Experiment Design and First Season Observations with the Degree Angular Scale Interferometer

Leitch, E. M.; Pryke, C.; Halverson, N. W.; Kovac, J. M.; Davidson, G. T.; LaRoque, Samuel J.; Schartman, E.; Yamasaki, Jorge; Carlstrom, J. E.; Holzapfel, W. L.; Dragovan, M.; Cartwright, J. K.; Mason, B. S.; Padin, S.; Pearson, T. J.; Readhead, A. C. S.; Shepherd, M. C.

doi:10.1086/338878

Cited by 53 publications

(36 citation statements)

References 17 publications

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“…Measurers of the CMB have been so productive of late that the previous round of results, saying that all is well with the flux anisotropies on various scales, are nearly contemporaneous with the polarization result: De Bernardis et al (2002) on agreement between DASI and BOOMERANG, Leitch et al (2002), Pryke et al (2002), Halverson et al (2002), Santos et al (2002), an independent look at some of the MAXIMA data.…”

Section: Polarization Of the 3 K Radiationmentioning

confidence: 88%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

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ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

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Section: Polarization Of the 3 K Radiationmentioning

confidence: 88%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

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“…QUaD was a 2.6 m Cassegrain radio telescope on the mount originally constructed for the DASI experiment (Leitch et al 2002). This is an az/el mount, with a third axis allowing the entire optics and receiver to be rotated around the line of sight.…”

Section: Instrument Observations and Mapsmentioning

confidence: 99%

THE QUaD GALACTIC PLANE SURVEY. II. A COMPACT SOURCE CATALOG

Culverhouse¹,

Bock²,

Bowden³

et al. 2011

ApJS

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We present a catalog of compact sources derived from the QUaD Galactic Plane Survey. The survey covers ∼800 deg 2 of the inner galaxy (|b| < 4 • ) in Stokes I, Q, and U parameters at 100 and 150 GHz, with angular resolutions of 5 and 3.5 arcmin, respectively. Five hundred and twenty-six unique sources are identified in I, of which 239 are spatially matched between frequency bands, with 53 (234) detected at 100 (150) GHz alone; 170 sources are identified as ultracompact H ii regions. Approximating the distribution of total intensity source fluxes as a power law, we find a slope of γ S,100 = −1.8 ± 0.4 at 100 GHz and γ S,150 = −2.2 ± 0.4 at 150 GHz. Similarly, the power-law index of the source two-point angular correlation function is γ θ,100 = −1.21 ± 0.04 and γ θ,150 = −1.25 ± 0.04. The total intensity spectral index distribution peaks at α I ∼ 0.25, indicating that dust emission is not the only source of radiation produced by these objects between 100 and 150 GHz; free-free radiation is likely significant in the 100 GHz band. Four sources are detected in polarized intensity P, of which three have matching counterparts in I. Three of the polarized sources lie close to the Galactic center, Sagittarius A*, Sagittarius B2, and the Galactic Radio Arc, while the fourth is RCW 49, a bright H ii region. An extended polarized source, undetected by the source extraction algorithm on account of its ∼0.• 5 size, is identified visually, and is an isolated example of large-scale polarized emission oriented distinctly from the bulk Galactic dust polarization.

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“…Since prior to recombination the matter and radiation fields were coupled, fluctuations in the mass density are reflected in the temperature of the radiation. Temperature fluctuations in the CMB were discovered by the COBE satellite (Smoot et al 1992) and are now being measured with ever increasing accuracy, particularly by detectors deployed in long-flight balloons (de Bernardis et al 2000, Hanany et al 2000, Leitch et al 2002. The spectrum of temperature fluctuations is just what inflation predicts: it is scale invariant on large scales and shows a series of "Doppler" or "acoustic" peaks which are the result of coherent acoustic oscillations experienced by the photonbaryon fluid before recombination.…”

Section: Building a Modelmentioning

confidence: 99%

Simulating the formation of cosmic structure

Frenk

2002

Philosophical Transactions of the Royal Society of London. Seri

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A timely combination of new theoretical ideas and observational discoveries has brought about significant advances in our understanding of cosmic evolution. Computer simulations have played a key role in these developments by providing the means to interpret astronomical data in the context of physical and cosmological theory. In the current paradigm, our Universe has a flat geometry, is undergoing accelerated expansion and is gravitationaly dominated by elementary particles that make up cold dark matter. Within this framework, it is possible to simulate in a computer the emergence of galaxies and other structures from small quantum fluctuations imprinted during an epoch of inflationary expansion shortly after the Big Bang. The simulations must take into account the evolution of the dark matter as well as the gaseous processes involved in the formation of stars and other visible components. Although many unresolved questions remain, a coherent picture for the formation of cosmic structure in now beginning to emerge.

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Experiment Design and First Season Observations with the Degree Angular Scale Interferometer

Cited by 53 publications

References 17 publications

Astrophysics in 2002

Astrophysics in 2002

THE QUaD GALACTIC PLANE SURVEY. II. A COMPACT SOURCE CATALOG

Simulating the formation of cosmic structure

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