Author: "Benton, S. J." - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Benton, S. J."' showing total 141 results

Start Over Author "Benton, S. J."

141 results on '"Benton, S. J."'

101. Bicep2/keck Array. Vii. Matrix Basede/bseparation Applied to Bicep2 and the Keck Array

Author: Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, Kate Denham, Barkats, Denis A., Benton, S. J., Bischoff, Colin A., Bock, J. J., Bowens-Rubin, Rachel, Brevik, J. A., Buder, I, Bullock, E., Buza, Victor, Connors, Jake Anthony, Crill, B. P., Duband, L., Dvorkin, Cora, Filippini, J. P., Fliescher, S., Grayson, J., Halpern, M., Harrison, Sarah, Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J., Karkare, Kirit Sukrit, Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, John M, Kuo, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O’Brient, R., IV, R. W. Ogburn, Orlando, A., Pryke, C., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C, Wu, W. L. K., and Yoon, K. W.
Subjects: cosmic background radiation, cosmology: observations, gravitational waves, inflation, polarization, pixel, tensor, harmonic, sphere, covariance, BICEP, B-mode, polarization: linear
Abstract: A linear polarization field on the sphere can be uniquely decomposed into an E-mode and a B-mode component. These two components are analytically defined in terms of spin-2 spherical harmonics. Maps that contain filtered modes on a partial sky can also be decomposed into E-mode and B-mode components. However, the lack of full sky information prevents orthogonally separating these components using spherical harmonics. In this paper, we present a technique for decomposing an incomplete map into E and B-mode components using E and B eigenmodes of the pixel covariance in the observed map. This method is found to orthogonally define E and B in the presence of both partial sky coverage and spatial filtering. This method has been applied to the Bicep2 and the Keck Array maps and results in reducing E to B leakage from ΛCDM E-modes to a level corresponding to a tensor-to-scalar ratio of, Astronomy
Published: 2016
Full Text: View/download PDF

102. Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band

Author: Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bischoff, Colin A., Bock, J. J., Bowens-Rubin, Rachel, Brevik, J. A., Buder, I, Bullock, E., Buza, Victor, Connors, Jake Anthony, Crill, B. P., Duband, L., Dvorkin, Cora, Filippini, J. P., Fliescher, S., Grayson, J., Halpern, M., Harrison, Sarah, Hilton, G. C., Hui, H., Irwin, K. D., Karkare, Kirit Sukrit, Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, John M, Kuo, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O’Brient, R., Ogburn, R. W., Orlando, A., Pryke, Clement L., Richter, Sonja Valeska, Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C, Wu, W. L. K., and Yoon, K. W.
Abstract: We present results from an analysis of all data taken by the BICEP2 and Keck Array cosmic microwave background (CMB) polarization experiments up to and including the 2014 observing season. This includes the first Keck Array observations at 95 GHz. The maps reach a depth of 50 nK deg in Stokes Q and U in the 150 GHz band and 127 nK deg in the 95 GHz band. We take auto- and cross-spectra between these maps and publicly available maps from WMAP and Planck at frequencies from 23 to 353 GHz. An excess over lensed ΛCDM is detected at modest significance in the 95 × 150 BB spectrum, and is consistent with the dust contribution expected from our previous work. No significant evidence for synchrotron emission is found in spectra such as 23 × 95, or for correlation between the dust and synchrotron sky patterns in spectra such as 23 × 353. We take the likelihood of all the spectra for a multicomponent model including lensed ΛCDM, dust, synchrotron, and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r) using priors on the frequency spectral behaviors of dust and synchrotron emission from previous analyses of WMAP and Planck data in other regions of the sky. This analysis yields an upper limit r0.05 < 0.09 at 95% confidence, which is robust to variations explored in analysis and priors. Combining these B-mode results with the (more model-dependent) constraints from Planck analysis of CMB temperature plus baryon acoustic oscillations and other data yields a combined limit r0.05 < 0.07 at 95% confidence. These are the strongest constraints to date on inflationary gravitational waves., Astronomy, Physics
Published: 2016
Full Text: View/download PDF

103. BICEP3: a 95GHz refracting telescope for degree-scale CMB polarization

Author: Holland, Wayne S., Zmuidzinas, Jonas, Ahmed, Z., Amiri, M., Benton, S. J., Bock, J. J., Bowens-Rubin, R., Buder, I., Bullock, E., Connors, J., Filippini, J. P., Grayson, J. A., Halpern, M., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kovac, J. M., Kuo, C. L., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C., Reintsema, C. D., Richter, S., Thompson, K. L., Turner, A. D., Vieregg, A. G., Wu, W. L. K., and Yoon, K. W.
Published: 2014
Full Text: View/download PDF

104. Keck array and BICEP3: spectral characterization of 5000+ detectors

Author: Holland, Wayne S., Zmuidzinas, Jonas, Karkare, K. S., Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Bonetti, J. A., Brevik, J. A., Buder, I., Bullock, E. W., Burger, B., Connors, J., Crill, B. P., Davis, G., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S. T., Golwala, S. R., Gordon, M. S., Grayson, J. A., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J. H., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Mason, P., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C. L., Reintsema, C. D., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Turner, A. D., Vieregg, A., Weber, A., Wong, C. L., Wu, W. L. K., and Yoon, K. W.
Published: 2014
Full Text: View/download PDF

105. Pointing control for the SPIDER balloon-borne telescope

Author: Stepp, Larry M., Gilmozzi, Roberto, Hall, Helen J., Shariff, J. A., Ade, P. A. R., Amiri, M., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Doré, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Gambrel, A. E., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Kuo, C. L., MacTavish, C. J., Mason, P. V., Megerian, K. G., Moncelsi, L., Morford, T. A., Nagy, J. M., Netterfield, C. B., O'Brient, R., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Soler, J. D., Trangsrud, A., Tucker, C. E., Tucker, R. S., Turner, A. D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Published: 2014
Full Text: View/download PDF

106. Design and construction of a carbon fiber gondola for the SPIDER balloon-borne telescope

Author: Stepp, Larry M., Gilmozzi, Roberto, Hall, Helen J., Soler, J. D., Ade, P. A. R., Amiri, M., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, C., Contaldi, C. C., Crill, B. P., Doré, O. P., Farhang, M., Filippini, Jeffrey P., Fissel, L. M., Fraisse, A. A., Gambrel, A. E., Gandilo, N. N., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. K., Kuo, C.-L., MacTavish, C. J., Mason, P. V., Megerian, K. G., Moncelsi, L., Morford, T., Nagy, J. M., Netterfield, C. B., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Shariff, J. A., Trangsrud, A., Tucker, C., Tucker, R. S., Turner, A. D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Published: 2014
Full Text: View/download PDF

107. bicep2/Keck Array. IV. Optical Characterization and Performance of the Bicep2 and Keck Array Experiments

Author: Ade, P. A. R., Aikin, R. W., Barkats, Denis A., Benton, S. J., Bischoff, Colin A., Bock, J. J., Bradford, K. J., Brevik, J. A., Buder, I, Bullock, E., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J. H., Karkare, Kirit Sukrit, Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, John M, Kuo, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O’Brient, R., IV, R. W. Ogburn, Orlando, A., Pryke, C, Richter, Sonja Valeska, Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, R. V., Teply, G. P., Thompson, K., Tolan, J. E., Turner, A. D., Vieregg, A. G., Weber, A. C., Wong, C, and Yoon, K. W.
Subjects: cosmic background radiation, cosmology: observations, gravitational waves, inflation, polarization
Abstract: bicep2 and the Keck Array are polarization-sensitive microwave telescopes that observe the cosmic microwave background (CMB) from the South Pole at degree angular scales in search of a signature of inflation imprinted as B-mode polarization in the CMB. bicep2 was deployed in late 2009, observed for three years until the end of 2012 at 150 GHz with 512 antenna-coupled transition edge sensor bolometers, and has reported a detection of B-mode polarization on degree angular scales. The Keck Array was first deployed in late 2010 and will observe through 2016 with five receivers at several frequencies (95, 150, and 220 GHz). bicep2 and the Keck Array share a common optical design and employ the field-proven bicep1 strategy of using small-aperture, cold, on-axis refractive optics, providing excellent control of systematics while maintaining a large field of view. This design allows for full characterization of far-field optical performance using microwave sources on the ground. Here we describe the optical design of both instruments and report a full characterization of the optical performance and beams of bicep2 and the Keck Array at 150 GHz., Astronomy
Published: 2015
Full Text: View/download PDF

108. BICEP2 III: Instrumental Systematics

Author: Ade, P. A. R., Aikin, R. W., Barkats, Denis A., Benton, S. J., Bischoff, Colin A., Bock, J. J., Brevik, J. A., Buder, I, Bullock, E., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Irwin, K. D., Karkare, Kirit Sukrit, Kaufman, J. P., Keating, B. G., Kernasovskiy, S. A., Kovac, John M, Kuo, C. L., Leitch, E. M., Lueker, M., Netterfield, C. B., Nguyen, H. T., O’Brient, R., IV, R. W. Ogburn, Orlando, Abigail Claire, Pryke, C, Richter, Sonja Valeska, Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, R. V., Teply, G. P., Tolan, J. E., Turner, A. D., Vieregg, A. G., Wong, C, and Yoon, K. W.
Subjects: cosmic background radiation, cosmology: observations, gravitational waves, inflation, instrumentation: polarimeters, methods: data analysis
Abstract: In a companion paper, we have reported a >5σ detection of degree scale B-mode polarization at 150 GHz by the Bicep2 experiment. Here we provide a detailed study of potential instrumental systematic contamination to that measurement. We focus extensively on spurious polarization that can potentially arise from beam imperfections. We present a heuristic classification of beam imperfections according to their symmetries and uniformities, and discuss how resulting contamination adds or cancels in maps that combine observations made at multiple orientations of the telescope about its boresight axis. We introduce a technique, which we call "deprojection," for filtering the leading order beam-induced contamination from time-ordered data, and show that it reduces power in Bicep2's actual and null-test BB spectra consistent with predictions using high signal-to-noise beam shape measurements. We detail the simulation pipeline that we use to directly simulate instrumental systematics and the calibration data used as input to that pipeline. Finally, we present the constraints on BB contamination from individual sources of potential systematics. We find that systematics contribute BB power that is a factor of ~10× below Bicep2's three-year statistical uncertainty, and negligible compared to the observed BB signal. The contribution to the best-fit tensor/scalar ratio is at a level equivalent to r = (3–6) × 10−3., Astronomy
Published: 2015
Full Text: View/download PDF

109. Joint Analysis of BICEP2/ Keck Array and Planck Data

Author: Ade, P. A. R., Aghanim, N., Ahmed, Z., Aikin, R. W., Alexander, Kate Denham, Arnaud, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barkats, D., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Benton, S. J., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bischoff, Colin A., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Brevik, J. A., Bucher, M., Buder, I., Bullock, E., Burigana, C., Butler, R. C., Buza, Victor, Calabrese, E., Cardoso, J.-F., Catalano, A., Challinor, A., Chary, R.-R., Chiang, H. C., Christensen, P. R., Colombo, L. P. L., Combet, C., Connors, Jake Anthony, Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J.-M., Désert, F.-X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dowell, C. D., Duband, L., Ducout, A., Dunkley, J., Dupac, X., Dvorkin, Cora, Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Filippini, J. P., Finelli, F., Fliescher, S., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., Golwala, S. R., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Halpern, M., Hansen, F. K., Hanson, D., Harrison, D. L., Hasselfield, M., Helou, G., Henrot-Versillé, S., Herranz, D., Hildebrandt, S. R., Hilton, G. C., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hristov, V. V., Huffenberger, K. M., Hui, H., Hurier, G., Irwin, K. D., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Karakci, A., Karkare, Kirit Sukrit, Kaufman, J. P., Keating, B. G., Kefeli, S., Keihänen, E., Kernasovskiy, S. A., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kovac, John M, Krachmalnicoff, N., Kunz, M., Kuo, C. L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leitch, E. M., Leonardi, R., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Lueker, M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Mason, P., Matarrese, S., Megerian, K. G., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nguyen, H. T., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O’Brient, R., Ogburn, R. W., Orlando, A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Pratt, G. W., Prunet, S., Pryke, Clement L., Puget, J.-L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Richter, Sonja Valeska, Ristorcelli, I., Rocha, G., Rossetti, M., Roudier, G., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Schwarz, R., Scott, D., Seiffert, M. D., Sheehy, C. D., Spencer, L. D., Staniszewski, Z. K., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J. A., Teply, G. P., Terenzi, L., Thompson, K. L., Toffolatti, L., Tolan, J. E., Tomasi, M., Tristram, M., Tucci, M., Turner, A. D., Valenziano, L., Valiviita, J., Van Tent, B., Vibert, L., Vielva, P., Vieregg, A. G., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Weber, A. C., Wehus, I. K., White, M., White, S. D. M., Willmert, J., Wong, C. L., Yoon, K. W., Yvon, D., Zacchei, A., and Zonca, A.
Abstract: We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400 deg2 patch of sky centered on RA 0h, Dec. −57.5deg. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2 μK deg in Q and U at 143 GHz). We detect 150×353 cross-correlation in B-modes at high significance. We fit the single- and cross-frequency power spectra at frequencies ≥150 GHz to a lensed-ΛCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parameterized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous \planck\ analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r0.05<0.12 at 95% confidence. Marginalizing over dust and r, lensing B-modes are detected at 7.0σ significance., Astronomy
Published: 2015
Full Text: View/download PDF

110. BICEP2. II. Experiment and three-year data set

Author: Ade, P. A. R., Aikin, R. W., Amiri, M., Barkats, Denis A., Benton, S. J., Bischoff, Colin A., Bock, J. J., Brevik, J. A., Buder, I., Bullock, E., Davis, G., Day, P. K., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Irwin, K. D., Karkare, Kirit Sukrit, Kaufman, J. P., Keating, B. G., Kernasovskiy, S. A., Kovac, John M, Kuo, C. L., Leitch, E. M., Llombart, N., Lueker, M., Netterfield, C. B., Nguyen, H. T., O, R., Ogburn, R. W., Orlando, Abigail Claire, Pryke, C, Reintsema, C. D., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Story, K. T., Sudiwala, R. V., Teply, G. P., Tolan, J. E., Turner, A. D., Vieregg, A. G., Wilson, P., Wong, C, and Yoon, K. W.
Subjects: cosmic background radiation, cosmology: observations, gravitational waves, inflation, instrumentation: polarimeters, telescopes
Abstract: We report on the design and performance of the BICEP2 instrument and on its three-year data set. BICEP2 was designed to measure the polarization of the cosmic microwave background (CMB) on angular scales of 1°-5°(l = 40-200), near the expected peak of the B-mode polarization signature of primordial gravitational waves from cosmic inflation. Measuring B-modes requires dramatic improvements in sensitivity combined with exquisite control of systematics. The BICEP2 telescope observed from the South Pole with a 26 cm aperture and cold, on-axis, refractive optics. BICEP2 also adopted a new detector design in which beam-defining slot antenna arrays couple to transition-edge sensor (TES) bolometers, all fabricated on a common substrate. The antenna-coupled TES detectors supported scalable fabrication and multiplexed readout that allowed BICEP2 to achieve a high detector count of 500 bolometers at 150 GHz, giving unprecedented sensitivity to B-modes at degree angular scales. After optimization of detector and readout parameters, BICEP2 achieved an instrument noise-equivalent temperature of 15.8 μ {K}\sqrt{{s}}. The full data set reached Stokes Q and U map depths of 87.2 nK in square-degree pixels (5.'2 μK) over an effective area of 384 deg2 within a 1000 deg2 field. These are the deepest CMB polarization maps at degree angular scales to date. The power spectrum analysis presented in a companion paper has resulted in a significant detection of B-mode polarization at degree scales., Astronomy
Published: 2014
Full Text: View/download PDF

111. 2010 BLASTPol Observations of the Magnetic Field of the Filamentary Galactic Cloud 'Lupus I'

Author: Matthews, Tristan, Ade, P., Angilè, F. E., Benton, S. J., Chapman, N. L., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N., Gundersen, J. O., Peter Hargrave, Galitzki, N. B., Klein, J., Korotkov, A., Moncelsi, L., Mroczkowski, T., Netterfield, C., Novak, G., Nutter, D., Olmi, L., Poidevin, F., Savini, G., Scott, D., Shariff, J., Soler, J. D., Thomas, N. E., Truch, M., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.

112. BLAST-pol: The Balloon-borne Large Aperture Submillimeter Telescope Plus Polarimeter

Author: Matthews, Tristan, Abe, P. A. R., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. D., Gandilo, N. N., Gundersen, J. O., Hargrave, P. C., Hughes, D. H., Klein, J., Korotkov, A. L., Macaluso, J., Moncelsi, L., Mroczkowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, E., Savini, G., Douglas Scott, Soler, J. D., Thomas, N. E., Truch, M. D. P., Tucker, C. E., Tucker, G. S., Ward-Thompson, D., and Wiebe, D. V.

113. Measurements of Degree-Scale B-mode Polarization with the BICEP/$Keck$ Experiments at South Pole

Author: Racine, Benjamin, Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Crumrine, M., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Fliescher, S., Grayson, J., Hall, G., Halpern, M., Harrison, S., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Lau, K., Larsen, N. A., Leitch, E. M., Lueker, M., Megerian, K. G., Moncelsi, L., Toshiya Namikawa, Netterfield, B., Nguyen, H. T., O Brient, R., Ogburn, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schwarz, R., Schillaci, A., Sheehy, C. D., Soliman, A., Germaine, T. St, Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, H., Yoon, K. W., Zhang, C., Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), BICEP, Keck, Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), satellite: Planck, Astrophysics::Instrumentation and Methods for Astrophysics, gravitational radiation: primordial, FOS: Physical sciences, cosmic background radiation: polarization, Astrophysics::Cosmology and Extragalactic Astrophysics, BICEP, frequency: high, detector: sensitivity, gravitation: lens, B-mode, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The BICEP and Keck Array experiments are a suite of small-aperture refracting telescopes observing the microwave sky from the South Pole. They target the degree-scale B-mode polarization signal imprinted in the Cosmic Microwave Background (CMB) by primordial gravitational waves. Such a measurement would shed light on the physics of the very early universe. While BICEP2 observed for the first time a B-mode signal at 150 GHz, higher frequencies from the Planck satellite showed that it could be entirely due to the polarized emission from Galactic dust, though uncertainty remained high. Keck Array has been observing the same region of the sky for several years, with an increased detector count, producing the deepest polarized CMB maps to date. New detectors at 95 GHz were installed in 2014, and at 220 GHz in 2015. These observations enable a better constraint of galactic foreground emissions, as presented here. In 2015, BICEP2 was replaced by BICEP3, a 10 times higher throughput telescope observing at 95 GHz, while Keck Array is now focusing on higher frequencies. In the near future, BICEP Array will replace Keck Array, and will allow unprecedented sensitivity to the gravitational wave signal. High resolution observations from the South Pole Telescope (SPT) will also be used to remove the lensing contribution to B-modes., Comment: 9 pages, 8 figures: conference proceedings, 53rd Rencontres de Moriond, Cosmology 2018

114. BLAST-pol: Balloon-borne Large Aperture Submillimeter Telescope for Polarimetery

Author: Thomas, Nicholas Evan, Ade, P. A. R., Angilè, F. E., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. M., Gandilo, N. N., Gundersen, J. O., Hargrave, P. C., Hughes, D. H., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Mroczkowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, E., Savini, G., Douglas Scott, Shariff, J. A., Soler, J. D., Truch, M. D. P., Tucker, C. E., Tucker, G. S., Ward-Thompson, D., and Wiebe, D. V.

115. 2010 BLASTPol Observations of the magnetic field of the filamentary galactic cloud 'Lupus I'

Author: Matthews, Tristan, Ade, P., Angile, F. E., Benton, S. J., Chapman, N. L., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N., Gundersen, J. O., Hargrave, P., Galitzki, N. B., Klein, J., Korotkov, A., Moncelsi, L., Mroczkowski, T., Netterfield, C., Novak, G., Nutter, D., Olmi, L., Poidevin, F., Savini, G., Scott, D., Shariff, J., Soler, J. D., Thomas, N. E., Truch, M., Tucker, C. E., Tucker, G. S., Ward-Thompson, D., Matthews, Tristan, Ade, P., Angile, F. E., Benton, S. J., Chapman, N. L., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N., Gundersen, J. O., Hargrave, P., Galitzki, N. B., Klein, J., Korotkov, A., Moncelsi, L., Mroczkowski, T., Netterfield, C., Novak, G., Nutter, D., Olmi, L., Poidevin, F., Savini, G., Scott, D., Shariff, J., Soler, J. D., Thomas, N. E., Truch, M., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.
Abstract: We present here 350 and 500 micron polarization observations of the Lupus I molecular cloud taken during the 2010 BLASTPol Antarctic flight. Lupus I is a nearby, isolated, young, and filamentary molecular cloud making it an ideal target to test magnetically regulated star formation models. In the presence of intermediate to strong magnetic fields (in comparison to turbulence), these models predict the formation of large filaments extended perpendicular to the local magnetic field direction as gas preferentially collapses along the field lines. We compare the BLASTPol polarization observations with previous optical polarimetry and find a uniform large-scale field direction from low to high density in Lupus I, consistent with magnetically regulated star formation models.

116. Thermal design and performance of the balloon-borne large aperture submillimeter telescope for polarimetry BLASTPol

Author: Soler, J. D., Ade, P. A. R., Angile, F. E., Benton, S. J., Devlin, M. J., Dober, B., Fisel, L. M., Fukui, Y., Galitzki, N., Gandilo, N. N., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Mroczkowski, A., Netterfield, C. B., Novak, G., Nutter, D., Pascale, E., Poidevin, F., Savini, G., Scott, D., Shariff, Jamil A., Thomas, N. E., Truch, M. D., Tucker, C. E., Tucker, G. S., Ward-Thompson, D., Soler, J. D., Ade, P. A. R., Angile, F. E., Benton, S. J., Devlin, M. J., Dober, B., Fisel, L. M., Fukui, Y., Galitzki, N., Gandilo, N. N., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, L., Mroczkowski, A., Netterfield, C. B., Novak, G., Nutter, D., Pascale, E., Poidevin, F., Savini, G., Scott, D., Shariff, Jamil A., Thomas, N. E., Truch, M. D., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.
Abstract: We present the thermal model of the Balloon-borne Large-Aperture Submillimeter Telescope for Polarimetry (BLASTPol). This instrument was successfully own in two circumpolar flights from McMurdo, Antarctica in 2010 and 2012. During these two flights, BLASTPol obtained unprecedented information about the magnetic field in molecular clouds through the measurement of the polarized thermal emission of interstellar dust grains. The thermal design of the experiment addresses the stability and control of the payload necessary for this kind of measurement. We describe the thermal modeling of the payload including the sun-shielding strategy. We present the in-flight thermal performance of the instrument and compare the predictions of the model with the temperatures registered during the flight. We describe the difficulties of modeling the thermal behavior of the balloon-borne platform and establish landmarks that can be used in the design of future balloon-borne instruments.

117. Ultra-thin large-aperture vacuum windows for millimeter wavelengths receivers

Author: Barkats, Denis, Dierickx, Marion I., Kovac, John M, Pentacoff, Chris, Ade, P. A. R, Ahmed, Z, Aikin, R. W, Alexander, K. D, Benton, S. J, Bischof, C. A, Bock, J. J, Bowens-Rubin, R, Brevik, J. A, Buder, I, Bullock, E, Buza, V, Connors, J, Cornelison, J, Crill, B. P, Crumrine, M, Duband, L, Dvorkin, C, Filippini, J. P, Fliescher, S, Grayson, J, Hall, G, Halpern, M, Harrison, S, Hildebrandt, S. R, Hilton, G. C, Hui, H, Irwin, K. D, Kang, J, Karkare, K. S, Karpel, E, Kaufman, J. P, Keating, B. G, Kefeli, S, Kernasovskiy, S. A, Kuo, C. L, Lau, K, Larsen, N. A, Leitch, E. M, Lueker, M, Megerian, K. G, Moncelsi, L, Namikawa, T, Nguyen, H. T, O'Brient, R, Ogburn IV, R. W., Palladino, S, Pryke, C, Racine, B, Richter, S, Schwarz, R, Schillaci, A, Sheehy, C. D, Soliman, A, St. Germaine, T, Staniszewski, Z. K, Steinbach, B, Sudiwala, R. V, Teply, G. P, Thompson, K. L., Tolan, J. E, Tucker, C, Turner, A. D, Umilta, C, Vieregg, A. G, Wandui, A, Weber, A. C, Wiebe, D. V, Willmert, J, Wong, C. L, Wu, W. L. K., Yang, H, Yoon, K. W, Zhang, Z, Barkats, Denis, Dierickx, Marion I., Kovac, John M, Pentacoff, Chris, Ade, P. A. R, Ahmed, Z, Aikin, R. W, Alexander, K. D, Benton, S. J, Bischof, C. A, Bock, J. J, Bowens-Rubin, R, Brevik, J. A, Buder, I, Bullock, E, Buza, V, Connors, J, Cornelison, J, Crill, B. P, Crumrine, M, Duband, L, Dvorkin, C, Filippini, J. P, Fliescher, S, Grayson, J, Hall, G, Halpern, M, Harrison, S, Hildebrandt, S. R, Hilton, G. C, Hui, H, Irwin, K. D, Kang, J, Karkare, K. S, Karpel, E, Kaufman, J. P, Keating, B. G, Kefeli, S, Kernasovskiy, S. A, Kuo, C. L, Lau, K, Larsen, N. A, Leitch, E. M, Lueker, M, Megerian, K. G, Moncelsi, L, Namikawa, T, Nguyen, H. T, O'Brient, R, Ogburn IV, R. W., Palladino, S, Pryke, C, Racine, B, Richter, S, Schwarz, R, Schillaci, A, Sheehy, C. D, Soliman, A, St. Germaine, T, Staniszewski, Z. K, Steinbach, B, Sudiwala, R. V, Teply, G. P, Thompson, K. L., Tolan, J. E, Tucker, C, Turner, A. D, Umilta, C, Vieregg, A. G, Wandui, A, Weber, A. C, Wiebe, D. V, Willmert, J, Wong, C. L, Wu, W. L. K., Yang, H, Yoon, K. W, and Zhang, Z
Abstract: Targeting faint polarization patterns arising from Primordial Gravitational Waves in the Cosmic Microwave Background requires excellent observational sensitivity. Optical elements in small aperture experiments such as Bicep3 and Keck Array are designed to optimize throughput and minimize losses from transmission, reflection and scattering at millimeter wavelengths. As aperture size increases, cryostat vacuum windows must withstand larger forces from atmospheric pressure and the solution has often led to a thicker window at the expense of larger transmission loss. We have identified a new candidate material for the fabrication of vacuum windows: with a tensile strength two orders of magnitude larger than previously used materials, woven high-modulus polyethylene could allow for dramatically thinner windows, and therefore significantly reduced losses and higher sensitivity. In these proceedings we investigate the suitability of high-modulus polyethylene windows for ground-based CMB experiments, such as current and future receivers in the Bicep/Keck Array program. This includes characterizing their optical transmission as well as their mechanical behavior under atmospheric pressure. We find that such ultra-thin materials are promising candidates to improve the performance of large-aperture instruments at millimeter wavelengths, and outline a plan for further tests ahead of a possible upcoming field deployment of such a science-grade window....

118. Design and construction of a carbon fiber gondola for the SPIDER balloon-borne telescope

Author: Soler, J. D., Ade, P. A. R., Amiri, M., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, C., Contaldi, C. C., Crill, B. P., Dore, O. P., Farhang, M., Filippini, Jeffrey P., Fissel, L. M., Fraisse, A. A., Gambrel, A. E., Gandilo, N. N., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. K., Kuo, C. -L., MacTavish, C. J., Mason, P. V., Megerian, K. G., Moncelsi, L., Morford, T., Nagy, J. M., Netterfield, C. B., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Shariff, J. A., Trangsrud, A., Tucker, C., Tucker, R. S., Turner, A. D., Weber, A. C., Wiebe, D. V., Young, E. Y., Soler, J. D., Ade, P. A. R., Amiri, M., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, C., Contaldi, C. C., Crill, B. P., Dore, O. P., Farhang, M., Filippini, Jeffrey P., Fissel, L. M., Fraisse, A. A., Gambrel, A. E., Gandilo, N. N., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. K., Kuo, C. -L., MacTavish, C. J., Mason, P. V., Megerian, K. G., Moncelsi, L., Morford, T., Nagy, J. M., Netterfield, C. B., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Shariff, J. A., Trangsrud, A., Tucker, C., Tucker, R. S., Turner, A. D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Abstract: We introduce the light-weight carbon fiber and aluminum gondola designed for the Spider balloon-borne telescope. Spider is designed to measure the polarization of the Cosmic Microwave Background radiation with unprecedented sensitivity and control of systematics in search of the imprint of inflation: a period of exponential expansion in the early Universe. The requirements of this balloon-borne instrument put tight constrains on the mass budget of the payload. The Spider gondola is designed to house the experiment and guarantee its operational and structural integrity during its balloon-borne flight, while using less than 10% of the total mass of the payload. We present a construction method for the gondola based on carbon fiber reinforced polymer tubes with aluminum inserts and aluminum multi-tube joints. We describe the validation of the model through Finite Element Analysis and mechanical tests.

119. Attitude determination for balloon-borne experiments

Author: Stepp, Larry M., Gilmozzi, Roberto, Hall, Helen J., Gandilo, N. N., Ade, P. A. R., Amiri, M., Angilè, F. E., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Doré, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., Young, E. Y., Stepp, Larry M., Gilmozzi, Roberto, Hall, Helen J., Gandilo, N. N., Ade, P. A. R., Amiri, M., Angilè, F. E., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Doré, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Golwala, S., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Abstract: An attitude determination system for balloon-borne experiments is presented. The system provides pointing information in azimuth and elevation for instruments flying on stratospheric balloons over Antarctica. In-flight attitude is given by the real-time combination of readings from star cameras, a magnetometer, sun sensors, GPS, gyroscopes, tilt sensors and an elevation encoder. Post-flight attitude reconstruction is determined from star camera solutions, interpolated by the gyroscopes using an extended Kalman Filter. The multi-sensor system was employed by the Balloon-borne Large Aperture Submillimeter Telescope for Polarimetry (BLASTPol), an experiment that measures polarized thermal emission from interstellar dust clouds. A similar system was designed for the upcoming flight of Spider, a Cosmic Microwave Background polarization experiment. The pointing requirements for these experiments are discussed, as well as the challenges in designing attitude reconstruction systems for high altitude balloon flights. In the 2010 and 2012 BLASTPol flights from McMurdo Station, Antarctica, the system demonstrated an accuracy of < 5’ rms in-flight, and < 5” rms post-flight.

120. Optical characterization of the BICEP3 CMB polarimeter at the South Pole

Author: Holland, Wayne S., Zmuidzinas, Jonas, Karkare, K. S., Ade, P. A. R., Ahmed, Z., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Buder, I., Bullock, E., Buza, V., Connors, J., Filippini, J. P., Fliescher, S. T., Grayson, J. A., Halpern, M., Harrison, S. A., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J. H., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Monticue, V., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C. L., Reintsema, C. D., Richter, S., St. Germaine, M. T., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Wandui, A., Weber, A., Willmert, J., Wong, C. L., Wu, W. L. K., Yoon, K. W., Holland, Wayne S., Zmuidzinas, Jonas, Karkare, K. S., Ade, P. A. R., Ahmed, Z., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Buder, I., Bullock, E., Buza, V., Connors, J., Filippini, J. P., Fliescher, S. T., Grayson, J. A., Halpern, M., Harrison, S. A., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J. H., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Monticue, V., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C. L., Reintsema, C. D., Richter, S., St. Germaine, M. T., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Wandui, A., Weber, A., Willmert, J., Wong, C. L., Wu, W. L. K., and Yoon, K. W.
Abstract: BICEP3 is a small-aperture refracting cosmic microwave background (CMB) telescope designed to make sensitive polarization maps in pursuit of a potential B-mode signal from inflationary gravitational waves. It is the latest in the Bicep/Keck Array series of CMB experiments located at the South Pole, which has provided the most stringent constraints on inflation to date. For the 2016 observing season, BICEP3 was outfitted with a full suite of 2400 optically coupled detectors operating at 95 GHz. In these proceedings we report on the far field beam performance using calibration data taken during the 2015-2016 summer deployment season in situ with a thermal chopped source. We generate high-fidelity per-detector beam maps, show the array-averaged beam profile, and characterize the differential beam response between co-located, orthogonally polarized detectors which contributes to the leading instrumental systematic in pair differencing experiments. We find that the levels of differential pointing, beamwidth, and ellipticity are similar to or lower than those measured for Bicep2 and Keck Array. The magnitude and distribution of Bicep3’s differential beam mismatch – and the level to which temperature-to-polarization leakage may be marginalized over or subtracted in analysis - will inform the design of next-generation CMB experiments with many thousands of detectors.

121. 2010 BLASTPol Observations of the magnetic field of the filamentary galactic cloud 'Lupus I'

Author: Matthews, Tristan, Ade, P., Angile, F. E., Benton, S. J., Chapman, N. L., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N., Gundersen, J. O., Hargrave, P., Galitzki, N. B., Klein, J., Korotkov, A., Moncelsi, L., Mroczkowski, T., Netterfield, C., Novak, G., Nutter, D., Olmi, L., Poidevin, F., Savini, G., Scott, D., Shariff, J., Soler, J. D., Thomas, N. E., Truch, M., Tucker, C. E., Tucker, G. S., Ward-Thompson, D., Matthews, Tristan, Ade, P., Angile, F. E., Benton, S. J., Chapman, N. L., Devlin, M. J., Dober, B., Fissel, L. M., Fukui, Y., Gandilo, N., Gundersen, J. O., Hargrave, P., Galitzki, N. B., Klein, J., Korotkov, A., Moncelsi, L., Mroczkowski, T., Netterfield, C., Novak, G., Nutter, D., Olmi, L., Poidevin, F., Savini, G., Scott, D., Shariff, J., Soler, J. D., Thomas, N. E., Truch, M., Tucker, C. E., Tucker, G. S., and Ward-Thompson, D.
Abstract: We present here 350 and 500 micron polarization observations of the Lupus I molecular cloud taken during the 2010 BLASTPol Antarctic flight. Lupus I is a nearby, isolated, young, and filamentary molecular cloud making it an ideal target to test magnetically regulated star formation models. In the presence of intermediate to strong magnetic fields (in comparison to turbulence), these models predict the formation of large filaments extended perpendicular to the local magnetic field direction as gas preferentially collapses along the field lines. We compare the BLASTPol polarization observations with previous optical polarimetry and find a uniform large-scale field direction from low to high density in Lupus I, consistent with magnetically regulated star formation models.

122. BLASTbus electronics: general-purpose readout and control for balloon-borne experiments

Author: Benton, S. J., Ade, P. A., Amiri, M., Angile, F. E., Bock, J. J., Bond, J. R., Sryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Dore, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Ogburn IV, R. W., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., Youn, E. Y., Benton, S. J., Ade, P. A., Amiri, M., Angile, F. E., Bock, J. J., Bond, J. R., Sryan, S. A., Chiang, H. C., Contaldi, C. R., Crill, B. P., Devlin, M. J., Dober, B., Dore, O. P., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Fukui, Y., Galitzki, N., Gambrel, A. E., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G. C., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, W. C., Kermish, Z. D., Klein, J., Korotkov, A. L., Kuo, C. L., MacTavish, C. J., Mason, P. V., Matthews, T. G., Megerian, K. G., Moncelsi, L., Morford, T. A., Mroczkowski, T. K., Nagy, J. M., Netterfield, C. B., Novak, G., Nutter, D., O'Brient, R., Ogburn IV, R. W., Pascale, E., Poidevin, F., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Savini, G., Scott, D., Shariff, J. A., Soler, J. D., Thomas, N. E., Trangsrud, A., Truch, M. D., Tucker, C. E., Tucker, G. S., Tucker, R. S., Turner, A. D., Ward-Thompson, D., Weber, A. C., Wiebe, D. V., and Youn, E. Y.
Abstract: We present the second generation BLASTbus electronics. The primary purposes of this system are detector readout, attitude control, and cryogenic housekeeping, for balloon-borne telescopes. Readout of neutron transmutation doped germanium (NTD-Ge) bolometers requires low noise and parallel acquisition of hundreds of analog signals. Controlling a telescope's attitude requires the capability to interface to a wide variety of sensors and motors, and to use them together in a fast, closed loop. To achieve these different goals, the BLASTbus system employs a flexible motherboard-daughterboard architecture. The programmable motherboard features a digital signal processor (DSP) and field-programmable gate array (FPGA), as well as slots for three daughterboards. The daughterboards provide the interface to the outside world, with versions for analog to digital conversion, and optoisolated digital input/output. With the versatility afforded by this design, the BLASTbus also finds uses in cryogenic, thermometry, and power systems. For accurate timing control to tie everything together, the system operates in a fully synchronous manner. BLASTbus electronics have been successfully deployed to the South Pole, and own on stratospheric balloons.

123. BICEP Array cryostat and mount design

Author: Crumrine, Michael, Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bishchoff, C. A., Bock, J. J., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Filescher, S., Grayson, J. A., Hall, G., Halpern, M., Harrison, S. A., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J. H., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kemasovskiy, S. A., Kovac, J. M., Kuo, C. L., Larsen, N. A., Lau, K., Leitch, E. M., Lueker, M. V., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn IV, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schwarz, R., Schillaci, A., Sheehy, C. D., Soliman, A., St. Germaine, T., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C. E., Turner, A. D., Umilta, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., WIllmert, J., Wong, C. L., Wu, W. L. K., Yang, E., Yoon, K. W., Zhang, C., Crumrine, Michael, Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bishchoff, C. A., Bock, J. J., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Filescher, S., Grayson, J. A., Hall, G., Halpern, M., Harrison, S. A., Hildebrandt, S. R., Hilton, G. C., Hui, H., Irwin, K. D., Kang, J. H., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kemasovskiy, S. A., Kovac, J. M., Kuo, C. L., Larsen, N. A., Lau, K., Leitch, E. M., Lueker, M. V., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn IV, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schwarz, R., Schillaci, A., Sheehy, C. D., Soliman, A., St. Germaine, T., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C. E., Turner, A. D., Umilta, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., WIllmert, J., Wong, C. L., Wu, W. L. K., Yang, E., Yoon, K. W., and Zhang, C.
Abstract: Bicep Array is a cosmic microwave background (CMB) polarization experiment that will begin observing at the South Pole in early 2019. This experiment replaces the five Bicep2 style receivers that compose the Keck Array with four larger Bicep3 style receivers observing at six frequencies from 30 to 270GHz. The 95GHz and 150GHz receivers will continue to push the already deep Bicep/Keck CMB maps while the 30/40GHz and 220/270GHz receivers will constrain the synchrotron and galactic dust foregrounds respectively. Here we report on the design and performance of the Bicep Array instruments focusing on the mount and cryostat systems....

124. BICEP3 performance overview and planned Keck Array upgrade

Author: Grayson, J. A., Ade, P. A. R., Ahmed, Z., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Buder, I., Bullock, E., Buza, V., Connors, J., Filippini, J. P., Fliescher, S., Halpern, M., Harrison, S., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Lefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kou, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Monticue, V., Namikawa, T., Netterfield, C. B., Nugyen, H. T., O'Brient, R., Ogburn IV, R. W., Pryke, C., Reintsema, C. D., Richter, S., Schwarz, R., Sorenson, C., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., Yoon, K. W., Grayson, J. A., Ade, P. A. R., Ahmed, Z., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Buder, I., Bullock, E., Buza, V., Connors, J., Filippini, J. P., Fliescher, S., Halpern, M., Harrison, S., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Lefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kou, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Monticue, V., Namikawa, T., Netterfield, C. B., Nugyen, H. T., O'Brient, R., Ogburn IV, R. W., Pryke, C., Reintsema, C. D., Richter, S., Schwarz, R., Sorenson, C., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wu, W. L. K., and Yoon, K. W.
Abstract: Bicep3 is a 520mm aperture, compact two-lens refractor designed to observe the polarization of the cosmic microwave background (CMB) at 95 GHz. Its focal plane consists of modularized tiles of antenna-coupled transition edge sensors (TESs), similar to those used in Bicep2 and the Keck Array. The increased per-receiver optical throughput compared to Bicep2/Keck Array, due to both its faster f=1:7 optics and the larger aperture, more than doubles the combined mapping speed of the Bicep/Keck program. The Bicep3 receiver was recently upgraded to a full complement of 20 tiles of detectors (2560 TESs) and is now beginning its second year of observation (and first science season) at the South Pole. We report on its current performance and observing plans. Given its high per-receiver throughput while maintaining the advantages of a compact design, Bicep3- class receivers are ideally suited as building blocks for a 3rd-generation CMB experiment, consisting of multiple receivers spanning 35 GHz to 270 GHz with total detector count in the tens of thousands. We present plans for such an array, the new "BICEP Array" that will replace the Keck Array at the South Pole, including design optimization, frequency coverage, and deployment/observing strategies.

125. Keck Array and BICEP3: spectral characterization of 5000+ detectors

Author: Karkare, K. S., Ade, Peter A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Bonetti, J. A., Brevik, J. A., Buder, I., Bullock, E. W., Burger, B., Connors, J., Crill, B. P., Davis, G., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S. T., Golwala, S. R., Gordon, M. S., Grayson, J. A., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J. H., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Mason, P., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C. L., Reintsema, C. D., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, Rashmikant, Teply, G. P., Thompson, K. L., Tolan, J. E., Turner, A. D., Vieregg, A., Weber, A., Wong, C. L., Wu, W. L. K., Yoon, K. W., Karkare, K. S., Ade, Peter A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Bonetti, J. A., Brevik, J. A., Buder, I., Bullock, E. W., Burger, B., Connors, J., Crill, B. P., Davis, G., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S. T., Golwala, S. R., Gordon, M. S., Grayson, J. A., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J. H., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Mason, P., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C. L., Reintsema, C. D., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, Rashmikant, Teply, G. P., Thompson, K. L., Tolan, J. E., Turner, A. D., Vieregg, A., Weber, A., Wong, C. L., Wu, W. L. K., and Yoon, K. W.
Abstract: The inflationary paradigm of the early universe predicts a stochastic background of gravitational waves which would generate a B-mode polarization pattern in the cosmic microwave background (CMB) at degree angular scales. Precise measurement of B-modes is one of the most compelling observational goals in modern cosmology. Since 2011, the Keck Array has deployed over 2500 transition edge sensor (TES) bolometer detectors at 100 and 150 GHz to the South Pole in pursuit of degree-scale B-modes, and Bicep3 will follow in 2015 with 2500 more at 100 GHz. Characterizing the spectral response of these detectors is important for controlling systematic effects that could lead to leakage from the temperature to polarization signal, and for understanding potential coupling to atmospheric and astrophysical emission lines. We present complete spectral characterization of the Keck Array detectors, made with a Martin-Puplett Fourier Transform Spectrometer at the South Pole, and preliminary spectra of Bicep3 detectors taken in lab. We show band centers and effective bandwidths for both Keck Array bands, and use models of the atmosphere at the South Pole to cross check our absolute calibration. Our procedure for obtaining interferograms in the field with automated 4-axis coupling to the focal plane represents an important step towards efficient and complete spectral characterization of next-generation instruments more than 10000 detectors.

126. The BICEP2 CMB polarization experiment

Author: Holland, Wayne S., Zmuidzinas, Jonas, Ogburn IV, R. W., Ade, Peter A. R., Aikin, R. W., Amiri, M., Benton, S. J., Bock, J. J., Bonetti, J. A., Brevik, J. A., Burger, B., Dowell, C. D., Duband, L., Filippini, J. P., Golwala, S. R., Halpern, M., Hasselfield, M., Hilton, G., Hristov, V. V., Irwin, K., Kaufman, J. P., Keating, B. G., Kovac, J. M., Kuo, C. L., Lange, A. E., Leitch, E. M., Netterfield, C. B., Nguyen, H. T., Orlando, A., Pryke, C. L., Reintsema, C., Richter, S., Ruhl, J. E., Runyan, M. C., Sheehy, C. D., Staniszewski, Z. K., Stokes, S. A., Sudiwala, Rashmikant V., Teply, G. P., Tolan, J. E., Turner, A. D., Wilson, P., Wong, C. L., Holland, Wayne S., Zmuidzinas, Jonas, Ogburn IV, R. W., Ade, Peter A. R., Aikin, R. W., Amiri, M., Benton, S. J., Bock, J. J., Bonetti, J. A., Brevik, J. A., Burger, B., Dowell, C. D., Duband, L., Filippini, J. P., Golwala, S. R., Halpern, M., Hasselfield, M., Hilton, G., Hristov, V. V., Irwin, K., Kaufman, J. P., Keating, B. G., Kovac, J. M., Kuo, C. L., Lange, A. E., Leitch, E. M., Netterfield, C. B., Nguyen, H. T., Orlando, A., Pryke, C. L., Reintsema, C., Richter, S., Ruhl, J. E., Runyan, M. C., Sheehy, C. D., Staniszewski, Z. K., Stokes, S. A., Sudiwala, Rashmikant V., Teply, G. P., Tolan, J. E., Turner, A. D., Wilson, P., and Wong, C. L.
Abstract: The Bicep2 telescope is designed to measure the polarization of the cosmic microwave background on angular scales near 2-4 degrees, near the expected peak of the B-mode polarization signal induced by primordial gravitational waves from inflation. Bicep2 follows the success of Bicep, which has set the most sensitive current limits on B-modes on 2-4 degree scales. The experiment adopts a new detector design in which beam-defining slot antennas are coupled to TES detectors photolithographically patterned in the same silicon wafer, with multiplexing SQUID readout. Bicep2 takes advantage of this design's higher focal-plane packing density, ease of fabrication, and multiplexing readout to field more detectors than Bicep1, improving mapping speed by nearly a factor of 10. Bicep2 was deployed to the South Pole in November 2009 with 500 polarization-sensitive detectors at 150 GHz, and is funded for two seasons of observation. The first months' data demonstrate the performance of the Caltech/JPL antenna-coupled TES arrays, and two years of observation with Bicep2 will achieve unprecedented sensitivity to B-modes on degree angular scales.

127. BLAST-pol: Balloon-borne Large Aperture Submillimeter Telescope for Polarimetery

Author: Thomas, N. E., Ade, Peter A. R., Angile, F. E., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. M., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, Lorenzo, Mrockowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Shariff, J. A., Soler, J. D., Truch, M. D. P., Tucker, Carole Elizabeth, Tucker, G. S., Ward-Thompson, Derek, Wiebe, D. V., Thomas, N. E., Ade, Peter A. R., Angile, F. E., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. M., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, Lorenzo, Mrockowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Shariff, J. A., Soler, J. D., Truch, M. D. P., Tucker, Carole Elizabeth, Tucker, G. S., Ward-Thompson, Derek, and Wiebe, D. V.
Abstract: BLAST-pol (Balloon-borne Large Aperture Submillimeter Telescope for Polarimetery) combines a 1.9 meter Cassegrain telescope and a submillimeter polarimeter that operates in three bands (250, 350, and 500 microns), each with 30% bandwidth. The detection system is comprised of 270 silicon-nitride micromesh bolometers distributed on three focal plane arrays with 30", 42", and 60" FWHM beam sizes, respectively. The detectors are a prototype for the SPIRE instrument used on Herschel. Polarization sensitivity is achieved by placing polarized grids on the bolometer arrays and with a rotatable Achromatic Half Wave Plate (AHWP) located in front of the arrays. The instrument operates on a balloon at an altitude of ~40km due to the high opacity of the earth’s sea level atmosphere at submillimeter wavelengths. The main scientific objective of BLAST-pol is to determine what role magnetic fields play in star formation. This is achieved by making large, high resolution, linear polarization maps of giant molecular clouds (GMCs), and their substructures. These maps can then be compared to maps created using numerical turbulence simulations to ascertain how magnetic fields affect the morphology and lifetime of these structures. The non-polarized version of BLAST has had two scientific flights and is scheduled to fly again as BLAST-pol in December 2010 from McMurdo, Antarctica.

128. BLAST-pol: The balloon-borne large aperture submillimeter telescope plus polarimeter

Author: Matthews, T., Ade, Peter A. R., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. D., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Macaluso, J., Moncelsi, Lorenzo, Mroczkowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Soler, J.D., Thomas, N. E., Truch, M. D. P., Tucker, Carole, Ward-Thompson, Derek, Wiebe, D. V., Matthews, T., Ade, Peter A. R., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. D., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Macaluso, J., Moncelsi, Lorenzo, Mroczkowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Soler, J.D., Thomas, N. E., Truch, M. D. P., Tucker, Carole, Ward-Thompson, Derek, and Wiebe, D. V.
Abstract: BLAST (The Balloon-borne Large Aperture Submillimeter Telescope) is a 1.9 meter telescope, that feeds a focal plane of 266 feedhorn-coupled bolometers at 250, 350 and 500 microns, with diffraction limited beam FWHM of 30 arcseconds at 250 microns. The experiment has been successfully flown from Sweden in 2005 and from Antarctica in 2006, as described in the poster by M. Truch and collaborators at this meeting. In this poster, we describe the upgrade that will add polarimetric capability to all three wavebands, thereby converting BLAST into BLAST-pol. Polarizing grids will be mounted in front of each of our detector arrays, and a 4 K rotating achromatic half-wave plate will be installed in the optical path, upstream from the cold pupil. BLAST-pol's primary science goal is to create deep, sensitive, large area maps of polarized dust emission in Galactic star forming clouds. For dozens of giant molecular clouds, we will produce three-color polarization maps covering the entire extent of each cloud, with sufficient resolution to probe into the dense cores. These data will provide an unprecedented view of the clouds' magnetic morphologies, the degree of order in the magnetic field, and the relationship to the filamentary structure that is commonly seen in these clouds. BLAST-pol will also measure high latitude polarized dust emission, the understanding of which is crucial for Cosmic Microwave Background Polarization experiments. BLAST-pol is currently under construction with a first flight planned for December 2009 from Antarctica.

129. Thermal architecture for the SPIDER flight cryostat

Author: Holland, Wayne S., Zmuidzinas, Jonas, Gudmundsson, J. E., Ade, Peter A. R., Amiri, M., Benton, S. J., Bihary, R., Bock, J. J., Bond, J. R., Bonetti, J. A., Bryan, S. A., Burger, B., Chiang, H. C., Contaldi, C. R., Crill, B. P., Dore, O., Farhang, M., Filippini, J., Fissel, L. M., Gandilo, N. N., Golwala, S. R., Halpern, M., Hasselfield, M., Hilton, G., Holmes, W., Hristov, V. V., Irwin, K. D., Jones, W. C., Kuo, C. L., MacTavish, C. J., Mason, P. V., Montroy, T. E., Morford, T. A., Netterfield, C. B., O'Dea, D. T., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Schenker, M. A., Shariff, J. A., Soler, J. D., Trangsrud, A., Tucker, Carole Elizabeth, Tucker, R. S., Turner, A. D., Holland, Wayne S., Zmuidzinas, Jonas, Gudmundsson, J. E., Ade, Peter A. R., Amiri, M., Benton, S. J., Bihary, R., Bock, J. J., Bond, J. R., Bonetti, J. A., Bryan, S. A., Burger, B., Chiang, H. C., Contaldi, C. R., Crill, B. P., Dore, O., Farhang, M., Filippini, J., Fissel, L. M., Gandilo, N. N., Golwala, S. R., Halpern, M., Hasselfield, M., Hilton, G., Holmes, W., Hristov, V. V., Irwin, K. D., Jones, W. C., Kuo, C. L., MacTavish, C. J., Mason, P. V., Montroy, T. E., Morford, T. A., Netterfield, C. B., O'Dea, D. T., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Schenker, M. A., Shariff, J. A., Soler, J. D., Trangsrud, A., Tucker, Carole Elizabeth, Tucker, R. S., and Turner, A. D.
Abstract: We describe the cryogenic system for SPIDER, a balloon-borne microwave polarimeter that will map 8% of the sky with degree-scale angular resolution. The system consists of a 1284 L liquid helium cryostat and a 16 L capillary-filled superfluid helium tank, which provide base operating temperatures of 4 K and 1.5 K, respectively. Closed-cycle 3He adsorption refrigerators supply sub-Kelvin cooling power to multiple focal planes, which are housed in monochromatic telescope inserts. The main helium tank is suspended inside the vacuum vessel with thermally insulating fiberglass flexures, and shielded from thermal radiation by a combination of two vapor cooled shields and multi-layer insulation. This system allows for an extremely low instrumental background and a hold time in excess of 25 days. The total mass of the cryogenic system, including cryogens, is approximately 1000 kg. This enables conventional long duration balloon flights. We will discuss the design, thermal analysis, and qualification of the cryogenic system.

130. SPIDER: a balloon-borne CMB polarimeter for large angular scales

Author: Holland, Wayne S, Zmuidzinas, Jonas, Filippini, J. P., Ade, Peter A. R., Amiri, M., Benton, S. J., Bihary, R., Bock, J. J., Bond, J. R., Bonetti, J. A., Bryan, S. A., Burger, B., Chiang, H. C., Contaldi, C. R., Crill, B. P., Dore, O., Farhang, M., Fissel, L. M., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G., Holmes, W., Hristov, V. V., Irwin, K. D., Jones, W. C., Kuo, C. L., MacTavish, C. J., Mason, P. V., Montroy, T. E., Morford, T. A., Netterfield, C. B., O'Dea, D. T., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Schenker, M. A., Shariff, J. A., Soler, J. D., Trangsrud, A., Tucker, Carole Elizabeth, Tucker, R. S., Turner, A. D., Holland, Wayne S, Zmuidzinas, Jonas, Filippini, J. P., Ade, Peter A. R., Amiri, M., Benton, S. J., Bihary, R., Bock, J. J., Bond, J. R., Bonetti, J. A., Bryan, S. A., Burger, B., Chiang, H. C., Contaldi, C. R., Crill, B. P., Dore, O., Farhang, M., Fissel, L. M., Gandilo, N. N., Golwala, S. R., Gudmundsson, J. E., Halpern, M., Hasselfield, M., Hilton, G., Holmes, W., Hristov, V. V., Irwin, K. D., Jones, W. C., Kuo, C. L., MacTavish, C. J., Mason, P. V., Montroy, T. E., Morford, T. A., Netterfield, C. B., O'Dea, D. T., Rahlin, A. S., Reintsema, C. D., Ruhl, J. E., Runyan, M. C., Schenker, M. A., Shariff, J. A., Soler, J. D., Trangsrud, A., Tucker, Carole Elizabeth, Tucker, R. S., and Turner, A. D.
Abstract: We describe SPIDER, a balloon-borne instrument to map the polarization of the millimeter-wave sky with degree angular resolution. Spider consists of six monochromatic refracting telescopes, each illuminating a focal plane of large-format antenna-coupled bolometer arrays. A total of 2,624 superconducting transition-edge sensors are distributed among three observing bands centered at 90, 150, and 280 GHz. A cold half-wave plate at the aperture of each telescope modulates the polarization of incoming light to control systematics. SPIDER's first flight will be a 20-30-day Antarctic balloon campaign in December 2011. This flight will map ~8% of the sky to achieve unprecedented sensitivity to the polarization signature of the gravitational wave background predicted by inflationary cosmology. The SPIDER mission will also serve as a proving ground for these detector technologies in preparation for a future satellite mission.

131. BLAST-pol: The balloon-borne large aperture submillimeter telescope plus polarimeter

Author: Matthews, T., Ade, Peter A. R., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. D., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Macaluso, J., Moncelsi, Lorenzo, Mroczkowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Soler, J.D., Thomas, N. E., Truch, M. D. P., Tucker, Carole, Ward-Thompson, Derek, Wiebe, D. V., Matthews, T., Ade, Peter A. R., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. D., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Macaluso, J., Moncelsi, Lorenzo, Mroczkowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Soler, J.D., Thomas, N. E., Truch, M. D. P., Tucker, Carole, Ward-Thompson, Derek, and Wiebe, D. V.
Abstract: BLAST (The Balloon-borne Large Aperture Submillimeter Telescope) is a 1.9 meter telescope, that feeds a focal plane of 266 feedhorn-coupled bolometers at 250, 350 and 500 microns, with diffraction limited beam FWHM of 30 arcseconds at 250 microns. The experiment has been successfully flown from Sweden in 2005 and from Antarctica in 2006, as described in the poster by M. Truch and collaborators at this meeting. In this poster, we describe the upgrade that will add polarimetric capability to all three wavebands, thereby converting BLAST into BLAST-pol. Polarizing grids will be mounted in front of each of our detector arrays, and a 4 K rotating achromatic half-wave plate will be installed in the optical path, upstream from the cold pupil. BLAST-pol's primary science goal is to create deep, sensitive, large area maps of polarized dust emission in Galactic star forming clouds. For dozens of giant molecular clouds, we will produce three-color polarization maps covering the entire extent of each cloud, with sufficient resolution to probe into the dense cores. These data will provide an unprecedented view of the clouds' magnetic morphologies, the degree of order in the magnetic field, and the relationship to the filamentary structure that is commonly seen in these clouds. BLAST-pol will also measure high latitude polarized dust emission, the understanding of which is crucial for Cosmic Microwave Background Polarization experiments. BLAST-pol is currently under construction with a first flight planned for December 2009 from Antarctica.

132. BLAST-pol: Balloon-borne Large Aperture Submillimeter Telescope for Polarimetery

Author: Thomas, N. E., Ade, Peter A. R., Angile, F. E., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. M., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, Lorenzo, Mrockowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Shariff, J. A., Soler, J. D., Truch, M. D. P., Tucker, Carole Elizabeth, Tucker, G. S., Ward-Thompson, Derek, Wiebe, D. V., Thomas, N. E., Ade, Peter A. R., Angile, F. E., Benton, S. J., Chapin, E. L., Devlin, M. J., Fissel, L. M., Gandilo, N. N., Gundersen, J. O., Hargrave, Peter Charles, Hughes, D. H., Klein, J., Korotkov, A. L., Matthews, T. G., Moncelsi, Lorenzo, Mrockowski, T., Netterfield, C. B., Novak, G., Olmi, L., Pascale, Enzo, Savini, Giorgio, Scott, D., Shariff, J. A., Soler, J. D., Truch, M. D. P., Tucker, Carole Elizabeth, Tucker, G. S., Ward-Thompson, Derek, and Wiebe, D. V.
Abstract: BLAST-pol (Balloon-borne Large Aperture Submillimeter Telescope for Polarimetery) combines a 1.9 meter Cassegrain telescope and a submillimeter polarimeter that operates in three bands (250, 350, and 500 microns), each with 30% bandwidth. The detection system is comprised of 270 silicon-nitride micromesh bolometers distributed on three focal plane arrays with 30", 42", and 60" FWHM beam sizes, respectively. The detectors are a prototype for the SPIRE instrument used on Herschel. Polarization sensitivity is achieved by placing polarized grids on the bolometer arrays and with a rotatable Achromatic Half Wave Plate (AHWP) located in front of the arrays. The instrument operates on a balloon at an altitude of ~40km due to the high opacity of the earth’s sea level atmosphere at submillimeter wavelengths. The main scientific objective of BLAST-pol is to determine what role magnetic fields play in star formation. This is achieved by making large, high resolution, linear polarization maps of giant molecular clouds (GMCs), and their substructures. These maps can then be compared to maps created using numerical turbulence simulations to ascertain how magnetic fields affect the morphology and lifetime of these structures. The non-polarized version of BLAST has had two scientific flights and is scheduled to fly again as BLAST-pol in December 2010 from McMurdo, Antarctica.

133. BICEP Array: a multi-frequency degree-scale CMB polarimeter

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, Hui, Howard, Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Bowens-Rubin, R., Brevik, J. A., Buder, I., Bullock, E., Buza, V., Connors, J., Cornelison, J., Crill, B. P., Crumrine, M., Dierickx, M., Duband, L., Dvorkin, C., Filippini, J. P., Fliescher, S., Grayson, J., Hall, G., Halpern, M., Harrison, S., Hildebrandt, S. R., Hilton, G. C., Irwin, K. D., Kang, J., Karkare, K. S., Karpel, E., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C.-L., Lau, K., Larsen, N. A., Leitch, E. M., Lueker, M., Megerian, K. G., Moncelsi, L., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Palladino, S., Pryke, C., Racine, B., Richter, S., Schwarz, R., Schillaci, A., Sheehy, C. D., Soliman, A., St. Germaine, T., Staniszewski, Z. K., Steinbach, B., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Umiltà, C., Vieregg, A. G., Wandui, A., Weber, A. C., Wiebe, D. V., Willmert, J., Wong, C. L., Wu, W. L. K., Yang, E., Yoon, K. W., and Zhang, C.
Published: 2018
Full Text: View/download PDF

134. Optical characterization of the BICEP3 CMB polarimeter at the South Pole

Author: Holland, Wayne S., Zmuidzinas, Jonas, Karkare, K. S., Ade, P. A. R., Ahmed, Z., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Boenish, H., Bowens-Rubin, R., Buder, I., Bullock, E., Buza, V., Connors, J., Filippini, J. P., Fliescher, S. T., Grayson, J. A., Halpern, M., Harrison, S. A., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Kang, J. H., Karpel, E., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Megerian, K. G., Monticue, V., Namikawa, T., Netterfield, C. B., Nguyen, H. T., O'Brient, R., Ogburn, R. W., Pryke, C. L., Reintsema, C. D., Richter, S., St. Germaine, M. T., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Steinbach, B., Teply, G. P., Thompson, K. L., Tolan, J. E., Tucker, C., Turner, A. D., Vieregg, A. G., Wandui, A., Weber, A., Willmert, J., Wong, C. L., Wu, W. L. K., and Yoon, K. W.
Published: 2016
Full Text: View/download PDF

135. IFPA Meeting 2011 workshop report I: Placenta: Predicting future health; roles of lipids in the growth and development of feto-placental unit; placental nutrient sensing; placental research to solve clinical problems--a translational approach.

Author: Acharya, G, Albrecht, C, Benton, S J, Cotechini, T, Dechend, R, Dilworth, M R, Duttaroy, A K, Grotmol, T, Heazell, A E, Jansson, T, Johnstone, E D, Jones, H N, Jones, R L, Lager, S, Laine, K, Nagirnaja, L, Nystad, M, Powell, T, Redman, C, and Sadovsky, Y
Published: 2012

136. Pre-flight integration and characterization of the SPIDER balloon-borne telescope

Author: Holland, Wayne S., Zmuidzinas, Jonas, Rahlin, A. S., Ade, P. A. R., Amiri, M., Benton, S. J., Bock, J. J., Bond, J. R., Bryan, S. A., Chiang, Hsin C., Contaldi, C. R., Crill, B. P., Doré, O., Farhang, M., Filippini, J. P., Fissel, L. M., Fraisse, A. A., Gambrel, A. E., Gandilo, N. N., Golwala, S., Gudmundsson, Jon E., Halpern, M., Hasselfield, M. F., Hilton, G., Holmes, W. A., Hristov, V. V., Irwin, K. D., Jones, William C., Kermish, Zigmund D., Kuo, C. L., MacTavish, C. J., Mason, P. V., Megerian, K., Moncelsi, L., Morford, T. A., Nagy, J. M., Netterfield, C. B., O'Brient, R., Reintsema, C., Ruhl, J. E., Runyan, M. C., Shariff, J. A., Soler, J. D., Trangsrud, A., Tucker, C., Tucker, R. S., Turner, A. D., Weber, A. C., Wiebe, D. V., and Young, E. Y.
Published: 2014
Full Text: View/download PDF

137. BICEP2 and Keck array: upgrades and improved beam characterization

Author: Holland, Wayne S., Zmuidzinas, Jonas, Buder, I., Ade, P. A. R., Ahmed, Z., Aikin, R. W., Alexander, K. D., Amiri, M., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Bonetti, J. A., Brevik, J. A., Bullock, E., Burger, B., Crill, B. P., Davis, G., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Gordon, M. S., Halpern, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hristov, V. V., Hui, H., Irwin, K. D., Karkare, K. S., Kaufman, J. P., Keating, B. G., Kefeli, S., Kernasovskiy, S. A., Kovac, J. M., Kuo, C. L., Leitch, E. M., Lueker, M., Mason, P., Megerian, K. G., Netterfield, C. B., Nguyen, H. T., O’Brient, R., Ogburn, R. W., Orlando, A., Pryke, C., Reintsema, C. D., Richter, S., Schwarz, R., Sheehy, C. D., Staniszewski, Z. K., Sudiwala, R. V., Teply, G. P., Thompson, K. L., Tolan, J. E., Turner, A. D., Vieregg, A. G., Weber, A. C., Wiebe, D. V., Wilson, P., Wong, C. L., and Yoon, K. W.
Published: 2014
Full Text: View/download PDF

138. Detection of B-Mode Polarization at Degree Angular Scales by BICEP2.

Author: Ade, P. A. R., Aikin, R. W., Barkats, D., Benton, S. J., Bischoff, C. A., Bock, J. J., Brevik, J. A., Buder, I., Bullock, E., Dowell, C. D., Duband, L., Filippini, J. P., Fliescher, S., Golwala, S. R., Halpem, M., Hasselfield, M., Hildebrandt, S. R., Hilton, G. C., Hristov, V. V., and Irwin, K. D.
Subjects: *COSMIC background radiation, *POLARISCOPE, *GRAVITATIONAL waves, *BOLOMETERS, *DETECTORS
Abstract: We report results from the BICEP2 experiment, a cosmic microwave background (CMB) polarimeter specifically designed to search for the signal of inflationary gravitational waves in the B-mode power spectrum around l ∼ 80. The telescope comprised a 26 cm aperture all-cold refracting optical system equipped with a focal plane of 512 antenna coupled transition edge sensor 150 GHz bolometers each with temperature sensitivity of ≈300 μKCMB √s . BICEP2 observed from the South Pole for three seasons from 2010 to 2012. A low-foreground region of sky with an effective area of 380 square deg was observed to a depth of 87 nK deg in Stokes Q and U. In this paper we describe the observations, data reduction, maps, simulations, and results. We find an excess of B-mode power over the base lensed-ACDM expectation in the range 30 < l < 150, inconsistent with the null hypothesis at a significance of > 5σ. Through jackknife tests and simulations based on detailed calibration measurements we show that systematic contamination is much smaller than the observed excess. Cross correlating against WMAP 23 GHz maps we find that Galactic synchrotron makes a negligible contribution to the observed signal. We also examine a number of available models of polarized dust emission and find that at their default parameter values they predict power ∼(5-10)× smaller than the observed excess signal (with no significant cross-correlation with our maps). However, these models are not sufficiently constrained by external public data to exclude the possibility of dust emission bright enough to explain the entire excess signal. Cross correlating BICEP2 against 100 GHz maps from the BICEP1 experiment, the excess signal is confirmed with 3σ significance and its spectral index is found to be consistent with that of the CMB, disfavoring dust at 1.7σ. The observed B-mode power spectrum is well fit by a lensed-ACDM + tensor theoretical model with tensor-to-scalar ratio r = 0.20+0.07-0.05, with r = 0 disfavored at 7.0σ. Accounting for the contribution of foreground, dust will shift this value downward by an amount which will be better constrained with upcoming data sets. [ABSTRACT FROM AUTHOR]
Published: 2014
Full Text: View/download PDF

139. Joint analysis of BICEP2/Keck array and planck data

Author: K. Ganga, N. Krachmalnicoff, Olivier Doré, W. A. Holmes, M. Lueker, Jose M. Diego, A. Mennella, Nabila Aghanim, Ben Rusholme, F. Elsner, Reijo Keskitalo, C. L. Wong, L. Toffolatti, H. T. Nguyen, J. Jewell, Federico Nati, Valeria Pettorino, Davide Maino, S. J. Benton, Anthony Lasenby, Jacques Delabrouille, Luca Terenzi, C. Combet, F. Piacentini, Simon D. M. White, J. A. Murphy, J. E. Tolan, W. Hovest, Cora Dvorkin, Fabio Finelli, R. Schwarz, M. Frailis, P. B. Lilje, Carlo Baccigalupi, James G. Bartlett, A. Mangilli, Jussi-Pekka Väliviita, F. Pasian, Alessandro Gruppuso, Sunil Golwala, E. Bullock, Guilaine Lagache, François Levrier, E. Hivon, E. Keihänen, M. Rowan-Robinson, G. Patanchon, F. Couchot, L. P. L. Colombo, Dmitry Novikov, Jake Connors, Antony Lewis, M. Tomasi, M. López-Caniego, George Helou, François R. Bouchet, L. A. Wade, Daniela Paoletti, Dipak Munshi, George Efstathiou, Jean-François Cardoso, Ingunn Kathrine Wehus, Marco Bersanelli, J.-F. Sygnet, E. Martínez-González, Etienne Pointecouteau, Charles R. Lawrence, A. D. Turner, J. Aumont, D. Herranz, R. W. Ogburn, J.-M. Lamarre, M. Tucci, Rafael Rebolo, A. C. Weber, Kevin M. Huffenberger, D. Yvon, Roger O'Brient, M. Piat, O. Perdereau, Alain Benoit, Planck Collaborations, Luca Valenziano, Massimiliano Lattanzi, Mark Halpern, Zeeshan Ahmed, S. R. Hildebrandt, E. M. Leitch, A. de Rosa, R. Sudiwala, Mika Juvela, C. Renault, Kate D. Alexander, N. Ponthieu, Alessandro Melchiorri, D. Santos, Hannu Kurki-Suonio, A. Ducout, Stéphane Plaszczynski, Marian Douspis, Daniel J. Mortlock, Fabrizio Villa, Luigi Danese, C. D. Sheehy, Carlo Burigana, G. Hurier, C. Pryke, M. Rossetti, Olivier Forni, L. Montier, M. Tristram, K. L. Thompson, Davide Pietrobon, Lloyd Knox, M.-A. Miville-Deschênes, R. Kneissl, Jörg P. Rachen, Pavel Naselsky, Colin A. Bischoff, R. J. Davis, Locke D. Spencer, Silvia Masi, Andrea Zacchei, W. C. Jones, Bicep, Michael Seiffert, G. Polenta, M. Linden-Vørnle, Duncan Hanson, R. C. Butler, Theodore Kisner, L. Perotto, F. K. Hansen, Bruce Partridge, F. Boulanger, J.-P. Bernard, William T. Reach, F. Noviello, D. L. Harrison, S. Donzelli, A. Renzi, J.-M. Delouis, J.-L. Puget, G. Roudier, Michele Liguori, A. Curto, S. Fliescher, J. F. Macías-Pérez, M. Maris, V. Stolyarov, H. K. Eriksen, Bruno Maffei, E. Franceschi, Benjamin D. Wandelt, Julian Borrill, Jeffrey P. Filippini, R. B. Barreiro, Calvin B. Netterfield, Graca Rocha, Roberta Paladini, T. J. Pearson, P. Vielva, S. Richter, Viktor Hristov, Grant Teply, L. Duband, Giorgio Savini, Michael P. Hobson, F. Pajot, Martin Kunz, A. Catalano, Laura Bonavera, R. A. Sunyaev, A. A. Fraisse, Justus A. Brevik, Mathieu Remazeilles, D. Sutton, Erminia Calabrese, Howard Hui, C. D. Dowell, Anne Lähteenmäki, Ranga-Ram Chary, J. Willmert, Anthony Challinor, M. Sandri, Jon E. Gudmundsson, L. Pagano, Robert A. Watson, L. Mendes, Sabino Matarrese, Victor Buza, A. Karakci, N. Mandolesi, K. G. Megerian, S. Galeotta, J. Knoche, Andrew H. Jaffe, A. Moneti, Simon Prunet, Gene C. Hilton, I. D. Novikov, I. Buder, Philip Lubin, S. A. Kernasovskiy, Peter G. Martin, P. Bielewicz, Jo Dunkley, H. Dole, Subhabrata Mitra, J. A. Tauber, M. Savelainen, L. Vibert, X. Dupac, Brian Keating, Adam Moss, P. de Bernardis, R. D. Davies, Denis Barkats, M. Reinecke, Peter Mason, K. Benabed, Nicola Bartolo, A.-S. Suur-Uski, Martin White, M. Bucher, Douglas Scott, Z. K. Staniszewski, J. R. Bond, E. Gjerløw, Andrea Zonca, Clive Dickinson, Krzysztof M. Gorski, A. Gregorio, H. C. Chiang, P. R. Christensen, E. Battaner, Chao-Lin Kuo, F. Cuttaia, Torsten A. Enßlin, James J. Bock, I. Ristorcelli, Anna Bonaldi, E. Falgarone, Monique Arnaud, Peter Meinhold, Serge Gratton, S. Kefeli, F.-X. Désert, J. González-Nuevo, J. P. Kaufman, Tuhin Ghosh, B. Van Tent, Hans Ulrik Nørgaard-Nielsen, A. J. Banday, Sophie Henrot-Versille, Paolo Natoli, John M Kovac, Kirit Karkare, A. Coulais, Kent D. Irwin, Jose Alberto Rubino-Martin, G. de Zotti, Ki Won Yoon, A. Benoit-Lévy, M. Giard, B. P. Crill, A. Frejsel, Matthew Hasselfield, T. R. Jaffe, M. Migliaccio, Peter A. R. Ade, Abigail G. Vieregg, Randol W. Aikin, R. Leonardi, A. Orlando, S. Galli, G. W. Pratt, Gianluca Morgante, 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), Département d'Astrophysique (ex SAP) (DAP), 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, Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies (SISSA / ISAS), Joint ALMA Observatory (JAO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), 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), 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), INO-CNR BEC Center and Dipartimento di Fisica, Università degli Studi di Trento (UNITN), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), 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 für Planetologie [Münster], Westfälische Wilhelms-Universität Münster (WWU), ONERA - The French Aerospace Lab [Châtillon], ONERA-Université Paris Saclay (COmUE), SCANCO Medical AG, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), 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), Institute for Climate and Atmospheric Science [Leeds] (ICAS), School of Earth and Environment [Leeds] (SEE), University of Leeds-University of Leeds, Dipartimento di Ingegneria Meccanica-Settore Materiali, Universita degli Studi di Padova, Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Dipartimento di Fisica, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], AUTRES, 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), Centre d'étude spatiale des rayonnements (CESR), 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, Laboratoire de Génie Electrique de Grenoble (G2ELab), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Agence nationale de sécurité sanitaire de l'alimentation, de l'environnement et du travail (ANSES), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [Vancouver], University of British Columbia (UBC), National Center for Atmospheric Research [Boulder] (NCAR), Queens Med Res Inst, Div Pathol, Univ Edinburgh, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, International Center for Relativistic Astrophysics (ICRA), Università degli Studi di Roma, School of Physics and Astronomy, University of Manchester [Manchester], Laboratory for Experimental Medicine and Endocrinology, Catholic University of Leuven (LEGENDO), Université Catholique de Louvain = Catholic University of Louvain (UCL), Dipartimento di Fisica, Universita` di Roma Tor Vergata, Università degli Studi di Roma Tor Vergata [Roma], Istituto Nazionale di Fisica Nucleare, Sezione di Padova (INFN, Sezione di Padova), Istituto Nazionale di Fisica Nucleare (INFN), Astrophysics Group, Blackett Laboratory, Imperial College London-Imperial College London, School of Social and Community Medicine [Bristol], University of Bristol [Bristol], Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), National High Magnetic Field Laboratory (NHMFL), Florida State University [Tallahassee] (FSU), Département de Physique des Particules (ex SPP) (DPP), BICEPS2/Keck Array, Planck, Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, R, P, Aghanim, N, Ahmed, Z, Aikin, R, Alexander, K, Arnaud, M, Aumont, J, Baccigalupi, C, Banday, A, Barkats, D, Barreiro, R, Bartlett, J, Bartolo, N, Battaner, E, Benabed, K, Benoit, A, Benoit Levy, A, Benton, S, Bernard, J, Bersanelli, M, Bielewicz, P, Bischoff, C, Bock, J, Bonaldi, A, Bonavera, L, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Brevik, J, Bucher, M, Buder, I, Bullock, E, Burigana, C, Butler, R, Buza, V, Calabrese, E, Cardoso, J, Catalano, A, Challinor, A, Chary, R, Chiang, H, Christensen, P, L, ., Combet, C, Connors, J, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, Rosa, A, Zotti, G, Delabrouille, J, Delouis, J, Desert, F, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Dore, O, Douspis, M, Dowell, C, Duband, L, Ducout, A, Dunkley, J, Dupac, X, Dvorkin, C, Efstathiou, G, Elsner, F, Ensslin, T, Eriksen, H, Falgarone, E, Filippini, J, Finelli, F, Fliescher, S, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Gjerlow, E, Golwala, S, Gonzalez Nuevo, J, Gorski, K, Gratton, S, Gregorio, A, Gruppuso, A, Gudmundsson, J, Halpern, M, Hansen, F, Hanson, D, Harrison, D, Hasselfield, M, Helou, G, Henrot Versillee, S, Herranz, D, Hildebrandt, S, Hilton, G, Hivon, E, Hobson, M, Holmes, W, Hovest, W, Hristov, V, Huffenberger, K, Hui, H, Hurier, G, Irwin, K, Jaffe, A, Jaffe, T, Jewell, J, Jones, W, Juvela, M, Karakci, A, Karkare, K, Kaufman, J, Keating, B, Kefeli, S, Keihanen, E, Kernasovskiy, S, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kovac, J, Krachmalnicoff, N, Kunz, M, Kuo, C, Kurki Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Lattanzi, M, Lawrence, C, Leitch, E, Leonardi, R, Levrier, F, Lewis, A, Liguori, M, Lilje, P, Linden Vornle, M, Lopez Caniego, M, Lubin, P, Lueker, M, Macias Perez, J, Maffei, B, Maino, D, Mandolesi, N, Mangilli, A, Maris, M, Martin, P, Martinez Gonzalez, E, Masi, S, Mason, P, Matarrese, S, Megerian, K, Meinhold, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Moss, A, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nguyen, H, Norgaard Nielsen, H, Noviello, F, Novikov, D, Novikov, I, O'Brient, R, Ogburn, R, Orlando, A, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Pearson, T, Perdereau, O, Perotto, L, Pettorino, V, Piacentini, F, Piat, M, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Pratt, G, Prunet, S, Pryke, C, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Renzi, A, Richter, S, Ristorcelli, I, Rocha, G, Rossetti, M, Roudier, G, Rowan Robinson, M, Rubino Martin, J, Rusholme, B, Sandri, M, Santos, D, Savelainen, M, Savini, G, Schwarz, R, Scott, D, Seiffert, M, Sheehy, C, Spencer, L, Staniszewski, Z, Stolyarov, V, Sudiwala, R, Sunyaev, R, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Teply, G, Terenzi, L, Thompson, K, Toffolatti, L, Tolan, J, Tomasi, M, Tristram, M, Tucci, M, Turner, A, Valenziano, L, Valiviita, J, Tent, B, Vibert, L, Vielva, P, Vieregg, A, Villa, F, Wade, L, Wandelt, B, Watson, R, Weber, A, Wehus, I, White, M, M, S, Willmert, J, Wong, C, Yoon, K, Yvon, D, Zacchei, A, Zonca, A, Bicep, K, Planck, C, 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 ), Département d'Astrophysique (ex SAP) ( DAP ), 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, Scuola Internazionale Superiore di Studi Avanzati / International School for Advanced Studies ( SISSA / ISAS ), Joint ALMA Observatory, Physique Corpusculaire et Cosmologie - Collège de France ( PCC ), Collège de France ( CdF ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Università di Trento, 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 ), HELFA - Hélium : du fondamental aux applications, Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes [Saint Martin d'Hères]-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 ), Westfälische Wilhelms-Universität Münster ( WWU ), 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 ), ONERA - The French Aerospace Lab ( Chatillon ), ONERA, 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 ), Institute for Climate and Atmospheric Science [Leeds] ( ICAS ), University of Leeds, Universita degli Studi di Padova = University of Padua = Université de Padoue, 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 ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), Università degli Studi di Roma 'La Sapienza' [Rome], APC - Gravitation ( APC-Gravitation ), 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 ) -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 ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, Laboratoire des Cryoréfrigérateurs et Cryogénie Spatiale ( LCCS ), Service des Basses Températures ( SBT - UMR 9004 ), Institut Nanosciences et Cryogénie ( INAC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ) -Institut Nanosciences et Cryogénie ( INAC ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Grenoble Alpes ( UGA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Génie Electrique de Grenoble ( G2ELab ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut polytechnique de Grenoble - Grenoble Institute of Technology ( Grenoble INP ) -Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique ( CNRS ) -Université Grenoble Alpes ( UGA ), Agence Nationale de Sécurité Sanitaire de l’Alimentation, de l’Environnement et du Travail ( ANSES Maisons-Alfort ), APC - Cosmologie, Collège de France ( CdF ) -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 ) -Collège de France ( CdF ) -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 ) -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 ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire de Paris-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna ( IASF-Bo ), Istituto Nazionale di Astrofisica ( INAF ), Department of Physics and Astronomy, University of British Columbia ( UBC ), National Center for Atmospheric Research [Boulder] ( NCAR ), Infrared Processing and Analysis Center ( IPAC ), California Institute of Technology ( CALTECH ), Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies ( FEMTO-ST ), Université de Technologie de Belfort-Montbeliard ( UTBM ) -Ecole Nationale Supérieure de Mécanique et des Microtechniques ( ENSMM ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Max-Planck-Institut für Astronomie ( MPIA ), International Center for Relativistic Astrophysics ( ICRA ), Laboratory for Experimental Medicine and Endocrinology, Catholic University of Leuven ( LEGENDO ), Université Catholique de Louvain ( UCL ), Università degli studi di Roma II, Istituto Nazionale di Fisica Nucleare, Sezione di Padova ( INFN, Sezione di Padova ), National Institute for Nuclear Physics ( INFN ), Antarctic Research a European Network for Astrophysics ( ARENA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -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 ), National High Magnetic Field Laboratory ( NHMFL ), Florida State University, Département de Physique des Particules (ex SPP) ( DPP ), National Science Foundation (US), European Research Council, Ministerio de Economía y Competitividad (España), Junta de Andalucía, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), 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), Westfälische Wilhelms-Universität Münster = University of Münster (WWU), DAAA, ONERA, Université Paris-Saclay [Châtillon], ONERA-Université Paris-Saclay, 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 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), LERMA Cergy (LERMA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), 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), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), School of Physics and Astronomy [Manchester], Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), 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), Département de Physique des Particules (ex SPP) (DPhP), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), 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), Université Grenoble Alpes (UGA)-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 Grenoble Alpes (UGA)-Institut de Recherche Interdisciplinaire de Grenoble (IRIG), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Université Catholique de Louvain (UCL), National Institute for Nuclear Physics (INFN), 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), Ade, P. A. R., Aghanim, N., Ahmed, Z., Aikin, R. W., Alexander, K. D., Arnaud, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barkats, D., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Benton, S. J., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bischoff, C. A., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Brevik, J. A., Bucher, M., Buder, I., Bullock, E., Burigana, C., Butler, R. C., Buza, V., Calabrese, E., Cardoso, J. F., Catalano, A., Challinor, A., Chary, R. R., Chiang, H. C., Christensen, P. R., Colombo, L. P. L., Combet, C., Connors, J., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dowell, C. D., Duband, L., Ducout, A., Dunkley, J., Dupac, X., Dvorkin, C., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Filippini, J. P., Finelli, F., Fliescher, S., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., Golwala, S. R., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Gudmundsson, J. E., Halpern, M., Hansen, F. K., Hanson, D., Harrison, D. L., Hasselfield, M., Helou, G., Henrot Versillé, S., Herranz, D., Hildebrandt, S. R., Hilton, G. C., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hristov, V. V., Huffenberger, K. M., Hui, H., Hurier, G., Irwin, K. D., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Karakci, A., Karkare, K. S., Kaufman, J. P., Keating, B. G., Kefeli, S., Keihänen, E., Kernasovskiy, S. A., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kovac, J. M., Krachmalnicoff, N., Kunz, M., Kuo, C. L., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leitch, E. M., Leonardi, R., Levrier, F., Lewis, A., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Lueker, M., Macías Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez González, E., Masi, S., Mason, P., Matarrese, S., Megerian, K. G., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nguyen, H. T., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Brient, R., Ogburn, R. W., Orlando, A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Pratt, G. W., Prunet, S., Pryke, C., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Richter, S., Ristorcelli, I., Rocha, G., Rossetti, M., Roudier, G., Rowan Robinson, M., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Schwarz, R., Scott, D., Seiffert, M. D., Sheehy, C. D., Spencer, L. D., Staniszewski, Z. K., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Teply, G. P., Terenzi, L., Thompson, K. L., Toffolatti, L., Tolan, J. E., Tomasi, M., Tristram, M., Tucci, M., Turner, A. D., Valenziano, L., Valiviita, J., Van Tent, B., Vibert, L., Vielva, P., Vieregg, A. G., Villa, F., Wade, L. A., Wandelt, B. D., Watson, R., Weber, A. C., Wehus, I. K., White, M., White, S. D. M., Willmert, J., Wong, C. L., Yoon, K. W., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Observational cosmology, High Energy Physics - Theory, Background radiations, Gravitational wave detectors and experiments, Astronomy, General Physics and Astronomy, ComputingMilieux_LEGALASPECTSOFCOMPUTING, Astrophysics, 01 natural sciences, Spectral line, General Relativity and Quantum Cosmology, law.invention, High Energy Physics - Phenomenology (hep-ph), law, Spectral behaviors, probe wmap observations gravity-waves polarization anisotropy emission submillimeter spectrum scaledust Physics, 010303 astronomy & astrophysics, QC, ComputingMilieux_MISCELLANEOUS, media_common, QB, Physics, Power-spectra, Lower frequencies, ta213, CDM modeling, Cross correlations, Dust emission, Joint analysis, Model variation, Polarization (waves), Synchrotron, High Energy Physics - Phenomenology, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, ta221, Cosmic background radiation, ta1171, Radio microwave, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, [ PHYS.ASTR.CO ] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Physics and Astronomy (all), Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Planck, ta216, Astrophysics::Galaxy Astrophysics, ta115, ta114, 010308 nuclear & particles physics, Gravitational wave, High Energy Physics - Theory (hep-th), Sky, [SDU]Sciences of the Universe [physics], Data_GENERAL
Abstract: We report the results of a joint analysis of data from BICEP2/Keck Array and Planck. BICEP2 and Keck Array have observed the same approximately 400 deg2 patch of sky centered on RA 0 h, Dec. −57.5°. The combined maps reach a depth of 57 nK deg in Stokes Q and U in a band centered at 150 GHz. Planck has observed the full sky in polarization at seven frequencies from 30 to 353 GHz, but much less deeply in any given region (1.2 μK deg in Q and U at 143 GHz). We detect 150×353 cross-correlation in B modes at high significance. We fit the single- and cross-frequency power spectra at frequencies ≥150 GHz to a lensed-ΛCDM model that includes dust and a possible contribution from inflationary gravitational waves (as parametrized by the tensor-to-scalar ratio r), using a prior on the frequency spectral behavior of polarized dust emission from previous Planck analysis of other regions of the sky. We find strong evidence for dust and no statistically significant evidence for tensor modes. We probe various model variations and extensions, including adding a synchrotron component in combination with lower frequency data, and find that these make little difference to the r constraint. Finally, we present an alternative analysis which is similar to a map-based cleaning of the dust contribution, and show that this gives similar constraints. The final result is expressed as a likelihood curve for r, and yields an upper limit r0.05, National Science Foundation (NSF) ANT-0742818 ANT-1044978 ANT-0742592 ANT-1110087, JPL Research and Technology Development Fund from the NASA 06-ARPA206-0040 10-SAT10-0017, National Science Foundation (NSF) ANT-1145172 ANT-1145143 ANT-1145248, Keck Foundation (Caltech), European Space Agency, Centre National D'etudes Spatiales, CNRS/INSU-IN2P3-INP (France), Italian Space Agency (ASI), Italian National Research Council, Istituto Nazionale Astrofisica (INAF), National Aeronautics & Space Administration (NASA), United States Department of Energy (DOE), Science & Technology Facilities Council (STFC), UKSA (UK), Consejo Superior de Investigaciones Cientificas (CSIC), MINECO (Spain), JA (Spain), RES (Spain), Finnish Funding Agency for Technology & Innovation (TEKES), AoF (Finland), CSC (Finland), Helmholtz Association, German Aerospace Centre (DLR), Max Planck Society, CSA (Canada), DTU Space (Denmark), SER/SSO (Switzerland), RCN (Norway), Science Foundation Ireland, Portuguese Foundation for Science and Technology, ERC (EU), European Union (EU), Science & Technology Facilities Council (STFC) ST/K00106X/1 ST/K001051/1 ST/K002805/1 ST/L000768/1 ST/K004131/1 ST/N001206/1 ST/K000985/1 ST/L000636/1 ST/K003674/1 ST/M007685/1 ST/L000393/1 ST/L000652/1, Villum Fonden 10056
Published: 2015

140. Constraints on Primordial Gravitational Waves Using Planck, WMAP, and New BICEP2/Keck Observations through the 2015 Season.

Author: Ade PAR, Ahmed Z, Aikin RW, Alexander KD, Barkats D, Benton SJ, Bischoff CA, Bock JJ, Bowens-Rubin R, Brevik JA, Buder I, Bullock E, Buza V, Connors J, Cornelison J, Crill BP, Crumrine M, Dierickx M, Duband L, Dvorkin C, Filippini JP, Fliescher S, Grayson J, Hall G, Halpern M, Harrison S, Hildebrandt SR, Hilton GC, Hui H, Irwin KD, Kang J, Karkare KS, Karpel E, Kaufman JP, Keating BG, Kefeli S, Kernasovskiy SA, Kovac JM, Kuo CL, Larsen NA, Lau K, Leitch EM, Lueker M, Megerian KG, Moncelsi L, Namikawa T, Netterfield CB, Nguyen HT, O'Brient R, Ogburn RW, Palladino S, Pryke C, Racine B, Richter S, Schillaci A, Schwarz R, Sheehy CD, Soliman A, St Germaine T, Staniszewski ZK, Steinbach B, Sudiwala RV, Teply GP, Thompson KL, Tolan JE, Tucker C, Turner AD, Umiltà C, Vieregg AG, Wandui A, Weber AC, Wiebe DV, Willmert J, Wong CL, Wu WLK, Yang H, Yoon KW, and Zhang C
Abstract: We present results from an analysis of all data taken by the bicep2/Keck CMB polarization experiments up to and including the 2015 observing season. This includes the first Keck Array observations at 220 GHz and additional observations at 95 and 150 GHz. The Q and U maps reach depths of 5.2, 2.9, and 26 μK_{CMB} arcmin at 95, 150, and 220 GHz, respectively, over an effective area of ≈400 square degrees. The 220 GHz maps achieve a signal to noise on polarized dust emission approximately equal to that of Planck at 353 GHz. We take auto and cross spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz. We evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-ΛCDM+r+dust+synchrotron+noise. The foreground model has seven parameters, and we impose priors on some of these using external information from Planck and WMAP derived from larger regions of sky. The model is shown to be an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint r_{0.05}<0.07 at 95% confidence, which tightens to r_{0.05}<0.06 in conjunction with Planck temperature measurements and other data. The lensing signal is detected at 8.8σ significance. Running a maximum likelihood search on simulations we obtain unbiased results and find that σ(r)=0.020. These are the strongest constraints to date on primordial gravitational waves.
Published: 2018
Full Text: View/download PDF

141. Andrée Gruslin award lecture: Metabolomics as an important modality to better understand preeclampsia.

Author: Benton SJ, Ly C, Vukovic S, and Bainbridge SA
Subjects: Animals, Biomarkers metabolism, Biomedical Research methods, Biomedical Research trends, Female, Humans, Metabolomics trends, Placenta physiopathology, Pre-Eclampsia diagnosis, Pre-Eclampsia physiopathology, Pregnancy, Research Design trends, Uterus metabolism, Uterus physiopathology, Metabolomics methods, Models, Biological, Placenta metabolism, Pre-Eclampsia metabolism, Pre-Eclampsia therapy, Precision Medicine
Abstract: Preeclampsia (PE) is a complex disorder that affects 3-5% of all pregnancies and is a leading cause of maternal and fetal morbidity and mortality. To date, the heterogeneity of clinical presentation, disease severity and outcomes have limited significant advances in early prediction, diagnosis, and therapeutic intervention of PE. The rapidly expanding field of metabolomics, which has the capacity to quantitatively detect low molecular weight compounds (metabolites) in tissue and biological fluids, shows tremendous promise in gaining a better understanding of PE. This review will discuss this emerging field and its contribution to recent advances in the understanding of PE pathophysiology, and identification of early predictive metabolic biomarkers for this complex disorder., (Copyright © 2016 IFPA, Elsevier Ltd. Published by Elsevier Ltd.. All rights reserved.)
Published: 2017
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Database

Publisher

141 results on '"Benton, S. J."'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources