Search

Your search keyword '"J. J. BOCK"' showing total 349 results
Start Over Author "J. J. BOCK"
349 results on '"J. J. BOCK"'

151. [Temporomandibular function after malocclusion operations compared with a representative population group study]

Author

P, Maurer, J J, Bock, C, Otto, A W, Eckert, and J, Schubert

Subjects
Adult, Male, Incidence, Mandible, Temporomandibular Joint Dysfunction Syndrome, Orthodontics, Corrective, Osteotomy, Cross-Sectional Studies, Postoperative Complications, Reference Values, Germany, Maxilla, Humans, Osteotomy, Le Fort, Female, Malocclusion, Follow-Up Studies
Abstract

The temporomandibular function of patients after orthognathic surgery was evaluated with the Helkimo index (D 0-III) and compared with a normal population.Temporomandibular disorders (TMD) were evaluated with the Helkimo index (D 0-III) in a group of patients (n=105, F=69, M=36) after osteotomies. The average follow-up time was 47 months (9-141 months). The osteotomies performed were as follows: 58 bilateral sagittal split osteotomies, 12 Le Fort I osteotomies, 22 bimaxillary osteotomies, and 13 segment-osteotomies. A control group (n=202, F=114, M=88, age 20-39 years) was examined in an epidemiological study. The statistical analysis was performed using Windows software SPSS 10.0.In 82.8% of the patients no symptoms or mild dysfunction were found. The comparison between the patient group (31.4%) and the control group (31.7%) revealed a similar frequency. The most frequent dysfunction was a reduced mobility of the mandible, which determined the statistical significance (p0,05) between the patients and the control group for the dysfunction group D II and D III. The chi-square test could not detect any difference between sex and the kind of osteotomy with regard to dysfunction.

Published
2003

152. 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

153. Large format long-wavelength GaAs/AlGaAs multi-quantum well infrared detector arrays for astronomy

Author

Michael E. Ressler, John K. Liu, Jason M. Mumolo, Michael W. Werner, J. J. Bock, D. Z. Ting, Sir B. Rafol, S. Bandara, and Sarath D. Gunapala

Subjects
Physics, business.industry, Detector, Computer Science::Software Engineering, Astronomy, Large format, Noise (electronics), Wavelength, Optics, Optoelectronics, Infrared detector, Quantum well infrared photodetector, business, Quantum well, Dark current
Abstract

A long-wavelength large format quantum well infrared photodetector (QWIP) focal plane array has been successfully used in a ground based astronomy experiment. QWIP arrays afford greater flexibility than the usual extrinsically doped semiconductor infrared (IR) arrays. The wavelength of the peak response and cutoff can be continuously tailored over a range wide enough to enable light detection at any wavelength range between 6-20 /spl mu/m. The spectral band width of these detectors can be tuned from narrow (/spl Delta//spl lambda///spl lambda/ /spl sim/ 10%) to wide (/spl Delta//spl lambda///spl lambda/ /spl sim/ 40 %) allowing various applications. Also, QWIP device parameters can be optimized to achieve extremely high performances at lower operating temperatures (/spl sim/ 30 K) due to exponential suppression of dark current. Furthermore, QWIPs offer low cost per pixel and highly uniform large format focal plane arrays (FPAs) mainly due to mature GaAs/AlGaAs growth and processing technologies. The other advantages of GaAs/AlGaAs based QWIPs are higher yield, lower 1/f noise and radiation hardness. Recently, we operated an infrared camera with a 256/spl times/256 QWIP array sensitive at 8.5 /spl mu/m at the prime focus of the 5 m Hale telescope, obtaining the images. The remarkable noise stability - and low 1/f noise - of QWIP focal plane arrays enable cameras to operate by modulating the optical signal with a nod period up to 100 s. A 500 s observation on dark sky renders a flat image with little indication of the low spatial frequency structures associated with imperfect sky subtraction or detector drifts.

Published
2003
Full Text
View/download PDF

154. Bolometric detectors for the High Frequency Instrument on Planck

Author

R. Sudiwala, R. S. Bhatia, Peter A. R. Ade, J. J. Bock, L. Husted, T. Koch, Minhee Yun, W. C. Jones, Christopher G. Paine, and Andrew E. Lange

Subjects
Physics, business.industry, Linear polarization, Detector, Cosmic microwave background, Bolometer, Electronic packaging, Astrophysics, Heat sink, law.invention, symbols.namesake, Cardinal point, Optics, law, symbols, Planck, business
Abstract

The High Frequency Instrument (HFI) on Planck will obtain all-sky images of the cosmic microwave background and other astrophysical sources of emission with resolution of 9 arcmin at 100 GHz, 7 arcmin at 143 GHz and 5 arcmin at 217, 353, 545 and 857 GHz. The HFI focal plane will contain 48 silicon nitride, micromesh, bolometric detectors operating from a 100 mK heat sink. Four detectors in each of the 6 bands will detect the sum of the power in both linear polarizations. Additionally, four pairs of detectors will provide sensitivity to linear polarization of emission at 143, 217 and 353 GHz. We report on the development of these detectors, which are being produced at the JPL Micro Devices Laboratory, packaged at JPL Electronics Packaging, characterized at 100 mK before delivery to our HFI consortium partners at Cardiff University.

Published
2003
Full Text
View/download PDF

155. ACBAR: The Arcminute Cosmology Bolometer Array Receiver

Author

M. C. Runyan, P. A. R. Ade, R. S. Bhatia, J. J. Bock, M. D. Daub, J. H. Goldstein, C. V. Haynes, W. L. Holzapfel, C. L. Kuo, A. E. Lange, J. Leong, M. Lueker, M. Newcomb, J. B. Peterson, C. Reichardt, J. Ruhl, G. Sirbi, E. Torbet, C. Tucker, A. D. Turner, and D. Woolsey

Subjects
Physics, Arcminute Cosmology Bolometer Array Receiver, Bolometer, Cosmic microwave background, Astrophysics (astro-ph), Astronomy, Viper telescope, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Galaxy, law.invention, Azimuth, Cardinal point, Space and Planetary Science, law, Gaussian beam
Abstract

We describe the Arcminute Cosmology Bolometer Array Receiver (ACBAR); a multifrequency millimeter-wave receiver designed for observations of the Cosmic Microwave Background (CMB) and the Sunyaev-Zel'dovich effect in clusters of galaxies. The ACBAR focal plane consists of a 16-pixel, background-limited, 240 mK bolometer array that can be configured to observe simultaneously at 150, 220, 280, and 350 GHz. With 4-5' FWHM Gaussian beam sizes and a 3 degree azimuth chop, ACBAR is sensitive to a wide range of angular scales. ACBAR was installed on the 2 m Viper telescope at the South Pole in January 2001. We describe the design of the instrument and its performance during the 2001 and 2002 observing seasons., Comment: 59 pages, 16 figures -- updated to reflect version published in ApJS

Published
2003
Full Text
View/download PDF

156. Peculiar Velocity Limits from Measurements of the Spectrum of the Sunyaev-Zel'dovich Effect in Six Clusters of Galaxies

Author

P. A. R. Ade, M. C. Runyan, Sarah E. Church, K. L. Thompson, P. D. Mauskopf, J. Hinderks, J. J. Bock, K. Ganga, Bradford Benson, and B. J. Philhour

Subjects
Physics, 010308 nuclear & particles physics, Infrared, media_common.quotation_subject, Cosmic microwave background, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Sunyaev–Zel'dovich effect, 01 natural sciences, Universe, Galaxy, Space and Planetary Science, 0103 physical sciences, Peculiar velocity, 010303 astronomy & astrophysics, Noise (radio), Galaxy cluster, Astrophysics::Galaxy Astrophysics, media_common
Abstract

We have made measurements of the Sunyaev-Zel'dovich (SZ) effect in six galaxy clusters at z > 0.2 using the Sunyaev-Zel'dovich Infrared Experiment (SuZIE II) in three frequency bands between 150 and 350 GHz. Simultaneous multi-frequency measurements have been used to distinguish between thermal and kinematic components of the SZ effect, and to significantly reduce the effects of variations in atmospheric emission which can otherwise dominate the noise. We have set limits to the peculiar velocities of each cluster with respect to the Hubble flow, and have used the cluster sample to set a 95% confidence limit of < 1410 km/s to the bulk flow of the intermediate-redshift universe in the direction of the CMB dipole. This is the first time that SZ measurements have been used to constrain bulk flows. We show that systematic uncertainties in peculiar velocity determinations from the SZ effect are likely to be dominated by submillimeter point sources and we discuss the level of this contamination., Submitted to Astrophysical Journal. 32 pages, 13 tables, 9 figures

Published
2003
Full Text
View/download PDF

157. GALACTIC DUST CONTAMINATION IN THE BOOMERANG MAPS

Author

M. Giacometti, E. Hivon, Enzo Pascale, J. E. Ruhl, Peter A. R. Ade, Andrew E. Lange, Calvin B. Netterfield, T. E. Montroy, P. de Bernardis, J. J. Bock, F. Piacentini, B. R Crill, Simon Prunet, Philip Daniel Mauskopf, A. Boscaleri, V. V. Hristov, and Serena Masi

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, BOOMERanG experiment, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Thermal emission, Contamination, Satellite, Anisotropy, Astrophysics::Galaxy Astrophysics, Cosmic dust, Dust emission
Abstract

Thermal emission from interstellar dust is a potential contaminant for sensitive measurements of Cosmic Microwave Background anisotropies. Here we analyze the mm-wave observations obtained by the BOOMERanG experiment at 90, 150, 240 and 410 GHz. Galactic emission has been detected at intermediate and high (b < -20°) Galactic latitudes, and is morphologically similar to the dust emission mapped by the IRAS satellite at 3000 GHz and by the DIRBE instrument on COBE at 1250 GHz. We show that the 410 GHz channel of BOOMERanG is a good monitor of dust emission, and that at 150 GHz the contamination is negligible with respect to the anisotropy of the cosmic microwave background (CMB) detected by the same instrument.

Published
2002
Full Text
View/download PDF

158. THE BOOMERANG/LDB INSTRUMENT

Author

F. Piacentini, K. Coble, J. E. Ruhl, Andrew E. Lange, Francesco Scaramuzzi, B. P. Crill, G. De Troia, D. Sforna, M. Giacometti, Enzo Pascale, A. Iacoangeli, P. Cardoni, L. Miglio, Peter Mason, V. V. Hristov, G. Romeo, E. Hivon, Calvin B. Netterfield, P. de Bernardis, J. J. Bock, T. E. Montroy, P. C. Farese, Philip Daniel Mauskopf, F. Pongetti, A. Boscaleri, Serena Masi, Peter A. R. Ade, and L. Martinis

Subjects
Physics, law, Bolometer, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, BOOMERanG experiment, Astronomy, High resolution, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cryogenics, Radiation, law.invention
Abstract

The BOOMERANG experiment provided the first high resolution map of the Cosmic Microwave Background (CMB) radiation. In this paper we summarize the main parts of the instrument, including bolometers, cryogenics, optics and pointing system. We show then how the instrument is designed to be robust to systematic effects.

Published
2002
Full Text
View/download PDF

159. Relative performance of filled and feedhorn-coupled focal-plane architectures

Author

J. J. Bock, Walter Kieran Gear, and Matthew Joseph Griffin

Subjects
Physics, Stray light, business.industry, Materials Science (miscellaneous), Astrophysics (astro-ph), Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Large format, Industrial and Manufacturing Engineering, Electromagnetic interference, law.invention, Cardinal point, Optics, Far infrared, law, Millimeter, Business and International Management, business
Abstract

Modern far infrared and submillimeter instruments require large format arrays. We consider the relative performance of filled array (bare pixel) and feedhorn-coupled architectures for bolometer focal planes. Based on typical array parameters, we quantify the relative observing speeds and comment on the merits of the different architectures. Filled arrays can provide higher mapping speed (by a factor of up to 3.5) and simpler observing modes at the expense of reduced sensitivity for pointed observations, increased detector numbers, and greater vulnerability to stray light and electromagnetic interference. Taking advantage of the filled array architecture requires strongly background limited detectors. At millimeter wavelengths, filled arrays must be surrounded by a sufficiently cold enclosure to minimize the background power from the instrument itself., Updated 4 September. Accepted for publication in Applied Optics. Available only in pdf. 45 pages inc. figures

Published
2002

160. A low noise, high thermal stability, 0.1 K test facility for the Planck HFI bolometers

Author

A. E. Lange, J. J. Bock, Christopher G. Paine, V. V. Hristov, Breon, S., DiPirro, M., Glaister, D., Hull, J., Kittel, P., Pecharsky, V., Radebaugh, R., Theilacker, J., VanSciver, S., Weisend, J., and Zeller, A.

Subjects
Physics, business.industry, Amplifier, Thermistor, Bolometer, JFET, Cryogenics, law.invention, Optics, law, Dilution refrigerator, business, Microwave, Noise (radio)
Abstract

We are developing a facility which will be used to characterize the bolometric detectors for Planck, an ESA mission to investigate the Cosmic Microwave Background. The bolometers operate at 0.1 K, employing neutron-transmutation doped (NTD) Ge thermistors with resistances of several megohms to achieve NEPs~1×10^(–17) W Hz^(–1/2). Characterization of the intrinsic noise of the bolometers at frequencies as low as 0.010 Hz dictates a test apparatus thermal stability of 40 nK Hz^(–1/2) to that frequency. This temperature stability is achieved via a multi-stage isolation and control geometry with high resolution thermometry implemented with NTD Ge thermistors, JFET source followers, and dedicated lock-in amplifiers. The test facility accommodates 24 channels of differential signal readout, for measurement of bolometer V(I) characteristics and intrinsic noise. The test facility also provides for modulated radiation in the submillimeter band incident on the bolometers, for measurement of the optical speed-of-response; this illumination can be reduced below detectable limits without interrupting cryogenic operation. A commercial Oxford Instruments dilution refrigerator provides the cryogenic environment for the test facility.

Published
2002

161. Interstellar dust in the BOOMERanG maps

Author

Simon Prunet, P. de Bernardis, M. Giacometti, J. E. Ruhl, F. Piacentini, Philip Daniel Mauskopf, Andrew E. Lange, B. P. Crill, V. V. Hristov, A. Boscaleri, T. E. Montroy, Enzo Pascale, Peter A. R. Ade, Calvin B. Netterfield, J. J. Bock, Silvia Masi, E. Hivon, De Petris, M., and Gervasi, M.

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Cosmic background radiation, BOOMERanG experiment, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Cosmic infrared background, Infrared cirrus, Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract

Interstellar dust (ISD) emission is present in the mm-wave maps obtained by the BOOMERanG experiment at intermediate and high Galactic latitudes. We find that, while being sub-dominant at the lower frequencies (90, 150, 240 GHz), thermal emission from ISD is dominant at 410 GHz, and is well correlated with the IRAS map at 100 μm. We find also that the angular power spectrum of ISD fluctuations at 410 GHz is a power law, and its level is negligible with respect to the angular power spectrum of the Cosmic Microwave Background (CMB) at 90 and 150 GHz.

Published
2002

162. Results from the first engineering run of BOLOCAM and plans for the future

Author

B. Knowles, Andrew E. Lange, Philip Daniel Mauskopf, D. Haig, Peter A. R. Ade, H. Nguyen, Jason Glenn, V. V. Hristov, S. G. Edgington, A. Goldin, B. K. Rownd, J. J. Bock, Sunil Golwala, De Petris, Marco, and Gervasi, Massimo

Subjects
Physics, Bolometer, Cosmic background radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, law.invention, Caltech Submillimeter Observatory, law, Extremely high frequency, Infrared cirrus, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Caltech Library Services, Cosmic dust
Abstract

We present results from the engineering run of the BOLOCAM receiver at the Caltech Submillimeter Observatory in May, 2000 and simulations of the sensitivity of the completed BOLOCAM receiver to astrophysical sources. BOLOCAM is a 144 element array of bolometers designed to operate in the millimeter wave atmospheric windows at 150, 220, and 280 GHz. These bands are well suited to studies of the Sunyaev-Zel'dovich effect in distant clusters of galaxies as well as measurements of the emission of interstellar dust.

Published
2002

163. The High Frequency Instrument of Planck: Requirements and Design

Author

J.-L. Puget, P. de Bernardis, J.-P. Torre, V. Yourchenko, R. S. Bhatia, A. Murphy, M. Piat, Andrew E. Lange, Bruno Maffei, Rashmikant V. Sudiwala, J.-M. Lamarre, J. J. Bock, Aurélien Benoit, M. Giard, F. R. Bouchet, Peter A. R. Ade, De Petris, M., and Gervasi, M.

Subjects
Physics, business.industry, media_common.quotation_subject, Bolometer, Cosmic microwave background, Cosmic background radiation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Submillimetre astronomy, law.invention, symbols.namesake, Optics, Sky, law, symbols, Satellite, Angular resolution, Planck, business, media_common
Abstract

The Planck satellite is a project of the European Space Agency based on a wide international collaboration, including United States and Canadian laboratories. It is dedicated to the measurement of the anisotropy of the Cosmic Microwave Background (CMB) with unprecedented sensitivity and angular resolution. The detectors of its High frequency Instrument (HFI) are bolometers cooled down to 100 mK. Their sensitivity will be limited by the photon noise of the CMB itself at low frequencies, and of the instrument background at high frequencies. The requirements on the measurement chain are directly related to the strategy of observation used for the satellite. Due to the scanning on the sky, time features of the measurement chain are directly transformed into angular features in the sky maps. This impacts the bolometer design as well as other elements: For example, the cooling system must present outstanding temperature stability, and the amplification chain must show, down to very low frequencies, a flat noise spectrum.

Published
2002

164. [Patient satisfaction with the outcome of surgical orthodontic intervention and effect of esthetic and functional criteria]

Author

P, Maurer, C, Otto, J J, Bock, A W, Eckert, and J, Schubert

Subjects
Adult, Male, Postoperative Complications, Treatment Outcome, Esthetics, Hyperesthesia, Patient Satisfaction, Humans, Female, Paresthesia, Surgery, Oral, Malocclusion
Abstract

The aim of the study was to analyze the influence of possible temporary or permanent disorders of sensation on the degree of the patient's satisfaction following an orthognathic operation.After an average of 47 months (range: 9-141), a follow-up examination was performed in 78 women (64.5%) and 43 men (35.5%) with an average age of 24.3 years (range: 19-40) at the time of operation. In 67 cases there had been a sagittal division of the mandible, in 11 cases a Le Fort I osteotomy, in 26 cases a bimaxillary osteotomy, in 4 cases an isolated genioplasty, and in 13 cases a segmental osteotomy in the upper or the lower jaw. In the peripheral area supplied by the nerves V2 and V3 sensation was examined by the two-point discrimination test and the result related to the patients' satisfaction using the chi-square test.The following qualities of sensation were recorded: anesthetic (2.7%), hypesthetic (16.6%), paresthetic (8.3%), and normesthetic (72.4%). The patients' satisfaction was rated as very satisfied in 51.3%, as satisfactory in 44.8%, and in 3.9% the patients' expectations had not been fulfilled; 75% regarded their outward appearance as markedly improved and a good 50% of the patients noted improved mastication. Therefore, three-fourths of all the patients would even be willing to be operated on again. Two-dimensional analysis, however, demonstrated only a weakly significant positive relationship between patient satisfaction and the preserved, or restored, sensation in the trigeminal region.

Published
2002

165. B2K: The polarization-sensitive BOOMERanG experiment

Author

G. De Troia, A. Boscaleri, G. Di Stefano, W. C. Jones, T. E. Montroy, F. Piacentini, P. de Bernardis, J. Watt, C. Mac Tavish, V. V. Hristov, A. Iacoangeli, Calvin B. Netterfield, J. E. Ruhl, Philip Daniel Mauskopf, E. Torbet, Andrew E. Lange, Enzo Pascale, Peter A. R. Ade, J. J. Bock, Theodore Kisner, G. Romeo, Silvia Masi, F. Pongetti, and Cecchini, Stefano

Subjects
Physics, Aerospace instrumentation, Linear polarization, business.industry, Bolometer, Cosmic microwave background, Cosmic background radiation, BOOMERanG experiment, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Polarization (waves), law.invention, Optics, Polarization sensitive, law, business
Abstract

We describe the new BOOMERanG payload, which is being prepared for a new circum-antarctic flight, with the aim to detect the linear polarization of the Cosmic Microwave Background (CMB). In addition to polarization capabilities, obtained by means of special bolometers, the instrument has been improved in the attitude reconstruction system and in the calibration system.

Published
2002

166. QUEST—A 2.6-m mm-wave telescope for CMB polarization studies

Author

Bruno Maffei, G. Pisano, M. Bowden, Sarah E. Church, Brian Keating, J. Hinderks, Andrew E. Lange, Walter Kieran Gear, Angela C. Taylor, Ben Rusholme, K. L. Thompson, Lucio Piccirillo, O. E. Mallie, K. Ganga, J. A. Murphy, J. J. Bock, Peter A. R. Ade, S. Melhuish, Cortiglioni, Stefano, Cecchini, Stefano, Sault, Robert, and Sbarra, Carla

Subjects
Background radiations, Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Radio microwave, Cosmic background radiation, cosmic background radiation, submillimetre waves, polarisation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Background radiations, Radiation mechanisms, polarization, Radio telescopes and instrumentation, heterodyne receivers, Photometric polarimetric and spectroscopic instrumentation, Radio microwave, radiofrequency cosmic radiation, cosmic background radiation, submillimetre waves, blackbody radiation, radiotelescopes, aerospace instrumentation, performance evaluation, polarisation, radioastronomy, heterodyne receivers, law.invention, Telescope, Radio telescopes and instrumentation, law, Radiation mechanisms, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, aerospace instrumentation, Astrophysics::Galaxy Astrophysics, radioastronomy, radiofrequency cosmic radiation, Physics, polarization, Photometric polarimetric and spectroscopic instrumentation, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Polarimeter, Polarization (waves), blackbody radiation, performance evaluation, Wavelength, radiotelescopes, Millimeter
Abstract

We describe QUEST (Q and U Extra—galactic Sub—mm Telescope), a CMB polarimeter, operating at millimetre wavelengths. Interesting features of its design are outlined.

Published
2002

167. Noise properties of the BOOMERANG instrument

Author

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

Subjects
Physics, Noise, Calibration (statistics), BOOMERanG experiment, Electronic engineering, Astronomy, Sensitivity (control systems)
Abstract

In this paper we report a short description of the BOOMERANG experiment explaining his scientific goal and the technologies implied. We concentrate then on the analysis of the noise properties discussing in particular the scan synchronous noise. Finally we present the calibration technique and the sensitivity of all the channels.

Published
2002
Full Text
View/download PDF

168. Use of high sensitivity bolometers for astronomy: Planck high frequency instrument

Author

Bruno Maffei, J.-M. Lamarre, R. S. Bhatia, M. Giard, P. de Bernardis, J.-P. Torre, F. R. Bouchet, Peter A. R. Ade, Aurélien Benoit, A. Murphy, J.-L. Puget, V. Yourchenko, J. J. Bock, Rashmikant V. Sudiwala, M. Piat, Andrew E. Lange, and Porter, F. S.

Subjects
Physics, business.industry, Cosmic microwave background, Bolometer, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Particle detector, law.invention, symbols.namesake, Optics, law, symbols, Angular resolution, Satellite, Planck, business, Sensitivity (electronics), Noise (radio)
Abstract

The Planck satellite is dedicated to the measurement of the anisotropy of the Cosmic Microwave Background (CMB) with unprecedented sensitivity and angular resolution. It is a project of the European Space Agency based on a wide international collaboration, including United States and Canadian laboratories. The detectors of its High Frequency Instrument (HFI) are bolometers cooled down to 100 mK. Their sensitivity will be limited by the photon noise of the CMB itself at low frequencies, and of the instrument background at high frequencies. The requirements on the measurement chain are directly related to the strategy of observation used for the satellite. This impacts the bolometer design as well as other elements: The cooling system must present outstanding temperature stability, and the amplification chain must show a flat noise spectrum down to very low frequencies.

Published
2002
Full Text
View/download PDF

169. l-space spectroscopy of the cosmic microwave background with the BOOMERanG experiment

Author

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

Subjects
Physics, background radiations, microwave, Cosmic microwave background, Cosmic background radiation, BOOMERanG experiment, Spherical harmonics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmology, radio, observational cosmology, Settore FIS/05 - Astronomia e Astrofisica, Observational cosmology, Cosmic infrared background, Cosmic noise
Abstract

The BOOMERanG experiment has recently produced detailed maps of the Cosmic Microwave Background, where sub-horizon structures are resolved with good signal to noise ratio. A power spectrum (spherical harmonics) analysis of the maps detects three peaks, at multipoles ℓ = (213_(-13)^(+10)),(541_(-32)^(+20))(845_(-25)^(+12)). In this paper we discuss the data analysis and the implications of these results for cosmology.

Published
2002

170. Z-Spec: A MM-wave spectrometer for measuring redshifts of submillimeter galaxies

Author

L. Earle, H. Nguyen, L. Duband, Jason Glenn, Charles M. Bradford, Mark Dragovan, B. J. Naylor, Jonas Zmuidzinas, J. J. Gromke, Hideo Matsuhara, J. J. Bock, and Porter, F. S.

Subjects
Physics, Spectrometer, business.industry, Bolometer, Physics::Optics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Grating, Submillimetre astronomy, Redshift, Galaxy, law.invention, Optics, law, business, Diffraction grating, Waveguide, Astrophysics::Galaxy Astrophysics
Abstract

We are building a background-limited, broadband millimeter-wave spectrometer (Z-Spec) for observations of CO rotational transitions from high-redshift dusty galaxies. The large instantaneous bandwidth (195 to 310 GHz) will enable redshifts of dust obscured galaxies to be unambiguously measured. Z-Spec uses a waveguide-coupled grating architecture in which the light propagation is confined within a parallel-plate waveguide. The grating is extremely compact compared to a classical free-space system. An array of silicon nitride bolometers cooled to 100 mK will provide background-limited performance. Z-Spec serves as a technology demonstration for a future space-borne far-infrared grating spectrometer.

Published
2002
Full Text
View/download PDF

171. Testing of Infrared Detectors Using a Zero Gravity Dilution Refrigerator

Author

J. J. Bock, Matthew Joseph Griffin, Alain Benoit, R. S. Bhatia, and Peter Mason

Subjects
Cryostat, Physics, business.industry, Bolometer, Thermistor, Electrical engineering, Cryocooler, Noise (electronics), law.invention, Optics, law, Zero gravity, Infrared detector, Dilution refrigerator, business
Abstract

We describe characterisation of the 100 mK dilution refrigerator, detectors and readout system for potential use on submillimetre spaceflight instruments. Relevant instruments include the High Frequency Instrument (HFI) on the Planck Surveyor mission for measurement of the anisotropies in the cosmic microwave background. The HFI will use a dilution refrigerator precooled by a 4 K mechanical cryocooler. We have used a modified variation of this zero gravity flight dilution system, precooled by a superfluid 4 He cryostat rather than mechanical cryocoolers. The cooling power at 100 mK was 102 nW. The prototype detector was of the bolometric spider web type with a germanium thermistor, as presently baselined for the HFI. The bolometer differential readout system used a sinusoidal AC bias, and is being further developed for flight use. Closed loop temperature control about a setpoint of 100 mK was also used. Dark bolometer tests were performed including measurement of detector heat capacity, time constant, noise and microphonic susceptibility. The bolometer achieved the sensitivity required for all channels of the HFI, but was a factor of three times slower than the slowest required device. A mechanical shaker was used to simulate the microphonic effects of cryocooler operation. For a bolometer acceleration of 21 m g rms at 100 mK with 73 nW of residual cooling power, the system exhibited no increase in low frequency noise above those levels measured for the response without microphonic excitation. This acceleration level was ~ 70 times greater than the level expected from the flight cryocoolers at the 4 K enclosure for the HFI. This gives us confidence in the proposed use of sensitive bolometers with cryocoolers for space missions.

Published
2002
Full Text
View/download PDF

172. Recent results from the cosmic microwave background radiation

Author

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

Subjects
Physics, Cosmic microwave background, Astronomy
Published
2001
Full Text
View/download PDF

173. Archeops: A High Resolution, Large Sky Coverage Balloon Experiment for Mapping CMB Anisotropies

Author

A. BENOIT, P. ADE, A. AMBLARD, R. ANSARI, E. AUBOURG, J. BARTLETT, J. P. BERNARD, R. S. BHATIA, A. BLANCHARD, J. J. BOCK, A. BOSCALERI, F. R. BOUCHET, A. BOURRACHOT, P. CAMUS, F. COUCHOT, P. DE BERNARDIS, J. DELABROUILLE, F. X. DESERT, O. DORE, M. DOUSPIS, L. DUMOULIN, X. DUPAC, P. FILLIATRE, K. GANGA, F. GANNAWAY, B. GAUTIER, M. GIARD, Y. GIRAUD HERAUD, R. GISPERT, L. GUGLIELMI, J. C. HAMILTON, S. HANANY, S. HENROT VERSILLE, V. V. HRISTOV, J. KAPLAN, G. LAGACHE, J. M. LAMARRE, A. E. LANGE, K. MADET, B. MAFFEI, D. MARRONE, S. MASI, J. A. MURPHY, F. NARAGHI, F. NATI, G. PERRIN, M. PIAT, J. L. PUGET, D. SANTOS, R. V. SUDIWALA, J. C. VANEL, D. VIBERT, E. WAKUI, D. YVON, Centre de Recherches sur les Très Basses Températures (CRTBT), Université Joseph Fourier - Grenoble 1 (UJF)-Institut National Polytechnique de Grenoble (INPG)-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Services communs OMP (UMS 831), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), ARCHEOPS, Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique de Grenoble (INPG)-Université Joseph Fourier - Grenoble 1 (UJF), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Benoit, A, Ade, P, Amblard, A, Ansari, R, Aubourg, E, Bartlett, J, Bernard, J, Bhatia, R, Blanchard, A, Bock, J, Boscaleri, A, Bouchet, F, Bourrachot, A, Camus, P, Couchot, F, DE BERNARDIS, P, Delabrouille, J, Desert, F, Dore, O, Douspis, M, Dumoulin, L, Dupac, X, Filliatre, P, Ganga, K, Gannaway, F, Gautier, B, Giard, M, GIRAUD HERAUD, Y, Gispert, R, Guglielmi, L, Hamilton, J, Hanany, S, HENROT VERSILLE, S, Hristov, V, Kaplan, J, Lagache, G, Lamarre, J, Lange, A, Madet, K, Maffei, B, Marrone, D, Masi, S, Murphy, J, Naraghi, F, Nati, F, Perrin, G, Piat, M, Puget, J, Santos, D, Sudiwala, R, Vanel, J, Vibert, D, Wakui, E, and Yvon, D

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Archeops is a balloon-borne instrument dedicated to measuring cosmic microwave background (CMB) temperature anisotropies at high angular resolution (8 arcminutes) over a large fraction (25%) of the sky in the millimetre domain. Based on Planck High Frequency Instrument (HFI) technology, cooled bolometers (0.1 K) scan the sky in total power mode with large circles at constant elevation. During the course of a 24-hour Arctic-night balloon flight, Archeops will observe a complete annulus on the sky in four frequency bands centered at 143, 217, 353 and 545 GHz with an expected sensitivity to CMB fluctuations of \~100muK for each of the 90 thousand 20 arcminute average pixels. We describe the instrument and its performance obtained during a test flight from Trapani (Sicily) to Spain in July 1999., Comment: 44 pages, 24 figures Full resolution postscript at http://publi.archeops.org

Published
2001
Full Text
View/download PDF

174. Images of the early universe from the BOOMERanG experiment

Author

J. J. Bock, B. P. Crill, E. Hivon, Pedro G. Ferreira, Andrew E. Lange, Nicola Vittorio, Philip Daniel Mauskopf, T. E. Montroy, J. Borrill, Silvia Masi, G. Romeo, D. Sforna, F. Piacentini, Andrew H. Jaffe, L. Miglio, Dmitry Pogosyan, Simon Prunet, P. Ade, A. Iacoangeli, P. C. Farese, Enzo Pascale, V. V. Hristov, G. De Troia, G. Polenta, M. Giacometti, Francesco Scaramuzzi, G. de Gasperis, K. Ganga, P. de Bernardis, S. Rao, A. Boscaleri, Alessandro Melchiorri, Calvin B. Netterfield, J. E. Ruhl, L. Martinis, J. R. Bond, Peter Mason, K. Coble, Wheeler, J. C., and Martel, H.

Subjects
Big Bang, Physics, Age of the universe, media_common.quotation_subject, BOOMERanG experiment, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Particle horizon, Universe, Metric expansion of space, De Sitter universe, Flatness problem, media_common
Abstract

The CMB is the fundamental tool to study the properties of the early universe and of the universe at large scales. In the framework of the Hot Big Bang model, when we look to the CMB we look back in time to the end of the plasma era, at a redshift ~ 1000, when the universe was ~ 50000 times younger, ~ 1000 times hotter and ~ 10^9 times denser than today. The image of the CMB can be used to study the physical processes there, to infer what happened before, and also to study the background geometry of our Universe.

Published
2001
Full Text
View/download PDF

175. MAXIMA: Millimeter-wave anisotropy experiment imaging array

Author

Bahman Rabii, A. Boscaleri, G. F. Smoot, C. D. Winant, V. V. Hristov, Pedro G. Ferreira, Shaul Hanany, J. Borrill, Paul L. Richards, M. E. Abroe, Junqiao Wu, Andrew H. Jaffe, J. Collins, A. T. Lee, P. de Bernardis, Calvin B. Netterfield, Sang-Yun Oh, Andrew E. Lange, Philip Daniel Mauskopf, Domingos Barbosa, J. J. Bock, B. Johnson, Amedeo Balbi, Peter A. R. Ade, Enzo Pascale, and R. Stompor

Subjects
Physics, Spectral index, Amplitude, Cosmic microwave background, Cosmic background radiation, Spectral density, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Anisotropy, Maxima, Square degree
Abstract

We discuss the status of the data obtained from the first two flights of the MAXIMA balloon-borne experiment. MAXIMA is sensitive to CMB fluctuations on angular scales from 10 arcmin to 5 degrees. The instrument uses a 16 element bolometric array with 3 frequency bands centered at 150, 240, and 410 GHz. An angular power spectrum of the CMB anisotropy has been obtained from the data of the first flight, MAXIMA-1, which shows a peak at l∼220 of 78±6 μK and an amplitude varying between 40 μK and 50 μK from 400

Published
2001
Full Text
View/download PDF

176. Detection of anisotropy in the Cosmic Microwave Background at horizon and sub-horizon scales with the BOOMERanG experiment

Author

S. Rao, A. Boscaleri, E. Hivon, Enzo Pascale, J. R. Bond, Pedro G. Ferreira, F. Pongetti, P. Miglio, Francesco Scaramuzzi, J. Borrill, K. Coble, Dmitry Pogosyan, F. Piacentini, D. Sforna, B. P. Crill, Andrew H. Jaffe, V. V. Hristov, N. Vottiorio, Calvin B. Netterfield, G. Romeo, Alessandro Melchiorri, G. De Troia, Simon Prunet, M. Giacometti, A. Iacoangeli, Philip Daniel Mauskopf, Peter Mason, G. de Gasperis, K. Ganga, J. J. Bock, Andrew E. Lange, P. de Bernardis, T. E. Montroy, Peter A. R. Ade, L. Martinis, Serena Masi, P. C. Farese, and J. E. Ruhl

Subjects
Physics, Scattering, Horizon, Astrophysics (astro-ph), Cosmic microwave background, BOOMERanG experiment, FOS: Physical sciences, Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, Settore FIS/05 - Astronomia e Astrofisica, Focus (optics), Anisotropy, Noise (radio)
Abstract

BOOMERanG has recently resolved structures on the last scattering surface at redshift ˜ 1100 with high signal to noise ratio. We review the technical advances which made this possible, and we focus on the current results for maps and power spectra, with special attention to the determination of the total mass-energy density in the Universe and of other cosmological parameters.

Published
2000

177. CMB ANISTROPIES: STATUS AND BOOMERANG

Author

J. R. Bond, P. de Bernardis, J. E. Ruhl, L. Miglio, Dmitry Pogosyan, J. Borrill, Andrew E. Lange, J. J. Bock, E. Hivon, F. Piacentini, Calvin B. Netterfield, Pedro G. Ferreira, Alessandro Melchiorri, G. Romeo, Enzo Pascale, G. De Troia, Francesco Scaramuzzi, M. Giacometti, T. E. Montroy, V. V. Hristov, P. D. Mauskopf, Andrew H. Jaffe, G. de Gasperis, K. Ganga, A. Iacoangelli, Simon Prunet, B. P. Crill, Nicola Vittorio, A. Boscaleri, K. Coble, Peter A. R. Ade, Serena Masi, P. C. Farese, and L. Martinis

Subjects
Cosmic microwave background, Astronomy
Published
2000
Full Text
View/download PDF

178. High Spatial Resolution Imaging of NGC 1068 in the Mid Infrared

Author

J. J. Bock, G. Neugebauer, K. Matthews, B. T. Soifer, E. E. Becklin, M. Ressler, K. Marsh, M. W. Werner, E. Egami, and R. Blandford

Subjects
Physics, Astrophysics (astro-ph), Doubly ionized oxygen, Flux, FOS: Physical sciences, Astronomy and Astrophysics, Torus, Astrophysics, Color temperature, Luminosity, Core (optical fiber), Space and Planetary Science, Absorption (electromagnetic radiation), Image resolution
Abstract

Mid-infrared observations of the central source of NGC 1068 have been obtained with a spatial resolution in the deconvolved image of 0.1" (~ 7pc). The central source is extended by ~1" in the north-south direction but appears unresolved in the east-west direction over most of its length. About two-thirds of its flux can be ascribed to a core structure which is itself elongated north-south and does not show a distinct unresolved compact source. The source is strongly asymmetric, extending significantly further to the north than to the south. The morphology of the mid-infrared emission appears similar to that of the radio jet, and has features which correlate with the images in [O III]. Its 12.5-24.5 micron color temperature ranges from 215 to 260 K and does not decrease smoothly with distance from the core. Silicate absorption is strongest in the core and to the south and is small in the north. The core, apparently containing two-thirds of the bolometric luminosity of the inner 4" diameter area, may be explained by a thick, dusty torus near the central AGN viewed at an angle of ~65 deg to its plane. There are, however, detailed difficulties with existing models, especially the narrow east-west width of the thin extended mid-infrared "tongue" to the north of the core. We interpret the tongue as re-processed visual and ultraviolet radiation that is strongly beamed and that originates in the AGN., Comment: 42 pages, 2 tables, 9 figures; Accepted for publication in AJ

Published
2000
Full Text
View/download PDF

179. MAXIMA-1: A measurement of the cosmic microwave background anisotropy on angular scales of 10 '-5 degrees

Author

Andrew H. Jaffe, Enzo Pascale, Sang-Yun Oh, Calvin B. Netterfield, J. Borrill, C. D. Winant, Paul L. Richards, V. V. Hristov, P. de Bernardis, R. Stompor, G. F. Smoot, Bahman Rabii, J. J. Bock, P. A. R. Ade, Pedro G. Ferreira, Aaron Lee, Shaul Hanany, Jiun-Huei Proty Wu, P. D. Mauskopf, Amedeo Balbi, Andrew E. Lange, and A. Boscaleri

Subjects
Physics, cosmic microwave background, 010308 nuclear & particles physics, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Spectral density, Dipole anisotropy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Photometer, Astrophysics, 01 natural sciences, law.invention, cosmology : observations, Amplitude, Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, law, 0103 physical sciences, Maxima, Anisotropy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Cosmic Background Imager
Abstract

We present a map and an angular power spectrum of the anisotropy of the cosmic microwave background (CMB) from the first flight of MAXIMA. MAXIMA is a balloon-borne experiment with an array of 16 bolometric photometers operated at 100 mK. MAXIMA observed a 124 square degrees region of the sky with 10 arcminute resolution at frequencies of 150, 240 and 410 GHz. The data were calibrated using in-flight measurements of the CMB dipole anisotropy. A map of the CMB anisotropy was produced from three 150 and one 240 GHz photometer without need for foreground subtractions. Analysis of this CMB map yields a power spectrum for the CMB anisotropy over the range 36 < l < 785. The spectrum shows a peak with an amplitude of 78 +/- 6 micro-Kelvin at l ~ 220 and an amplitude varying between ~40 micro-Kelvin and ~50 micro-Kelvin for 400 < l < 785.

Published
2000

180. A COSMIC MICROWAVE BACKGROUND LENSING MASS MAP AND ITS CORRELATION WITH THE COSMIC INFRARED BACKGROUND

Author

N. W. Halverson, R. Williamson, M. Lueker, T. de Haan, M. Brodwin, K. A. Aird, J. Mehl, S. Hoover, Elizabeth George, G. Marsden, G. P. Holder, C. L. Reichardt, S. S. Meyer, J. D. Hrubes, K. K. Schaffer, Daniel P. Marrone, C. Pryke, Daniel M. Luong-Van, Bradford Benson, A. van Engelen, S. Padin, W. L. Holzapfel, Erik Shirokoff, Marius Millea, K. T. Story, Benjamin L. Schulz, J. T. Sayre, T. M. Crawford, J. D. Vieira, J. P. Dudley, T. E. Montroy, E. M. Leitch, S. Bhattacharya, J. E. Ruhl, Joseph J. Mohr, M. A. Dobbs, O. Zahn, Ryan Keisler, Lindsey Bleem, Chihway Chang, A. T. Crites, Jeff McMahon, Michael Zemcov, J. J. Bock, K. Vanderlinde, H-M. Cho, A. A. Stark, Helmuth Spieler, A. Conley, T. Plagge, John E. Carlstrom, L. Shaw, Z. K. Staniszewski, Zhen Hou, Marco Viero, Adrian T. Lee, and Lloyd Knox

Subjects
Physics, 010308 nuclear & particles physics, Cosmic microwave background, Astrophysics::Instrumentation and Methods for Astrophysics, Sigma, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Redshift, Gravitation, Spire, South Pole Telescope, Space and Planetary Science, Cosmic infrared background, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We use a temperature map of the cosmic microwave background (CMB) obtained using the South Pole Telescope at 150 GHz to construct a map of the gravitational convergence to z ~ 1100, revealing the fluctuations in the projected mass density. This map shows individual features that are significant at the ~ 4 sigma level, providing the first image of CMB lensing convergence. We cross-correlate this map with Herschel/SPIRE maps covering 90 square degrees at wavelengths of 500, 350, and 250 microns. We show that these submillimeter-wavelength (submm) maps are strongly correlated with the lensing convergence map, with detection significances in each of the three submm bands ranging from 6.7 to 8.8 sigma. We fit the measurement of the cross power spectrum assuming a simple constant bias model and infer bias factors of b=1.3-1.8, with a statistical uncertainty of 15%, depending on the assumed model for the redshift distribution of the dusty galaxies that are contributing to the Herschel/SPIRE maps.

Published
2013
Full Text
View/download PDF

181. Effect of Mo/Cu Superconducting Bilayer Geometry on Ultra-Sensitive Transition-Edge Sensor Performance

Author

W. A. Holmes, J. J. Bock, Charles M. Bradford, M. Kenyon, Pierre Echternach, Andrew D. Beyer, B. Bumble, and Marcus Runyan

Subjects
Superconductivity, Materials science, Bilayer, Thermistor, chemistry.chemical_element, Geometry, Condensed Matter Physics, Electronic, Optical and Magnetic Materials, chemistry, Electrical resistance and conductance, Proximity effect (superconductivity), Electrical and Electronic Engineering, Transition edge sensor, Tin, Noise-equivalent power
Abstract

We built membrane-isolated transition-edge sensors (TESs) for the background-limited infrared/sub-mm spectrograph using Mo/Cu superconducting bilayer thermistors of varying geometry and found that undesired proximity effects, including the so-called longitudinal proximity effect (LoPE) and the latitudinal inverse proximity effect, affect both the superconducting transition temperature TC and the sharpness of the transition α = dlogR/dlogT. The LoPE and latitudinal inverse proximity effect arise because of unintentional proximity effects between the bilayer thermistors, the superconducting wiring of the TES circuitry, and normal metal decorations added to mitigate the LoPE. We examined Mo/Cu bilayer films with widths of 120 μm and lengths of 5, 10, 20, 40, and 120 μm, and studied the variation of TC, α, and approximate 80% resistance per square (R0.8) with Ti (TC ~ 500 mK) and TiN (TC ~ 3.8 K) wiring to the devices. We found larger α values in general for the Ti wiring, where α was as high as 90 for 20-120 μm devices and decreased to 20 for 5-μm-wide devices. We then built arrays of TESs with bilayer thermistor lengths of 10 μm, Ti contacts, TiN wiring, and Au borders. The devices were expected to demonstrate a noise equivalent power less than or equal to 10-19 W/Hz1/2. We report a measured noise equivalent power at 87 mK of (0.95 ±0.2) × 10-19 W/Hz1/2 and a response time τ of (360 ± 30)ms on our best device with a thermal conductance x1/2 = (15 ±5)fW/K, TC = (120.5 ±3.5)mK, and stray power PD = (135 ±85)aW. The thermistor had a value of RN = 6 mΩ and value of α = dlogR/dlogT between 10 and 60 in the transition. We compare our measured performance with the performance specifications needed for ultrasensitive TESs on the Background-Limited Infrared/Sub-mm Spectrograph (BLISS) and discuss paths forward.

Published
2013
Full Text
View/download PDF

183. Planckearly results. I. ThePlanckmission

Author

P. A. R. Ade[82], N. Aghanim[54], M. Arnaud[68], M. Ashdown[66-4], J. Aumont[54], C. Baccigalupi[80], M. Baker[37], A. Balbi[31], A. J. Banday[89-9-73], R. B. Barreiro[62], J. G. Bartlett[3-64], E. Battaner[91], K. Benabed[55], K. Bennett[38], A. Benoît[53], J.-P. Bernard[89-9], M. Bersanelli[28-46], R. Bhatia[5], J. J. Bock[64-10], A. Bonaldi[42], J. R. Bond[6], J. Borrill[72-84], F. R. Bouchet[55], T. Bradshaw[79], M. Bremer[38], M. Bucher[3], C. Burigana[45], R. C. Butler[45], P. Cabella[31], C. M. Cantalupo[72], B. Cappellini[46], J.-F. Cardoso[69-3-55], R. Carr[35], M. Casale[35], A. Catalano[3-67], L. Cayón[21], A. Challinor[59-66-12], A. Chamballu[51], J. Charra[54], R.-R. Chary[52], L.-Y. Chiang[58], C. Chiang[20], P. R. Christensen[76-32], D. L. Clements[51], S. Colombi[55], F. Couchot[71], A. Coulais[67], B. P. Crill[64-77], G. Crone[38], M. Crook[79], F. Cuttaia[45], L. Danese[80], O. D'Arcangelo[63], R. D. Davies[65], R. J. Davis[65], P. de Bernardis[27], J. de Bruin[37], G. de Gasperis[31], A. de Rosa[45], G. de Zotti[42-80], J. Delabrouille[3], J.-M. Delouis[55], F.-X. Désert[49], J. Dick[80], C. Dickinson[65], K. Dolag[73], H. Dole[54], S. Donzelli[46-60], O. Doré[64-10], U. Dörl[73], M. Douspis[54], X. Dupac[36], G. Efstathiou[59], T. A. Enßlin[73], H. K. Eriksen[60], F. Finelli[45], S. Foley[37], O. Forni[89-9], P. Fosalba[56], M. Frailis[44], E. Franceschi[45], M. Freschi[36], T. C. Gaier[64], S. Galeotta[44], J. Gallegos[36], B. Gandolfo[37], K. Ganga[3-52], M. Giard[89-9], G. Giardino[38], G. Gienger[37], Y. Giraud-Héraud[3], J. González[35], J. González-Nuevo[80], K. M. Górski[64, 93], S. Gratton[66, 59], A. Gregorio[29], A. Gruppuso[45], G. Guyot[48], J. Haissinski[71], F. K. Hansen[60], D. Harrison[59-66], G. Helou[10], S. Henrot-Versillé[71], C. Hernández-Monteagudo[73], D. Herranz[62], S. R. Hildebrandt[10-70-61], E. Hivon[55], M. Hobson[4], W. A. Holmes[64], A. Hornstrup[14], W. Hovest[73], R. J. Hoyland[61], K. M. Huffenberger[92], A. H. Jaffe[51], T. Jagemann[36], W. C. Jones[20], J. J. Juillet[87], M. Juvela[19], P. Kangaslahti[64], E. Keihänen[19], R. Keskitalo[64-19], T. S. Kisner[72], R. Kneissl[34-5], L. Knox[23], M. Krassenburg[38], H. Kurki-Suonio[19-40], G. Lagache[54], A. Lähteenmäki[1-40], J.-M. Lamarre[67], A. E. Lange[52], A. Lasenby[4-66], R. J. Laureijs[38], C. R. Lawrence[64], S. Leach[80], J. P. Leahy[65], R. Leonardi[36-38-24], C. Leroy[54-89-9], P. B. Lilje[60-11], M. Linden-Vørnle[14], M. López-Caniego[62], S. Lowe[65], P. M. Lubin[24], J. F. Macías-Pérez[70], T. Maciaszek[7], C. J. MacTavish[66], B. Maffei[65], D. Maino[28-46], N. Mandolesi[45], R. Mann[81], M. Maris[44], E. Martínez-González[62], S. Masi[27], M. Massardi[42], S. Matarrese[26], F. Matthai[73], P. Mazzotta[31], A. McDonald[37], P. McGehee[52], P. R. Meinhold[24], A. Melchiorri[27], J.-B. Melin[13], L. Mendes[36], A. Mennella[28-44], C. Mevi[37], R. Miniscalco[37], S. Mitra[64], M.-A. Miville-Deschênes[54-6], A. Moneti[55], L. Montier[89-9], G. Morgante[45], N. Morisset[50], D. Mortlock[51], D. Munshi[82-59], A. Murphy[75], P. Naselsky[76-32], P. Natoli[30-2-45], C. B. Netterfield[16], H. U. Nørgaard-Nielsen[14], F. Noviello[54], D. Novikov[51], I. Novikov[76], I. J. O'Dwyer[64], I. Ortiz[35], S. Osborne[86], P. Osuna[35], C. A. Oxborrow[14], F. Pajot[54], R. Paladini[85, 10], B. Partridge[39], F. Pasian[44], T. Passvogel[38], G. Patanchon[3], D. Pearson[64], T. J. Pearson[10-52], O. Perdereau[71], L. Perotto[70], F. Perrotta[80], F. Piacentini[27], M. Piat[3], E. Pierpaoli[18], S. Plaszczynski[71], P. Platania[63], E. Pointecouteau[89-9], G. Polenta[2-43], N. Ponthieu[54], L. Popa[57], T. Poutanen[40-19-1], G. Prézeau[10-64], S. Prunet[55], J.-L. Puget[54], J. P. Rachen[73], W. T. Reach[90], R. Rebolo[61-33], M. Reinecke[73], J.-M. Reix[87], C. Renault[70], S. Ricciardi[45], T. Riller[73], I. Ristorcelli[89-9], G. Rocha[64-10], C. Rosset[3], M. Rowan-Robinson[51], J. A. Rubiño-Martín[61-33], B. Rusholme[52], E. Salerno[8], M. Sandri[45], D. Santos[70], G. Savini[78], B. M. Schaefer[88], D. Scott[17], M. D. Seiffert[64], P. Shellard[12], A. Simonetto[63], G. F. Smoot[22-72-3], C. Sozzi[63], J.-L. Starck[68-13], J. Sternberg[38], F. Stivoli[47], V. Stolyarov[4], R. Stompor[3], L. Stringhetti[45], R. Sudiwala[82], R. Sunyaev[73-83], J.-F. Sygnet[55], D. Tapiador[35], J. A. Tauber[38], D. Tavagnacco[44], D. Taylor[35], L. Terenzi[45], D. Texier[35], L. Toffolatti[15], M. Tomasi[28-46], J.-P. Torre[54], M. Tristram[71], J. Tuovinen[74], M. Türler[50], M. Tuttlebee[37], G. Umana[41], L. Valenziano[45], J. Valiviita[60], J. Varis[74], L. Vibert[54], P. Vielva[62], F. Villa[45], N. Vittorio[31], L. A. Wade[64], B. D. Wandelt[55-25], C. Watson[37], S. D. M. White[73], M. White[22], A. Wilkinson[65], D. Yvon[13], A. Zacchei[44], A. Zonca[24], Plank Collaboration, Universidad de Cantabria, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), 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), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Recherche en Informatique (LRI), Université Paris-Sud - Paris 11 (UP11)-CentraleSupélec-Centre National de la Recherche Scientifique (CNRS), PLANCK, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Baker, M., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Bennett, K., Benoît, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bradshaw, T., Bremer, M., Bucher, M., Burigana, C., Butler, R. C., Cabella, P., Cantalupo, C. M., Cappellini, B., Cardoso, J. F., Carr, R., Casale, M., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Charra, J., Chary, R. R., Chiang, L. Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Crone, G., Crook, M., Cuttaia, F., Danese, L., D'Arcangelo, O., Davies, R. D., Davis, R. J., de Bernardis, P., de Bruin, J., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dick, J., Dickinson, C., Dolag, K., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Foley, S., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Freschi, M., Gaier, T. C., Galeotta, S., Gallegos, J., Gandolfo, B., Ganga, K., Giard, M., Giardino, G., Giraud Héraud, Y., González, J., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Guyot, G., Haissinski, J., Hansen, F. K., Harrison, D., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jagemann, T., Jones, W. C., Juillet, J. J., Juvela, M., Kangaslahti, P., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Krassenburg, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lange, A. E., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., Leroy, C., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lowe, S., Lubin, P. M., Macías Pérez, J. F., Maciaszek, T., Mactavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Mcdonald, A., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Melin, J. B., Mendes, L., Mennella, A., Mevi, C., Miniscalco, R., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Ortiz, I., Osborne, S., Osuna, P., Oxborrow, C. A., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Passvogel, T., Patanchon, G., Pearson, D., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Reix, J. M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan Robinson, M., Rubiño Martín, J. A., Rusholme, B., Salerno, E., Sandri, M., Santos, D., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Simonetto, A., Smoot, G. F., Sozzi, C., Starck, J. L., Sternberg, J., Stivoli, F., Stolyarov, V., Stompor, R., Stringhetti, L., Sudiwala, R., Sunyaev, R., Sygnet, J. F., Tapiador, D., Tauber, J. A., Tavagnacco, Daniele, Taylor, D., Terenzi, L., Texier, D., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Varis, J., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, C., White, S. D. M., White, M., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A., Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), 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), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Département de Physique des Particules (ex SPP) (DPP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Hélium : du fondamental aux applications (HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), CentraleSupélec-Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, and Helsinki Institute of Physics

Subjects
Experimental Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Computer science, Surveys, Cosmic background radiation, 7. Clean energy, 01 natural sciences, CMB physics, Space vehicles: instruments, Instrumentation: detectors, observations [Cosmology], Instrumentation, 010303 astronomy & astrophysics, detectors [Instrumentation], QB, detectors, media_common, Planck ESA mission, Conjunction (astronomy), Cosmology: observations, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmology, observations, Early results, cosmic backround radiation, instruments, symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], cosmology: observations, cosmic background radiation, surveys, space vehicles: instruments, instrumentation: detectors, catalogs, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, space vehicles, cosmology, instrumentation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, education, FOS: Physical sciences, Catalogs, Space vehicles, instruments [Space vehicles], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Planck, Early release, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010308 nuclear & particles physics, Payload, Astronomy, Astronomy and Astrophysics, 115 Astronomy, Space science, Catalogues, Astrophysics - Astrophysics of Galaxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), Satellite
Abstract

16 páginas, 14 figuras, 3 tablas.-- Planck Collaboration: et al., The European Space Agency’s Planck satellite was launched on 14 May 2009, and has been surveying the sky stably and continuously since 13 August 2009. Its performance is well in line with expectations, and it will continue to gather scientific data until the end of its cryogenic lifetime. We give an overview of the history of Planck in its first year of operations, and describe some of the key performance aspects of the satellite. This paper is part of a package submitted in conjunction with Planck’s Early Release Compact Source Catalogue, the first data product based on Planck to be released publicly. The package describes the scientific performance of the Planck payload, and presents results on a variety of astrophysical topics related to the sources included in the Catalogue, as well as selected topics on diffuse emission., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU).

Published
2011
Full Text
View/download PDF

184. Radial distribution of gas and dust in spiral galaxies

Author

M. Pohlen, L. Cortese, M. W. L. Smith, S. A. Eales, A. Boselli, G. J. Bendo, H. L. Gomez, A. Papageorgiou, R. Auld, M. Baes, J. J. Bock, M. Bradford, V. Buat, N. Castro-Rodriguez, P. Chanial, S. Charlot, L. Ciesla, D. L. Clements, A. Cooray, D. Cormier, E. Dwek, D. Elbaz, M. Galametz, F. Galliano, W. K. Gear, J. Glenn, M. Griffin, S. Hony, K. G. Isaak, L. R. Levenson, N. Lu, S. Madden, B. O'Halloran, K. Okumura, S. Oliver, M. J. Page, P. Panuzzo, T. J. Parkin, I. Perez-Fournon, N. Rangwala, E. E. Rigby, H. Roussel, A. Rykala, N. Sacchi, M. Sauvage, B. Schulz, M. R. P. Schirm, L. Spinoglio, J. A. Stevens, S. Srinivasan, M. Symeonidis, M. Trichas, M. Vaccari, L. Vigroux, C. D. Wilson, H. Wozniak, G. S. Wright, W. W. Zeilinger, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Metallicity, nuclei [galaxies], galaxies [submillimeter], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spatial distribution, galaxies [infrared], 01 natural sciences, law.invention, law, 0103 physical sciences, fundamental parameters [galaxies], Astrophysics::Solar and Stellar Astrophysics, DUST EMISSION, Variation (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, Spiral galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Photometer, Virgo Cluster, Galaxy, spiral [galaxies], Physics and Astronomy, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract

With appropriate spatial resolution, images of spiral galaxies in thermal infrared (similar to 10 mu m and beyond) often reveal a bright central component, distinct from the stellar bulge, superimposed on a disk with prominent spiral arms. ISO and Spitzer studies have shown that much of the scatter in the mid-infrared colors of spiral galaxies is related to changes in the relative importance of these two components, rather than to other modifications, such as the morphological type or star formation rate, that affect the properties of the galaxy as a whole. With the Herschel imaging capability from 70 to 500 mu m, we revisit this two-component approach at longer wavelengths, to see if it still provides a working description of the brightness distribution of galaxies, and to determine its implications on the interpretation of global far-infrared properties of galaxies. We quantify the luminosity of the central component by both a decomposition of the radial surface brightness profile and a direct extraction in 2D. We find the central component contribution is variable within the three galaxies in our sample, possibly connected more directly to the presence of a bar than to the morphological type. The central component's relative contribution is at its maximum in the mid-infrared range and drops around 160 mu m to reach a constant value beyond 200 mu m. The central component contains a greater fraction of hot dust than the disk component, and while the colors of the central components are scattered, colors of the disk components are more homogenous from one galaxy to the next.

Published
2010
Full Text
View/download PDF

185. A rocket-borne observation of diffuse far-infrared emission from interstellar dust

Author

Philip Daniel Mauskopf, V. V. Hristov, Masahiro Tanaka, Paul L. Richards, J. J. Bock, Mitsunobu Kawada, T. Matsumoto, Hideo Matsuhara, Andrew E. Lange, and Shuji Matsuura

Subjects
Physics, Molecular cloud, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Photometer, Spectral bands, law.invention, Telescope, Far infrared, law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Infrared cirrus, Emission spectrum, Astrophysics::Galaxy Astrophysics, Cosmic dust
Abstract

We report observations of diffuse far‐infrared emission from interstellar dust at high Galactic latitudes using a rocket‐borne, liquid‐helium cooled telescope and photometer. The photometer has 5 spectral bands ranging from 90 μm to 190 μm with 0.5°∼0.65°FWHM fields‐of‐view. The detectors, stressed and unstressed Ge:Ga photoconductors, were cooled to 1 K and coupled to charge integrating amplifiers to achieve high sensitivity. We observed regions near Ursa Major including infrared cirrus, high latitude molecular clouds, and the HI hole, a region of uniquely low neutral hydrogen column density. Preliminary analysis shows a strong correlation of the emission at 134, 154, and 186 μm with 100 μm IRAS data.

Published
1992
Full Text
View/download PDF

186. Observation of [CII] 158 μm emission from the diffuse interstellar medium

Author

Paul L. Richards, Philip Daniel Mauskopf, Hideo Matsuhara, V. V. Hristov, Shuji Matsuura, Mitsunobu Kawada, Masahiro Tanaka, J. J. Bock, T. Matsumoto, and Andrew E. Lange

Subjects
Physics, Ursa Major, Astrophysics::High Energy Astrophysical Phenomena, Molecular cloud, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Galaxy, Interstellar medium, Far infrared, Infrared cirrus, Atomic physics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We report the first direct detection of 158 μm [CII] line emission from the diffuse interstellar medium at high galactic latitude. We measured the integrated line intensity in a 36’ field‐of‐view along a triangular scan in a 5°×20° region in Ursa Major using a rocket‐borne, liquid helium cooled spectrophotometer. The scans included high latitude infrared cirrus, molecular clouds, a bright external galaxy, M82, and the HI Hole, a region of uniquely low neutral hydrogen column density. Emission from [CII] is observed in all regions, and in the absence of CO emission it is well correlated with neutral hydrogen column density. We deduce a [CII] gas cooling rate of (2.6±0.6)×10−26 ergs s−1 H‐atom−1, in good agreement with a recent observation of UV absorption lines at high galactic latitude.

Published
1992
Full Text
View/download PDF

187. Optical coupling

Author

J J Bock, J Gundersen, A T Lee, P L Richards, and E Wollack

Subjects
History, Computer Science Applications, Education
Published
2009
Full Text
View/download PDF

188. ERRATUM: 'A SEARCH FOR COSMIC MICROWAVE BACKGROUND ANISOTROPIES ON ARCMINUTE SCALES WITH BOLOCAM' (2009, ApJ, 690, 1597)

Author

Peter A. R. Ade, J. J. Bock, Jack Sayers, Glenn Laurent, S. F. Edgington, Sunil Golwala, James E. Aguirre, D. Haig, Jason Glenn, H. T. Nguyen, Philip Daniel Mauskopf, A. Goldin, P. Rossinot, and Andrew E. Lange

Subjects
Physics, Space and Planetary Science, media_common.quotation_subject, Cosmic microwave background, Astronomy, Astronomy and Astrophysics, Astrophysics, Anisotropy, Electromagnetic radiation, Microwave, Universe, media_common
Published
2009
Full Text
View/download PDF

189. ERRATUM

Author

R. Stompor, Peter A. R. Ade, P. de Bernardis, Sang-Yun Oh, J. Borrill, A. T. Lee, Paul L. Richards, A. Boscaleri, Bahman Rabii, Shaul Hanany, Pedro G. Ferreira, Enzo Pascale, C. D. Winant, V. V. Hristov, Amedeo Balbi, G. F. Smoot, J. J. Bock, Junqiao Wu, and Andrew H. Jaffe

Subjects
Physics, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, 010306 general physics, Maxima, 01 natural sciences
Published
2001
Full Text
View/download PDF

190. A rocket-borne observation of the near-infrared sky brightness

Author

Mitsunobu Kawada, Masahiro Tanaka, Manabu Noda, Shuji Matsuura, Toshio Matsumoto, Hideo Matsuhara, and J. J. Bock

Subjects
Physics, Brightness, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Near-infrared spectroscopy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, Latitude, Wavelength, Space and Planetary Science, Sky brightness, Astrophysics::Galaxy Astrophysics, Background radiation
Abstract

Accepted: 1994-04-26, 資料番号: SA1001324000

Published
1994
Full Text
View/download PDF

191. Mini-Hoffmann External Fixator for Fractures of the Hand

Author

J. J. Bock

Subjects
Orthodontics, External fixation, Articular fracture, External fixator, business.industry, medicine.medical_treatment, Medicine, Fracture site, business
Abstract

The Hoffmann mini-external fixator is a simple versatile device that has been useful in the treatment of many small fractures involving the hand, foot and maxiofacial injuries. My paper will be confined to its use in the hand. It has been very valuable for treatment of unstable comminuted fractures, arthrodeses, conditions associated with extensive bone loss, comminution and loss of stability, reimplantation and digital lengthening.

Published
1982
Full Text
View/download PDF

192. BICEP2/Keck Array XI: Beam Characterization and Temperature-to-Polarization Leakage in the BK15 Data Set.

Author

P. A. R. Ade, Z. Ahmed, R. W. Aikin, D. Barkats, S. J. Benton, C. A. Bischoff, J. J. Bock, R. Bowens-Rubin, J. A. Brevik, I. Buder, E. Bullock, V. Buza, J. Connors, J. Cornelison, B. P. Crill, M. Crumrine, M. Dierickx, L. Duband, J. P. Filippini, and S. Fliescher

Subjects
COSMIC background radiation, LEAKAGE
Abstract

Precision measurements of cosmic microwave background (CMB) polarization require extreme control of instrumental systematics. In a companion paper we have presented cosmological constraints from observations with the BICEP2 and Keck Array experiments up to and including the 2015 observing season (BK15), resulting in the deepest CMB polarization maps to date and a statistical sensitivity to the tensor-to-scalar ratio of σ(r) = 0.020. In this work we characterize the beams and constrain potential systematic contamination from main beam shape mismatch at the three BK15 frequencies (95, 150, and 220 GHz). Far-field maps of 7360 distinct beam patterns taken from 2010–2015 are used to measure differential beam parameters and predict the contribution of temperature-to-polarization leakage to the BK15 B-mode maps. In the multifrequency, multicomponent likelihood analysis that uses BK15, Planck, and Wilkinson Microwave Anisotropy Probe maps to separate sky components, we find that adding this predicted leakage to simulations induces a bias of Δr = 0.0027 ± 0.0019. Future results using higher-quality beam maps and improved techniques to detect such leakage in CMB data will substantially reduce this uncertainty, enabling the levels of systematics control needed for BICEP Array and other experiments that plan to definitively probe large-field inflation. [ABSTRACT FROM AUTHOR]

Published
2019
Full Text
View/download PDF

193. Imaging the early universe with the BOOMERANG experiment

Author

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

Subjects
Inflation (cosmology), Big Bang, Physics, General Relativity and Quantum Cosmology, Age of the universe, De Sitter universe, Cosmic microwave background, BOOMERanG experiment, Astronomy, Lambda-CDM model, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Flatness problem
Abstract

The BOOMERanG experiment has recently detected temperature fluctuations the Cosmic Microwave Background (CMB), the otherwise isotropic radiation coming from the early Universe. These anisotropies have a low contrast (about 30 ppm) and feature a peculiar angular power spectrum at angles corresponding to sub-horizon scales at recombination. In the current cosmological model, these structures result from acoustic oscillations in the primeval plasma. In the framework of the Hot Big Bang theory with the inflationary hypothesis, the statistical properties of the image of the CMB allow us to measure most of the cosmological parameters.

194. 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

195. Planck 2015 results. II. Low Frequency Instrument data processing

Author

E. Martínez-González, F. Couchot, Hannu Kurki-Suonio, M. Piat, T. Riller, P. A. R. Ade, W. A. Holmes, B. Racine, S. Mottet, Peregrine McGehee, J.-F. Sygnet, F. Cuttaia, D. L. Clements, N. Ponthieu, L. Sanselme, J. J. Bock, X. Dupac, A. Curto, Simon Prunet, Jérôme Bobin, A. Chamballu, R. Kneissl, R. Keskitalo, Steven Gratton, K. Ganga, P. Bielewicz, G. Rocha, William T. Reach, O. Doré, J.-L. Puget, D. L. Harrison, Jean-François Cardoso, L. Perotto, Jose M. Diego, Lloyd Knox, E. P. S. Shellard, R. Paladini, O. Herent, W. Hovest, E. Pointecouteau, P. B. Lilje, R. J. Laureijs, J. A. Tauber, R. B. Barreiro, Michele Liguori, J. Borrill, A. Benoit-Lévy, Fernando Atrio-Barandela, K. M. Górski, M. Tristram, J. Delabrouille, F. Piacentini, L. Vibert, M. Giard, F. Noviello, D. Hanson, Aurelien A. Fraisse, R. J. Davis, G. Hurier, A. Gregorio, George Helou, François R. Bouchet, Calvin B. Netterfield, B. P. Crill, Charles R. Lawrence, G. Patanchon, J. F. Macías-Pérez, G. Roudier, Fabio Finelli, D. Pietrobon, Carol Anne Oxborrow, A. Zonca, D. Yvon, Bruno Maffei, F. Paci, Lung-Yih Chiang, Silvia Masi, S. D. M. White, F. Pajot, R. D. Davies, M. Le Jeune, A. de Rosa, H. C. Chiang, Sophie Henrot-Versille, L. P. L. Colombo, Michael P. Hobson, Peter Meinhold, K. Benabed, F. Perrotta, Dmitry Novikov, M. Frailis, Daniele Tavagnacco, Carlo Baccigalupi, F.-X. Désert, Alessandro Melchiorri, Julien Lesgourgues, Mika Juvela, E. Hivon, Xin Chen, J. R. Bond, Dipak Munshi, François Orieux, George Efstathiou, J.-M. Lamarre, Alessandro Gruppuso, Nicola Vittorio, M. Arnaud, J. González-Nuevo, A. Zacchei, T. Poutanen, C. Armitage-Caplan, G. W. Pratt, B. Rusholme, Michael Rowan-Robinson, Andrew H. Jaffe, Fabio Pasian, F. Villa, J.-P. Bernard, Gianluca Morgante, G. Umana, Sabino Matarrese, Marc-Antoine Miville-Deschenes, L. Montier, Locke D. Spencer, Philip Lubin, A. Moneti, Luca Valenziano, S. Mitra, J. Knoche, Allan Hornstrup, Michele Maris, Federico Nati, Z. Hou, Torsten A. Enßlin, M. Ashdown, Anthony Lasenby, H. K. Eriksen, M. Tomasi, D. Paoletti, G. Lagache, S. Osborne, R. V. Sudiwala, E. Keihänen, Jean-Luc Starck, S. R. Hildebrandt, D. J. Marshall, Luca Terenzi, C. Combet, V. Stolyarov, C. J. MacTavish, P. R. Christensen, Marco Bersanelli, B. D. Wandelt, Rafael Rebolo, A. Coulais, T. R. Jaffe, D. Herranz, M. Kunz, P. Natoli, Martin Reinecke, E. Battaner, Carlo Burigana, L. Mendes, Pavel D. Naselsky, F. Boulanger, L. Danese, P. de Bernardis, Stéphane Plaszczynski, Mathieu Remazeilles, I. Ristorcelli, G. de Zotti, Giovanna Giardino, Clive Dickinson, M. Douspis, D. Sutton, J. Aumont, J. Valiviita, C. North, A. Sauvé, Aurélien Benoit, Lawrence A. Wade, S. Ricciardi, B. Van Tent, A. J. Banday, F. Sureau, Nazzareno Mandolesi, J.-M. Delouis, C. Rosset, Jon E. Gudmundsson, L. Pagano, Hans Ulrik Nørgaard-Nielsen, R. Stompor, D. Girard, F. Matthai, Jörg P. Rachen, C. Renault, A.-S. Suur-Uski, D. Santos, M. Bucher, M. Migliaccio, R. Leonardi, Olivier Forni, F. K. Hansen, M. Tucci, Stéphane Colombi, M. Bridges, E. Franceschi, P. Vielva, S. Galeotta, Pierrick Martin, Elena Pierpaoli, Y. Giraud-Héraud, Pasquale Mazzotta, H. Dole, Theodore Kisner, Claude Leroy, I. D. Novikov, G. Prézeau, M. López-Caniego, R.-R. Chary, L. Popa, Daniel J. Mortlock, C. Hernández-Monteagudo, Kevin M. Huffenberger, Jo Dunkley, G. Polenta, M. Linden-Vørnle, Sarah E. Church, J. W. Bowyer, W. C. Jones, A. Mennella, Nabila Aghanim, O. Perdereau, S. Donzelli, Giorgio Savini, A. Catalano, S. Techene, Ade, P. A. R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., Barreiro, R. B., Bartolo, N., Basak, S., Battaglia, PAOLA MARIA, Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cardoso, J. F., Castex, G., Catalano, A., Chamballu, A., Christensen, P. R., Colombi, S., Colombo, L. P. L., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, Simona, Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschet, C., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud Héraud, Y., Gjerløw, E., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Hanson, D., Harrison, D. L., Henrot Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T. S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., Lindholm, V., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Novikov, D., Novikov, I., Oppermann, N., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, Erik, Rosset, C., Rossetti, M., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Stolyarov, V., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Wehus, I. K., Wilkinson, A., Yvon, D., Zacchei, A, Zonca, A., Ade, P, Aghanim, N, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, A, Barreiro, R, Bartolo, N, Basak, S, Battaglia, P, Battaner, E, Benabed, K, Benoît, A, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bock, J, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Bucher, M, Burigana, C, Butler, R, Calabrese, E, Cardoso, J, Castex, G, Catalano, A, Chamballu, A, Christensen, P, Colombi, S, Colombo, L, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, T, Eriksen, H, Fergusson, J, Finelli, F, Forni, O, Frailis, M, Franceschet, C, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Giard, M, Giraud Héraud, Y, Gjerløw, E, González Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, F, Hanson, D, Harrison, D, Henrot Versillé, S, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Hurier, G, Jaffe, A, Jaffe, T, Juvela, M, Keihänen, E, Keskitalo, R, Kiiveri, K, Kisner, T, Knoche, J, Krachmalnicoff, N, Kunz, M, Kurki Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leahy, J, Leonardi, R, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, Lindholm, V, López Caniego, M, Lubin, P, Macías Pérez, J, Maggio, G, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Mazzotta, P, Mcgehee, P, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Montier, L, Morgante, G, Morisset, N, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nørgaard Nielsen, H, Novikov, D, Novikov, I, Oppermann, N, Paci, F, Pagano, L, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, T, Peel, M, Perdereau, O, Perotto, L, Perrotta, F, Pettorino, V, Piacentini, F, Pierpaoli, E, Pietrobon, D, Pointecouteau, E, Polenta, G, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Rachen, J, Rebolo, R, Reinecke, M, Remazeilles, M, Renzi, A, Rocha, G, Romelli, E, Rosset, C, Rossetti, M, Roudier, G, Rubiño Martín, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Scott, D, Seiffert, M, Shellard, E, Spencer, L, Stolyarov, V, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Türler, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vassallo, T, Vielva, P, Villa, F, Wade, L, Wandelt, B, Watson, R, Wehus, I, Wilkinson, A, Yvon, D, Zonca, A, Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Planck, Hélium : du fondamental aux applications (NEEL - HELFA), 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), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Space vehicles: instruments – Methods:data analysis – cosmic microwave background, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], 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], Astronomy, Cosmic microwave background, FOS: Physical sciences, Space vehicles: instrument, Cosmic background radiation, 01 natural sciences, NO, instruments [Space vehicles], Optics, Settore FIS/05 - Astronomia e Astrofisica, Methods: data analysis, 0103 physical sciences, instrument [Space vehicles], Calibration, Space vehicles: instruments, Astronomy and Astrophysics, Space and Planetary Science, Angular resolution, data analysis [Methods], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), QC, QB, Physics, 010308 nuclear & particles physics, business.industry, Instrument Data, Detector, Spectral density, Ranging, Astronomy and Astrophysic, data analysi [Methods], business, Astrophysics - Instrumentation and Methods for Astrophysics, Noise (radio), Methods: data analysi, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CSIC, Consejo Superior de Investigaciones Científicas; ERC, European Research Council; MINECO, Ministerio de Economía y Competitividad; MPG, Max-Planck-Gesellschaft; NASA, National Aeronautics and Space Administration; etc., Ade, P.A.R., Aghanim, N., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A.J., Barreiro, R.B., Bartolo, N., Basak, S., Battaglia, P., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Bucher, M., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Castex, G., Catalano, A., Chamballu, A., Christensen, P.R., Colombi, S., Colombo, L.P.L., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Fergusson, J., Finelli, F., Forni, O., Frailis, M., Franceschet, C., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K.M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F.K., Hanson, D., Harrison, D.L., Henrot-Versillé, S., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Juvela, M., Keihänen, E., Keskitalo, R., Kiiveri, K., Kisner, T.S., Knoche, J., Krachmalnicoff, N., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leahy, J.P., Leonardi, R., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lubin, P.M., Macías-Pérez, J.F., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P.G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., McGehee, P., Meinhold, P.R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Murphy, J.A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Nørgaard-Nielsen, H.U., Novikov, D., Novikov, I., Oppermann, N., Paci, F., Pagano, L., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T.J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Pierpaoli, E., Pietrobon, D., Pointecouteau, E., Polenta, G., Pratt, G.W., Prézeau, G., Prunet, S., Puget, J.-L., Rachen, J.P., Rebolo, R., Reinecke, M., Remazeilles, M., Renzi, A., Rocha, G., Romelli, E., Rosset, C., Rossetti, M., Roudier, G., Rubiño-Martín, J.A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Scott, D., Seiffert, M.D., Shellard, E.P.S., Spencer, L.D., Stolyarov, V., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vassallo, T., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Watson, R., Wehus, I.K., Wilkinson, A., Yvon, D., Zacchei, A., Zonca, A.

Full Text
View/download PDF

196. Cosmic Microwave Background Fluctuations

Author

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

Subjects
Big Bang, Physics, Cosmic neutrino background, General Relativity and Quantum Cosmology, Age of the universe, Ultimate fate of the universe, Cosmic microwave background, Astronomy, Lambda-CDM model, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Baryon acoustic oscillations, Physical cosmology
Abstract

Several experiments have recently detected very low contrast, sub-horizon scale structures in the Cosmic Microwave Background (CMB). In the current cosmological model, these structures result from acoustic oscillations of the primeval plasma at recombination ( $z \sim 1100$ ). In the framework of the Hot Big Bang theory with the inflation hypothesis, the statistical properties of the image of the CMB allow us to measure most of the cosmological parameters.

197. Maps of the millimetre sky from the BOOMERanG experiment

Author

A. Boscaleri, J. J. Bock, Andrew H. Jaffe, Carlo R. Contaldi, J. Borrill, Max Tegmark, Amedeo Balbi, F. Piacentini, Philip Daniel Mauskopf, B. P. Crill, Simon Prunet, T. E. Montroy, Andrew E. Lange, Nicola Vittorio, S. Ricciardi, Dmitry Pogosyan, Theodore Kisner, Enzo Pascale, G. Polenta, P. Natoli, A. Iacoangeli, G. De Troia, M. Giacometti, V. V. Hristov, Alessandro Melchiorri, G. de Gasperis, K. Ganga, J. E. Ruhl, J. R. Bond, W. C. Jones, A. de-Oliveria Costa, P. Cabella, G. Romeo, Federico Nati, C. J. MacTavish, P. de Bernardis, Peter Mason, Calvin B. Netterfield, Peter A. R. Ade, Silvia Masi, and E. Hivon

Subjects
Physics, Linear polarization, media_common.quotation_subject, Horizon, Cosmic microwave background, Astrophysics (astro-ph), BOOMERanG experiment, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CMB cold spot, Amplitude, Settore FIS/05 - Astronomia e Astrofisica, Sky, Millimeter, Astrophysics::Galaxy Astrophysics, media_common
Abstract

In the 1998-99 flight, BOOMERanG has produced maps of $\sim 4 %$ of the sky at high Galactic latitudes, at frequencies of 90, 150, 240 and 410 GHz, with resolution $\simgt 10'$. The faint structure of the Cosmic Microwave Background at horizon and sub-horizon scales is evident in these maps. These maps compare well to the maps recently obtained at lower frequencies by the WMAP experiment. Here we compare the amplitude and morphology of the structures observed in the two sets of maps. We also outline the polarization sensitive version of BOOMERanG, which was flown early this year to measure the linear polarization of the microwave sky at 150, 240 and 350 GHz., Comment: IAU Symposium 216: Maps of the Cosmos. Sydney 14-17 July 2003 - ASP Conference Series

198. CMB Polarization B-mode Delensing with SPTpol and Herschel.

Author

A. Manzotti, K. T. Story, W. L. K. Wu, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, L. E. Bleem, J. J. Bock, J. E. Carlstrom, C. L. Chang, H. C. Chiang, H-M. Cho, R. Citron, A. Conley, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, and S. Dodelson

Subjects
COSMIC background radiation, POLARIZATION (Nuclear physics), ANISOTROPY, GRAVITATIONAL waves, NULL hypothesis
Abstract

We present a demonstration of delensing the observed cosmic microwave background (CMB) B-mode polarization anisotropy. This process of reducing the gravitational-lensing-generated B-mode component will become increasingly important for improving searches for the B modes produced by primordial gravitational waves. In this work, we delens B-mode maps constructed from multi-frequency SPTpol observations of a 90 deg2 patch of sky by subtracting a B-mode template constructed from two inputs: SPTpol E-mode maps and a lensing potential map estimated from the Herschel 500 μm map of the cosmic infrared background. We find that our delensing procedure reduces the measured B-mode power spectrum by % in the multipole range this is shown to be consistent with expectations from simulations and to be robust against systematics. The null hypothesis of no delensing is rejected at . Furthermore, we build and use a suite of realistic simulations to study the general properties of the delensing process and find that the delensing efficiency achieved in this work is limited primarily by the noise in the lensing potential map. We demonstrate the importance of including realistic experimental non-idealities in the delensing forecasts used to inform instrument and survey-strategy planning of upcoming lower-noise experiments, such as CMB-S4. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

199. A New Limit on CMB Circular Polarization from SPIDER.

Author

J. M. Nagy, P. A. R. Ade, M. Amiri, S. J. Benton, A. S. Bergman, R. Bihary, J. J. Bock, J. R. Bond, S. A. Bryan, H. C. Chiang, C. R. Contaldi, O. Doré, A. J. Duivenvoorden, H. K. Eriksen, M. Farhang, J. P. Filippini, L. M. Fissel, A. A. Fraisse, K. Freese, and M. Galloway

Subjects
COSMIC background radiation, CIRCULAR polarization, LINEAR polarization, ELECTRONIC modulators, ASTROPHYSICAL radiation
Abstract

We present a new upper limit on cosmic microwave background (CMB) circular polarization from the 2015 flight of Spider, a balloon-borne telescope designed to search for B-mode linear polarization from cosmic inflation. Although the level of circular polarization in the CMB is predicted to be very small, experimental limits provide a valuable test of the underlying models. By exploiting the nonzero circular-to-linear polarization coupling of the half-wave plate polarization modulators, data from Spider's 2015 Antarctic flight provide a constraint on Stokes V at 95 and 150 GHz in the range . No other limits exist over this full range of angular scales, and Spider improves on the previous limit by several orders of magnitude, providing 95% C.L. constraints on ranging from 141 to 255 μK2 at 150 GHz for a thermal CMB spectrum. As linear CMB polarization experiments become increasingly sensitive, the techniques described in this paper can be applied to obtain even stronger constraints on circular polarization. [ABSTRACT FROM AUTHOR]

Published
2017
Full Text
View/download PDF

200. Bicep2/KECK ARRAY VIII: MEASUREMENT OF GRAVITATIONAL LENSING FROM LARGE-SCALE B-MODE POLARIZATION.

Author

P. A. R. Ade, Z. Ahmed, R. W. Aikin, K. D. Alexander, D. Barkats, S. J. Benton, C. A. Bischoff, J. J. Bock, R. Bowens-Rubin, J. A. Brevik, I. Buder, E. Bullock, V. Buza, J. Connors, B. P. Crill, L. Duband, C. Dvorkin, J. P. Filippini, S. Fliescher, and J. Grayson

Subjects
POLARIZATION microscopy, GRAVITATIONAL lenses, COSMIC background radiation, METAPHYSICAL cosmology, APODIZATION
Abstract

We present measurements of polarization lensing using the 150 GHz maps, which include all data taken by the BICEP2 and KeckArray Cosmic Microwave Background polarization experiments up to and including the 2014 observing season (BK14). Despite their modest angular resolution (), the excellent sensitivity (∼3μK-arcmin) of these maps makes it possible to directly reconstruct the lensing potential using only information at larger angular scales (). From the auto-spectrum of the reconstructed potential, we measure an amplitude of the spectrum to be (Planck ΛCDM prediction corresponds to ) and reject the no-lensing hypothesis at , which is the highest significance achieved to date using an EB lensing estimator. Taking the cross-spectrum of the reconstructed potential with the Planck 2015 lensing map yields . These direct measurements of are consistent with the ΛCDM cosmology and with that derived from the previously reported BK14 B-mode auto-spectrum (). We perform a series of null tests and consistency checks to show that these results are robust against systematics and are insensitive to analysis choices. These results unambiguously demonstrate that the B modes previously reported by BICEP/Keck at intermediate angular scales () are dominated by gravitational lensing. The good agreement between the lensing amplitudes obtained from the lensing reconstruction and B-mode spectrum starts to place constraints on any alternative cosmological sources of B modes at these angular scales. [ABSTRACT FROM AUTHOR]

Published
2016
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results