Simons Array

Simons Array
Name	Simons Array
Organization	Simons Foundation
Established	2013
Wavelength	Microwave
Diameter	3.5 m (per receiver)

Simons Array The Simons Array is an experimental array of cosmic microwave background receivers designed to measure polarization anisotropies with high sensitivity. It builds on prior instruments and collaborations to probe cosmological parameters, inflationary physics, and large-scale structure through precision observations of the Cosmic Microwave Background. The project involves multinational teams from academic institutions, observatories, and funding bodies focused on observational cosmology.

Overview

The Simons Array evolved from predecessors including POLARBEAR, BICEP programs, and the Atacama Cosmology Telescope community, situating itself within a lineage of experiments such as South Pole Telescope, Planck (spacecraft), and COBE. Its design mirrors approaches used by missions like WMAP and instruments developed at facilities such as Caltech, Harvard–Smithsonian Center for Astrophysics, Princeton University, University of California, Berkeley, and Stanford University. The collaboration engages with science priorities articulated by panels including the NAS Decadal Survey and partnerships with projects like CMB-S4 and LiteBIRD.

Instrumentation and Design

Each receiver in the Array integrates detector technologies similar to those used in Transition-edge sensor arrays and Kinetic inductance detector research pioneered at institutions like NIST, Jet Propulsion Laboratory, and Argonne National Laboratory. Optical elements and cryogenic systems reflect engineering practices from National Radio Astronomy Observatory facilities and designs informed by experiments at the South Pole Telescope and Atacama Large Millimeter/submillimeter Array. Frequency bands span ranges employed in studies by Planck (spacecraft), with polarization modulators and anti-reflection coatings drawing on heritage from BICEP2 and Keck Array implementations. Readout electronics utilize multiplexing techniques developed in collaboration with groups at Massachusetts Institute of Technology and Brookhaven National Laboratory.

Observing Sites and Deployment

The Array is deployed at high, dry sites with heritage from projects at the Atacama Desert and Chajnantor Plateau to take advantage of atmospheric transparency used by observatories like ALMA and APEX. Logistics and operations coordinate with regional agencies including the Comisión Nacional de Investigación Científica y Tecnológica and institutions such as University of Tokyo groups that have participated in Antarctic and Andean observing campaigns. Deployment strategies echo lessons from South Pole Station campaigns and mount designs common to arrays operated by European Southern Observatory and NRAO.

Science Goals and Results

Science objectives target measurement of primordial B-mode polarization relevant to inflationary models proposed by theorists associated with universities like Harvard University, MIT, and University of Cambridge. The Array’s sensitivity aids constraints on parameters including the tensor-to-scalar ratio discussed in analyses by teams at Princeton University and University of Chicago, and helps map lensing potential in synergy with galaxy surveys like Sloan Digital Sky Survey and Dark Energy Survey. Results complement findings from Planck (spacecraft), refine foreground separation techniques developed alongside WMAP analyses, and contribute to publications in journals associated with American Physical Society and Institute of Physics communities.

Data Processing and Analysis

Data pipelines build on frameworks used by POLARBEAR and BICEP teams, employing map-making algorithms and power-spectrum estimators similar to methods developed at NASA Goddard Space Flight Center and Los Alamos National Laboratory. Foreground mitigation leverages component-separation approaches pioneered in Planck (spacecraft) data releases and incorporates cross-correlation techniques with catalogs from Pan-STARRS and Two Micron All-Sky Survey. Computational resources and software engineering are supported by centers like NERSC and XSEDE, with visualization and statistical inference following practices from groups at Brown University and University of California, San Diego.

Collaborations and Funding

The Simons Array collaboration includes researchers from institutions such as University of Minnesota, Carnegie Mellon University, University of British Columbia, University of Tokyo, and University of California, San Diego, and coordinates with international partners from laboratories like RIKEN and CERN-affiliated groups for instrumentation expertise. Funding streams involve private foundations including the Simons Foundation and national agencies such as National Science Foundation, Japan Society for the Promotion of Science, and competitive grants overseen by organizations like DOE and national research councils in partner countries. Collaborative governance follows models used by consortia behind Atacama Cosmology Telescope and South Pole Telescope programs.

Category:Cosmic microwave background experiments