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