Design, Implementation, and Testing of the
                    <i>Microwave Anisotropy Probe</i>
                    Radiometers

Jarosik, N.; Bennett, C. L.; Halpern, M.; Hinshaw, G.; Kogut, A.; Limon, M.; Meyer, S. S.; Page, Lyman A.; Pospieszalski, M.W.; Spergel, David N.; Tucker, Gregory S.; Wilkinson, David T.; Wollack, Edward J.; Wright, E. L.; Zhang, Z.

doi:10.1086/346080

Cited by 171 publications

(175 citation statements)

References 8 publications

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“…The basic OCRA design was based on the prototype demonstrator for the Planck Low Frequency Instrument (Mandolesi et al 2000) and is similar to the K-band receivers mounted on the WMAP spacecraft (Jarosik et al 2003). The nominal system specification is presented in Table 1.…”

Section: Ocra-pmentioning

confidence: 99%

Survey of planetary nebulae at 30 GHz with OCRA-p

Pazderska¹,

Gawroński²,

Feiler³

et al. 2009

A&A

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Aims. We report the results of a survey of 442 planetary nebulae at 30 GHz. The purpose of the survey is to develop a list of planetary nebulae as calibration sources that could be used for high frequency calibration in future. For 41 PNe with sufficient data, we test the emission mechanisms in order to evaluate whether or not spinning dust plays an important role in their spectra at 30 GHz. Methods. The 30-GHz data were obtained with a twin-beam differencing radiometer, OCRA-p, which is in operation on the Toruń 32-m telescope. Sources were scanned both in right ascension and declination. We estimated flux densities at 30 GHz using a free-free emission model and compared it with our data. Results. The primary result is a catalogue containing the flux densities of 93 planetary nebulae at 30 GHz. Sources with sufficient data were compared with a spectral model of free-free emission. The model shows that free-free emission can generally explain the observed flux densities at 30 GHz thus no other emission mechanism is needed to account for the high-frequency spectra.

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Section: Ocra-pmentioning

confidence: 99%

Survey of planetary nebulae at 30 GHz with OCRA-p

Pazderska¹,

Gawroński²,

Feiler³

et al. 2009

A&A

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“…The LFI receivers are based on an additive correlation concept, or pseudo-correlation, analogous to schemes used in previous applications in early works (Blum 1959), as well as in recent CMB experiments (Staggs et al 1996;Jarosik et al 2003). The LFI design introduces new features that optimise stability and immunity to systematics within the constraints imposed by cryogenic operation and by integration into a complex payload such as Planck.…”

Section: Receiver Designmentioning

confidence: 99%

Planckpre-launch status: Design and description of the Low Frequency Instrument

Bersanelli

Mandolesi

Butler

et al. 2010

A&A

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In this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA programme dedicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisation in three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100−850 GHz) will be covered by the HFI instrument. The LFI is an array of microwave radiometers based on state-of-the-art indium phosphide cryogenic HEMT amplifiers implemented in a differential system using blackbody loads as reference signals. The front end is cooled to 20 K for optimal sensitivity and the reference loads are cooled to 4 K to minimise low-frequency noise. We provide an overview of the LFI, discuss the leading scientific requirements, and describe the design solutions adopted for the various hardware subsystems. The main drivers of the radiometric, optical, and thermal design are discussed, including the stringent requirements on sensitivity, stability, and rejection of systematic effects. Further details on the key instrument units and the results of ground calibration are provided in a set of companion papers.

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“…System level implementations of polarization modulation employ such devices such as half-wave plates (HWP; Reichborn-Kjennerud et al 2010;Fraisse et al 2013;Kusaka et al 2014), Faraday rotators (Moyerman et al 2013), and phase switched receiver architectures (Jarosik et al 2003;Bersanelli et al 2010;QUIET Collaboration et al 2013) that vary the polarization state of the incoming radiation for synchronous demodulation and detection of the signal. In the ideal case, unpolarized and polarized components of the incoming radiation are treated independently by the system architecture and analysis pipeline.…”

Section: Introductionmentioning

confidence: 99%

Recovery of Large Angular Scale CMB Polarization for Instruments Employing Variable-Delay Polarization Modulators

Miller

Chuss

Marriage

et al. 2016

ApJ

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Variable-delay Polarization Modulators (VPMs) are currently being implemented in experiments designed to measure the polarization of the cosmic microwave background on large angular scales because of their capability for providing rapid, front-end polarization modulation and control over systematic errors. Despite the advantages provided by the VPM, it is important to identify and mitigate any time-varying effects that leak into the synchronously modulated component of the signal. In this paper, the effect of emission from a 300 K VPM on the system performance is considered and addressed. Though instrument design can greatly reduce the influence of modulated VPM emission, some residual modulated signal is expected. VPM emission is treated in the presence of rotational misalignments and temperature variation. Simulations of time-ordered data are used to evaluate the effect of these residual errors on the power spectrum. The analysis and modeling in this paper guides experimentalists on the critical aspects of observations using VPMs as front-end modulators. By implementing the characterizations and controls as described, front-end VPM modulation can be very powerful for mitigating 1/f noise in large angular scale polarimetric surveys. None of the systematic errors studied fundamentally limit the detection and characterization of B-modes on large scales for a tensor-to-scalar ratio of r=0.01. Indeed, r<0.01 is achievable with commensurately improved characterizations and controls.

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Design, Implementation, and Testing of the Microwave Anisotropy Probe Radiometers

Cited by 171 publications

References 8 publications

Survey of planetary nebulae at 30 GHz with OCRA-p

Survey of planetary nebulae at 30 GHz with OCRA-p

Planckpre-launch status: Design and description of the Low Frequency Instrument

Recovery of Large Angular Scale CMB Polarization for Instruments Employing Variable-Delay Polarization Modulators

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