The 10 Meter South Pole Telescope

By J. Carlstrom, P. Ade, K. Aird, B. Benson, L. Bleem, S. Busetti, C. Chang, E. Chauvin, Hsiao-mei Cho, T. Crawford and 34 more. 2009

591 citations recorded by the source corpus.

The South Pole Telescope (SPT) is a 10 m diameter, wide-field, offset Gregorian telescope with a 966 pixel, multicolor, millimeter-wave, bolometer camera. It is located at the Amundsen-Scott South Pole station in Antarctica. The design of the SPT emphasizes careful control of spillover and scattering, to minimize noise and false signals due to ground pickup. The key initial project is a large-area survey at wavelengths of 3, 2, and 1.3 mm, to detect clusters of galaxies via the Sunyaev-Zel’dovich effect and to measure the small-scale angular power spectrum of the cosmic microwave background (CMB). The data will be used to characterize the primordial matter power spectrum and to place constraints on the equation of state of dark energy. A second-generation camera will measure the polarization of the CMB, potentially leading to constraints on the neutrino mass and the energy scale of inflation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/71916f909978ac031a22f9003946c2d561f9ca04

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Citations in the corpus

Planck intermediate results: V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect (2012, unknown): “In parallel, SZ observations with instruments such as the Sunyaev-Zeldovich Array (SZA, Muchovej et al. 2007), the South Pole Telescope (SPT, Carlstrom et al. 2011), the Atacama Cosmology Telescope (ACT, Swetz et al. 2011), and Planck (Tauber et al. 2010 ) 1 have recently started to deliver on the…”
GALAXY CLUSTERS DISCOVERED VIA THE SUNYAEV–ZEL'DOVICH EFFECT IN THE 2500-SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “The SPT (Carlstrom et al. 2011) is a 10 m diameter telescope located at the National Science Foundation AmundsenScott South Pole station in Antarctica.”
COSMOLOGICAL CONSTRAINTS FROM SUNYAEV–ZEL'DOVICH-SELECTED CLUSTERS WITH X-RAY OBSERVATIONS IN THE FIRST 178 deg2 OF THE SOUTH POLE TELESCOPE SURVEY (2011, background): “Details of the telescope and receiver can be found in Padin et al. (2008), Carlstrom et al. (2011), and Dobbs et al. (2012).”
Dusty Star Forming Galaxies at High Redshift (2014, methodology): “South Pole Telescope [SPT], 2008–present The South Pole Telescope is a 10mmillimeter wave telescope located at the geographic south pole in Antarctica designed to detect low-contrast signals like anisotropies in the cosmicmicrowave background (Carlstrom et al., 2011).”
A SUNYAEV–ZEL'DOVICH-SELECTED SAMPLE OF THE MOST MASSIVE GALAXY CLUSTERS IN THE 2500 deg2 SOUTH POLE TELESCOPE SURVEY (2011, background): “Single observations of fields of this size can be completed in an hour or two, allowing a regular schedule of interleaved calibrations (see S09 and Carlstrom et al. (2011) for details).”
The Dark Energy Survey Image Processing Pipeline (2018, background): “2), overlapping SDSS Stripe 82 along the celestial equator and ∼ 2500deg2 of South Pole Telescope footprint (Carlstrom et al. 2011).”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, background): “The South Pole Telescope (SPT, Carlstrom et al. 2011) and the Atacama Cosmology Telescope (ACT, Fowler et al. 2007) have sufficient sensitivity, angular resolution, and frequency coverage to measure the power spectrum of the thermal SZ (tSZ) effect and to place increasingly strong upper limits on…”
ALMA REDSHIFTS OF MILLIMETER-SELECTED GALAXIES FROM THE SPT SURVEY: THE REDSHIFT DISTRIBUTION OF DUSTY STAR-FORMING GALAXIES (2013, methodology): “This has changed dramatically over the past years with the advent of large area surveys from Herschel (specifically H-ATLAS and HerMES Eales et al. 2010; Oliver et al. 2010) and the South Pole Telescope (SPT-SZ, Carlstrom et al. 2011).”
A MEASUREMENT OF GRAVITATIONAL LENSING OF THE MICROWAVE BACKGROUND USING SOUTH POLE TELESCOPE DATA (2012, background): “The telescope and receiver are discussed in more detail in Ruhl et al. (2004), Padin et al. (2008), and Carlstrom et al. (2011).”
Elucidating ΛCDM: Impact of Baryon Acoustic Oscillation Measurements on the Hubble Constant Discrepancy (2017, background): “…Telescope polarization-sensitive receiver (ACTPol; Thornton et al. 2016; Louis et al. 2017; Sherwin et al. 2016) two-season survey, covering 548 deg2, and the 2500 deg2 South Pole Telescope Sunyaev-Zel’dovich survey (SPT-SZ; Carlstrom et al. 2011; Story et al. 2013; van Engelen et al. 2012).”
Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich cluster counts (2013, methodology): “The Planck cluster sample is complementary to those from observations using the South Pole Telescope (SPT, Carlstrom et al. 2011) and the Atacama Cosmology Telescope (ACT, Swetz et al. 2011), whose teams recently published the first large samples of SZ-selected clusters (Reichardt et al. 2013;…”
GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, background): “…prominence with the launch of the Herschel Space Observatory (Herschel; Pilbratt et al. 2010) and the advent of the South Pole Telescope (SPT; Carlstrom et al. 2011) and the Atacama Cosmology Telescope (Swetz et al. 2011): wide-field surveys at submillimeter (submm) and millimeter (mm)…”
Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Cosmological implications from two decades of spectroscopic surveys at the Apache Point Observatory (2020, methodology): “This came through dedicated CMB experiments including ACT (Fowler et al. 2007), SPT (Carlstrom et al. 2011) and the Wilkinson Microwave Anisotropy Probe (WMAP; Bennett et al. 2013).”
ARCONS: A 2024 Pixel Optical through Near-IR Cryogenic Imaging Spectrophotometer (2013, background): “…technology for astronomical observations over most of the electromagnetic spectrum, notably in the far infrared through millimeter (0.1–3 mm) (Bintley et al. 2010; Niemack et al. 2008; Carlstrom et al. 2011), Xray (Kelley et al. 2009), and gamma-ray (Doriese et al. 2007) wavelength ranges.”