http://hdl.handle.net/2122/293 2013-05-23T10:05:44Z http://hdl.handle.net/2122/7259 Title: Automatic scaling of polar ionograms Authors: Scotto, C.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma2, Roma, Italia; Pezzopane, M.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma2, Roma, Italia Abstract: The Istituto Nazionale di Geosifica e Vulcanologia (INGV) software for automatic scaling of ionograms (Autoscala) was improved by introducing a system to identify D region absorption events, spread-F condition (frequency spreading in the F region), and Z-ray propagation. The algorithm was applied to a series of ionograms recorded by the AIS-INGV (Advanced Ionospheric Sounder-INGV) ionosonde installed at the Mario Zucchelli Station (74.78S, 164.18E), Terra Nova Bay, Antarctica. Critical cases are shown to illustrate the behaviour of the software. 2012-01-31T23:00:00Z http://hdl.handle.net/2122/7239 Title: Unusual nighttime impulsive foF2 enhancement below the southern anomaly crest under geomagnetically quiet conditions Authors: Pezzopane, M.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma2, Roma, Italia; Fagundes, P. R.; Ciraolo, L.; Correia, E.; Cabrera, M. A.; Ezquer, R. G. Abstract: An unusual nighttime impulsive electron density enhancement was observed on 6 March 2010 over a wide region of South America, below the southern crest of the equatorial anomaly, under low solar activity and quiet geomagnetic conditions. The phenomenon was observed almost simultaneously by the F2 layer critical frequency ( foF2) recorded at three ionospheric stations which are widely distributed in space, namely Cachoeira Paulista (22.4°S, 44.6°W, magnetic latitude 13.4°S), São José dos Campos (23.2°S, 45.9°W, magnetic latitude 14.1°S), Brazil, and Tucumán (26.9°S, 65.4°W, magnetic latitude 16.8°S), Argentina. Although in a more restricted region over Tucumán, the phenomenon was also observed by the total electron content (TEC) maps computed by usingmeasurements from 12 GPS receivers. The investigated phenomenon is very particular because besides being of brief duration, it is characterized by a pronounced compression of the ionosphere. This compression was clearly visible both by the virtual height of the base of the F region (h′F) recorded at the aforementioned ionospheric stations, and by both the vertical electron density profiles and the slab thickness computed over Tucumán. Consequently, neither an enhanced fountain effect nor plasma diffusion from the plasmasphere can be considered as the single cause of this unusual event. A thorough analysis of isoheight and isofrequency ionosonde plots suggest that traveling ionospheric disturbances (TIDs) caused by gravity wave (GW) propagation could have likely played a significant role in causing the phenomenon. 2011-12-08T23:00:00Z http://hdl.handle.net/2122/6899 Title: Properties of Galactic cirrus clouds observed by BOOMERanG Authors: Veneziani, M.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; APC, Université Paris Diderot, 75013 Paris, France; Ade, P. A. R.; Department of Physics and Astronomy, Cardiff University, Cardiff, UK; Bock, J. J; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA; Boscaleri, A.; IFAC-CNR, 50127, Firenze, Italy; Crill, B. P.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA; de Bernardis, P.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; De Gasperis, G.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; De Oliveira - Costa, A.; Department of Physics, MIT, Cambridge, MA 02139, USA; De Troia, G.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ganga, K. M.; APC, Université Paris Diderot, 75013 Paris, France; Jones, W. C.; Department of Physics, Princeton University, Princeton, NJ 08544; Kisner, T. S.; Case Western Reserve University, Cleveland, OH 44106, USA; Lange, A. E.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; MacTavish, C. J.; Astrophysics Group, Imperial College, London, UK; Masi, S.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Mauskopf, P. D.; Department of Physics and Astronomy, Cardiff University, Cardiff, UK; Montroy, T. E.; Case Western Reserve University, Cleveland, OH 44106, USA; Natoli, P.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Pascale, E.; Physics Department, University of Toronto, Toronto ON, Canada; Piacentini, F.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Pietrobon, D.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Institute of Cosmology and Gravitation, U. of Portsmouth, UK; Polenta, G.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; ASI Science Data Center, c/o ESRIN, 00044 Frascati, Italy; INAF-Osservatorio Astronomico di Roma, I-00040 Monte Porzio Catone, Italy; Ricciardi, S.; Computational Research Division, LBNL, Berkeley, CA 94720, USA; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ruhl, J. E.; Case Western Reserve University, Cleveland, OH 44106, USA; Netterfield, C. B.; Physics Department, University of Toronto, Toronto ON, Canada Abstract: The physical properties of galactic cirrus emission are not well characterized. BOOMERANG is a balloonborne experiment designed to study the cosmic microwave background at high angular resolution in the millimeter range. The BOOMERANG 245 and 345 GHz 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 ) where BOOMERANG performed its deepest integration, combining the BOOMERANG data with other available datasets at different wavelengths. We have detected 8 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 observationswith different instruments at differentwavelengths 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 in the frequency range 23–3000 GHz (13 mm 100 μm 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. 2009-12-31T23:00:00Z http://hdl.handle.net/2122/5773 Title: Origin of basalt fire-fountain eruptions on Earth versus the Moon Authors: Rutherford, M. J.; Department of Geological Sciences, Brown University, Providence, Rhode Island 02912, USA; Papale, P.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Pisa, Pisa, Italia Abstract: Fire-fountain eruptions of basaltic magma occur on Earth at centers such as Kilauea (Hawaii), and deposits from apparently similar eruptions have been found on the lunar surface. The driving force for terrestrial fire-fountain eruptions is the exsolution of dissolved CO2 based on gases dissolved in melt inclusions trapped in olivine phenocrysts and the relatively high oxidation state of these magmas. Gases released at the vent show that SO2, and eventually H2O, are partitioned into the CO2-rich gas, adding to the gas volume. In contrast, analytical and experimental studies of lunar samples indicate that the gas phase responsible for driving the lunar eruptions was CO-rich and produced by the oxidation of C (graphite) carried in the slowly ascending low-fO2 basalt. The graphite oxidation occurs when the pressure in the ascending lunar magma reaches that of the graphite-gas reaction surface (40 ± 1 MPa or ~8 km depth for the Apollo 17 orange-glass magma). As graphite is oxidized, some FeO is reduced, potentially forming a Fe-rich metal phase, and Fe-rich metal spherules are present in beads in lunar glass deposits. Other gas species such as S, Cl, and F partitioned variously into CO-rich lunar volcanic gas, and appear in surface coatings on the glass spherules. Modeling of the magma flow from 8 km depth to the lunar surface shows that the gas bubble volume fraction (assuming initial C at 50–500 ppm levels) ranges from 0.5 to 0.8 at the surface, the exit velocity ranges from 15 to 35 m/s, and the low-viscosity magma fragments only as it erupts at the lunar surface. 2009-02-28T23:00:00Z http://hdl.handle.net/2122/5601 Title: Subdegree Sunyaev-Zel'dovich Signal from Multifrequency BOOMERanG observations Authors: Veneziani, M.; Center for Cosmology, University of California, Irvine, CA 92697, USA; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; APC, Université Paris Diderot, 75013 Paris, France; Amblard, A.; Center for Cosmology, University of California, Irvine, CA 92697, USA; Cooray, A.; Center for Cosmology, University of California, Irvine, CA 92697, USA; Piacentini, F.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Pietrobon, D.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Institute of Cosmology and Gravitation, University of Portsmouth, UK; Serra, P.; Center for Cosmology, University of California, Irvine, CA 92697, USA; Ade, P. A. R.; Department of Physics and Astronomy, Cardiff University, Cardiff, UK; Bock, J. J.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA; Bond, J. R.; CITA, University of Toronto, Toronto, ON M5S 3H8, Canada; Borrill, J.; Computational Research Division, LBNL, Berkeley, CA 94720, USA; Boscaleri, A.; IFAC-CNR, 50127, Firenze, Italy; Cabella, P.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Contaldi, C. R.; Theoretical Physics Group, Imperial College, London, UK; Crill, B. P.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA; de Bernardis, P.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; De Gasperis, G.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; de Oliveira-Costa, A.; Department of Physics, MIT, Cambridge, MA 02139, USA; De Troia, G.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ganga, K. M.; APC, Université Paris Diderot, 75013 Paris, France; Hivon, E.; Institut d’Astrophysique de Paris, 75014 Paris, France; Jones, W. C.; Department of Physics, Princeton University, Princeton, NJ 08544, USA; Kisner, T. S.; Case Western Reserve University, Cleveland, OH 44106, USA; Lange, A. E.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; MacTavish, C. J.; Astrophysics Group, Imperial College, London, UK; Masi, S.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Mauskopf, P. D; Department of Physics and Astronomy, Cardiff University, Cardiff, UK; Melchiorri, A.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Montroy, T. E.; Case Western Reserve University, Cleveland, OH 44106, USA; Natoli, P.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Netterfield, C. B.; Physics Department, University of Toronto, Toronto ON, Canada; Pascale, E.; Physics Department, University of Toronto, Toronto ON, Canada; Polenta, G.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; ASI Science Data Center, c/o ESRIN, 00044 Frascati, Italy; INAF - Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy; Ricciardi, S.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Space Sciences Laboratory, UC Berkeley CA, USA; Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ruhl, J. E; Case Western Reserve University, Cleveland, OH 44106, USA; Santini, P.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Tegmark, M.; Department of Physics, MIT, Cambridge, MA 02139, USA; Vittorio, N.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy 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 μK (2sigma) for rms SZ fluctuations in a broad bin between multipoles of 250 and 1200 at the Rayleigh-Jeans (RJ) end of the spectrum. The resulting upper limit on the local universe normalization of the density perturbations with BOOMERANG SZ data alone is sigma_sz_8 < 1.14 at the 95% confidence level. When combined with other CMB anisotropy and SZ measurements, we find sigma_SZ_8 < 0.92 (95% c.l.). 2009-08-31T22:00:00Z http://hdl.handle.net/2122/5559 Title: BOOMERanG Constraints on Primordial Non-Gaussianity from Analytical Minkowski Functionals Authors: Natoli, P.; Dipartimento di Fisica, Universita' di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy; INFN, Sezione di Tor Vergata, Roma, Italy; De Troia, G.; Dipartimento di Fisica, Universita' di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy; Hikage, C.; Department of Astrophysical Sciences, Princeton University, Peyton Hall, Princeton NJ 08544, USA; School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA; Komatsu, E.; Texas Cosmology Center, University of Texas at Austin, 1 University Station, C1400, Austin, TX 78712, USA; Migliaccio, M.; Dipartimento di Fisica, Universita' di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy; Ade, P. A. R.; School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA; Bock, J. J.; Jet Propulsion Laboratory, Pasadena, CA, USA; Bond, J.R.; Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada; Borrill, J.; Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, UC Berkeley, CA, USA; Boscaleri, A.; IFAC-CNR, Firenze, Italy; Contaldi, C. R.; Theoretical Physics Group, Imperial College, London; Crill, B. P.; Jet Propulsion Laboratory, Pasadena, CA, USA; de Bernardis, P.; Dipartimento di Fisica, Universita' La Sapienza, Roma, Italy; de Gasperis, G.; Dipartimento di Fisica, Universita' di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy; A. de Oliveira-Costa, A.; Department of Physics, MIT, Cambridge, MA 02139, USA; Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Hivon, E.; Institut d’Astrophysique, Paris, France; Kisner, T. S.; Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, UC Berkeley, CA, USA; Jones, W. C.; Department of Physics, Princeton University, Princeton, NJ 0854, USA; Lange, A. E.; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA; Masi, S.; Dipartimento di Fisica, Universita' La Sapienza, Roma, Italy; Mauskop, P. D.; School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA; MacTavish, C. J.; Astrophysics Group, Imperial College, London; Melchiorri, A.; Dipartimento di Fisica, Universita' La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy; Montroy, T. E.; Physics Department, Case Western Reserve University, Cleveland, OH, USA; Netterfield, C. B.; Physics Department, University of Toronto, Toronto, Ontario, Canada; Pascale, E.; Physics Department, University of Toronto, Toronto, Ontario, Canada; Piacentini, F.; Dipartimento di Fisica, Universit`a La Sapienza, Roma, Italyr; Polentao, G.; Dipartimento di Fisica, Universita' La Sapienza, Roma, Italyl; ASI Science Data Center, c/o ESRIN, 00044 Frascati, Italy; INAF - Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy; Ricciardi, S.; Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, UC Berkeley, CA, USAl; Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ruhl, J. E.; Physics Department, Case Western Reserve University, Cleveland, OH, USA; Tegmark, M.; Department of Physics, MIT, Cambridge, MA 02139, USA Cle; Veneziani, M.; Dipartimento di Fisica, Universit`a La Sapienza, Roma, Italyeodi; Vittorio, N.; Dipartimento di Fisica, Universita' di Roma “Tor Vergata”, Via della Ricerca Scientifica, 1 I-00133 Roma, Italy Abstract: We use Minkowski Functionals (MF) to constrain a primordial non-Gaussian contribu- tion 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 fNL without the need for non-Gaussian simulations. We find -1020 < fNL < 390 at 95% CL, significantly improving the previous constraints by De Troia et al. (2007) on the BOOMERanG 2003 dataset. These are the best fNL limits to date for suborbital probes. 2008-12-31T23:00:00Z http://hdl.handle.net/2122/5543 Title: Properties of Galactic cirrus clouds observed by BOOMERanG Authors: Veneziani, M.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy;APC, Université Paris Diderot, 75013 Paris, France; Ade, P. A. R.; Department of Physics and Astronomy, Cardiff University, Cardiff, UK; Bock, J. K.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA; Boscaleri, A.; IFAC-CNR, 50127, Firenze, Italy; Crill, B. P.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; California Institute of Technology, Pasadena, CA 91125, USA; P. de Bernardis, P.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; De Gasperis, G.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; De Oliveira-Costa, A.; Department of Physics, MIT, Cambridge, MA 02139, USA; De Troia, G.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ganga, K. M.; APC, Université Paris Diderot, 75013 Paris, France; Jones, W. C.; Department of Physics, Princeton University, Princeton, NJ 08544; Kisner, T. S.; Case Western Reserve University, Cleveland, OH 44106, USA; Lange, A. E.; Jet Propulsion Laboratory, Pasadena, CA 91109, USA; MacTavish, C. J.; Astrophysics Group, Imperial College, London, UK; Masi, S.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Mauskopf, P. D.; Department of Physics and Astronomy, Cardiff University, Cardiff, UK; Montroy, T. E.; Case Western Reserve University, Cleveland, OH 44106, USA; Natoli, P.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Netterfield, C. B.; Physics Department, University of Toronto, Toronto ON, Canada; Pascale, E.; Physics Department, University of Toronto, Toronto ON, Canada; Piacentini, F.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Pietrobon, D.; Dipartimento di Fisica, Università di Roma “Tor Vergata”, Rome, Italy; Institute of Cosmology and Gravitation, U. of Portsmouth, UK; Polenta, G.; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; ASI Science Data Center, c/o ESRIN, 00044 Frascati, Italy; INAF-Osservatorio Astronomico di Roma, I-00040 Monte Porzio; Ricciardi, S.; Computational Research Division, LBNL, Berkeley, CA 94720, USA; Dipartimento di Fisica, Università di Roma “La Sapienza”, Rome, Italy; Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ruhl, J. E.; Case Western Reserve University, Cleveland, OH 44106, USA Abstract: The physical properties of Galactic cirrus emission are not well characterized. BOOMERANG is a balloonborne experiment designed to study the Cosmic Microwave Background at high angular resolution in the millimetre range. The BOOMERANG 245 and 345 GHz 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 where BOOMERANG performed its deepest integration, combining the BOOMERANG data with other available datasets at different wavelengths. We have detected 7 emission patches in the 345 GHz map, consistent with cirrus dust in the IRAS 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 IRAS, DIRBE, BOOMERANG and WMAP in the frequency range 23–5000 GHz (13 mm to 60 μm wavelength). We fit the measured spectra with a combination of thermal and non-thermal spectra considering two models for the thermal emission. The first model assumes the emission to be isothermal with a variable spectral index. The second model considers two temperatures in the cloud, both the components spectral indices being set to 2. The two models are statistically equivalent and the estimated temperatures are consistent. A 10 K component has been detected at high latitudes. In our sample, assuming the isothermal model, the temperature of the thermal component varies in the 20 – 25 K range and its emissivity spectral index is in the 0.5 – 1.5 range. The spectral index of the non-thermal emission at lower frequencies covers the -1.6 – -2 range in antenna temperature. We could not identify a clear 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. 2008-12-31T23:00:00Z http://hdl.handle.net/2122/5237 Title: Complexity in the sunspot cycle Authors: Consolini, G.; INAF – Istituto di Fisica dello Spazio Interplanetario, 00133 Roma, Italy; Tozzi, R.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma2, Roma, Italia; De Michelis, P.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione CNT, Roma, Italia Abstract: The occurrence of complexity in the solar cycle, as monitored by the sunspot area butterfly diagram, is investigated by means of the natural orthogonal composition (NOC) technique and information theory approach. Although the butterfly diagram may be reconstructed using only two modes as already found in other papers for the Hale cycle, on deeper investigation it is possible to notice that the high variability, complexity, and stochasticity observed during the solar cycle are missing. A full description of the complex evolution of the solar cycle requires at least 30 modes. We show that these modes identify two different dynamical regimes, whose existence is also confirmed by the analysis of the Lyapunov exponents of the associated principal components. We suggest that the existence of these two physical dynamical regimes is at the origin of the dynamical complexity of the solar cycle. We attempt a discussion of these dynamical regimes also in terms of a nearly stable dynamo process described by the first two modes and a local superficial turbulent dynamo responsible for the more stochastic features observed in the solar cycle. 2009-11-02T23:00:00Z http://hdl.handle.net/2122/4555 Title: A Measurement of the CMB <EE> Spectrum from the 2003 Flight Authors: Montroy, T. E.; Physics Department, Case Western Reserve University, Cleveland, OH, USA; Ade, P. A. R.; Dept. of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK; Bock, J. J.; Jet Propulsion Laboratory, Pasadena, CA, USA; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA; Bond, J. R.; Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario, Canada; Borrill, J.; Computational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Space Sciences Laboratory, University of California, Berkeley, CA, USA; Boscaleri, A.; IFAC-CNR, Firenze, Italy; Cabella, P.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy; Contaldi, C. R.; Astrophysics Group, Imperial College, London, UK; Crill, B. P.; IPAC, California Institute of Technology, Pasadena, CA, USA; de Bernardis, P.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; De Gasperis, G.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy; De Oliveira-Costa, A.; Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA; De Troia, G.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Hivon, E.; IPAC, California Institute of Technology, Pasadena, CA, USA; Jaffe, A. H.; Astrophysics Group, Imperial College, London, UK; Kisner, T. S.; Physics Department, Case Western Reserve University, Cleveland, OH, USA; Dept. of Physics, University of California, Santa Barbara, CA, USA; Jones, W. C.; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA; Lange, A. E.; Observational Cosmology, California Institute of Technology, Pasadena, CA, USA; Masi, S.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Mauskopf, P. D.; Dept. of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK; MacTavish, C. J.; Physics Department, University of Toronto, Toronto, Ontario, Canada; Melchiorri, A.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; INFN, Sezione di Roma 1, Roma, Italy; Natoli, P.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy; Netterfield, C. B.; Physics Department, University of Toronto, Toronto, Ontario, Canada; Department of Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, Canada; Pascale, E.; Physics Department, University of Toronto, Toronto, Ontario, Canada; Piacentini, F.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Pogosyan, D.; Physics Dept., University of Alberta, Edmonton, Alberta, Canada; Polenta, G.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Prunet, S.; Institut d’Astrophysique, Paris, France; Ricciardi, S.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ruhl, J. E.; Physics Department, Case Western Reserve University, Cleveland, OH, USA; Santini, P.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Tegmark, M.; Dept. of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA; Veneziani, M.; Dipartimento di Fisica, Universit`a di Roma La Sapienza, Roma, Italy; Vittorio, N.; Dipartimento di Fisica, Universit`a di Roma Tor Vergata, Roma, Italy; INFN, Sezione di Roma 2, Roma, Italy Abstract: We report measurements of the CMB polarization power spectra from the 2003 January Antarctic flight of BOOMERANG. The primary results come from 6 days of observation of a patch covering 0.22% of the sky centered near R:A: ¼ 82N5, decl: ¼ 45 . 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 nonzero hEEi signal in the range 201 < l < 1000 with a significance of 4.8 , a 2 upper limit of 8.6 K2 for any hBBi contribution, and a 2 upper limit of 7.0 K2 for the hEBi spectrum. Estimates of foreground intensity fluctuations and the nondetection of hBBi and hEBi signals rule out any significant contribution from Galactic foregrounds. The results are consistent with a CDM cosmology seeded by adiabatic perturbations.We note that this is the first detection of CMB polarization with bolometric detectors. 2006-08-19T22:00:00Z http://hdl.handle.net/2122/4501 Title: Searching for non-Gaussian signals in the BOOMERanG 2003 CMB map: Preliminary results Authors: De Troia, G.; Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Ade, P. A. R.; bDepartment of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK; Bock, J. J.; cJet Propulsion Laboratory, Pasadena, CA, USA; Bond, J. R.; dCanadian Institute for Theoretical Astrophysics, University of Toronto, Canada; Borrill, J.; eComputational Research Division, Lawrence Berkeley National Laboratory, Berkeley, CA, USA; Boscaleri, A.; fIFAC-CNR, Firenze, Italy; Cabella, P.; gAstrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK; Contaldi, C. R.; dCanadian Institute for Theoretical Astrophysics, University of Toronto, Canada; Crill, B. P.; hIPAC, California Institute of Technology, Pasadena, CA, USA; De Bernardis, P.; aDipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; De Gasperis, G.; iDipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy; De Oliveira-Costa, A.; jDepartment of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA; Di Stefano, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ferreira, P. G.; gAstrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UK; Hivon, E.; hIPAC, California Institute of Technology, Pasadena, CA, USA; Jaffe, A.; lTheoretical Physics Group, Imperial College, London, UK; Kisner, T.; mPhysics Department, Case Western Reserve University, Cleveland, OH, USA; Kunz, M.; Départment de Physique Théorique, Université de Genève, 24 quai Ernest, Ansermet, Genève 4, Switzerland; Jones, W. C.; pObservational Cosmology, California Institute of Technology, Pasadena, CA, USA; Lange, A. E.; pObservational Cosmology, California Institute of Technology, Pasadena, CA, USA; Masi, S.; aDipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Mauskopf, P. D.; Department of Physics and Astronomy, Cardiff University, Cardiff CF24 3YB, Wales, UK; MacTavish, C.; qPhysics Department, University of Toronto, Toronto, Ont., Canada; Melchiorri, A.; aDipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Montroy, T.; mPhysics Department, Case Western Reserve University, Cleveland, OH, USA; Natoli, P.; iDipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy; Netterfield, C. B.; Physics Department, University of Toronto, Toronto, Ont., Canada; Pascale, E.; Physics Department, University of Toronto, Toronto, Ont., Canada; Piacentini, F.; Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Pogosyan, D.; Department of Physics, University of Alberta, Edmonton, AB, Canada; Polenta, G.; Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Prunet, S.; uInstitut dÁstrophysique, Paris, France; Ricciardi, S.; aDipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Romeo, G.; Istituto Nazionale di Geofisica e Vulcanologia, Sezione Roma1, Roma, Italia; Ruhl, J. E.; mPhysics Department, Case Western Reserve University, Cleveland, OH, USA; Santini, P.; aDipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Tegmark, M.; Department of Physics, Massachusetts Institute of Technology, Cambridge, MA, USA; Veneziani, M.; Dipartimento di Fisica, Università La Sapienza, Piazzale A. Moro 2, I-00185 Roma, Italy; Vittorio, N.; Dipartimento di Fisica, Università Tor Vergata, Via della Ricerca Scientifica, 1, I-00133 Roma, Italy 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 fNL as −300 < fNL < 650 at 68% CL and −800 < fNL < 1050 at 95% CL. 2007-11-30T23:00:00Z