<i>Planck</i>intermediate results

Arnaud, M.; 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.; Bobin, J.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Brogan, C. L.; Burigana, C.; Cardoso, J.-F.; Catalano, A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Colombi, S.; Colombo, L. P. L.; Crill, B. P.; Curto, A.; Cuttaia, F.; Davies, R. D.; Davis, R. J.; Bernardis, P. de; Rosa, A. de; Zotti, G. de; Delabrouille, J.; Désert, F.‐X.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Doré, O.; Dupac, X.; 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.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D. L.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hobson, M.; Holmes, W. A.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneißl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López‐Caniego, M.; Lubin, P. M.; Maino, D.; Maris, M.; Marshall, D. J.; Martín, 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, John A.; Naselsky, P.; Nati, F.; Noviello, F.; Novikov, D.; Новиков, И. Д.; Oppermann, N.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.; Pasian, F.; Peel, M.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, É.; Polenta, G.; Popa, L.; Pratt, G. W.; Puget, J.; Rachen, J. P.; Reach, W. T.; Reich, W.; Reinecke, M.; Remazeilles, M.; Renault, C.; Rho, Jeonghee; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Stolyarov, V.; 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.; Väliviita, J.; Tent, B. Van; Vielva, P.; Villa, F.; Wade, L. A.; Yvon, D.; Zacchei, A.; Zonca, A.

doi:10.1051/0004-6361/201425022

Cited by 54 publications

(5 citation statements)

References 64 publications

(65 reference statements)

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“…In Section 2.1, we reported that the broadband radio spectrum showed a spectral break at ν brk = 36 ± 6 GHz, at which the spectrum steepened from α 1 = 0.52 ± 0.02 to α 2 = 1.34 ± 0.21 by Δα = 0.85 ± 0.21. This result has confirmed the finding of Arnaud et al (2016). Notably, such a break in the spectral index is often seen as a result of synchrotron losses in various active galactic nuclei (e.g., Inoue & Takahara 1996;Kataoka et al 1999).…”

Section: Estimation Of the Magnetic Field Strengthsupporting

confidence: 84%

“…Based on SED modeling, the magnetic field strengths were estimated to be B SED ; 24 μG and 30 μG for the NE and SW shells, respectively. However, recent Planck observations indicated a spectral curvature above 10 GHz (Arnaud et al 2016); thus, the radio-to-X-ray spectrum may not connect smoothly as opposed to that determined by SED models by various authors. This is supported by the fact that the optical/ultraviolet (UV) counterpart of SN 1006 is extremely faint except for the bright Hα filament in the NW shell (Winkler et al 2003;Korreck et al 2004).…”

Section: Introductionmentioning

confidence: 80%

“…We analyzed all the archival Planck Low Frequency Instrument data containing 30, 44, and 70 GHz fluxes and 100 GHz data from the High Frequency Instrument to identify the high-frequency spectral features of SN 1006. Based on Arnaud et al (2016), the flux densities were measured using standard aperture photometry, with the source size centered on SN 1006 and the diameter scaled to θ ap = 1.5 θ s . Here, θ s is the source size estimated from θ s = q q + b SNR 2 2 , where θ SNR and θ b are the spatial distribution of SN 1006 and the Planck beam size (Ade et al 2014a;Aghanim et al 2014a), respectively.…”

Section: Broadband Radio Spectrummentioning

confidence: 99%

“…The uncertainties for the flux densities were the root sum square of calibration uncertainty (Ade et al 2014b;Aghanim et al 2014b) and propagated statistical errors. The statistical errors considered the number of pixels in the source aperture and background annulus and the standard deviation within the background annulus (Arnaud et al 2016).…”

Section: Broadband Radio Spectrummentioning

confidence: 99%

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Observational Evidence for Magnetic Field Amplification in SN 1006

Tao,

Kataoka,

Tanaka

2024

ApJL

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We report the first observational evidence for magnetic field amplification in the northeast/southwest (NE/SW) shells of supernova remnant SN 1006, one of the most promising sites of cosmic ray acceleration. In previous studies, the strength of magnetic fields in these shells was estimated to be B SED ≃ 25 μG from the spectral energy distribution, where the synchrotron emission from relativistic electrons accounted for radio to X-rays, along with the inverse Compton emission extending from the GeV to TeV energy bands. However, the analysis of broadband radio data, ranging from 1.37 to 100 GHz, indicated that the radio spectrum steepened from α 1 = 0.52 ± 0.02 to α 2 = 1.34 ± 0.21 by Δα = 0.85 ± 0.21. This is naturally interpreted as a cooling break under a strong magnetic field of B brk ≥ 2 mG. Moreover, the high-resolution MeerKAT image indicated that the width of the radio NE/SW shells was broader than that of the X-ray shell by a factor of only 3−20, as measured by Chandra. Such narrow radio shells can be naturally explained if the magnetic field responsible for the radio emissions is B R ≥ 2 mG. Assuming that the magnetic field is locally enhanced by a factor of approximately a = 100 along the NE/SW shells, we argue that the filling factor, which is the volume ratio of such a magnetically enhanced region to that of the entire shell, must be as low as approximately k = 2.5 × 10−5.

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Section: Estimation Of the Magnetic Field Strengthsupporting

confidence: 84%

Section: Introductionmentioning

confidence: 80%

Section: Broadband Radio Spectrummentioning

confidence: 99%

Section: Broadband Radio Spectrummentioning

confidence: 99%

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Observational Evidence for Magnetic Field Amplification in SN 1006

Tao,

Kataoka,

Tanaka

2024

ApJL

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“…The high precision cosmological observations [1][2][3][4][5] strongly suggest that the Universe is expanding, and surprisingly the nature of expansion is accelerating. Data also reveals that the onset of this acceleration is a recent phenomenon and has started at around z ∼ 0.5 [6,7].…”

Section: Introductionmentioning

confidence: 99%

Perturbation in an interacting dark universe

Sinha¹,

Banerjee²,

Das³

2022

Preprint

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In this paper we have considered an interacting model of dark energy and have looked into the evolution of the dark sectors. By solving the perturbation equations numerically, we have studied the imprints on the growth of matter as well as dark energy fluctuations. It has been found that for higher rate of interaction strength for the coupling term, visible imprints on the dark energy density fluctuations are observed at the early epochs of evolution.

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Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Kim

2020

Astron Nachr

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We investigate the broadband emission properties of the pulsar wind nebula (PWN) 3C 58 using a spectral energy distribution (SED) model. We attempt to match simultaneously the broadband SED and spatial variations of X‐ray emission in the PWN. We further use the model to explain a possible far‐IR feature of which a hint was recently suggested in 3C 58: a small bump at ∼1011 GHz in the PLANCK and Herschel bands. While external dust emission may easily explain the observed bump, it may be the internal emission of the source, implying an additional population of particles. Although significance for the bump is not high, here we explore possible origins of the IR bump using the emission model, and find that a population of electrons with GeV energies can explain it. If it is produced in the PWN, it may provide new insights into particle acceleration and flows in PWNe.

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Planckintermediate results

Cited by 54 publications

References 64 publications

Observational Evidence for Magnetic Field Amplification in SN 1006

Observational Evidence for Magnetic Field Amplification in SN 1006

Perturbation in an interacting dark universe

Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

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