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DACOTA
The Dense Array for COsmological Transi5ons
David DeBoer1, Geoffrey Bower1, Garre> Kea5ng1, Richard Plambeck1, Tzu-‐Ching Chang2, Paul Ho2, Daniel Marrone3, Anthony
Readhead4 1UC Berkeley 2Academia Sinica Ins5tute for Astronomy and Astrophysics 3University of Arizona 4California Ins5tute of Technology
Cosmic Dawn: How was the Milky Way Formed?
Cosmic Dawn: Mul5-‐Pronged Approach
Neutral Hydrogen
Massive Galaxies Ionized Gas
The Mul5tude of Galaxies: Milky Way Building Blocks
Z = 6 Z = 3 Z = 8
CO Luminosity Es5mates
• O-‐O-‐M approach (Carilli 2010) • Compute needed SFR for reioniza5on • Get other rela5onships to go from that to something observable.
• SFR à LIR à LCO
Simple Halo Model (essen5ally same assump5ons)
• Lidz et al 2011 (Ap J 741:70) • Parameterized by the minimum mass halo hos5ng CO luminous galaxies:
Munoz et al 2013
Model for Lower z • Pullen et al 2012 • Models with different CO luminosity assump5ons:
– A : Halo mass to CO luminosity – B : Star forma5on rate to CO luminosity
Evolu5on of Molecular Gas
Z=6
Z=3
OMG
• Phased development of techniques/instrumenta5on for red-‐shieed CO – piggy-‐back to higher z – upper limits -‐> detec5on -‐> sta5s5cs -‐> imaging
• Leveraging the tremendous amount of work done in HI EOR – smaller signal, but easier foregrounds
• Use exis5ng facili5es to start
• What is desired is the spa5al power spectrum, not an image (yet) – k is the 3-‐D wavenumber of the spa5al PS – Interferometric u,v coordinates are just scaled versions of k in the plane of the sky (k )
– On cosmological scales, the frequency axis provides the “line-‐of-‐sight” image coordinate • Its transform is the k coordinate
• What is desired is the spa5al power spectrum, not an image (yet) – k is the 3-‐D wavenumber of the spa5al PS – Interferometric u,v coordinates are just scaled versions of k in the plane of the sky (k )
– On cosmological scales, the frequency axis provides the “line-‐of-‐sight” image coordinate • Its transform is the k coordinate
• What is desired is the spa5al power spectrum, not an image (yet) – k is the 3-‐D wavenumber of the spa5al PS – Interferometric u,v coordinates are just scaled versions of k in the plane of the sky (k )
– On cosmological scales, the frequency axis provides the “line-‐of-‐sight” image coordinate • Its transform is the k coordinate
J=2-‐1
J=1-‐0
For an “imaging” interferometer
CARMA (SZA)
Redundant Interferometer
Redundant Interferometer
Unrotated Version
AMIBA
Sensi5vity & Boost Factor
AMIBA
AMIBA – no ro
ta5on
SZA
DACOTA-‐I Sensi5vity @ z=6
Sensi5vity @ z=3
Measurement
Frequencies
Diameter
Config
Technical Overview
Technical Overview
Technical Overview
Cross-‐correla5on
Cross-‐correla5on
Future
PAPER
PAPER
