Post on 08-Feb-2016
description
X-ray Optical microwaveCosmology at KIPAC
The Survey5000 square degrees (overlap with SPT and
VISTA)Five-band (grizY) + VISTA (JHK) photometry to z
= 1.5Shapes and photo-z for 300 million galaxiesOver 250,000 galaxy clusters Well-measured light curves for 2500 Type 1a
supernovae
DES Cosmology … complimentaryprobes in a single catalog …
Galaxy ClustersGravitational LensingLarge Scale Structure and BAOType Ia Supernovae
The Instrument at CTIODECam 570 megapix cameraUpgraded 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, NonGaussianityRoodman: Active Optics System, Image Quality, Galaxy Clusters & LensingSchindler: All Sky CameraWechsler: N-body & Galaxy Simulations, Galaxy Clusters, Dwarf Galaxies and more
Several Rotations available this year: Commissioning First survey season SimulationsWell situated for thesis work over next five years
All-Sky camera on the mountain at CTIO(Lewis/Schindler)
Weak lensing – shape and magnificationGalaxy clusters – mass calibrations and distributionsTheory 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) swa@stanford.edu
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) swa@stanford.edu
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