The advanced cosmic microwave explorer - A millimeter-wave telescope and stabilized platform

Meinhold, P. R.; Chingcuanco, Alfredo O.; Gundersen, J. O.; Schuster, Jeffrey; Seiffert, M. D.; Lubin, P. M.; Morris, David C.; Villela, T.

doi:10.1086/172414

Cited by 28 publications

(14 citation statements)

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“…A detailed description of the instrument can be found in Meinhold et al (1993), while the detail of the 1994 observations and data reduction is described in Gundersen et al (1995). Frequencies and beam width for these channels are given in Table 1.…”

Section: Microwave Datamentioning

confidence: 99%

Correlation of the South Pole 94 data with $\mathsf{100 \mu}$m and 408 MHz maps

Hamilton

Ganga

2001

A&A

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Abstract. We present a correlation between the ACME/SP94 CMB anisotropy data at 25 to 45 GHz with the IRAS/DIRBE data and the Haslam 408 MHz data. We find a marginal correlation between the dust and the Q-band CMB data but none between the CMB data and the Haslam map. While the amplitude of the correlation with the dust is larger than that expected from naive models of dust emission, it does not dominate the sky emission.

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Section: Microwave Datamentioning

confidence: 99%

Correlation of the South Pole 94 data with $\mathsf{100 \mu}$m and 408 MHz maps

Hamilton

Ganga

2001

A&A

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“…MAX is an off-axis Gregorian telescope with a bolometric photometer mounted on an attitude-controlled balloon platform. The instrument has been described extensively elsewhere (Fischer et al 1992, Alsop et al 1992, Meinhold et al 1993b. The telescope has a 1 m off-axis parabolic primary with an elliptical secondary which sinusoidally chops the beam in azimuth at 5.4 Hz with a peak-to-peak throw of 1.…”

Section: Instrumentmentioning

confidence: 99%

The Second Measurement of Anisotropy in the Cosmic Microwave Background Radiation at 0[fdg]5 Scales near the Star μ Pegasi

Lim

Clapp

Devlin

et al. 1996

The Astrophysical Journal

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During the fifth flight of the Microwave Anisotropy Experiment (MAX5), we revisited a region with significant dust emission near the star Mu Pegasi. A 3.5 cm −1 low frequency channel has been added since the previous measurement (Meinhold et al. 1993a). The data in each channel clearly show structure correlated with IRAS 100 µm dust emission. The spectrum of the structure in the 6, 9 and 14 cm −1 channels is described byand T dust = 19 K and B ν is the Planck function. However, this model predicts a smaller amplitude in the 3.5 cm −1 band than is observed. Considering only linear combinations of the data independent of the best fit foreground spectrum for the three lower channels, we find an upper limit to CMBR fluctuations of ∆T /T = C l l(l+1) 2π 1 2 ≤ 1.3 × 10 −5 at the 95% confidence level. The result is for a flat band power spectrum and does not include a 10% uncertainty in calibration.It is consistent with our previous observation in the region.Subject headings: cosmic microwave background -cosmology: observations -3 -

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“…The telescope design, which obeys the Dragone-Mizugutch condition (Dragone 1978;Mizuguchi et al 1976), is similar to that of BEAST, a telescope dedicated to mapping CMB temperature anisotropies (Childers et al 2005;Figueiredo et al 2005;Meinhold et al 2005;Mejía et al 2005;O'Dwyer et al 2005;Donzelli 2006), and uses identical aluminum coated carbon fiber reflectors. Figure 1 shows the optical design including the primary, 0.9 m diameter ellipsoidal secondary, and the Dewar that houses the receivers.…”

Section: Telescopementioning

confidence: 99%

“…12 This table, as described in Meinhold et al (1993) was used previously to observe CMB temperature anisotropies from the South Pole.…”

Section: Telescopementioning

confidence: 99%

Untitled

2008

ASTROPHYS J SUPPL S

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The White Mountain Polarimeter (WMPol) is a dedicated ground-based microwave telescope and receiver system for observing polarization of the cosmic microwave background. WMPol is located at an altitude of 3880 m on a plateau in the White Mountains of Eastern California, at the Barcroft Facility of the University of California White Mountain Research Station. Presented here is a description of the instrument and the data collected during 2004 April through October. We set an upper limit on E-mode polarization of 14 K (95% confidence limit) in the multipole range 170 < l < 240. This result was obtained with 422 hr of observations of a 3 deg 2 sky area about the North Celestial Pole, using a 42 GHz polarimeter. This upper limit is consistent with EE polarization predicted from a standard ÃCDM concordance model.

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The advanced cosmic microwave explorer - A millimeter-wave telescope and stabilized platform

Cited by 28 publications

References 0 publications

Correlation of the South Pole 94 data with $\mathsf{100 \mu}$m and 408 MHz maps

Correlation of the South Pole 94 data with $\mathsf{100 \mu}$m and 408 MHz maps

The Second Measurement of Anisotropy in the Cosmic Microwave Background Radiation at 0[fdg]5 Scales near the Star μ Pegasi

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