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The Archeops gondola being launched
Alternative namesARCHEOPS Edit this at Wikidata
Wavelength143, 217, 353, 545 GHz (2.096, 1.382, 0.849, 0.550 mm)
First light1999 Edit this on Wikidata
Decommissioned2002 Edit this on Wikidata
Telescope stylecosmic microwave background experiment
radio telescope Edit this on Wikidata
Angular resolution15 arcminute Edit this on Wikidata
Websitearcheops.planck.fr Edit this at Wikidata
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Archeops was a balloon-borne instrument dedicated to measuring the Cosmic microwave background (CMB) temperature anisotropies. The study of this radiation is essential to obtain precise information on the evolution of the Universe: density, Hubble constant, age of the Universe, etc. To achieve this goal, measurements were done with devices cooled down at 100mK temperature placed at the focus of a warm telescope. To avoid atmospheric disturbance the whole apparatus is placed on a gondola below a helium balloon that reaches 40 km altitude.

Archeops has four bands in the millimeter domain (143, 217, 353 and 545 GHz) with a high angular resolution (about 15 arcminutes) in order to constrain small anisotropy scales, as well as a large sky coverage fraction (30%) in order to minimize the intrinsic cosmic variance.

Instrument and flights


The instrument was designed by adapting concepts put forward for the High Frequency Instrument of Planck surveyor (Planck-HFI) and using balloon-borne constraints.[1] Namely, it consists of an open 3He-4He dilution cryostat cooling spiderweb-type bolometers at 100 mK; cold individual optics with horns at different temperature stages (0.1, 1.6, 10 K) and an off-axis Gregorian telescope.

The CMB signal is measured by the 143 and 217 GHz detectors while interstellar dust emission and atmospheric emission are monitored with the 353 (polarized) and 545 GHz detectors. The whole instrument is baffled so as to avoid stray radiation from the Earth and the balloon.

To cover as far as 30% of the sky, the payload was spinning mostly above the atmosphere, scanning the sky in circles with a fixed elevation of roughly 41 degrees. The gondola, at a float altitude above 32 km, spins across the sky at a rate of 2 rpm which, combined with the Earth rotation, produces a well sampled sky at each frequency.

Archeops flew for the first time in Trapani (Sicily) with four–hours integration time. Then, the upgraded instrument was launched three times from the Esrange base near Kiruna (Sweden) by the CNES during 2 consecutive Winter seasons (2001 and 2002). The last and best flight on Feb. 7th, 2002 yields 12.5 hours of CMB–type data (at ceiling altitude and by night) from a 19–hours total. The balloon landed in Siberia and it was recovered (with its precious data recorded on–board) by a Franco–Russian team with –40°C weather.


Archeops CMB map

Archeops has linked, for the first time and before WMAP, the large angular scales (previously measured by COBE) to the first acoustic peak region.[2][3]

From its results, inflation motivated cosmologies have been reinforced with a flat Universe (total energy density Ωtot = 1 within 3%). When combined with complementary cosmological datasets regarding the value of Hubble's constant, Archeops gives constraints on the dark energy density and the baryonic density in very good agreement with other independent estimations based on supernovae measurements and big bang nucleosynthesis.[4]

Archeops has given the first polarized maps of the galactic dust emission with this resolution.[5][6]


  1. ^ Benoît, A.; et al. (2002). "Archeops: A High Resolution, Large Sky Coverage Balloon Experiment for Mapping CMB Anisotropies". Astroparticle Physics. 17 (2): 101–124. arXiv:astro-ph/0106152. Bibcode:2002APh....17..101B. doi:10.1016/S0927-6505(01)00141-4.
  2. ^ Benoît, A.; et al. (2003). "The Cosmic Microwave Background Anisotropy Power Spectrum measured by Archeops". Astronomy and Astrophysics. 399 (3): L19. arXiv:astro-ph/0210305. Bibcode:2003A&A...399L..19B. doi:10.1051/0004-6361:20021850.
  3. ^ Tristram, M.; et al. (2005). "The CMB temperature power spectrum from an improved analysis of the Archeops data". Astronomy and Astrophysics. 436 (3): 785. arXiv:astro-ph/0411633. Bibcode:2005A&A...436..785T. doi:10.1051/0004-6361:20042416.
  4. ^ Benoît, A.; et al. (2003). "Cosmological constraints from Archeops". Astronomy and Astrophysics. 399 (3): L25. arXiv:astro-ph/0210306. Bibcode:2003A&A...399L..25B. doi:10.1051/0004-6361:20021722.
  5. ^ Benoît, A.; et al. (2004). "First Detection of Polarization of the Submillimetre Diffuse Galactic Dust Emission by Archeops". Astronomy and Astrophysics. 424: 571. arXiv:astro-ph/0306222. Bibcode:2004A&A...424..571B. doi:10.1051/0004-6361:20040042.
  6. ^ Ponthieu, N.; et al. (2005). "Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops". Astronomy and Astrophysics. 444 (1): 327. arXiv:astro-ph/0501427. Bibcode:2005A&A...444..327P. doi:10.1051/0004-6361:20052715.