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38 results on '"Hanany S"'

1. SOFIA Far-infrared Imaging Polarimetry of M82 and NGC 253: Exploring the Supergalactic Wind

Author: Jones, T., Dowell, C., Lopez Rodriguez, E., Zweibel, E., Berthoud, M., Chuss, D., Goldsmith, P., Hamilton, R., Hanany, S., Harper, D., Lazarian, A., Looney, L., Michail, J., Morris, M., Novak, G., Santos, F., Sheth, K., Stacey, G., Staguhn, J., Stephens, I., Tassis, K., Trinh, C., Volpert, C., Werner, M., Wollack, E., and Team, H.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present far-infrared polarimetry observations of M82 at 53 and 154 Œºm and NGC 253 at 89 Œºm, which were taken with High-resolution Airborne Wideband Camera-plus (HAWC+) in polarimetry mode on the Stratospheric Observatory for Infrared Astronomy. The polarization of M82 at 53 Œºm clearly shows a magnetic field geometry perpendicular to the disk in the hot dust emission. For M82 the polarization at 154 Œºm shows a combination of field geometry perpendicular to the disk in the nuclear region, but closer to parallel to the disk away from the nucleus. The fractional polarization at 53 Œºm (154 Œºm) ranges from 7% (3%) off nucleus to 0.5% (0.3%) near the nucleus. A simple interpretation of the observations of M82 invokes a massive polar outflow, dragging the field along, from a region ~700 pc in diameter that has entrained some of the gas and dust, creating a vertical field geometry seen mostly in the hotter (53 Œºm) dust emission. This outflow sits within a larger disk with a more typical planar geometry that more strongly contributes to the cooler (154 Œºm) dust emission. For NGC 253, the polarization at 89 Œºm is dominated by a planar geometry in the tilted disk, with weak indication of a vertical geometry above and below the plane from the nucleus. The polarization observations of NGC 253 at 53 Œºm were of a insufficient signal-to-noise ratio for a detailed analysis.
Published: 2019

2. The Far-infrared Polarization Spectrum of œÅ Ophiuchi A from HAWC+/SOFIA Observations

Author: Santos, F., Chuss, D., Dowell, C., Houde, M., Looney, L., Lopez Rodriguez, E., Novak, G., Ward-Thompson, D., Berthoud, M., Dale, D., Guerra, J., Hamilton, R., Hanany, S., Harper, D., Henning, T., Jones, T., Lazarian, A., Michail, J., Morris, M., Staguhn, J., Stephens, I., Tassis, K., Trinh, C., Van Camp, E., Volpert, C., and Wollack, E.
Subjects: Astrophysics::Galaxy Astrophysics
Abstract: We report on polarimetric maps made with HAWC+/SOFIA toward œÅ Oph A, the densest portion of the œÅ Ophiuchi molecular complex. We employed HAWC+ bands C (89 Œºm) and D (154 Œºm). The slope of the polarization spectrum was investigated by defining the quantity {{ \mathcal R }}{DC}={p}D/{p}C, where p C and p D represent polarization degrees in bands C and D, respectively. We find a clear correlation between {{ \mathcal R }}{DC} and the molecular hydrogen column density across the cloud. A positive slope ({{ \mathcal R }}{DC} > 1) dominates the lower-density and well-illuminated portions of the cloud, which are heated by the high-mass star Oph S1, whereas a transition to a negative slope ({{ \mathcal R }}{DC} < 1) is observed toward the denser and less evenly illuminated cloud core. We interpret the trends as due to a combination of (1) warm grains at the cloud outskirts, which are efficiently aligned by the abundant exposure to radiation from Oph S1, as proposed in the radiative torques theory; and (2) cold grains deep in the cloud core, which are poorly aligned owing to shielding from external radiation. To assess this interpretation, we developed a very simple toy model using a spherically symmetric cloud core based on Herschel data and verified that the predicted variation of {{ \mathcal R }}{DC} is consistent with the observations. This result introduces a new method that can be used to probe the grain alignment efficiency in molecular clouds, based on the analysis of trends in the far-infrared polarization spectrum.
Published: 2019

3. HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1

Author: Chuss, D., Andersson, B., Bally, J., Dotson, J., Dowell, C., Guerra, J., Harper, D., Houde, M., Jones, T., Lazarian, A., Lopez Rodriguez, E., Michail, J., Morris, M., Novak, G., Siah, J., Staguhn, J., Vaillancourt, J., Volpert, C., Werner, M., Wollack, E., Benford, D., Berthoud, M., Cox, E., Crutcher, R., Dale, D., Fissel, L., Goldsmith, P., Hamilton, R., Hanany, S., Henning, T., Looney, L., Moseley, S., Santos, F., Stephens, I., Tassis, K., Trinh, C., Van Camp, E., Ward-Thompson, D., and Team, H.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report new polarimetric and photometric maps of the massive star- forming region OMC-1 using the HAWC+ instrument on the Stratospheric Observatory for Infrared Astronomy. We present continuum polarimetric and photometric measurements of this region at 53, 89, 154, and 214 Œºm at angular resolutions of 5‚Ä≥, 8‚Ä≥, 14‚Ä≥, and 19‚Ä≥ for the four bands, respectively. The photometric maps enable the computation of improved spectral energy distributions for the region. We find that at the longer wavelengths, the inferred magnetic field configuration matches the ‚Äúhourglass‚Äù configuration seen in previous studies, indicating magnetically regulated star formation. The field morphology differs at the shorter wavelengths. The magnetic field inferred at these wavelengths traces the bipolar structure of the explosive Becklin- Neugebauer/Kleinman-Low outflow emerging from OMC-1 behind the Orion Nebula. Using statistical methods to estimate the field strength in the region, we find that the explosion dominates the magnetic field near the center of the feature. Farther out, the magnetic field is close to energetic equilibrium with the ejecta and may be providing confinement to the explosion. The correlation between polarization fraction and the local polarization angle dispersion indicates that the depolarization as a function of unpolarized intensity is a result of intrinsic field geometry as opposed to decreases in grain alignment efficiency in denser regions.
Published: 2019

4. Exploring cosmic origins with CORE: Extragalactic sources in cosmic microwave background maps

Author: De Zotti, G, González-Nuevo, J, Lopez-Caniego, M, Negrello, M, Greenslade, J, Hernández-Monteagudo, C, Delabrouille, J, Cai, Z-Y, Bonato, M, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, AJ, Banerji, R, Bartlett, JG, Bartolo, N, Basak, S, Bersanelli, M, Biesiada, M, Bilicki, M, Bonaldi, A, Bonavera, L, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Calvo, M, Carvalho, CS, Castellano, MG, Challinor, A, Chluba, J, Clements, DL, Clesse, S, Colafrancesco, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Diego, JM, Di Valentino, E, Errard, J, Feeney, SM, Fernández-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, RT, Gerbino, M, Grandis, S, Hagstotz, S, Hanany, S, Handley, W, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lasenby, A, Lattanzi, M, Le Brun, A, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-Gonzalez, E, Martins, CJAP, Masi, S, Massardi, M, Matarrese, S, McCarthy, D, Melchiorri, A, Melin, J-B, Molinari, D, Monfardini, A, Natoli, P, Notari, A, Paiella, A, Paoletti, D, Partridge, RB, Patanchon, G, Piat, M, Pisano, G, Polastri, L, and Polenta, G
Subjects: astro-ph.GA, galaxy evolution, Molecular, Astrophysics::Cosmology and Extragalactic Astrophysics, Atomic, Nuclear & Particles Physics, Particle and Plasma Physics, active galactic nuclei, CMBR experiments, astro-ph.CO, Nuclear, galaxy surveys, Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences
Abstract: We discuss the potential of a next generation space-borne Cosmic Microwave Background (CMB) experiment for studies of extragalactic sources. Our analysis has particular bearing on the definition of the future space project, CORE, that has been submitted in response to ESA's call for a Medium-size mission opportunity as the successor of the Planck satellite. Even though the effective telescope size will be somewhat smaller than that of Planck, CORE will have a considerably better angular resolution at its highest frequencies, since, in contrast with Planck, it will be diffraction limited at all frequencies. The improved resolution implies a considerable decrease of the source confusion, i.e. substantially fainter detection limits. In particular, CORE will detect thousands of strongly lensed high-z galaxies distributed over the full sky. The extreme brightness of these galaxies will make it possible to study them, via follow-up observations, in extraordinary detail. Also, the CORE resolution matches the typical sizes of high-z galaxy proto-clusters much better than the Planck resolution, resulting in a much higher detection efficiency; these objects will be caught in an evolutionary phase beyond the reach of surveys in other wavebands. Furthermore, CORE will provide unique information on the evolution of the star formation in virialized groups and clusters of galaxies up to the highest possible redshifts. Finally, thanks to its very high sensitivity, CORE will detect the polarized emission of thousands of radio sources and, for the first time, of dusty galaxies, at mm and sub-mm wavelengths, respectively.
Published: 2018

5. Exploring cosmic origins with CORE: Mitigation of systematic effects

Author: Natoli, P, Ashdown, M, Banerji, R, Borrill, J, Buzzelli, A, de Gasperis, G, Delabrouille, J, Hivon, E, Molinari, D, Patanchon, G, Polastri, L, Tomasi, M, Bouchet, FR, Henrot-Versillé, S, Hoang, DT, Keskitalo, R, Kiiveri, K, Kisner, T, Lindholm, V, McCarthy, D, Piacentini, F, Perdereau, O, Polenta, G, Tristram, M, Achucarro, A, Ade, P, Allison, R, Baccigalupi, C, Ballardini, M, Banday, AJ, Bartlett, J, Bartolo, N, Basak, S, Baumann, D, Bersanelli, M, Bonaldi, A, Bonato, M, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Cai, Z-Y, Calvo, M, Carvalho, C-S, Castellano, MG, Challinor, A, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, De Zotti, G, Di Valentino, E, Diego, J-M, Errard, J, Feeney, S, Fernandez-Cobos, R, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Gruppuso, A, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hervías-Caimapo, C, Hills, M, Keihänen, E, Kitching, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Lesgourgues, J, Lewis, A, Liguori, M, López-Caniego, M, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-González, E, Martins, CJAP, Masi, S, Matarrese, S, Melchiorri, A, Melin, J-B, Migliaccio, M, Monfardini, A, Negrello, M, Notari, A, Pagano, L, and Paiella, A
Subjects: CMBR polarisation, Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Bioengineering, ComputerApplications_COMPUTERSINOTHERSYSTEMS, Nuclear & Particles Physics, Atomic, Particle and Plasma Physics, CMBR experiments, astro-ph.CO, Nuclear, gravitational waves and CMBR polarization, Astronomical and Space Sciences, astro-ph.IM
Abstract: We present an analysis of the main systematic effects that could impact the measurement of CMB polarization with the proposed CORE space mission. We employ timeline-to-map simulations to verify that the CORE instrumental set-up and scanning strategy allow us to measure sky polarization to a level of accuracy adequate to the mission science goals. We also show how the CORE observations can be processed to mitigate the level of contamination by potentially worrying systematics, including intensity-to-polarization leakage due to bandpass mismatch, asymmetric main beams, pointing errors and correlated noise. We use analysis techniques that are well validated on data from current missions such as Planck to demonstrate how the residual contamination of the measurements by these effects can be brought to a level low enough not to hamper the scientific capability of the mission, nor significantly increase the overall error budget. We also present a prototype of the CORE photometric calibration pipeline, based on that used for Planck, and discuss its robustness to systematics, showing how CORE can achieve its calibration requirements. While a fine-grained assessment of the impact of systematics requires a level of knowledge of the system that can only be achieved in a future study phase, the analysis presented here strongly suggests that the main areas of concern for the CORE mission can be addressed using existing knowledge, techniques and algorithms.
Published: 2018

6. Exploring cosmic origins with CORE: Survey requirements and mission design

Author: Delabrouille, J, de Bernardis, P, Bouchet, FR, Achúcarro, A, Ade, PAR, Allison, R, Arroja, F, Artal, E, Ashdown, M, Baccigalupi, C, Ballardini, M, Banday, AJ, Banerji, R, Barbosa, D, Bartlett, J, Bartolo, N, Basak, S, Baselmans, JJA, Basu, K, Battistelli, ES, Battye, R, Baumann, D, Benoít, A, Bersanelli, M, Bideaud, A, Biesiada, M, Bilicki, M, Bonaldi, A, Bonato, M, Borrill, J, Boulanger, F, Brinckmann, T, Brown, ML, Bucher, M, Burigana, C, Buzzelli, A, Cabass, G, Cai, Z-Y, Calvo, M, Caputo, A, Carvalho, C-S, Casas, FJ, Castellano, G, Catalano, A, Challinor, A, Charles, I, Chluba, J, Clements, DL, Clesse, S, Colafrancesco, S, Colantoni, I, Contreras, D, Coppolecchia, A, Crook, M, D'Alessandro, G, D'Amico, G, da Silva, A, de Avillez, M, de Gasperis, G, De Petris, M, de Zotti, G, Danese, L, Désert, F-X, Desjacques, V, Di Valentino, E, Dickinson, C, Diego, JM, Doyle, S, Durrer, R, Dvorkin, C, Eriksen, HK, Errard, J, Feeney, S, Fernández-Cobos, R, Finelli, F, Forastieri, F, Franceschet, C, Fuskeland, U, Galli, S, Génova-Santos, RT, Gerbino, M, Giusarma, E, Gomez, A, González-Nuevo, J, Grandis, S, Greenslade, J, Goupy, J, Hagstotz, S, Hanany, S, Handley, W, Henrot-Versillé, S, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hindmarsh, M, Hivon, E, Hoang, DT, Hooper, DC, Hu, B, and Keihänen, E
Subjects: CMBR polarisation, gravitational lensing, Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Astrophysics::Cosmology and Extragalactic Astrophysics, Nuclear & Particles Physics, Atomic, Particle and Plasma Physics, Affordable and Clean Energy, CMBR experiments, astro-ph.CO, physics of the early universe, Nuclear, Astronomical and Space Sciences, astro-ph.IM
Abstract: Future observations of cosmic microwave background (CMB) polarisation have the potential to answer some of the most fundamental questions of modern physics and cosmology, including: what physical process gave birth to the Universe we see today? What are the dark matter and dark energy that seem to constitute 95% of the energy density of the Universe? Do we need extensions to the standard model of particle physics and fundamental interactions? Is the ΛCDM cosmological scenario correct, or are we missing an essential piece of the puzzle? In this paper, we list the requirements for a future CMB polarisation survey addressing these scientific objectives, and discuss the design drivers of the COREmfive space mission proposed to ESA in answer to the "M5" call for a medium-sized mission. The rationale and options, and the methodologies used to assess the mission's performance, are of interest to other future CMB mission design studies. COREmfive has 19 frequency channels, distributed over a broad frequency range, spanning the 60-600 GHz interval, to control astrophysical foreground emission. The angular resolution ranges from 2′ to 18′, and the aggregate CMB sensitivity is about 2 μKċarcmin. The observations are made with a single integrated focal-plane instrument, consisting of an array of 2100 cryogenically-cooled, linearly-polarised detectors at the focus of a 1.2-m aperture cross-Dragone telescope. The mission is designed to minimise all sources of systematic effects, which must be controlled so that no more than 10-4 of the intensity leaks into polarisation maps, and no more than about 1% of E-type polarisation leaks into B-type modes. COREmfive observes the sky from a large Lissajous orbit around the Sun-Earth L2 point on an orbit that offers stable observing conditions and avoids contamination from sidelobe pick-up of stray radiation originating from the Sun, Earth, and Moon. The entire sky is observed repeatedly during four years of continuous scanning, with a combination of three rotations of the spacecraft over different timescales. With about 50% of the sky covered every few days, this scan strategy provides the mitigation of systematic effects and the internal redundancy that are needed to convincingly extract the primordial B-mode signal on large angular scales, and check with adequate sensitivity the consistency of the observations in several independent data subsets. COREmfive is designed as a "near-ultimate" CMB polarisation mission which, for optimal complementarity with ground-based observations, will perform the observations that are known to be essential to CMB polarisation science and cannot be obtained by any other means than a dedicated space mission. It will provide well-characterised, highly-redundant multi-frequency observations of polarisation at all the scales where foreground emission and cosmic variance dominate the final uncertainty for obtaining precision CMB science, as well as 2′ angular resolution maps of high-frequency foreground emission in the 300-600 GHz frequency range, essential for complementarity with future ground-based observations with large telescopes that can observe the CMB with the same beamsize.
Published: 2018

7. Exploring cosmic origins with CORE: Gravitational lensing of the CMB

Author: Challinor, A, Allison, R, Carron, J, Errard, J, Feeney, S, Kitching, T, Lesgourgues, J, Lewis, A, Zubeldia, I, Achucarro, A, Ade, P, Ashdown, M, Ballardini, M, Banday, AJ, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Baumann, D, Bersanelli, M, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, ZY, Calvo, M, Carvalho, CS, Castellano, G, Chluba, J, Clesse, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, De Bernardis, P, De Gasperis, G, Zotti, GD, Delabrouille, J, Valentino, ED, Diego, JM, Fernandez-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Genova-Santos, R, Gerbino, M, González-Nuevo, J, Grandis, S, Greenslade, J, Hagstotz, S, Hanany, S, Handley, W, Hernandez-Monteagudo, C, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kunz, M, Kurki-Suonio, H, Lamagna, L, Lasenby, A, Lattanzi, M, Liguori, M, Lindholm, V, López-Caniego, M, Luzzi, G, Maffei, B, Martinez-González, E, Martins, CJAP, Masi, S, Matarrese, S, McCarthy, D, Melchiorri, A, Melin, JB, Molinari, D, Monfardini, A, Natoli, P, Negrello, M, Notari, A, Paiella, A, Paoletti, D, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rubino-Martin, JA, Salvati, L, Challinor, Anthony [0000-0003-3479-7823], Handley, William [0000-0002-5866-0445], Lasenby, Anthony [0000-0002-8208-6332], and Apollo - University of Cambridge Repository
Subjects: CMBR polarisation, Particle and Plasma Physics, gravitational lensing, astro-ph.CO, Molecular, Nuclear, Astrophysics::Cosmology and Extragalactic Astrophysics, neutrino masses from cosmology, inflation, Nuclear & Particles Physics, Atomic, Astronomical and Space Sciences
Abstract: Lensing of the cosmic microwave background (CMB) is now a well-developed probe of the clustering of the large-scale mass distribution over a broad range of redshifts. By exploiting the non-Gaussian imprints of lensing in the polarization of the CMB, the CORE mission will allow production of a clean map of the lensing deflections over nearly the full-sky. The number of high-S/N modes in this map will exceed current CMB lensing maps by a factor of 40, and the measurement will be sample-variance limited on all scales where linear theory is valid. Here, we summarise this mission product and discuss the science that will follow from its power spectrum and the cross-correlation with other clustering data. For example, the summed mass of neutrinos will be determined to an accuracy of 17 meV combining CORE lensing and CMB two-point information with contemporaneous measurements of the baryon acoustic oscillation feature in the clustering of galaxies, three times smaller than the minimum total mass allowed by neutrino oscillation measurements. Lensing has applications across many other science goals of CORE, including the search for B-mode polarization from primordial gravitational waves. Here, lens-induced B-modes will dominate over instrument noise, limiting constraints on the power spectrum amplitude of primordial gravitational waves. With lensing reconstructed by CORE, one can "delens" the observed polarization internally, reducing the lensing B-mode power by 60 %. This can be improved to 70 % by combining lensing and measurements of the cosmic infrared background from CORE, leading to an improvement of a factor of 2.5 in the error on the amplitude of primordial gravitational waves compared to no delensing (in the null hypothesis of no primordial B-modes). Lensing measurements from CORE will allow calibration of the halo masses of the tens of thousands of galaxy clusters that it will find, with constraints dominated by the clean polarization-based estimators. The 19 frequency channels proposed for CORE will allow accurate removal of Galactic emission from CMB maps. We present initial findings that show that residual Galactic foreground contamination will not be a significant source of bias for lensing power spectrum measurements with CORE.
Published: 2018

8. Exploring cosmic origins with CORE: The instrument

Author: de Bernardis, P, Ade, PAR, Baselmans, JJA, Battistelli, ES, Benoit, A, Bersanelli, M, Bideaud, A, Calvo, M, Casas, FJ, Castellano, MG, Catalano, A, Charles, I, Colantoni, I, Columbro, F, Coppolecchia, A, Crook, M, D'Alessandro, G, De Petris, M, Delabrouille, J, Doyle, S, Franceschet, C, Gomez, A, Goupy, J, Hanany, S, Hills, M, Lamagna, L, Macias-Perez, J, Maffei, B, Martin, S, Martinez-Gonzalez, E, Masi, S, McCarthy, D, Mennella, A, Monfardini, A, Noviello, F, Paiella, A, Piacentini, F, Piat, M, Pisano, G, Signorelli, G, Tan, CY, Tartari, A, Trappe, N, Triqueneaux, S, Tucker, C, Vermeulen, G, Young, K, Zannoni, M, Achúcarro, A, Allison, R, Artall, E, Ashdown, M, Ballardini, M, Banday, AJ, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, ZY, Carvalho, CS, Challinor, A, Chluba, J, Clesse, S, De Gasperis, G, De Zotti, G, Di Valentino, E, Diego, JM, Errard, J, Feeney, S, Fernandez-Cobos, R, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Hagstotz, S, Greenslade, J, Handley, W, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lasenby, A, Lattanzi, M, Lesgourgues, J, and Lewis, A
Subjects: CMBR polarisation, Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Astrophysics::Cosmology and Extragalactic Astrophysics, Nuclear & Particles Physics, Atomic, Particle and Plasma Physics, CMBR experiments, astro-ph.CO, Nuclear, CMBR detectors, inflation, physics.ins-det, Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences, astro-ph.IM
Abstract: We describe a space-borne, multi-band, multi-beam polarimeter aiming at a precise and accurate measurement of the polarization of the Cosmic Microwave Background. The instrument is optimized to be compatible with the strict budget requirements of a medium-size space mission within the Cosmic Vision Programme of the European Space Agency. The instrument has no moving parts, and uses arrays of diffraction-limited Kinetic Inductance Detectors to cover the frequency range from 60 GHz to 600 GHz in 19 wide bands, in the focal plane of a 1.2 m aperture telescope cooled at 40 K, allowing for an accurate extraction of the CMB signal from polarized foreground emission. The projected CMB polarization survey sensitivity of this instrument, after foregrounds removal, is 1.7 μKċarcmin. The design is robust enough to allow, if needed, a downscoped version of the instrument covering the 100 GHz to 600 GHz range with a 0.8 m aperture telescope cooled at 85 K, with a projected CMB polarization survey sensitivity of 3.2 μKċarcmin.
Published: 2018

9. Exploring Cosmic Origins with CORE: Extragalactic sources in Cosmic Microwave Background maps

Author: Zotti, G. De, González-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernández-Monteagudo, C., Delabrouille, J., Cai, Z. -Y., Bonato, M., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartlett, J. G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clements, D. L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., De Gasperis, G., Diego, J. M., Valentino, E. Di, Errard, J., Feeney, S. M., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R. T., Gerbino, M., Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A. Le, Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Massardi, M., Matarrese, S., Mccarthy, D., Melchiorri, A., Melin, J. -B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R. B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B. F., Rubiño-Martín, J. -A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Väliviita, J., De Weygaert, R. Van, Tent, B. Van, Vennin, V., Vielva, P., Vittorio, N., Young, K., Zannoni, M., D'Alessandro, Giuseppe, AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -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 ), 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 ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Institut Lagrange de Paris, Sorbonne Universités, Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Département de Physique des Particules (ex SPP) ( DPP ), 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 d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), CORE, 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)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-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), Cryogénie (NEEL - Cryo), 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 Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), 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), 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), 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, Hélium : du fondamental aux applications (NEEL - HELFA), Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Zotti, G, González-Nuevo, J, Lopez-Caniego, M, Negrello, M, Greenslade, J, Hernández-Monteagudo, C, Delabrouille, J, Cai, Z, Bonato, M, Achúcarro, A, Ade, P, Allison, R, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bersanelli, M, Biesiada, M, Bilicki, M, Bonaldi, A, Bonavera, L, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Calvo, M, Carvalho, C, Castellano, M, Challinor, A, Chluba, J, Clements, D, Clesse, S, Colafrancesco, S, Colantoni, I, Coppolecchia, A, Crook, M, D'Alessandro, G, de Bernardis, P, de Gasperis, G, Diego, J, Valentino, E, Errard, J, Feeney, S, Fernández-Cobos, R, Ferraro, S, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, Grandis, S, Hagstotz, S, Hanany, S, Handley, W, Hervias-Caimapo, C, Hills, M, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamagna, L, Lasenby, A, Lattanzi, M, Brun, A, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Maffei, B, Mandolesi, N, Martinez-Gonzalez, E, Martins, C, Masi, S, Massardi, M, Matarrese, S, Mccarthy, D, Melchiorri, A, Melin, J, Molinari, D, Monfardini, A, Natoli, P, Notari, A, Paiella, A, Paoletti, D, Partridge, R, Patanchon, G, Piat, M, Pisano, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rossi, G, Roukema, B, Rubiño-Martín, J, Salvati, L, Scott, D, Serjeant, S, Tartari, A, Toffolatti, L, Tomasi, M, Trappe, N, Triqueneaux, S, Trombetti, T, Tucci, M, Tucker, C, Väliviita, J, de Weygaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Young, K, Zannoni, M, Astronomy, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Département de Physique des Particules (ex SPP) (DPP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), 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]), Sorbonne Université (SU), 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Science and Technology Facilities Council (STFC), Science and Technology Facilities Council, 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), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Helsinki Institute of Physics, and Department of Physics
Subjects: LENSED GALAXIES, Brightness, POLARIZATION, active galactic nuclei, CMBR experiments, galaxy evolution, galaxy surveys, POINT SOURCES, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Cosmic microwave background, galaxy evolution, Astrophysics, CMB, 01 natural sciences, Physics, Particles & Fields, law.invention, law, CMBR experiments, galaxy surveys, 010303 astronomy & astrophysics, QC, QB, Physics, COSMIC cancer database, Nuclear & Particles Physics, PLANCK, COMPACT SOURCE CATALOG, ALL-SKY SURVEY, Physical Sciences, astro-ph.CO, symbols, GALAXY FORMATION, CMBR experiment, Astrophysics - Cosmology and Nongalactic Astrophysics, RADIO-SOURCES, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxy survey, astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, NO, Telescope, symbols.namesake, FIS/05 - ASTRONOMIA E ASTROFISICA, 0202 Atomic, Molecular, Nuclear, Particle And Plasma Physics, Settore FIS/05 - Astronomia e Astrofisica, active galactic nuclei, Astronomy and Astrophysics, 0103 physical sciences, Planck, Astrophysics::Galaxy Astrophysics, HERSCHEL, Science & Technology, 010308 nuclear & particles physics, Star formation, HERSCHEL-ATLAS, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, EVOLUTION, 0201 Astronomical And Space Sciences, LUMINOSITY FUNCTION, Astrophysics of Galaxies (astro-ph.GA), SKY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Work supported in part by ASI/INAF agreement n. 2014-024-R.1 and by PRIN–INAF 2014 “Probing the AGN/galaxy co-evolution through ultra-deep and ultra-high resolution radio surveys”. JGN acknowledges financial support from the Spanish MINECO for a “Ramon y Cajal” fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). CH-M acknowledges the financial support of the Spanish MINECO through I+D project AYA-2015-66211-C2-2-P. MB is supported by the Netherlands Organization for Scientific Research, NWO, through grant number 614.001.451, and by the Polish National Science Centre under contract UMO-2012/07/D/ST9/02785. CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). GR acknowledges support from the National Research Foundation of Korea (NRF) through NRF-SGER 2014055950 funded by the Korean Ministry of Education, Science and Technology (MoEST), and from the faculty research fund of Sejong University in 2016., Zotti, G.D., González-Nuevo, J., Lopez-Caniego, M., Negrello, M., Greenslade, J., Hernández-Monteagudo, C., Delabrouille, J., Cai, Z.-Y., Bonato, M., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A.J., Banerji, R., Bartlett, J.G., Bartolo, N., Basak, S., Bersanelli, M., Biesiada, M., Bilicki, M., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Calvo, M., Carvalho, C.S., Castellano, M.G., Challinor, A., Chluba, J., Clements, D.L., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D'Alessandro, G., De Bernardis, P., De Gasperis, G., Diego, J.M., Valentino, E.D., Errard, J., Feeney, S.M., Fernández-Cobos, R., Ferraro, S., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R.T., Gerbino, M., Grandis, S., Hagstotz, S., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamagna, L., Lasenby, A., Lattanzi, M., Brun, A.L., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C.J.A.P., Masi, S., Massardi, M., Matarrese, S., McCarthy, D., Melchiorri, A., Melin, J.-B., Molinari, D., Monfardini, A., Natoli, P., Notari, A., Paiella, A., Paoletti, D., Partridge, R.B., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Roukema, B.F., Rubiño-Martín, J.-A., Salvati, L., Scott, D., Serjeant, S., Tartari, A., Toffolatti, L., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Tucci, M., Tucker, C., Väliviita, J., De Weygaert, R.V., Tent, B.V., Vennin, V., Vielva, P., Vittorio, N., Young, K., Zannoni, M.
Published: 2016
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10. Maps of the CMB temperature anisotropy: From the time-ordered data to the maximum-likelihood solution

Author: Stompor, R, Balbi, A, Borrill, J, Ferreira, P, Hanany, S, Jaffel, A, Lee, A, Oh, S, Rabii, B, Richards, P, Smoot, G, Winant, C, and Wu, JHP
Published: 2016
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11. CMB Analysis of Boomerang and Maxima and the Cosmic Parameters {Omega_tot,Omega_b h^2,Omega_cdm h^2,Omega_Lambda,n_s}

Author: Bond, JR, Ade, P, Balbi, A, Bock, J, Borrill, J, Boscaleri, A, Coble, K, Crill, B, Bernardis, PD, Farese, P, Ferreira, P, Ganga, K, Giacometti, M, Hanany, S, Hivon, E, Hristov, V, Iacoangeli, A, Jaffe, A, Lange, A, Lee, A, Martinis, L, Masi, S, Mauskopf, P, Melchiorri, A, Montroy, T, Netterfield, B, Oh, S, Pascale, E, Piacentini, F, Pogosyan, D, Prunet, S, Rabii, B, Rao, S, Richards, P, Romeo, G, Ruhl, J, Scaramuzzi, F, Sforna, D, Sigurdson, K, Smoot, G, Stompor, R, Winant, C, and Wu, P
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We show how estimates of parameters characterizing inflation-based theories of structure formation localized over the past year when large scale structure (LSS) information from galaxy and cluster surveys was combined with the rapidly developing cosmic microwave background (CMB) data, especially from the recent Boomerang and Maxima balloon experiments. All current CMB data plus a relatively weak prior probability on the Hubble constant, age and LSS points to little mean curvature (Omega_{tot} = 1.08\pm 0.06) and nearly scale invariant initial fluctuations (n_s =1.03\pm 0.08), both predictions of (non-baroque) inflation theory. We emphasize the role that degeneracy among parameters in the L_{pk} = 212\pm 7 position of the (first acoustic) peak plays in defining the $\Omega_{tot}$ range upon marginalization over other variables. Though the CDM density is in the expected range (\Omega_{cdm}h^2=0.17\pm 0.02), the baryon density Omega_bh^2=0.030\pm 0.005 is somewhat above the independent 0.019\pm 0.002 nucleosynthesis estimate. CMB+LSS gives independent evidence for dark energy (Omega_\Lambda=0.66\pm 0.06) at the same level as from supernova (SN1) observations, with a phenomenological quintessence equation of state limited by SN1+CMB+LSS to w_Q
Published: 2016

12. MAXIMA-1: A Measurement of the Cosmic Microwave Background Anisotropy on angular scales of 10 arcminutes to 5 degrees

Author: Hanany, S, Ade, P, Balbi, A, Bock, J, Borrill, J, Boscaleri, A, Bernardis, PD, Ferreira, PG, Hristov, VV, Jaffe, AH, Lange, AE, Lee, AT, Mauskopf, PD, Netterfield, CB, Oh, S, Pascale, E, Rabii, B, Richards, PL, Smoot, GF, Stompor, R, Winant, CD, and Wu, JHP
Subjects: Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
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., Reflects version accepted for publication in Ap J Letters
Published: 2016
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13. The Quintessential CMB, Past and Future

Author: Bond, JR, Pogosyan, D, Prunet, S, Sigurdson, K, collaboration, TM, Ade, P, Balbi, A, Bock, J, Borrill, J, Boscaleri, A, Coble, K, Crill, B, Bernardis, P, Farese, P, Ferreira, P, Ganga, K, Giacometti, M, Hanany, S, Hivon, E, Hristov, V, Iacoangeli, A, Jaffe, A, Lange, A, Lee, A, and Martinis, L
Abstract: The past, present and future of cosmic microwave background (CMB) anisotropy research is discussed, with emphasis on the Boomerang and Maxima balloon experiments. These data are combined with large scale structure (LSS) information and high redshift supernova (SN1) observations to explore the inflation-based cosmic structure formation paradigm. Here we primarily focus on a simplified inflation parameter set, {omega_b,omega_{cdm},Omega_{tot}, Omega_Q,w_Q, n_s,tau_C, sigma_8}. After marginalizing over the other cosmic and experimental variables, we find the current CMB+LSS+SN1 data gives Omega_{tot}=1.04\pm 0.05, consistent with (non-baroque) inflation theory. Restricting to Omega_{tot}=1, we find a nearly scale invariant spectrum, n_s =1.03 \pm 0.07. The CDM density, omega_{cdm}=0.17\pm 0.02, is in the expected range, but the baryon density, omega_b=0.030\pm 0.004, is slightly larger than the current nucleosynthesis estimate. Substantial dark energy is inferred, Omega_Q\approx 0.68\pm 0.05, and CMB+LSS Omega_Q values are compatible with the independent SN1 estimates. The dark energy equation of state, parameterized by a quintessence-field pressure-to-density ratio w_Q, is not well determined by CMB+LSS (w_Q
Published: 2016
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14. The Cosmic Background Radiation circa nu2K

Author: Bond, J. R., Pogosyan, D., Prunet, S., collaboration, the MaxiBoom, Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Coble, K., Crill, B., de Bernardis, P., Farese, P., Ferreira, P., Ganga, K., Giacometti, M., Hanany, S., Hivon, E., Hristov, V., Iacoangeli, A., Jaffe, A., Lange, A., Lee, A., Martinis, L., Masi, S., Mauskopf, P., Melchiorri, A., Montroy, T., Netterfield, B., Oh, S., Pascale, E., Piacentini, F., Rabii, B., Rao, S., Richards, P., Romeo, G., Ruhl, J., Scaramuzzi, F., Sforna, D., Smoot, G., Stompor, R., Winant, C., and Wu, P.
Subjects: Inflation (cosmology), Physics, Nuclear and High Energy Physics, Structure formation, Astrophysics (astro-ph), Cosmic microwave background, Cosmic background radiation, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Omega, Atomic and Molecular Physics, and Optics, Redshift, Big Bang nucleosynthesis, High Energy Physics::Experiment, Neutrino
Abstract: We describe the implications of cosmic microwave background (CMB) observations and galaxy and cluster surveys of large scale structure (LSS) for theories of cosmic structure formation, especially emphasizing the recent Boomerang and Maxima CMB balloon experiments. The inflation-based cosmic structure formation paradigm we have been operating with for two decades has never been in better shape. Here we primarily focus on a simplified inflation parameter set, {omega_b,omega_{cdm},Omega_{tot}, Omega_\Lambda,n_s,\tau_C, \sigma_8}. Combining all of the current CMB+LSS data points to the remarkable conclusion that the local Hubble patch we can access has little mean curvature (Omega_{tot}=1.08\pm 0.06) and the initial fluctuations were nearly scale invariant (n_s=1.03\pm 0.08), both predictions of (non-baroque) inflation theory. The baryon density is found to be slightly larger than that preferred by independent Big Bang Nucleosynthesis estimates (omega_b=0.030\pm 0.005 cf. 0.019\pm 0.002). The CDM density is in the expected range (omega_{cdm}=0.17 \pm 0.02). Even stranger is the CMB+LSS evidence that the density of the universe is dominated by unclustered energy akin to the cosmological constant (Omega_\Lambda=0.66\pm 0.06), at the same level as that inferred from high redshift supernova observations. We also sketch the CMB+LSS implications for massive neutrinos., Comment: 7 pages, 4 figs., in Proc. Neutrino 2000 (Elsevier), CITA-2000-63
Published: 2016
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15. Cosmology from Maxima-1, Boomerang and COBE/DMR CMB Observations

Author: Jaffe, A, Ade, P, Balbi, A, Bock, J, Bond, JR, Borrill, J, Boscaleri, A, Coble, K, Crill, B, Bernardis, P, Farese, P, Ferreira, P, Ganga, K, Giacometti, M, Hanany, S, Hivon, E, Hristov, V, Iacoangeli, A, Lange, A, Lee, A, Martinis, L, Masi, S, Mauskopf, P, Melchiorri, A, and Montroy, T
Abstract: Recent results from BOOMERANG-98 and MAXIMA-1, taken together with COBE-DMR, provide consistent and high signal-to-noise measurements of the CMB power spectrum at spherical harmonic multipole bands over $2
Published: 2016

16. MAXIMA: Millimeter-wave anisotropy experiment imaging array

Author: Winant, C, Abroe, M, Ade, P, Balbi, A, Barbosa, D, Bock, J, Borrill, J, Boscaleri, A, Collins, J, de Bernardis, P, Ferreira, P, Hanany, S, Hristov, V, Jaffe, A, Johnson, B, Lange, A, Lee, A, Mauskopf, P, Netterfield, C, Oh, S, Pascale, E, Rabii, B, Richards, P, Stompor, R, and Smoot, G
Published: 2016

17. The Origin of the Universe as Revealed Through the Polarization of the Cosmic Microwave Background

Author: Dodelson, S, Easther, R, Hanany, S, McAllister, L, Meyer, S, Page, L, Ade, P, Amblard, A, Ashoorioon, A, Baccigalupi, C, Balbi, A, Bartlett, J, Bartolo, N, Baumann, D, Beltran, M, Benford, D, Birkinshaw, M, Bock, J, Bond, D, Borrill, J, Bouchet, F, Bridges, M, Bunn, E, Calabrese, E, and Cantalupo, C
Abstract: Modern cosmology has sharpened questions posed for millennia about the origin of our cosmic habitat. The age-old questions have been transformed into two pressing issues primed for attack in the coming decade: How did the Universe begin? and What physical laws govern the Universe at the highest energies? The clearest window onto these questions is the pattern of polarization in the Cosmic Microwave Background (CMB), which is uniquely sensitive to primordial gravity waves. A detection of the special pattern produced by gravity waves would be not only an unprecedented discovery, but also a direct probe of physics at the earliest observable instants of our Universe. Experiments which map CMB polarization over the coming decade will lead us on our first steps towards answering these age-old questions.
Published: 2016

18. Neutrino physics from the cosmic microwave background and large scale structure

Author: Abazajian, KN, Arnold, K, Austermann, J, Benson, BA, Bischoff, C, Bock, J, Bond, JR, Borrill, J, Calabrese, E, Carlstrom, JE, Carvalho, CS, Chang, CL, Chiang, HC, Church, S, Cooray, A, Crawford, TM, Dawson, KS, Das, S, Devlin, MJ, Dobbs, M, Dodelson, S, Doré, O, Dunkley, J, Errard, J, Fraisse, A, Gallicchio, J, Halverson, NW, Hanany, S, Hildebrandt, SR, Hincks, A, Hlozek, R, Holder, G, Holzapfel, WL, Honscheid, K, Hu, W, Hubmayr, J, Irwin, K, Jones, WC, Kamionkowski, M, Keating, B, Keisler, R, Knox, L, Komatsu, E, Kovac, J, Kuo, C-L, Lawrence, C, Lee, AT, Leitch, E, Linder, E, Lubin, P, McMahon, J, Miller, A, Newburgh, L, Niemack, MD, Nguyen, H, Nguyen, HT, Page, L, Pryke, C, Reichardt, CL, Ruhl, JE, Sehgal, N, Seljak, U, Sievers, J, Silverstein, E, Slosar, A, Smith, KM, Spergel, D, Staggs, ST, Stark, A, Stompor, R, Vieregg, AG, Wang, G, Watson, S, Wollack, EJ, Wu, WLK, Yoon, KW, Zahn, O, and Topical Conveners: K.N. Abazajian, JE Carlstrom
Subjects: Particle and Plasma Physics, astro-ph.CO, Molecular, hep-ph, Nuclear, Large scale structure, Neutrinos, Atomic, Nuclear & Particles Physics, Astronomical and Space Sciences, Cosmology, Cosmic microwave background
Abstract: This is a report on the status and prospects of the quantification of neutrino properties through the cosmological neutrino background for the Cosmic Frontier of the Division of Particles and Fields Community Summer Study long-term planning exercise. Experiments planned and underway are prepared to study the cosmological neutrino background in detail via its influence on distance-redshift relations and the growth of structure. The program for the next decade described in this document, including upcoming spectroscopic galaxy surveys eBOSS and DESI and a new Stage-IV CMB polarization experiment CMB-S4, will achieve σ(σmν) = 16 meV and σ(Neff) = 0.020. Such a mass measurement will produce a high significance detection of non-zero σmν, whose lower bound derived from atmospheric and solar neutrino oscillation data is about 58 meV. If neutrinos have a minimal normal mass hierarchy, this measurement will definitively rule out the inverted neutrino mass hierarchy, shedding light on one of the most puzzling aspects of the Standard Model of particle physics - the origin of mass. This precise a measurement of Neff will allow for high sensitivity to any light and dark degrees of freedom produced in the big bang and a precision test of the standard cosmological model prediction that Neff = 3.046.
Published: 2015

19. Inflation physics from the cosmic microwave background and large scale structure

Author: Abazajian, KN, Arnold, K, Austermann, J, Benson, BA, Bischoff, C, Bock, J, Bond, JR, Borrill, J, Buder, I, Burke, DL, Calabrese, E, Carlstrom, JE, Carvalho, CS, Chang, CL, Chiang, HC, Church, S, Cooray, A, Crawford, TM, Crill, BP, Dawson, KS, Das, S, Devlin, MJ, Dobbs, M, Dodelson, S, Doré, O, Dunkley, J, Feng, JL, Fraisse, A, Gallicchio, J, Giddings, SB, Green, D, Halverson, NW, Hanany, S, Hanson, D, Hildebrandt, SR, Hincks, A, Hlozek, R, Holder, G, Holzapfel, WL, Honscheid, K, Horowitz, G, Hu, W, Hubmayr, J, Irwin, K, Jackson, M, Jones, WC, Kallosh, R, Kamionkowski, M, Keating, B, Keisler, R, Kinney, W, Knox, L, Komatsu, E, Kovac, J, Kuo, C-L, Kusaka, A, Lawrence, C, Lee, AT, Leitch, E, Linde, A, Linder, E, Lubin, P, Maldacena, J, Martinec, E, McMahon, J, Miller, A, Mukhanov, V, Newburgh, L, Niemack, MD, Nguyen, H, Nguyen, HT, Page, L, Pryke, C, Reichardt, CL, Ruhl, JE, Sehgal, N, Seljak, U, Senatore, L, Sievers, J, Silverstein, E, Slosar, A, Smith, KM, Spergel, D, Staggs, ST, Stark, A, Stompor, R, Vieregg, AG, Wang, G, Watson, S, Wollack, EJ, Wu, WLK, Yoon, KW, Zahn, O, Zaldarriaga, M, and Carlstrom, AT Lee Topical Conveners JE
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Astrophysics::Cosmology and Extragalactic Astrophysics, Inflation, Early Universe, Atomic, Nuclear & Particles Physics, Cosmology, Particle and Plasma Physics, Cosmic Microwave Background, astro-ph.CO, Nuclear, Large-scale Structure, Astronomical and Space Sciences
Abstract: Fluctuations in the intensity and polarization of the cosmic microwave background (CMB) and the large-scale distribution of matter in the universe each contain clues about the nature of the earliest moments of time. The next generation of CMB and large-scale structure (LSS) experiments are poised to test the leading paradigm for these earliest moments-the theory of cosmic inflation-and to detect the imprints of the inflationary epoch, thereby dramatically increasing our understanding of fundamental physics and the early universe. A future CMB experiment with sufficient angular resolution and frequency coverage that surveys at least 1% of the sky to a depth of 1 uK-arcmin can deliver a constraint on the tensor-to-scalar ratio that will either result in a 5σ measurement of the energy scale of inflation or rule out all large-field inflation models, even in the presence of foregrounds and the gravitational lensing B-mode signal. LSS experiments, particularly spectroscopic surveys such as the Dark Energy Spectroscopic Instrument, will complement the CMB effort by improving current constraints on running of the spectral index by up to a factor of four, improving constraints on curvature by a factor of ten, and providing non-Gaussianity constraints that are competitive with the current CMB bounds.
Published: 2015

20. CMB Telescopes and Optical Systems

Author: Hanany, S., Niemack, M., and Page, L.
Subjects: Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The cosmic microwave background radiation (CMB) is now firmly established as a fundamental and essential probe of the geometry, constituents, and birth of the Universe. The CMB is a potent observable because it can be measured with precision and accuracy. Just as importantly, theoretical models of the Universe can predict the characteristics of the CMB to high accuracy, and those predictions can be directly compared to observations. There are multiple aspects associated with making a precise measurement. In this review, we focus on optical components for the instrumentation used to measure the CMB polarization and temperature anisotropy. We begin with an overview of general considerations for CMB observations and discuss common concepts used in the community. We next consider a variety of alternatives available for a designer of a CMB telescope. Our discussion is guided by the ground and balloon-based instruments that have been implemented over the years. In the same vein, we compare the arc-minute resolution Atacama Cosmology Telescope (ACT) and the South Pole Telescope (SPT). CMB interferometers are presented briefly. We conclude with a comparison of the four CMB satellites, Relikt, COBE, WMAP, and Planck, to demonstrate a remarkable evolution in design, sensitivity, resolution, and complexity over the past thirty years., Comment: To appear in: Planets, Stars and Stellar Systems (PSSS), Volume 1: Telescopes and Instrumentation
Published: 2012
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21. The Origin of the Universe as Revealed Through the Polarization of the Cosmic Microwave Background

Author: Dodelson, S., Easther, R., Hanany, S., McAllister, L., Meyer, S., Page, L., Ade, P., Amblard, A., Ashoorioon, A., Baccigalupi, C., Balbi, A., Bartlett, J., Bartolo, N., Baumann, D., Beltran, M., Benford, D., Birkinshaw, M., Bock, J., Bond, D., Borrill, J., Bouchet, F., Bridges, M., Bunn, E., Calabrese, E., Cantalupo, C., Caramete, A., Carbone, C., Carroll, S., Chatterjee, S., Chen, X., Church, S., Chuss, D., Contaldi, C., Cooray, A., Creminelli, P., Das, S., De Bernardis, F., de Bernardis, P., Delabrouille, J., Desert, F. -X., Devlin, M., Dickinson, C., Dicker, S., DiPirro, M., Dobbs, M., Dore, O., Dotson, J., Dunkley, J., Dvorkin, C., Eriksen, H. K., Falvella, M. Cristina, Finley, D., Finkbeiner, D., Fixsen, D., Flauger, R., Fosalba, P., Fowler, J., Galli, S., Gates, E., Gear, W., Giraud-Heraud, Y., Gorski, K., Greene, B., and Gruppuso, A.
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Modern cosmology has sharpened questions posed for millennia about the origin of our cosmic habitat. The age-old questions have been transformed into two pressing issues primed for attack in the coming decade: How did the Universe begin? and What physical laws govern the Universe at the highest energies? The clearest window onto these questions is the pattern of polarization in the Cosmic Microwave Background (CMB), which is uniquely sensitive to primordial gravity waves. A detection of the special pattern produced by gravity waves would be not only an unprecedented discovery, but also a direct probe of physics at the earliest observable instants of our Universe. Experiments which map CMB polarization over the coming decade will lead us on our first steps towards answering these age-old questions., Comment: Science White Paper submitted to the US Astro2010 Decadal Survey. Full list of 212 author available at http://cmbpol.uchicago.edu
Published: 2009
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22. Cosmological implications of the MAXIMA-I high resolution Cosmic Microwave Background anisotropy measurement

Author: Stompor, R., Abroe, M., Ade, P., Balbi, A., Barbosa, D., Bock, J., Borrill, J., Boscaleri, A., DE BERNARDIS, Paolo, Ferreira, P. G., Hanany, S., Hristov, V., Jaffe, A. H., Lee, A. T., Pascale, Enzo, Rabii, B., Richards, P. L., Smoot, G. F., Winant, C. D., and J. H. P., Wu
Subjects: High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: We discuss the cosmological implications of the new constraints on the power spectrum of the Cosmic Microwave Background Anisotropy derived from a new high resolution analysis of the MAXIMA-1 measurement (Lee et al. 2001). The power spectrum shows excess power at $\ell \sim 860$ over the average level of power at $411 \le\ell \le 785.$ This excess is statistically significant on the 95% confidence level. Such a feature is consistent with the presence of a third acoustic peak, which is a generic prediction of inflation-based models. The height and the position of the excess power match the predictions of a family of inflationary models with cosmological parameters that are fixed to fit the CMB data previously provided by BOOMERANG-LDB and MAXIMA-1 experiments (e.g., Jaffe et al.2001). Our results, therefore, lend support for inflationary models and more generally for the dominance of coherent perturbations in the structure formation of the Universe. At the same time, they seem to disfavor a large variety of the non-standard (but still inflation-based) models that have been proposed to improve the quality of fits to the CMB data and consistency with other cosmological observables. Within standard inflationary models, our results combined with the COBE-DMR data give best fit values and 95% confidence limits for the baryon density, $\Omega_b h^2\simeq 0.033{\pm 0.013}$, and the total density, $\Omega=0.9{+0.18\atop -0.16}$. The primordial spectrum slope ($n_s$) and the optical depth to the last scattering surface ($\tau_c$) are found to be degenerate and to obey the relation $n_s \simeq 0.46 \tau_c + (0.99 \pm 0.14)$, for $\tau_c \le 0.5$ (all 95% c.l.)., Comment: Replaced to match a published version
Published: 2001

23. The Quintessential CMB, Past and Future

Author: Bond, JR, Pogosyan, D, Prunet, S, Sigurdson, K, collaboration, TM, Ade, P, Balbi, A, Bock, J, Borrill, J, Boscaleri, A, Coble, K, Crill, B, Bernardis, PD, Farese, P, Ferreira, P, Ganga, K, Giacometti, M, Hanany, S, Hivon, E, Hristov, V, Iacoangeli, A, Jaffe, A, Lange, A, Lee, A, Martinis, L, Masi, S, Mauskopf, P, Melchiorri, A, Montroy, T, Netterfield, B, Oh, S, Pascale, E, Piacentini, F, Rabii, B, Rao, S, Richards, P, Romeo, G, Ruhl, J, Scaramuzzi, F, Sforna, D, Smoot, G, Stompor, R, Winant, C, and Wu, P
Subjects: Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: The past, present and future of cosmic microwave background (CMB) anisotropy research is discussed, with emphasis on the Boomerang and Maxima balloon experiments. These data are combined with large scale structure (LSS) information and high redshift supernova (SN1) observations to explore the inflation-based cosmic structure formation paradigm. Here we primarily focus on a simplified inflation parameter set, {omega_b,omega_{cdm},Omega_{tot}, Omega_Q,w_Q, n_s,tau_C, sigma_8}. After marginalizing over the other cosmic and experimental variables, we find the current CMB+LSS+SN1 data gives Omega_{tot}=1.04\pm 0.05, consistent with (non-baroque) inflation theory. Restricting to Omega_{tot}=1, we find a nearly scale invariant spectrum, n_s =1.03 \pm 0.07. The CDM density, omega_{cdm}=0.17\pm 0.02, is in the expected range, but the baryon density, omega_b=0.030\pm 0.004, is slightly larger than the current nucleosynthesis estimate. Substantial dark energy is inferred, Omega_Q\approx 0.68\pm 0.05, and CMB+LSS Omega_Q values are compatible with the independent SN1 estimates. The dark energy equation of state, parameterized by a quintessence-field pressure-to-density ratio w_Q, is not well determined by CMB+LSS (w_Q
Published: 2000

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

Author: Bond, J. R., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Coble, K., Crill, B., de Bernardis, P., Farese, P., Ferreira, P., Ganga, K., Giacometti, M., Hanany, S., Hivon, E., Hristov, V., Iacoangeli, A., Jaffe, A., Lange, A., Lee, A., Martinis, L., Masi, S., Mauskopf, P., Melchiorri, A., Montroy, T., Netterfield, B., Oh, S., Pascale, E., Piacentini, F., Pogosyan, D., Prunet, S., Rabii, B., Rao, S., Richards, P., Romeo, G., Ruhl, J., Scaramuzzi, F., Sforna, D., Sigurdson, K., Smoot, G., Stompor, R., Winant, C., and Wu, P.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We show how estimates of parameters characterizing inflation-based theories of structure formation localized over the past year when large scale structure (LSS) information from galaxy and cluster surveys was combined with the rapidly developing cosmic microwave background (CMB) data, especially from the recent Boomerang and Maxima balloon experiments. All current CMB data plus a relatively weak prior probability on the Hubble constant, age and LSS points to little mean curvature (Omega_{tot} = 1.08\pm 0.06) and nearly scale invariant initial fluctuations (n_s =1.03\pm 0.08), both predictions of (non-baroque) inflation theory. We emphasize the role that degeneracy among parameters in the L_{pk} = 212\pm 7 position of the (first acoustic) peak plays in defining the $��_{tot}$ range upon marginalization over other variables. Though the CDM density is in the expected range (��_{cdm}h^2=0.17\pm 0.02), the baryon density Omega_bh^2=0.030\pm 0.005 is somewhat above the independent 0.019\pm 0.002 nucleosynthesis estimate. CMB+LSS gives independent evidence for dark energy (Omega_��=0.66\pm 0.06) at the same level as from supernova (SN1) observations, with a phenomenological quintessence equation of state limited by SN1+CMB+LSS to w_Q, 11 pages, 3 figs., in Proc. IAU Symposium 201 (PASP), CITA-2000-65
Published: 2000
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25. WOMBAT & FORECAST: Making Realistic Maps of the Microwave Sky

Author: Jaffe, A. H., Gawiser, E., Finkbeiner, D., Baker, J. C., Balbi, A., Davis, M., Hanany, S., Holzapfel, W., Krumholz, M., Leonidas Moustakas, Robinson, J., Scannapieco, E., Smoot, G. F., and Silk, J.
Subjects: Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: The Wavelength-Oriented Microwave Background Analysis Team (WOMBAT) is constructing microwave maps which will be more realistic than previous simulations. Our foreground models represent a considerable improvement: where spatial templates are available for a given foreground, we predict the flux and spectral index of that component at each place on the sky and estimate uncertainties. We will produce maps containing simulated CMB anisotropy combined with expected foregrounds. The simulated maps will be provided to the community as the WOMBAT Challenge, so such maps can be analyzed to extract cosmological parameters by scientists who are unaware of their input values. This will test the efficacy of foreground subtraction, power spectrum analysis, and parameter estimation techniques and help identify the areas most in need of progress. These maps are also part of the FORECAST project, which allows web-based access to the known foreground maps for the planning of CMB missions., Comment: 10 pages, color figures, WOMBAT Challenge simulations now available at: http://astro.berkeley.edu/wombat/ . Invited review in "Microwave Foregrounds", eds. A. de Oliveira-Costa & M. Tegmark (ASP, San Francisco, 1999)
Published: 1999
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26. The Maxima and Boomerang Experiments

Author: Hanany, S., Collaboration, MAXIMA, and Collaboration, BOOMERANG
Subjects: Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract: MAXIMA and BOOMERanG are balloon borne experiments designed to map the cosmic microwave background anisotropy power spectrum from l=10 to l=900 with high resolution. Here we describe the program of observations, the experiments, their capabilities, and their expected performance., Comment: 3 pages, Latex, sprocl.sty file attached, to appear in the Proceedings of the 18th Texas Symposium on Relativistic Astrophysics
Published: 1997
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27. The MAX and MAXIMA Experiments

Author: Hanany, S., collaboration, MAX, and collaboration, MAXIMA
Subjects: Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics
Abstract: We summarize the performance of the MAX experiment during its 5 years of operation and present a compilation of the results to date. We describe MAXIMA, a balloon borne experiment employing an array of detectors in the focal plane, that will provide sensitive measurements of the power spectrum between l~60 and l~650., Comment: 6 pages, 1 fig., Latex and additional .sty files attached. To appear in the Proceedings of The XXXI Moriond Meeting "Microwave Background Anisotropies"
Published: 1996
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28. Evidence for a Flat Universe from the North American Flight of BOOMERANG

Author: Crill, B. P., Ade, P. A. R., Paolo de Bernardis, Bock, J. J., Borrill, J., Boscaleri, A., Gasperis, G., Troia, Grazia, Farese, P., Ferreira, P. G., Ganga, K., Giacometti, M., Hanany, S., Hivon, E. F., Hristov, V. V., Iacoangeli, Armando, Jaffe, A. H., Lange, A. E., Lee, A. T., Silvia Masi, Mauskopf, P. D., Melchiorri, Francesco, Alessandro Melchiorri, Miglio, L., Montroy, T., Netterfield, C. B., Enzo Pascale, Francesco Piacentini, Richards, L., Romeo, G., Ruhl, J. E., Scannapieco, E., Scaramuzzi, F., Stompor, R., and Vittorio, N.

29. Design of the detectors for EBEX, a balloon-borne cosmic microwave background polarimeter

Author: Westbrook, Benjamin, Aboobaker, A. M., Peter Ade, Aubin, F., Baccigalupi, C., Bandura, K., Bao, C., Borrill, J., Chapman, D., Didier, J., Dobbs, M., Gold, B., Grain, J., Grainger, W., Hanany, S., Helson, K., Hillbrand, S. N., Hilton, G., Hubmayr, H., Irwin, K., Johnson, B., Jaffe, A., Jones, T. J., Kisner, T., Klein, J., Korotkov, A., Leach, S., Lee, A. T., Levinson, L., Limon, M., Macdermid, K., Miller, A. D., Milligan, M., Pascale, E., Raach, K., Reichborn-Kjennerud, B., Sagiv, I., Smecher, G., Stompor, R., Tristram, M., Tucker, G. S., and Zilic, K.

30. The E and B EXperiment EBEX

Author: Helson, Kyle, Aboobaker, A. M., Peter Ade, Aubin, F., Baccigalupi, C., Bandura, K., Bao, C., Borrill, J., Chandra, B., Chapman, D., Didier, J., Dobbs, M., Gold, B., Grain, J., Grainger, W., Hanany, S., Hillbrand, S. N., Hilton, G., Hubmayr, H., Irwin, K., Johnson, B., Jaffe, A., Jones, T. J., Kisner, T., Klein, J., Korotkov, A., Leach, S., Lee, A. T., Levinson, L., Limon, M., Macdermid, K., Miller, A. D., Milligan, M., Pascale, E., Qiu, C., Raach, K., Reichborn-Kjennerud, B., Reintsema, C., Sagiv, I., Smecher, G., Stompor, R., Tristram, M., Tucker, G. S., Westbrook, B., Yadav, A. P., Zaldarriaga, M., and Zilic, K.

31. Prototype demonstration of the broadband anti-reflection coating on sapphire using a sub-wavelength structure

Author: Matsumura, T., Takaku, R., Hanany, S., Imada, H., Ishino, H., Katayama, N., Kobayashi, Y., Komatsu, K., Kuniaki Konishi, Kuwata-Gonokami, M., Nakamura, S., Sakurai, H., Sakurai, Y., Wen, Q., Young, K., and Yumoto, J.

32. The E and B EXperiment (EBEX); Progress and Status

Author: Sagiv, Ilan, Aboobaker, A. M., Ade, P., Aubin, F., Baccigalupi, C., Borrill, J., Chapman, D., Didier, J., Dobbs, M., Grainger, W., Hanany, S., Hilbrand, S., Hogen-Chin, C., Hubmayr, H., Johnson, B., Jaffe, A., Jones, T., Klein, J., Korotkov, A., Leach, S., Lee, A., Levinson, L., Michele Limon, Macaluso, J., Macdermid, K., Matsumura, T., Meng, X., Miller, A., Milligan, M., Pascale, E., Polsgrove, D., Ponthieu, N., Reichborn-Kjennerud, B., Renbarger, T., Stivoli, F., Stompor, R., Tran, H., Tucker, G., Vinokurov, J., Zaldarriaga, M., Zilic, K., Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), 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), APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Stompor, Radoslaw, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)
Subjects: [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We report on the status of EBEX, a NASA-funded balloon-borne polarimeter designed to measure the B-mode polarization of the cosmic microwave background radiation. The EBEX receiver is designed to set a 2σ upper limit on an inflationary tensor-to-scalar ratio of 0.02. This limit assumes a 14-day flight, a scan pattern covering 420 square degrees of the sky, and foreground subtraction to levels below detector noise. The instrument employs a 1.5 meter Gregorian-type telescope and 1440 bolometric transition edge sensor detectors distributed over two focal planes. Polarization is measured using a rotating achromatic half wave plate (AHWP) and a fixed polarizing grid. The AHWP is continuously rotated using a superconducting magnetic bearing. Sky signals will be observed in three bands centered at 150, 250 and 410 GHz, providing strong leverage against the polarized dust foreground. Integration of the gondola and the receiver will occur in fall 2008. A short-duration test flight employing 384 detectors in one focal plane is planned for 2009.

33. EBEX: A Balloon-Borne CMB Polarization Experiment

Author: Chapman, Daniel, Aboobaker, A. M., Peter Ade, Aubin, F., Baccigalupi, C., Bandura, K., Bao, C., Borrill, J., Didier, J., Dobbs, M., Gold, B., Grain, J., Grainger, W., Hanany, S., Helson, K., Hillbrand, S. N., Hilton, G., Hubmayr, H., Irwin, K., Johnson, B., Jaffe, A., Jones, T. J., Kisner, T., Klein, J., Korotkov, A., Leach, S., Lee, A. T., Levinson, L., Limon, M., Macdermid, K., Miller, A. D., Milligan, M., Pascale, E., Raach, K., Reichborn-Kjennerud, B., Sagiv, I., Smecher, G., Stompor, R., Tristram, M., Tucker, G. S., Westbrook, B., and Zilic, K.

34. MAXIMA-1: A measurement of the cosmic microwave background anisotropy on angular scales of 10′-5°

Author: Hanany, S., Ade, P., Balbi, A., Bock, J., Borrill, J., Boscaleri, A., Paolo de Bernardis, Ferreira, P. G., Hristov, V. V., Jaffe, A. H., Lange, A. E., Lee, A. T., Mauskopf, P. D., Netterfield, C. B., Oh, S., Pascale, E., Rabii, B., Richards, P. L., Smoot, G. F., Stompor, R., Winant, C. D., and Wu, J. H. P.

35. Exploring Cosmic Origins with CORE: Cluster Science

Author: Melin, J. -B, Bonaldi, A., Remazeilles, M., Hagstotz, S., Diego, J. M., Hernández-Monteagudo, C., Génova-Santos, R. T., Luzzi, G., Martins, C. J. A. P., Grandis, S., Mohr, J. J., Bartlett, J. G., Delabrouille, J., Ferraro, S., Tramonte, D., Rubiño-Martín, J. A., Macìas-Pérez, J. F., Achúcarro, A., Ade, P., Allison, R., Ashdown, M., Ballardini, M., Banday, A. J., Banerji, R., Bartolo, N., Basak, S., Baselmans, J., Basu, K., Battye, R. A., Baumann, D., Bersanelli, M., Bonato, M., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z. -Y, Calvo, M., Carvalho, C. S., Castellano, M. G., Challinor, A., Chluba, J., Clesse, S., Colafrancesco, S., Colantoni, I., Coppolecchia, A., Crook, M., D Alessandro, G., Bernardis, P., Gasperis, G., Petris, M., Zotti, G., Di Valentino, E., Errard, J., Feeney, S. M., Fernández-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Gerbino, M., González-Nuevo, J., Greenslade, J., Hanany, S., Handley, W., Hervias-Caimapo, C., Hills, M., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Le Brun, A. M. C., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Lopez-Caniego, M., Maffei, B., Martinez-Gonzalez, E., Masi, S., Mccarthy, D., Melchiorri, A., Molinari, D., Monfardini, A., Natoli, P., Negrello, M., Notari, A., Paiella, A., Paoletti, D., Patanchon, G., Piat, M., Pisano, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Roman, M., Salvati, L., Tartari, A., Tomasi, M., Trappe, N., Triqueneaux, S., Trombetti, T., Carole Tucker, Väliviita, J., Weygaert, R., Tent, B., Vennin, V., Vielva, P., Vittorio, N., Weller, J., Young, K., Zannoni, M., and Core, For The Collaboration

36. Exploring cosmic origins with CORE: mitigation of systematic effects

Author: Natoli, P., Ashdown, M., Banerji, R., Borrill, J., Buzzelli, A., Gasperis, G., Delabrouille, J., Eric Hivon, Molinari, D., Patanchon, G., Polastri, L., Tomasi, M., Bouchet, F. R., Henrot-Versillé, S., Hoang, D. T., Keskitalo, R., Kiiveri, K., Kisner, T., Lindholm, V., Mccarthy, D., Piacentini, F., Perdereau, O., Polenta, G., Tristram, M., Achucarro, A., Ade, P., Allison, R., Baccigalupi, C., Ballardini, M., Banday, A. J., Bartlett, J., Bartolo, N., Basak, S., Baselmans, J., Baumann, D., Bersanelli, M., Bonaldi, A., Bonato, M., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Cai, Z. -Y, Calvo, M., Carvalho, C. -S, Castellano, G., Challinor, A., Chluba, J., Clesse, S., Colantoni, I., Coppolecchia, A., Crook, M., D Alessandro, G., Bernardis, P., Zotti, G., Di Valentino, E., Diego, J. -M, Errard, J., Feeney, S., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Genova-Santos, R., Gerbino, M., Gonzalez-Nuevo, J., Grandis, S., Greenslade, J., Gruppuso, A., Hagstotz, S., Hanany, S., Handley, W., Hernandez-Monteagudo, C., Hervias-Caimapo, C., Hills, M., Keihänen, E., Kitching, T., Kunz, M., Kurki-Suonio, H., Lamagna, L., Lasenby, A., Lattanzi, M., Lesgourgues, J., Lewis, A., Liguori, M., López-Caniego, M., Luzzi, G., Maffei, B., Mandolesi, N., Martinez-Gonzalez, E., Martins, C. J. A. P., Masi, S., Melchiorri, A., Melin, J. -B, Migliaccio, M., Monfardini, A., Negrello, M., Notari, A., Pagano, L., Paiella, A., Paoletti, D., Piat, M., Pisano, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rossi, G., Rubino-Martin, J. -A, Salvati, L., Signorelli, G., Tartari, A., Tramonte, D., Trappe, N., Trombetti, T., Tucker, C., Valiviita, J., Weijgaert, R., Tent, B., Vennin, V., Vielva, P., Vittorio, N., Wallis, C., Young, K., Zannoni, M., and Core, For The Collaboration

37. 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

38. Exploring Cosmic Origins with CORE: The Instrument

Author: P. de Bernardis, P.A.R. Ade, J.J.A. Baselmans, E.S. Battistelli, A. Benoit, M. Bersanelli, A. Bideaud, M. Calvo, F.J. Casas, M.G. Castellano, A. Catalano, I. Charles, I. Colantoni, F. Columbro, A. Coppolecchia, M. Crook, G. D'Alessandro, M. De Petris, J. Delabrouille, S. Doyle, C. Franceschet, A. Gomez, J. Goupy, S. Hanany, M. Hills, L. Lamagna, J. Macias-Perez, B. Maffei, S. Martin, E. Martinez-Gonzalez, S. Masi, D. McCarthy, A. Mennella, A. Monfardini, F. Noviello, A. Paiella, F. Piacentini, M. Piat, G. Pisano, G. Signorelli, C.Y. Tan, A. Tartari, N. Trappe, S. Triqueneaux, C. Tucker, G. Vermeulen, K. Young, M. Zannoni, A. Achúcarro, R. Allison, E. Artall, M. Ashdown, M. Ballardini, A.J. Banday, R. Banerji, J. Bartlett, N. Bartolo, S. Basak, A. Bonaldi, M. Bonato, J. Borrill, F. Bouchet, F. Boulanger, T. Brinckmann, M. Bucher, C. Burigana, A. Buzzelli, Z.Y. Cai, C.S. Carvalho, A. Challinor, J. Chluba, S. Clesse, G. De Gasperis, G. De Zotti, E. Di Valentino, J.M. Diego, J. Errard, S. Feeney, R. Fernandez-Cobos, F. Finelli, F. Forastieri, S. Galli, R. Génova-Santos, M. Gerbino, J. González-Nuevo, S. Hagstotz, J. Greenslade, W. Handley, C. Hernández-Monteagudo, C. Hervias-Caimapo, E. Hivon, K. Kiiveri, T. Kisner, T. Kitching, M. Kunz, H. Kurki-Suonio, A. Lasenby, M. Lattanzi, J. Lesgourgues, A. Lewis, M. Liguori, V. Lindholm, G. Luzzi, C.J.A.P. Martins, S. Matarrese, A. Melchiorri, J.B. Melin, D. Molinari, P. Natoli, M. Negrello, A. Notari, D. Paoletti, G. Patanchon, L. Polastri, G. Polenta, A. Pollo, V. Poulin, M. Quartin, M. Remazeilles, M. Roman, J.A. Rubiño-Martín, L. Salvati, M. Tomasi, D. Tramonte, T. Trombetti, J. Väliviita, R. Van de Weyjgaert, B. van Tent, V. Vennin, P. Vielva, N. Vittorio, 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]), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-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), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Département de Physique des Particules (ex SPP) (DPP), 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 d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), CORE, Hélium : du fondamental aux applications (NEEL - HELFA), 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]), Cryogénie (NEEL - Cryo), 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]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale (LCCS), Service des Basses Températures (SBT ), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Fondamentale (CEA) (DRF (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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 National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Helsinki Institute of Physics, Department of Physics, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Sorbonne Universités, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), de Bernardis, P, Ade, P, Baselmans, J, Battistelli, E, Benoit, A, Bersanelli, M, Bideaud, A, Calvo, M, Casas, F, Castellano, M, Catalano, A, Charles, I, Colantoni, I, Columbro, F, Coppolecchia, A, Crook, M, D'Alessandro, G, Petris, M, Delabrouille, J, Doyle, S, Franceschet, C, Gomez, A, Goupy, J, Hanany, S, Hills, M, Lamagna, L, Macias-Perez, J, Maffei, B, Martin, S, Martinez-Gonzalez, E, Masi, S, Mccarthy, D, Mennella, A, Monfardini, A, Noviello, F, Paiella, A, Piacentini, F, Piat, M, Pisano, G, Signorelli, G, Tan, C, Tartari, A, Trappe, N, Triqueneaux, S, Tucker, C, Vermeulen, G, Young, K, Zannoni, M, Achúcarro, A, Allison, R, Artall, E, Ashdown, M, Ballardini, M, Banday, A, Banerji, R, Bartlett, J, Bartolo, N, Basak, S, Bonaldi, A, Bonato, M, Borrill, J, Bouchet, F, Boulanger, F, Brinckmann, T, Bucher, M, Burigana, C, Buzzelli, A, Cai, Z, Carvalho, C, Challinor, A, Chluba, J, Clesse, S, Gasperis, G, Zotti, G, Valentino, E, Diego, J, Errard, J, Feeney, S, Fernandez-Cobos, R, Finelli, F, Forastieri, F, Galli, S, Génova-Santos, R, Gerbino, M, González-Nuevo, J, Hagstotz, S, Greenslade, J, Handley, W, Hernández-Monteagudo, C, Hervias-Caimapo, C, Hivon, E, Kiiveri, K, Kisner, T, Kitching, T, Kunz, M, Kurki-Suonio, H, Lasenby, A, Lattanzi, M, Lesgourgues, J, Lewis, A, Liguori, M, Lindholm, V, Luzzi, G, Martins, C, Matarrese, S, Melchiorri, A, Melin, J, Molinari, D, Natoli, P, Negrello, M, Notari, A, Paoletti, D, Patanchon, G, Polastri, L, Polenta, G, Pollo, A, Poulin, V, Quartin, M, Remazeilles, M, Roman, M, Rubiño-Martín, J, Salvati, L, Tomasi, M, Tramonte, D, Trombetti, T, Väliviita, J, de Weyjgaert, R, Tent, B, Vennin, V, Vielva, P, Vittorio, N, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), 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 ) -Université Grenoble Alpes ( UGA ), Institut Nanosciences et Cryogénie ( INAC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ), AstroParticule et Cosmologie ( APC - UMR 7164 ), 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 Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), 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 ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -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 ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Département de Physique des Particules (ex SPP) ( DPP ), 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 d'Annecy-le-Vieux de Physique Théorique ( LAPTH ), Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -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: [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Kinetic inductance detectors, Cosmic microwave background, KINETIC INDUCTANCE DETECTORS, cosmic background radiation: polarization, DUAL-REFLECTOR ANTENNAS, 01 natural sciences, 7. Clean energy, BAND, law.invention, law, CMBR experiments, physics.ins-det, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, QC, QB, CALIBRATION, Physics, COSMIC cancer database, COMBINATIONS, Astrophysics::Instrumentation and Methods for Astrophysics, Instrumentation and Detectors (physics.ins-det), Polarization (waves), PLANCK, Cardinal point, experimental equipment, astro-ph.CO, CMBR detectors, CMBR experiment, astro-ph.IM, physics - instrumentation and detectors, Astrophysics - Instrumentation and Methods for Astrophysics, CMBR polarization, ination, Astronomy and Astrophysics, CMBR detector, Astrophysics - Cosmology and Nongalactic Astrophysics, PRESCRIBED GEOMETRIC PARAMETERS, CMBR polarisation, Cosmic Vision, Cosmology and Nongalactic Astrophysics (astro-ph.CO), kinetic, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, Telescope, FIS/05 - ASTRONOMIA E ASTROFISICA, Optics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, PRE-LAUNCH STATUS, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], inflation, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, beam: polarization, detector, 010308 nuclear & particles physics, business.industry, beam: width, Polarimeter, PERFORMANCE, WAVELENGTHS, 115 Astronomy, Space science, sensitivity, CMBR detectors, CMBR experiments, CMBR polarisation, inflation, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: PdB acknowledges support from University of Rome La Sapienza (project “Cosmologia di Precisione 2015”) and from the Italian Space Agency (Agreement 2016-019-H.0 “Kinetic Inductance Detectors for Space”). CJM is supported by an FCT Research Professorship, contract reference IF/00064/2012, funded by FCT/MCTES (Portugal) and POPH/FSE (EC). C.H.-M. acknowledges the financial support of the Spanish Ministry of Economy and Competitiveness via I+D project AYA-2015-66211-C2-2-P. GDZ acknowledges the financial support of ASI/INAF agreement n. 2014-024-R.1. J.G.N. acknowledges financial support from the Spanish MINECO for a “Ramon y Cajal” fellowship (RYC-2013-13256) and the I+D 2015 project AYA2015-65887-P (MINECO/FEDER). F.J.C., E.M.-G. and P.V. acknowledge support from the Spanish Ministerio de Econom´ıa y Competitividad project ESP2015-70646- C2-1-R co-financed with EU FEDER funds., De Bernardis, P., Ade, P.A.R., Baselmans, J.J.A., Battistelli, E.S., Benoit, A., Bersanelli, M., Bideaud, A., Calvo, M., Casas, F.J., Castellano, M.G., Catalano, A., Charles, I., Colantoni, I., Columbro, F., Coppolecchia, A., Crook, M., D'Alessandro, G., Petris, M.D., Delabrouille, J., Doyle, S., Franceschet, C., Gomez, A., Goupy, J., Hanany, S., Hills, M., Lamagna, L., Macias-Perez, J., Maffei, B., Martin, S., Martinez-Gonzalez, E., Masi, S., McCarthy, D., Mennella, A., Monfardini, A., Noviello, F., Paiella, A., Piacentini, F., Piat, M., Pisano, G., Signorelli, G., Tan, C.Y., Tartari, A., Trappe, N., Triqueneaux, S., Tucker, C., Vermeulen, G., Young, K., Zannoni, M., Achúcarro, A., Allison, R., Artall, E., Ashdown, M., Ballardini, M., Banday, A.J., Banerji, R., Bartlett, J., Bartolo, N., Basak, S., Bonaldi, A., Bonato, M., Borrill, J., Bouchet, F., Boulanger, F., Brinckmann, T., Bucher, M., Burigana, C., Buzzelli, A., Cai, Z.Y., Carvalho, C.S., Challinor, A., Chluba, J., Clesse, S., Gasperis, G.D., Zotti, G.D., Valentino, E.D., Diego, J.M., Errard, J., Feeney, S., Fernandez-Cobos, R., Finelli, F., Forastieri, F., Galli, S., Génova-Santos, R., Gerbino, M., González-Nuevo, J., Hagstotz, S., Greenslade, J., Handley, W., Hernández-Monteagudo, C., Hervias-Caimapo, C., Hivon, E., Kiiveri, K., Kisner, T., Kitching, T., Kunz, M., Kurki-Suonio, H., Lasenby, A., Lattanzi, M., Lesgourgues, J., Lewis, A., Liguori, M., Lindholm, V., Luzzi, G., Martins, C.J.A.P., Matarrese, S., Melchiorri, A., Melin, J.B., Molinari, D., Natoli, P., Negrello, M., Notari, A., Paoletti, D., Patanchon, G., Polastri, L., Polenta, G., Pollo, A., Poulin, V., Quartin, M., Remazeilles, M., Roman, M., Rubiño-Martín, J.A., Salvati, L., Tomasi, M., Tramonte, D., Trombetti, T., Väliviita, J., De Weyjgaert, R.V., Tent, B.V., Vennin, V., Vielva, P., Vittorio, N.
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