- a compared to the largest group of at least 73 quasars – structures in the universe. -
October 2013 by Observer Editor, Paul Tartabini
BACKBACK BAYBAY observerobserver The Official Newsletter of the Back Bay Amateur Astronomers P.O. Box 9877, Virginia Beach, VA 23450-9877 Looking Up! EPHEMERALS Editor’s Note: This month’s Looking Up column was written october 2013 by Observer Editor, Paul Tartabini. Have you ever found yourself “giving up” on deep sky observing at your home because of light pollution? As much as I love observing at dark locations, a fact of life for me right now is that most of my observing takes place at my home in the middle of the light-polluted 10/11, 7:30 PM Peninsula. I have learned to adapt and have acquired quite Garden Stars a love for double stars and lunar observing, but I recently Norfolk Botanical Gardens noticed that I was neglecting deep sky observing from home, not because I wasn’t interested, but mostly because of my frustration with light pollution and yard lights. 10/25 After reading an article in the November Sky and Skywatch Telescope on viewing globular clusters of the Andromeda Northwest River Park galaxy, I decided that I could not wait until the next chance I had to get out to a dark site to try to find one of these extragalactic treats. So on Oct. 3, I spent about an hour using blankets, tarps and even taped newspaper to 10/31 - 11/02 block every single extraneous light source that I could see East Coast Star Party from my favorite observing spot. I set my alarm for early Coinjock, NC morning, when I knew light pollution is at its minimum. -