10 meter South Pole Telescope Low noise, precision telescope 20 um rms surface accuracy 1 arc second pointing 1.0 arcminute at 2 mm ‘chop’ entire telescope.

Slides:

Advertisements

Similar presentations

Cosmology with the South Pole Telescope Zak Staniszewski (Case)

Advertisements

The South Pole Telescope Galaxy Cluster Survey Joe Mohr Ludwig-Maximilians University Max Planck Insitute for Extraterrestrial Physics Munich SPT BCS e-ROSITA.

Astronomy & Astrophysics in Antarctic 2012 AAAC 11 May 2012 Scott Borg Division of Antarctic Sciences Office of Polar Programs National Science Foundation.

K. Ganga – CMB Science and Observations 1 Rencontres du Vietnam /08 The QuaD CMB Polarization Experiment K. Ganga APC.

Dark Energy Survey The DES Collaboration Josh Frieman, Ofer Lahav, JW.

Cluster Cosmology at LPPC Illuminating Dark Energy with BCS and PISCO F. William High 2 nd Year Grad Student Harvard Univ Dept of Physics Monday, 21 August.

The National Science Foundation The Dark Energy Survey J. Frieman, M. Becker, J. Carlstrom, M. Gladders, W. Hu, R. Kessler, B. Koester, A. Kravtsov, for.

Characterizing Millimeter Wavelength Atmospheric Fluctuations at the South Pole William L. Holzapfel (UCB) In collaboration with: R. Shane Bussmann (UCB)

Universe in a box: simulating formation of cosmic structures Andrey Kravtsov Department of Astronomy & Astrophysics Center for Cosmological Physics (CfCP)

1 ACT  Atacama Cosmology Telescope  Funded by NSF  Will measure CMB fluctuations on small angular scales  Probe the primordial power spectrum and the.

University of California, Berkeley

K.S. Dawson, W.L. Holzapfel, E.D. Reese University of California at Berkeley, Berkeley, CA J.E. Carlstrom, S.J. LaRoque, D. Nagai University of Chicago,

BICEP: B ackground I maging of C osmic E xtragalactic P olarization “The Muscle Behind Curls” Jamie Bock Hien Nguyen Caltech/JPL Andrew Lange Brian Keating.

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

CMB polarisation results from QUIET

Advanced Cosmology Bolometer Array Receiver (ACBAR) on Viper Jeff Peterson - CMU –Ravinder Bhatia (Caltech) –Jamie Bock (JPL) –Andrew Lange (Caltech) –Peter.

Einstein Polarization Interferometer for Cosmology (EPIC) Peter Timbie University of Wisconsin - Madison Beyond Einstein SLAC May

Probing The Dark Universe Josh Frieman Fermilab & The University of Chicago Link to Learn, May, 2011.

Statistics of the Weak-lensing Convergence Field Sheng Wang Brookhaven National Laboratory Columbia University Collaborators: Zoltán Haiman, Morgan May,

Thoughts on Ground-based lensing measurements Chao-Lin Kuo Stanford/SLAC KIPAC.

The Atacama B-mode Search: A TES-Based CMB Polarization Instrument CMBpol Workshop, Chicago July 2, 2009 Joe Fowler Princeton University.

Craig Lawrie Advisor: Dr. John Ruhl Abstract Software is developed for the detection of galaxy clusters in data gathered by the South Pole Telescope (SPT).

August '04 - Joe Mohr Blanco Instrument Review Presentations to Blanco Instrument Review Panel Intro and Science 1 Mohr Intro and Science 1 Mohr Science.

Preliminary Results from the SZA Amber Miller Columbia University Photo: Leitch New Views of the Universe Kavli Inaugural Sypmosium Dec 11th, Chicago.

PHY306 1 Modern cosmology 4: The cosmic microwave background Expectations Experiments: from COBE to Planck  COBE  ground-based experiments  WMAP  Planck.

Early times CMB.

● DES Galaxy Cluster Mock Catalogs – Local cluster luminosity function (LF), luminosity-mass, and number-mass relations (within R 200 virial region) from.

The Atacama Cosmology Telescope New Views of the Universe December 11, 2005 Joe Fowler Princeton University.

Search for B-modes in CMB Polarization  QUIET and other experiments Osamu Tajima (KEK) The QUIET Collaboration Ultimate High Energy Physics QUIET collaboration.

The APEX Sunyaev Zel'dovich Experiment Observations Matt Dobbs McGill University On behalf of the APEX-SZ collaboration.

Astronomy & Astrophysics Advisory Committee (AAAC) May 11, 2006 Vladimir Papitashvili Antarctic Sciences Section Office of Polar Programs National Science.

Cosmology with Cluster Surveys Subha Majumdar Canadian Institute of Theoretical Astrophysics Toronto along with Joe Mohr, Martin White & Jose Diego International.

The KAT/SKA project and Related Research Catherine Cress (UKZN/KAT/UWC)

June 27, 2008Scott Dodelson1 Numerical Cosmology Argonne-Fermilab-University of Chicago Collaboration Meeting.

Astronomy and Astrophysics in Antarctica Current U.S. Projects and Challenges Scott Borg, Director, Division of Antarctic Sciences Vladimir Papitashvili,

SUNYAEV-ZELDOVICH EFFECT. OUTLINE  What is SZE  What Can we learn from SZE  SZE Cluster Surveys  Experimental Issues  SZ Surveys are coming: What.

Using the Sunyaev-Zel'dovich Array in Detailed Studies of Galaxy Clusters 3 rd Biennial Leopoldina Conference Dark Energy 9 th October 2008 Tony Mroczkowski.

Jim Annis for the DES Collaboration BIRP Meeting August 12, 2004 Tucson Design of the Dark Energy Survey James Annis.

Cosmology with Gravitaional Lensing

Sept. 18, 2008SLUO 2008 Annual Meeting CMB Polarization Measurements Sarah Church John Fox, Chao-Lin Kuo, Sami Tantawi, Dan Van Winkle KIPAC/Stanford Physics/SLAC.

1 QUIET The Search for B-Mode Polarization in the Cosmic Microwave Background Using Coherent HEMT Detectors A Proposed New Initiative for Fermilab April.

Chao-Lin Kuo Stanford Physics/SLAC

High Resolution Measurements of CMB Anisotropies with ACBAR U.C. Berkeley: W.L. Holzapfel (co-PI) M.D. Daub M. Lueker Case-Western: J. Ruhl (co-PI) J.

Array for Microwave Background Anisotropy AMiBA SZ Science AMiBA Team NTU Physics Figure 4. Simulated AMiBA deep surveys of a 1deg 2 field (no primary.

Complementary Probes of Dark Energy Josh Frieman Snowmass 2001.

DES Collaboration Meeting – Dec. 11, Dark Energy Survey Science Proposal Josh Frieman

1 1 Dark Energy with SNAP and other Next Generation Probes Eric Linder Berkeley Lab.

Lec2 Mapping Structure (Frieman)

Mechanics Physics12 Mass & weight Mechanics Physics12 Mass & weight.

FIRST LIGHT A selection of future facilities relevant to the formation and evolution of galaxies Wavelength Sensitivity Spatial resolution.

CMB, lensing, and non-Gaussianities

150GHz 100GHz 220GHz Galactic Latitude (Deg) A Millimeter Wave Galactic Plane Survey with the BICEP Polarimeter Evan Bierman (U.C. San Diego) and C. Darren.

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.

Mapping our Universe for Precision Cosmology Max Tegmark, MIT.

APEX stuff – 4 Feb 2003 Martin White Department of Physics Department of Astronomy UC Berkeley Lawrence Berkeley National Lab.

CTIO Camera Mtg - Dec ‘03 Studies of Dark Energy with Galaxy Clusters Joe Mohr Department of Astronomy Department of Physics University of Illinois.

Cheng Zhao Supervisor: Charling Tao

BICEP2 Results & Its Implication on inflation models and Cosmology Seokcheon Lee 48 th Workshop on Gravitation & NR May. 16 th

Jochen Weller Decrypting the Universe Edinburgh, October, 2007 未来の暗黒エネルギー実験の相補性.

Fingerprints in the CMB from Reionization Gil Holder.

Wilkinson Microwave Anisotropy Probe (WMAP) By Susan Creager April 20, 2006.

Towards the first detection using SPT polarisation

April 21, 2016, 7:30pm Hanson Hall, Room 102, Augustana College

The Cosmic Background Imager

Miller Lab - Columbia Currently in the lab…

A 10-m Diameter Submillimeter-wave Telescope for the South Pole

The Instrument cm Cassegrain antennas 6-meter platform

A Measurement of CMB Polarization with QUaD

A Submillimeter and CMBR Observatory for the South Pole

Joe Mohr A 6m Telescope for the South Pole: a Status Report Florence CMB Coordination Meeting, 2018 Joe Mohr

Presentation transcript:

10 meter South Pole Telescope Low noise, precision telescope 20 um rms surface accuracy 1 arc second pointing 1.0 arcminute at 2 mm ‘chop’ entire telescope 3 levels of shielding Key Observations sq deg SZE survey - deep CMB anisotropy fields - deep CMB Polarization fields 1000 Element Bolometer Array - 3 to 4 interchangeable bands (90) 150, 250 & 270 GHz - cooled to 250mK by closed cycle cooler – no cryogens Science goals - investigate properties of the ‘Dark Energy’ that pervades the universe and accelerates its expansion - constrain the mass of the neutrino - search for the signature of primordial Gravitational waves and test models for the origin of the universe

SPT Collaborators Principals: John Carlstrom (U. Chicago) Bill Holzapfel (UCB) Adrian Lee (UCB) Erik Leitch (Chicago) Stephan Meyer (Chicago) Joe Mohr (UIUC) Steve Padin (Chicago) Clem Pryke (Chicago) John Ruhl (Case-Western) Helmuth Spieler (UCB) Tony Stark (CfA) With help from: Wayne Hu (Chicago) Andrey Kravtsov (Chicago) Josh Frieman (Chicago) Martin White (UCB) Postdocs: Tom Crawford (Chicago) Sherry Cho (UCB) Matt Dobbs (UCB) Nils Halverson (UCB) Subharbrata Majumdar (UIUC) Marcus Runyan (KICP Fellow) Students: Chris Greer, Mathew Sharp, Sarah Hansen (Chicago) Po Kin Leung & Yen-Ting Lin (UIUC) Jon Leong & Z. Staniszewski (Case) Martin Lueker, Tom Plagge, Trevor Lanting, Jared Mehl, Dan Schwan, Erik Shirkoff (UCB) KICP NSF – OPP Raytheon PSC

Predicted dN/dz for SPT 4000 sq degree SZE Cluster Survey ~25,000 clusters!

SPT Polarization Simulations Simulations by Tom Crawford

SPT Impact on SP Logistics Timeline: –FY05:Foundation –FY06:Infrastructure and Shields –FY07: Telescope and start observations –FY08: Polarimeter deployment? FY08 – FY20 tbd Weight: –Foundation and Shields: >750klbs; Telescope: 450 klbs Power: –170 kW peak, 60 kW average observing South Pole Population: –Summer: 4-6 steady state (+12 for FY07 deployment) –Winter: 2 dedicated winterovers DSL Space: –SPT RX lab space is about 25% of 1 st floor DSL 1 st floor filled by SPT RX room, machine shop, IT Room, building mechanics, power distribution, mini-cryofacility –SPT computer/control is about 25% of 2 nd floor much of 2 nd floor still unassigned Data transmission: –30 GBytes/day after compression