21CMA 21 Centimeter Array a.k.a. PAST. Reionization 21cm: hyperfine transition of neutral Hydrogen.

Slides:

Advertisements

Similar presentations

21cm cosmology T. Chang, UP, J. Peterson, P. McDonald PRL 100, (2008) UP, L. Staveley-Smith, J. Peterson, T. Chang, MNRAS, 394, 6 (2009)

Advertisements

MeerKAT Large Survey Projects SAAO Board, Roy Booth (SA SKA Project)

21 cm Cosmology Jeff Peterson, CMU -Existing telescopes and data -Intensity Mapping -Fixed Cylinders.

Cosmology using 21 cm emission Jeff Peterson, CMU Talk 1…Update on early ionization telescopes (LOFAR, PAST, GMRT) Talk 2…Proposed Redshift survey.

Dark Energy BAO Intensity Mapping T. Chang, UP, J. Peterson, P. McDonald PRL 100, (March 5, 2008) UP, L. Staveley-Smith, J. Peterson, T. Chang arXiv:

The Cylinder Radio Telescope: Observing the CMB Paul A. Fleiner Ph 70 Popular Presentation May 10, 2011.

Hydrogen 21cm Cosmology Tzu-Ching Chang (ASIAA)

ASTR Fall Semester Joel E. Tohline, Alumni Professor Office: 247 Nicholson Hall [Slides from Lecture19]

Probing the field of Radio Astronomy with the SKA and the Hartebeesthoek Radio Observatory: An Engineer’s perspective Sunelle Otto Hartebeesthoek Radio.

Introduction to Radio Astronomy Updated February 2009.

Non-linear matter power spectrum to 1% accuracy between dynamical dark energy models Matt Francis University of Sydney Geraint Lewis (University of Sydney)

The Dark Age… before the stars, beyond the galaxies…

The Green Bank Telescope a powerful instrument for enhancing ALMA science Unblocked Aperture Low sidelobes gives high dynamic range Resistance to Interference.

Lecture 2: Observational constraints on dark energy Shinji Tsujikawa (Tokyo University of Science)

Nikolaos Nikoloudakis Friday lunch talk 12/6/09 Supported by a Marie Curie Early Stage Training Fellowship.

PRE-SUSY Karlsruhe July 2007 Rocky Kolb The University of Chicago Cosmology 101 Rocky I : The Universe Observed Rocky II :Dark Matter Rocky III :Dark Energy.

Galaxies What is a galaxy? How many stars are there in an average galaxy? About how many galaxies are there in the universe? What is the name of our galaxy?

Cosmology with the 21 cm Transition Steve Furlanetto Yale University September 25, 2006 Steve Furlanetto Yale University September 25, 2006.

Satellite observation systems and reference systems (ae4-e01) Signal Propagation E. Schrama.

The Structure Formation Cookbook 1. Initial Conditions: A Theory for the Origin of Density Perturbations in the Early Universe Primordial Inflation: initial.

A Primer on SZ Surveys Gil Holder Institute for Advanced Study.

Large Scale Simulations of Reionization Garrelt Mellema Stockholm Observatory Collaborators: Ilian Iliev, Paul Shapiro, Marcelo Alvarez, Ue-Li Pen, Hugh.

What is the Dark Matter? What about “ordinary” non-luminous matter (basically, made from proton, neutrons and electrons)? “Dead stars” (White Dwarfs,

Title people CHIME: the Canadian Hydrogen Intensity Mapping Experiment. Mark Halpern Kris Sigurdson Sigi Stiemer Tom Landecker Jeff Peterson Dick Bond.

VLBI in Africa Michael Bietenholz Hartebeesthoek Radio Observatory.

“First Light” From New Probes of the Dark Ages and Reionization Judd D. Bowman (Caltech) Hubble Fellows Symposium 2008.

The Swedish contribution to EU-HOU: A Hands-On Radio Astronomy exercise Mapping the Galaxy using hydrogen Daniel Johansson Christer Andersson.

Polarization-assisted WMAP-NVSS Cross Correlation Collaborators: K-W Ng(IoP, AS) Ue-Li Pen (CITA) Guo Chin Liu (ASIAA)

The Square Kilometre Array Department of Astronomy and Atmospheric Sciences, Kyungpook National University 김경묵, 박진태, 방태양, 신지혜, 조창현, 정수진, 현화수 Survey Science.

Random Media in Radio Astronomy Atmospherepath length ~ 6 Km Ionospherepath length ~100 Km Interstellar Plasma path length ~ pc (3 x Km)

Yi Mao, MIT Collaborators: Max Tegmark, Alan Guth, Matias Zaldarriaga, Matt McQuinn, Oliver Zahn, Tom Faulkner, Ted Bunn, Serkan Cabi Constraining cosmological.

Modern State of Cosmology V.N. Lukash Astro Space Centre of Lebedev Physics Institute Cherenkov Conference-2004.

Title people CHIME: the Canadian Hydrogen Intensity Mapping Experiment. Mark Halpern Kris Sigurdson Sigi Stiemer Tom Landecker Jeff Peterson Dick Bond.

Galaxies Nimisha G. Kantharia National Centre for Radio Astrophysics Tata Institute of FundamentalResearch Pune.

1 100 SKA stations (2020 ) Projets avec SKA. 2 Telescope Project (~2020) for a giant radiotelescope in the centimetre-metre range one square kilometre.

Charling Tao, NAOC August 2006 Dark Energy Constraints from BA0 Wang Yun astro/ph

Andreas Horneffer for the LOPES Collaboration Detecting Radio Pulses from Air Showers with LOPES.

Constraints on Dark Energy from CMB Eiichiro Komatsu University of Texas at Austin Dark Energy February 27, 2006.

21 cm Reionization Forecast and Search at GMRT

Low Frequency Background and Cosmology Xuelei Chen National Astronomical Observatories Kashigar, September 10th 2005.

THE MURCHISON WIDEFIELD ARRAY: FROM COMMISSIONING TO OBSERVING D. Oberoi 1,2, I. H. Cairns 3, L. D. Matthews 2 and L. Benkevitch 2 on behalf of the MWA.

Cosmology. We can simulate how a nearly smooth distribution of dark matter turns into our lumpy, grainy Universe with its hierarchy of structures -

Anadian ydrogen ntensity apping xperiment CHIMECHIME CHIMECHIME WiggleZ Dark Ages Stars 13.7Gy CMB Big Bang Reionization 1100 z∞ SDSS 7Gy CHIME.

Asymmetric Planetary Nebulae IV La Palma, Canary Islands Water Fountains in Pre-Planetary Nebulae Mark Claussen NRAO June 19, 2007 Hancock, New Hampshire.

Michael Doran Institute for Theoretical Physics Universität Heidelberg Time Evolution of Dark Energy (if any …)

RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing, August RadioAstron space VLBI mission: early results. XXVIII GA IAU, Beijing,

The Distributions of Baryons in the Universe and the Warm Hot Intergalactic Medium Baryonic budget at z=0 Overall thermal timeline of baryons from z=1000.

The Mission  Explore the Dark Ages through the neutral hydrogen distribution  Constrain the populations of the first stars and first black holes.  Measure.

The Australia Telescope National Facility Ray Norris CSIRO ATNF.

23 Sep The Feasibility of Constraining Dark Energy Using LAMOST Redshift Survey L.Sun Peking Univ./ CPPM.

1 Dalit Engelhardt Boston University Summer 2006 REU Observational Cosmology Advisor: Prof. Peter Timbie University of Wisconsin-Madison.

ASKAP Update David DeBoer ASKAP Project Director 26 May 2010.

Potential of a Low Frequency Array (LOFAR) for Ionospheric and Solar Observations ABSTRACT: The Low Frequency Array (LOFAR) is a proposed large radio telescope.

Suijian Xue ( 薛随建 ) National Astronomical Observatories, Chinese Academy of Sciences JEJU, Korea Regional Report Astronomical Activities Update.

Astrophysics from the Moon in the Radio Band Gianfranco Brunetti INAF - IRA, Bologna.

Remote Quadrupole Measurements from Reionization Gil Holder Collaborators: Jon Dudley; Alex van Engelen (McGill) Ilian Iliev (CITA/Zurich); Olivier Dore.

Universe Tenth Edition Chapter 25 Cosmology: The Origin and Evolution of the Universe Roger Freedman Robert Geller William Kaufmann III.

Brenna Flaugher for the DES Collaboration; DPF Meeting August 27, 2004 Riverside,CA Fermilab, U Illinois, U Chicago, LBNL, CTIO/NOAO 1 Dark Energy and.

Probing Dark Energy with Cosmological Observations Fan, Zuhui ( 范祖辉 ) Dept. of Astronomy Peking University.

The distant Universe and something about gravitational waves.

Why do we need interferometry? Measuring the gas distribution and rotation in disk galaxies: radio observations with interferometer arrays and aperture.

A Proposed Collaboration Between LIGO-Virgo and Swift to Improve the Chances to Detect Gravitational Waves from Core Collapse Supernovae Kiranjyot (Jasmine)

The ARA concept and history construction activities Future plans The ARA concept and history construction activities Future plans Kara.

32nd International Cosmic Ray Conference August 2011, Beijing China First detection of extensive air showers by the TREND self-triggering radio experiment.

Development of the 21CMA radio-detection array (Xinjiang/China) for the observation of UHE neutrinos showers Didier Charrier1, Pascal Lautridou1, Olivier.

Asantha Cooray (Caltech) Based on Seto & Cooray, PRL, astro-ph/

The Progress of Seshan VGOS Station Construction

The arrival of Gravitational Waves and the EEE network:

A Search for water masers in High-redshift un-beamed AGNs: T. Ghosh, S

Graduate Course: Cosmology

Presentation transcript:

21CMA 21 Centimeter Array a.k.a. PAST

Reionization 21cm: hyperfine transition of neutral Hydrogen

21CMA a.k.a. PAST Basic ideas: an experiment, not an observatory use cheap, off-the -shelf technology (i.e. TV+PC) simple design (looking at NCP) choose site with minimal EM interference to become operational before MWA/LOFAR Xiang-Ping Wu (NAOC) Ue-Li Pen (CITA) Jeff Peterson (Carnegie)

VLBI Map of 21CMA site 21CMA

E N Urumuqi Ulastai

Log-Periodic antenna

20m A pod (127 antenna)

correlator arrayLNAfilteramplifier Optical transmitter Opt. fibre Optical receiver ADC 21CMA data collection system

Basic Design of 21CMRA At z=9, 10 comoving Mpc  ~ 0.6 MHz,  ~ 3.6 arcmin frequency range MHz (6.1<z<19.3) baseline: 2 km, (at 140 MHz, 3.6 arcmin) Collecting Area 10 4 m 2 A/L 2 ~ 0.01

Schedule & Status summer 2003 Ue-Li, Jeff, Xiang-Ping discussed the idea autumn 2003 site search began, Ulastai chosen March antennae prototype, first image August 2004 array design finished January 2005 batch I (first 20 pods) constructed summer 2005 batch II (60 pods) construction, data collecting electronics installation January 2006 fully operational Total cost estimate: M yuan, now borrowing from other groups in NAOC, will apply a grant, please support!

January 1, 2005

First skymap (dirty) 3C CR390.3 NCP 3CR061.1

Dark Energy? AP test power spectrum measurement lensing...

Discussion on dark energy observation

Dark Energy? Observation Data Theoretical Assumptions General RelativityCosmo Principle Model IModel II Model III

Ways to measure dark energy Gravitational test: luminosity distance angular diameter distance growth of perturbation solar system & beyond Non-Gravitational test: variation of constants dark energy interaction supernovae & GRB gravitational lensing cluster large scale structure CMB 21cm gravitational wave micro-gravity, solar system & lab

What can we do in China Existing projects: LAMOST, 21CMA New Projects: ?