GMRT 610 Mhz Observations of Galaxy Clusters in the ACT Equatorial Sample
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16Th HEAD Meeting Session Table of Contents
16th HEAD Meeting Sun Valley, Idaho – August, 2017 Meeting Abstracts Session Table of Contents 99 – Public Talk - Revealing the Hidden, High Energy Sun, 204 – Mid-Career Prize Talk - X-ray Winds from Black Rachel Osten Holes, Jon Miller 100 – Solar/Stellar Compact I 205 – ISM & Galaxies 101 – AGN in Dwarf Galaxies 206 – First Results from NICER: X-ray Astrophysics from 102 – High-Energy and Multiwavelength Polarimetry: the International Space Station Current Status and New Frontiers 300 – Black Holes Across the Mass Spectrum 103 – Missions & Instruments Poster Session 301 – The Future of Spectral-Timing of Compact Objects 104 – First Results from NICER: X-ray Astrophysics from 302 – Synergies with the Millihertz Gravitational Wave the International Space Station Poster Session Universe 105 – Galaxy Clusters and Cosmology Poster Session 303 – Dissertation Prize Talk - Stellar Death by Black 106 – AGN Poster Session Hole: How Tidal Disruption Events Unveil the High 107 – ISM & Galaxies Poster Session Energy Universe, Eric Coughlin 108 – Stellar Compact Poster Session 304 – Missions & Instruments 109 – Black Holes, Neutron Stars and ULX Sources Poster 305 – SNR/GRB/Gravitational Waves Session 306 – Cosmic Ray Feedback: From Supernova Remnants 110 – Supernovae and Particle Acceleration Poster Session to Galaxy Clusters 111 – Electromagnetic & Gravitational Transients Poster 307 – Diagnosing Astrophysics of Collisional Plasmas - A Session Joint HEAD/LAD Session 112 – Physics of Hot Plasmas Poster Session 400 – Solar/Stellar Compact II 113 -
Where Are the Missing Baryons in Clusters?
1 Where Are the Missing Baryons in Clusters? Bilhuda Rasheed Adviser: Dr. Neta Bahcall Submitted in partial fulfillment of the requirements for the degree of Bachelor of Arts Department of Astrophysical Sciences Princeton University May 2010 I hereby declare that I am the sole author of this thesis. I authorize Princeton University to lend this thesis to other institutions or individuals for the purpose of scholarly research. Bilhuda Rasheed I further authorize Princeton University to reproduce this thesis by photocopying or by other means, in total or in part, at the request of other institutions or individuals for the purpose of scholarly research. Bilhuda Rasheed Abstract We address previous claims that the baryon fraction in clusters is significantly below the cosmic value of the baryon fraction as determined from WMAP 7-year results. We use X-ray and SZ observations to determine the slope of the gas density profile to R200. This is shallower than the slope of total mass density (NFW) profile. We use the gas density slope to extrapolate the X-ray observations of gas fraction at R500 to the virial radius (R100). The gas fraction increases beyond R500 for all cluster masses. We add the stellar fraction as determined from COSMOS and 2MASS samples, with ICL contributing 10% to the stellar fraction. For massive clusters 14 (M500 ∼ 7 × 10 M ), the baryon fraction reaches the cosmic baryon fraction at Rvir± 20%. Poorer clusters and groups typically reach 75–85% of the cosmic baryon fraction at the virial radius. We compare these results with simulations which take into account gravitational shock-heating, star formation, heating from SNe and AGN, and energy transfer from dark matter. -
MASS and LIGHT of ABELL 370: a STRONG and WEAK LENSING ANALYSIS ABSTRACT We Present a New Gravitational Lens Model of the Hubble
Draft version October 15, 2018 Preprint typeset using LATEX style emulateapj v. 01/23/15 MASS AND LIGHT OF ABELL 370: A STRONG AND WEAK LENSING ANALYSIS V. Strait1, M. Bradacˇ1, A. Hoag1, K.-H. Huang1, T. Treu2, X. Wang2,4, R. Amorin6,7, M. Castellano5, A. Fontana5, B.-C. Lemaux1, E. Merlin5, K.B. Schmidt3, T. Schrabback8, A. Tomczack1, M. Trenti9,10, and B. Vulcani9,11 1Physics Department, University of California, Davis, CA 95616, USA 2Department of Physics and Astronomy, UCLA, Los Angeles, CA, 90095-1547, USA 3Leibniz-Institut f¨urAstrophysik Postdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 4Department of Physics, University of California, Santa Barbara, CA, 93106-9530, USA 5INAF - Osservatorio Astronomico di Roma Via Frascati 33 - 00040 Monte Porzio Catone, 00040 Rome, Italy 6Cavendish Laboratory, University of Cambridge, 19 JJ Thomson Avenue, CB3 0HE, Cambridge, UK 7Kavli Institute for Cosmology, University of Cambridge, Madingley Rd., CB3 0HA, Cambridge, UK 8Argelander-Institut f¨urAstronomie, Auf dem H¨ugel71, D-53121 Bonn, Germany 9School of Physics, University of Melbourne, Parkville, Victoria, Australia 10ARC Centre of Excellence fot All Sky Astrophysics in 3 Dimensions (ASTRO 3D) and 11INAF - Astronomical Observatory of Padora, 35122 Padova, Italy Draft version October 15, 2018 ABSTRACT We present a new gravitational lens model of the Hubble Frontier Fields cluster Abell 370 (z = 0:375) using imaging and spectroscopy from Hubble Space Telescope and ground-based spectroscopy. We combine constraints from a catalog of 909 weakly lensed galaxies and 39 multiply-imaged sources comprised of 114 multiple images, including a system of multiply-imaged candidates at z = 7:84 ± 0:02, to obtain a best-fit mass distribution using the cluster lens modeling code Strong and Weak Lensing United. -
List of Reserved Targets Sent to GRANTECAN for the Exploitation of the MEGARA Guaranteed Time at GTC
List of Reserved Targets sent to GRANTECAN for the exploitation of the MEGARA Guaranteed Time at GTC List of Reserved Targets sent to GRANTECAN for the exploitation of the MEGARA Guaranteed Time at GTC List of Reserved Targets sent to GRANTECAN for the exploitation of the MEGARA Guaranteed Time at GTC INDEX 1. MEGADES – MEGARA GALAXY DISKS EVOLUTION SURVEY: S4G .................. 3 2. MEGADES – MEGARA GALAXY DISKS EVOLUTION SURVEY: M33 ............... 11 3. SPECTROSCOPIC STUDY OF COMPACT STELLAR CLUSTERS AND THEIR SURROUNDINGS IN NEARBY GALAXIES ........................................................................ 12 4. THE CHEMICAL COMPOSITION OF PHOTOIONIZED NEBULAE¡ERROR! MARCADOR NO DEFINIDO. 5. CHROMOSPHERIC ACTIVITY AND AGE OF SOLAR ANALOGS IN OPEN CLUSTERS ................................................................ ¡ERROR! MARCADOR NO DEFINIDO. 6. STUDY OF STELLAR POPULATIONS AND GAS PROPERTIES IN STAR FORMING GALAXIES ............................................................................................................ 14 7. DISSECTING Z∼2-3 HEII-EMITTERS: SPECTRAL TEMPLATES FOR THE SOURCES OF THE COSMIC DAWN ................................................................................... 16 8. CHEMODYNAMICS OF METAL-POOR EXTREME EMISSION LINE GALAXIES AT INTERMEDIATE Z ...................................................................................... 18 9. CONSTRAINING WOLF-RAYET STARS IN EXTREMELY METAL-POOR GALAXIES ................................................................................................................................ -
An ISOCAM Survey Through Gravitationally Lensing Galaxy Clusters
A&A 431, 433–449 (2005) Astronomy DOI: 10.1051/0004-6361:20041782 & c ESO 2005 Astrophysics An ISOCAM survey through gravitationally lensing galaxy clusters IV. Luminous infrared galaxies in Cl 0024+1654 and the dynamical status of clusters D. Coia1, B. McBreen1,L.Metcalfe2,3,A.Biviano4, B. Altieri2,S.Ott5,B.Fort6,J.-P.Kneib7,8, Y. Mellier6,9, M.-A. Miville-Deschênes10 , B. O’Halloran1,11, and C. Sanchez-Fernandez2 1 Department of Experimental Physics, University College, Belfield, Dublin 4, Ireland e-mail: [email protected] 2 XMM-Newton Science Operations Centre, European Space Agency, Villafranca del Castillo, PO Box 50727, 28080 Madrid, Spain 3 ISO Data Centre, European Space Agency, Villafranca del Castillo, PO Box 50727, 28080 Madrid, Spain 4 INAF/Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11, 34131, Trieste, Italy 5 Science Operations and Data Systems Division of ESA, ESTEC, Keplerlaan 1, 2200 AG Noordwijk, The Netherlands 6 Institut d’Astrophysique de Paris, 98 bis boulevard Arago, 75014 Paris, France 7 Observatoire Midi-Pyrénées, 14 avenue Edouard Belin, 31400 Toulouse, France 8 California Institute of Technology, Pasadena, CA 91125, USA 9 Observatoire de Paris, 61 avenue de l’Observatoire, 75014 Paris, France 10 Canadian Institute for Theoretical Astrophysics, 60 St-George Street, Toronto, Ontario M5S 3H8, Canada 11 Dunsink Observatory, Castleknock, Dublin 15, Ireland Received 3 August 2004 / Accepted 26 October 2004 Abstract. Observations of the core of the massive cluster Cl 0024+1654, at a redshift z ∼ 0.39, were obtained with the Infrared Space Observatory using ISOCAM at 6.7 µm (hereafter 7 µm) and 14.3 µm (hereafter 15 µm). -
The Legacy of Einstein's Eclipse, Gravitational Lensing
The Legacy of Einstein’s Eclipse, Gravitational Lensing Jorge L. Cervantes-Cota 1, Salvador Galindo-Uribarri 1 and George F. Smoot 2,3,4,* 1 Department of Physics, National Institute for Nuclear Research, Km 36.5 Carretera Mexico-Toluca, Ocoyoacac, C.P.52750 Mexico State, Mexico; [email protected] (J.L.C.-C.); [email protected] (S.G.-U.) 2 IAS TT & WF Chao Foundation Professor, Institute for Advanced Study, Hong Kong University of Science and Technology, Clear Water Bay, Kowloon, Hong Kong 3 Université Sorbonne Paris Cité, Laboratoire APC-PCCP, Université Paris Diderot, 10 rue Alice Domon et Leonie Duquet, CEDEX 13, 75205 Paris, France 4 Department of Physics and LBNL, University of California, MS Bldg 50-5505 LBNL, 1 Cyclotron Road, Berkeley, CA 94720, USA * Correspondence: [email protected]; Tel.: +1-510-486-5505 Abstract: A hundred years ago, two British expeditions measured the deflection of starlight by the Sun’s gravitational field, confirming the prediction made by Einstein’s General Theory of Relativity. One hundred years later many physicists around the world are involved in studying the consequences and use as a research tool, of the deflection of light by gravitational fields, a discipline that today receives the generic name of Gravitational Lensing. The present review aims to commemorate the centenary of Einstein’s Eclipse expeditions by presenting a historical perspective of the development and milestones on gravitational light bending, covering from early XIX century speculations, to its current use as an important research tool in astronomy and cosmology. Keywords: gravitational lensing; history of science PACS: 01.65.+g; 98.62.Sb 1. -
Hubble Space Telescope
Hubble Space Telescope Tom Brown STUC Meeting – October 20, 2016 • All science instruments and subsystems are funconing well – Decision made to stay in 3-gyro mode Summary as long as possible (3-3-3-1-1) – Instrument teams busy with standard support and calibraon but looking for improvements and expanded capabilies • Cycle 24 – TAC met 5-10 June, noficaons 24 June – Phase II & budget deadline was 21 July – Cycle 24 officially began on 1 October – Exoplanet & Juno programs prominent • Observing efficiency remains excellent – C23 avg 85 orbits/week and 51% efficiency – New “schedule gap” pilot program execung • HST Contract Extension – 1 July 2016 to 30 June 2021 – Senior Review feedback very posive Frontier Fields Completed Abell 2744 MACSJ0416.1-2403 MACSJ0717.5+3745 MACSJ1149.5+2223 Abell S1063 Abell 370 Frontier Fields Completed Abell 2744-par MACSJ0416.1-2403-par MACSJ0717.5+3745-par MACSJ1149.5+2223-par Abell S1063-par Abell 370-par Frontier Fields Completed Last two fields (Abell S1063, Abell 370) completed 11 Sep 2016 V1.0 high-level HST data products released for all but Abell 370 epoch 2 V0.5 Abell 370 epoch 2 – 3 Oct 2016 V1.0 Abell 370 epoch 2 - by 31 Oct 2016 V2.0 for all clusters - by 15 Dec 2016 Lensing models done for 2 clusters. Next 2 in Feb 2017, then last 2 in Sep 2017. Hubble Science Productivity Remains High Recent Safing Events • STIS suspended on 19 June 2016 while passing through the South Atlantic Anomaly – Consistent with Single Event Upset – Recovered 21 June 2016 with no issues • HST payload safed due to lockup of Science -
Morphology and Kinematics of Z ∼ 1 Galaxies As Seen Through Gravitational Telescopes
Universita` degli Studi di Napoli \Federico II" Dipartimento di Fisica \Ettore Pancini" Corso di Laurea in Fisica Anno Accademico 2017/2018 Tesi di Laurea Magistrale Morphology and kinematics of z ∼ 1 galaxies as seen through gravitational telescopes Relatore: Prof. Giovanni Covone Candidato: Maria Vittoria Milo Matricola: N94000352 Se parlassi le lingue degli uomini e degli angeli, ma non avessi amore, sarei un rame risonante o uno squillante cembalo. Se avessi il dono di profezia e conoscessi tutti i misteri e tutta la scienza e avessi tutta la fede in modo da spostare i monti, ma non avessi amore, non sarei nulla. Se distribuissi tutti i miei beni per nutrire i poveri, se dessi il mio corpo a essere arso, e non avessi amore, non mi gioverebbe a niente. (1 Corinzi 13:1-3) ii Abstract Observing high−z galaxies is an hard challenge for astrophysicists. As much we go back in time (and therefore far away in space), the Universe in which we live becomes smaller, denser and hotter. On the other hand, at high redshift, astro- nomical objects result as fainter as smaller to make their detection impossible even for the most powerful today's telescopes. Hence, trying to determine the morphol- ogy of these high−z galaxies and even to characterize their physical properties (such as kinematics) would result just a dream of a crazy astrophysicist. Fortu- nately, Nature offers a way out, allowing us to overcome the obstacle. Telescopes able to observe regions of the Universe never before reached by any human or artificial \eye" already exist! These are galaxy clusters, the largest known grav- itationally bound structures in the Universe. -
New Evidence for Dark Matter
New evidence for dark matter A. Boyarsky1,2, O. Ruchayskiy1, D. Iakubovskyi2, A.V. Macci`o3, D. Malyshev4 1Ecole Polytechnique F´ed´erale de Lausanne, FSB/ITP/LPPC, BSP CH-1015, Lausanne, Switzerland 2Bogolyubov Institute for Theoretical Physics, Metrologichna str., 14-b, Kiev 03680, Ukraine 3Max-Planck-Institut f¨ur Astronomie, K¨onigstuhl 17, 69117 Heidelberg, Germany 4Dublin Institute for Advanced Studies, 31 Fitzwilliam Place, Dublin 2, Ireland Observations of star motion, emissions from hot ionized gas, gravitational lensing and other tracers demonstrate that the dynamics of galaxies and galaxy clusters cannot be explained by the Newtonian potential produced by visible matter only [1–4]. The simplest resolution assumes that a significant fraction of matter in the Universe, dominating the dynamics of objects from dwarf galaxies to galaxy clusters, does not interact with electromagnetic radiation (hence the name dark matter). This elegant hypothesis poses, however, a major challenge to the highly successful Standard Model of particle physics, as it was realized that dark matter cannot be made of known elementary particles [4]. The quest for direct evidence of the presence of dark matter and for its properties thus becomes of crucial importance for building a fundamental theory of nature. Here we present a new universal relation, satisfied by matter distributions at all observed scales, and show its amaz- ingly good and detailed agreement with the predictions of the most up-to-date pure dark matter simulations of structure formation in the Universe [5–7]. This behaviour seems to be insensitive to the complicated feedback of ordinary matter on dark matter. -
2 the Reflector J
2 THE REFLECTOR ✶ J UNE 2012 4 President’s Notes opean Southern Observatory, Germany) opean Southern Observatory, Report on NEAF 2012; League considering internationaal 5 International Dark-Sky Association IDA’s monthly newsletter Night Watch tino Romaniello (Eur 7 2012 National Young Astronomer Awards 9 Deep Sky Objects edit: NASA, ESA, and Mar The Bridal Veil Nebula 10 The changing view of amateur astronomy Is amateur astronomy getting the interest it once had? 12 As far as Abell George Abell and the galaxy cluster surveys 2012 Leslie C. Peltier Award itle photograph: NGC 1850, the double cluster; Cr 14 T 15 Maximize your membership! A refresher course on League membership benefits 16 Observing Awards 18 Coming Events Devote a weekend to a star party near you Our cover: Contributor Jim Edlin took this image at the Texas Star Party on April 18, 2012 at about 3:50 a.m. Jim added that the star party “was great” with clear skies every night. The shot chosen for the cover was taken with a Nikon D800 which has very low noise and a 36 Mp chip. The exposure was taken at 6400 ISO at 30 second and was enhanced and color corrected in Photoshop. Silhouetted against the Milky Way is Jim’s 28- inch f-3.6 Dobsonian. To our contributors: The copy and photo deadline for the September 2012 issue is July 15. Please send your stories and photos to magazine Editor, Andy Oliver ([email protected]), by then. The Astronomical League invites your comments regarding the magazine. How can we improve it and make it a more valuable source for you, our members? Please respond to Andy Oliver at the email address above. -
Table of Contents May AAC General Meeting No Summer AAC Meetings
TTThehehe FFFTheocalocalocal Atlanta Astronomy Club PPPointointoint Vol. 29 No. 12Established 1947 Editor: Tom Faber May 2017 Table of Contents No Summer AAC Meetings Page 1... May General Meeting, No Summer Meetings, DAV Picnic Due to a decision made by the AAC Board of Directors earlier this year, Page 2... April Meeting Report and Photos the Atlanta Astronomy Club will not hold meetings during the summer months of June, July, and August. This decision was made due to low Page 3... Next CEA Meeting, President’s Desk, Ga Astronomers Mtg attendance at the summer meetings and the difficulty in finding speakers Page 4... Historic Refractor Moving to Arkansas for the summer months. So the next meeting of the Atlanta Astronomy Page 5... Astronomy Day at the Tellus Science Museum Club will be in September at a time and location to be announced. The Charlie Elliott Astronomy chapter of the Atlanta Astronomy Club will Page 6... Hubble Images Galaxy Cluster Abell 370 hold meetings during the summer and have observing after their meetings, Page 7... AAC Online, Memberships, Contact Info weather permitting. AAC members are encouraged to attend these Page 8... Calendar, AAC List Serv Info, Focal Point Deadline meetings. The CEA summer meetings will be on Saturday June 24, July 22, and August 19. Also, since the new moon is now starting to occur around the 3rd weekend of the month, to avoid conflicting with other events held on new moon May AAC General Meeting weekends, starting in September the monthly meetings of the AAC will move to the second Saturday of the month. -
The Hi Gas Content of Galaxies Around Abell 370, a Galaxy Cluster at Z = 0.37
Mon. Not. R. Astron. Soc. 000, 1–27 (2009) Printed 29 October 2018 (MN LATEX style file v2.2) The Hi gas content of galaxies around Abell 370, a galaxy cluster at z = 0.37 Philip Lah1⋆, Michael B. Pracy1, Jayaram N. Chengalur2, Frank H. Briggs1, Matthew Colless3, Roberto De Propris4, Shaun Ferris1, Brian P. Schmidt1 and Bradley E. Tucker1 1 Research School of Astronomy & Astrophysics, The Australian National University, Weston Creek, ACT 2611, Australia 2 National Centre for Radio Astrophysics, Post Bag 3, Ganeshkhind, Pune 411 007, India 3 Anglo-Australian Observatory, PO Box 296, Epping, NSW 2111, Australia 4 Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile Accepted ... Received ...; in original form ... ABSTRACT We used observations from the Giant Metrewave Radio Telescope to measure the atomic hydrogen gas content of 324 galaxies around the galaxy cluster Abell 370 at a redshift of z = 0.37 (a look-back time of ∼4 billion years). The Hi 21-cm emission from these galaxies was measured by coadding their signals using precise optical redshifts obtained with the Anglo-Australian Telescope. The average Hi mass measured for 9 all 324 galaxies is (6.6 ± 3.5) × 10 M⊙, while the average Hi mass measured for 9 the 105 optically blue galaxies is (19.0 ± 6.5) × 10 M⊙. The significant quantities of gas found around Abell 370, suggest that there has been substantial evolution in the gas content of galaxy clusters since redshift z = 0.37. The total amount of atomic hydrogen gas found around Abell 370 is up to ∼8 times more than that seen around the Coma cluster, a nearby galaxy cluster of similar size.