Suman Majumdar
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Large-Scale Structure Under Λ-CDM Paradigm
Large-Scale Structure under Λ-CDM Paradigm Timothy Faerber Astrophysical Tests of Physical Theories - May 2020 1 Introduction We live in a universe dominated by matter and energy. On the smallest scale, all matter and energy is composed of \elementary particles", as predicted by the standard model of particle physics, seen in Figure 1. Figure 1: The Standard Model of Particle Physics All of these particles interact or are influenced via one of the four funda- mental forces of nature: the electromagnetic force (responsible for every- day forces, i.e. friction and tension), the nuclear weak force (responsible 1 for beta decay), the nuclear strong force (responsible for binding of neu- trons and electrons to form more atoms), and the gravitational force (responsible for the gravitational attraction between two massive bod- ies) [4]. In this paper we will focus on the gravitational force and the effect that it has on carving out the Large-Scale Structure (LSS) that we see when observing our universe on the scale of superclusters of galaxies (≈ 110 − 130h−1Mpc) [5]. The LSS in our universe is composed of many gravitationally-bound smaller-scale structures such as groups of galax- ies (less than ≈ 30 − 50 giant galaxies, individual galaxies, gas clouds, stars and planets. On scales the size of superclusters, gravity dominates the other three fundamental forces, however without them, small-scale structures could not exist to form the LSS observed. Responsible for holding together every atom in the universe, and thus making it possi- ble for matter to exist as we know it, is the electromagnetic force. -
I–Visibility Correlation Somnath Bharadwaj & Shiv K. Sethi
J. Astrophys. Astr. (2001) 22, 293–307 HI Fluctuations at Large Redshifts: I–Visibility correlation Somnath Bharadwaj1 & Shiv K. Sethi2∗ 1Department of Physics and Meteorology & Center for Theoretical Studies, I.I.T. Kharagpur, 721 302, India email: [email protected] 2Raman Research Institute, C. V. Raman Avenue, Sadashivnagar, Bangalore 560 080, India email: [email protected] Received 2002 March 15; accepted 2002 May 31 Abstract. We investigate the possibility of probing the large scale structure in the universe at large redshifts by studying fluctuations in the redshifted 1420 MHz emission from the neutral hydrogen (HI) at early epochs. The neutral hydrogen content of the universe is known from absorp- < tion studies for z ∼ 4.5. The HI distribution is expected to be inhomoge- neous in the gravitational instability picture and this inhomogeneity leads to anisotropy in the redshifted HI emission. The best hope of detecting this anisotropy is by using a large low-frequency interferometric instru- ment like the Giant Meter-Wave Radio Telescope (GMRT). We calculate the visibility correlation function hVν(U)Vν0 (U)i at two frequencies ν and ν0 of the redshifted HI emission for an interferometric observation. In par- ticular we give numerical results for the two GMRT channels centered around ν = 325 MHz and ν = 610 MHz from density inhomogeneity and peculiar velocity of the HI distribution. The visibility correlation is ' 10−10–10−9 Jy2. We calculate the signal-to-noise for detecting the cor- relation signal in the presence of system noise and show that the GMRT might detect the signal for integration times ' 100 hrs. -
Prospects for Detecting the 326.5 Mhz Redshifted 21-Cm HI Signal with the Ooty Radio Telescope (ORT)
J. Astrophys. Astr. (2014) 35, 157–182 c Indian Academy of Sciences Prospects for Detecting the 326.5 MHz Redshifted 21-cm HI Signal with the Ooty Radio Telescope (ORT) Sk. Saiyad Ali1,∗ & Somnath Bharadwaj2 1Department of Physics, Jadavpur University, Kolkata 700 032, India. 2Department of Physics and Meteorology & Centre for Theoretical Studies, IIT Kharagpur, Kharagpur 721 302, India. ∗e-mail: [email protected] Received 7 October 2013; accepted 13 February 2014 Abstract. Observations of the redshifted 21-cm HI fluctuations promise to be an important probe of the post-reionization era (z ≤ 6). In this paper we calculate the expected signal and foregrounds for the upgraded Ooty Radio Telescope (ORT) which operates at frequency νo = 326.5MHz which corresponds to redshift z = 3.35. Assuming that the visibilities contain only the HI signal and system noise, we show that a 3σ detec- tion of the HI signal (∼ 1 mK) is possible at angular scales 11 to 3◦ with ≈1000 h of observation. Foreground removal is one of the major chal- lenges for a statistical detection of the redshifted 21 cm HI signal. We assess the contribution of different foregrounds and find that the 326.5 MHz sky is dominated by the extragalactic point sources at the angular scales of our interest. The expected total foregrounds are 104−105 times higher than the HI signal. Key words. Cosmology: large scale structure of Universe—intergalactic medium—diffuse radiation. 1. Introduction The study of the evolution of cosmic structure has been an important subject in cos- mology. In the post reionization era (z < 6) the 21-cm emission originates from dense pockets of self-shielded hydrogen. -
Small-Scale Secondary Anisotropics in the Cosmic Microwave Background
Small-Scale Secondary Anisotropics in the Cosmic Microwave Background by Jonathan Dudley M.Sc. Department of Physics McGill University Montreal, Quebec August 2007 A thesis submitted to McGill University in partial fulfilment of the requirements of the degree of Master of Science in Physics © Jonathan Dudley (2007) Library and Bibliotheque et 1*1 Archives Canada Archives Canada Published Heritage Direction du Branch Patrimoine de I'edition 395 Wellington Street 395, rue Wellington Ottawa ON K1A0N4 Ottawa ON K1A0N4 Canada Canada Your file Votre reference ISBN: 978-0-494-51263-0 Our file Notre reference ISBN: 978-0-494-51263-0 NOTICE: AVIS: The author has granted a non L'auteur a accorde une licence non exclusive exclusive license allowing Library permettant a la Bibliotheque et Archives and Archives Canada to reproduce, Canada de reproduire, publier, archiver, publish, archive, preserve, conserve, sauvegarder, conserver, transmettre au public communicate to the public by par telecommunication ou par Plntemet, prefer, telecommunication or on the Internet, distribuer et vendre des theses partout dans loan, distribute and sell theses le monde, a des fins commerciales ou autres, worldwide, for commercial or non sur support microforme, papier, electronique commercial purposes, in microform, et/ou autres formats. paper, electronic and/or any other formats. The author retains copyright L'auteur conserve la propriete du droit d'auteur ownership and moral rights in et des droits moraux qui protege cette these. this thesis. Neither the thesis Ni la these ni des extraits substantiels de nor substantial extracts from it celle-ci ne doivent etre imprimes ou autrement may be printed or otherwise reproduits sans son autorisation. -
Effects of the Sources of Reionization on 21Cm Redshiftspace Distortions
Effects of the sources of reionization on 21-cm redshift-space distortions Article (Published Version) Majumdar, Suman, Jensen, Hannes, Mellema, Garrelt, Chapman, Emma, Abdalla, Filipe B, Lee, Kai-Yan, Iliev, Ilian T, Dixon, Keri L, Datta, Kanan K, Ciardi, Benedetta, Fernandez, Elizabeth R, Jelić, Vibor, Koopmans, Léon V E and Zaroubi, Saleem (2015) Effects of the sources of reionization on 21-cm redshift-space distortions. Monthly Notices of the Royal Astronomical Society, 456 (2). pp. 2080-2094. ISSN 0035-8711 This version is available from Sussex Research Online: http://sro.sussex.ac.uk/id/eprint/69098/ This document is made available in accordance with publisher policies and may differ from the published version or from the version of record. If you wish to cite this item you are advised to consult the publisher’s version. Please see the URL above for details on accessing the published version. Copyright and reuse: Sussex Research Online is a digital repository of the research output of the University. Copyright and all moral rights to the version of the paper presented here belong to the individual author(s) and/or other copyright owners. To the extent reasonable and practicable, the material made available in SRO has been checked for eligibility before being made available. Copies of full text items generally can be reproduced, displayed or performed and given to third parties in any format or medium for personal research or study, educational, or not-for-profit purposes without prior permission or charge, provided that the authors, title and full bibliographic details are credited, a hyperlink and/or URL is given for the original metadata page and the content is not changed in any way. -
Jonathan R. Pritchard Reader in Astrostatistics
Jonathan R. Pritchard Reader in Astrostatistics Contact Imperial College Office: +44 (0)207 594 7557 Information Astrophysics Group Fax: +44 (0)207 594 7772 Blackett Laboratory Cell: +44 (0)751 841 8007 Prince Consort Road E-mail: [email protected] London WWW: http://pritchardjr.github.io SW7 2AZ UK ORCID: http://orcid.org/0000-0003-4127-5353 Biographical Date of Birth: 26 January 1980 Citizenship: British Information Research Theoretical cosmology, reionization, cosmological 21 cm line, large scale structure, cosmic microwave Interests background, inflation, dark energy, neutrino mass Research Imperial College, London, UK Experience Reader in Astrostatistics September, 2018 - present Senior Lecturer in Astrostatistics September, 2015 - August 2018 Lecturer in Astrostatistics October, 2011 - August, 2015 Research in cosmology, the epoch of reionization, and astrostatistics. Teaching of undergraduate physics. Supervision of MSc and PhD projects. Mentoring of postdoctoral researchers. Harvard-Smithsonian Center for Astrophysics, Cambridge, Massachusetts, USA ITC Fellow September, 2010 - August, 2011 Hubble Fellow September, 2007 - August, 2010 Post-doctoral research in cosmology, the epoch of reionization, and the theory of the 21 cm line. California Institute of Technology, Pasadena, California, USA Graduate Student September, 2002 - June, 2007 Ph.D. research in cosmology, CMB B-modes, and the early Universe. Cambridge University, Cambridge, UK Part III Research project December, 2001 - August, 2002 Master's level research into bound fermionic states around black holes, using a gauge theory of gravity. Advisor: Anthony Lasenby. California Institute of Technology, Pasadena, California, USA Summer Undergraduate Research Fellowship July, 2001 - September, 2001 Undergraduate level research into quintessence models for dark energy. Advisor: Marc Kamionkowski. -
Large Scale Structure
PRAMANA c Indian Academy of Sciences Vol. 53, No. 6 — journal of December 1999 physics pp. 977–987 Large scale structure SOMNATH BHARADWAJ Department of Physics and Meteorology and Centre for Theoretical Studies, Indian Institute of Technology, Kharagpur 721 302, India Email: [email protected] Abstract. We briefly discuss some aspects of the problem of forming large scale structures in the Universe. The basic picture that initially small perturbations generated by inflation grow by the process of gravitational instability to give the observed structures is largely consistent with the observations. The growth of the perturbations depends crucially on the contents of the Universe, and we discuss a few variants of the cold dark matter model. Many of these models are consistent with present observations. Future observations hold the possibility of deciding amongst these models. Keywords. Cosmology; theory; large scale structure. PACS Nos 98.65.Dx 1. Introduction Our present understanding of the Universe is based on two important assumptions 1. the Universe is homogeneous and isotropic on large scales 2. gravitation governs the dynamics of the Universe on large scales. The time-evolution of such a Universe can be described by just one function of time – the ´Øµ scale factor a which tells us about the expansion or contraction of the Universe (these ´Øµ being the only two possibilities which preserve assumption (1). The evolution of a is governed by the laws of gravitation eq. (4), and the observation that all the distant galax- ies are moving away from us leads us to the conclusion that the Universe is expanding [1]. -
Advancing Precision Cosmology with 21 Cm Intensity Mapping by Kiyoshi
Advancing precision cosmology with 21 cm intensity mapping by Kiyoshi Wesley Masui A thesis submitted in conformity with the requirements for the degree of Doctor of Philosophy Graduate Department of Physics University of Toronto c Copyright 2013 by Kiyoshi Wesley Masui Abstract Advancing precision cosmology with 21 cm intensity mapping Kiyoshi Wesley Masui Doctor of Philosophy Graduate Department of Physics University of Toronto 2013 In this thesis we make progress toward establishing the observational method of 21 cm intensity mapping as a sensitive and efficient method for mapping the large-scale struc- ture of the Universe. In Part I we undertake theoretical studies to better understand the potential of intensity mapping. This includes forecasting the ability of intensity mapping experiments to constrain alternative explanations to dark energy for the Universe's accel- erated expansion. We also consider how 21 cm observations of the neutral gas in the early Universe (after recombination but before reionization) could be used to detect primordial gravity waves, thus providing a window into cosmological inflation. Finally we show that scientifically interesting measurements could in principle be performed using intensity mapping in the near term, using existing telescopes in pilot surveys or prototypes for larger dedicated surveys. Part II describes observational efforts to perform some of the first measurements using 21 cm intensity mapping. We develop a general data analysis pipeline for analyzing intensity mapping data from single dish radio telescopes. We then apply the pipeline to observations using the Green Bank Telescope. By cross-correlating the intensity mapping survey with a traditional galaxy redshift survey we put a lower bound on the amplitude of the 21 cm signal. -
Dr Emma Chapman
Dr Emma Chapman – Curriculum Vitae Work Address: Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, United Kingdom E-Mail: [email protected] Website: https://dremmachapman.wordpress.com Research Interests: Foreground mitigation; Epoch of reionisation; Cosmology; Radio interferometry and data reduction; Signal processing Career Summary Royal Society Dorothy Hodgkin Fellowship Imperial College London Oct 2018 – Present My fellowship is centred around research into the Epoch of Reionisation (EoR), contributing to its detection through membership of the LOFAR core EoR team and leading a focus group on foreground removal within the SKA working group. I supervise one PhD student, Iandeep Hothi. Royal Astronomical Society Research Fellowship Imperial College London Oct 2015 – Oct 2018 Postdoctoral Researcher University College London Dec 2013 – Oct 2015 SKA-funded postdoctoral research position, continuing personal research and contributing to the organization of the SKA EoR pipeline within the SKA SDP consortium. PhD University College London Oct 2010 – Dec 2013 Thesis title: Seeing the Light: Foreground Removal in the Dark and Dim Ages, supervised by Dr Filipe Abdalla. MPhys Durham University Oct 2006 – July 2010 Integrated masters in Theoretical Physics awarded as a First. Overall Firsts achieved in every year and every module with an overall degree percentage of 81%. Research Prizes and Major Grants 2018 Royal Society Research Enhancement Award, £97,000 2018 Royal Society Dorothy -
Chapter 6 Foregrounds and Their Mitigation
Chapter 6 Foregrounds and their mitigation1 Emma Chapman (Imperial College London) Vibor Jelic´ (Ruder Boskoviˇ c´ Institute) Abstract The low-frequency radio sky is dominated by the diffuse synchrotron emis- sion of our Galaxy and extragalactic radio sources related to Active Galactic Nuclei and star-forming galaxies. This foreground emission is much brighter than the cosmological 21 cm emission from the Cosmic Dawn and Epoch of Reionization. Studying the physical properties of the foregrounds is therefore of fundamental importance for their mitigation in the cosmological 21 cm ex- periments. This chapter gives a comprehensive overview of the foregrounds and our current state-of-the-art knowledge about their mitigation. 6.1 What are the foregrounds? A detection of the redshifted 21 cm emission from the Cosmic Dawn (CD) and Epoch of Reionization (EoR) is a daunting task due to a number of chal- lenges, which are different in nature and complexity. One of them is the extremely prominent foreground emission, which dominates the sky at low arXiv:1909.12369v1 [astro-ph.CO] 26 Sep 2019 radio frequencies. This emission intervenes like fog on an autumn morning and obscures our view towards the neutral hydrogen regions from the times of the first “stars” in the Universe. To clear the view and to make the detec- tion possible, we need to study the foreground emission in great detail and 1To appear as a book chapter in “The Cosmic 21-cm Revolution: Charting the first billion years of our Universe”, Ed. Andrei Mesinger (Bristol: IOP Publishing Ltd.) AAS-IOP ebooks (http://www.iopscience.org/books/aas). -
Epoch of Reionization/Cosmic Dawn Science With
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The Stabilizing Effect of Spacetime Expansion on Relativistic Fluids with Sharp Results for the Radiation Equation of State
THE STABILIZING EFFECT OF SPACETIME EXPANSION ON RELATIVISTIC FLUIDS WITH SHARP RESULTS FOR THE RADIATION EQUATION OF STATE JARED SPECK∗ Abstract. In this article, we study the 1 + 3 dimensional relativistic Euler equations on a pre-specified conformally flat expanding spacetime background with spatial slices that are diffeomorphic to R3. We assume that the fluid ver- 2 ifies the equation of state p = csρ, where 0 ≤ cs ≤ p1/3 is the speed of sound. We also assume that the inverse of the scale factor associated to the expanding spacetime metric verifies a cs−dependent time-integrability condi- tion. Under these assumptions, we use the vectorfield energy method to prove that an explicit family of physically motivated, spatially homogeneous, and spatially isotropic fluid solutions is globally future-stable under small pertur- bations of their initial conditions. The explicit solutions corresponding to each scale factor are analogs of the well-known spatially flat Friedmann-Lemaˆıtre- Robertson-Walker family. Our nonlinear analysis, which exploits dissipative terms generated by the expansion, shows that the perturbed solutions exist for all future times and remain close to the explicit solutions. This work is an extension of previous results, which showed that an analogous stability result holds when the spacetime is exponentially expanding. In the case of the radi- ation equation of state p = (1/3)ρ, we also show that if the time-integrability condition for the inverse of the scale factor fails to hold, then the explicit fluid solutions are unstable. More precisely, we show that arbitrarily small smooth perturbations of the explicit solutions’ initial conditions can launch perturbed solutions that form shocks in finite time.