DOCSLIB.ORG

Curriculum Vitae

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Curriculum Vitae CURRICULUM VITAE Carlos Hern´andez Monteagudo March 2008 Name Carlos Hern´andez Monteagudo Date of Birth 27th Sept 1975 Citizenship Spanish Current Address Dept. of Physics & Astronomy University of Pennsylvania 209 South 33rd Str. PA 19104, Philadelphia. USA e-mail [email protected] Research Experience and Education 2007- Post-doc Fellowship at the Max Planck Institut f¨ur Astrophysik, Munich, Germany. 2005-2007 Post-doc Fellowship associated to the Atacama Cosmology Telescope (ACT) at the University of Pennsylvania, Philadelphia, PA, US. 2002-2005 Post-doc Fellowship associated to the European Research Network CMBNet at the Max Planck Institut f¨ur Astrophysik, Munich, Germany. 1999-2002 Ph.D. : Intrinsic and Cluster Induced Temperature Anisotropies in the CMB Supervisor: Dr. F. Atrio–Barandela, Dr. A. Kashlinsky University of Salamanca, Salamanca, Spain 1 1997-1999 M.Sc. : Distortions and temperature anisotropies induced on the CMB by the population of galaxy clusters, (in Spanish) Supervisor: Dr. F. Atrio–Barandela University of Salamanca, Salamanca, Spain 1993-1997 B.Sc. in Physics University of Salamanca, Salamanca, Spain. Research Interests Theoretical and observational aspects of temperature anisotropies of the Cosmic Microwave Background (CMB) radiation: generation of intrinsic CMB temperature anisotropies during Hydrogen recombination, reionization and interaction of first metals with CMB photons, signatures of the growth of the large scale structure on the CMB via the Integrated Sachs-Wolfe and the Rees-Sciama effects, distortion of the CMB blackbody spectrum by hot electron plasma via the thermal Sunyaev-Zel’dovich effect, imprint of pe- culiar velocities on CMB temperature fluctuations via the kinematic Sunyaev-Zel’dovich effect, study of bulk flows and constraints on Dark Energy due to growth of peculiar velocities measured by the kinematic Sunyaev-Zel’dovich effect, effect of local gas on the CMB temperature anisotropy field, study of correlation properties of excursion sets in Gaussian fields and applications on analyses of CMB maps. Talks and Contributions. 2007 December, invited talk Buscando trazas de los primeros metales en el Universo, University of Salamanca, (Spain) 2007 December, contribution Status of the ISW Project, Working Group 5 General Meeting, Institute d’Astrophysique Spatiale, Paris (France) 2007 August, contribution A Model for the IR Source Clustering, ACT General Meeting, Princeton University, Princeton, US. 2007 April, contribution On the Evidendence for ISW in WMAP Data, BICOS meeting, Bilbao, Spain. 2007 January, invited talk First Metals in the Universe and CMB Observations, Carnegie-Mellon University, Pittsburgh, US. 2006 December, invited talk First Metals in the Universe and CMB Obervations, Christmas Workshop, Universidad Aut´onoma de Madrid, Madrid, Spain. 2006 November, invited talk Probing the Baryons in the Universe through CMB Observations, Laboratoire d’Physique Theorique, Orsay, Paris, France. 2006 October, invited talk A New Probe for Reionization?, Columbia University, New York, US. 2006 August, contribution The Spectral Signature of the Local Baryons in the CMB, Modern Cosmology, Inflation, CMB and LSS, Benasque, Spain. 2006 June, contribution The CMB and the Low-z Baryons, Astrophysics Workshop, Eotvos Laboratory, Budapest, Hungary. 2006 April, poster The thermal Sunyaev-Zel’dovich Effect of the Missing Baryons, CMB and Physics of the Early Universe, Ischia, Italy. 2006 January, contribution Correlation Properties of the kinematic Sunyaev-Zel’dovich Effect and Implications for Dark Energy, Aspen Center for Physics, Colorado, US. 2005 November, Colloquium The Influence of Large Scale Structure on WMAP’s First Year Data, NASA Goddard Space Flight Center, Maryland, US. 2005 September, contribution Is there evidence of ISW in WMAP’s first year data? at the Spanish Relativity Meeting (ERES), Oviedo, Spain 2005 May, contribution On the kSZ signal in ACT clusters, at the ACT General Meeting in Princeton University, New Jersey, US. 2004 September, contribution Cross Terms and Weak Frequency dependent Signals in the CMB Sky at the Joint European and National Astronomy Meeting (JENAM), Granada, Spain 2004 July, contribution The Effect of Hot Gas in First Year WMAP Data,by at the 20th IAP Colloquium on CMB Physics,Paris,France 2003 September, invited talk ”Hot Gas in the Universe: WMAP’s View”, at the Astrophysikalisches Institut Potsdam, Potsdam, Germany 2001 May, contribution ”Determining Cosmic Microwave Background Structure from its Peak Distribution”, given at the CMBNet Workshop on Science and Parameter Extraction, Rome, Italy. Visits 2007 December, invited to Departamento de F´ısica, University of Salamanca, Salamanca, Spain. 2007 September, invited to Insituto de F´ısica de Cantabria, Santander, Spain. 2007 April, invited to Max Planck Institut f¨ur Astrophysik, Munich, Germany. 2007 January, invited to Carnegie-Mellon University, Pittsburgh, US. 2006 December, invitied to Universidad Aut´onoma de Madrid, Madrid, Spain. 2006 November, invited to Laboratoire d’Physique Theorique, Paris, France. 2006 October, invited to Columbia University, New York, US. 2006 June, invited to Max Planck Insitut f¨ur Astrophysik, Garching bei M¨unchen, Germany. 2005 December, invited to Max Planck Insitut f¨ur Astrophysik, Garching bei M¨unchen, Germany. 2005 December, invited to NASA Goddard Space Flight Center, Maryland, US. 2005 October, invited to the California Institute of Technology (Caltech), Pasadena, California, US. 2005 May, invited to the Max Planck Insitut f¨ur Astrophysik, Garching bei M¨unchen, Germany. 2004 April, invited to the Instituto de Astrof´ısica de Canarias, (IAC), Canary Islands, Spain 2003 September, invited to Astrophysikalisches Institut Potsdam, Potsdam, Germany 2001 April-May, visited Instituto de Astrof´ısica de Canarias, (IAC), Canary Islands, Spain. 2000 October-December, visited NASA Goddard Space Flight Center, Maryland, United States. 1999 August - September, visited the Astrophysikalisches Institut Potsdam, Potsdam, Germany. Schools and Congresses 2007 December, attended Planck’s Working Group General Meeting,heldat Institute d’Astrophysique Sp`atiale, Orsay-Paris, France. 2007 September, attended the PAU-BAU General Meeting,heldat Campus Universitario de Teruel, Teruel, Spain. 2007 August, attended the ACT General Meeting,heldatPrinceton University, Princeton, US. 2007 April, attended the BICOS meeting, held in Bilbao, Spain. 2006 December, invited to the Christmas Workshop,heldatthe Universidad Aut´onoma de Madrid, Madrid, Spain. 2006 August, attended the conference Modern Cosmology, Inflation, CMB and LSS, help in Benasque, Spain. 2006 June, attended the Astrophysics Workshop organised by Z.Haiman, Budapest, Hungary. 2006 April, attended the conference CMB and Physics of the Early Universe, held in Ischia, Italy. 2006 January, attended the conference Dark Matter and Baryons in the Universe, held at the Aspen Center for Physics, Colorado, US. 2005 May, attended the ACT General Meeting held at Princeton University, New Jersey, US. 2005 March, attended the Joint Oxford Princeton Cosmology meeting, held at Princeton University, New Jersey, US. 2004 September, attended the Joint European and National Astronomy Meeting, held in Granada, Spain, and presented the poster The Effect of Hot Gas in First Year WMAP Data,by C.Hern´andez-Monteagudo, R.G´enova-Santos & Atrio-Barandela 2004 July, attended the 20th IAP Colloquium on CMB Physics, held in Paris, France 2004 April, invited to the Oort Workshop CMB and First Objects at the End of the Dark Ages: Observational Consequences of Reionization at Universiteit Leiden, Leiden, Holland 2004 January, attended the II Symposium on the Planck mission Setting the Scene, Paris, France, and presented the posters Cross Terms and Weak Signals in the CMB Sky,byC.Hern´andez-Monteagudo & R.A. Sunyaev, CMB Observations and Metal Production during the Dark Ages, by K.Basu, C.Hern´andez-Monteagudo R.A. Sunyaev, and Measuring Dark Matter Flows in Merging Clusters of Galaxies, by J.A.Rubi˜no–Mart´ın, C.Hern´andez-Monteagudo & T. Enßlin. 2002 December, attended the XXI Symposium on Relativistic Astrophysics Texas in Tuscany, Florence, Italy, and presented the poster CMB Observations and the Production of Chemical Elements at the End of the Dark Ages,byK.Basu, C.Hern´andez-Monteagudo & R.A. Sunyaev 2002 December, organized and participated in the CMBNet Meeting CMB Cosmology: Where Are We? held in Ringberg Castle, Bavaria, Germany 2000 August, attended MPA/ESO/MPE Joint Astronomy Meeting, Mining the Sky , held in Munich, Germany, and presented the poster Measuring Bulk Flows with Kinematic Sunyaev-Zeldovich effect,by F.Atrio-Barandela, C.Hern´andez-Monteagudo & J.P.M¨ucket. 2000 January, attended congress Energy Densities in the Universe, held in Les Arcs, France, and presented the poster On the Number Density of Sunyaev-Zel’dovich Clusters, by C.Hern´andez–Monteagudo, F.Atrio–Barandela and J.P.M¨ucket. 1999 December, attended Daniel Chalonge School of Astrophysics: Current Topics in Astrofundamental Physics, held in Erice, Sicily, Italy. 1998 June, attended congress The Cosmic Microwave Background Radiation and the Planck Mission, held in Santander, Spain. 1997 November, attended IX Canary Islands Winter School of Astrophysics, Large Databases in the Internet Age, Canary Islands, Spain. Selected Five Recent Refereed Publications: • ”Oxygen pumping II: Probing the Inhomogeneous Metal Enrichment at the Epoch of Reionization with High Frequency
Load more

Recommended publications
  • Understanding Cosmic Acceleration: Connecting Theory and Observation
    Understanding Cosmic Acceleration V(!) ! E Hivon Hiranya Peiris Hubble Fellow/ Enrico Fermi Fellow University of Chicago #OMPOSITIONOFAND+ECosmic HistoryY%VENTS$ UR/ INGTHE%CosmicVOLUTIONOFTHE5 MysteryNIVERSE presentpresent energy energy Y density "7totTOT = 1(k=0)K density DAR RADIATION KENER dark energy YDENSIT DARK G (73%) DARKMATTER Y G ENERGY dark matter DARK MA(23.6%)TTER TIONOFENER WHITEWELLUNDERSTOOD DARKNESSPROPORTIONALTOPOORUNDERSTANDING BARYONS BARbaryonsYONS AC (4.4%) FR !42 !33 !22 !16 !12 Fractional Energy Density 10 s 10 s 10 s 10 s 10 s 1 sec 380 kyr 14 Gyr ~1015 GeV SCALEFACTimeTOR ~1 MeV ~0.2 MeV 4IME TS TS TS TS TS TSEC TKYR T'YR Y Y Planck GUT Y T=100 TeV nucleosynthesis Y IES TION TS EOUT DIAL ORS TIONS G TION TION Z T Energy THESIS symmetry (ILC XA 100) MA EN EE WNOF ESTHESIS V IMOR GENERATEOBSERVABLE IT OR ELER ALTHEOR TIONS EF SIGNATURESINTHE#-" EAKSYMMETR EIONIZA INOFR Y% OMBINA R E6 EAKDO #X ONASYMMETR SIC W '54SYMMETR IMELINEOF EFFWR Y Y EC TUR O NUCLEOSYN ), * +E R 4 PLANCKENER Generation BR TR TURBA UC PH Cosmic Microwave NEUTR OUSTICOSCILLA BAR TIONOFPR ER A AC STR of primordial ELEC non-linear growth of P 44 LIMITOFACC Background Emitted perturbations perturbations: GENER ES carries signature of signature on CMB TUR GENERATIONOFGRAVITYWAVES INITIALDENSITYPERTURBATIONS acoustic#-"%MITT oscillationsED NON LINEARSTR andUCTUR EIMPARTS #!0-!0OBSERVES#-" ANDINITIALDENSITYPERTURBATIONS GROWIMPARTINGFLUCTUATIONS CARIESSIGNATUREOFACOUSTIC SIGNATUREON#-"THROUGH *throughEFFWRITESUPANDGR weakADUATES WHICHSEEDSTRUCTUREFORMATION
    [Show full text]
  • Licia Verde ICREA & ICC-UB BARCELONA
    Licia Verde ICREA & ICC-UB BARCELONA Challenges of par.cle physics: the cosmology connecon http://icc.ub.edu/~liciaverde Context and overview • Cosmology over the past 20 years has made the transition to precision cosmology • Cosmology has moved from a data-starved science to a data-driven science • Cosmology has now a standard model. The standard cosmological model only needs few parameters to describe origin composition and evolution of the Universe • Big difference between modeling and understanding • Implies Challenges and opportunities Precision cosmology ΛCDM: The standard cosmological model Just 6 numbers….. describe the Universe composition and evolution Homogenous background Perturbations connecons • Inflaon • Dark maer (some 80% of all the maer) • Dark energy (some 80% of all there is) • Origin of (the rest of) the maer • Neutrinos (~0.5% of maer, but sll) • … Primary CMB temperature informaon content has been saturated. The near future is large-scale structure. SDSS LRG galaxies power spectrum (Reid et al. 2010) 13 billion years of gravita2onal evolu2on Longer-term .mescale: CMB polarizaon Can now do (precision) tests of fundamental physics with cosmological data “We can’t live in a state of perpetual doubt, so we make up the best story possible and we live as if the story were true.” Daniel Kahneman about theories GR, big bang, choice of metric, nucelosynthesis, etc etc… Cosmology tends to rely heavily on models (both for “signal” and “noise”) Essen.ally, all models are wrong , but some are useful (Box and Draper 1987) With
    [Show full text]
  • Curriculum Vitae Í
    Royal Observatory Blackford Hill Alexander Mead Edinburgh EH9 3HJ, UK B [email protected] curriculum vitae Í https://alexander-mead.github.io. Academic appointments 2020 – 2021 GLOBE senior postdoctoral researcher, cosmological structure formation, University of Edinburgh, Catherine Heymans. 2017 – 2020 Marie Sklodowska Curie Fellowship, weak lensing, University of Barcelona and University of British Columbia, Licia Verde and Ludovic van Waerbeke. 2015 – 2017 Candian Institute of Theoretical Astrophysics National Fellowship, weak lensing, University of British Columbia, Ludovic van Waerbeke. 2014 – 2015 Postdoctoral fellow, baryonic feedback, matter clustering, weak lensing, University of Edinburgh, Catherine Heymans. Education 2010 – 2014 PhD, cosmological structure formation, University of Edinburgh, John Peacock. 2005 – 2010 MPhys, University of Oxford, first class, Millard Exhibition, Trinity scholarship. Awards 2016 Marie Sklodowska Curie Fellowship, UBC and Barcelona. 2015 CITA National Fellowship, UBC and CITA. 2012 Vitae Postgraduates Who Tutor Award (nomination), Edinburgh. 2012 Teach First Innovative Teaching Award (nomination), Edinburgh. 2010 STFC funded PhD position, Edinburgh. 2010 Peter Fisher prize, top results in college, Oxford. 2009 Trinity College Scholarship, first-class results in exams, Oxford. 2008 Millard Exhibition, high standard of academic work, Oxford. PhD thesis Title Demographics of dark-matter haloes in standard and non-standard cosmologies Supervisors John Peacock, Alan Heavens, Sylvain de la Torre, Lucas Lombriser 1/6 Description (1) Tuning the halo model of structure formation to accurately predict the full non- linear matter power spectrum as a function of cosmological parameters. (2) Rescaling cosmological simulations, in terms of both matter distributions and halo catalogues, between cosmological models. (3) Rescaling simulations from standard to modified gravity models.
    [Show full text]
  • Licia Verde ICREA & ICC-UB-IEEC Barcelona, Spain Oiu, Oslo, Norway
    Licia Verde ICREA & ICC-UB-IEEC Barcelona, Spain OiU, Oslo, Norway Neutrino masses from cosmology! http://icc.ub.edu/~liciaverde Recent developments: data CMB (Planck and ACT/SPT) Sloan Digital Sky Survey BOSS, WIGGLEZ Baryon Acoustic Oscillations & clustering NEWS: FUTURE DATA recent developments: theory Better modeling of non-linearities via N-body simulations (and perturbation theory) Avalanche of data over the last ~10 yr Detailed statistical properties of these ripples tell us a lot about the Universe Avalanche of data over the last ~10 yr Detailed statistical properties of these ripples tell us a lot about the Universe Extremely successful standard cosmological model Look for deviaons from the standard model Test physics on which it is based and beyond it •" Dark energy •" Nature of ini<al condi<ons: Adiabacity, Gaussianity •" Neutrino proper<es •" Inflaon proper<es •" Beyond the standard model physics… ASIDE: We only have one observable universe The curse of cosmology We can only make observations (and only of the observable Universe) not experiments: we fit models (i.e. constrain numerical values of parameters) to the observations: Any statement is model dependent Gastrophysics and non-linearities get in the way : Different observations are more or less “trustable”, it is however somewhat a question of personal taste (think about Standard & Poor’s credit rating for countries): Any statement depends on the data-set chosen Results will depend on the data you (are willing to) consider. I try to use > A rating ;) ….And the Blessing
    [Show full text]
  • First Year Wilkinson Microwave Anisotropy Probe (Wmap) Observations: Interpretation of the Tt and Te Angular Power Spectrum Peaks
    SUBMITTED TO The Astrophysical Journal Preprint typeset using LATEX style emulateapj v. 11/12/01 FIRST YEAR WILKINSON MICROWAVE ANISOTROPY PROBE (WMAP) OBSERVATIONS: INTERPRETATION OF THE TT AND TE ANGULAR POWER SPECTRUM PEAKS L. PAGE1, M. R. NOLTA1, C. BARNES1, C. L. BENNETT2, M. HALPERN3, G. HINSHAW2, N. JAROSIK1, A. KOGUT2, M. LIMON2,8 , S. S. MEYER4, H. V. PEIRIS5, D. N. SPERGEL5, G. S. TUCKER6,8, E. WOLLACK2, E. L. WRIGHT7 [email protected] Subject headings: cosmic microwave background, cosmology: observations Submitted to The Astrophysical Journal ABSTRACT The CMB has distinct peaks in both its temperature angular power spectrum (TT) and temperature-polarization ¢ cross-power spectrum (TE). From the WMAP data we find the first peak in the temperature spectrum at = 220 ¡ 1 ¡ ¢ ¡ £ ¡ ¢ ¡ ¡ ¢ ¡ £ 0 ¡ 8 with an amplitude of 74 7 0 5 K; the first trough at = 411 7 3 5 with an amplitude of 41 0 0 5 K; ¡ ¢ ¡ £ and the second peak at = 546 ¢ 10 with an amplitude of 48 8 0 9 K. The TE spectrum has an antipeak at 2 2 − ¢ £ ¢ ¢ £ = 137 ¢ 9 with a cross-power of 35 9 K , and a peak at = 329 19 with cross-power 105 18 K . All uncertainties are 1 ¤ and include calibration and beam errors. An intuition for how the data determine the cosmological parameters may be gained by limiting one’s attention to a subset of parameters and their effects on the peak characteristics. We interpret the peaks in the context of a 2 2 ¦ ¦ flat adiabatic ¥ CDM model with the goal of showing how the cosmic baryon density, bh , matter density, mh , scalar index, ns, and age of the universe are encoded in their positions and amplitudes.
    [Show full text]
  • Cosmological Implications of WMAP First Year Results (Licia Verde
    Cosmological implications of WMAP first year results Licia Verde University of Pennsylvania Cosmological implications of WMAP first year results Licia Verde University of Pennsylvania www.physics.upenn.edu/~lverde Overview Wilkinson Microwave Anisotropy Probe What we can learn from CMB and why What we have learned from WMAP Adding external data sets into the analysis What all this tells us about the Universe Conclusions David Wilkinson 1935-2002 WMAP A partnership between NASA/GSFC and Princeton Science Team: NASA/GSFC Chuck Bennett (PI) Michael Greason Bob Hill Gary Hinshaw Al Kogut Michele Limon Nils Odegard Janet Weiland Ed Wollack Brown UCLA Greg Tucker Ned Wright Princeton Chris Barnes Lyman Page Norm Jarosik Hiranya Peiris UBC Chicago Eiichiro Komatsu David Spergel Mark Halpern Stephan Meyer Michael Nolta Licia Verde Launched from cape Canaveral on June 30 2001 Phasing loops Lunar swingby Trajectory Official arrival date: 100 days to L2, 1.5e6 km from Earth. Oct 1, 2001 (Most of) WMAP Science Team, August 2002 WMAP’s Purpose To make a high resolution map of the cosmic microwave background (CMB) radiation to determine the cosmology of our universe. •Structures of the CMB carry cosmological information (Age, Composition…) •The cleanest picture of the infant universe Æ a clue to very early universe WILKINSON MICROWAVE ANISOTROPY PROBE Fossil light from 380,000 years after the Big-Bang 15 papers since February 2003… I will try to be brief http://lambda.gsfc.nasa.gov COBE ‘92 Bennett et al 2003 T IME EM T Big Bang P. Cosmic History Inflation-like epoch. new ρradiation = ρmatter zeq = 3230 tU = 56 kyr new CMB decouples from plasma t = 380 kyr zdec = 1089 U T CMB = 2970 K First stars form new z r = 20 t U = 200 Myr NOW new t = 13.7 Gyr MAP990011 z = 0 U T CMB = 2.725K Study cosmology with the CMB: “Seeing sound” (W.
    [Show full text]
  • A Practical Guide to Basic Statistical Techniques for Data Analysis In
    A practical guide to Basic Statistical Techniques for Data Analysis in Cosmology Licia Verde∗ ICREA & Institute of Space Sciences (IEEC-CSIC), Fac. Ciencies, Campus UAB Torre C5 parell 2 Bellaterra (Spain) Abstract This is the summary of 4 Lectures given at the XIX Canary islands winter school of Astrophysics ”The Cosmic Microwave Background, from quantum Fluctuations to the present Universe”. arXiv:0712.3028v2 [astro-ph] 7 Jan 2008 ∗Electronic address: [email protected] 1 Contents I. INTRODUCTION 3 II. Probabilities 4 A. What’s probability: Bayesian vs Frequentist 4 B. Dealing with probabilities 5 C. Moments and cumulants 7 D. Useful trick: the generating function 8 E. Two useful distributions 8 1. The Poisson distribution 8 2. The Gaussian distribution 9 III. Modeling of data and statistical inference 10 A. Chisquare, goodness of fit and confidence regions 11 1. Goodness of fit 12 2. Confidence region 13 B. Likelihoods 13 1. Confidence levels for likelihood 14 C. Marginalization, combining different experiments 14 D. An example 16 IV. Description of random fields 16 A. Gaussian random fields 18 B. Basic tools 19 1. The importance of the Power spectrum 21 C. Examples of real world issues 22 1. Discrete Fourier transform 23 2. Window, selection function, masks etc 24 3. pros and cons of ξ(r) and P (k) 25 4. ... and for CMB? 26 5. Noise and beams 27 6. Aside: Higher orders correlations 29 2 V. More on Likelihoods 30 VI. Monte Carlo methods 33 A. Monte Carlo error estimation 33 B. Monte Carlo Markov Chains 34 C.
    [Show full text]
  • Isocurvature Modes and Baryon Acoustic Oscillations
    Preprint typeset in JHEP style - PAPER VERSION Isocurvature modes and Baryon Acoustic Oscillations Anna Mangilli ICC-UB (Instituto de Ciencias del Cosmos at Universitad de Barcelona), Marti i Franques 1, Barcelona, Spain & Institute of Space Sciences (IEEC-CSIC), Fac. Ciencies, Campus UAB, Bellaterra [email protected] Licia Verde ICC-UB (Instituto de Ciencias del Cosmos at Universitad de Barcelona), Marti i Franques 1, Barcelona, Spain & Institute of Space Sciences (IEEC-CSIC), Fac. Ciencies, Campus UAB, Bellaterra &ICREA (Institucio’ Catalana de Recerca i Estudis Avancats) [email protected] Maria Beltran Department of Astronomy and Astrophysics, The University of Chicago, 5640 S Ellis, Chicago IL 60637, USA [email protected] Abstract: The measurement of Baryonic Acoustic Oscillations from galaxy surveys is well known to be a robust and powerful tool to constrain dark energy. This method relies on the knowledge of the size of the acoustic horizon at radiation drag derived from Cosmic Microwave Background Anisotropy measurements. In this paper we quantify the effect of non-standard initial conditions in the form of an isocurvature component on the determination of dark energy parameters from future BAO surveys. In particular, if there arXiv:1006.3806v1 [astro-ph.CO] 18 Jun 2010 is an isocurvature component (at a level still allowed by present data) but it is ignored in the CMB analysis, the sound horizon and cosmological parameters determination is biased, and, as a consequence, future surveys may incorrectly suggest deviations from a cosmological constant. In order to recover an unbiased determination of the sound horizon and dark energy parameters, a component of isocurvature perturbations must be included in the model when analyzing CMB data.
    [Show full text]
  • A Taste of Cosmology
    A taste of cosmology Licia Verde http://icc.ub.edu/~liciaverde OUTLINE • The standard cosmological model • The successes of cosmology over the past 10 years • Cosmic Microwave Background • Large-scale structure • Inflation and outlook for the future Lectures and additional material will appear at http://icc.ub.edu/~liciaverde/CLASHEP.html Cosmology Cosmos= Universe, Order, beauty -logy= study Greek! Study of the Universe as a whole Aim at getting an understanding of: -its origin -its structure and composition (where do galaxies, stars, planets, people come from?) -its evolution -its fate In general for cosmologists galaxies are points…. Scales involved! 3d19Km 1d18Km 1.2d4Km 40AU=6d9Km New units of measure For distance, we use pc, Kpc & Mpc For comparison, mean Earth-Sun distance (Astronomical Unit): " Cosmologists often express masses " in units of the solar mass: MOTIVATION • Cosmology over the past 15 years has made the transition to precision cosmology • Cosmology has moved from a data-starved science to a data-driven science • Cosmology has now a standard model. The standard cosmological model only needs few parameters to describe origin composition and evolution of the Universe • Big difference between modeling and understanding Motivation: Why should you care about observational cosmology? Deep connections between cosmology and fundamental physics Testing fundamental physics by looking up at the sky is not new The interplay between astrophysics and fundamental physics has already produced spectacular findings (e.g. the solar neutrino
    [Show full text]
  • (Lack Of) Cosmological Evidence for Dark Radiation After Planck
    Prepared for submission to JCAP (Lack of) Cosmological evidence for dark radiation after Planck Licia Verde,a;b Stephen M. Feeney,c Daniel J. Mortlockd;e and Hiranya V. Peirisc;f aICREA & ICC, Institut de Ciencies del Cosmos, Universitat de Barcelona (IEEC-UB), Marti i Franques 1, Barcelona 08028, Spain bTheory Group, Physics Department, CERN, CH-1211, Geneva 23, Switzerland cDepartment of Physics and Astronomy, University College London, London WC1E 6BT, U.K. dAstrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ, U.K. eDepartment of Mathematics, Imperial College London, London SW7 2AZ, U.K. f Kavli Institute for Theoretical Physics, Kohn Hall, University of California, Santa Barbara, CA 93106, USA E-mail: [email protected], [email protected], [email protected], [email protected] Abstract. We use Bayesian model comparison to determine whether extensions to Standard-Model neutrino physics { primarily additional effective numbers of neutrinos and/or massive neutrinos { are merited by the latest cosmological data. Given the significant advances in cosmic microwave back- ground (CMB) observations represented by the Planck data, we examine whether Planck temperature and CMB lensing data, in combination with lower redshift data, have strengthened (or weakened) the previous findings. We conclude that the state-of-the-art cosmological data do not show evidence for deviations from the standard (ΛCDM) cosmological model (which has three massless neutrino fami- lies). This does not mean that the model is necessarily correct { in fact we know it is incomplete as arXiv:1307.2904v2 [astro-ph.CO] 10 Sep 2013 neutrinos are not massless { but it does imply that deviations from the standard model (e.g., non-zero neutrino mass) are too small compared to the current experimental uncertainties to be inferred from cosmological data alone.
    [Show full text]
  • Shapefit: Extracting the Power Spectrum Shape Information in Galaxy Surveys Beyond BAO and RSD
    Prepared for submission to JCAP ShapeFit: Extracting the power spectrum shape information in galaxy surveys beyond BAO and RSD Samuel Brieden,1;2 H´ector Gil-Mar´ın,1 Licia Verde1;3 1ICC, University of Barcelona, IEEC-UB, Mart´ıi Franqu`es,1, E-08028 Barcelona, Spain 2Dept. de F´ısicaQu`antica i Astrof´ısica,Universitat de Barcelona, Mart´ıi Franqu`es1, E- 08028 Barcelona, Spain. 3ICREA, Pg. Llu´ısCompanys 23, Barcelona, E-08010, Spain. Abstract. In the standard (classic) approach, galaxy clustering measurements from spectro- scopic surveys are compressed into baryon acoustic oscillations and redshift space distortions measurements, which in turn can be compared to cosmological models. Recent works have shown that avoiding this intermediate step and fitting directly the full power spectrum sig- nal (full modelling) leads to much tighter constraints on cosmological parameters. Here we show where this extra information is coming from and extend the classic approach with one additional effective parameter, such that it captures, effectively, the same amount of infor- mation as the full modelling approach, but in a model-independent way. We validate this new method (ShapeFit) on mock catalogs, and compare its performance to the full mod- elling approach finding both to deliver equivalent results. The ShapeFit extension of the classic approach promotes the standard analyses at the level of full modelling ones in terms of information content, with the advantages of i) being more model independent; ii) offering an understanding of the origin of the
    [Show full text]
  • Licia Verde University of Pennsylvania
    Complementarity in Dark Energy measurements Complementarity of optical data in constraining dark energy Licia Verde University of Pennsylvania www.physics.upenn.edu/~lverde The situation: SN 1A (Riess et al 04) CMB+ CMB(WMAP ext) H prior (HST Key project) LSS (2dF Verde et al 02) Assuming a flat Universe…. CMB (WMAPext) CMB+H SN(Riess et al 04) Assuming a flat Universe…. CMB (WMAPext) CMB+Galaxy surveys SN(Riess et al 04) But, why constant? Assuming a flat Universe…. Baryon oscill. SDSS Eisenstein et al. 05 CTIO +CMB+SN Jarvis et al 05 (75 sq degrees, no redshifts) + CFHTLS Sembloni et al 05 (3 sq degrees) But, why w constant? Why flatness? THE SYMPTOMS Or OBSERVATIONAL EFFECTS of DARK ENERGY Recession velocity vs brightness of standard candles: dL(z) CMB acoustic peaks: Da to last scattering Da to zsurvey LSS: perturbations amplitude today, to be compared with CMB (or Matter density today) HOW TO MAKE A DIAGNOSIS? Any modification of gravity of the form of f( R ) can be written as a quintessence model for a(t) This degeneracy is lifted when considering the growth of structure Effort in determining what the growth of structure is in a given Dark Energy model! combination of approaches! We can “measure” dark energy because of its effects on the expansion history of the universe and the growth of structure a&(t) 1 dz = H (z) = − a(t) (1+ z) dt 0 dt 2 2 d (1 z) (1 z') dz' H = H 0[ρ(z) / ρ(0)] SN: measure dL L = + ∫ + z dz' CMB: θ A and ISW a(t) S See Rocky&Josh talks LSS or LENSING: g(z) or a(t) S S AGES: H(z) a(t) S dz z dz' Standard clocks H −1 (1 z)5/ 2{ (0) (0)exp[3 w ]}1/ 2 0 = − + Ωm + ΩQ ∫ Q dt 0 (1+ z') ρ&Q = −3H (z)(1+ w(z))ρQ COMPLEMENTARITY IS THE KEY! The questions we want to ask: Example: Is it a cosmological constant? Measurements of the A rolling scalar field? A fluid? growth of cosmological Is it a w= -1? w(z)? structures will help to disentangle the two cases.
    [Show full text]