DOCSLIB.ORG

Synergies Between 21Cm & Optical Surveys for Probing Large Scale Cosmic Structure

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Synergies Between 21Cm & Optical Surveys for Probing Large Scale Cosmic Structure Synergies Between 21cm & Optical Surveys for Probing Large Scale Cosmic Structure PhD Thesis By Steven D. CUNNINGTON Institute of Cosmology & Gravitation UNIVERSITY OF PORTSMOUTH The thesis is submitted in partial fulfilment of the requirements for the award of the degree of Doctor of Cosmology of the University of Portsmouth. Submission: SEPTEMBER 2019 Supervisors: Prof. David Bacon Dr. Alkistis Pourtsidou ABSTRACT e are currently living through an era of precision cosmology where we have gathered a substantial amount of data with the aim of understanding our Universe. However, W our current understanding is far from complete as our most successful cosmological model relies on the Universe’s energy-matter content being vastly dominated by components that are not yet detected and not currently compatible with our wider general model of physics. This leaves plenty more investigation to be done and new techniques for probing our Universe are highly sought after. Mapping unresolved neutral hydrogen within galaxies is one of these novel techniques and has been gaining momentum over the last decade. By using the 21cm signal from neutral hydrogen, which traces the underlying large scale cosmic structure, we can map and statistically analyse 3D density distributions and compare these to theoretical models. I provide a detailed introduction to this novel HI intensity mapping technique in Chapter2. This thesis also explores what gains can be made by combining HI intensity mapping data with more conventional optical galaxy redshift surveys. There are many reasons why a cross- correlation such as this will be beneficial. While the intensity mapping technique is developed and refined, optical data can boost the inherently weak HI signal allowing detection and a deeper understanding of the intensity mapping process. Also in the future, when we have dedicated intensity mapping instruments gathering data, cross-correlations will see reductions in the different systematics which could otherwise dominate the uncertainty in any auto-correlations. With the use of computer simulations, I look to forecast benefits to be gained from this synergy and in Chapter3 I provide an example of how H I intensity maps can be used to constrain photometric redshifts on optical imaging surveys. The largest problem preventing the success of HI intensity mapping comes from 21cm fore- grounds whose signals dominate by several orders of magnitude over the weak HI cosmological signal. While we have several methods for cleaning these foregrounds, understanding the impact these reconstructions have on the data is crucial and is the key theme in Chapters4 and5. Again using computer simulations of cosmological HI intensity mapping signals and their foreground contamination, I show how foregrounds can be removed and with some additional treatment, successfully used in cross-correlation with an optical photometric galaxy survey. This indicates a promising future for cosmology and suggests the next-generation of optical telescopes such as LSST and Euclid, should benefit hugely from synergies with intensity mapping data provided by a next-generation radio telescope such as the SKA. ii DEDICATION &ACKNOWLEDGEMENTS “Like a cow that every day in 10 years sees the train cross in front at the same time. If you ask the cow, ‘what time is the train going to come’, it is not going to know the right answer." — Mauricio Pochettino would like to begin by thanking my brilliant supervisors, David and Alkistis, both of whom I am in an infinite state of debt to. During my PhD I have seen both of them receive promo- Itions and they are thoroughly deserving of this success. I have been truly fortunate to have two academics with a seemingly endless supply of knowledge and patience and a large part of my development is owed to them. I would also like to thank all of my (past and present) collaborators Ian Harrison, Laura Wolz, Chris Blake and Julian Bautista, each of whom it has been a pleasure to work with and learn from. Furthermore, I thank the many talented colleagues and acquaintances within the cosmology community who have helped with useful discussions and advice such as David Alonso, Phil Bull, Stefano Camera, Emma Chapman, Benjamin Joachimi, Mario Santos, Anna Zoldan, and no doubt many more. Throughout my PhD I have been fortunate enough to be offered the chance to speak at a number of local astronomical societies or science groups. The enthusiasm I find at every one of these volunteer-run groups is astounding and I am grateful for the excellent engagement I receive when I discuss my research with these groups. Some of the most challenging questions I have received after providing a talk have come from these sessions and they have motivated me to broaden my knowledge as far as possible. Were it not for my regular opportunities to play football, I feel this PhD would have tested my sanity far more. So therefore I am grateful for all those around the University of Portsmouth I have played with. In particular I would like to thank our 5-a-side team ICG Intergalácticos, whose rapid progression in the University Staff League I hope will continue. Also, a thank you to all those involved in our series of 11-a-side matches against the Physics undergraduate students, especially since the staff are still leading the series 3-1! I am grateful to my parents and a wide supporting family who provide the foundations to my life. I would like to end by thanking the most important person in my life. You have been with me since the start of my higher education in Physics and your love and companionship has helped more than you will ever realise or I’ll ever be able to express. My partner Justine, I dedicate this to you. ——————————————————————————————————————————— My work is supported by the University of Portsmouth. Numerical computations for this thesis were done on the Sciama High Performance Compute (HPC) cluster which is supported by the ICG, SEPNet, and the University of Portsmouth. iii TABLEOF CONTENTS Page Author’s Declaration vii Dissemination vii Preface viii 1 Introduction 1 1.1 The Space-Time Metric.................................. 3 1.2 Cosmological Observables & Parameters ........................ 4 1.2.1 Redshift ....................................... 4 1.2.2 Distances ..................................... 5 1.2.3 Hubble Parameter ................................. 7 1.3 Friedmann Cosmological Models............................ 8 1.3.1 Friedmann Equations.............................. 8 1.3.2 Equation of State................................. 9 1.3.3 Late-Time Acceleration & Dark Energy.................... 9 1.4 ¤CDM............................................ 10 1.4.1 The Cosmological Constant (¤) .........................11 1.4.2 Cold Dark Matter (CDM) ............................ 13 1.5 Large-Scale Cosmic Structure...............................14 1.5.1 Two-Point Correlation Function & Power Spectrum ............ 15 1.5.2 Structure Growth................................. 15 1.5.3 Redshift Space Distortions ........................... 18 1.6 Summary...........................................21 2 HI (21cm) Intensity Mapping 23 2.1 Cosmic History of Hydrogen............................... 23 2.1.1 The Early Universe.................................24 2.1.2 Dark Ages & the Epoch of Reionization.....................24 2.1.3 HI in the Post-Reionization Universe..................... 25 2.2 Mapping Unresolved 21cm Emission.......................... 25 2.2.1 Intensity Response for Radio Telescopes................... 26 2.2.2 Interferometer or Single-Dish ......................... 28 iv TABLE OF CONTENTS 2.2.3 Telescope Systematics.............................. 29 2.2.4 Cross-Correlation with Optical Surveys.................... 30 2.3 HI Cosmological Formalism............................... 32 2.3.1 Characterising the 21cm Signal ........................ 33 2.3.2 Power Spectrum ................................. 36 2.3.3 HI Halo Model .................................. 38 2.4 Simulating 21cm Cosmology............................... 39 2.4.1 Building Structure ................................ 39 2.4.2 Assigning HI ................................... 40 2.4.3 Mocks for HI-Galaxy Cross-Correlations....................41 2.5 Summary.......................................... 43 3 Clustering-Based Redshift Estimation with HI Intensity Maps 45 3.1 Introduction ........................................ 45 3.2 Simulations..........................................47 3.2.1 Simulating HI Intensity Maps ......................... 48 3.2.2 Optical Galaxy Sample.............................. 53 3.3 Estimator Formalism....................................54 3.3.1 Bias Treatment ...................................57 3.4 Results & Discussion ................................... 58 3.4.1 Bright HI-Rich Sources ............................. 59 3.4.2 Foreground Removal............................... 60 3.4.3 Varying Beam Size................................ 63 3.4.4 Improvement on Photometric Redshift Measurements ...........67 3.5 Summary.......................................... 69 4 Foreground Contamination in HI Intensity Maps 73 4.1 Introduction .........................................74 4.2 Cosmological Signals & Their Simulation ....................... 75 4.2.1 HI Intensity Map Simulation.......................... 79 4.2.2 Optical Galaxy Catalogue Simulation..................... 82 4.3 21cm Foregrounds & Their Simulation..........................84 4.3.1 Galactic Synchrotron ...............................84 4.3.2
Load more

Recommended publications
  • Estimating the Redshift Distribution of Photometric Galaxy Samples
    Mon. Not. R. Astron. Soc. 390, 118–130 (2008) doi:10.1111/j.1365-2966.2008.13510.x Estimating the redshift distribution of photometric galaxy samples Marcos Lima,1,2 Carlos E. Cunha,2,3 Hiroaki Oyaizu,2,3 Joshua Frieman,2,3,4 Huan Lin4 and Erin S. Sheldon5 1Department of Physics, University of Chicago, Chicago, IL 60637, USA 2Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637, USA 3Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA 4Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510, USA 5Center for Cosmology and Particle Physics and Department of Physics, New York University, New York, NY 10003, USA Accepted 2008 May 29. Received 2008 May 20; in original form 2008 January 24 ABSTRACT We present an empirical method for estimating the underlying redshift distribution N(z)of galaxy photometric samples from photometric observables. The method does not rely on photometric redshift (photo-z) estimates for individual galaxies, which typically suffer from biases. Instead, it assigns weights to galaxies in a spectroscopic subsample such that the weighted distributions of photometric observables (e.g. multiband magnitudes) match the corresponding distributions for the photometric sample. The weights are estimated using a nearest neighbour technique that ensures stability in sparsely populated regions of colour– magnitude space. The derived weights are then summed in redshift bins to create the redshift distribution. We apply this weighting technique to data from the Sloan Digital Sky Survey as well as to mock catalogues for the Dark Energy Survey, and compare the results to those from the estimation of photo-zs derived by a neural network algorithm.
    [Show full text]
  • Probing Star Formation and Radio Activity Using Faint Galaxy Redshift Surveys
    Durham E-Theses Probing star formation and radio activity using faint galaxy redshift surveys Davies, Gregory Tudor How to cite: Davies, Gregory Tudor (2008) Probing star formation and radio activity using faint galaxy redshift surveys, Durham theses, Durham University. Available at Durham E-Theses Online: http://etheses.dur.ac.uk/2224/ Use policy The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that: • a full bibliographic reference is made to the original source • a link is made to the metadata record in Durham E-Theses • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders. Please consult the full Durham E-Theses policy for further details. Academic Support Oce, Durham University, University Oce, Old Elvet, Durham DH1 3HP e-mail: [email protected] Tel: +44 0191 334 6107 http://etheses.dur.ac.uk Probing Star Formation and Radio Activity using Faint Galaxy Redshift Survey by Gregory Tudor Davies A thesis submitted to the University of Durham in accordance with the regulations for admittance to the Degree of Doctor of Philosophy. Department of Physics University of Durham October 2008 The copyright of this thesis rests with the author or the university to which it was submitted. No quotation from it, or information derived from it may be published without the prior written consent of the author or university, and any information derived from it should be acknowledged.
    [Show full text]
  • Hydrogen 21-Cm Intensity Mapping at Redshift
    Hydrogen 21-cm Intensity Mapping at redshift 0.8 Tzu-Ching Chang1,2, Ue-Li Pen2, Kevin Bandura3, & Jeffrey B. Peterson3 1IAA, Academia Sinica, P.O. Box 23-141, Taipei 10617, Taiwan 2CITA, University of Toronto, 60 St.George St., Toronto, ON, M5S 3H8, Canada 3Department of Physics, Carnegie Mellon University, 5000 Forbes Ave, Pittsburgh, PA 15213, USA Observations of 21-cm radio emission by neutral hydrogen at redshifts z ∼ 0.5 to ∼ 2.5 are expected to provide a sensitive probe of cosmic dark energy 1 2. This is particularly true around the onset of acceleration at z ∼ 1, where traditional optical cosmology becomes very difficult because of the infrared opacity of the atmosphere. Hitherto, 21-cm emission has been detected only to z=0.24 3. More distant galaxies generally are too faint for individual detections but it is possible to measure the aggregate emission from many unresolved galaxies in the ’cosmic web’. Here we report a three dimensional 21-cm intensity field at z=0.53 to 1.12. We then co-add HI emission from the volumes surrounding about ten thousand galaxies arXiv:1007.3709v1 [astro-ph.CO] 21 Jul 2010 (from the DEEP2 optical galaxy redshift survey 4). We detect the aggregate 21-cm glow at a significance of ∼ 4 sigma. The DEEP2 optical redshift survey 4 provides a rich sample for study of the Universe at redshifts near one. The team recorded optical spectra for 50,000 faint galaxies out to redshift z =1.4, utilizing the DEIMOS spectrograph on the Keck II telescope.
    [Show full text]
  • Estimating the Redshift Distribution of Photometric Galaxy Samples II
    Mon. Not. R. Astron. Soc. 000, 000–000 (0000) Printed 19 June 2018 (MN LATEX style file v2.2) Estimating the Redshift Distribution of Photometric Galaxy Samples II. Applications and Tests of a New Method Carlos E. Cunha1,2,3⋆, Marcos Lima2,4,5, Hiroaki Oyaizu1,2, Joshua Frieman1,2,6, Huan Lin6 1Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637 2Kavli Institute for Cosmological Physics, University of Chicago, Chicago, IL 60637 3Department of Physics, University of Michigan, 450 Church St., Ann Arbor, MI 48109 4Department of Physics, University of Chicago, Chicago, IL 60637 5Department of Physics and Astronomy, University of Pennsylvania, Philadelphia, PA 19104 6Center for Particle Astrophysics, Fermi National Accelerator Laboratory, Batavia, IL 60510 19 June 2018 ABSTRACT In Lima et al. (2008) we presented a new method for estimating the redshift distribution, N(z), of a photometric galaxy sample, using photometric observables and weighted sampling from a spectroscopic subsample of the data. In this paper, we extend this method and explore various applications of it, using both simulations of and real data from the SDSS. In addition to estimating the redshift distribution for an entire sample, the weighting method enables accurate estimates of the red- shift probability distribution, p(z), for each galaxy in a photometric sample. Use of p(z) in cosmological analyses can substantially reduce biases associated with tradi- tional photometric redshifts, in which a single redshift estimate is associated with each galaxy. The weighting procedure also naturally indicates which galaxies in the photometric sample are expected to have accurate redshift estimates, namely those that lie in regions of photometric-observable space that are well sampled by the spec- troscopic subsample.
    [Show full text]
  • The Environment on Few Mpc Scales of Infrared Luminous Galaxies At
    The Environment on few Mpc scales of Infrared Luminous Galaxies at Redshifts z∼1. D. Marcillac 1, G. H. Rieke1, C. Papovich1,2, C. N. A. Willmer1, B. J. Weiner1, A. L. Coil 1,3, M. C. Cooper1,2,4 B. F. Gerke4, J. Woo 5, J. A. Newman3,6, A. Georgakakis7, E. S. Laird7, K. Nandra7, G. G. Fazio9, J.-S. Huang9, D. C. Koo8 ABSTRACT We investigate the environment of infrared luminous galaxies (LIR[8-1000 11 µm] > 10 L⊙). We focus on the redshift range 0.7 ≤ z ≤ 1, where these galaxies dominate the star formation activity and play a significant role in galaxy evolu- tion. We employ MIPS 24µm data to identify infrared galaxies in the Extended Groth Strip (EGS). We use a local density indicator to probe the environment on few Mpc scales and a group member catalog, both of which make use of the DEEP2 spectroscopic redshift catalog, to quantify the environment of these galaxies. We find that the local environment of LIRGs and ULIRGs is intermediate between that of blue and red galaxies. LIRGs and ULIRGs avoid underdense environments and inhabit local environments that are more dense on average than those of other DEEP2 galaxies at similar redshifts. However, when the comparison sample of the non-IR DEEP2 galaxies is restricted to have the same range of stellar mass, color, or luminosity as the IR–galaxies, there is no longer 1Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721 2Spitzer Fellow arXiv:0712.0033v1 [astro-ph] 1 Dec 2007 3Hubble Fellow 4Department of Astronomy, University of California, Berkeley, CA 94720 –
    [Show full text]
  • UC Berkeley UC Berkeley Previously Published Works
    View metadata, citation and similar papers at core.ac.uk brought to you by CORE provided by eScholarship - University of California UC Berkeley UC Berkeley Previously Published Works Title Mitigating the impact of the DESI fiber assignment on galaxy clustering Permalink https://escholarship.org/uc/item/80r966fg Journal Journal of Cosmology and Astroparticle Physics, 2017(03) ISSN 1475-7516 Authors Burden, Angela Padmanabhan, Nikhil Cahn, Robert N et al. Publication Date 2017-03-01 DOI 10.1088/1475-7516/2017/03/001 Peer reviewed eScholarship.org Powered by the California Digital Library University of California Prepared for submission to JCAP Mitigating the Impact of the DESI Fiber Assignment on Galaxy Clustering Angela Burdena Nikhil Padmanabhana Robert N. Cahnb Martin J. Whiteb;c;d Lado Samushiae aDept. of Physics, Yale University, New Haven, CT 06511, USA bPhysics Division, Lawrence Berkeley National Laboratory,1 Cyclotron Road, Berkeley, CA 94720, USA cDepartment of Physics, University of California, Berkeley, California dDepartment of Astronomy, University of California, Berkeley, California ePhysics Department, Kansas State University,116 Cardwell Hall,1228 N. 17th St. Manhat- tan, KS 66506 E-mail: [email protected] Abstract. We present a simple strategy to mitigate the impact of an incomplete spectroscopic redshift galaxy sample as a result of fiber assignment and survey tiling. The method has been designed for the Dark Energy Spectroscopic Instrument (DESI) galaxy survey but may have applications beyond this. We propose a modification to the usual correlation function that nulls the almost purely angular modes affected by survey incompleteness due to fiber assignment. Predictions of this modified statistic can be calculated given a model of the two point correlation function.
    [Show full text]
  • Gravitational Lensing of the Supernovae from the Supernova Legacy Survey (SNLS) Ayan Mitra
    Gravitational Lensing of the supernovae from the Supernova Legacy Survey (SNLS) Ayan Mitra To cite this version: Ayan Mitra. Gravitational Lensing of the supernovae from the Supernova Legacy Survey (SNLS). Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]. Sorbonne Universités, UPMC Univ Paris 06, CNRS, LIP6 UMR 7606, 4 place Jussieu 75005 Paris., 2016. English. tel-01797973 HAL Id: tel-01797973 https://tel.archives-ouvertes.fr/tel-01797973 Submitted on 23 May 2018 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. THÈSE DE DOCTORAT DE L’UNIVERSITÉ PIERRE ET MARIE CURIE Spécialité Astrophysique et Cosmologie Particules, Noyaux et Cosmos (ED 517) Présentée par M. Ayan MITRA En vue de l’obtention du grade de DOCTEUR de l’UNIVERSITÉ PIERRE et MARIE CURIE Gravitational lensing of the supernovae from the SuperNova Legacy Survey Date de la soutenance : le 30 septembre 2016 devant le jury composé de : M. Dominique FOUCHEZ Examinateur Mme Delphine HARDIN Directrice de thèse M. Michael JOYCE Examinateur Mme Simona MEI Rapporteur Mme Cécile RENAULT Rapporteur Mme Vanina RUHLMANN-KLEIDER Examinateur ii Contents 1 Cosmology 3 1.1 A homogeneous expanding universe . .3 1.2 The Friedman universe .
    [Show full text]
  • Growth of Cosmic Structure: Probing Dark Energy Beyond Expansion
    BNL-107345-2015-JA Growth of Cosmic Structure: Probing Dark Energy Beyond Expansion Conveners: Dragan Huterer, David Kirkby Rachel Bean, Andrew Connolly, Kyle Dawson, Scott Dodelson, August Evrard, Bhuvnesh Jain, Michael Jarvis, Eric Linder, Rachel Mandelbaum, Morgan May, Alvise Raccanelli, Beth Reid, Eduardo Rozo, Fabian Schmidt, Neelima Sehgal, AnˇzeSlosar, Alex van Engelen, Hao-Yi Wu, Gongbo Zhao 1 Executive Summary The quantity and quality of cosmic structure observations have greatly accelerated in recent years, and further leaps forward will be facilitated by imminent projects. These will enable us to map the evolution of dark and baryonic matter density fluctuations over cosmic history. The way that these fluctuations vary over space and time is sensitive to several pieces of fundamental physics: the primordial perturbations generated by GUT-scale physics; neutrino masses and interactions; the nature of dark matter and dark energy. We focus on the last of these here: the ways that combining probes of growth with those of the cosmic expansion such as distance-redshift relations will pin down the mechanism driving the acceleration of the Universe. One way to explain the acceleration of the Universe is invoke dark energy parameterized by an equation of state w. Distance measurements provide one set of constraints on w, but dark energy also affects how rapidly structure grows; the greater the acceleration, the more suppressed the growth of structure. Upcoming surveys are therefore designed to probe w with direct observations of the distance scale and the growth of structure, each complementing the other on systematic errors and constraints on dark energy. A consistent set of results will greatly increase the reliability of the final answer.
    [Show full text]
  • The DEEP2 Galaxy Redshift Survey: Clustering of Galaxies in Early Data
    The DEEP2 Galaxy Redshift Survey: Clustering of Galaxies in Early Data The Harvard community has made this article openly available. Please share how this access benefits you. Your story matters Citation Coil, Alison L., Marc Davis, Darren S. Madgwick, Jeffrey A. Newman, Christopher J. Conselice, Michael Cooper, Richard S. Ellis, et al. 2004. “The DEEP2 Galaxy Redshift Survey: Clustering of Galaxies in Early Data.” The Astrophysical Journal 609 (2) (July 10): 525–538. doi:10.1086/421337. Published Version doi:10.1086/421337 Citable link http://nrs.harvard.edu/urn-3:HUL.InstRepos:33462899 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, 609:525–538, 2004 July 10 # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE DEEP2 GALAXY REDSHIFT SURVEY: CLUSTERING OF GALAXIES IN EARLY DATA Alison L. Coil,1 Marc Davis,1 Darren S. Madgwick,1 Jeffrey A. Newman,1 Christopher J. Conselice,2 Michael Cooper,1 Richard S. Ellis,2 S. M. Faber,3 Douglas P. Finkbeiner,4 Puragra Guhathakurta,3, 5 Nick Kaiser,6 David C. Koo,3 Andrew C. Phillips,3 Charles C. Steidel,2 Benjamin J. Weiner,3 Christopher N. A. Willmer,3, 7 and Renbin Yan1 Received 2003 May 21; accepted 2004 March 23 ABSTRACT We measure the two-point correlation function (rp;) in a sample of 2219 galaxies between z ¼ 0:7 and 1.35 to a magnitude limit of RAB ¼ 24:1 from the first season of the DEEP2 Galaxy Redshift Survey.
    [Show full text]
  • The Evolution of Luminous Compact Blue Galaxies in COSMOS Between Z~0.0-1.0
    Graduate Theses, Dissertations, and Problem Reports 2017 The Evolution of Luminous Compact Blue Galaxies in COSMOS between z~0.0-1.0 Lucas Hunt Follow this and additional works at: https://researchrepository.wvu.edu/etd Recommended Citation Hunt, Lucas, "The Evolution of Luminous Compact Blue Galaxies in COSMOS between z~0.0-1.0" (2017). Graduate Theses, Dissertations, and Problem Reports. 5841. https://researchrepository.wvu.edu/etd/5841 This Dissertation is protected by copyright and/or related rights. It has been brought to you by the The Research Repository @ WVU with permission from the rights-holder(s). You are free to use this Dissertation in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you must obtain permission from the rights-holder(s) directly, unless additional rights are indicated by a Creative Commons license in the record and/ or on the work itself. This Dissertation has been accepted for inclusion in WVU Graduate Theses, Dissertations, and Problem Reports collection by an authorized administrator of The Research Repository @ WVU. For more information, please contact [email protected]. The Evolution of Luminous Compact Blue Galaxies in COSMOS between z∼0.0-1.0 Lucas Hunt Dissertation Submitted to The Eberly College of Arts and Sciences at West Virginia University in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Physics Dr. D.J. Pisano Ph.D., Chair Dr. Loren Anderson Ph.D. Dr. Sean McWilliams Ph.D. Dr. John Jones Ph.D. Moragntown, West Virginia 2017 Keywords: galaxies: evolution; galaxies: star formation; radio continuum: galaxies; radio lines: Copyright 2017 Lucas Hunt Abstract The Evolution of Luminous Compact Blue Galaxies in COSMOS between z∼0.0-1.0 Lucas Hunt Luminous Compact Blue Galaxies are bright, compact star forming galax- ies that are common in the distant universe, but rare locally.
    [Show full text]
  • UC Santa Cruz UC Santa Cruz Electronic Theses and Dissertations
    UC Santa Cruz UC Santa Cruz Electronic Theses and Dissertations Title Shaping Galaxy Evolution with Galaxy Structure Permalink https://escholarship.org/uc/item/9sq624hk Author Cheung, Edmond Publication Date 2014 Peer reviewed|Thesis/dissertation eScholarship.org Powered by the California Digital Library University of California UNIVERSITY OF CALIFORNIA SANTA CRUZ SHAPING GALAXY EVOLUTION WITH GALAXY STRUCTURE A dissertation submitted in partial satisfaction of the requirements for the degree of Doctor of Philosophy in ASTRONOMY & ASTROPHYSICS by Edmond Cheung June 2014 The Dissertation of Edmond Cheung is approved: Professor Sandra M. Faber, Chair Professor David C. Koo Professor Charlie Conroy Dean Tyrus Miller Vice Provost and Dean of Graduate Studies Copyright c by Edmond Cheung 2014 Table of Contents List of Figures vi List of Tables viii Abstract ix Dedication xi Acknowledgments xii 1 Introduction1 2 The Dependence of Quenching upon the Inner Structure of Galaxies at 0:5 ≤ z < 0:8 in the DEEP2/AEGIS Survey7 2.1 Introduction....................................7 2.2 Data........................................ 16 2.2.1 CFHT BRI Photometric Catalog..................... 16 2.2.2 HST ACS V+I Imaging and SExtractor Photometry........... 16 2.2.3 GIM2D.................................. 17 2.2.4 DEEP2 + DEEP3 Redshift Survey.................... 19 2.2.5 Photometric Redshifts.......................... 20 2.2.6 Rest-frame Absolute B Magnitudes and U - B Colors.......... 20 2.2.7 Stellar Masses.............................. 22 2.2.8 Error Estimates.............................. 24 2.3 Sample Selection................................. 26 2.3.1 Completeness............................... 29 2.4 Results....................................... 32 2.4.1 The Most Discriminating Color Parameter................ 32 2.4.2 Properties of Galaxies in the M∗=re Overlap Region..........
    [Show full text]
  • Probabilistic Photometric Redshifts in the Era of Petascale Astronomy
    c 2014 by Matias Carrasco Kind. All rights reserved. PROBABILISTIC PHOTOMETRIC REDSHIFTS IN THE ERA OF PETASCALE ASTRONOMY BY MATIAS CARRASCO KIND DISSERTATION Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Astronomy in the Graduate College of the University of Illinois at Urbana-Champaign, 2014 Urbana, Illinois Doctoral Committee: Associate Professor Robert J. Brunner, Chair Associate Professor Athol J. Kemball Associate Professor Paul M. Ricker Professor Jon J. Thaler Abstract With the growth of large photometric surveys, accurately estimating photometric redshifts, preferably as a probability density function (PDF), and fully understanding the implicit systematic uncertainties in this process has become increasingly important. These surveys are expected to obtain images of billions of distinct galaxies. As a result, storing and analyzing all of these photometric redshift PDFs will be non-trivial, and this challenge becomes even more severe if a survey plans to compute and store multiple different PDFs. In this thesis, we have developed an end-to-end framework that will compute accurate and robust photometric redshift PDFs for massive data sets by using two new, state-of-the-art machine learning techniques that are based on a random forest and a random atlas, respectively. By using data from several photometric surveys, we demonstrate the applicability of these new techniques, and we demonstrate that our new approach is among the best techniques currently available. We also show how different techniques can be combined by using novel Bayesian techniques to improve the photometric redshift precision to unprecedented levels while also presenting new approaches to better identify outliers.
    [Show full text]