x-ray optical microwave cosmology at kipac. the survey 5000 square degrees (overlap with spt and...
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X-ray Optical microwaveCosmology at KIPAC
The Survey
5000 square degrees (overlap with SPT and VISTA)
Five-band (grizY) + VISTA (JHK) photometry to z = 1.5
Shapes and photo-z for 300 million galaxies
Over 250,000 galaxy clusters
Well-measured light curves for 2500 Type 1a supernovae
DES Cosmology … complimentaryprobes in a single catalog …
Galaxy Clusters
Gravitational Lensing
Large Scale Structure and BAO
Type Ia Supernovae
The Instrument at CTIO
DECam 570 megapix camera
Upgraded Blanco 4m telescope
Dark Energy Survey (DES)
4
Fornax Cluster
DES First light
DES First light
NGC1365 in Fornax
DES First Light
47 Tuc (Globular Cluster)
Giga-parsec N-BodySimulation
SDSS Galaxy Data
DES simulated galaxy catalog …
The “Stanford Mocks”(Wechsler)
Cosmology with Galaxy ClustersCluster finding and characterizationCalibrations of mass proxiesDark matter halos and mass functionsSpatial distributions and primordial non-Gaussianity
Mock Galaxy Cluster
Top: cluster finder result
Bottom: line-of-sight complexity in mass determination
DES at KIPAC Faculty MembersBurke: Photometric Calibrations, Galaxy Clusters,
NonGaussianity
Roodman: Active Optics System, Image Quality, Galaxy
Clusters & Lensing
Schindler: All Sky Camera
Wechsler: N-body & Galaxy Simulations, Galaxy Clusters,
Dwarf Galaxies and more
Several Rotations available this year:
Commissioning
First survey season
Simulations
Well situated for thesis work over next five years
All-Sky camera on the mountain at CTIO(Lewis/Schindler)
Weak lensing – shape and magnification
Galaxy clusters – mass calibrations and distributions
Theory and simulation – galaxies and clusters
• will image half the sky every 3 days (first light 2020)
• lots of diverse applications: dark matter, dark energy, milky way structure, galaxy formation, solar system, optical transients
• Kahn: project lead at SLAC, PI for LSST camera
• Burke, Schindler, Burchat, Wechsler, Roodman, Allen
• lensing (Kahn, Burchat)
• hardware (Kahn, Roodman, Schindler)
• LSS, clusters (Allen), galaxies
• LSST Dark Energy Science Collaboration
Simionescu et al. 2011, Science 331, 1576
Project 1: the `virialization’ of galaxy clusters
Allen group: (xoc.stanford.edu) [email protected]
Understanding the formation of the largest-scale structures `as it happens’ and their equilibrium configurations (X-ray, optical, mm, radio) astrophysics and cosmology.
The Perseus Cluster (z=0.02)
Using rare collisions of massive galaxy clusters (X-ray, gravitational lensing, optical, mm) to probe astrophysics and the nature of dark matter. Using statistical measurements of clusters to probe dark energy (Allen et al 2011, ARA&A, 49, 409).
Project 2: cosmic collisions and the dark universe
Allen group: (xoc.stanford.edu) [email protected]
MACSJ0025.4-1222 (z=0.59)
Red: Baryons (X-ray emission)Blue: Dark Matter (lensing)
Roger Blandford - Cosmology
• Gravitational lensing in an inhomogeneous universe– Using large numerical simulations to learn how
to perform precision cosmological measurements
• Behavior of stars as they orbit massive black holes– There could be systems of stars orbiting holes
like planets orbiting stars
• Assembly of massive black holes– What are the physical processes that govern the
evolution of black hole mass and spin in the nuclei of galaxies and how do they relate to observations
• Heating of intergalactic gas– It looks like rich galaxy clusters are surrounded
by strong shocks. Are these the sources of ultra high energy cosmic rays?
Cosmic Microwave Background Polarization
E B
Kuo Group: BICEP1/BICEP2/Keck/POLAR-1/POLAR Array @ South Pole
POLAR Array
~ 1 rotation student
50detectors
250detectors
1,000detectors
2,000detectors
20,000detectors
POLAR-1
Sarah Church’s Group (1-2 rotators F, W, Sp)A Range of Cosmological Science with Radio Telescopes:
• Inflation through polarization of the Cosmic Microwave Background radiation (QUIET II).
• Epoch of reionization through measurements of highly redshifted CO lines (large-format radio interferometer).
• Star formation history through molecular gas studies (Argus at the Green Bank Telescope).
• Rotators participate in design tasks, prototype fabrication and testing.
• In the longer term, thesis projects will include deployment, data taking and analysis.
• Visit our lab – Varian 203/204 or stop by my office – Varian 344
QUIET Phase I
Credit: NASA, ESA, and the Hubble Heritage Team (STScI/AURA)-ESA/Hubble Collaboration
Argus
Star formation in colliding galaxies
QUIET I limits to B-modes