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23 results on '"G. De Troia"'

1. Searching for non-Gaussian signals in the BOOMERANG 2003 CMB maps

Author

P. Cabella, Dmitry Pogosyan, Pedro G. Ferreira, Ted Kisner, Enzo Pascale, Peter A. R. Ade, Martin Kunz, S. Ricciardi, M. Veneziani, Max Tegmark, F. Piacentini, J. R. Bond, Paolo Natoli, Andrew E. Lange, Philip Daniel Mauskopf, Eric Hivon, Silvia Masi, T. E. Montroy, Calvin B. Netterfield, Simon Prunet, G. Di Stefano, G. de Gasperis, B. P. Crill, Andrew H. Jaffe, Sabino Matarrese, Nicola Vittorio, P. Santini, Alessandro Melchiorri, A. de Oliveira-Costa, A. Boscaleri, G. Polenta, Julian Borrill, J. E. Ruhl, Giovanni Romeo, G. De Troia, Michele Liguori, W. C. Jones, James J. Bock, C. J. MacTavish, P. de Bernardis, and Carlo R. Contaldi

Subjects
Physics, cosmic microwave background, Gaussian, Cosmic microwave background, Astrophysics (astro-ph), Cosmic background radiation, Estimator, FOS: Physical sciences, Astronomy and Astrophysics, Cosmology: Cosmic Microwave Background, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, symbols.namesake, Amplitude, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, Minkowski space, symbols, Statistical physics, Nonlinear coupling, QC
Abstract

We analyze the BOOMERanG 2003 (B03) 145 GHz temperature map to constrain the amplitude of a non Gaussian, primordial contribution to CMB fluctuations. We perform a pixel space analysis restricted to a portion of the map chosen in view of high sensitivity, very low foreground contamination and tight control of systematic effects. We set up an estimator based on the three Minkowski functionals which relies on high quality simulated data, including non Gaussian CMB maps. We find good agreement with the Gaussian hypothesis and derive the first limits based on BOOMERanG data for the non linear coupling parameter f_NL as -300, Comment: accepted for publication in ApJ. Letters

Published
2016
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2. BOOMERanG constraints on primordial non-Gaussianity from analytical Minkowski functionals

Author

W. C. Jones, Peter A. R. Ade, Chiaki Hikage, B. P. Crill, Max Tegmark, Philip Daniel Mauskopf, Nicola Vittorio, Eiichiro Komatsu, T. E. Montroy, Enzo Pascale, G. De Troia, Ted Kisner, G. Di Stefano, G. Polenta, C. J. MacTavish, F. Piacentini, Julian Borrill, P. de Bernardis, S. Ricciardi, Carlo R. Contaldi, Andrew E. Lange, J. E. Ruhl, Eric Hivon, Calvin B. Netterfield, Silvia Masi, Alessandro Melchiorri, A. de Oliveira-Costa, James J. Bock, Giovanni Romeo, J. R. Bond, G. de Gasperis, M. Veneziani, Paolo Natoli, M. Migliaccio, and A. Boscaleri

Subjects
Physics, Field (physics), 010308 nuclear & particles physics, Cosmic microwave background, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Joint analysis, 01 natural sciences, Space and Planetary Science, Coupling parameter, Non-Gaussianity, 0103 physical sciences, Minkowski space, Limit (mathematics), 010303 astronomy & astrophysics, Mathematical physics
Abstract

We use Minkowski Functionals (MF) to constrain a primordial non-Gaussian contribution to the CMB intensity field as observed in the 150 GHz and 145 GHz BOOMERanG maps from the 1998 and 2003 flights, respectively, performing for the first time a joint analysis of the two datasets. A perturbative expansion of the MF formulae in the limit of a weakly non-Gaussian field yields analytical formulae, derived by Hikage et al. (2006), which can be used to constrain the coupling parameter f_NL without the need for non-Gaussian simulations. We find -1020

Published
2010
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3. Observations of the temperature and polarization anisotropies with Boomerang 2003

Author

Giovanni Romeo, F. Piacentini, A. de Oliveira-Costa, S. Ricciardi, Paola Santini, C. J. MacTavish, J. E. Ruhl, J. R. Bond, B. P. Crill, Andrew E. Lange, Silvia Masi, Calvin B. Netterfield, T. S. Kisner, W. C. Jones, Nicola Vittorio, G. De Troia, E. Hivon, G. de Gasperis, T. E. Montroy, Dmitry Pogosyan, Julian Borrill, P. de Bernardis, G. Polenta, A. Boscaleri, Paolo Cabella, Max Tegmark, Peter A. R. Ade, Philip Daniel Mauskopf, M. Veneziani, Andrew H. Jaffe, Alessandro Melchiorri, Simon Prunet, J. J. Bock, Enzo Pascale, Carlo R. Contaldi, P. Natoli, and G. Di Stefano

Subjects
media_common.quotation_subject, Cosmic microwave background, BOOMERanG experiment, Cosmology, Observations, Polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, cosmic microwave background, cosmology, observations, polarization, Spectral line, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Planck, media_common, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Galactic plane, Polarization (waves), Square degree, Space and Planetary Science, Sky, symbols
Abstract

The Boomerang experiment completed its final long duration balloon (LDB) flight over Antarctica in January 2003. The focal plane was upgraded to accommodate four sets of 145 GHz polarization sensitive bolometers (PSBs), identical to those to be flown on the Planck HFI instrument. Approximately, 195 hours of science observations were obtained during this flight, including 75 hours distributed over 1.84% of the sky and an additional 120 hours concentrated on a region covering 0.22% of the sky. We derive the angular power spectra of the cosmic microwave background (cmb) temperature and polarization anisotropies from these data. The temperature anisotropies are detected with high signal to noise on angular scales ranging from several degrees to ∼10 arcminutes. The curl-free (EE) component is detected at ∼4.8σ, and a two-sigma upper limit on the curl (BB) component of 8.6 μK2 is obtained on scales corresponding to ∼0.5°. Both the temperature and polarization anisotropies are found to be consistent with a concordance ΛCDM cosmology that is seeded by adiabatic density perturbations. In addition to the cmb observations, Boomerang03 surveyed a ∼300 square degree region centered on the Galactic plane. These observations represent the first light for polarization sensitive bolometers, which are currently operational in two South-Pole based polarimeters, as well as Planck HFI, at frequencies ranging from 100 to 350 GHz (3 mm to 850 μm).

Published
2006
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4. Instrument, method, brightness, and polarization maps from the 2003 flight of BOOMERanG

Author

Simon Prunet, Carlo R. Contaldi, P. Cabella, A. Boscaleri, Federico Nati, M. Veneziani, G. de Gasperis, Max Tegmark, Philip Daniel Mauskopf, S. Ricciardi, J. Borrill, Andrew H. Jaffe, L. Nati, F. Piacentini, Enzo Pascale, Calvin B. Netterfield, Giovanni Romeo, A. de Oliveira-Costa, G. Di Stefano, B. P. Crill, A. Iacoangeli, Andrew E. Lange, Theodore Kisner, Peter Mason, W. C. Jones, Nicola Vittorio, P. Natoli, Peter A. R. Ade, Dmitry Pogosyan, G. Polenta, Paola Santini, T. E. Montroy, G. De Troia, Hristov, J. R. Bond, James J. Bock, P. Ehlers, J. E. Ruhl, E. Hivon, Silvia Masi, C. J. MacTavish, E. Torbet, P. de Bernardis, and C. Marini-Bettolo

Subjects
cosmic microwave background, Brightness, instrumentation: polarimeters, techniques: polarimetric, ISM: clouds, ISM: HII regions, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, symbols.namesake, instrumentation : polarimeters, ism : clouds, ism : hii regions, ism: clouds, ism: hii regions, techniques : polarimetric, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Stokes parameters, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, media_common, Physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galactic plane, Polarization (waves), CMB cold spot, Amplitude, 13. Climate action, Space and Planetary Science, Sky, symbols
Abstract

We present the BOOMERanG-03 experiment and maps of the Stokes parameters I, Q, U of the microwave sky obtained during a 14 day balloon flight in 2003. Three regions of the southern sky were surveyed: a deep survey (~ 90 square degrees) and a shallow survey (~ 750 square degrees) at high Galactic latitudes (both centered at RA ~ 5.5 h, dec ~ -45 deg) and a survey of ~ 300 square degrees across the Galactic plane at RA ~ 9.1 h, dec ~ -47 deg. All three surveys were carried out in three wide frequency bands centered at 145, 245 and 345 GHz, with an angular resolution of ~ 10'. The 145 GHz maps of Stokes I are dominated by Cosmic Microwave Background (CMB) temperature anisotropy, which is mapped with high signal to noise ratio. The measured anisotropy pattern is consistent with the pattern measured in the same region by BOOMERanG-98 and by WMAP. The 145 GHz maps of Stokes Q and U provide a robust statistical detection of polarization of the CMB when subjected to a power spectrum analysis. This amplitude of the polarization is consistent with that of the CMB in the $\Lambda$CDM cosmological scenario. At 145 GHz, in the CMB surveys, the intensity and polarization of the astrophysical foregrounds are found to be negligible with respect to the cosmological signal. At 245 and 345 GHz we detect ISD emission correlated to the 3000 GHz IRAS/DIRBE maps, and give upper limits for any other non-CMB component. We also present intensity maps of the surveyed section of the Galactic plane. These are compared to monitors of different interstellar components, showing that a variety of emission mechanisms is present in that region., Comment: see http://oberon.roma1.infn.it/boomerang/b2k and http://cmb.phys.cwru.edu/boomerang/ for a high resolution version

Published
2006
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5. ELLIPTICITY ANALYSIS OF THE BOOMERanG CMB MAPS

Author

Enzo Pascale, F. Piacentini, Philip Daniel Mauskopf, Carlo Luciano Bianco, Silvia Masi, Andrew E. Lange, Eric Hivon, P. de Bernardis, T. E. Montroy, James J. Bock, B. P. Crill, Calvin B. Netterfield, G. Polenta, A. L. Kashin, Ken Ganga, J. E. Ruhl, Paolo Natoli, G. De Troia, M. Giacometti, Viktor Hristov, Vahe Gurzadyan, Peter A. R. Ade, and A. Boscaleri

Subjects
Physics, cosmic microwave background, Orientation (computer vision), Astrophysics (astro-ph), Noise map, Cosmic microwave background, FOS: Physical sciences, Estimator, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Curvature, Mixing (mathematics), Space and Planetary Science, Anisotropy, Mathematical Physics, Noise (radio)
Abstract

The properties of the Cosmic Microwave Background (CMB) maps carry valuable cosmological information. Here we report the results of the analysis hot and cold CMB anisotropy spots in the BOOMERanG 150 GHz map in terms of number, area, ellipticity, vs. temperature threshold. We carried out this analysis for the map obtained by summing independent measurement channels (signal plus noise map) and for a comparison map (noise only map) obtained by differencing the same channels. The anisotropy areas (spots) have been identified for both maps for various temperature thresholds and a catalog of the spots has been produced. The orientation (obliquity) of the spots is random for both maps. We computed the mean elongation of spots obtained from the maps at a given temperature threshold using a simple estimator. We found that for the sum map there is a region of temperature thresholds where the average elongation is not dependent on the threshold. Its value is ~ 2.3 for cold areas and ~ 2.2 for hot areas. This is a non-trivial result. The bias of the estimator is less than 0.4 for areas of size less than 30', and smaller for larger areas. The presence of noise also biases the ellipticity by less than 0.3. These biases have not been subtracted in the results quoted above. The threshold independent and random obliquity behaviour in the sum map is stable against pointing reconstruction accuracy and noise level of the data, thus confirming that these are actual properties of the dataset. The data used here give a hint of high ellipticity for the largest spots. Analogous elongation properties of CMB anisotropies had been detected for COBE-DMR 4-year data. If this is due to geodesics mixing, it would point to a non zero curvature of the Universe., Comment: Addendums on the more detailed description of the algorithms and on the non zero curvature

Published
2003
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6. Search for Non-Gaussian Signals in the BOOMERANG Maps: Pixel-Space Analysis

Author

Simon Prunet, Julian Borrill, Dmitry Pogosyan, Andrew E. Lange, Eric Hivon, B. P. Crill, F. Piacentini, Carlo R. Contaldi, Nicola Vittorio, Philip Daniel Mauskopf, A. Zeppilli, Calvin B. Netterfield, J. E. Ruhl, Alessandro Melchiorri, Ken Ganga, Giovanni Romeo, T. E. Montroy, G. Polenta, Enzo Pascale, Peter A. R. Ade, A. H. Jaffe, J. R. Bond, Paolo Natoli, James J. Bock, G. De Troia, M. Giacometti, Viktor Hristov, G. de Gasperis, P. de Bernardis, Silvia Masi, and A. Boscaleri

Subjects
cosmic microwave background, Field (physics), Gaussian, media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Minkowski space, Range (statistics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Cosmology: Cosmic Microwave Background, Astronomy and Astrophysics, Space and Planetary Science, Sky, Skewness, Kurtosis, symbols
Abstract

We search the BOOMERanG maps of the anisotropy of the Cosmic Microwave Background (CMB) for deviations from gaussianity. In this paper we focus on analysis techniques in pixel-space, and compute skewness, kurtosis and Minkowski functionals for the BOOMERanG maps and for gaussian simulations of the CMB sky. We do not find any significant deviation from gaussianity in the high galactic latitude section of the 150 GHz map. We do find deviations from gaussianity at lower latitudes and at 410 GHz, and we ascribe them to Galactic dust contamination. Using non-gaussian simulations of instrumental systematic effects, of foregrounds, and of sample non-gaussian cosmological models, we set upper limits to the non-gaussian component of the temperature field in the BOOMERanG maps. For fluctuations distributed as a 1 DOF $\chi^2$ mixed to the main gaussian component our upper limits are in the few % range., Comment: changes to reflect version accepted by ApJ Letters

Published
2002
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7. The BOOMERANG North America Instrument: A Balloon‐borne Bolometric Radiometer Optimized for Measurements of Cosmic Background Radiation Anisotropies from 0.̊3 to 4o

Author

H. M. Del Castillo, Calvin B. Netterfield, P. A. R. Ade, J. E. Ruhl, E. Hivon, J. J. Bock, P. de Bernardis, Paolo Palangio, B. P. Crill, A. Iacoangeli, F. Piacentini, P. D. Mauskopf, Enzo Pascale, Alvise Raccanelli, S. Rao, A. Boscaleri, G. De Troia, G. Romeo, Andrew E. Lange, M. Giacometti, Silvia Masi, V. V. Hristov, P. Cardoni, R. Bathia, P. C. Farese, L. Miglio, and Francesco Scaramuzzi

Subjects
Physics, Radiometer, business.industry, media_common.quotation_subject, Astrophysics (astro-ph), Bolometer, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic background radiation, FOS: Physical sciences, Spectral density, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cryogenics, Radiation, law.invention, Optics, Space and Planetary Science, law, Sky, business, media_common
Abstract

We describe the BOOMERANG North America (BNA) instrument, a balloon-borne bolometric radiometer designed to map the Cosmic Microwave Background (CMB) radiation with 0.3 deg resolution over a significant portion of the sky. This receiver employs new technologies in bolometers, readout electronics, millimeter-wave optics and filters, cryogenics, scan and attitude reconstruction. All these subsystems are described in detail in this paper. The system has been fully calibrated in flight using a variety of techniques which are described and compared. It has been able to obtain a measurement of the first peak in the CMB angular power spectrum in a single balloon flight, few hours long, and was a prototype of the BOOMERANG Long Duration Balloon (BLDB) experiment., 40 pages, 22 figures, submitted to ApJ

Published
2002
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8. Residual noise covariance for Planck low-resolution data analysis

Author

T. Poutanen, Hannu Kurki-Suonio, F. Paci, G. De Troia, Ted Kisner, James G. Bartlett, Alessandro Gruppuso, Charles R. Lawrence, Radek Stompor, E. Keihänen, Graca Rocha, Paolo Cabella, C. Cantalupo, Eric Hivon, Krzysztof M. Gorski, Reijo Keskitalo, Julian Borrill, H. K. Eriksen, Fabio Finelli, G. Polenta, Andrew H. Jaffe, A. de Rosa, M. Ashdown, G. de Gasperis, Paolo Natoli, Oxford Astrophysics, University of Oxford [Oxford], APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Dipartimento di Fisica, Universita` di Roma Tor Vergata, Università degli Studi di Roma Tor Vergata [Roma], Department of Physics, Helsinki Institute of Physics, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of Oxford, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
cosmic microwave background, cosmology: observations, methods: data analysis, methods: numerical, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Monte Carlo method, FOS: Physical sciences, Astrophysics, 01 natural sciences, 114 Physical sciences, Window function, Cosmic microwave background, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, Aliasing, 0103 physical sciences, observations [Cosmology], data analysis [Methods], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, numerical [Methods], 010308 nuclear & particles physics, HEALPix, Spectral density, Astronomy and Astrophysics, Covariance, 115 Astronomy, Space science, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Noise, Space and Planetary Science, astro-ph.CO, Astrophysics - Instrumentation and Methods for Astrophysics, Algorithm, Smoothing, Astrophysics - Cosmology and Nongalactic Astrophysics, astro-ph.IM
Abstract

29 páginas, 16+6 figuras, 4 tablas.-- et al., [Aims]: We develop and validate tools for estimating residual noise covariance in Planck frequency maps, we also quantify signal error effects and compare different techniques to produce low-resolution maps. [Methods]: We derived analytical estimates of covariance of the residual noise contained in low-resolution maps produced using a number of mapmaking approaches. We tested these analytical predictions using both Monte Carlo simulations and by applying them to angular power spectrum estimation. We used simulations to quantify the level of signal errors incurred in the different resolution downgrading schemes considered in this work. [Results]: We find excellent agreement between the optimal residual noise covariance matrices and Monte Carlo noise maps. For destriping mapmakers, the extent of agreement is dictated by the knee frequency of the correlated noise component and the chosen baseline offset length. Signal striping is shown to be insignificant when properly dealt with. In map resolution downgrading, we find that a carefully selected window function is required to reduce aliasing to the subpercent level at multipoles, ℓ > 2Nside, where Nside is the HEALPix resolution parameter. We show that, for a polarization measurement, reliable characterization of the residual noise is required to draw reliable constraints on large-scale anisotropy. [Conclusions]: Methods presented and tested in this paper allow for production of low-resolution maps with both controlled sky signal error level and a reliable estimate of covariance of the residual noise. We have also presented a method for smoothing the residual noise covariance matrices to describe the noise correlations in smoothed, bandwidth-limited maps.

Published
2010
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9. Properties of Galactic Cirrus Clouds Observed by BOOMERANG

Author

J. E. Ruhl, A. Boscaleri, G. Di Stefano, F. Piacentini, Silvia Masi, G. De Troia, A. de Oliveira-Costa, Peter A. R. Ade, Enzo Pascale, T. E. Montroy, W. C. Jones, G. Polenta, C. J. MacTavish, Davide Pietrobon, P. de Bernardis, Philip Daniel Mauskopf, Calvin B. Netterfield, Ken Ganga, Giovanni Romeo, James J. Bock, S. Ricciardi, B. P. Crill, M. Veneziani, Theodore Kisner, Andrew E. Lange, Paolo Natoli, G. de Gasperis, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, QUaD, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, cosmology: observations, ism: clouds, radio continuum: ism, submillimeter: ism, submillimiter: ism, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, ISM: clouds, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Emissivity, Angular resolution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Spectral index, 010308 nuclear & particles physics, Astronomy and Astrophysics, radio continuum: ISM, 13. Climate action, Space and Planetary Science, submillimeter: ISM, Cirrus, Microwave, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The physical properties of galactic cirrus emission are not well characterized. BOOMERanG is a balloon-borne experiment designed to study the cosmic microwave background at high angular resolution in the millimeter range. The BOOMERanG 245 and 345GHz channels are sensitive to interstellar signals, in a spectral range intermediate between FIR and microwave frequencies. We look for physical characteristics of cirrus structures in a region at high galactic latitudes (b~-40{\deg}) where BOOMERanG performed its deepest integration, combining the BOOMERanG data with other available datasets at different wavelengths. We have detected eight emission patches in the 345 GHz map, consistent with cirrus dust in the Infrared Astronomical Satellite maps. The analysis technique we have developed allows to identify the location and the shape of cirrus clouds, and to extract the flux from observations with different instruments at different wavelengths and angular resolutions. We study the integrated flux emitted from these cirrus clouds using data from Infrared Astronomical Satellite (IRAS), DIRBE, BOOMERanG and Wilkinson Microwave Anisotropy Probe (WMAP) in the frequency range 23-3000 GHz (13 mm 100 micron wavelength). We fit the measured spectral energy distributions with a combination of a grey body and a power-law spectra considering two models for the thermal emission. The temperature of the thermal dust component varies in the 7 - 20 K range and its emissivity spectral index is in the 1 - 5 range. We identified a physical relation between temperature and spectral index as had been proposed in previous works. This technique can be proficiently used for the forthcoming Planck and Herschel missions data., Comment: accepted for publication in The Astrophysical Journal

Published
2010
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10. Planck pre-launch status: The Planck-LFI programme

Author

P. B. Lilje, Amedeo Balbi, Fabio Finelli, S. Leach, Roger J. Hoyland, L. A. Wade, Krzysztof M. Gorski, F. Gasparo, E. Franceschi, Luigi Danese, Jose M. Diego, T. Riller, Christopher G. Paine, M. C. Falvella, Hannu Kurki-Suonio, A. Mennella, Francesca Perrotta, Joseph Silk, Matthias Bartelmann, U. Dörl, L. Mendes, A. Bonaldi, Jose Alberto Rubino-Martin, Carlo Burigana, Sabino Matarrese, Anne Lähteenmäki, G. de Zotti, Torsten A. Enßlin, G. Prézeau, M. Bremer, E. Keihänen, M. Prina, S. Galeotta, M. Sandri, G. De Troia, X. Dupac, L. Popa, L. Pérez-Cuevas, S. Donzelli, Althea Wilkinson, Adam Moss, M. Maris, Alessandro Melchiorri, F. Pasian, Kevin M. Huffenberger, R. Hell, J. Dick, Rafael Rebolo, R. J. Davis, Reijo Keskitalo, F. Gomez, M. López-Caniego, Michael Janssen, Ted Kisner, G. Giardino, Luca Terenzi, Davide Maino, Anna Gregorio, M. Tomasi, N. Mandolesi, F. K. Hansen, Pradeep Bhandari, Eduardo Artal, Fabrizio Villa, Enrique Martínez-González, Charles R. Lawrence, Todd Gaier, J. P. Leahy, O. D'Arcangelo, Andrea Zacchei, T. Passvogel, J. Sternberg, Alessandro Gruppuso, F. Matthai, Julian Borrill, Paolo Cabella, S. Ricciardi, Steven Levin, Jörg P. Rachen, Nicola Vittorio, Peter Meinhold, N. Morisset, Marc Türler, Jussi Varis, Marco Bersanelli, R. Rohlfs, A. Nash, Sergi R. Hildebrandt, B. Cappellini, Diego Herranz, J. Marti-Canales, J. González-Nuevo, Martin White, Douglas Scott, George F. Smoot, R. B. Barreiro, N. Roddis, Emanuele Salerno, Michael Seiffert, P. Vielva, S. N. White, Marcella Massardi, J. A. Tauber, F. Cuttaia, Renzo Nesti, T. Poutanen, A. J. Banday, R. C. Butler, R. D. Davies, Robert C. Bowman, S. R. Lowe, José Miguel Herreros, Luca Stringhetti, Paolo Natoli, J. Tuovinen, H. K. Eriksen, Rodrigo Leonardi, David Pearson, Bruce Partridge, T. Jaffe, G. Polenta, Clive Dickinson, G. de Gasperis, M. Frailis, L. De Angelis, Carlo Baccigalupi, Philip Lubin, C. Cantalupo, A. de Rosa, F. Stivoli, Gianluca Morgante, Andrea Zonca, G. Crone, Luca Valenziano, T. J. L. Courvoisier, M. Malaspina, Carlo Sozzi, Graca Rocha, M. Reinecke, A. Simonetto, G. Morigi, K. Bennett, W. Hovest, Department of Physics, Helsinki Institute of Physics, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Mandolesi, N, Bersanelli, M, BUTLER R., C, Artal, E, Baccigalupi, C, Balbi, A, BANDAY A., J, BARREIRO R., B, Bartelmann, M, Bennett, K, Bhandari, P, Bonaldi, A, Borrill, J, Bremer, M, Burigana, C, BOWMAN R., C, Cabella, P, Cantalupo, C, Cappellini, B, Courvoisier, T, Crone, G, Cuttaia, F, Danese, L, Darcangelo, O, DAVIES R., D, DAVIS R., J, DE ANGELIS, L, DE GASPERIS, G, DE ROSA, A, DE TROIA, G, DE ZOTTI, G, Dick, J, Dickinson, C, DIEGO J., M, Donzelli, S, Dorl, U, Dupac, X, ENLIN T., A, ERIKSEN H., K, FALVELLA M., C, Finelli, F, Frailis, M, Franceschi, E, Gaier, T, Galeotta, S, Gasparo, F, Giardino, G, Gomez, F, GONZALEZ NUEVO, J, GORSKI K., M, Gregorio, Anna, Gruppuso, A, Hansen, F, Hell, R, Herranz, D, HERREROS J., M, Hildebrandt, S, Hovest, W, Hoyland, R, Huffenberger, K, Janssen, M, Jaffe, T, Keihanen, E, Keskitalo, R, Kisner, T, KURKI SUONIO, H, Lahteenmaki, A, LAWRENCE C., R, M., S, J., Leach, Leahy, P, Leonardi, R, Levin, S, LILJE P., B, LOPEZ CANIEGO, M, LOWE S., R, LUBIN P., M, Maino, D, Malaspina, M, Maris, M, MARTI CANALES, J, MARTINEZ GONZALEZ, E, Massardi, M, Matarrese, S, Matthai, F, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Morgante, G, Morigi, G, Morisset, N, Moss, A, Nash, A, Natoli, P, Nesti, R, Paine, C, Partridge, B, Pasian, F, Passvogel, T, Pearson, D, PEREZ CUEVAS, L, Perrotta, F, Polenta, G, POPA L., A, Poutanen, T, Prezeau, G, Prina, M, RACHEN J., P, Rebolo, R, Reinecke, M, Ricciardi, S, Riller, T, Rocha, G, Roddis, N, Rohlfs, R, RUBINO MARTIN J., A, Salerno, E, Sandri, M, Scott, D, Seiffert, M, Silk, J, Simonetto, A, SMOOT G., F, Sozzi, C, Sternberg, J, Stivoli, F, Stringhetti, L, Tauber, J, Terenzi, L, Tomasi, M, Tuovinen, J, Turler, M, Valenziano, L, Varis, J, Vielva, P, Villa, F, Vittorio, N, Wade, L, White, M, White, S, Wilkinson, A, Zacchei, A, Zonca, A., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Universidad de Cantabria

Subjects
Electromagnetic spectrum, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], submillimeter: generaltelescopes, cosmic microwave background, space vehicles: instruments, submillimeter: general, instrumentation: polarimeters, telescopes, instrumentation: detectors, Cosmic microwave background, data analysis, Astrophysics, general [Submillimeter], 7. Clean energy, 01 natural sciences, LARGE-AREA TELESCOPE, CMB physics, cosmic microwave backgroundin, 010303 astronomy & astrophysics, detectors [Instrumentation], media_common, Physics, Data processing, Planck ESA mission, Galactic and extragalactic asrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, STRAYLIGHT CONTAMINATION, LOW-FREQUENCY INSTRUMENT, DMR SKY MAPS, MICROWAVE BACKGROUND MAPS, galactic and extragalactic astrophysics, symbols, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, GALACTIC FOREGROUNDS, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], COMPONENT SEPARATION, Cosmic microwawe background, media_common.quotation_subject, ANGULAR POWER SPECTRA, education, strumentation: detectors, FOS: Physical sciences, Context (language use), Astrophysics::Cosmology and Extragalactic Astrophysics, 114 Physical sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], instruments [Space vehicles], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Calibration, Ground segment, Planck, Instrumentation and Methods for Astrophysics (astro-ph.IM), DATA-PROCESSING CENTERS, Remote sensing, polarimeters [Instrumentation], 010308 nuclear & particles physics, Astronomy and Astrophysics, calibration, 115 Astronomy, Space science, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Sky, NON-GAUSSIANITY, space vehicles, Telescopes
Abstract

24 páginas, 16 figuras, 5 tablas.-- et al., This paper provides an overview of the Low Frequency Instrument (LFI) programme within the ESA Planck mission. The LFI instrument has been developed to produce high precision maps of the microwave sky at frequencies in the range 27–77 GHz, below the peak of the cosmic microwave background (CMB) radiation spectrum. The scientific goals are described, ranging from fundamental cosmology to Galactic and extragalactic astrophysics. The instrument design and development are outlined, together with the model philosophy and testing strategy. The instrument is presented in the context of the Planck mission. The LFI approach to ground and inflight calibration is described. We also describe the LFI ground segment. We present the results of a number of tests demonstrating the capability of the LFI data processing centre (DPC) to properly reduce and analyse LFI flight data, from telemetry information to calibrated and cleaned time ordered data, sky maps at each frequency (in temperature and polarization), component emission maps (CMB and diffuse foregrounds), catalogs for various classes of sources (the Early Release Compact Source Catalogue and the Final Compact Source Catalogue). The organization of the LFI consortium is briefly presented as well as the role of the core team in data analysis and scientific exploitation. All tests carried out on the LFI flight model demonstrate the excellent performance of the instrument and its various subunits. The data analysis pipeline has been tested and its main steps verified. In the first three months after launch, the commissioning, calibration, performance, and verification phases will be completed, after which Planck will begin its operational life, in which LFI will have an integral part., The Planck-LFI project is developed by an International Consortium led by Italy and involving Canada, Finland, Germany, Norway, Spain, Switzerland, UK and USA. The Italian contribution to Planck is supported by the Agenzia Spaziale Italiana (ASI) and INAF. We also wish to thank the many people of the Herschel/Planck Project and RSSD of ESA, ASI, THALES Alenia Space Industries and the LFI Consortium that have contributed to the realization of LFI. We are grateful to our HFI colleagues for such a fruitful collaboration during so many years of common work. The German participation at the Max-Planck-Institut für Astrophysik is funded by the Bundesministerium für Wirtschaft und Technologie through the Raumfahrt- Agentur of the Deutsches Zentrum für Luft- und Raumfahrt (DLR) [FKZ: 50 OP 0901] and by the Max-Planck-Gesellschaft (MPG). The Finnish contribution is supported by the Finnish Funding Agency for Technology and Innovation (Tekes) and the Academy of Finland. The Spanish participation is funded by Ministerio de Ciencia e Innovacion through the project ESP2004-07067-C03 and AYA2007-68058-C03. The UK contribution is supported by the Science and Technology Facilities Council (STFC). C. Baccigalupi and F. Perrotta acknowledge partial support of the NASA LTSA Grant NNG04CG90G.

Published
2010
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11. SUBDEGREE SUNYAEV-ZEL'DOVICH SIGNAL FROM MULTIFREQUENCY BOOMERANG OBSERVATIONS

Author

Giovanni Romeo, M. Veneziani, Paolo Serra, Paolo Natoli, Paola Santini, W. C. Jones, T. E. Montroy, Max Tegmark, Philip Daniel Mauskopf, F. Piacentini, G. de Gasperis, Carlo R. Contaldi, Ken Ganga, G. Polenta, B. P. Crill, J. R. Bond, C. J. MacTavish, Alessandro Melchiorri, A. de Oliveira-Costa, Davide Pietrobon, S. Ricciardi, Nicola Vittorio, A. Boscaleri, Calvin B. Netterfield, Julian Borrill, Asantha Cooray, Andrew E. Lange, Eric Hivon, Theodore Kisner, Peter A. R. Ade, Enzo Pascale, P. de Bernardis, Paolo Cabella, A. Amblard, Silvia Masi, G. Di Stefano, James J. Bock, J. E. Ruhl, G. De Troia, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Dipartimento di Fisica, Universita` di Roma Tor Vergata, Università degli Studi di Roma Tor Vergata [Roma], APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Physique Corpusculaire et Cosmologie - Collège de France (PCC), and Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Normalization (statistics), cosmic microwave background, Photon, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmological parameters, cosmology: observations, large-scale structure of universe, 01 natural sciences, Signal, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Anisotropy, 010303 astronomy & astrophysics, media_common, Physics, Spectral signature, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Sigma, Astronomy and Astrophysics, Universe, Space and Planetary Science, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Sunyaev-Zel'dovich (SZ) effect is the inverse Compton-scattering of cosmic microwave background (CMB) photons by hot electrons in the intervening gas throughout the universe. The effect has a distinct spectral signature that allows its separation from other signals in multifrequency CMB datasets. Using CMB anisotropies measured at three frequencies by the BOOMERanG 2003 flight we constrain SZ fluctuations in the 10 arcmin to 1 deg angular range. Propagating errors and potential systematic effects through simulations, we obtain an overall upper limit of 15.3 uK (2 sigma) for rms SZ fluctuations in a broad bin between multipoles of of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. When combined with other CMB anisotropy and SZ measurements, we find that the local universe normalization of the density perturbations is sigma-8(SZ) < 0.96 at the 95% confidence level, consistent with sigma-8 determined from primordial perturbations., accepted for publication in ApJ. Letters

Published
2009
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12. Searching for non-Gaussian signals in the BOOMERanG 2003 CMB map: Preliminary results

Author

Calvin B. Netterfield, T. E. Montroy, A. Boscaleri, Carlo R. Contaldi, M. Veneziani, Peter A. R. Ade, Paolo Natoli, P. Cabella, W. C. Jones, Giovanni Romeo, Julian Borrill, G. Di Stefano, Martin Kunz, Andrew H. Jaffe, F. Piacentini, Simon Prunet, Alessandro Melchiorri, Dmitry Pogosyan, A. de Oliveira-Costa, Enzo Pascale, Andrew E. Lange, Ted Kisner, Max Tegmark, Eric Hivon, James J. Bock, Philip Daniel Mauskopf, J. R. Bond, G. de Gasperis, B. P. Crill, G. Polenta, P. Santini, Nicola Vittorio, S. Ricciardi, Sabino Matarrese, Silvia Masi, Pedro G. Ferreira, Michele Liguori, C. J. MacTavish, P. de Bernardis, G. De Troia, and J. E. Ruhl

Subjects
Physics, Pixel, Gaussian, Cosmic microwave background, Estimator, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), Computational physics, symbols.namesake, Amplitude, Space and Planetary Science, Minkowski space, symbols, Sensitivity (control systems)
Abstract

We analyze the BOOMERanG 2003 (B03) 145 GHz temperature map to constrain the amplitude of a non Gaussian, primordial contribution to CMB fluctuations. We perform a pixel space analysis restricted to a portion of the map chosen in view of high sensitivity, very low foreground contamination and tight control of systematic effects. We set up an estimator based on the three Minkowski functionals which relies on high quality simulated data, including non Gaussian CMB maps. We find good agreement with the Gaussian hypothesis and derive the first limits based on BOOMERanG data for the non linear coupling parameter f_NL as -300

Published
2007

13. CMB polarization with BOOMERANG 2003

Author

T. E. Montroy, Alessandro Melchiorri, Paola Santini, T. S. Kisner, E. Hivon, C. Marini-Bettolo, Giovanni Romeo, Calvin B. Netterfield, A. Boscaleri, Federico Nati, S. Ricciardi, F. Piacentini, L. Nati, J. E. Ruhl, Dmitry Pogosyan, A. de Oliveira-Costa, Paolo Cabella, Enzo Pascale, Andrew H. Jaffe, J. J. Bock, Julian Borrill, Silvia Masi, B. P. Crill, P. Natoli, Carlo R. Contaldi, Peter A. R. Ade, Nicola Vittorio, Andrew E. Lange, G. Di Stefano, C. J. MacTavish, P. de Bernardis, M. Veneziani, G. Polenta, J. R. Bond, Simon Prunet, G. De Troia, Max Tegmark, Philip Daniel Mauskopf, G. de Gasperis, and W. C. Jones

Subjects
Physics, Cosmic microwave background, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, CMB, Polarization (waves), Cosmology, Polarization, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, cmb, cosmology, polarization
Abstract

This paper reports results from the Boomerang 2003 flights, devoted to the measurement of intensity and polarization of the cosmic microwave background radiation. In particular, it is focused on the power angular power spectra and on the control of possible contamination from systematic effects and foregrounds.

Published
2007

14. The millimeter sky as seen with BOOMERanG

Author

C. Marini Bettolo, Carlo R. Contaldi, Andrew E. Lange, E. Hivon, Simon Prunet, P. Ehlers, J. E. Ruhl, S. Ricciardi, C. J. MacTavish, A. de Oliveira-Costa, P. de Bernardis, Silvia Masi, G. de Gasperis, Dmitry Pogosyan, A. Iacoangeli, J. R. Bond, J. Borrill, G. De Troia, F. Piacentini, Paola Santini, W. C. Jones, G. Polenta, Max Tegmark, Viktor Hristov, Philip Daniel Mauskopf, B. P. Crill, E. Torbet, Peter Mason, Andrew H. Jaffe, Nicola Vittorio, Calvin B. Netterfield, Federico Nati, Paolo Cabella, P. Natoli, Giovanni Romeo, L. Nati, G. Di Stefano, Enzo Pascale, T. S. Kisner, J. J. Bock, T. E. Montroy, A. Boscaleri, Peter A. R. Ade, and M. Veneziani

Subjects
cosmic microwave background anisotropy and polarization, media_common.quotation_subject, Cosmic microwave background, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radio spectrum, law.invention, Telescope, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, law, Stokes parameters, Astrophysics::Galaxy Astrophysics, media_common, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Galactic plane, galactic foreground, Polarization (waves), CMB cold spot, Space and Planetary Science, Sky, symbols, cosmology
Abstract

BOOMERanG is a balloon-borne, mm-wave scanning telescope, which measured the first images of the CMB with sub-horizon resolution in 1998. In 2003 the instrument has been flown again with polarization sensitive bolometers, and has produced maps of the Stokes parameters I, Q, U of the microwave sky. Three regions of the southern sky were surveyed: a deep (∼90 square degrees) and a shallow survey (∼750 square degrees) at high Galactic latitudes, and a survey of ∼300 square degrees across a southern section of the Galactic plane. The experiment measured simultaneously three wide frequency bands centered at 145, 245 and 345 GHz, with an angular resolution of ∼10′. The 145 GHz temperature maps are dominated by Cosmic Microwave Background (CMB) anisotropy, which is mapped with high signal to noise ratio. The map is consistent with the pattern measured in the same region by BOOMERanG-98 and by WMAP. At 145 GHz, in the high latitude surveys, the intensity and polarization of the astrophysical foregrounds are found to be negligible with respect to the cosmological signal. At 245 and 345 GHz we detect ISD emission correlated to the 3000 GHz IRAS/DIRBE maps. The Q and U maps at high latitudes are dominated by detector noise: a power spectrum analysis allows us to extract from the maps a significant CMB polarization signal.

Published
2007

15. A Measurement of the Angular Power Spectrum of the CMB Temperature Anisotropy from the 2003 Flight of BOOMERANG

Author

G. Di Stefano, Giovanni Romeo, Enzo Pascale, P. Cabella, E. Hivon, Carlo R. Contaldi, Dmitry Pogosyan, M. Veneziani, Peter A. R. Ade, G. de Gasperis, Simon Prunet, T. E. Montroy, B. P. Crill, G. De Troia, Nicola Vittorio, G. Polenta, W. C. Jones, Barth Netterfield, Max Tegmark, Philip Daniel Mauskopf, Paola Santini, J. R. Bond, Julian Borrill, Silvia Masi, Paolo Natoli, Andrew E. Lange, Andrew H. Jaffe, Alessandro Melchiorri, A. de Oliveira-Costa, C. J. MacTavish, P. de Bernardis, James J. Bock, S. Ricciardi, J. E. Ruhl, Theodore Kisner, F. Piacentini, and A. Boscaleri

Subjects
cosmic microwave background, instrumentation : detectors, Field (physics), media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology: Observations, 01 natural sciences, law.invention, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, law, 0103 physical sciences, Planck, Anisotropy, 010303 astronomy & astrophysics, media_common, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, cosmology : observations, cosmology: observations, instrumentation: detectors, Cosmology: Cosmic Microwave Background, Astronomy and Astrophysics, Instrumentation: Detectors, Space and Planetary Science, Sky, symbols, Multipole expansion
Abstract

We report on observations of the Cosmic Microwave Background (CMB) obtained during the January 2003 flight of Boomerang . These results are derived from 195 hours of observation with four 145 GHz Polarization Sensitive Bolometer (PSB) pairs, identical in design to the four 143 GHz Planck HFI polarized pixels. The data include 75 hours of observations distributed over 1.84% of the sky with an additional 120 hours concentrated on the central portion of the field, itself representing 0.22% of the full sky. From these data we derive an estimate of the angular power spectrum of temperature fluctuations of the CMB in 24 bands over the multipole range (50 < l < 1500). A series of features, consistent with those expected from acoustic oscillations in the primordial photon-baryon fluid, are clearly evident in the power spectrum, as is the exponential damping of power on scales smaller than the photon mean free path at the epoch of last scattering (l > 900). As a consistency check, the collaboration has performed two fully independent analyses of the time ordered data, which are found to be in excellent agreement., 11 pages, 7 figures, 3 tables. High resolution figures and data are available at http://cmb.phys.cwru.edu/boomerang/ and http://oberon.roma1.infn.it/boomerang/b2k

Published
2006

16. Cosmological Parameters from the 2003 Flight of BOOMERANG

Author

Peter A. R. Ade, Dmitry Pogosyan, T. E. Montroy, Andrew E. Lange, W. C. Jones, Eric Hivon, Max Tegmark, Philip Daniel Mauskopf, Theodore Kisner, M. Veneziani, B. P. Crill, F. Piacentini, Nicola Vittorio, Julian Borrill, Silvia Masi, James J. Bock, Alessandro Melchiorri, A. de Oliveira-Costa, Enzo Pascale, S. Ricciardi, A. H. Jaffe, C. J. MacTavish, A. Lewis, G. Di Stefano, Simon Prunet, P. de Bernardis, Calvin B. Netterfield, Paolo Cabella, J. E. Ruhl, G. Polenta, G. De Troia, J. R. Bond, Paolo Natoli, G. de Gasperis, Giovanni Romeo, P. Santini, A. Boscaleri, and Carlo R. Contaldi

Subjects
cosmic microwave background, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Curvature, 01 natural sciences, Spectral line, law.invention, Telescope, High Energy Physics - Phenomenology (hep-ph), Settore FIS/05 - Astronomia e Astrofisica, law, 0103 physical sciences, cosmological parameters, polarization, 010303 astronomy & astrophysics, Physics, Spectral index, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Cosmology: Cosmic Microwave Background, Cosmology: Cosmological Parameters, Polarization, Cosmology: Cosmic Microwave Background, Astronomy and Astrophysics, Redshift, High Energy Physics - Phenomenology, Cosmology: Cosmological Parameters, Space and Planetary Science, Dark energy, Neutrino
Abstract

We present the cosmological parameters from the CMB intensity and polarization power spectra of the 2003 Antarctic flight of the BOOMERANG telescope. The BOOMERANG data alone constrains the parameters of the $\Lambda$CDM model remarkably well and is consistent with constraints from a multi-experiment combined CMB data set. We add LSS data from the 2dF and SDSS redshift surveys to the combined CMB data set and test several extensions to the standard model including: running of the spectral index, curvature, tensor modes, the effect of massive neutrinos, and an effective equation of state for dark energy. We also include an analysis of constraints to a model which allows a CDM isocurvature admixture., Comment: 18 pages, 10 figures, submitted to ApJ

Published
2006

17. A Measurement of the CMB Spectrum from the 2003 Flight of BOOMERANG

Author

J. Borrill, F. Piacentini, Alessandro Melchiorri, A. de Oliveira-Costa, Theodore Kisner, P. Cabella, Calvin B. Netterfield, J. E. Ruhl, E. Hivon, Enzo Pascale, T. E. Montroy, D. Pogosyan, G. Romeo, S. Ricciardi, P. D. Mauskopf, Carlo R. Contaldi, P. A. R. Ade, Simon Prunet, J. R. Bond, P. Natoli, W. C. Jones, Max Tegmark, C. J. MacTavish, B. P. Crill, J. J. Bock, M. Veneziani, G. De Troia, G. de Gasperis, Nicola Vittorio, P. de Bernardis, Andrew E. Lange, G. Di Stefano, G. Polenta, Andrew H. Jaffe, Paola Santini, Silvia Masi, and A. Boscaleri

Subjects
media_common.quotation_subject, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, Cosmology, law.invention, Settore FIS/05 - Astronomia e Astrofisica, law, 0103 physical sciences, Adiabatic process, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Physics, 010308 nuclear & particles physics, Bolometer, Detector, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Cosmology: Cosmic Microwave Background, Polarization (waves), Cosmology: Cosmic Microwave Background, Instrumentation: Detectors, Instrumentation: Detectors, Space and Planetary Science, Sky
Abstract

We report measurements of the CMB polarization power spectra from the January 2003 Antarctic flight of BOOMERANG. The primary results come from six days of observation of a patch covering 0.22% of the sky centered near R.A. = 82.5 deg., Dec= -45 deg. The observations were made using four pairs of polarization sensitive bolometers operating in bands centered at 145 GHz. Using two independent analysis pipelines, we measure a non-zero signal in the range 100< l contribution, and a 2-sigma upper limit of 7.0 uK^2 for the spectrum. Estimates of foreground intensity fluctuations and the non-detection of and signals rule out any significant contribution from galactic foregrounds. The results are consistent with a Lambda-CDM cosmology seeded by adiabatic perturbations. We note that this is the first detection of CMB polarization with bolometric detectors., Comment: Submitted to Astrophysical Journal

Published
2005
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18. The trispectrum of the cosmic microwave background on subdegree angular scales: an analysis of the BOOMERanG data

Author

G. De Troia, M. Giacometti, J. R. Bond, P. A. R. Ade, B. P. Crill, Martin Kunz, G. Polenta, Andrew E. Lange, F. Piacentini, G. Romeo, A. Boscaleri, T. E. Montroy, J. J. Bock, P. D. Mauskopf, P. Natoli, V. V. Hristov, J. E. Ruhl, Enzo Pascale, Silvia Masi, E. Hivon, Carlo R. Contaldi, Pedro G. Ferreira, P. de Bernardis, and Calvin B. Netterfield

Subjects
Physics, Gaussian, media_common.quotation_subject, Cosmic microwave background, Astrophysics (astro-ph), High resolution, FOS: Physical sciences, Astronomy and Astrophysics, Probability density function, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, Fourth order, Space and Planetary Science, Sky, symbols, Statistical physics, Trispectrum, Anisotropy, media_common
Abstract

The trispectrum of the cosmic microwave background can be used to assess the level of non-Gaussianity on cosmological scales. It probes the fourth order moment, as a function of angular scale, of the probability distribution function of fluctuations and has been shown to be sensitive to primordial non-gaussianity, secondary anisotropies (such as the Ostriker-Vishniac effect) and systematic effects (such as astrophysical foregrounds). In this paper we develop a formalism for estimating the trispectrum from high resolution sky maps which incorporates the impact of finite sky coverage. This leads to a series of operations applied to the data set to minimize the effects of contamination due to the Gaussian component and correlations between estimates at different scales. To illustrate the effect of the estimation process, we apply our procedure to the BOOMERanG data set and show that it is consistent with Gaussianity. This work presents the first estimation of the CMB trispectrum on sub-degree scales., 14 pages, submitted to MNRAS

Published
2003

19. Multiple Peaks in the Angular Power Spectrum of the Cosmic Microwave Background: Significance and Consequences for Cosmology

Author

G. De Troia, M. Giacometti, Dmitry Pogosyan, K. Ganga, Simon Prunet, Philip Daniel Mauskopf, Alessandro Melchiorri, Carlo R. Contaldi, E. Hivon, F. Pongetti, F. Piacentini, G. Polenta, Andrew H. Jaffe, T. E. Montroy, Peter A. R. Ade, J. E. Ruhl, James J. Bock, Giovanni Romeo, L. Martinis, Andrew E. Lange, Julian Borrill, B. P. Crill, A. Iacoangeli, F. Scaramuzzi, K. Coble, J. R. Bond, P. C. Farese, Calvin B. Netterfield, P. de Bernardis, Silvia Masi, A. Boscaleri, Viktor Hristov, Enzo Pascale, P. V. Mason, and W. C. Jones

Subjects
Physics, Spectral index, Particle physics, 010308 nuclear & particles physics, Cosmic microwave background, Astrophysics (astro-ph), BOOMERanG experiment, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Parameter space, 01 natural sciences, Omega, Amplitude, Space and Planetary Science, 0103 physical sciences, Optical depth (astrophysics), cosmic microwave background, cosmological parameters, cosmology : observations, cosmology: observations, 010303 astronomy & astrophysics
Abstract

Three peaks and two dips have been detected in the power spectrum of the cosmic microwave background from the BOOMERANG experiment, at $\ell \sim 210, 540, 840$ and $\ell \sim 420, 750$, respectively. Using model-independent analyses, we find that all five features are statistically significant and we measure their location and amplitude. These are consistent with the adiabatic inflationary model. We also calculate the mean and variance of the peak and dip locations and amplitudes in a large 7-dimensional parameter space of such models, which gives good agreement with the model-independent estimates, and forecast where the next few peaks and dips should be found if the basic paradigm is correct. We test the robustness of our results by comparing Bayesian marginalization techniques on this space with likelihood maximization techniques applied to a second 7-dimensional cosmological parameter space, using an independent computational pipeline, and find excellent agreement: $\Omega_{\rm tot} = 1.02^{+0.06}_{-0.05}$ {\it vs.} $1.04 \pm 0.05$, $\Omega_b h^2 = 0.022^{+0.004}_{-0.003}$ {\it vs.} $0.019^{+0.005}_{-0.004}$, and $n_s = 0.96^{+0.10}_{-0.09}$ {\it vs.} $0.90 \pm 0.08$. The deviation in primordial spectral index $n_s$ is a consequence of the strong correlation with the optical depth., Comment: 15 pages, 6 figures, submitted to Ap.J

Published
2001

20. A Measurement of Omega from the North American Test Flight of Boomerang

Author

A. Boscaleri, Calvin B. Netterfield, F. Piacentini, G. De Troia, M. Giacometti, Alessandro Melchiorri, Andrew E. Lange, L. Miglio, Silvia Masi, Viktor Hristov, Peter A. R. Ade, G. de Gasperis, P. C. Farese, Pedro G. Ferreira, Philip Daniel Mauskopf, Giovanni Romeo, Enzo Pascale, A. H. Jaffe, P. de Bernardis, J. E. Ruhl, Ken Ganga, B. P. Crill, Nicola Vittorio, Julian Borrill, and James J. Bock

Subjects
Astrophysics and Astronomy, Cold dark matter, Cosmic microwave background, BOOMERanG experiment, FOS: Physical sciences, Astrophysics, Cosmological constant, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Omega, General Relativity and Quantum Cosmology, Methods: Data Analysis, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Cosmology: Dark Matter, Astrophysics (astro-ph), Spectral density, Astronomy and Astrophysics, Cosmology: Cosmic Microwave Background, Redshift, Supernova, Cosmology: Cosmic Microwave Background, Cosmology: Dark Matter, Methods: Data Analysis, Space and Planetary Science
Abstract

We use the angular power spectrum of the Cosmic Microwave Background, measured during the North American test flight of the BOOMERANG experiment, to constrain the geometry of the universe. Within the class of Cold Dark Matter models, we find that the overall fractional energy density of the universe, Omega, is constrained to be 0.85 < Omega < 1.25 at the 68% confidence level. Combined with the COBE measurement and the high redshift supernovae data we obtain new constraints on the fractional matter density and the cosmological constant., 4 pages, 3 figures LaTeX, emulateapj.sty

Published
1999

21. Measurement of a Peak in the Cosmic Microwave Background Power Spectrum from the North American test flight of BOOMERANG

Author

Alessandro Melchiorri, Evan Scannapieco, A. Boscaleri, T. E. Montroy, K. Ganga, F. Piacentini, Peter A. R. Ade, Shaul Hanany, Silvia Masi, J. E. Ruhl, F. Scaramuzzi, P. C. Farese, Pedro G. Ferreira, Julian Borrill, B. P. Crill, Enzo Pascale, Paul L. Richards, Nicola Vittorio, A. H. Jaffe, P. de Bernardis, A. Iacoangeli, James J. Bock, F. Melchiorri, Philip Daniel Mauskopf, G. De Troia, M. Giacometti, L. Miglio, Andrew E. Lange, Adrian T. Lee, G. DeGasperis, Radek Stompor, Viktor Hristov, Giovanni Romeo, and Calvin B. Netterfield

Subjects
Astrophysics and Astronomy, Cosmic microwave background, BOOMERanG experiment, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Cosmology: Observations, General Relativity and Quantum Cosmology, law.invention, High Energy Physics - Experiment, Telescope, High Energy Physics - Experiment (hep-ex), Methods: Data Analysis, Settore FIS/05 - Astronomia e Astrofisica, law, 0103 physical sciences, Anisotropy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Balloons, 010308 nuclear & particles physics, Bolometer, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy and Astrophysics, Cosmology: Cosmic Microwave Background, Full width at half maximum, Amplitude, Space and Planetary Science, Instrumentation: Photometers, Balloons, Cosmology: Cosmic Microwave Background, Cosmology: Observations, Instrumentation: Photometers, Methods: Data Analysis, Telescopes, Telescopes
Abstract

We describe a measurement of the angular power spectrum of anisotropies in the Cosmic Microwave Background (CMB) from 0.3 degrees to ~10 degrees from the North American test flight of the BOOMERANG experiment. BOOMERANG is a balloon-borne telescope with a bolometric receiver designed to map CMB anisotropies on a Long Duration Balloon flight. During a 6-hour test flight of a prototype system in 1997, we mapped > 200 square degrees at high galactic latitudes in two bands centered at 90 and 150 GHz with a resolution of 26 and 16.6 arcmin FWHM respectively. Analysis of the maps gives a power spectrum with a peak at angular scales of ~1 degree with an amplitude ~70 uK., 5 pages, 1 figure LaTeX, emulateapj.sty

Published
1999

22. Calibration of balloon-borne CMB experiments

Author

G. De Troia, L. Miglio, and P. de Bernardis

Subjects
Physics, Propagation of uncertainty, Space and Planetary Science, Planet, Calibration (statistics), Cosmic microwave background, Astronomy, Dipole anisotropy, Astronomy and Astrophysics, Astrophysics, Kinematics, Anisotropy
Abstract

We give a tutorial description of two calibration techniques suitable for present CMB anisotropy scanning experiments: observations of planets and observations of the kinematic dipole anisotropy. A few examples of data and simulations are given, together with the relevant formulas and a discussion of error propagation effects.

23. Mapping the CMB sky: The BOOMERanG experiment

Author

P. de Bernardis, Peter A. R. Ade, L. Miglio, J. J. Bock, Aaron Lee, L. Martinis, P. C. Farese, A. Iacoangeli, Paul L. Richards, F. Piacentini, T. E. Montroy, J. E. Ruhl, Silvia Masi, M. Giacommetti, Philip Daniel Mauskopf, B. P. Crill, A. Boscaleri, Francesco Scaramuzzi, Francesco Melchiorri, Andrew E. Lange, Enzo Pascale, Peter Mason, G. De Troia, R. Artusa, V. V. Hristov, and Calvin B. Netterfield

Subjects
Physics, media_common.quotation_subject, Astrophysics (astro-ph), Cosmic microwave background, BOOMERanG experiment, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics, law.invention, Telescope, Space and Planetary Science, law, Sky, Short duration, media_common, Stratospheric balloon
Abstract

We describe the BOOMERanG experiment, a stratospheric balloon telescope intended to measure the Cosmic Microwave Background anisotropy at angular scales between a few degrees and ten arcminutes. The experiment has been optimized for a long duration (7 to 14 days) flight circumnavigating Antarctica at the end of 1998. A test flight was performed on Aug.30, 1997 in Texas. The level of performance achieved in the test flight was satisfactory and compatible with the requirements for the long duration flight., 11 pages, 6 figures

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