South Pole Telescope

By Tony Stark. 2007

273 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/e603b513a8df4bd780b5e92bba4a7b787f6f474b

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Citations in the corpus

Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe (2014, methodology): “However, the heating phase is rather short such that this energy injection does not influence the gas significantly on longer time-scales due to efficient cooling. on a ‘counting procedure’ of some kind, for example using surveys of galaxy clusters in X-ray emission (e.g. the upcoming eROSITA missio”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES FROM THE 2500 SQUARE-DEGREE SPT-SZ SURVEY (2014, background): “The telescope, receiver, and detectors are discussed in more detail in Ruhl et al. (2004), Padin et al. (2008), Shirokoff et al. (2009), and Carlstrom et al. (2011).”
Effects of scale-dependent non-Gaussianity on cosmological structures (2007, methodology): “are not subject to the same set of systematic eﬀects as CMB measurements are, so this method provides a valuable complement to the CMB. Upcoming large mass-limited surveys of galaxy clusters with SPT [80], ACT [81], and Planck [82] will yield data sets particularly well suited to the joint analysis ”
SPT-3G: a next-generation cosmic microwave background polarization experiment on the South Pole telescope (2014, background): “The spt is a 10 meter telescope optimized for sensitive, high-resolution measurements of the CMB anisotropy and mm-wave sky.(1,2) The telescope is located at the NSF Amundsen-Scott South Pole station, one of the best developed sites on Earth for mm-wave observations, with particularly low levels of ”
MEASUREMENTS OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH THE SOUTH POLE TELESCOPE (2009, background): “Further details of the receiver and telescope can be found in Ruhl et al. (2004), Padin et al. (2008) and Carlstrom et al. (2009).”
Consistently large cosmic flows on scales of 100 h−1 Mpc: a challenge for the standard ΛCDM cosmology (2008, methodology): “So other techniques, such as those based on the kinetic SZ effect (Sunyaev & Zeldovich 1972; Rephaeli & Lahav 1991; Haehnelt & Tegmark 1996; Ruhl et al. 2004; Kosowsky 2006; Kashlinsky et al. 2008b; Zhang et al. 2008) will be needed to access independent volumes.”
X-Ray and Sunyaev-Zel’dovich Effect Measurements of the Gas Mass Fraction in Galaxy Clusters (2006, background): “– 3 – Future large scale cluster surveys are being pursued which exploit the critical cosmo- logical dependence of the evolution of cluster abundance to provide independent, precise determinations of ΩM , ΩΛ, σ8 and the equation of state of dark energy, w(z) (e.g., Kneissl et al. 2001; Romer et al. ”
A MEASUREMENT OF SECONDARY COSMIC MICROWAVE BACKGROUND ANISOTROPIES WITH TWO YEARS OF SOUTH POLE TELESCOPE OBSERVATIONS (2011, background): “The telescope and receiver are discussed in more detail in Ruhl et al. (2004), Padin et al. (2008), and Carlstrom et al. (2011).”
A MEASUREMENT OF THE DAMPING TAIL OF THE COSMIC MICROWAVE BACKGROUND POWER SPECTRUM WITH THE SOUTH POLE TELESCOPE (2011, background): “The telescope and receiver are discussed in further detail in Ruhl et al. (2004), Padin et al. (2008), and 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).”
Improved constraints on dark energy from Chandra X-ray observations of the largest relaxed galaxy clusters (2007, background): “The advent of new, large area SZ surveys (e.g. Ruhl et al. 2004) will soon provide important new target lists of hot, X-ray luminous high redshift clusters.”
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…”
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”
THz Instruments for Space (2007, background): “Future opportunities are highlighted and it is for the reader to judge whether these will have a chance to be realized within the backdrop of continuing (or diminishing) public support for everything space.”
THE BLANCO COSMOLOGY SURVEY: DATA ACQUISITION, PROCESSING, CALIBRATION, QUALITY DIAGNOSTICS, AND DATA RELEASE (2012, background): “Over the last decade there have been several mmwave cluster studies in the Southern Hemisphere, including ACBAR (Reichardt et al. 2009), ACT (Fowler 2004), APEX (Gonzalez et al. 2001) and SPT (Ruhl et al. 2004).”
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.”