<i>Planck</i>2013 results. XIV. Zodiacal emission

Ade, Peter A. R.; Aghanim, N.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoı̂t, A.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso, J.-F.; Catalano, A.; Chamballu, A.; Chary, R.-R.; Chen, X.; Chiang, H. C.; Chiang, L.-Y; Christensen, P. R.; Church, S.; Clements, D. L.; Colley, J.-M.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Bernardis, P. de; Rosa, A. De; Zotti, G. de; Delabrouille, J.; Delouis, J.-M.; Désert, F.‐X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli⋆, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giraud‐Héraud, Y.; González‐Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Hélou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; 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.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, Julien; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López‐Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martín, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M.-A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Mottet, S.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Новиков, И. Д.; Osborne, S.; O'Sullivan, Créidhe M.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, É.; Polegre, Arturo Martin; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; 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.; Rowan-Robinson, M.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Smoot, G. F.; Spencer, L. D.; Starck, Jean-Luc; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sureau, F.; Sutton, D.; Suur-Uski, A.-S.; Sygnet, J.-F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Väliviita, J.; Tent, B. Van; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.

doi:10.1051/0004-6361/201321562

Cited by 100 publications

(9 citation statements)

References 73 publications

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“…An obvious (subdominant) source of microwave radiation is the dust grains, and their emission might contribute to or modify the observed CMB anomalies [103][104][105]. The zodiacal cloud has been studied in detail for the Planck 2013 release [106] and the Planck team in its 2015 analysis subtracted a fit to the Kelsall model for the zodiacal cloud before map making [20]. The Kelsall model [107] attempts to capture the solar system dust emission in the infrared and microwaves and is based on the analysis of COBE DIRBE observations.…”

Section: Solar Systemmentioning

confidence: 99%

CMB anomalies after Planck

Schwarz

Copi

Huterer

et al. 2016

Class. Quantum Grav.

341

357

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Abstract. Several unexpected features have been observed in the microwave sky at large angular scales, both by WMAP an by Planck. Among those features is a lack of both variance and correlation on the largest angular scales, alignment of the lowest multipole moments with one another and with the motion and geometry of the Solar System, a hemispherical power asymmetry or dipolar power modulation, a preference for odd parity modes and an unexpectedly large cold spot in the Southern hemisphere. The individual p-values of the significance of these features are in the per mille to per cent level, when compared to the expectations of the best-fit inflationary ΛCDM model. Some pairs of those features are demonstrably uncorrelated, increasing their combined statistical significance and indicating a significant detection of CMB features at angular scales larger than a few degrees on top of the standard model. Despite numerous detailed investigations, we still lack a clear understanding of these large-scale features, which seem to imply a violation of statistical isotropy and scale invariance of inflationary perturbations. In this contribution we present a critical analysis of our current understanding and discuss several ideas of how to make further progress.

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Section: Solar Systemmentioning

confidence: 99%

CMB anomalies after Planck

Schwarz

Copi

Huterer

et al. 2016

Class. Quantum Grav.

341

357

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“…For the present study, the size distribution of cosmic dust particles was assumed to be represented by a broken power law with a differential index −2 to −3 below the break diameter D break and a differential index −4 to −5 above D break . COBE observations indicate that D break lies between 30 µm and 60 µm [ Fixsen and Dwek , ], which is supported by measurements of weak ZC emission at submillimeter wavelengths by the Planck telescope launched in 2009 [ Ade et al ., ]. Here we assume D break = 36 µm, which corresponds to a dust composition in between amorphous carbon ( D break ~ 28 µm) and silicate ( D break ~ 64 µm) [ Fixsen and Dwek , ].…”

Section: Mass and Velocity Distributions Of Dust From Different Sourcesmentioning

confidence: 99%

Sources of cosmic dust in the Earth's atmosphere

Carrillo‐Sánchez

Vokrouhlický

Pokorný

et al. 2016

Geophysical Research Letters

176

221

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There are four known sources of dust in the inner solar system: Jupiter Family comets, asteroids, Halley Type comets, and Oort Cloud comets. Here we combine the mass, velocity, and radiant distributions of these cosmic dust populations from an astronomical model with a chemical ablation model to estimate the injection rates of Na and Fe into the Earth's upper atmosphere, as well as the flux of cosmic spherules to the surface. Comparing these parameters to lidar observations of the vertical Na and Fe fluxes above 87.5 km, and the measured cosmic spherule accretion rate at South Pole, shows that Jupiter Family Comets contribute (80 ± 17)% of the total input mass (43 ± 14 t d −1 ), in good accord with Cosmic Background Explorer and Planck observations of the zodiacal cloud.

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“…Originally, Nesvorný et al (2011a) proposed D * = 100 μm to match the results derived from the measurements obtained with the Long Duration Exposure Facility (LDEF; Love & Brownlee 1993). However, in J15 we also investigated the case of D * = 30 μm derived from Planck satellite observations (Ade et al 2014), which provided better agreement to the radar observations because they implied that the characteristic particle mass of the incoming flux is about a factor of 27 smaller than the original ZoDy, and thus more easily made "undetectable. "…”

Section: Introductionmentioning

confidence: 99%

Radar Detectability Studies of Slow and Small Zodiacal Dust Cloud Particles. III. The Role of Sodium and the Head Echo Size on the Probability of Detection

Janches

Swarnalingam

Carrillo‐Sánchez

et al. 2017

ApJ

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We present a path forward on a long-standing issue concerning the flux of small and slow meteoroids, which are believed to be the dominant portion of the incoming meteoric mass flux into the Earth's atmosphere. Such a flux, which is predicted by dynamical dust models of the Zodiacal Cloud, is not evident in ground-based radar observations. For decades this was attributed to the fact that the radars used for meteor observations lack the sensitivity to detect this population, due to the small amount of ionization produced by slow-velocity meteors. Such a hypothesis has been challenged by the introduction of meteor head echo (HE) observations with High Power and Large Aperture radars, in particular the Arecibo 430 MHz radar. Janches et al. developed a probabilistic approach to estimate the detectability of meteors by these radars and initially showed that, with the current knowledge of ablation and ionization, such particles should dominate the detected rates by one to two orders of magnitude compared to the actual observations. In this paper, we include results in our model from recently published laboratory measurements, which showed that (1) the ablation of Na is less intense covering a wider altitude range; and (2) the ionization probability, b ip , for Na atoms in the air is up to two orders of magnitude smaller for low speeds than originally believed. By applying these results and using a somewhat smaller size of the HE radar target we offer a solution that reconciles these observations with model predictions.

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Planck2013 results. XIV. Zodiacal emission

Cited by 100 publications

References 73 publications

CMB anomalies after Planck

CMB anomalies after Planck

Sources of cosmic dust in the Earth's atmosphere

Radar Detectability Studies of Slow and Small Zodiacal Dust Cloud Particles. III. The Role of Sodium and the Head Echo Size on the Probability of Detection

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