The South Pole Telescope

Ruhl, J. E.; Ade, Peter A. R.; Carlstrom, J. E.; Cho, Hsiao-Mei; Crawford, T. M.; Dobbs, M.; Greer, C.; Halverson, N. W.; Holzapfel, W. L.; Lanting, T.; Lee, Adrian T.; Leitch, E. M.; Leong, J.; Lü, Wei; Lueker, M.; Mehl, J.; Meyer, S. S.; Mohr, J. J.; Padin, S.; Plagge, T.; Pryke, C.; Runyan, M. C.; Schwan, D.; Sharp, Matthew; Spieler, H.; Staniszewski, Z.; Stark, A. A.

doi:10.1117/12.552473

Cited by 214 publications

(53 citation statements)

References 56 publications

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“…This catalog will on its own enable an important cosmological study of dark energy and gravity. Moreover, a number of wide-area cluster surveys in other wavebands will also have produced catalogs in the LSST era, including the SPT SZ survey (Ruhl et al 2004;Staniszewski et al 2008) over several thousand deg 2 , the Planck all-sky SZ 4 survey and an all-sky X-ray survey from eROSITA 5 .…”

Section: The Lsst Cluster Samplementioning

confidence: 99%

LSST Science Book, Version 2.0

Abell¹,

Burke²,

Hamuy³

et al. 2009

544

653

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Prepared by the LSST Science Collaborations, with contributions from the LSST Project. PrefaceMajor advances in our understanding of the Universe over the history of astronomy have often arisen from dramatic improvements in our ability to observe the sky to greater depth, in previously unexplored wavebands, with higher precision, or with improved spatial, spectral, or temporal resolution. Aided by rapid progress in information technology, current sky surveys are again changing the way we view and study the Universe, and the next-generation instruments, and the surveys that will be made with them, will maintain this revolutionary progress. Substantial progress in the important scientific problems of the next decade (determining the nature of dark energy and dark matter, studying the evolution of galaxies and the structure of our own Milky Way, opening up the time domain to discover faint variable objects, and mapping both the inner and outer Solar System) all require wide-field repeated deep imaging of the sky in optical bands.The wide-fast-deep science requirement leads to a single wide-field telescope and camera which can repeatedly survey the sky with deep short exposures. The Large Synoptic Survey Telescope (LSST), a dedicated telecope with an effective aperture of 6.7 meters and a field of view of 9.6 deg 2 , will make major contributions to all these scientific areas and more. It will carry out a survey of 20,000 deg 2 of the sky in six broad photometric bands, imaging each region of sky roughly 2000 times (1000 pairs of back-to-back 15-sec exposures) over a ten-year survey lifetime.The LSST project will deliver fully calibrated survey data to the United States scientific community and the public with no proprietary period. Near real-time alerts for transients will also be provided worldwide. A goal is worldwide participation in all data products. The survey will enable comprehensive exploration of the Solar System beyond the Kuiper Belt, new understanding of the structure of our Galaxy and that of the Local Group, and vast opportunities in cosmology and galaxy evolution using data for billions of distant galaxies. Since many of these science programs will involve the use of the world's largest non-proprietary database, a key goal is maximizing the usability of the data. Experience with previous surveys is that often their most exciting scientific results were unanticipated at the time that the survey was designed; we fully expect this to be the case for the LSST as well.The purpose of this Science Book is to examine and document in detail science goals, opportunities, and capabilities that will be provided by the LSST. The book addresses key questions that will be confronted by the LSST survey, and it poses new questions to be addressed by future study. It contains previously available material (including a number of White Papers submitted to the ASTRO2010 Decadal Survey) as well as new results from a year-long campaign of study and evaluation. This book does not attempt to be complete; there are many ...

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Section: The Lsst Cluster Samplementioning

confidence: 99%

LSST Science Book, Version 2.0

Abell¹,

Burke²,

Hamuy³

et al. 2009

544

653

View full text Add to dashboard Cite

show abstract

“…Yet, most of new generation MM wave CMBR projects chose multi-element bolometer arrays to reach highest sensitivity in the ground based experiment. NET CM BR = 260 − 280µKs 1/2 per detector must be reached in 1000 element array of TES bolometers at 10 m South Pole Telescope(SPT) in 20% bandwidth at 95 GHz and 150 GHz (Ruhl et al, 2004). Millimeter Bolometric Array Camera(MBAC) with 3 1000-element TES bolometer arrays at 150 GHz/220 GHz/270 GHz is under development now for In a ground based experiment at sea level atmospheric effects contribute much more than astrophysical foregrounds nevertheless we should take them into account to better prepare the experiment.…”

Section: −17mentioning

confidence: 99%

Spectral spatial fluctuations of CMBR: Strategy and concept of the experiment

2008

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Spectral Spatial Fluctuations (SSF) of the Cosmic Microwave Background Radiation (CMBR) temperature are considered as a result of an interaction of primordial atoms and molecules with CMBR in proto-objects moving with peculiar velocities relative to the CMBR. Expected optimistic values of ∆T /T are 2×10 −5 −2×10 −6 for SSF caused by HeH + at z =20-30 which are possible redshifts of early reionization scenario. The bandwidth of the lines is 0.1-2% depending on the scale of protoobjects and redshifts. For the SSF search CMBR maps in different spectral channels are to be observed and then processed by the Difference method. Simulation of the experiment is made for MSRT (Tuorla Observatory, Finland) equipped with a 7 × 4 beam cryo-microbolometer array with a chopping flat and frequency multiplexer providing up to 7 spectral channels in each beam (88-100 GHz). Expected ∆T/T limit in the experiment is 2×10 −5 with 6 ′ -7 ′ angular and 2% frequency resolution. Simulation shows that SSF may be recognized in the angular power spectrum when S/N in single frequency CMBR maps is as small as 1.17 or even something less for white noise. Such an experiment gives us a possibility to set upper limit of SSF in MM band and prepare future SSF observations.

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“…Combined with a greater sensitivity than optical or X-ray surveys to high-redshift objects, this makes SZ-selected cluster samples well suited for measuring the evolution of the cluster mass function over a wide range in redshift. Experiments such as the Atacama Cosmology Telescope (Kosowsky 2003) and the South Pole Telescope (Ruhl et al 2004) are currently surveying the microwave sky to develop large catalogs of galaxy clusters that are uniformly selected by the SZ flux.…”

Section: Introductionmentioning

confidence: 99%

Sharpening the Precision of the Sunyaev-Zel'dovich Power Spectrum

Shaw

Zahn

Holder

et al. 2009

ApJ

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Using both halo model calculations and a large sample of simulated SZ maps, we demonstrate that high-mass clusters add significant non-Gaussian variance to measurements of the SZ power spectrum amplitude. The difficulty in correctly accounting theoretically for the contribution of these objects to the uncertainty in C leads to a reduced sensitivity to σ 8 . We show that a simple solution is to mask out the brightest clusters in the map before measuring the power spectrum. We demonstrate that fairly conservative masking can reduce the variance and Gaussianize the statistics significantly, thus increasing the sensitivity to cosmological parameters. Choosing which objects to mask is nontrivial; we found that using a fixed sky density produced a well-defined and well-behaved estimate that can easily be applied to real maps. For example, masking the 10 (90) brightest clusters in a 100 deg 2 SZ map will improve the sensitivity to C by a factor of two at = 1000 (2000) and 1.5 at = 2000 (4000). We show that even in the presence of astrophysical foregrounds (primary cosmic microwave background and point sources) and instrument noise, one can increase the precision on measurements of σ 8 by masking up to 0.9 clusters deg −2 .

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The South Pole Telescope

Cited by 214 publications

References 56 publications

LSST Science Book, Version 2.0

LSST Science Book, Version 2.0

Spectral spatial fluctuations of CMBR: Strategy and concept of the experiment

Sharpening the Precision of the Sunyaev-Zel'dovich Power Spectrum

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