A Measurement by BOOMERANG of Multiple Peaks in the Angular Power Spectrum of the Cosmic Microwave Background
C. B. NetterfieldDepartment of Physics and Department of Astronomy and Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, CanadaP. A. R. AdeQueen Mary and Westfield College, Mile End Road, London E14NS, UKJ. J. BockJet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109J. R. BondCanadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, CanadaJ. BorrillNational Energy Research Scientific Computing Center, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, M/S 50-4049, Berkeley, CA 94720A. BoscaleriK. CobleDepartment of Physics, University of California at Santa Barbara, Broida Hall, Building 562, Santa Barbara, CA 93106C. R. ContaldiCanadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, CanadaB. P. CrillDivision of Physics, Mathematics and Astronomy, California Institute of Technology, MS 102-33, Pasadena, CA 91125P. de BernardisDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyP. FareseDepartment of Physics, University of California at Santa Barbara, Broida Hall, Building 562, Santa Barbara, CA 93106K. GangaInfrared Processing and Analysis Center, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125M. GiacomettiDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyE. HivonInfrared Processing and Analysis Center, California Institute of Technology, MS 100-22, 770 South Wilson Avenue, Pasadena, CA 91125V. V. HristovDivision of Physics, Mathematics and Astronomy, California Institute of Technology, MS 102-33, Pasadena, CA 91125A. IacoangeliDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyA. H. JaffeDepartment of Astronomy, Space Sciences Lab, and Center for Particle Astrophysics, University of California at Berkeley, 601 Campbell Hall 3411, Berkeley, CA 94720W. C. JonesDivision of Physics, Mathematics and Astronomy, California Institute of Technology, MS 102-33, Pasadena, CA 91125A. E. LangeDivision of Physics, Mathematics and Astronomy, California Institute of Technology, MS 102-33, Pasadena, CA 91125L. MartinisDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyS. MasiDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyP. MasonDivision of Physics, Mathematics and Astronomy, California Institute of Technology, MS 102-33, Pasadena, CA 91125P. D. MauskopfDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UKA. MelchiorriNuclear and Astrophysics Laboratory, University of Oxford, Keble Road, Oxford OX 3RH, UKT. MontroyDepartment of Physics, University of California at Santa Barbara, Broida Hall, Building 562, Santa Barbara, CA 93106E. PascaleF. PiacentiniDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyD. PogosyanCanadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, CanadaF. PongettiDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, ItalyS. PrunetCanadian Institute for Theoretical Astrophysics, University of Toronto, 60 St. George Street, Toronto, ON M5S 3H8, CanadaG. RomeoIstituto Nazionale di Geofisica, Via di Vigna Murata, 605, I-00143 Rome, ItalyJ. E. RuhlDepartment of Physics, University of California at Santa Barbara, Broida Hall, Building 562, Santa Barbara, CA 93106F. ScaramuzziDipartimento di Fisica, Università La Sapienza, Piazzale Aldo Moro, 2, I-00185 Rome, Italy
2002en
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Annotatsiya
This paper presents a measurement of the angular power spectrum of the Cosmic Microwave Background from l=75 to l=1025 (~10' to 5 degrees) from a combined analysis of four 150 GHz channels in the BOOMERANG experiment. The spectrum contains multiple peaks and minima, as predicted by standard adiabatic-inflationary models in which the primordial plasma undergoes acoustic oscillations. These results significantly constrain the values of Omega_tot, Omega_b h^2, Omega_c h^2 and n_s.
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