The Optical Design and Characterization of the Microwave Anisotropy Probe

By L. Page, C. Jackson, C. Barnès, C. Bennett, M. Halpern, Gary F. Hinshaw, N. Jarosik, Alan Kogut, M. Limon, S. Meyer and 10 more. 2003

246 citations recorded by the source corpus.

The primary goal of the MAP satellite, now in orbit, is to make high-fidelity polarization-sensitive maps of the full sky in five frequency bands between 20 and 100 GHz. From these maps we will characterize the properties of the cosmic microwave background (CMB) anisotropy and Galactic and extragalactic emission on angular scales ranging from the effective beam size, less than 0.°23, to the full sky. MAP is a differential microwave radiometer. Two back-to-back shaped offset Gregorian telescopes feed two mirror symmetric arrays of 10 corrugated feeds. We describe the prelaunch design and characterization of the optical system, compare the optical models to the measurements, and consider multiple possible sources of systematic error.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0fbeea57054bb8a148bff38647414f24ad5f2639

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. F. Tavecchio
2. Bing Zhang
3. G. Ghisellini
4. C. Dermer
5. Luigi Foschini
6. Y. Kovalev
7. E. Orlando
8. L. Maraschi

In Nuclear and High Energy Physics

1. F. Tavecchio
2. G. Ghisellini
3. C. Dermer
4. Luigi Foschini
5. L. Maraschi
6. E. Orlando
7. Y. Kovalev
8. J. Finke

Citations in the corpus

• The Atacama Cosmology Telescope: The Receiver and Instrumentation (2010, unknown): “Using the instrument passband (normalized by the peak in the composite passband), we follow the method of Page et al. (2003) for calculating the effective central frequency of broadband sources, including the CMB and SZ effect.”
• First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Foreground Emission (2003, unknown): “The maps are then filtered by bl/(b 2 lC cmb l +C noise), (Tegmark & de Oliveira-Costa 1998; Refregier et al. 2000), where bl is the transfer function of the WMAP beam pattern (Page et al. 2003a), Ccmbl is the CMB angular power spectrum, and Cnoise is the noise power.”
• BLAZARS AS ULTRA-HIGH-ENERGY COSMIC-RAY SOURCES: IMPLICATIONS FOR TeV GAMMA-RAY OBSERVATIONS (2011, background): “…AGN detected at TeV energies consist mainly of high-synchrotron-peaked BL Lac objects, including the ultra-variable TeV blazars Mrk 421 (z=0.031; Fossati et al. 2008), Mrk 501 (z=0.033; Albert et al. 2007b) and PKS 2155-304 (z=0.116; Aharonian et al. 2007a), and the apparently non-variable TeV…”
• THE SPECTRAL ENERGY DISTRIBUTIONS OF FERMI BLAZARS (2016, background): “8 by Fossati et al. (2008), it can be seen that there is also an anti-correlation between log νp and αRO for the whole sample.”
• Extreme TeV blazars and the intergalactic magnetic field (2010, background): “Support to the idea that the emission mainly originates in a single region comes from the existence of a characteristic timescales, thought to be related to the size of the emittingregion3, and from the tight correlation between variations at very different frequencies (e.g. Fossati et al. 2008)4.”
• INSIGHTS INTO THE HIGH-ENERGY γ-RAY EMISSION OF MARKARIAN 501 FROM EXTENSIVE MULTIFREQUENCY OBSERVATIONS IN THE FERMI ERA (2011, background): “– 54 – the simple scaling FTeV ∝ F 2keV which would be expected from the class of SSC models in which the highest-energy electrons upscatter (in the Thomson regime) their own synchrotron photons to the TeV band (see, e.g., Gliozzi et al. 2006; Fossati et al. 2008).”
• Synchrotron Self-Compton Analysis of TeV X-Ray-Selected BL Lacertae Objects (2008, methodology): “The model fits of Fossati et al. (2008) give δD = 100 and B = 1 G for a blob size of R′b = 1×1014 cm which is similar to our fits, except with a larger B.”