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42 results on '"Fanciullo, L."'

1. The JCMT BISTRO Survey: Multi-wavelength polarimetry of bright regions in NGC 2071 in the far-infrared/submillimetre range, with POL-2 and HAWC+

Author

Fanciullo, L., Kemper, F., Pattle, K., Koch, P. M., Sadavoy, S., Coudé, S., Soam, A., Hoang, T., Onaka, T., Gouellec, V. J. M. Le, Arzoumanian, D., Berry, D., Eswaraiah, C., Chung, E. J., Furuya, R., Hull, C. L. H., Hwang, J., Johnstone, D., Kang, J. -h., Kim, K. H., Kirchschlager, F., Könyves, V., Kwon, J., Kwon, W., Lai, S. -P., Lee, C. W., Liu, T., Lyo, A. -R., Stephens, I., Tamura, M., Tang, X., Ward-Thompson, D., Whitworth, A., and Shinnaga, H.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Polarized dust emission is a key tracer in the study of interstellar medium and of star formation. The observed polarization, however, is a product of magnetic field structure, dust grain properties and grain alignment efficiency, as well as their variations in the line of sight, making it difficult to interpret polarization unambiguously. The comparison of polarimetry at multiple wavelengths is a possible way of mitigating this problem. We use data from HAWC+/SOFIA and from SCUBA-2/POL-2 (from the BISTRO survey) to analyse the NGC 2071 molecular cloud at 154, 214 and 850 $\mu$m. The polarization angle changes significantly with wavelength over part of NGC 2071, suggesting a change in magnetic field morphology on the line of sight as each wavelength best traces different dust populations. Other possible explanations are the existence of more than one polarization mechanism in the cloud or scattering from very large grains. The observed change of polarization fraction with wavelength, and the 214-to-154 $\mu$m polarization ratio in particular, are difficult to reproduce with current dust models under the assumption of uniform alignment efficiency. We also show that the standard procedure of using monochromatic intensity as a proxy for column density may produce spurious results at HAWC+ wavelengths. Using both long-wavelength (POL-2, 850 $\mu$m) and short-wavelength (HAWC+, $\lesssim 200\, \mu$m) polarimetry is key in obtaining these results. This study clearly shows the importance of multi-wavelength polarimetry at submillimeter bands to understand the dust properties of molecular clouds and the relationship between magnetic field and star formation., Comment: Main article: 18 pages, 11 figures. Online supplemental material: 2 pages, 3 figures

Published
2022
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2. Dust polarized emission observations of NGC 6334; BISTRO reveals the details of the complex but organized magnetic field structure of the high-mass star-forming hub-filament network

Author

Arzoumanian, D., Furuya, R., Hasegawa, T., Tahani, M., Sadavoy, S., Hull, C. L. H., Johnstone, D., Koch, P. M., Inutsuka, S. -i., Doi, Y., Hoang, T., Onaka, T., Iwasaki, K., Shimajiri, Y., Inoue, T., Peretto, N., André, P., Bastien, P., Berry, D., Chen, H. -R. V., Di Francesco, J., Eswaraiah, C., Fanciullo, L., Fissel, L. M., Hwang, J., Kang, J. -h., Kim, G., Kim, K. -T., Kirchschlager, F., Kwon, W., Lee, C. W., Liu, H. -L., Lyo, A. -R., Pattle, K., Soam, A., Tang, X., Whitworth, A., Ching, T. -C., Coudé, S., Wang, J. -W., Ward-Thompson, D., Lai, S. -P., Qiu, K., Bourke, T. L., Byun, D. -Y., Chen, M., Chen, Z., Chen, W. P., Cho, J., Choi, Y., Choi, M., Chrysostomou, A., Chung, E. J., Dai, S., Diep, P. N., Duan, H. -Y., Duan, Y., Eden, D., Fiege, J., Franzmann, E., Friberg, P., Fuller, G., Gledhill, T., Graves, S., Greaves, J., Griffin, M., Gu, Q., Han, I., Hatchell, J., Hayashi, S., Houde, M., Jeong, I. -G., Kang, M., Kang, S. -j., Kataoka, A., Kawabata, K., Kemper, F., Kim, M. -R., Kim, K. H., Kim, J., Kim, S., Kirk, J., Kobayashi, M. I. N., Konyves, V., Kusune, T., Kwon, J., Lacaille, K., Law, C. -Y., Lee, C. -F., Lee, Y. -H., Lee, S. -S., Lee, H., Lee, J. -E., Li, H. -b., Li, D., Liu, J., Liu, T., Liu, S. -Y., Lu, X., Mairs, S., Matsumura, M., Matthews, B., Moriarty-Schieven, G., Nagata, T., Nakamura, F., Nakanishi, H., Ngoc, N. B., Ohashi, N., Park, G., Parsons, H., Pyo, T. -S., Qian, L., Rao, R., Rawlings, J., Rawlings, M., Retter, B., Richer, J., Rigby, A., Saito, H., Savini, G., Scaife, A., Seta, M., Shinnaga, H., Tamura, M., Tang, Y. -W., Tomisaka, K., Tram, L. N., Tsukamoto, Y., Viti, S., Wang, H., Xie, J., Yen, H. -W., Yoo, H., Yuan, J., Yun, H. -S., Zenko, T., Zhang, G., Zhang, C. -P., Zhang, Y., Zhou, J., Zhu, L., de Looze, I., Dowell, C. D., Eyres, S., Falle, S., Friesen, R., Robitaille, J. -F., and van Loo, S.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

[Abridged] Filaments and hubs have received special attention recently thanks to studies showing their role in star formation. While the column density and velocity structures of both filaments and hubs have been studied, their magnetic fields (B-field) are not yet characterized. We aim to understand the role of the B-field in the dynamical evolution of the NGC 6334 hub-filament network. We present new observations of the dust polarized emission at 850$\mu$m towards NGC 6334 obtained with the JCMT/POL-2. We study the distribution and dispersion of the polarized intensity ($PI$), the polarization fraction ($PF$), and the B-field angle ($\theta_{B}$). We derive the power spectrum of the intensity and $\theta_{B}$ along the ridge crest. Our analyses show a complex B-field structure when observed over the whole region ($\sim10$ pc), however, at smaller scales ($\sim1$ pc), $\theta_{B}$ varies coherently along the filaments. The observed power spectrum of $\theta_{B}$ can be well represented with a power law function with a slope $-1.33\pm0.23$, which is $\sim20\%$ shallower than that of $I$. This result is compatible with the properties of simulated filaments and may indicate the processes at play in the formation of filaments. $\theta_{B}$ rotates from being mostly perpendicular to the filament crests to mostly parallel as they merge with the hubs. This variation of $\theta_{B}$ may be tracing local velocity flows of matter in-falling onto the hubs. Our analysis suggests a variation of the energy balance along the crests of these filaments, from magnetically critical/supercritical at their far ends to magnetically subcritical near the hubs. We detect an increase of $PF$ towards the high-column density star cluster-forming hubs that may result from the increase of grain alignment efficiency due to stellar radiation from the newborn stars., Comment: Accepted for publication in Astronomy & Astrophysics

Published
2020
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3. JINGLE -- IV. Dust, HI gas and metal scaling laws in the local Universe

Author

De Looze, I., Lamperti, I., Saintonge, A., Relano, M., Smith, M. W. L., Clark, C. J. R., Wilson, C. D., Decleir, M., Jones, A. P., Kennicutt, R. C., Accurso, G., Brinks, E., Bureau, M., Cigan, P., Clements, D. L., De Vis, P., Fanciullo, L, Gao, Y., Gear, W. K., Ho, L. C., Hwang, H. S., Michalowski, M. J., Lee, J. C., Li, C., Lin, L., Liu, T., Lomaeva, M., Pan, H. -A., Sargent, M., Williams, T., Xiao, T., and Zhu, M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Scaling laws of dust, HI gas and metal mass with stellar mass, specific star formation rate and metallicity are crucial to our understanding of the buildup of galaxies through their enrichment with metals and dust. In this work, we analyse how the dust and metal content varies with specific gas mass ($M_{\text{HI}}$/$M_{\star}$) across a diverse sample of 423 nearby galaxies. The observed trends are interpreted with a set of Dust and Element evolUtion modelS (DEUS) - incluidng stellar dust production, grain growth, and dust destruction - within a Bayesian framework to enable a rigorous search of the multi-dimensional parameter space. We find that these scaling laws for galaxies with $-1.0\lesssim \log M_{\text{HI}}$/$M_{\star}\lesssim0$ can be reproduced using closed-box models with high fractions (37-89$\%$) of supernova dust surviving a reverse shock, relatively low grain growth efficiencies ($\epsilon$=30-40), and long dus lifetimes (1-2\,Gyr). The models have present-day dust masses with similar contributions from stellar sources (50-80\,$\%$) and grain growth (20-50\,$\%$). Over the entire lifetime of these galaxies, the contribution from stardust ($>$90\,$\%$) outweighs the fraction of dust grown in the interstellar medium ($<$10$\%$). Our results provide an alternative for the chemical evolution models that require extremely low supernova dust production efficiencies and short grain growth timescales to reproduce local scaling laws, and could help solving the conundrum on whether or not grains can grow efficiently in the interstellar medium., Comment: 56 pages, 30 figures, accepted for publication in MNRAS

Published
2020
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4. Dust models compatible with Planck intensity and polarization data in translucent lines of sight

Author

Guillet, V., Fanciullo, L., Verstraete, L., Boulanger, F., Jones, A. P., Miville-Deschênes, M. -A., Ysard, N., Levrier, F., and Alves, M.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The dust properties inferred from the analysis of Planck observations in total and polarized emission challenge current dust models. We propose new dust models compatible with polarized and unpolarized data in extinction and emission for translucent lines of sight ($0.5 < A_V < 2.5$). We amended the DustEM tool to model polarized extinction and emission. We fit the spectral dependence of the mean extinction, polarized extinction, SED and polarized SED with PAHs, astrosilicates and amorphous carbon (a-C). The astrosilicate population is aligned along the magnetic field lines, while the a-C population may be aligned or not. With their current optical properties, oblate astrosilicate grains are not emissive enough to reproduce the emission to extinction polarization ratio $P_{353}/p_V$ derived with Planck data. Models using prolate astrosilicate grains with an elongation $a/b=3$ and an inclusion of 20% of porosity succeed. The spectral dependence of the polarized SED is steeper in our models than in the data. Models perform slightly better when a-C grains are aligned. A small (6%) volume inclusion of a-C in the astrosilicate matrix removes the need for porosity and perfect grain alignment, and improves the fit to the polarized SED. Dust models based on astrosilicates can be reconciled with Planck data by adapting the shape of grains and adding inclusions of porosity or a-C in the astrosilicate matrix.

Published
2017
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6. The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point

Author

Jones, A. P., Fanciullo, L., Koehler, M., Verstraete, L., Guillet, V., Bocchio, M., and Ysard, N.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Context. The evolution of amorphous hydrocarbon materials, a-C(:H), principally resulting from ultraviolet (UV) photon absorption- induced processing, are likely at the heart of the variations in the observed properties of dust in the interstellar medium. Aims. The consequences of the size-dependent and compositional variations in a-C(:H), from aliphatic-rich a-C:H to aromatic-rich a-C, are studied within the context of the interstellar dust extinction and emission. Methods. Newly-derived optical property data for a-C(:H) materials, combined with that for an amorphous forsterite-type silicate with iron nano-particle inclusions, a-SilFe, are used to explore dust evolution in the interstellar medium. Results. We present a new dust model that consists of a power-law distribution of small a-C grains and log-normal distributions of large a-SilFe and a-C(:H) grains. The model, which is firmly anchored by laboratory-data, is shown to quite naturally explain the variations in the infrared (IR) to far-ultraviolet (FUV) extinction, the 217 nm UV bump, the IR absorption and emission bands and the IR-mm dust emission. Conclusions. The major strengths of the new model are its inherent simplicity and built-in capacity to follow dust evolution in interstellar media. We show that mantle accretion in molecular clouds and UV photo-processing in photo-dominated regions are likely the major drivers of dust evolution., Comment: 22 pages, 20 figures

Published
2014
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7. Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Alina, D., Aniano, G., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Beichman, C., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J. -F., Catalano, A., Chamballu, A., Chary, R. -R., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., 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., Désert, F. -X., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Magalhães, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Poidevin, F., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., and Zonca, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust, bringing new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, $p_V$ , and the optical depth in the V band to the star, $\tau_V$. Toward these stars we measure the submillimetre polarized intensity, $P_S$, and total intensity, $I_S$, in the Planck 353 GHz channel. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, $R_{S/V} = (P_S/I_S)/(p_V/\tau_V)$ and $R_{P/p} = P_S/p_V$ , the latter focusing directly on the polarization properties of the aligned grain population alone. We find $R_{S/V}$ = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and $R_{P/p}$ = 5.4 MJy sr$^{-1}$, with uncertainties 0.2 and 0.3 MJy sr$^{-1}$, respectively. Our estimate of $R_{S/V}$ is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. However, our estimate of $R_{P/p}$ is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, $R_{P/p}$, indicates that changes to the optical properties in the models of the aligned grain population are required.

Published
2014
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8. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Alina, D., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Arzoumanian, D., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J. -F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., 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., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V. -M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J. D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., and Zonca, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Polarized emission observed by Planck HFI at 353 GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions $p$ and angles $\psi$. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction $p_\mathrm{max}$ decreases with column density $N_\mathrm{H}$ in the more opaque fields with $N_\mathrm{H} > 10^{21}\,\mathrm{cm}^{-2}$; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical (MHD) turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction $p_\mathrm{max}$ in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function $\mathcal{S}$. [abridged], Comment: Part of a series of four papers, accepted for publication in A&A

Published
2014
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9. Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible⋆

Author

Ade, PAR, Aghanim, N, Alina, D, Aniano, G, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Battaner, E, Beichman, C, Benabed, K, Benoit-Lévy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Burigana, C, Cardoso, J-F, Catalano, A, Chamballu, A, Chary, R-R, Chiang, HC, Christensen, PR, Colombi, S, Colombo, LPL, Combet, C, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Désert, F-X, Dickinson, C, Diego, JM, Donzelli, S, Doré, O, Douspis, M, Dunkley, J, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Falgarone, E, Fanciullo, L, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, FK, Harrison, DL, Helou, G, Hernández-Monteagudo, C, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Huffenberger, KM, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J-M, Lasenby, A, and Lawrence, CR

Subjects
Astronomical Sciences, Physical Sciences, polarization, dust, extinction, ISM: clouds, ISM: magnetic fields, submillimeter: ISM, astro-ph.GA, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust. In addition to the information on the direction of the Galactic magnetic field, this also brings new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust, and therefore of the important dust model parameters, composition, size, and shape. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, pV, and the optical depth in the V band to the star, τV. Toward these stars we measure the submillimetre polarized intensity, PS, and total intensity, IS, in the Planck 353 GHz channel. We compare the column density measure in the visible, E(B - V), with that inferred from the Planck product map of the submillimetre dust optical depth and compare the polarization direction (position angle) in the visible with that in the submillimetre. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, RS/V = (PS/IS)/(pV/τV) and RP/p = PS/pV, the latter focusing directly on the polarization properties of the aligned grain population alone. We find RS/V = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and RP/p = 5.4 MJy sr-1, with uncertainties 0.2 and 0.3 MJy sr-1, respectively. Our estimate of RS/V is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. This estimate provides new empirical validation of many of the common underlying assumptions of the models, but is not yet very discriminating among them. However, our estimate of RP/p is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, RP/p, indicates that changes to the optical properties in the models of the aligned grain population are required. These new diagnostics, together with the spectral dependence in the submillimetre from Planck, will be important for constraining and understanding the full complexity of the grain models, and for interpreting the Planck thermal dust polarization and refinement of the separation of this contamination of the cosmic microwave background.

Published
2015

10. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence⋆

Author

Ade, PAR, Aghanim, N, Alina, D, Alves, MIR, Aniano, G, Armitage-Caplan, C, Arnaud, M, Arzoumanian, D, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Battaner, E, Benabed, K, Benoit-Lévy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Burigana, C, Cardoso, J-F, Catalano, A, Chamballu, A, Chiang, HC, Christensen, PR, Colombi, S, Colombo, LPL, Combet, C, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Donzelli, S, Doré, O, Douspis, M, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Falgarone, E, Fanciullo, L, Ferrière, K, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, FK, Harrison, DL, Helou, G, Hernández-Monteagudo, C, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Huffenberger, KM, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J-M, Lasenby, A, Lawrence, CR, Leonardi, R, and Levrier, F

Subjects
Astronomical Sciences, Physical Sciences, ISM: general, dust, extinction, ISM: magnetic fields, ISM: clouds, infrared: ISM, submillimeter: ISM, astro-ph.GA, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

Polarized emission observed by Planck HFI at 353? GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction pmax decreases with column density NH in the more opaque fields with NH> 1021 cm-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction pmax in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function S. However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties.

Published
2015

11. B-fields in Star-forming Region Observations (BISTRO): Magnetic Fields in the Filamentary Structures of Serpens Main

Author

Kwon, W, Pattle, K, Sadavoy, S, Hull, CLH, Johnstone, D, Ward-Thompson, D, Francesco, JD, Koch, PM, Furuya, R, Doi, Y, Le Gouellec, VJM, Hwang, J, Lyo, AR, Soam, A, Tang, X, Hoang, T, Kirchschlager, F, Eswaraiah, C, Fanciullo, L, Kim, KH, Onaka, T, Könyves, V, Kang, JH, Lee, CW, Tamura, M, Bastien, P, Hasegawa, T, Lai, SP, Qiu, K, Berry, D, Arzoumanian, D, Bourke, TL, Byun, DY, Chen, WP, Chen, HRV, Chen, M, Chen, Z, Ching, TC, Cho, J, Choi, Y, Choi, M, Chrysostomou, A, Chung, EJ, Coudé, S, Dai, S, Diep, PN, Duan, Y, Duan, HY, Eden, D, Fiege, J, Fissel, LM, Franzmann, E, Friberg, P, Friesen, R, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Inoue, T, Inutsuka, SI, Iwasaki, K, Jeong, IG, Kang, M, Karoly, J, Kataoka, A, Kawabata, K, Kemper, F, Kim, KT, Kim, G, Kim, MR, Kim, S, Kim, J, Kirk, J, Kobayashi, MIN, Kusune, T, Kwon, J, Lacaille, K, Law, CY, Lee, CF, Lee, YH, Lee, H, Lee, JE, Lee, SS, Li, D, Li, HB, Lin, SJ, Liu, SY, Liu, HL, Liu, J, Liu, T, Lu, X, Mairs, S, Matsumura, M, Kwon, W [0000-0003-4022-4132], Pattle, K [0000-0002-8557-3582], Sadavoy, S [0000-0001-7474-6874], Hull, CLH [0000-0002-8975-7573], Johnstone, D [0000-0002-6773-459X], Ward-Thompson, D [0000-0003-1140-2761], Francesco, JD [0000-0002-9289-2450], Koch, PM [0000-0003-2777-5861], Furuya, R [0000-0003-0646-8782], Doi, Y [0000-0001-8746-6548], Le Gouellec, VJM [0000-0002-5714-799X], Hwang, J [0000-0001-7866-2686], Lyo, AR [0000-0002-9907-8427], Soam, A [0000-0002-6386-2906], Tang, X [0000-0002-4154-4309], Hoang, T [0000-0003-2017-0982], Kirchschlager, F [0000-0002-3036-0184], Fanciullo, L [0000-0001-9930-9240], Kim, KH [0000-0001-9597-7196], Onaka, T [0000-0002-8234-6747], Könyves, V [0000-0002-3746-1498], Kang, JH [0000-0001-7379-6263], Tamura, M [0000-0002-6510-0681], Bastien, P [0000-0002-0794-3859], Lai, SP [0000-0001-5522-486X], Qiu, K [0000-0002-5093-5088], Arzoumanian, D [0000-0002-1959-7201], Bourke, TL [0000-0001-7491-0048], Byun, DY [0000-0003-1157-4109], Chen, WP [0000-0002-5519-0628], Chen, HRV [0000-0002-9774-1846], Chen, Z [0000-0003-0849-0692], Ching, TC [0000-0001-8516-2532], Cho, J [0000-0003-1725-4376], Chrysostomou, A [0000-0002-9583-8644], Chung, EJ [0000-0003-0014-1527], Coudé, S [0000-0002-0859-0805], Duan, HY [0000-0002-7022-4742], Eden, D [0000-0002-5881-3229], Fissel, LM [0000-0002-4666-609X], Franzmann, E [0000-0003-2142-0357], Friberg, P [0000-0002-8010-8454], Friesen, R [0000-0001-7594-8128], Fuller, G [0000-0001-8509-1818], Gledhill, T [0000-0002-2859-4600], Graves, S [0000-0001-9361-5781], Greaves, J [0000-0002-3133-413X], Gu, Q [0000-0002-2826-1902], Hatchell, J [0000-0002-4870-2760], Houde, M [0000-0003-4420-8674], Inoue, T [0000-0002-7935-8771], Inutsuka, SI [0000-0003-4366-6518], Iwasaki, K [0000-0002-2707-7548], Kang, M [0000-0002-5016-050X], Kataoka, A [0000-0003-4562-4119], Kawabata, K [0000-0001-6099-9539], Kemper, F [0000-0003-2743-8240], Kim, KT [0000-0003-2412-7092], Kim, G [0000-0003-2011-8172], Kim, MR [0000-0002-1408-7747], Kim, S [0000-0001-9333-5608], Kim, J [0000-0002-1229-0426], Kirk, J [0000-0002-4552-7477], Kobayashi, MIN [0000-0003-3990-1204], Kusune, T [0000-0002-9218-9319], Kwon, J [0000-0003-2815-7774], Lacaille, K [0000-0001-9870-5663], Law, CY [0000-0003-1964-970X], Lee, CF [0000-0002-3024-5864], Lee, YH [0000-0001-6047-701X], Lee, H [0000-0003-3465-3213], Lee, JE [0000-0003-3119-2087], Lee, SS [0000-0002-6269-594X], Li, D [0000-0003-3010-7661], Li, HB [0000-0003-2641-9240], Lin, SJ [0000-0002-6868-4483], Liu, SY [0000-0003-4603-7119], Liu, J [0000-0002-4774-2998], Lu, X [0000-0003-2619-9305], Mairs, S [0000-0002-6956-0730], Matsumura, M [0000-0002-6906-0103], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, Interstellar Matter and the Local Universe, 51 Physical Sciences, Astrophysics::Galaxy Astrophysics
Abstract

We present 850 μm polarimetric observations toward the Serpens Main molecular cloud obtained using the POL-2 polarimeter on the James Clerk Maxwell Telescope as part of the B-fields In STar-forming Region Observations survey. These observations probe the magnetic field morphology of the Serpens Main molecular cloud on about 6000 au scales, which consists of cores and six filaments with different physical properties such as density and star formation activity. Using the histogram of relative orientation (HRO) technique, we find that magnetic fields are parallel to filaments in less-dense filamentary structures where N H 2 < 0.93 × 10 22 cm−2 (magnetic fields perpendicular to density gradients), while they are perpendicular to filaments (magnetic fields parallel to density gradients) in dense filamentary structures with star formation activity. Moreover, applying the HRO technique to denser core regions, we find that magnetic field orientations change to become perpendicular to density gradients again at N H 2 ≈ 4.6 × 10 22 cm−2. This can be interpreted as a signature of core formation. At N H 2 ≈ 16 × 10 22 cm−2, magnetic fields change back to being parallel to density gradients once again, which can be understood to be due to magnetic fields being dragged in by infalling material. In addition, we estimate the magnetic field strengths of the filaments (B POS = 60–300 μG)) using the Davis–Chandrasekhar–Fermi method and discuss whether the filaments are gravitationally unstable based on magnetic field and turbulence energy densities.

Published
2022
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12. The JCMT BISTRO Survey: Revealing the Diverse Magnetic Field Morphologies in Taurus Dense Cores with Sensitive Submillimeter Polarimetry

Author

Eswaraiah, C, Li, D, Furuya, RS, Hasegawa, T, Ward-Thompson, D, Qiu, K, Ohashi, N, Pattle, K, Sadavoy, S, Hull, CLH, Berry, D, Doi, Y, Ching, TC, Lai, SP, Wang, JW, Koch, PM, Kwon, J, Kwon, W, Bastien, P, Arzoumanian, D, Coudé, S, Soam, A, Fanciullo, L, Yen, HW, Liu, J, Hoang, T, Ping Chen, W, Shimajiri, Y, Liu, T, Chen, Z, Li, HB, Lyo, AR, Hwang, J, Johnstone, D, Rao, R, Bich Ngoc, N, Ngoc Diep, P, Mairs, S, Parsons, H, Tamura, M, Tahani, M, Vivien Chen, HR, Nakamura, F, Shinnaga, H, Tang, YW, Cho, J, Won Lee, C, Inutsuka, SI, Inoue, T, Iwasaki, K, Qian, L, Xie, J, Liu, HL, Zhang, CP, Chen, M, Zhang, G, Zhu, L, Zhou, J, André, P, Liu, SY, Yuan, J, Lu, X, Peretto, N, Bourke, TL, Byun, DY, Dai, S, Duan, Y, Duan, HY, Eden, D, Matthews, B, Fiege, J, Fissel, LM, Kim, KT, Lee, CF, Kim, J, Pyo, TS, Choi, Y, Choi, M, Chrysostomou, A, Jung Chung, E, Ngoc Tram, L, Franzmann, E, Friberg, P, Friesen, R, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Kawabata, K, Jeong, IG, Kang, JH, Kang, SJ, Kang, M, Eswaraiah, C [0000-0003-4761-6139], Furuya, RS [0000-0003-0646-8782], Hasegawa, T [0000-0003-1853-0184], Ward-Thompson, D [0000-0003-1140-2761], Qiu, K [0000-0002-5093-5088], Ohashi, N [0000-0003-0998-5064], Pattle, K [0000-0002-8557-3582], Sadavoy, S [0000-0001-7474-6874], Hull, CLH [0000-0002-8975-7573], Berry, D [0000-0001-6524-2447], Doi, Y [0000-0001-8746-6548], Ching, TC [0000-0001-8516-2532], Lai, SP [0000-0001-5522-486X], Wang, JW [0000-0002-6668-974X], Koch, PM [0000-0003-2777-5861], Kwon, J [0000-0003-2815-7774], Kwon, W [0000-0003-4022-4132], Bastien, P [0000-0002-0794-3859], Arzoumanian, D [0000-0002-1959-7201], Coudé, S [0000-0002-0859-0805], Soam, A [0000-0002-6386-2906], Fanciullo, L [0000-0001-9930-9240], Yen, HW [0000-0003-1412-893X], Liu, J [0000-0002-4774-2998], Hoang, T [0000-0003-2017-0982], Ping Chen, W [0000-0003-0262-272X], Shimajiri, Y [0000-0001-9368-3143], Liu, T [0000-0002-5286-2564], Chen, Z [0000-0003-0849-0692], Li, HB [0000-0003-2641-9240], Lyo, AR [0000-0002-9907-8427], Hwang, J [0000-0001-7866-2686], Johnstone, D [0000-0002-6773-459X], Rao, R [0000-0002-1407-7944], Bich Ngoc, N [0000-0002-5913-5554], Ngoc Diep, P [0000-0002-2808-0888], Mairs, S [0000-0002-6956-0730], Parsons, H [0000-0002-6327-3423], Tamura, M [0000-0002-6510-0681], Tahani, M [0000-0001-8749-1436], Vivien Chen, HR [0000-0002-9774-1846], Nakamura, F [0000-0001-5431-2294], Shinnaga, H [0000-0001-9407-6775], Tang, YW [0000-0002-0675-276X], Cho, J [0000-0003-1725-4376], Won Lee, C [0000-0002-3179-6334], Inutsuka, SI [0000-0003-4366-6518], Iwasaki, K [0000-0002-2707-7548], Qian, L [0000-0003-0597-0957], Xie, J [0000-0002-2738-146X], Liu, HL [0000-0003-3343-9645], Zhang, CP [0000-0002-4428-3183], Zhou, J [0000-0003-0356-818X], André, P [0000-0002-3413-2293], Liu, SY [0000-0003-4603-7119], Lu, X [0000-0003-2619-9305], Bourke, TL [0000-0001-7491-0048], Byun, DY [0000-0003-1157-4109], Eden, D [0000-0002-5881-3229], Matthews, B [0000-0003-3017-9577], Fissel, LM [0000-0002-4666-609X], Kim, KT [0000-0003-2412-7092], Lee, CF [0000-0002-3024-5864], Kim, J [0000-0002-1229-0426], Pyo, TS [0000-0002-3273-0804], Chrysostomou, A [0000-0002-9583-8644], Jung Chung, E [0000-0003-0014-1527], Ngoc Tram, L [0000-0002-6488-8227], Franzmann, E [0000-0003-2142-0357], Friberg, P [0000-0002-8010-8454], Friesen, R [0000-0001-7594-8128], Fuller, G [0000-0001-8509-1818], Gledhill, T [0000-0002-2859-4600], Graves, S [0000-0001-9361-5781], Griffin, M [0000-0002-0033-177X], Gu, Q [0000-0002-2826-1902], Hatchell, J [0000-0002-4870-2760], Houde, M [0000-0003-4420-8674], Kawabata, K [0000-0001-6099-9539], Jeong, IG [0000-0002-5492-6832], Kang, JH [0000-0001-7379-6263], Kang, SJ [0000-0002-5004-7216], Kang, M [0000-0002-5016-050X], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 51 Physical Sciences
Abstract

We have obtained sensitive dust continuum polarization observations at 850 μm in the B213 region of Taurus using POL-2 on SCUBA-2 at the James Clerk Maxwell Telescope as part of the B-fields in STar-forming Region Observations (BISTRO) survey. These observations allow us to probe magnetic field (B-field) at high spatial resolution (∼2000 au or ∼0.01 pc at 140 pc) in two protostellar cores (K04166 and K04169) and one prestellar core (Miz-8b) that lie within the B213 filament. Using the Davis–Chandrasekhar–Fermi method, we estimate the B-field strengths in K04166, K04169, and Miz-8b to be 38 ± 14, 44 ± 16, and 12 ± 5 μG, respectively. These cores show distinct mean B-field orientations. The B-field in K04166 is well ordered and aligned parallel to the orientations of the core minor axis, outflows, core rotation axis, and large-scale uniform B-field, in accordance with magnetically regulated star formation via ambipolar diffusion taking place in K04166. The B-field in K04169 is found to be ordered but oriented nearly perpendicular to the core minor axis and large-scale B-field and not well correlated with other axes. In contrast, Miz-8b exhibits a disordered B-field that shows no preferred alignment with the core minor axis or large-scale field. We found that only one core, K04166, retains a memory of the large-scale uniform B-field. The other two cores, K04169 and Miz-8b, are decoupled from the large-scale field. Such a complex B-field configuration could be caused by gas inflow onto the filament, even in the presence of a substantial magnetic flux.

Published
2021

13. The JCMT BISTRO survey: An 850/450μm polarization study of NGC 2071IR in Orion B

Author

Lyo, AR, Kim, J, Sadavoy, S, Johnstone, D, Berry, D, Pattle, K, Kwon, W, Bastien, P, Onaka, T, Di Francesco, J, Kang, JH, Furuya, R, Hull, CLH, Tamura, M, Koch, PM, Ward-Thompson, D, Hasegawa, T, Hoang, T, Arzoumanian, D, Lee, CW, Lee, CF, Byun, DY, Kirchschlager, F, Doi, Y, Kim, KT, Hwang, J, Diep, PN, Fanciullo, L, Lee, SS, Park, G, Yoo, H, Chung, EJ, Whitworth, A, Mairs, S, Soam, A, Liu, T, Tang, X, Coudé, S, André, P, Bourke, TL, Chen, HRV, Chen, Z, Chen, WP, Chen, M, Ching, TC, Choi, M, Choi, Y, Chrysostomou, A, Dai, S, Zhang, CP, Duan, HY, Duan, Y, Cho, J, Eden, D, Eswaraiah, C, Eyres, S, Fiege, J, Fissel, LM, Franzmann, E, Friberg, P, Friesen, R, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Inoue, T, Inutsuka, SI, Iwasaki, K, Jeong, IG, Kang, M, Kataoka, A, Kawabata, K, Kim, G, Kim, MR, Kim, S, Kim, KH, Kirk, J, Kobayashi, MIN, Kemper, F, Könyves, V, Kusune, T, Kwon, J, Lacaille, K, Lai, SP, Lee, JE, Lee, YH, Lee, H, Li, D, Li, HB, Liu, HL, Law, CY, Liu, J, Liu, SY, Lyo, AR [0000-0002-9907-8427], Kim, J [0000-0002-1229-0426], Johnstone, D [0000-0002-6773-459X], Pattle, K [0000-0002-8557-3582], Kwon, W [0000-0003-4022-4132], Bastien, P [0000-0002-0794-3859], Onaka, T [0000-0002-8234-6747], Kang, JH [0000-0001-7379-6263], Furuya, R [0000-0003-0646-8782], Hull, CLH [0000-0002-8975-7573], Tamura, M [0000-0002-6510-0681], Koch, PM [0000-0003-2777-5861], Ward-Thompson, D [0000-0003-1140-2761], Hoang, T [0000-0003-2017-0982], Arzoumanian, D [0000-0002-1959-7201], Lee, CF [0000-0002-3024-5864], Byun, DY [0000-0003-1157-4109], Kirchschlager, F [0000-0002-3036-0184], Doi, Y [0000-0001-8746-6548], Kim, KT [0000-0003-2412-7092], Hwang, J [0000-0001-7866-2686], Lee, SS [0000-0002-6269-594X], Park, G [0000-0001-8467-3736], Yoo, H [0000-0002-8578-1728], Chung, EJ [0000-0003-0014-1527], Mairs, S [0000-0002-6956-0730], Soam, A [0000-0002-6386-2906], Liu, T [0000-0002-5286-2564], Tang, X [0000-0002-4154-4309], Coudé, S [0000-0002-0859-0805], André, P [0000-0002-3413-2293], Bourke, TL [0000-0001-7491-0048], Chen, Z [0000-0003-0849-0692], Chen, WP [0000-0002-5519-0628], Ching, TC [0000-0001-8516-2532], Chrysostomou, A [0000-0002-9583-8644], Zhang, CP [0000-0002-4428-3183], Cho, J [0000-0003-1725-4376], Eden, D [0000-0002-5881-3229], Franzmann, E [0000-0003-2142-0357], Friberg, P [0000-0002-8010-8454], Friesen, R [0000-0001-7594-8128], Fuller, G [0000-0001-8509-1818], Gledhill, T [0000-0002-2859-4600], Graves, S [0000-0001-9361-5781], Gu, Q [0000-0002-2826-1902], Hatchell, J [0000-0002-4870-2760], Houde, M [0000-0003-4420-8674], Inoue, T [0000-0002-7935-8771], Inutsuka, SI [0000-0003-4366-6518], Iwasaki, K [0000-0002-2707-7548], Kang, M [0000-0002-5016-050X], Kataoka, A [0000-0003-4562-4119], Kawabata, K [0000-0001-6099-9539], Kim, G [0000-0003-2011-8172], Kim, MR [0000-0002-1408-7747], Kim, S [0000-0001-9333-5608], Kirk, J [0000-0002-4552-7477], Kobayashi, MIN [0000-0003-3990-1204], Kemper, F [0000-0003-2743-8240], Könyves, V [0000-0002-3746-1498], Kusune, T [0000-0002-9218-9319], Kwon, J [0000-0003-2815-7774], Lacaille, K [0000-0001-9870-5663], Lai, SP [0000-0001-5522-486X], Lee, JE [0000-0003-3119-2087], Lee, YH [0000-0001-6047-701X], Lee, H [0000-0003-3465-3213], Li, D [0000-0003-3010-7661], Li, HB [0000-0003-2641-9240], Law, CY [0000-0003-1964-970X], Liu, J [0000-0002-4774-2998], Liu, SY [0000-0003-4603-7119], and Apollo - University of Cambridge Repository

Subjects
5101 Astronomical Sciences, 51 Physical Sciences
Abstract

We present the results of simultaneous 450 μm and 850 μm polarization observations toward the massive star-forming region NGC 2071IR, a target of the BISTRO (B-fields in STar-forming Region Observations) Survey, using the POL-2 polarimeter and SCUBA-2 camera mounted on the James Clerk Maxwell Telescope. We find a pinched magnetic field morphology in the central dense core region, which could be due to a rotating toroidal disklike structure and a bipolar outflow originating from the central young stellar object IRS 3. Using the modified Davis–Chandrasekhar–Fermi method, we obtain a plane-of-sky magnetic field strength of 563 ± 421 μG in the central ∼0.12 pc region from 850 μm polarization data. The corresponding magnetic energy density of 2.04 × 10−8 erg cm−3 is comparable to the turbulent and gravitational energy densities in the region. We find that the magnetic field direction is very well aligned with the whole of the IRS 3 bipolar outflow structure. We find that the median value of polarization fractions is 3.0% at 450 μm in the central 3′ region, which is larger than the median value of 1.2% at 850 μm. The trend could be due to the better alignment of warmer dust in the strong radiation environment. We also find that polarization fractions decrease with intensity at both wavelengths, with slopes, determined by fitting a Rician noise model of 0.59 ± 0.03 at 450 μm and 0.36 ± 0.04 at 850 μm, respectively. We think that the shallow slope at 850 μm is due to grain alignment at the center being assisted by strong radiation from the central young stellar objects.

Published
2021
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14. Dust polarized emission observations of NGC 6334

Author

Arzoumanian, D, Furuya, RS, Hasegawa, T, Tahani, M, Sadavoy, S, Hull, CLH, Johnstone, D, Koch, PM, Inutsuka, S, Doi, Y, Hoang, T, Onaka, T, Iwasaki, K, Shimajiri, Y, Inoue, T, Peretto, N, André, P, Bastien, P, Berry, D, Chen, H-RV, Di Francesco, J, Eswaraiah, C, Fanciullo, L, Fissel, LM, Hwang, J, Kang, J-H, Kim, G, Kim, K-T, Kirchschlager, F, Kwon, W, Lee, CW, Liu, H-L, Lyo, A-R, Pattle, K, Soam, A, Tang, X, Whitworth, A, Ching, T-C, Coudé, S, Wang, J-W, Ward-Thompson, D, Lai, S-P, Qiu, K, Bourke, TL, Byun, D-Y, Chen, M, Chen, Z, Chen, WP, Cho, J, Choi, Y, Choi, M, Chrysostomou, A, Chung, EJ, Dai, S, Diep, PN, Duan, H-Y, Duan, Y, Eden, D, Fiege, J, Franzmann, E, Friberg, P, Fuller, G, Gledhill, T, Graves, S, Greaves, J, Griffin, M, Gu, Q, Han, I, Hatchell, J, Hayashi, S, Houde, M, Jeong, I-G, Kang, M, Kang, S-J, Kataoka, A, Kawabata, K, Kemper, F, Kim, M-R, Kim, KH, Kim, J, Kim, S, Kirk, J, Kobayashi, MIN, Könyves, V, Kusune, T, Kwon, J, Lacaille, K, Law, C-Y, Lee, C-F, Lee, Y-H, Lee, S-S, Lee, H, Lee, J-E, Li, H-B, Li, D, Li, DL, Liu, J, Liu, T, Liu, S-Y, Lu, X, Mairs, S, Matsumura, M, Matthews, B, Moriarty-Schieven, G, Nagata, T, Nakamura, F, Nakanishi, H, Ngoc, NB, Ohashi, N, Park, G, Parsons, H, Pyo, T-S, Qian, L, Rao, R, Rawlings, J, Rawlings, M, Retter, B, Richer, J, Rigby, A, Saito, H, Savini, G, Scaife, A, Seta, M, Shinnaga, H, Tamura, M, Tang, Y-W, Tomisaka, K, Tram, LN, Tsukamoto, Y, Viti, S, Wang, H, Xie, J, Yen, H-W, Yoo, H, Yuan, J, Yun, H-S, Zenko, T, Zhang, G, Zhang, C-P, Zhang, Y, Zhou, J, Zhu, L, de Looze, I, Dowell, CD, Eyres, S, Falle, S, Friesen, R, Robitaille, J-F, and van Loo, S

Subjects
Astrophysics::Galaxy Astrophysics
Abstract

Context. Molecular filaments and hubs have received special attention recently thanks to new studies showing their key role in star formation. While the (column) density and velocity structures of both filaments and hubs have been carefully studied, their magnetic field (B-field) properties have yet to be characterized. Consequently, the role of B-fields in the formation and evolution of hub-filament systems is not well constrained. Aims. We aim to understand the role of the B-field and its interplay with turbulence and gravity in the dynamical evolution of the NGC 6334 filament network that harbours cluster-forming hubs and high-mass star formation. Methods. We present new observations of the dust polarized emission at 850 μm toward the 2 pc × 10 pc map of NGC 6334 at a spatial resolution of 0.09 pc obtained with the James Clerk Maxwell Telescope (JCMT) as part of the B-field In STar-forming Region Observations (BISTRO) survey. We study the distribution and dispersion of the polarized intensity (PI), the polarization fraction (PF), and the plane-of-the-sky B-field angle (χB_POS) toward the whole region, along the 10 pc-long ridge and along the sub-filaments connected to the ridge and the hubs. We derived the power spectra of the intensity and χBPOS along the ridge crest and compared them with the results obtained from simulated filaments. Results. The observations span ~3 orders of magnitude in Stokes I and PI and ~2 orders of magnitude in PF (from ~0.2 to ~ 20%). A large scatter in PI and PF is observed for a given value of I. Our analyses show a complex B-field structure when observed over the whole region (~ 10 pc); however, at smaller scales (~1 pc), χBPOS varies coherently along the crests of the filament network. The observed power spectrum of χBPOS can be well represented with a power law function with a slope of − 1.33 ± 0.23, which is ~20% shallower than that of I. We find that this result is compatible with the properties of simulated filaments and may indicate the physical processes at play in the formation and evolution of star-forming filaments. Along the sub-filaments, χBPOS rotates frombeing mostly perpendicular or randomly oriented with respect to the crests to mostly parallel as the sub-filaments merge with the ridge and hubs. This variation of the B-field structure along the sub-filaments may be tracing local velocity flows of infalling matter in the ridge and hubs. Our analysis also suggests a variation in the energy balance along the crests of these sub-filaments, from magnetically critical or supercritical at their far ends to magnetically subcritical near the ridge and hubs. We also detect an increase in PF toward the high-column density (NH2 ≳ 1023 cm−2) star cluster-forming hubs. These latter large PF values may be explained by the increase in grain alignment efficiency due to stellar radiation from the newborn stars, combined with an ordered B-field structure. Conclusions. These observational results reveal for the first time the characteristics of the small-scale (down to ~ 0.1 pc) B-field structure of a 10 pc-long hub-filament system. Our analyses show variations in the polarization properties along the sub-filaments that may be tracing the evolution of their physical properties during their interaction with the ridge and hubs. We also detect an impact of feedback from young high-mass stars on the local B-field structure and the polarization properties, which could put constraints on possible models for dust grain alignment and provide important hints as to the interplay between the star formation activity and interstellar B-fields.

Published
2021

15. JINGLE – IV. Dust, H i gas, and metal scaling laws in the local Universe

Author

De Looze, I, primary, Lamperti, I, primary, Saintonge, A, primary, Relaño, M, primary, Smith, M W L, primary, Clark, C J R, primary, Wilson, C D, primary, Decleir, M, primary, Jones, A P, primary, Kennicutt, R C, primary, Accurso, G, primary, Brinks, E, primary, Bureau, M, primary, Cigan, P, primary, Clements, D L, primary, De Vis, P, primary, Fanciullo, L, primary, Gao, Y, primary, Gear, W K, primary, Ho, L C, primary, Hwang, H S, primary, Michałowski, M J, primary, Lee, J C, primary, Li, C, primary, Lin, L, primary, Liu, T, primary, Lomaeva, M, primary, Pan, H-A, primary, Sargent, M, primary, Williams, T, primary, Xiao, T, primary, and Zhu, M, primary

Published
2020
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16. Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Alina, D., Aniano, G., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Beichman, C., Benabed, K., Benoit-L√©vy, A., J-P, Bernard, Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., J-F, Cardoso, Catalano, A., Chamballu, A., R-R, Chary, Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., Bernardis, P., Rosa, A., Zotti, G., Delabrouille, J., F-X, D√©sert, Clive Dickinson, Diego, J. M., Donzelli, S., Dor√©, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., En√ülin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-H√©raud, Y., Gonz√°lez-Nuevo, J., G√≥rski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hern√°ndez-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keih√§nen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., L√§hteenm√§ki, A., J-M, Lamarre, Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-V√∏rnle, M., L√≥pez-Caniego, M., Lubin, P. M., Mac√ ̸as-P√©rez, J. F., Maffei, B., Magalh√£es, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Mart√ ̸nez-Gonz√°lez, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., M-A, Miville-Desch√™nes, Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Poidevin, F., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., J-L, Puget, Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., A-S, Suur-Uski, J-F, Sygnet, Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zonca, A., 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), 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), 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), 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 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), PLANCK, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), École normale supérieure - Paris (ENS-PSL), 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), Anne Lähteenmäki Group, Department of Radio Science and Engineering, Aalto-yliopisto, Aalto University, European Commission, Consejo Superior de Investigaciones Científicas (España), Junta de Andalucía, Ministerio de Ciencia e Innovación (España), European Research Council, Ade, P, Aghanim, N, Alina, D, Aniano, G, Armitage Caplan, C, Arnaud, M, Ashdown, M, Atrio Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Battaner, E, Beichman, C, Benabed, K, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bock, J, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Burigana, C, Cardoso, J, Catalano, A, Chamballu, A, Chary, R, Chiang, H, Christensen, P, Colombi, S, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Désert, F, Dickinson, C, Diego, J, Donzelli, S, Doré, O, Douspis, M, Dunkley, J, Dupac, X, Efstathiou, G, Enßlin, T, Eriksen, H, Falgarone, E, Fanciullo, L, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud Héraud, Y, González Nuevo, J, Górski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Harrison, D, Helou, G, Hernández Monteagudo, C, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Huffenberger, K, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, López Caniego, M, Lubin, P, Macías Pérez, J, Maffei, B, Magalhães, A, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martínez González, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Miville Deschênes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Noviello, F, Novikov, D, Novikov, I, Oxborrow, C, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Pasian, F, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pietrobon, D, Plaszczynski, S, Poidevin, F, Pointecouteau, E, Polenta, G, Popa, L, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rusholme, B, Sandri, M, Savini, G, Scott, D, Spencer, L, Stolyarov, V, Stompor, R, Sudiwala, R, Sutton, D, Suur Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, L, Wandelt, B, Zonca, A, Ade, P. A. R., Aghanim, N., Alina, D., Aniano, G., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Beichman, C., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J. F., Catalano, A., Chamballu, A., Chary, R. R., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., 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., Désert, F. X., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Magalhães, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Poidevin, F., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zonca, A., 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)-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), 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), Department of Physics, and Helsinki Institute of Physics

Subjects
magnetic field [ISM], Astronomy, cloud [ISM], Astrophysics, MOLECULAR CLOUD, 7. Clean energy, ISM: clouds, Light scattering, Polarization, extinction / ISM: clouds / ISM: magnetic fields / submillimeter: ISM, QB, Physics, education.field_of_study, general [ISM], Dust extinction, ISM: magnetic fields, Submillimeter: ISM, Astronomy and Astrophysics, Space and Planetary Science, extinction, WAVELENGTH DEPENDENCE, Polarization (waves), EXTINCTION, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, polarization / dust, Degree of polarization, dust, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], CAMPO MAGNÉTICO, clouds [ISM], Population, MU-M, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, symbols.namesake, ISM: magnetic field, Settore FIS/05 - Astronomia e Astrofisica, ISM: cloud, Planck, education, ISM [submillimeter], Dust, extinction, Astrophysics::Galaxy Astrophysics, dust, extinction, polarization [ISM], LINEAR-POLARIZATION, SUBMILLIMETER POLARIZATION, SPECTRUM, polarization, magnetic fields [ISM], Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Interstellar medium, Stars, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], INFRARED POLARIZATION, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), PROBE WMAP OBSERVATIONS, STARS, V band
Abstract

et al., The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust. In addition to the information on the direction of the Galactic magnetic field, this also brings new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust, and therefore of the important dust model parameters, composition, size, and shape. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, pV, and the optical depth in the V band to the star, τV. Toward these stars we measure the submillimetre polarized intensity, PS, and total intensity, IS, in the Planck 353 GHz channel. We compare the column density measure in the visible, E(B − V), with that inferred from the Planck product map of the submillimetre dust optical depth and compare the polarization direction (position angle) in the visible with that in the submillimetre. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, RS /V = (PS/IS) / (pV/τV) and RP/p = PS/pV, the latter focusing directly on the polarization properties of the aligned grain population alone.We find RS /V = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and RP/p = 5.4 MJy sr-1, with uncertainties 0.2 and 0.3 MJy sr-1, respectively. Our estimate of RS /V is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. This estimate provides new empirical validation of many of the common underlying assumptions of the models, but is not yet very discriminating among them. However, our estimate of RP/p is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, RP/p, indicates that changes to the optical properties in the models of the aligned grain population are required. These new diagnostics, together with the spectral dependence in the submillimetre from Planck,will be important for constraining and understanding the full complexity of the grain models, and for interpreting the Planck thermal dust polarization and refinement of the separation of this contamination of the cosmic microwave background., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007−2013) / ERC grant agreement No. 267934.

Published
2015
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17. Dust models compatible with Planck intensity and polarization data in translucent lines of sight

Author

Guillet, V., Fanciullo, L., Verstraete, L., Boulanger, F., Jones, A. P., Miville-Deschênes, M.-A., Ysard, N., Levrier, F., Alves, M., Miville-Deschênes, A., 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), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Sorbonne Université (SU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Laboratoire Pluridisciplinaire de Recherche en Ingénierie des Systèmes, Mécanique et Energétique (PRISME), Université d'Orléans (UO)-Ecole Nationale Supérieure d'Ingénieurs de Bourges (ENSI Bourges), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), and 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)

Subjects
Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, methods: numerical, symbols.namesake, 0103 physical sciences, Planck, education, Porosity, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [PHYS]Physics [physics], education.field_of_study, polarization, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, extinction, Spectral density, Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Magnetic field, Sight, Amorphous carbon, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, submillimeter: ISM, dust, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

Context. Current dust models are challenged by the dust properties inferred from the analysis of Planck observations in total and polarized emission. Aims. We propose new dust models compatible with polarized and unpolarized data in extinction and emission for translucent lines of sight (0.5 < AV < 2.5). Methods. We amended the DustEM tool to model polarized extinction and emission. We fit the spectral dependence of the mean extinction, polarized extinction, total and polarized spectral energy distributions (SEDs) with polycyclic aromatic hydrocarbons, astrosilicate and amorphous carbon (a-C) grains. The astrosilicate population is aligned along the magnetic field lines, while the a-C population may be aligned or not. Results. With their current optical properties, oblate astrosilicate grains are not emissive enough to reproduce the emission to extinction polarization ratio P353∕pV derived with Planck data. Successful models are those using prolate astrosilicate grains with an elongation a∕b = 3 and an inclusion of 20% porosity. The spectral dependence of the polarized SED is steeper in our models than in the data. Models perform slightly better when a-C grains are aligned. A small (6%) volume inclusion of a-C in the astrosilicate matrix removes the need for porosity and perfect grain alignment, and improves the fit to the polarized SED. Conclusions. Dust models based on astrosilicates can be reconciled with Planck data by adapting the shape of grains and adding inclusions of porosity or a-C in the astrosilicate matrix.

Published
2018
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20. Physical activity and sedentary lifestyle in children with type 1 diabetes: a multicentre Italian study

Author

Fainardi, V., Scarabello, C., Cangelosi, A., Fanciullo, L., Mastrorilli, C., Giannini, C., Mohn, A., Dario Iafusco, La Loggia, A., Lombardo, F., Toni, S., Valerio, G., Franzese, A., Prisco, F., Chiarelli, F., Vanelli, M., Fainardi, V, Scarabello, C, Cangelosi, A, Fanciullo, L, Mastrorilli, C, Giannini, C, Mohn, A, Iafusco, Dario, La Loggia, A, Lombardo, F, Toni, S, Valerio, G, Franzese, A, Prisco, F, Chiarelli, F, Vanelli, M., V., Fainardi, C., Scarabello, A., Cangelosi, L., Fanciullo, C., Mastrorilli, C., Giannini, A., Mohn, D., Iafusco, A. L., Loggia, F., Lombardo, S., Toni, G., Valerio, Franzese, Adriana, F., Prisco, F., Chiarelli, and M., Vanelli

Subjects
Adolescent, Child, Diabetes Mellitu, Glycated Hemoglobin, Male, Adolescent, type 1 diabetes, Health Behavior, Glycosylated, physical activity, epidemiology, Male, Motor Activity, Sedentary Lifestyle, Motor Activity, sedentary behaviours, Diabetes Mellitus, Type 1, Italy, Humans, Female, analysis, Humans, Italy, blood/psychology/therapy, Female, Health Behavior, Hemoglobin A, Sedentary Behavior, Child, Type 1
Abstract

BACKGROUND: Regular Physical Activity (RPA) is one of the cornerstones of Type 1 Diabetes (T1D) therapy, but conflicting results are reported in the literature. AIM: To compare (RPA) and Sedentary Lifestyle (SL) among children with type 1 diabetes (T1D) and healthy peers. SUBJECTS AND METHODS: Seven Italian paediatric diabetes centres enrolled 129 children with T1D and 214 healthy peers who were interviewed by a telephone questionnaire on physical activity level, sedentary lifestyle and clinical data. RESULTS: Compared to healthy peers, children with T1D: performed the same amount of RPA, were more frequently engaged in team sports (p = 0.018), described RPA as an enjoyable activity (p = 0.033), not boring (p = 0.035), a chance to spend time with peers (p = 0.033) and to meet new friends (p = 0.016). Children with T1D were finally used to consume less snacks during watching TV (p < 0.001) or after physical activity (p < 0.001 ). HbA1c values were not related with time spent in physical activity, in watching TV or in playing video-games. CONCLUSIONS: Most interviewed children with T1D are physically active and perform the same amount of exercise as their healthy peers. They demonstrate to consider RPA a source of enjoyment and sociality and not a therapeutic imposition.

Published
2011

21. Planck intermediate results: XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization

Author

Ade, P. A. R., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Zotti, G., Delabrouille, J., Désert, F. -X., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, Guilaine, Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J.F., Maffei, B., Magalhães, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Pietrobon, D., Plaszczynski, Stéphane, Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Salerno, E., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, Radek, Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wandelt, B. D., Zacchei, A., Zonca, A., 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), 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), 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), 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 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), PLANCK, European Space Agency, European Research Council, Centre National de la Recherche Scientifique (France), Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Fundação para a Ciência e a Tecnologia (Portugal), Science Foundation Ireland, Research Council of Norway, DTU Space (Denmark), Federal Ministry of Education and Research (Germany), Academy of Finland, Center for Science (Finland), Junta de Andalucía, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), Science and Technology Facilities Council (UK), UK Space Agency, Consiglio Nazionale delle Ricerche, National Aeronautics and Space Administration (US), Department of Energy (US), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), École normale supérieure - Paris (ENS-PSL), 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), Department of Physics, Helsinki Institute of Physics, Ade, P, Alves, M, Aniano, G, Armitage-Caplan, C, Arnaud, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bock, J, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Burigana, C, Cardoso, J, Catalano, A, Chamballu, A, Chiang, H, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Zotti, G, Delabrouille, J, Desert, F, Dickinson, C, Diego, J, Donzelli, S, Dore, O, Douspis, M, Dunkley, J, Dupac, X, Ensslin, T, Eriksen, H, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Harrison, D, Helou, G, Hernandez-Monteagudo, C, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Jaffe, A, Jaffe, T, Jones, W, Keihanen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lawrence, C, Leahy, J, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maffei, B, Magalhaes, A, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Noviello, F, Novikov, D, Novikov, I, Oppermann, N, Oxborrow, C, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Popa, L, Pratt, G, Rachen, J, Reach, W, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rubino-Martin, J, Rusholme, B, Salerno, E, Sandri, M, Savini, G, Scott, D, Spencer, L, Stolyarov, V, Stompor, R, Sudiwala, R, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wandelt, B, Zacchei, A, Zonca, A, Ade, P. A. R., Alves, M. I. R., Aniano, G., Armitage Caplan, C., Arnaud, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Burigana, C., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, H. C., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Zotti, G., Delabrouille, J., Désert, F. X., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Lawrence, C. R., Leahy, J. P., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maffei, B., Magalhães, A. M., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubiño Martín, J. A., Rusholme, B., Salerno, E., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wandelt, B. D., Zacchei, A., Zonca, A., 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)-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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)

Subjects
Astronomy, WMAP OBSERVATIONS, Astrophysics, 7. Clean energy, law.invention, law, Polarization, Astrophysics::Solar and Stellar Astrophysics, general [radiation mechanisms], QB, Physics, Infrared: ISM, general [ISM], FOREGROUND EMISSION, general [mechanisms], ISM [infrared], Polarization (waves), DMR SKY MAPS, CMB cold spot, Synchrotron, INFRAVERMELHO, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, symbols, Spectral energy distribution, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, INTERSTELLAR DUST, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COMPONENT SEPARATION, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy: general, ISM: general, Radiation mechanisms: general, Submillimeter: ISM, NO, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, Planck, ISM [submillimeter], general [Galaxy], Astrophysics::Galaxy Astrophysics, Cosmic dust, SUBMILLIMETER POLARIZATION, MAGNETIC NANOPARTICLES, polarization, SPINNING DUST, Astronomy and Astrophysics, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, MICROWAVE-ANISOTROPY-PROBE, Interstellar medium, radiation, polarization / ISM: general / Galaxy: general / radiation mechanisms: general / submillimeter: ISM / infrared: ISM, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), H-ALPHA EMISSION, Microwave
Abstract

Interstellar and circumstellar matter.-- et al., Planck has mapped the intensity and polarization of the sky at microwave frequencies with unprecedented sensitivity. We use these data to characterize the frequency dependence of dust emission. We make use of the Planck 353 GHz I, Q, and U Stokes maps as dust templates, and cross-correlate them with the Planck and WMAP data at 12 frequencies from 23 to 353 GHz, over circular patches with 10° radius. The cross-correlation analysis is performed for both intensity and polarization data in a consistent manner. The results are corrected for the chance correlation between the templates and the anisotropies of the cosmic microwave background. We use a mask that focuses our analysis on the diffuse interstellar medium at intermediate Galactic latitudes. We determine the spectral indices of dust emission in intensity and polarization between 100 and 353 GHz, for each sky patch. Both indices are found to be remarkably constant over the sky. The mean values, 1.59 ± 0.02 for polarization and 1.51 ± 0.01 for intensity, for a mean dust temperature of 19.6 K, are close, but significantly different (3.6σ). We determine the mean spectral energy distribution (SED) of the microwave emission, correlated with the 353 GHz dust templates, by averaging the results of the correlation over all sky patches. We find that the mean SED increases for decreasing frequencies at ν< 60 GHz for both intensity and polarization. The rise of the polarization SED towards low frequencies may be accounted for by a synchrotron component correlated with dust, with no need for any polarization of the anomalous microwave emission. We use a spectral model to separate the synchrotron and dust polarization and to characterize the spectral dependence of the dust polarization fraction. The polarization fraction (p) of the dust emission decreases by (21 ± 6)% from 353 to 70 GHz. We discuss this result within the context of existing dust models. The decrease in p could indicate differences in polarization efficiency among components of interstellar dust (e.g., carbon versus silicate grains). Our observational results provide inputs to quantify and optimize the separation between Galactic and cosmological polarization., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and J.A. (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934.

Published
2015
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23. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Author

Ade, P.A.R., Aghanim, N., Alina, D., Alves, M.I.R., Aniano, G., Armitage-Caplan, C., Arnaud, Martha B., Arzoumanian, D., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., 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., Dickinson, C., Diego, J.M., Donzelli, S., Dore, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gonzalez-Nuevo, J., Gorski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Harrison, D., Helou, G., Hernandez-Monteagudo, C., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Huffenberger, K.M., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschenes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.Anthony, Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C.A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V.-M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G.W., Prunet, S., Puget, J.-L., Rachen, J.P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J.D., Spencer, L., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Zonca, A., Ade, P.A.R., Aghanim, N., Alina, D., Alves, M.I.R., Aniano, G., Armitage-Caplan, C., Arnaud, Martha B., Arzoumanian, D., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., 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., Dickinson, C., Diego, J.M., Donzelli, S., Dore, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gonzalez-Nuevo, J., Gorski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Harrison, D., Helou, G., Hernandez-Monteagudo, C., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Huffenberger, K.M., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschenes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.Anthony, Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C.A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V.-M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G.W., Prunet, S., Puget, J.-L., Rachen, J.P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J.D., Spencer, L., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., and Zonca, A.

Published
2015

24. Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible

Author

Ade, P.A.R., Aghanim, N., Alina, D., Aniano, G., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Battaner, E., Beichman, C., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chary, R.-R., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., 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., Desert, F.-X., Dickinson, C., Diego, J.M., Donzelli, S., Dore, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gonzalez-Nuevo, J., Gorski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Harrison, D., Helou, G., Hernandez-Monteagudo, C., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Huffenberger, K.M., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J.-M., Lasenby, A., Lawrence, C.R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maffei, B., Magalhães, A.M., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschenes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.Anthony, Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C.A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Poidevin, F., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G.W., Prunet, S., Puget, J.-L., Rachen, J.P., Reach, W.T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Zonca, A., Ade, P.A.R., Aghanim, N., Alina, D., Aniano, G., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Battaner, E., Beichman, C., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bock, J.J., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chary, R.-R., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., 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., Desert, F.-X., Dickinson, C., Diego, J.M., Donzelli, S., Dore, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Fanciullo, L., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., Gonzalez-Nuevo, J., Gorski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Harrison, D., Helou, G., Hernandez-Monteagudo, C., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hornstrup, A., Huffenberger, K.M., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J.-M., Lasenby, A., Lawrence, C.R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maffei, B., Magalhães, A.M., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschenes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.Anthony, Naselsky, P., Nati, F., Natoli, P., Netterfield, C.B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C.A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Poidevin, F., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G.W., Prunet, S., Puget, J.-L., Rachen, J.P., Reach, W.T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., and Zonca, A.

Published
2015

25. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Author

Cardoso, J. F., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Piat, M., Remazeilles, M., Rosset, C., Roudier, G., Stompor, R., Kunz, M., Natoli, P., Polenta, G., Mandolesi, N., Ashdown, M., Curto, A., Hobson, M., Lasenby, A., Stolyarov, V., Chiang, H.C., Kneissl, R., Bond, J.R., Martin, P. G., Miville-Deschênes, M. A., Alina, D., Banday, A.J., Bernard, J.-P., Bielewicz, P., Ferrière, K., Forni, O., Giard, M., Jaffe, T.R., Montier, L., Pointecouteau, E., Ristorcelli, I., Doré, O., Helou, G., Hildebrandt, S.R., Rocha, G., Hernández-Monteagudo, C., Borrill, J., Keskitalo, R., Chamballu, A., Hornstrup, Allan, Linden-Vørnle, Michael, Oxborrow, Carol Anne, Tucci, M., Atrio-Barandela, F., Toffolatti, L., Netterfield, C.B., Rachen, J.P., Scott, D., Colombo, L.P.L., Benoit-Lévy, A., Huffenberger, K.M., Juvela, M., Keihänen, E., Kurki-Suonio, H., Suur-Uski, A. S., Valiviita, J., Fraisse, A. A., Jones, W.C., Lubin, P.M., Zonca, A., Wandelt, B.D., Liguori, M., Matarrese, S., Burigana, C., De Bernardis, P., Masi, S., Melchiorri, A., Nati, F., Pagano, L., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Mazzotta, P., Christensen, P.R., Naselsky, P., Dupac, X., Leonardi, R., Mendes, L., Tauber, J.A., Umana, G., De Zotti, G., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Morgante, G., Paoletti, D., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Jaffe, A.H., Mortlock, D., Novikov, D., Pelkonen, V. M., Rusholme, B., Aghanim, N., Alves, M.I.R., Aniano, G., Arzoumanian, D., Aumont, J., Boulanger, F., Bracco, A., Douspis, M., Fanciullo, L., Ghosh, T., Guillet, V., Lagache, G., Pajot, Fernand, Puget, J. L., Soler, J. D., Benabed, K., Bouchet, F.R., Colombi, S., Hivon, E., Moneti, A., Prunet, S., Sygnet, J. F., Popa, L., Efstathiou, G., Harrison, D.L., Migliaccio, M., Sutton, D., Eriksen, H.K., Hansen, F. K., Lilje, P.B., Barreiro, R.B., Diego, J.M., González-Nuevo, J., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Pietrobon, D., Wade, L.A., Davies, R.D., Davis, R. J., Dickinson, C., Noviello, F., Couchot, F., Perdereau, O., Plaszczynski, S., Tristram, M., Catalano, A., Coulais, A., Falgarone, E., Lamarre, J. M., Levrier, F., Arnaud, M., Marshall, D.J., Pratt, G.W., Combet, C., Macías-Pérez, J.F., Perotto, L., Renault, C., Van Tent, B., Kisner, T.S., Enßlin, T.A., Knoche, J., Reinecke, M., Riller, T., Murphy, J.A., Novikov, I., Baccigalupi, C., Danese, L., Perrotta, F., Ade, P.A.R., Munshi, D., Spencer, L.D., Sudiwala, R., Armitage-Caplan, C., Battaner, E., Cardoso, J. F., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Piat, M., Remazeilles, M., Rosset, C., Roudier, G., Stompor, R., Kunz, M., Natoli, P., Polenta, G., Mandolesi, N., Ashdown, M., Curto, A., Hobson, M., Lasenby, A., Stolyarov, V., Chiang, H.C., Kneissl, R., Bond, J.R., Martin, P. G., Miville-Deschênes, M. A., Alina, D., Banday, A.J., Bernard, J.-P., Bielewicz, P., Ferrière, K., Forni, O., Giard, M., Jaffe, T.R., Montier, L., Pointecouteau, E., Ristorcelli, I., Doré, O., Helou, G., Hildebrandt, S.R., Rocha, G., Hernández-Monteagudo, C., Borrill, J., Keskitalo, R., Chamballu, A., Hornstrup, Allan, Linden-Vørnle, Michael, Oxborrow, Carol Anne, Tucci, M., Atrio-Barandela, F., Toffolatti, L., Netterfield, C.B., Rachen, J.P., Scott, D., Colombo, L.P.L., Benoit-Lévy, A., Huffenberger, K.M., Juvela, M., Keihänen, E., Kurki-Suonio, H., Suur-Uski, A. S., Valiviita, J., Fraisse, A. A., Jones, W.C., Lubin, P.M., Zonca, A., Wandelt, B.D., Liguori, M., Matarrese, S., Burigana, C., De Bernardis, P., Masi, S., Melchiorri, A., Nati, F., Pagano, L., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Mazzotta, P., Christensen, P.R., Naselsky, P., Dupac, X., Leonardi, R., Mendes, L., Tauber, J.A., Umana, G., De Zotti, G., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Morgante, G., Paoletti, D., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Jaffe, A.H., Mortlock, D., Novikov, D., Pelkonen, V. M., Rusholme, B., Aghanim, N., Alves, M.I.R., Aniano, G., Arzoumanian, D., Aumont, J., Boulanger, F., Bracco, A., Douspis, M., Fanciullo, L., Ghosh, T., Guillet, V., Lagache, G., Pajot, Fernand, Puget, J. L., Soler, J. D., Benabed, K., Bouchet, F.R., Colombi, S., Hivon, E., Moneti, A., Prunet, S., Sygnet, J. F., Popa, L., Efstathiou, G., Harrison, D.L., Migliaccio, M., Sutton, D., Eriksen, H.K., Hansen, F. K., Lilje, P.B., Barreiro, R.B., Diego, J.M., González-Nuevo, J., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Pietrobon, D., Wade, L.A., Davies, R.D., Davis, R. J., Dickinson, C., Noviello, F., Couchot, F., Perdereau, O., Plaszczynski, S., Tristram, M., Catalano, A., Coulais, A., Falgarone, E., Lamarre, J. M., Levrier, F., Arnaud, M., Marshall, D.J., Pratt, G.W., Combet, C., Macías-Pérez, J.F., Perotto, L., Renault, C., Van Tent, B., Kisner, T.S., Enßlin, T.A., Knoche, J., Reinecke, M., Riller, T., Murphy, J.A., Novikov, I., Baccigalupi, C., Danese, L., Perrotta, F., Ade, P.A.R., Munshi, D., Spencer, L.D., Sudiwala, R., Armitage-Caplan, C., and Battaner, E.

Published
2015

26. Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible

Author

Cardoso, J.F., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Piat, M., Remazeilles, M., Rosset, C., Roudier, G., Stompor, R., Lähteenmäki, A., Kunz, M., Natoli, P., Polenta, G., Mandolesi, N., Ashdown, M., Curto, A., Hobson, M., Lasenby, A., Stolyarov, V., Chiang, H.C., Kneissl, R., Bond, J.R., Martin, P.G., Miville-Deschênes, M.A., Alina, D., Banday, A.J., Bernard, J.P., Bielewicz, P., Forni, O., Giard, M., Jaffe, T.R., Montier, L., Pointecouteau, E., Ristorcelli, I., Beichman, C., Bock, J.J., Doré, O., Helou, G., Hildebrandt, S.R., Rocha, G., Hernández-Monteagudo, C., Borrill, J., Keskitalo, R., Rebolo, R., Chamballu, A., Hornstrup, Allan, Linden-Vørnle, Michael, Oxborrow, Carol Anne, Tucci, M., Atrio-Barandela, F., Toffolatti, L., Netterfield, C.B., Rachen, J.P., Scott, D., Colombo, L.P.L., Benoit-Lévy, A., Poidevin, F., Huffenberger, K.M., Juvela, M., Keihänen, E., Kurki-Suonio, H., Suur-Uski, A.-S., Valiviita, J., Fraisse, A.A., Jones, W.C., Lubin, P.M., Zonca, A., Wandelt, B.D., Liguori, M., Matarrese, S., Burigana, C., De Bernardis, P., Masi, S., Melchiorri, A., Nati, F., Pagano, L., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Mazzotta, P., Christensen, P. R., Naselsky, P., Dupac, X., Leonardi, R., Mendes, L., Tauber, J.A., Umana, G., De Zotti, G., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Morgante, G., Paoletti, D., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Désert, F.X., Jaffe, A.H., Mortlock, D., Novikov, D., Chary, R.R., Paladini, R., Rusholme, B., Aghanim, N., Aniano, G., Aumont, J., Boulanger, F., Douspis, M., Fanciullo, L., Ghosh, T., Guillet, V., Lagache, G., Pajot, Fernand, Puget, J.L., Benabed, K., Bouchet, F.R., Colombi, S., Hivon, E., Moneti, A., Prunet, S., Sygnet, J. F., Popa, L., Efstathiou, G., Harrison, D.L., Migliaccio, M., Sutton, D., Eriksen, H.K., Hansen, F.K., Lilje, P.B., Magalhães, A.M., Barreiro, R.B., Diego, J.M., González-Nuevo, J., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Pietrobon, D., Wade, L.A., Davies, R.D., Davis, R.J., Dickinson, C., Maffei, B., Noviello, F., Couchot, F., Perdereau, O., Plaszczynski, S., Tristram, M., Catalano, A., Coulais, A., Falgarone, E., Lamarre, J. M., Levrier, F., Arnaud, M., Marshall, D.J., Pratt, G.W., Combet, C., Macías-Pérez, J.F., Perotto, L., Renault, C., Van Tent, B., Kisner, T.S., Enßlin, T.A., Knoche, J., Reinecke, M., Riller, T., Murphy, J.A., Novikov, I., Savini, G., Baccigalupi, C., Danese, L., Perrotta, F., Ade, P.A.R., Munshi, D., Spencer, L.D., Sudiwala, R., Armitage-Caplan, C., Dunkley, J., Reach, W.T., Battaner, E., Cardoso, J.F., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Piat, M., Remazeilles, M., Rosset, C., Roudier, G., Stompor, R., Lähteenmäki, A., Kunz, M., Natoli, P., Polenta, G., Mandolesi, N., Ashdown, M., Curto, A., Hobson, M., Lasenby, A., Stolyarov, V., Chiang, H.C., Kneissl, R., Bond, J.R., Martin, P.G., Miville-Deschênes, M.A., Alina, D., Banday, A.J., Bernard, J.P., Bielewicz, P., Forni, O., Giard, M., Jaffe, T.R., Montier, L., Pointecouteau, E., Ristorcelli, I., Beichman, C., Bock, J.J., Doré, O., Helou, G., Hildebrandt, S.R., Rocha, G., Hernández-Monteagudo, C., Borrill, J., Keskitalo, R., Rebolo, R., Chamballu, A., Hornstrup, Allan, Linden-Vørnle, Michael, Oxborrow, Carol Anne, Tucci, M., Atrio-Barandela, F., Toffolatti, L., Netterfield, C.B., Rachen, J.P., Scott, D., Colombo, L.P.L., Benoit-Lévy, A., Poidevin, F., Huffenberger, K.M., Juvela, M., Keihänen, E., Kurki-Suonio, H., Suur-Uski, A.-S., Valiviita, J., Fraisse, A.A., Jones, W.C., Lubin, P.M., Zonca, A., Wandelt, B.D., Liguori, M., Matarrese, S., Burigana, C., De Bernardis, P., Masi, S., Melchiorri, A., Nati, F., Pagano, L., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Mazzotta, P., Christensen, P. R., Naselsky, P., Dupac, X., Leonardi, R., Mendes, L., Tauber, J.A., Umana, G., De Zotti, G., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Morgante, G., Paoletti, D., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Désert, F.X., Jaffe, A.H., Mortlock, D., Novikov, D., Chary, R.R., Paladini, R., Rusholme, B., Aghanim, N., Aniano, G., Aumont, J., Boulanger, F., Douspis, M., Fanciullo, L., Ghosh, T., Guillet, V., Lagache, G., Pajot, Fernand, Puget, J.L., Benabed, K., Bouchet, F.R., Colombi, S., Hivon, E., Moneti, A., Prunet, S., Sygnet, J. F., Popa, L., Efstathiou, G., Harrison, D.L., Migliaccio, M., Sutton, D., Eriksen, H.K., Hansen, F.K., Lilje, P.B., Magalhães, A.M., Barreiro, R.B., Diego, J.M., González-Nuevo, J., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Pietrobon, D., Wade, L.A., Davies, R.D., Davis, R.J., Dickinson, C., Maffei, B., Noviello, F., Couchot, F., Perdereau, O., Plaszczynski, S., Tristram, M., Catalano, A., Coulais, A., Falgarone, E., Lamarre, J. M., Levrier, F., Arnaud, M., Marshall, D.J., Pratt, G.W., Combet, C., Macías-Pérez, J.F., Perotto, L., Renault, C., Van Tent, B., Kisner, T.S., Enßlin, T.A., Knoche, J., Reinecke, M., Riller, T., Murphy, J.A., Novikov, I., Savini, G., Baccigalupi, C., Danese, L., Perrotta, F., Ade, P.A.R., Munshi, D., Spencer, L.D., Sudiwala, R., Armitage-Caplan, C., Dunkley, J., Reach, W.T., and Battaner, E.

Published
2015

29. Prostate vascular flow: The effect of the ejaculation on the power doppler ultrasonographic examination.

Author

Alonge, S., Melandri, M., Fanciullo, L., Lacalandra, G. M., and Aiudi, G.

Subjects
DOG diseases, PROSTATE disease diagnosis, EJACULATION, BLOOD flow measurement, DOPPLER ultrasonography
Abstract

Contents: Power Doppler sonography (PD) can accurately depict tissue perfusion, recognize slow flows, and is relatively angle independent. The monitoring of local blood flow by Doppler ultrasonography is helpful in differentiating prostatic physio‐pathological conditions, but the recognizing of physiological variables that could affect it is crucial to apply this technique in clinical practice. This study aimed to evaluate if ejaculation affects blood flow to the prostate and to state how long this effect lasts. Serial PD examinations of prostate were performed in 18 dogs (1–5 years, 6–40 kg) immediately before (T0) and after (T1) the ejaculation, and repeated 6 (T2), 18 (T3) and 24 (T4) hours later. For each examination, two representative PD images were chosen and ranked by two independent observers according to the following scoring system: 0 = mild subcapsular (S) vascularization without clear evidence of parenchymal (P) vascularization; 1 = moderate P and S vascularization; 2 = severe S and moderate P vascularization; 3 = severe P and moderate S vascularization; 4 = severe P and S vascularization. Interobserver agreement was assessed using Kappa of Cohen. Ranked data, grouped according to time, were compared by ANOVA and Tukey HSD test (p < .05). Variations in the vascular flow pattern at different times were observed for all dogs. The statistical analysis evidenced a significant difference for T0 vs T1 and vs T2 and vs T3 (p < .01), with no significant difference for T0 vs T4 (p > .05). Interobserver agreement was very good (Kappa of Cohen = 0.86). This study demonstrated a definite increase in vascular flow to the prostate after ejaculation. The present results suggest a minimum of 24 hr sexual rest before the PD examination of the gland. This result should be taken into account whenever Doppler sonography is used to evaluate potential hyperaemia in dogs suspected of having prostate abnormalities. [ABSTRACT FROM AUTHOR]

Published
2018
Full Text
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32. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Author

Ade, P. A. R., Aghanim, N., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Arzoumanian, D., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., 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., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V. -M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J. D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zonca, A., Macias-Perez, J.F., Ade, P. A. R., Aghanim, N., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Arzoumanian, D., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., 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., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V. -M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J. D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zonca, A., and Macias-Perez, J.F.

Abstract

Polarized emission observed by Planck HFI at 353 GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions $p$ and angles $\psi$. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction $p_\mathrm{max}$ decreases with column density $N_\mathrm{H}$ in the more opaque fields with $N_\mathrm{H} > 10^{21}\,\mathrm{cm}^{-2}$; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical (MHD) turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction $p_\mathrm{max}$ in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function $\Delta\psi$. [abridged]

34. Planck intermediate results. XX. Comparison of polarized thermal emission from Galactic dust with simulations of MHD turbulence

Author

A. Coulais, G. de Zotti, A. Benoit-Lévy, B. P. Crill, B. Van Tent, Francesca Perrotta, F. Atrio-Barandela, S. Ricciardi, T. Riller, Federico Nati, Anna Gregorio, R. B. Barreiro, A. Mennella, Y. Giraud-Héraud, Torsten A. Enßlin, Radek Stompor, Jörg P. Rachen, Allan Hornstrup, D. Sutton, X. Dupac, M. Tomasi, Ben Rusholme, Mika Juvela, D. Alina, Jacques Delabrouille, Rashmikant V. Sudiwala, Marc-Antoine Miville-Deschênes, Luca Terenzi, C. Combet, Doris Arzoumanian, Etienne Pointecouteau, Marco Bersanelli, A. De Rosa, L. Fanciullo, L. Popa, J.-F. Cardoso, Jose M. Diego, A. Moneti, Benjamin D. Wandelt, Julian Borrill, Eric Hivon, Stéphane Plaszczynski, Kevin M. Huffenberger, Katia Ferrière, H. K. Eriksen, Ken Ganga, F. Noviello, O. Doré, Gianluca Morgante, Carlo Burigana, Paolo Natoli, Fabio Finelli, M. Piat, Michael P. Hobson, L. A. Montier, C. A. Oxborrow, F. Boulanger, Fabrizio Villa, J.-P. Bernard, M. I. R. Alves, Alessandro Gruppuso, Pavel Naselsky, C. Armitage-Caplan, L. Mendes, Sabino Matarrese, W. Holmes, John Bond, Peter G. Martin, F. Piacentini, Douglas J. Marshall, Igor D. Novikov, A. Curto, E. Battaner, J.-M. Lamarre, Andrea Zonca, François R. Bouchet, Juan D. Soler, R. J. Davis, J. A. Tauber, D. L. Harrison, H. C. Chiang, George Helou, Luigi Danese, V. Stolyarov, Monique Arnaud, Hannu Kurki-Suonio, M. Migliaccio, R. Kneissl, A. Catalano, L. Pagano, Karim Benabed, Tuhin Ghosh, Charles R. Lawrence, M. Tucci, Enrique Martínez-González, F. Pajot, F. Couchot, T. R. Jaffe, Nabila Aghanim, F. Pasian, Alessandro Melchiorri, Andrea Bracco, R. D. Davies, P. B. Lilje, Peter A. R. Ade, G. Polenta, Clive Dickinson, V.-M. Pelkonen, I. Ristorcelli, G. Umana, Davide Pietrobon, Ted Kisner, M. Ashdown, Edith Falgarone, S. Donzelli, Marian Douspis, Davide Maino, A. A. Fraisse, G. Aniano, L. Toffolatti, Sergi R. Hildebrandt, L. P. L. Colombo, Anthony Lasenby, E. Keihänen, G. W. Pratt, Krzysztof M. Gorski, Calvin B. Netterfield, Stephane Colombi, Martin Kunz, P. R. Christensen, A. J. Banday, Dmitry Novikov, L. A. Wade, Daniela Paoletti, A. Chamballu, R. Leonardi, C. Rosset, G. Roudier, Dipak Munshi, Mathieu Remazeilles, George Efstathiou, Michele Liguori, M. Linden-Vørnle, Jussi Valiviita, Vincent Guillet, J. González-Nuevo, Silvia Masi, Locke D. Spencer, J. Knoche, Simon Prunet, P. Bielewicz, Olivier Forni, M. Frailis, M. Reinecke, Carlo Baccigalupi, François Levrier, C. Hernández-Monteagudo, F. K. Hansen, J.-F. Sygnet, Luca Valenziano, E. Franceschi, S. Galeotta, J. Aumont, J. F. Macías-Pérez, Graca Rocha, Douglas Scott, N. Mandolesi, Andrew H. Jaffe, Philip Lubin, P. de Bernardis, L. Perotto, O. Perdereau, A.-S. Suur-Uski, M. Giard, M. Maris, Reijo Keskitalo, Guilaine Lagache, M. López-Caniego, Daniel J. Mortlock, M. Sandri, P. Vielva, J. A. Murphy, Matthieu Tristram, Pasquale Mazzotta, C. Renault, F. Cuttaia, Jean-Loup Puget, W. C. Jones, Consejo Superior de Investigaciones Científicas (España), European Research Council, Junta de Andalucía, European Commission, Ministerio de Ciencia e Innovación (España), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Planck, Department of Physics, Helsinki Institute of Physics, Ade, P, Aghanim, N, Alina, D, Alves, M, Aniano, G, Armitage-Caplan, C, Arnaud, M, Arzoumanian, D, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit-Levy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bracco, A, Burigana, C, Cardoso, J, Catalano, A, Chamballu, A, Chiang, H, Christensen, P, Colombi, S, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Donzelli, S, Dore, O, Douspis, M, Dupac, X, Efstathiou, G, Ensslin, T, Eriksen, H, Falgarone, E, Fanciullo, L, Ferriere, K, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, F, Harrison, D, Helou, G, Hernandez-Monteagudo, C, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Huffenberger, K, Jaffe, A, Jaffe, T, Jones, W, Juvela, M, Keihanen, E, Keskitalo, R, Kisner, T, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Levrier, F, Liguori, M, Lilje, P, Linden-Vornle, M, Lopez-Caniego, M, Lubin, P, Macias-Perez, J, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martinez-Gonzalez, E, Masi, S, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Noviello, F, Novikov, D, Novikov, I, Oxborrow, C, Pagano, L, Pajot, F, Paoletti, D, Pasian, F, Pelkonen, V, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Popa, L, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rusholme, B, Sandri, M, Scott, D, Soler, J, Spencer, L, Stolyarov, V, Stompor, R, Sudiwala, R, Sutton, D, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, L, Wandelt, B, Zonca, A, Ade, P. A. R., Aghanim, N., Alina, D., Alves, M. I. R., Aniano, G., Armitage Caplan, C., Arnaud, M., Arzoumanian, D., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Cardoso, J. F., Catalano, A., Chamballu, A., Chiang, H. C., Christensen, P. R., Colombi, S., Colombo, L. P. L., Combet, C., 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., Dickinson, C., Diego, J. M., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Fanciullo, L., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gregorio, Anna, Gruppuso, A., Guillet, V., Hansen, F. K., Harrison, D. L., Helou, G., Hernández Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Kunz, M., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lasenby, A., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oxborrow, C. A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Pelkonen, V. M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Prunet, S., Puget, J. L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rusholme, B., Sandri, M., Scott, D., Soler, J. D., Spencer, L. D., Stolyarov, V., Stompor, R., Sudiwala, R., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zonca, A., Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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)-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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP)

Subjects
statistical [Methods], magnetic field [ISM], Astronomy, cloud [ISM], Astrophysics, 7. Clean energy, ISM: clouds, TAURUS, Anisotropy, ComputingMilieux_MISCELLANEOUS, QB, ASSOCIATIONS, Physics, infrared: ISM, Dust , extinction, Line-of-sight, general [ISM], extinction, ADAPTIVE MESH REFINEMENT, ISM [Submillimeter], Dust, SUBMILLIMETER EMISSION, Polarization (waves), Magnetic field, symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, submillimeter: ISM, INTERSTELLAR POLARIZATION, dust, extinction, ISM: magnetic fields, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Atomic physics, clouds [ISM], EFFICIENCY, Opacity, GRAIN ALIGNMENT, ISM [Infrared], FOS: Physical sciences, MAGNETIC-FIELDS, NO, Dust, extinction, Infrared: ISM, ISM: general, Submillimeter: ISM, Astronomy and Astrophysics, Space and Planetary Science, symbols.namesake, ISM: magnetic field, Settore FIS/05 - Astronomia e Astrofisica, ISM: cloud, RADIATIVE TORQUE ALIGNMENT, Planck, Astrophysics::Galaxy Astrophysics, Brewster's angle, numerical [Methods], magnetic fields [ISM], Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Observational [Methods], [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR CLOUDS, Magnetohydrodynamics
Abstract

et al., Polarized emission observed by Planck HFI at 353 GHz towards a sample of nearby fields is presented, focusing on the statistics of polarization fractions p and angles ψ. The polarization fractions and column densities in these nearby fields are representative of the range of values obtained over the whole sky. We find that: (i) the largest polarization fractions are reached in the most diffuse fields; (ii) the maximum polarization fraction pmax decreases with column density NH in the more opaque fields with NH> 1021 cm-2; and (iii) the polarization fraction along a given line of sight is correlated with the local spatial coherence of the polarization angle. These observations are compared to polarized emission maps computed in simulations of anisotropic magnetohydrodynamical turbulence in which we assume a uniform intrinsic polarization fraction of the dust grains. We find that an estimate of this parameter may be recovered from the maximum polarization fraction pmax in diffuse regions where the magnetic field is ordered on large scales and perpendicular to the line of sight. This emphasizes the impact of anisotropies of the magnetic field on the emerging polarization signal. The decrease of the maximum polarization fraction with column density in nearby molecular clouds is well reproduced in the simulations, indicating that it is essentially due to the turbulent structure of the magnetic field: an accumulation of variously polarized structures along the line of sight leads to such an anti-correlation. In the simulations, polarization fractions are also found to anti-correlate with the angle dispersion function . However, the dispersion of the polarization angle for a given polarization fraction is found to be larger in the simulations than in the observations, suggesting a shortcoming in the physical content of these numerical models. In summary, we find that the turbulent structure of the magnetic field is able to reproduce the main statistical properties of the dust polarization as observed in a variety of nearby clouds, dense cores excluded, and that the large-scale field orientation with respect to the line of sight plays a major role in the quantitative analysis of these statistical properties., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013) / ERC grant agreement No. 267934.

Published
2015
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35. Pregnancy Effect on Echocardiographic Parameters in Great Dane Bitches.

Author

Melandri M, Spalla I, Fanciullo L, and Alonge S

Abstract

Pregnancy is associated with adaptation of the left ventricular (LV) function. Due to differences between breeds in baseline echocardiographic values and specific predispositions for myocardial diseases, breed-specific echocardiographic parameters may be helpful to evaluate whether the systolic function varies during pregnancy. This study enrolled nine healthy Great Dane bitches with uncomplicated pregnancy. Echocardiographic M-mode and B-mode data were collected before ovulation and within 7 days of the predicted parturition term. Evaluated parameters were: LV dimension in diastole (LVd) and systole (LVs), end-diastolic (EDVI) and end-systolic (ESVI) volumes indexed to body surface area (BSA), end-diastolic (EDV) and end-systolic (ESV), end-point-septal-separation (EPSS), left atrium to aortic root ratio (LA/Ao), sphericity index (SI), ejection fraction (EF), fractional shortening (FS), stroke volume (SV), heart rate (HR), and cardiac output (CO). The ANOVA showed a statistical effect of the age of gestation ( p < 0.01) on the increase of diastolic dimensions and functional parameters and on the decrease of systolic dimensions. The CO increase parallels the rise in SV and HR ( p < 0.01). No statistical differences were observed for EPSS, LA/Ao, and SI. The changes in cardiac chambers and function are likely to reflect maternal adaptation to allow the fetal development in uncomplicated pregnancy. The present study provides specific echocardiographic values in uncomplicated pregnancy of Great Danes, showing that the systolic function is enhanced and that the increase in preload, observed during gestation, is the likely mechanism.

Published
2020
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36. Management of Corneal Bee Sting Injuries.

Author

Rai RR, Gonzalez-Gonzalez LA, Papakostas TD, Siracuse-Lee D, Dunphy R, Fanciullo L, Cakiner-Egilmez T, and Daly MK

Subjects
Administration, Topical, Corneal Injuries diagnosis, Corneal Pachymetry, Drug Therapy, Combination, Eye Foreign Bodies diagnosis, Follow-Up Studies, Humans, Insect Bites and Stings diagnosis, Male, Middle Aged, Tomography, Optical Coherence, Visual Acuity, Anti-Bacterial Agents administration & dosage, Cornea diagnostic imaging, Corneal Injuries therapy, Eye Foreign Bodies therapy, Glucocorticoids administration & dosage, Insect Bites and Stings therapy
Abstract

Purpose: To review the management of keratitis after corneal bee stings and to report a case of deep stromal corneal infiltrate secondary to a retained bee stinger managed conservatively in a patient who presented three days after unsanitary manipulation of the stinger apparatus., Methods: Case report and review of literature., Results: A 57-year-old male beekeeper was evaluated for pain, blurry vision, and photosensitivity after a corneal bee sting. Of note, the venom sac had been removed with dirty tweezers three days prior to his visit. On exam, a focal infiltrate with diffuse edema was seen surrounding a retained bee stinger in the peripheral cornea. Trace cells in the anterior chamber were also noted. Based on a high suspicion for infectious keratitis, a conservative treatment strategy was elected. Administration of broad-spectrum topical antibiotics with concomitant abstention of corticosteroids led to rapid resolution of the symptoms. Over 16 months of follow-up, the stinger has remained in situ without migration and the patient has maintained 20/20 visual acuity without complications. There is debate on the preferred method for the management of corneal injury secondary to bee stings, especially when it is associated with a retained stinger. We herein present our findings in our appraisal of reported cases., Conclusion: In the aftermath of an ocular bee sting, close surveillance for inflammation and infection is essential. Individual manifestations of these injuries vary in timing, type, and severity; therefore, the accessibility of the stinger and the evolving clinical picture should guide therapeutic decisions.

Published
2017
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37. The cycling of carbon into and out of dust.

Author

Jones AP, Ysard N, Köhler M, Fanciullo L, Bocchio M, Micelotta E, Verstraete L, and Guillet V

Abstract

Observational evidence seems to indicate that the depletion of interstellar carbon into dust shows rather wide variations and that carbon undergoes rather rapid recycling in the interstellar medium (ISM). Small hydrocarbon grains are processed in photo-dissociation regions by UV photons, by ion and electron collisions in interstellar shock waves and by cosmic rays. A significant fraction of hydrocarbon dust must therefore be re-formed by accretion in the dense, molecular ISM. A new dust model (Jones et al., Astron. Astrophys., 2013, 558, A62) shows that variations in the dust observables in the diffuse interstellar medium (n(H) < or = 10(3) cm(-3)), can be explained by systematic and environmentally-driven changes in the small hydrocarbon grain population. Here we explore the consequences of gas-phase carbon accretion onto the surfaces of grains in the transition regions between the diffuse ISM and molecular clouds (e.g., Jones, Astron. Astrophys., 2013, 555, A39). We find that significant carbonaceous dust re-processing and/or mantle accretion can occur in the outer regions of molecular clouds and that this dust will have significantly different optical properties from the dust in the adjacent diffuse ISM. We conclude that the (re-)processing and cycling of carbon into and out of dust is perhaps the key to advancing our understanding of dust evolution in the ISM.

Published
2014
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38. Children with type 1-diabetes from ethnic minorities: vulnerable patients needing a tailored medical support.

Author

Vanelli M, Cangelosi AM, Fanciullo L, Scarabello C, Monti G, Gkliati D, Mastrorilli C, Iovane B, and Chiari G

Subjects
Adolescent, Blood Glucose analysis, Child, Child, Preschool, Diabetes Mellitus, Type 1 therapy, Female, Glycated Hemoglobin analysis, Humans, Male, Diabetes Mellitus, Type 1 ethnology, Minority Groups
Abstract

Background and Aim: Newly diagnosed children with type 1 diabetes from ethnic minorities are a growing presence in outpatient pediatric clinics, and are reported as a group at risk of poor metabolic control. In the present study we investigated the barriers affecting chances of minority diabetic children to achieve the same metabolic targets of native peers with type 1 diabetes., Materials and Methods: The study investigated 35 children from ethnic minorities (group 1) admitted to the Children University Hospital of Parma, Italy, from 1st January 2000 to December 31st, 2011, and data concerning current age, gender, ethnicity, age at diabetes onset, HbA1c, DKA severity degree at diagnosis, insulin therapy, annual number of out patient clinic visits, number of admissions for acute decompensation, and treatment cost. A short questionnaire on background, family situation, difficulties in diabetes monitoring, and outpatient clinic procedures completed the study. The results were compared with data collected from 30 matched native peers (group 2)., Results: Mean HbA1c level at admittance was higher in Group 1 (11.8 +/- 1.0%) than in Group 2 (9.0 +/- 2.2%; p=0.000). The differences were confirmed when HbAlc mean cumulative values (8.6 +/- 2.1 vs 7.6 +/- 1.1; p=0.022) were calculated. Group 1 children at admission showed poorer metabolic conditions and longer stay at hospital (16 +/- 3 days) than Group 2 patients (8 +/- 2 days; p=0.000). The total costs for DKA treatment and family education resulted higher in group 1 (+54%) than in group 2 patients. Discontinuous capillary blood glucose monitoring and outpatient clinic visits missed were more frequent in Group 1 than in group 2 patients. Thirteen patients in group 1 needed a re-admittance to hospital because of a hypoglycemia (5 cases) or a hyperglycemia (8 cases). The same episodes were not recorded in group 2 patients. Most of parents expressed the wish to be supported with educational material in their own language., Conclusions: Children with TDM belonging to an ethnic minority had poorer metabolic control compared with native patients. This results from several cultural, educational, economic deficiencies which influence their family life and probably reduced their chances to obtain a better control.

Published
2012

39. Sulfonylurea-responsive neonatal diabetes mellitus diagnosed through molecular genetics in two children and in one adult after a long period of insulin treatment.

Author

Fanciullo L, Iovane B, Gkliati D, Monti G, Sponzilli I, Cangelosi AM, Matrorilli C, Chiari G, Barbetti F, Dall'Aglio E, and Vanelli M

Subjects
Child, Diabetes Mellitus diagnosis, Diabetes Mellitus genetics, Female, Humans, Infant, Newborn, Male, Mutation, Potassium Channels, Inwardly Rectifying genetics, Diabetes Mellitus drug therapy, Insulin therapeutic use, Sulfonylurea Compounds therapeutic use
Abstract

A permanent neonatal diabetes mellitus has finally been diagnosed through molecular genetics in two children and one adult after 9 to 35 years of uninterrupted insulin treatment. These patients developed diabetes before 6 months of age and were autoantibody negative. In one boy, a mutation in the KCNJ11 gene was identified at 9 years of age. In the other two patients (daughter and father, 12.6 and 25 years old respectively) the new gene variant (ABCC8/L213P) was found. Switching from insulin to sulfonylurea treatment leads to the definitive discontinuance of insulin therapy, improving metabolic control as well as the amelioration of the associated neurodevelopmental disabilities in the young girl in which an intermediate Development Delay, Epilepsy, Neonatal Diabetes syndrome was diagnosed.

Published
2012

40. Physical activity and sedentary lifestyle in children with type 1 diabetes: a multicentre Italian study.

Author

Fainardi V, Scarabello C, Cangelosi A, Fanciullo L, Mastrorilli C, Giannini C, Mohn A, Iafusco D, La Loggia A, Lombardo F, Toni S, Valerio G, Franzese A, Prisco F, Chiarelli F, and Vanelli M

Subjects
Adolescent, Child, Female, Glycated Hemoglobin analysis, Health Behavior, Humans, Italy epidemiology, Male, Motor Activity, Diabetes Mellitus, Type 1 blood, Diabetes Mellitus, Type 1 psychology, Diabetes Mellitus, Type 1 therapy, Sedentary Behavior
Abstract

Background: Regular Physical Activity (RPA) is one of the cornerstones of Type 1 Diabetes (T1D) therapy, but conflicting results are reported in the literature., Aim: To compare (RPA) and Sedentary Lifestyle (SL) among children with type 1 diabetes (T1D) and healthy peers., Subjects and Methods: Seven Italian paediatric diabetes centres enrolled 129 children with T1D and 214 healthy peers who were interviewed by a telephone questionnaire on physical activity level, sedentary lifestyle and clinical data., Results: Compared to healthy peers, children with T1D: performed the same amount of RPA, were more frequently engaged in team sports (p = 0.018), described RPA as an enjoyable activity (p = 0.033), not boring (p = 0.035), a chance to spend time with peers (p = 0.033) and to meet new friends (p = 0.016). Children with T1D were finally used to consume less snacks during watching TV (p < 0.001) or after physical activity (p < 0.001 ). HbA1c values were not related with time spent in physical activity, in watching TV or in playing video-games., Conclusions: Most interviewed children with T1D are physically active and perform the same amount of exercise as their healthy peers. They demonstrate to consider RPA a source of enjoyment and sociality and not a therapeutic imposition. (www.actabiomedica.it)

Published
2011

41. Differences between ethnic minority and native children in breakfast habits.

Author

Mont G, Gkliati D, Fanciullo L, Mastrorilli C, Finistrella V, Volta E, Ruggerini A, Ciati R, and Vanelli M

Subjects
Adolescent, Child, Female, Humans, Italy, Life Style, Male, Overweight ethnology, Risk Factors, Feeding Behavior ethnology, Minority Health
Abstract

Aim of this study was to investigate the breakfast habits in a cohort of school ethnic minority (EM) children admitted to a summer sport school (SSS) in order to evaluate the possible differences with their Italian peers (IP). One hundred-seventy-nine children aged 6-14 years were interviewed through a questionnaire about breakfast behaviors and nutrition habits. The results were compared with those obtained in a randomized sample of 179 Italian peers (IP) attending the same SSS. EM children skip breakfast more frequently than IP (15% vs 7%; p = 0.029). The omissions are attributed to the lack of time (45% vs 54%) and not being hungry upon waking (44% vs 38%). During weekends the percentage of breakfast skippers decreased of about 3 percentage points but persisted a significant difference between the two groups (p = 0.024). EM children who did not have breakfast show a mean BMI higher than breakfast consumers (p = 0.05). Bakery products and milk were the most frequently consumed food and drink in EM and IP children (68% vs 70% and 71% vs 76% respectively). EM children chose and prepared personally breakfast at home more frequently than IP (54% vs 22%). These EM children were more inclined to skip breakfast (p = 0.025) and to have an elevated BMI (p = 0.006) than IP. An educational program, for ethnic minority families, in different languages and according to their cultural, religious and socio-economic influences could be a possible means for changing their lifestyle and reducing their risk to become overweight.

Published
2011

42. Celiac disease in children with type 1 diabetes: impact of gluten free diet on diabetes management.

Author

Sponzilli I, Chiari G, Iovane B, Scarabello C, Gkliati D, Monti G, Fanciullo L, de'Angelis GL, and Vanelli M

Subjects
Adolescent, Case-Control Studies, Celiac Disease immunology, Child, Child, Preschool, Comorbidity, Female, Glycated Hemoglobin, Humans, Male, Retrospective Studies, Celiac Disease diet therapy, Celiac Disease epidemiology, Diabetes Mellitus, Type 1 epidemiology, Diet, Gluten-Free
Abstract

Unlabelled: Background and aim of the work the coexistence of Type 1 Diabetes (T1D) and celiac disease (CD) has been long established., Methods: Between January 2000 and December 2009, biopsy-proven CD was diagnosed in 12 children with T1D, giving a prevalence of 4.8 % in our out-patient clinic population. For each patient with coexisting T1D and CD, two control subjects with T1D and without CD who matched for age, sex and duration of diabetes were chosen. Prospective study follow up lasted 24 months. At the enrolment time, and at 2-month intervals, time from diagnosis of T1D to diagnosis of CD, presence of gastrointestinal symptoms, HbA1c value, body mass index (BMI), Height and Weight SDS were collected by a single observer. Daily insulin requirements were also retained., Results: In 3 children, CD predated the onset of T1D and these children were excluded from the analysis. The 9 children who subsequently developed CD became earlier diabetic than control group (p=0.002). Eight of these children had CD diagnosis within 1 year after T1D onset. Seven out of 9 children were positive for TTG antibodies and all were positive for EMA. A significant increase in insulin requirement was found in CD children after 1 year of GFD (p= 0.02). The mean HbAlc value in CD children was higher than in the control subjects (p<0.01).A significant increase in the insulin requirement after 1 year in the GFD compliant children was found. There was a significant improvement in height-SDS after institution of GFD in the GFD-compliant children. Families of children with both T1D and CD reported higher burden than those affected by T1D only (p=0.001). The health care providers perceived family burden to increase with CD appearance (p<0.05)., Conclusion: Our study supports the importance of screening for CD in children with T1D 1. The early treatment with GFD of biopsy-confirmed CD children promotes a significant catch-up growth and prevents a growth failure during the follow-up.

Published
2010

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