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Line 2: {{Infobox Telescope \| name = Archeops \| image = [[Image:Archeops gondola at launch.jpg\|250px\|]] \| caption = The Archeops gondola being launched \| organization = Line 26: == Instrument and flights == The instrument was designed by adapting concepts put forward for the High Frequency Instrument of [[Planck Surveyor\|Planck surveyor]] (Planck-HFI) and using balloon-borne constraints.<ref>{{cite journal \| doi=10.1016/S0927-6505(01)00141-4 \| first=A. \| last=Benoit \| ~~coauthors~~author2=et al. \| year=2002 \| title=Archeops: A High Resolution, Large Sky Coverage Balloon Experiment for Mapping CMB Anisotropies \| journal=Astropart. Phys. \| volume=17 \| pages=101–124 \| arxiv=astro-ph/0106152 \|bibcode = 2002APh....17..101B }}</ref> Namely, it consists of an open 3He-4He dilution cryostat cooling spiderweb-type [[bolometer]]s at 100 mK; cold individual optics with horns at different temperature stages (0.1, 1.6, 10 K) and an off-axis [[Gregorian telescope]]. Line 38: == Results == [[Image:Archeops last flight map.jpg\|thumb\|300px\|right\|Archeops CMB map]] Archeops has linked, for the first time and before [[WMAP]], the large angular scales (previously measured by [[Cosmic Background Explorer\|COBE]]) to the first acoustic peak region.<ref>{{cite journal \| first=A. \| last=Benoit \| ~~coauthors~~author2=et al. \| year=2003 \| title=The Cosmic Microwave Background Anisotropy Power Spectrum measured by Archeops \| journal=A&A \| volume=399 \| pages=L19 \| arxiv=astro-ph/0210305 \|bibcode = 2003A&A...399L..19B \|doi = 10.1051/0004-6361:20021850 }}</ref><ref>{{cite journal \| first=M. \| last=Tristram \| ~~coauthors~~author2=et al. \| year=2005 \| title=The CMB temperature power spectrum from an improved analysis of the Archeops data \| journal=A&A \| volume=436 \| pages=785 \| arxiv=astro-ph/0411633 \|bibcode = 2005A&A...436..785T \|doi = 10.1051/0004-6361:20042416 }}</ref> From its results, inflation motivated cosmologies have been reinforced with a flat Universe (total energy density Ω<sub>tot</sub> = 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.<ref>{{cite journal \| first=A. \| last=Benoit \| ~~coauthors~~author2=et al. \| year=2003 \| title=Title: Cosmological constraints from Archeops \| journal=A&A \| volume=399 \| pages=L25 \| arxiv=astro-ph/0210306 \|bibcode = 2003A&A...399L..25B \|doi = 10.1051/0004-6361:20021722 }}</ref> Archeops has given the first and still unique polarized maps of the galactic dust emission with this resolution.<ref>{{cite journal \| first=A. \| last=Benoit \| ~~coauthors~~author2=et al. \| year=2004 \| title=First Detection of Polarization of the Submillimetre Diffuse Galactic Dust Emission by Archeops \| journal=A&A \| volume=424 \| pages=571 \| arxiv=astro-ph/0306222 \|bibcode = 2004A&A...424..571B \|doi = 10.1051/0004-6361:20040042 }}</ref><ref>{{cite journal \| first=N. \| last=Ponthieu \| ~~coauthors~~author2=et al.\| year=2005 \| title=Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops \| journal=A&A \| volume=444 \| pages=327 \| arxiv=astro-ph/0501427 \|bibcode = 2005A&A...444..327P \|doi = 10.1051/0004-6361:20052715 }}</ref> == References ==

Archeops: Difference between revisions