The Atacama Cosmology Telescope

By A. Kosowsky. 2003

358 citations recorded by the source corpus.

Abstract The proposed Atacama Cosmology Telescope (ACT) project is described. This multi-institution collaboration aims to produce arcminute-resolution and micro-Kelvin sensitivity maps of the microwave background temperature over 200 square degree of the sky in three frequency bands. We give a brief overview of the scientific motivations for such a map, followed by a design outline of our 6-m custom telescope, an overview of our proposed bolometer array detector technology, and site considerations and scan strategy. We also describe associated optical and X-ray galaxy cluster surveys.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/deade3a343509e28f8d06ff07d3352178a52c24d

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Citations in the corpus

The X-Ray Luminosity-Mass Relation for Local Clusters of Galaxies (2006, background): “Sunyaev-Zel’dovich (SZ) surveys, based on interferometric (Holder et al. 2000; Loh et al. 2005), or bolometric (Schwan et al. 2003; Kosowsky 2003; Ruhl et al. 2004) approaches, will ultimately extend the reach of the cluster population to z ∼ 3.”
Transition-Edge Sensors (2005, methodology): “It will be used in many instruments including a TES x-ray calorimeter array for NASA’s Constellation-X observatory [30], an x-ray microanalysis array at NIST, SAFIRE [170], a 288-pixel first-light instrument on SOFIA, the Penn Array on the Green Bank Telescope [171], the Millimeter Bolometer Array C”
Indirect dark matter signatures in the cosmic dark ages. I. Generalizing the bound on s-wave dark matter annihilation from Planck results (2015, background): “Exquisitely sensitive measurements of the CMB by a range of experiments (e.g. WMAP [4], SPT [5,6] and ACT [7]), and most recently by the Planck satellite [8], can thus place robust and modelindependent constraints on such energy injections (e.g. [9–22]).”
The Atacama Cosmology Telescope: two-season ACTPol spectra and parameters (2016, methodology): “[29] we mask Fourier modes with |kx| < 90 and |ky| < 50 to remove scansynchronous contamination.”
Characterizing the Cluster Lens Population (2005, background): “Upcoming X-ray (Romer et al. 2001; Ebeling et al. 2001) Sunyaev-Zeldovich (Carlstrom, Holder, & Reese 2002; Kosowsky 2003; Schwan et al. 2003), and opti- 1 Hubble Fellow 2 Department of Astronomy, University of California Berkeley, Berkeley, CA 94720 3 Princeton University Observatory, Princeton,…”
The Atacama Cosmology Telescope: The Receiver and Instrumentation (2010, neutral): “Vertical error estimated from machining tolerances. bErrors are estimated from machining and assembly tolerances. cThe number varies across the array and the “±” indicates the maximum and minimum of the range. and 218GHz bands and over 93% in the 277GHz band (Swetz 2009).”
IMPACT OF CLUSTER PHYSICS ON THE SUNYAEV–ZEL'DOVICH POWER SPECTRUM (2010, methodology): “Experiments such as the South Pole Telescope (Ruhl et al. 2004), the Atacama Cosmology Telescope (Kosowsky 2003) and Planck5 are currently surveying the microwave sky with the goal of identifying clusters via their SZ signature on the cosmic microwave background (CMB), thus constructing large…”
Observational Constraints on Cosmic Reionization (2006, background): “The Atacama 1http://universe.nasa.gov/program/inflation.html Cosmology Telescope (ACT, (Kosowsky(2003))) is a 6 m telescope operating in three frequency bands (145, 225, and 265 GHz) with ≃ 1′ angular resolution.”
MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, background): “2010; Abbott et al. 2005; Vikhlinin et al. 2009; Kosowsky 2003; Staniszewski et al. 2009; Bartlett et al. 2008; Fang & Haiman 2008).”
Clusters of Galaxies in the First Half of the Universe from the IRAC Shallow Survey (2008, background): “Removing this uncertainty is amajor goal of upcoming Sunyaev-Zeldovich cluster surveys such as the SZA (Sunyaev-Zeldovich Array; Loh et al. 2005), AMI (ArcminuteMicrokelvin Imager; Kneissl et al. 2001), ACT (Atacama Cosmology Telescope; Kosowsky 2003), and SPT (South Pole Telescope; Ruhl et al. 2004”