Professor Pedro Ferreira: Publications

From the time-ordered data to the Maximum-Likelihood temperature maps of the Cosmic Microwave Backgorund anisotropy

(2000)

Authors:

R Stompor, A Balbi, J Borrill, P Ferreira, S Hanany, A Jaffe, A Lee, S Oh, B Rabii, P Richards, G Smoot, C Winant, J-HP Wu

Constraints on Cosmological Parameters from MAXIMA-1

The Astrophysical Journal American Astronomical Society 545:1 (2000) l1-l4

Authors:

A Balbi, P Ade, J Bock, J Borrill, A Boscaleri, P De Bernardis, PG Ferreira, S Hanany, V Hristov, AH Jaffe, AT Lee, S Oh, E Pascale, B Rabii, PL Richards, GF Smoot, R Stompor, CD Winant, JHP Wu

MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on Angular Scales of 10'-5°

The Astrophysical Journal American Astronomical Society 545:1 (2000) l5-l9

Authors:

S Hanany, P Ade, A Balbi, J Bock, J Borrill, A Boscaleri, P de Bernardis, PG Ferreira, VV Hristov, AH Jaffe, AE Lange, AT Lee, PD Mauskopf, CB Netterfield, S Oh, E Pascale, B Rabii, PL Richards, GF Smoot, R Stompor, CD Winant, JHP Wu

First results from the BOOMERanG experiment

ArXiv astro-ph/0011469 (2000)

Authors:

P de Bernardis, PAR Ade, JJ Bock, JR Bond, J Borrill, A Boscaleri, K Coble, BP Crill, G De Gasperis, G De Troia, PC Farese, PG Ferreira, K Ganga, M Giacometti, E Hivon, VV Hristov, A Iacoangeli, AH Jaffe, AE Lange, L Martinis, S Masi, P Mason, PD Mauskopf, A Melchiorri, L Miglio, T Montroy, CB Netterfield, E Pascale, F Piacentini, D Pogosyan, F Pongetti, S Prunet, S Rao, G Romeo, JE Ruhl, F Scaramuzzi, D Sforna, N Vittorio

Abstract:

We report the first results from the BOOMERanG experiment, which mapped at 90, 150, 240 and 410 GHz a wide (3%) region of the microwave sky with minimal local contamination. From the data of the best 150 GHz detector we find evidence for a well defined peak in the power spectrum of temperature fluctuations of the Cosmic Microwave Background, localized at $\ell = 197 \pm 6$, with an amplitude of $(68 \pm 8) \mu K_{CMB}$. The location, width and amplitude of the peak is suggestive of acoustic oscillations in the primeval plasma. In the framework of inflationary adiabatic cosmological models the measured spectrum allows a Bayesian estimate of the curvature of the Universe and of other cosmological parameters. With reasonable priors we find $\Omega = (1.07 \pm 0.06)$ and $n_s = (1.00 \pm 0.08)$ (68%C.L.) in excellent agreement with the expectations from the simplest inflationary theories. We also discuss the limits on the density of baryons, of cold dark matter and on the cosmological constant.

CMB Analysis of Boomerang & Maxima & the Cosmic Parameters {Omega_tot,Omega_b h^2,Omega_cdm h^2,Omega_Lambda,n_s}

ArXiv astro-ph/0011378 (2000)

Authors:

JR Bond, P Ade, A Balbi, J Bock, J Borrill, A Boscaleri, K Coble, B Crill, P de Bernardis, P Farese, P Ferreira, K Ganga, M Giacometti, S Hanany, E Hivon, V Hristov, A Iacoangeli, A Jaffe, A Lange, A Lee, L Martinis, S Masi, P Mauskopf, A Melchiorri, T Montroy, B Netterfield, S Oh, E Pascale, F Piacentini, D Pogosyan, S Prunet, B Rabii, S Rao, P Richards, G Romeo, J Ruhl, F Scaramuzzi, D Sforna, K Sigurdson, G Smoot, R Stompor, C Winant, P Wu

Abstract:

We show how estimates of parameters characterizing inflation-based theories of structure formation localized over the past year when large scale structure (LSS) information from galaxy and cluster surveys was combined with the rapidly developing cosmic microwave background (CMB) data, especially from the recent Boomerang and Maxima balloon experiments. All current CMB data plus a relatively weak prior probability on the Hubble constant, age and LSS points to little mean curvature (Omega_{tot} = 1.08\pm 0.06) and nearly scale invariant initial fluctuations (n_s =1.03\pm 0.08), both predictions of (non-baroque) inflation theory. We emphasize the role that degeneracy among parameters in the L_{pk} = 212\pm 7 position of the (first acoustic) peak plays in defining the $\Omega_{tot}$ range upon marginalization over other variables. Though the CDM density is in the expected range (\Omega_{cdm}h^2=0.17\pm 0.02), the baryon density Omega_bh^2=0.030\pm 0.005 is somewhat above the independent 0.019\pm 0.002 nucleosynthesis estimate. CMB+LSS gives independent evidence for dark energy (Omega_\Lambda=0.66\pm 0.06) at the same level as from supernova (SN1) observations, with a phenomenological quintessence equation of state limited by SN1+CMB+LSS to w_Q<-0.7 cf. the w_Q=-1 cosmological constant case.

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