DISCOVERY A Unique Center with Unique Opportunities Direct and unique access to data from the most powerful experiments available today : –The Large Hadron.

Slides:



Advertisements
Similar presentations
Observation of the Universe from the Moon – Elisabetta Cavazzuti – LNF May 7, 2007 ITALIAN VISION FOR MOON EXPLORATION OBSERVATION OF THE UNIVERSE FROM.
Advertisements

QUIET Q/U Imaging ExperimenT Osamu Tajima (KEK) QUIET collaboration 1.
1 N U PECC 2012 Copenhagen. 12/05/11Jens Jørgen Gaardhøje, NBI & DISCOVERY2 Morphology of CMB and HIC. Commonality and perspectives. P. Naselsky, PLANCK.
Planck 2013 results, implications for cosmology
Combined Energy Spectra of Flux and Anisotropy Identifying Anisotropic Source Populations of Gamma-rays or Neutrinos Sheldon Campbell The Ohio State University.
Systematic effects in cosmic microwave background polarization and power spectrum estimation SKA 2010 Postgraduate Bursary Conference, Stellenbosch Institute.
The Big Bang Or… The Standard Model. Precepts of the standard model The laws of Physics are the same throughout the Universe. The Universe is expanding.
Contamination of the CMB Planck data by galactic polarized emissions L. Fauvet, J.F. Macίas-Pérez.
Theoretical work on Cosmology and Structure Formation Massimo Ricotti.
Component Separation of Polarized Data Application to PLANCK Jonathan Aumont J-F. Macías-Pérez, M. Tristram, D. Santos
Stardust in the Early Universe Erik Elfgren Luleå University of Technology Swedish National Graduate School of Space Technology.
Deciphering the gamma-ray background: stafrorming galaxies, AGN, and the search for Dark Matter in the GeV Band. Vasiliki Pavlidou Einstein Fellow Shin’ichiro.
Primordial BHs. 2 Main reviews and articles astro-ph/ Primordial Black Holes - Recent Developments astro-ph/ Gamma Rays from Primordial.
The International Linear Collider Barry Barish iThemba Cape Town 21-Oct-05.
1 On the road to discovery of relic gravitational waves: From cosmic microwave background radiation Wen Zhao Department of Astronomy University of Science.
Cosmic Microwave Background (CMB) Peter Holrick and Roman Werpachowski.
Modelling radio galaxies in simulations: CMB contaminants and SKA / Meerkat sources by Fidy A. RAMAMONJISOA MSc Project University of the Western Cape.
New States of Matter and RHIC Outstanding questions about strongly interacting matter: How does matter behave at very high temperature and/or density?
P olarized R adiation I maging and S pectroscopy M ission Probing cosmic structures and radiation with the ultimate polarimetric spectro-imaging of the.
PHY306 1 Modern cosmology 4: The cosmic microwave background Expectations Experiments: from COBE to Planck  COBE  ground-based experiments  WMAP  Planck.
Physics Session Summary Nobuchika Okada Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization (KEK) TILC09, Tsukuba,
Early times CMB.
Bill Reach 2009 May 14 Greater IPAC Technology Symposium.
The Cosmic Microwave Background Lecture 2 Elena Pierpaoli.
CMB observations and results Dmitry Pogosyan University of Alberta Lake Louise, February, 2003 Lecture 1: What can Cosmic Microwave Background tell us.
Intro to Cosmology! OR What is our Universe?. The Latest High Resolution Image of the Cosmic Microwave Background Radiation Low Energy RegionHigh Energy.
The Energy in our Universe Dr. Darrel Smith Department of Physics.
The Revolution for the Rest of Us George Musser 6 October 2006.
COSMOLOGY SL - summary. STRUCTURES Structure  Solar system  Galaxy  Local group  Cluster  Super-cluster Cosmological principle  Homogeneity – no.
AS2001 / 2101 Chemical Evolution of the Universe Keith Horne Room 315A
MAPping the Universe ►Introduction: the birth of a new cosmology ►The cosmic microwave background ►Measuring the CMB ►Results from WMAP ►The future of.
AS2001 Chemical Evolution of the Universe Keith Horne 315a
LHC conference - Isfahan
Joint analysis of Archeops and WMAP observations of the CMB G. Patanchon (University of British Columbia) for the Archeops collaboration.
PHY306 1 Modern cosmology 4: The cosmic microwave background Expectations Experiments: from COBE to Planck  COBE  ground-based experiments  WMAP  Planck.
Exotic Physics in the Dark Ages Katie Mack Institute of Astronomy / Kavli Institute for Cosmology, University of Cambridge.
High Energy Nuclear Physics and the Nature of Matter Outstanding questions about strongly interacting matter: How does matter behave at very high temperature.
The measurement of q 0 If objects are observed at large distances of known brightness (standard candles), we can measure the amount of deceleration since.
Anomalies of low multipoles of WMAP
Cosmic Microwave Background Carlo Baccigalupi, SISSA CMB lectures at TRR33, see the complete program at darkuniverse.uni-hd.de/view/Main/WinterSchoolLecture5.
Collaborators within DK-Planck community Lung-Yih Chiang (NBI) Andrei Doroshkevich (TAC,ASC FIRAN) Per Rex Christensen (NBI) Igor D. Novikov ( NBI) Pavel.
The Far-Infrared Universe: from the Universe’s oldest light to the birth of its youngest stars Jeremy P. Scott, on behalf of Locke D. Spencer Physics and.
The Planck Satellite Hannu Kurki-Suonio University of Helsinki Finnish-Japanese Workshop on Particle Cosmology, Helsinki
Chapter 17 The Beginning of Time. Running the Expansion Backward Temperature of the Universe from the Big Bang to the present (10 10 years ~ 3 x
Structure Formation in the Universe Concentrate on: the origin of structure in the Universe How do we make progress?How do we make progress? What are the.
Collider searchIndirect Detection Direct Detection.
Planck Report on the status of the mission Carlo Baccigalupi, SISSA.
MARCH 11YPM 2015  ray from Galactic Center Tanmoy Mondal SRF PRL Dark Matter ?
Observation and Data Analysis Activityin SPOrt and BaR-SPOrt Exp.s Ettore Carretti Bologna 7-9 January 2004.
Search for a Z′ boson in the dimuon channel in p-p collisions at √s = 7TeV with CMS experiment at the Large Hadron Collider Search for a Z′ boson in the.
Astrophysics from the Moon in the Radio Band Gianfranco Brunetti INAF - IRA, Bologna.
Blind Component Separation for Polarized Obseravations of the CMB Jonathan Aumont, Juan-Francisco Macias-Perez Rencontres de Moriond 2006 La.
The Cosmic Microwave Background
Compelling Scientific Questions The International Linear Collider will answer key questions about matter, energy, space and time We now sample some of.
FIRST LIGHT A selection of future facilities relevant to the formation and evolution of galaxies Wavelength Sensitivity Spatial resolution.
The Planck Satellite Matthew Trimble 10/1/12. Useful Physics Observing at a redshift = looking at light from a very distant object that was emitted a.
Theoretical Motivation for Submm-VLBI of Sgr A* Heino Falcke ASTRON, Dwingeloo University of Nijmegen.
Cosmic Microwave Background Carlo Baccigalupi, SISSA CMB lectures at TRR33, see the complete program at darkuniverse.uni-hd.de/view/Main/WinterSchoolLecture5.
Cosmic Background Explorer: COBE
“VERITAS Science Highlights” VERITAS: TeV Astroparticle Physics Array of four 12-m Cherenkov telescopes Unprecedented sensitivity: ~100 GeV to ~30 TeV.
PLANCK TEAM of the DISCOVERY Center. The most mysterious problems.
CMB physics Zong-Kuan Guo 《现代宇宙学》
Topics on Dark Matter Annihilation
Cosmic Microwave Background Polarization
Planck mission All information and images in these slides can be found browsing through
Can dark matter annihilation account for the cosmic e+- excesses?
12th Marcel Grossman Meeting,
The Beginning of Time (Birth Of The Universe)
Primordial BHs.
“B-mode from space” workshop,
Presentation transcript:

DISCOVERY A Unique Center with Unique Opportunities Direct and unique access to data from the most powerful experiments available today : –The Large Hadron Collider (LHC) at CERN exploring p+p and Pb+Pb collisions at unprecedented high energies (ATLAS and ALICE experiments) –The Planck satellite mission with unique resolution and sensitivity of the sky. 1 DISCOVERY unites strong groups in: Theory, Fundamental Particle Physics, Quark Gluon Plasma Physics Cosmic Microwave Radiation Physics, …which most places rarely work together.

DC PLANCK Team DISCOVERY CENTER OF EXCELLENCE IN PARTICLE PHYSICS, PHENOMENOLOGY & COSMOLOGY

Boomerang map WMAP

Discovery Synergy “at large” TT1. Testing new models of inflation. TT1a. The Higgs boson driven inflation. Theoretical basis of these models was widely discussed in the paper “ Observational consequences of the Standard Model Higgs inflation variants” L.A. Popa JCAP10(2011)025. L.A. Popa TT2. Testing 3+1 and 3+2 neutrino mass models with cosmology and short baseline experiments TT3. Single field inflation or curvaton scenario ?

Pre-cosmological science from PLANCK ( ) 1. Calibration and foregrounds

The epoch of precision astro-particle physics and cosmology 1.”Full” control of systematic effects 2. Unprecedented accuracy in reconstruction of the foregrounds

1. Discovery and prediction of new kind of foreground. Galactic foregrounds Extragalactic foreground Synchrotron Dust emission Free-free Solar system (Kuiper belt objects) QVW PLANCK discoveries Spinning dust, Cold core objects NBI Discovery center,2012

Can KBO foreground resolve the maximum number of problems of CMB anomalies? DC contribution to Working Group “Fundamental physics with PLANCK”

Pre-cosmological science from PLANCK ( ) 2. Astro-particle physics and the Dark Matter

The PLANCK HAZE Most likely we have detected the synchrotron emission from the center of the Milky Way

2. Planck data and templates Planck (Tauber et al. 2010; Planck Collaboration I 2011) is the third generation space mission to measure the anisotropy of the cosmic microwave background (CMB). It observes the sky in nine frequency bands covering 30–857GHz with high sensitivity and angular resolution from 31′ to 5′. The Low Frequency Instrument (LFI; Mandolesi et al. 2010; Bersanelli et al. 2010;Mennella et al. 2011) covers the 30, 44, and 70GHz bands with amplifiers cooled to 20K. The High Frequency Instrument (HFI; Lamarre et al. 2010; Planck HFI Core Team 2011a) covers the 100, 143, 217, 353, 545, and 857GHz bands with bolometers cooled to 0.1K. Polarisation is measured in all but the highest two bands (Leahy et al. 2010; Rosset et al. 2010)

Suggestions include 1.enhanced supernova rates (Biermann et al.2010), a Galactic wind (Crocker & Aharonian 2011), 2.a jet generated by accretion onto the central black hole (Guo & Mathews 2011; Guo et al. 2011), 3.and co-annihilation of dark matter (DM) particles in the Galactic halo (Finkbeiner 2004b; Hooper et al.2007; Lin et al. 2010; Dobler et al. 2011). However, while each of these scenarios can reproduce some of the properties of the haze/bubbles well, none can completely match all of the observed characteristics.

2. Fingerprint of the synchrotron haze in polarization 3. Anomalies of the TT, TE, EE power spectra Hydrogen recombination

TT2. Testing the properties of the DARK MATTER and long living particles in the Universe through ionization history of the cosmic plasma. (DC contribution to FPP ) TT2a. Annihilating Dark Matter and TT-power spectrum. WMAP

Cosmological science from PLANCK ( ) 2. Cosmology, theory of inflation, anomalies

Parity test of the CMB. (DC contribution to FPP). Parity asymmetry of the CMB: Parity violation in Weak interactions P(r)=-r PT(r)=-T(r)-most represented ! From micro- to macro scales Possible explanations: Local violation of Copernican principle Non-trivial topology of space and time Local foreground. Debris of the solar system formation? Effects of systematics and calibration New physics, New sources of emissivity from the space, Improvement of the data sets and creditability of the PLANCK mission.

Two components “gas” of even and odd phases. Separation !! Pearson’s random walk in the space of phases Even Odd

Synergy of Discovery Center CMB-ALICE-T

Early Universe vs. Collisions of Heavy Ions. Synergy of Discovery. DISCOVERY presentation by xx213/5/2012 CMB skyHeavy Ion Collision

Spherical harmonics. Resonance to Vn 22 m=1 m=2 m=3 m=4 V2V2 V4V4 (m=2)-(n=2) ( m=4)-(n=4) L=4,m=0

Conclusion 1. List of hirings (post doc, ph.d. ): since 2010 the DC Planck team has 1 post doc (J.Kim ( ), 1 PhD student (M. Hansen, )+ new hired PhD student A.M. Frejsel ( ). In addition 1 PhD student has association with Discovery Planck team (S. Ramazanov ) and 1 post doc ( Hao Liu, ) 2. Since 2010 we have attended in 34 conferences and schools 3. funds attracted : 6.1 Mkr 4. Summary of papers and citations, talks given : 52 papers, 1609 citations(NASA ADS), 32 talks New proposal- second part of the meeting.