The Antarctic Sun, February 4, 2001
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UNIVERSIT`A DEGLI STUDI DI TRIESTE Using Hydrodynamical
UNIVERSITA` DEGLI STUDI DI TRIESTE Facolt`adi Scienze Matematiche, Fisiche e Naturali Dottorato di Ricerca in Fisica - XX Ciclo Using hydrodynamical simulations to combine Sunyaev–Zeldovich and X–ray studies of galaxy clusters DOTTORANDA COORDINATORE DEL COLLEGIO DEI DOCENTI Silvia Ameglio Chiar.mo Prof. Gaetano Senatore, Universit`adi Trieste TUTORE Chiar.mo Prof. Stefano Borgani, Universit`adi Trieste RELATORE Chiar.mo Prof. Stefano Borgani, Universit`adi Trieste a.a. 2006/2007 Contents 1 Introduction 1 2 Clusters of galaxies: an overview 5 2.1 X–rayemission ................................. 6 2.2 The Sunyaev–Zeldovich effect (SZ) . ... 8 2.2.1 The thermal Sunyaev–Zeldovich effect (tSZ) . .... 8 2.2.2 The kinetic Sunyaev–Zeldovich effect . 11 2.3 Statusofobservations . .. .. .. .. .. .. .. .. 11 2.3.1 X–rays.................................. 11 2.3.2 The Sunyaev–Zeldovich effect . 17 2.4 Cosmology with galaxy clusters . 23 2.5 Conclusions ................................... 29 3 Hydrodynamical simulations of galaxy clusters 31 3.1 The gravitational dynamics: the N–body TREE code . ...... 31 3.2 The gas physics: Smoothed Particle Hydrodynamics (SPH) ........ 33 3.3 Thesetofsimulatedclusters . 35 3.3.1 Thermal processes in the IntraCluster Medium (ICM) . ..... 38 3.3.2 The sample of simulated clusters . 40 3.3.3 Generation of tSZ, X–ray and temperature maps . 41 3.4 Definitionsoftemperature. 45 4 The angular diameter distance measurement 51 4.1 The polytropic β–model ............................ 53 4.2 DA from combined X-ray and tSZ observations . 53 4.3 Results...................................... 55 4.3.1 Resultsfromtheisothermalmodel . 55 4.3.2 Resultsfromthepolytropicfit . 57 4.3.3 Implications for cosmological parameters . ...... 60 4.4 Conclusions .................................. -
Detection of Polarization in the Cosmic Microwave Background Using DASI
Detection of Polarization in the Cosmic Microwave Background using DASI Thesis by John M. Kovac A Dissertation Submitted to the Faculty of the Division of the Physical Sciences in Candidacy for the Degree of Doctor of Philosophy The University of Chicago Chicago, Illinois 2003 Copyright c 2003 by John M. Kovac ° (Defended August 4, 2003) All rights reserved Acknowledgements Abstract This is a sample acknowledgement section. I would like to take this opportunity to The past several years have seen the emergence of a new standard cosmological model thank everyone who contributed to this thesis. in which small temperature di®erences in the cosmic microwave background (CMB) I would like to take this opportunity to thank everyone. I would like to take on degree angular scales are understood to arise from acoustic oscillations in the hot this opportunity to thank everyone. I would like to take this opportunity to thank plasma of the early universe, sourced by primordial adiabatic density fluctuations. In everyone. the context of this model, recent measurements of the temperature fluctuations have led to profound conclusions about the origin, evolution and composition of the uni- verse. Given knowledge of the temperature angular power spectrum, this theoretical framework yields a prediction for the level of the CMB polarization with essentially no free parameters. A determination of the CMB polarization would therefore provide a critical test of the underlying theoretical framework of this standard model. In this thesis, we report the detection of polarized anisotropy in the Cosmic Mi- crowave Background radiation with the Degree Angular Scale Interferometer (DASI), located at the Amundsen-Scott South Pole research station. -
2006-2007 Science Planning Summaries
Project Indexes Find information about projects approved for the 2006-2007 USAP field season using the available indexes. Project Web Sites Find more information about 2006-2007 USAP projects by viewing project web sites. More Information Additional information pertaining to the 2006-2007 Field Season. Home Page Station Schedules Air Operations Staffed Field Camps Event Numbering System 2006-2007 USAP Field Season Project Indexes Project Indexes Find information about projects approved for the 2006-2007 USAP field season using the USAP Program Indexes available indexes. Aeronomy and Astrophysics Dr. Bernard Lettau, Program Director (acting) Project Web Sites Biology and Medicine Dr. Roberta Marinelli, Program Director Find more information about 2006-2007 USAP projects by Geology and Geophysics viewing project web sites. Dr. Thomas Wagner, Program Director Glaciology Dr. Julie Palais, Program Director More Information Ocean and Climate Systems Additional information pertaining Dr. Bernhard Lettau, Program Director to the 2006-2007 Field Season. Artists and Writers Home Page Ms. Kim Silverman, Program Director Station Schedules USAP Station and Vessel Indexes Air Operations Staffed Field Camps Amundsen-Scott South Pole Station Event Numbering System McMurdo Station Palmer Station RVIB Nathaniel B. Palmer ARSV Laurence M. Gould Special Projects Principal Investigator Index Deploying Team Members Index Institution Index Event Number Index Technical Event Index Project Web Sites 2006-2007 USAP Field Season Project Indexes Project Indexes Find information about projects approved for the 2006-2007 USAP field season using the Project Web Sites available indexes. Principal Investigator/Link Event No. Project Title Aghion, Anne W-218-M Works and days: An antarctic Project Web Sites chronicle Find more information about 2006-2007 USAP projects by Ainley, David B-031-M Adélie penguin response to viewing project web sites. -
From Current Cmbology to Its Polarization and SZ Frontiers Circa TAW8 3
AMiBA 2001: High-z Clusters, Missing Baryons, and CMB Polarization ASP Conference Series, Vol. 999, 2002 L-W Chen, C-P Ma, K-W Ng and U-L Pen, eds Concluding Remarks: From Current CMBology to its Polarization and Sunyaev-Zeldovich Frontiers circa TAW8 J. Richard Bond Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, M5S 3H8, Canada Abstract. I highlight the remarkable advances in the past few years in CMB research on total primary anisotropies, in determining the power spectrum, deriving cosmological parameters from it, and more generally lending credence to the basic inflation-based paradigm for cosmic struc- ture formation, with a flat geometry, substantial dark matter and dark energy, baryonic density in good accord with that from nucleosynthe- sis, and a nearly scale invariant initial fluctuation spectrum. Some pa- rameters are nearly degenerate with others and CMB polarization and many non-CMB probes are needed to determine them, even within the paradigm. Such probes and their tools were the theme of the TAW8 meeting: our grand future of CMB polarization, with AMiBA, ACBAR, B2K2, CBI, COMPASS, CUPMAP, DASI, MAP, MAXIPOL, PIQUE, Planck, POLAR, Polatron, QUEST, Sport/BaRSport, and of Sunyaev- Zeldovich experiments, also using an array of platforms and detectors, e.g., AMiBA, AMI (Ryle+), CBI, CARMA (OVROmm+BIMA), MINT, SZA, BOLOCAM+CSO, LMT, ACT. The SZ probe will be informed and augmented by new ambitious attacks on other cluster-system observables discussed at TAW8: X-ray, optical, weak lensing. Interpreting the mix is complicated by such issues as entropy injection, inhomogeneity, non- sphericity, non-equilibrium, and these effects must be sorted out for the cluster system to contribute to “high precision cosmology”, especially the quintessential physics of the dark energy that adds further mystery to a dark matter dominated Universe. -
Observational Cosmology - 30H Course 218.163.109.230 Et Al
Observational cosmology - 30h course 218.163.109.230 et al. (2004–2014) PDF generated using the open source mwlib toolkit. See http://code.pediapress.com/ for more information. PDF generated at: Thu, 31 Oct 2013 03:42:03 UTC Contents Articles Observational cosmology 1 Observations: expansion, nucleosynthesis, CMB 5 Redshift 5 Hubble's law 19 Metric expansion of space 29 Big Bang nucleosynthesis 41 Cosmic microwave background 47 Hot big bang model 58 Friedmann equations 58 Friedmann–Lemaître–Robertson–Walker metric 62 Distance measures (cosmology) 68 Observations: up to 10 Gpc/h 71 Observable universe 71 Structure formation 82 Galaxy formation and evolution 88 Quasar 93 Active galactic nucleus 99 Galaxy filament 106 Phenomenological model: LambdaCDM + MOND 111 Lambda-CDM model 111 Inflation (cosmology) 116 Modified Newtonian dynamics 129 Towards a physical model 137 Shape of the universe 137 Inhomogeneous cosmology 143 Back-reaction 144 References Article Sources and Contributors 145 Image Sources, Licenses and Contributors 148 Article Licenses License 150 Observational cosmology 1 Observational cosmology Observational cosmology is the study of the structure, the evolution and the origin of the universe through observation, using instruments such as telescopes and cosmic ray detectors. Early observations The science of physical cosmology as it is practiced today had its subject material defined in the years following the Shapley-Curtis debate when it was determined that the universe had a larger scale than the Milky Way galaxy. This was precipitated by observations that established the size and the dynamics of the cosmos that could be explained by Einstein's General Theory of Relativity. -
Extrapolation of Galactic Dust Emission at 100 Microns to Cosmic Microwave Background Radiation Frequencies Using FIRAS
Extrapolation of Galactic Dust Emission at 100 Microns to Cosmic Microwave Background Radiation Frequencies Using FIRAS The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Finkbeiner, Douglas P., Marc Davis, and David J. Schlegel. 1999. “Extrapolation of Galactic Dust Emission at 100 Microns to Cosmic Microwave Background Radiation Frequencies Using FIRAS.” The Astrophysical Journal 524 (2) (October 20): 867–886. doi:10.1086/307852. Published Version 10.1086/307852 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:33462888 Terms of Use This article was downloaded from Harvard University’s DASH repository, and is made available under the terms and conditions applicable to Other Posted Material, as set forth at http:// nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of- use#LAA THE ASTROPHYSICAL JOURNAL, 524:867È886, 1999 October 20 ( 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. EXTRAPOLATION OF GALACTIC DUST EMISSION AT 100 MICRONS TO COSMIC MICROWAVE BACKGROUND RADIATION FREQUENCIES USING FIRAS DOUGLAS P. FINKBEINER AND MARC DAVIS University of California at Berkeley, Departments of Physics and Astronomy, 601 Campbell Hall, Berkeley, CA 94720; dÐnk=astro.berkeley.edu, marc=deep.berkeley.edu AND DAVID J. SCHLEGEL Princeton University, Department of Astrophysics, Peyton Hall, Princeton, NJ 08544; schlegel=astro.princeton.edu Received 1999 March 5; accepted 1999 June 8 ABSTRACT We present predicted full-sky maps of submillimeter and microwave emission from the di†use inter- stellar dust in the Galaxy. These maps are extrapolated from the 100 km emission and 100/240 km Ñux ratio maps that Schlegel, Finkbeiner, & Davis generated from IRAS and COBE/DIRBE data. -
A Fast Iterative Multi-Grid Map-Making Algorithm for CMB Experiments
A&A 374, 358–370 (2001) Astronomy DOI: 10.1051/0004-6361:20010692 & c ESO 2001 Astrophysics MAPCUMBA: A fast iterative multi-grid map-making algorithm for CMB experiments O. Dor´e1,R.Teyssier1,2,F.R.Bouchet1,D.Vibert1, and S. Prunet3 1 Institut d’Astrophysique de Paris, 98bis, Boulevard Arago, 75014 Paris, France 2 Service d’Astrophysique, DAPNIA, Centre d’Etudes´ de Saclay, 91191 Gif-sur-Yvette, France 3 CITA, McLennan Labs, 60 St George Street, Toronto, ON M5S 3H8, Canada Received 21 December 2000 / Accepted 2 May 2001 Abstract. The data analysis of current Cosmic Microwave Background (CMB) experiments like BOOMERanG or MAXIMA poses severe challenges which already stretch the limits of current (super-) computer capabilities, if brute force methods are used. In this paper we present a practical solution for the optimal map making problem which can be used directly for next generation CMB experiments like ARCHEOPS and TopHat, and can probably be extended relatively easily to the full PLANCK case. This solution is based on an iterative multi-grid Jacobi algorithm which is both fast and memory sparing. Indeed, if there are Ntod data points along the one dimensional timeline to analyse, the number of operations is of O(Ntod ln Ntod) and the memory requirement is O(Ntod). Timing and accuracy issues have been analysed on simulated ARCHEOPS and TopHat data, and we discuss as well the issue of the joint evaluation of the signal and noise statistical properties. Key words. methods: data analysis – cosmic microwave background 1. Introduction in this massive computing approach, i.e. -
Mid-Infrared Selection of Brown Dwarfs and High-Redshift Quasars
Submitted to the Astrophysical Journal Mid-Infrared Selection of Brown Dwarfs and High-Redshift Quasars Daniel Stern1, J. Davy Kirkpatrick2, Lori E. Allen3, Chao Bian4, Andrew Blain4, Kate Brand5, Mark Brodwin1, Michael J. I. Brown6, Richard Cool7, Vandana Desai4, Arjun Dey8, Peter Eisenhardt1, Anthony Gonzalez9, Buell T. Jannuzi8, Karin Menendez-Delmestre4, Howard A. Smith3, B. T. Soifer4,10, Glenn P. Tiede11 & E. Wright12 ABSTRACT We discuss color selection of rare objects in a wide-field, multiband survey span- ning from the optical to the mid-infrared. Simple color criteria simultaneously identify and distinguish two of the most sought after astrophysical sources: the coolest brown dwarfs and the most distant quasars. We present spectroscopically-confirmed examples of each class identified in the IRAC Shallow Survey of the Bo¨otes field of the NOAO Deep Wide-Field Survey. ISS J142950.9+333012 is a T4.5 brown dwarf at a distance of approximately 42 pc, and ISS J142738.5+331242 is a radio-loud quasar at redshift z = 6.12. Our selection criteria identify a total of four candidates over 8 square degrees of the Bo¨otes field. The other two candidates are both confirmed 5.5 <z< 6 quasars, previously reported by Cool et al. (2006). We discuss the implications of these dis- coveries and conclude that there are excellent prospects for extending such searches to cooler brown dwarfs and higher redshift quasars. 1Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Dr., Mail Stop 169-506, Pasadena, CA 91109 [e-mail: [email protected]] -
National Science Foundation
This document has been archived. National Science Foundation U.S. Antarctic Program 1999-2000 National Science Foundation U.S. Antarctic Program 1999-2000 i CONTENTS U.S. Antarctic Program, 1999-2000 . .ii Aeronomy and Astrophysics . 1 Biology and Medicine . 12 Antarctic Pack Ice Seals . 25 Long-term ecological research . 28 Environmental Monitoring Program . 31 Geology and Geophysics . 32 Cape Roberts International Drilling Project . 47 Glaciology . 51 Siple Dome Ice Coring . 55 International Trans-Antarctic Scientific Expedition . 57 Ocean and Climate Systems . 60 ii During the 1999-2000 austral summer and the Station by a team of scientists from the PROGRAM,U.S. ANTARCTIC 1999-2000 2000 austral winter, the U.S. Antarctic Program United States, New Zealand, Italy, Australia, will support more than 800 researchers and the United Kingdom, and Germany other participants in the U.S. Antarctic Program • long-term ecological research in the at three year-round stations (McMurdo, McMurdo Dry Valleys and in the Palmer Amundsen-Scott South Pole, and Palmer), Station region of the Antarctic Peninsula aboard two research ships (Laurence M. Gould and Nathaniel B. Palmer) in the Ross Sea and in Science teams also will use networks of the Antarctic Peninsula region, at remote field automatic weather stations, automated geo- camps, and in cooperation with the national physical observatories, ultraviolet-radiation antarctic programs of the other Antarctic Treaty monitors, and a high-altitude, long-duration nations. These projects, funded and managed balloon that will circumnavigate the continent by the National Science Foundation (NSF), are and carry instruments for an optical investiga- part of the international effort to understand tion of solar activity. -
Cosmology from Antarctica Antony A
Cosmology from Antarctica Antony A. Stark ABSTRACT. We are in a golden age of observational cosmology, where measurements of the universe have progressed from crude estimates to precise knowledge. Many of these observations are made from the Antarctic, where conditions are particularly favorable. When we use telescopes to look out at the distant universe, we are also looking back in time because the speed of light is finite. Looking out 13.7 billion years, the cosmic micro- wave background (CMB) comes from a time shortly after the big bang. The first attempt at CMB observations from the Antarctic plateau was an expedition to the South Pole in December 1986 by the Radio Physics Research group at Bell Laboratories. The measured sky noise and opacity were highly encouraging. In the austral summer of 1988–1989, three CMB groups participated in the “Cucumber” campaign, where a temporary summer- only site dedicated to CMB anisotropy measurements was set up 2 km from South Pole Sta- tion. Winter observations became possible with the establishment in 1990 of the Center for Astrophysical Research in Antarctica (CARA), a U.S. National Science Foundation Science and Technology Center, which developed year- round observing facilities in the “Dark Sector,” a section of Amundsen- Scott South Pole Station dedicated to astronomical observations. Scientists at CARA fielded several astronomical instruments: Antarctic Sub- millimeter Telescope and Remote Observatory (AST/RO), South Pole Infrared Explorer (SPIREX), White Dish, Python, Viper, Arcminute Cosmology Bolometer Array Receiver (ACBAR), and Degree- Angular Scale Interferometer (DASI). By 2001, data from CARA, together with Balloon Observations of Millimetric Extragalactic Radiation and Geophys- ics (BOOMERANG), a CMB experiment on a long- duration balloon launched from Mc- Murdo Station on the coast of Antarctica, showed clear evidence that the overall geometry of the universe is flat, as opposed to being open or closed. -
A Bit of History Satellites Balloons Ground-Based
Experimental Landscape ● A Bit of History ● Satellites ● Balloons ● Ground-Based Ground-Based Experiments There have been many: ABS, ACBAR, ACME, ACT, AMI, AMiBA, APEX, ATCA, BEAST, BICEP[2|3]/Keck, BIMA, CAPMAP, CAT, CBI, CLASS, COBRA, COSMOSOMAS, DASI, MAT, MUSTANG, OVRO, Penzias & Wilson, etc., PIQUE, Polatron, Polarbear, Python, QUaD, QUBIC, QUIET, QUIJOTE, Saskatoon, SP94, SPT, SuZIE, SZA, Tenerife, VSA, White Dish & more! QUAD 2017-11-17 Ganga/Experimental Landscape 2/33 Balloons There have been a number: 19 GHz Survey, Archeops, ARGO, ARCADE, BOOMERanG, EBEX, FIRS, MAX, MAXIMA, MSAM, PIPER, QMAP, Spider, TopHat, & more! BOOMERANG 2017-11-17 Ganga/Experimental Landscape 3/33 Satellites There have been 4 (or 5?): Relikt, COBE, WMAP, Planck (+IRTS!) Planck 2017-11-17 Ganga/Experimental Landscape 4/33 Rockets & Airplanes For example, COBRA, Berkeley-Nagoya Excess, U2 Anisotropy Measurements & others... It’s difficult to get integration time on these platforms, so while they are still used in the infrared, they are no longer often used for the http://aether.lbl.gov/www/projects/U2/ CMB. 2017-11-17 Ganga/Experimental Landscape 5/33 (from R. Stompor) Radek Stompor http://litebird.jp/eng/ 2017-11-17 Ganga/Experimental Landscape 6/33 Other Satellite Possibilities ● US “CMB Probe” ● CORE-like – Studying two possibilities – Discussions ongoing ● Imager with India/ISRO & others ● Spectrophotometer – Could include imager – Inputs being prepared for AND low-angular- the Decadal Process resolution spectrophotometer? https://zzz.physics.umn.edu/ipsig/ -
Imagine the Universe News - 1 March 2001 3/7/01 6:40 PM
Imagine the Universe News - 1 March 2001 3/7/01 6:40 PM ˚enter search text ____________________________________________________________________________________________ Imaginemagine the Universe News Thee Latest on the Structure and Evolution of Our Universe For More ____________________________________________________________________________________________ Information... Vol 5. No. 4 1 March 2001 Classyassy Antarctic Balloon Learn more Capturesr es the Earliest Light of about the Universe electromagnetic radiation. McMurdo Station,n, Antarctica -- If you think penguins in Antarctica look classy in their tuxedos, you shoulduld see our scientific balloon wearing a top hat. Read questions and answers about cosmology. Visit the TopHat, an innovativevative hat-shaped TopHat site! astronomy experimentriment that sits on top of a balloon, circled around the frozen continent Antarctic at 120,000 feet foror nearly two weeks in Experiments for Beginning January, collectingng light from the cosmic Scientists microwave backgroundgroundradiation . The flight was a success, and TopHat scientists are noww back in the relative warmth of the Unitednited States, beginning the News Archive yearlong processs of analyzing the data. Observing the microwaveicrowave background, formed about 300,0000,000 years after the big bang, enables scientistsientists to understand the nature of our Universeiverse when it was an infant. The radiationtion comes from an era before the creationon of stars andgalaxies . The Universe is now about 10 to 15 billion TopHat Launch years old. Click for larger image. "It is remarkable that we can determine so much with such data," said Stephan Meyer, a TopHat scientist at the University of Chicago. "For instance, we can measure the mass of the Universe to about 10 percent accuracy. The data will also help to establish whether the Universe will expand forever, or eventually collapse upon itself." TopHat measures the clumpiness of matter when the Universe was very young.