Archeops: a high resolution, large sky coverage balloon experiment for mapping cosmic microwave background anisotropies

Benoı̂t, A.; Ade, Peter A. R.; Amblard, A.; Ansari, R.; Aubourg, É.; Bartlett, J. G.; Bernard, J.-P.; Bhatia, R.; Blanchard, Alain; Bock, J. J.; Boscaleri, A.; Bouchet, F. R.; Bourrachot, A.; Camus, P.; Couchot, F.; Bernardis, P. de; Delabrouille, J.; Désert, F.‐X.; Doré, O.; Douspis, M.; Dumoulin, L.; Dupac, X.; Filliatre, P.; Ganga, K.; Gannaway, F.; Gautier, Brice; Giard, M.; Giraud‐Héraud, Y.; Gispert, R.; Guglielmi, L.; Hamilton, J. C.; Hanany, Shaul; Henrot-Versillé, S.; Hristov, V. V.; Kaplan, J.; Lagache, G.; Lamarre, J.-M.; Lange, A. E.; Madet, K.; Maffei, B.; Marrone, Daniel P.; Masi, S.; Murphy, J. A.; Naraghi, F.; Nati, F.; Perrin, G.; Piat, M.; Puget, J.‐L.; Santos, D.; Sudiwala, R.; Vanel, Jean-Charles; Vibert, D.; Wakui, E.; Yvon, D.

doi:10.1016/s0927-6505(01)00141-4

Cited by 58 publications

(22 citation statements)

References 18 publications

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“…The LSPE payload will spin at constant speed (3 rpm) around the zenith axis, keeping the telescope boresight at constant elevation for long periods. This strategy is similar to the one adopted by the Archeops balloon experiment 45 , and shares several commonalities also with the Planck satellite 7 . The elevation will be changed occasionally, in order to extend the full coverage, and to execute specific calibration observations, such as scans of planets or other calibration sources.…”

Section: Observation Strategymentioning

confidence: 87%

“…It produces a sky map where optical star signals can be identified if compared to a catalogue, thus giving the telescopes pointing with respect to the sky coordinates. It is based on the same solution we developed for the successful Archeops flights (which was carried out during the polar night, as planned for LSPE) 44,45 . This is based on simple and reliable components, providing high resolution and sensitivity with fast response, as needed in a fast sky scanning instrument.…”

Section: The Fast Star Sensormentioning

confidence: 99%

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The Large-Scale Polarization Explorer (LSPE)

et al. 2012

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The LSPE is a balloon-borne mission aimed at measuring the polarization of the Cosmic Microwave Background (CMB) at large angular scales, and in particular to constrain the curl component of CMB polarization (B-modes) produced by tensor perturbations generated during cosmic inflation, in the very early universe. Its primary target is to improve the limit on the ratio of tensor to scalar perturbations amplitudes down to r = 0.03, at 99.7% confidence. A second target is to produce wide maps of foreground polarization generated in our Galaxy by synchrotron emission and interstellar dust emission. These will be important to map Galactic magnetic fields and to study the properties of ionized gas and of diffuse interstellar dust in our Galaxy. The mission is optimized for large angular scales, with coarse angular resolution (around 1.5 degrees FWHM), and wide sky coverage (25% of the sky). The payload will fly in a circumpolar long duration balloon mission during the polar night. Using the Earth as a giant solar shield, the instrument will spin in azimuth, observing a large fraction of the northern sky. The payload will host two instruments. An array of coherent polarimeters using cryogenic HEMT amplifiers will survey the sky at 43 and 90 GHz. An array of bolometric polarimeters, using large throughput multi-mode bolometers and rotating Half Wave Plates (HWP), will survey the same sky region in three bands at 95, 145 and 245 GHz. The wide frequency coverage will allow optimal control of the polarized foregrounds, with comparable angular resolution at all frequencies.

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Section: Observation Strategymentioning

confidence: 87%

Section: The Fast Star Sensormentioning

confidence: 99%

The Large-Scale Polarization Explorer (LSPE)

et al. 2012

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“…The 1.5×1.8 m parabolic primary mirror weighed 42kg and was previously used in Archeops (Benoît et al 2002). The 1.2×1.3 m and 22kg secondary, a section of an ellipsoid of revolution, was fabricated for EBEX.…”

Section: Ambient Temperature Telescopementioning

confidence: 99%

The EBEX Balloon-borne Experiment—Optics, Receiver, and Polarimetry

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Araujo

et al. 2018

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The E and B Experiment (EBEX) was a long-duration balloon-borne cosmic microwave background (CMB) polarimeter that flew over Antarctica in 2012. We describe the experiment's optical system, receiver, and polarimetric approach and report on their in-flight performance. EBEX had three frequency bands centered on 150, 250, and 410GHz. To make efficient use of limited mass and space, we designed a 115cm 2 sr highthroughput optical system that had two ambient temperature mirrors and four antireflection-coated polyethylene lenses per focal plane. All frequency bands shared the same optical train. Polarimetry was achieved with a continuously rotating achromatic half-wave plate (AHWP) that was levitated with a superconducting magnetic bearing (SMB). This is the first use of an SMB in astrophysics. Rotation stability was 0.45% over a period of 10 hr, and angular position accuracy was 0°. 01. The measured modulation efficiency was above 90% for all bands. To our knowledge the 109% fractional bandwidth of the AHWP was the broadest implemented to date. The receiver, composed of one lens and the AHWP at a temperature of 4K, the polarizing grid and other lenses at 1K, and the two focal planes at 0.25K, performed according to specifications, giving focal plane temperature stability with a fluctuation power spectrum that had a 1/f knee at 2mHz. EBEX was the first balloon-borne instrument to implement technologies characteristic of modern CMB polarimeters, including high-throughput optical systems, and large arrays of transition edge sensor bolometric detectors with multiplexed readouts.

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“…The solution that is used for the HFI is original. A prototype of it has recently been tested with success on the Archeops balloonborne experiment 6 . The architecture of the detector assembly is represented in Fig.…”

Section: Architecture Of the Detector Assemblymentioning

confidence: 99%

Planck-HFI thermal architecture: from requirements to solutions

et al. 2003

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The Planck-High Frequency Instrument (HFI) will use 48 bolometers cooled to 100mK by a dilution cooler to map the Cosmic Microwave Background (CMB) with a sensitivity of ∆T/T~2.10-6 and an angular resolution of 5 minutes of arc. This instrument will therefore be about 1000 times more sensitive than the COBE-DMR experiment. This contribution will focus mainly on the thermal architecture of this instrument and its consequences on the fundamental and instrumental fluctuations of the photon flux produced on the detectors by the instrument itself. In a first step, we will demonstrate that the thermal and optical design of the HFI allow to reach the ultimate sensitivity set by photon noise of the CMB at millimeter wavelength. Nevertheless, to reach such high sensitivity, the thermal behavior of each cryogenic stages should also be controlled in order to damp thermal fluctuations that can be taken as astrophysical signal. The requirement in thermal fluctuation on each stage has been defined in the frequency domain to degrade the overall sensitivity by less than 5%. This leads to unprecedented stability specifications that should be achieved down to 16mHz. We will present the design of the HFI thermal architecture, based on active and passive damping, and show how its performances were improved thanks to thermal simulations.

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Archeops: a high resolution, large sky coverage balloon experiment for mapping cosmic microwave background anisotropies

Cited by 58 publications

References 18 publications

The Large-Scale Polarization Explorer (LSPE)

The Large-Scale Polarization Explorer (LSPE)

The EBEX Balloon-borne Experiment—Optics, Receiver, and Polarimetry

Planck-HFI thermal architecture: from requirements to solutions

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