Planetary brightness temperature measurements at 8.6 mm and 3.1 mm wavelengths

Ulich, B. L.; Cogdell, J. R.; Davis, James F.

doi:10.1016/0019-1035(73)90139-5

Cited by 28 publications

(6 citation statements)

References 73 publications

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“…For an ideal radiometer, the combination of sky temperature and typical measurement signals will not compress the amplifiers. However, calibration sources are typically much warmer than the CMB and so compression can have important consequences when deriving responsivities from astronomical or other sources (for example, the Moon is ∼223 K; Ulich et al 1973). For the Q-band array, responsivity measurements in the laboratory and at the site with different calibration sources were all consistent with each other, confirming that the modules were not operating in a compressed regime.…”

Section: Responsivitiesmentioning

confidence: 72%

“…The emission from the ∼0. • 5 Moon varies across its face (Ulich et al 1973); polarized responsivities for a single detector could vary between the brightest and darkest portions of the Moon's face by 20% (worst case 50%). Ultimately this meant we could not use the Moon to calibrate the responsivities for the W-band receiver as we could with the Q-band receiver or we would have misestimated our responsivity (and hence our noise) by at least 20%.…”

Section: Responsivitiesmentioning

confidence: 99%

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The Q/U Imaging Experiment Instrument

Bischoff

Brizius

Buder

et al. 2013

ApJ

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The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(∼1 • ). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4 m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs 1/2 ) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs 1/2 at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range ∼ 25-975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument.

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Section: Responsivitiesmentioning

confidence: 72%

Section: Responsivitiesmentioning

confidence: 99%

The Q/U Imaging Experiment Instrument

Bischoff

Brizius

Buder

et al. 2013

ApJ

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“…al. (1986), Rather, Ulich & Ade (1974), Ulich & Conklin (1976), Ulich (1974), Ulich, Cogdell & Davis (1973) and Whitcomb et. al.…”

Section: Simulationsmentioning

confidence: 95%

“…This may be achieved by the calibration of any offsets in the nominal values of the geometric-calibration parameters discussed below. A more detailed discussion of the reference systems and the attitude analysis may be found in van Leeuwen et al (2002) and Harrison & van Leeuwen (2005).…”

Section: P O I N T I N G R E C O N S T Ru C T I O Nmentioning

confidence: 99%

“…The geometric calibration is the process whereby all the line-of-sight positions of the detectors are recovered, at any time during the observations. The relationship between the pointing and time may depend on multiple parameters, discussed in full in van Leeuwen et al (2002); here we discuss only those parameters which require calibrating with the science data. The remaining geometric-calibration parameters may be determined solely from the star tracker data.…”

Section: Introductionmentioning

confidence: 99%

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The geometric calibration of the Planck satellite using solar system objects

Harrison

Leeuwen

2006

Monthly Notices of the Royal Astronomical Society

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The geometric calibration of the Planck satellite using the planetary transits is investigated, together with the reconstruction of any offsets from the nominal layout of the focal plane. The methods presented here may be applied to a single focal plane transit of a planet, to find the values of the geometric‐calibration parameters at the epoch of the transit or all the transits over the course of the mission. The pointing requirements are easily met, with the pointing reconstruction being dominated by the errors due to the star tracker.

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