Work, Leisure and Human Needs

Sayers, Sean

doi:10.1177/072551368601400107

Cited by 6 publications

(9 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Optical shot and Bose noise contribute in roughly equal amounts to the total photon noise at each observing frequency, with the BLIP NEP γ ≃ 1.5 mK/ √ Hz (2.3 mK CM B / √ Hz) at 143 GHz and the BLIP NEP γ ≃ 0.8 mK/ √ Hz (4.5 mK CM B / √ Hz) at 268 GHz. 2 More details of the Bolocam instrument can be found in Glenn et al (1998), Glenn et al (2003), Haig et al (2004), and Sayers (2007).…”

Section: Instrument Descriptionmentioning

confidence: 99%

Studies of Millimeter-Wave Atmospheric Noise Above Mauna Kea

Sayers

Golwala

Ade

et al. 2009

ApJ

View full text Add to dashboard Cite

We report measurements of the fluctuations in atmospheric emission (atmospheric noise) above Mauna Kea recorded with Bolocam at 143 and 268 GHz from the Caltech Submillimeter Observatory (CSO). The 143 GHz data were collected during a 40 night observing run in late 2003, and the 268 GHz observations were made in early 2004 and early 2005 over a total of 60 nights. Below ≃ 0.5 Hz, the data time-streams are dominated by atmospheric noise in all observing conditions. The atmospheric noise data are consistent with a Kolmogorov-Taylor (K-T) turbulence model for a thin wind-driven screen, and the median amplitude of the fluctuations is 280 mK 2 rad −5/3 at 143 GHz and 4000 mK 2 rad −5/3 at 268 GHz. Comparing our results with previous ACBAR data, we find that the normalization of the power spectrum of the atmospheric noise fluctuations is a factor of ≃ 80 larger above Mauna Kea than above the South Pole at millimeter wavelengths. Most of this difference is due to the fact that the atmosphere above the South Pole is much drier than the atmosphere above Mauna Kea. However, the atmosphere above the South Pole is slightly more stable as well: the fractional fluctuations in the column depth of precipitable water vapor are a factor of ≃ √ 2 smaller at the South Pole compared to Mauna Kea. Based

show abstract

Section: Instrument Descriptionmentioning

confidence: 99%

Studies of Millimeter-Wave Atmospheric Noise Above Mauna Kea

Sayers

Golwala

Ade

et al. 2009

ApJ

View full text Add to dashboard Cite

show abstract

“…Then (5) becomes equivalent to (12) [ 1 : 2( * ), 1( * ) ], and this, in conjunction with Theorem 3 in Sayers [12], then gives us…”

Section: Preliminariesmentioning

confidence: 96%

“…Of the remaining 247 cases, exactly 81 are further eliminated by conditions (7) The remaining sixteen cases (of the 136 mentioned above) are eliminated once we prove three further lemmata, namely Lemmata (7) through (35) will also eliminate every possible case for the exponents in (1) if we assume any one of Ω(N ) = 29, 31, or 33. Therefore, recalling that it is known that Ω(N ) ≥ 29 (Sayers [12]), it suffices, for the proof of Theorem 1, to prove the lemmata stated in (14) through (35); we outline these proofs in the following section.…”

Section: Preliminariesmentioning

confidence: 99%

See 1 more Smart Citation

On the total number of prime factors of an odd perfect number

Iannucci

Sorli

2003

Math. Comp.

View full text Add to dashboard Cite

show abstract

“…After the first high-pass filter, we remove a 2dimensional spatial polynomial function across the array (Sayers 2007;Halverson et al 2009) at each sample in the timestream. During this process, referred to as spatial template removal, we fit the polynomial either across the entire array, or individually for each of the six detector wafers to improve removal of correlated signals on scales smaller than the 0.4 • field-of-view.…”

Section: Removal Of Timestream Contaminationmentioning

confidence: 99%

Galaxy cluster scaling relations measured with APEX-SZ

Bender

Kennedy

Basu

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present thermal Sunyaev-Zel'dovich effect (SZE) measurements for 42 galaxy clusters observed at 150 GHz with the APEX-SZ experiment. For each cluster, we model the pressure profile and calculate the integrated Comptonization Y to estimate the total thermal energy of the intracluster medium (ICM). We compare the measured Y values to X-ray observables of the ICM from the literature (cluster gas mass M gas , temperature T X , and Y X = M gas T X ) that relate to total cluster mass. We measure power law scaling relations, including an intrinsic scatter, between the SZE and X-ray observables for three subsamples within the set of 42 clusters that have uniform X-ray analysis in the literature. We observe that differences between these X-ray analyses introduce significant variability into the measured scaling relations, particularly affecting the normalization. For all three subsamples, we find results consistent with a self-similar model of cluster evolution dominated by gravitational effects. Comparing to predictions from numerical simulations, these scaling relations prefer models that include cooling and feedback in the ICM. Lastly, we measure an intrinsic scatter of ∼ 28 per cent in the Y − Y X scaling relation for all three subsamples.

show abstract

Work, Leisure and Human Needs

Cited by 6 publications

References 0 publications

Studies of Millimeter-Wave Atmospheric Noise Above Mauna Kea

Studies of Millimeter-Wave Atmospheric Noise Above Mauna Kea

On the total number of prime factors of an odd perfect number

Galaxy cluster scaling relations measured with APEX-SZ

Contact Info

Product

Resources

About