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@article{Arnaud:2016:0004-6361/201425022,
author = {Arnaud, M and Ashdown, M and Atrio-Barandela, F and Aumont, J and Baccigalupi, C and Banday, AJ and Barreiro, RB and Battaner, E and Benabed, K and Benoit-Levy, A and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bobin, J and Bond, JR and Borrill, J and Bouchet, FR and Brogan, CL and Burigana, C and Cardoso, J-F and Catalano, A and Chamballu, A and Chiang, HC and Christensen, PR and Colombi, S and Colombo, LPL and Crill, BP and Curto, A and Cuttaia, F and Davies, RD and Davis, RJ and de, Bernardis P and de, Rosa A and de, Zotti G and Delabrouille, J and Desert, F-X and Dickinson, C and Diego, JM and Donzelli, S and Dore, O and Dupac, X and Ensslin, TA and Eriksen, HK and Finelli, F and Forni, O and Frailis, M and Fraisse, AA and Franceschi, E and Galeotta, S and Ganga, K and Giard, M and Giraud-Heraud, Y and Gonzalez-Nuevo, J and Gorski, KM and Gregorio, A and Gruppuso, A and Hansen, FK and Harrison, DL and Hernandez-Monteagudo, C and Herranz, D and Hildebrandt, SR and Hobson, M },
doi = {0004-6361/201425022},
journal = {Astronomy & Astrophysics},
title = {Planck intermediate results XXXI. Microwave survey of Galactic supernova remnants},
url = {http://dx.doi.org/10.1051/0004-6361/201425022},
volume = {586},
year = {2016}
}

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TY  - JOUR
AB  - The all-sky Planck survey in 9 frequency bands was used to search for emission from all 274 known Galactic supernova remnants. Of these, 16 were detected in at least two Planck frequencies. The radio-through-microwave spectral energy distributions were compiled to determine the mechanism for microwave emission. In only one case, IC 443, is there high-frequency emission clearly from dust associated with the supernova remnant. In all cases, the low-frequency emission is from synchrotron radiation. As predicted for a population of relativistic particles with energy distribution that extends continuously to high energies, a single power law is evident for many sources, including the Crab and PKS 1209-51/52. A decrease in flux density relative to the extrapolation of radio emission is evident in several sources. Their spectral energy distributions can be approximated as broken power laws, Sν ∝ ν−α, with the spectral index, α, increasing by 0.5–1 above a break frequency in the range 10–60 GHz. The break could be due to synchrotron losses.
AU  - Arnaud,M
AU  - Ashdown,M
AU  - Atrio-Barandela,F
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Battaner,E
AU  - Benabed,K
AU  - Benoit-Levy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bobin,J
AU  - Bond,JR
AU  - Borrill,J
AU  - Bouchet,FR
AU  - Brogan,CL
AU  - Burigana,C
AU  - Cardoso,J-F
AU  - Catalano,A
AU  - Chamballu,A
AU  - Chiang,HC
AU  - Christensen,PR
AU  - Colombi,S
AU  - Colombo,LPL
AU  - Crill,BP
AU  - Curto,A
AU  - Cuttaia,F
AU  - Davies,RD
AU  - Davis,RJ
AU  - de,Bernardis P
AU  - de,Rosa A
AU  - de,Zotti G
AU  - Delabrouille,J
AU  - Desert,F-X
AU  - Dickinson,C
AU  - Diego,JM
AU  - Donzelli,S
AU  - Dore,O
AU  - Dupac,X
AU  - Ensslin,TA
AU  - Eriksen,HK
AU  - Finelli,F
AU  - Forni,O
AU  - Frailis,M
AU  - Fraisse,AA
AU  - Franceschi,E
AU  - Galeotta,S
AU  - Ganga,K
AU  - Giard,M
AU  - Giraud-Heraud,Y
AU  - Gonzalez-Nuevo,J
AU  - Gorski,KM
AU  - Gregorio,A
AU  - Gruppuso,A
AU  - Hansen,FK
AU  - Harrison,DL
AU  - Hernandez-Monteagudo,C
AU  - Herranz,D
AU  - Hildebrandt,SR
AU  - Hobson,M
AU  - Holmes,WA
AU  - Huffenberger,KM
AU  - Jaffe,AH
AU  - Jaffe,TR
AU  - Keihaenen,E
AU  - Keskitalo,R
AU  - Kisner,TS
AU  - Kneissl,R
AU  - Knoche,J
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lahteenmaki,A
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Lawrence,CR
AU  - Leonardi,R
AU  - Liguori,M
AU  - Lilje,PB
AU  - Linden-Vornle,M
AU  - Lopez-Caniego,M
AU  - Lubin,PM
AU  - Maino,D
AU  - Maris,M
AU  - Marshall,DJ
AU  - Martin,PG
AU  - Martinez-Gonzalez,E
AU  - Masi,S
AU  - Matarrese,S
AU  - Mazzotta,P
AU  - Melchiorri,A
AU  - Mendes,L
AU  - Mennella,A
AU  - Migliaccio,M
AU  - Miville-Deschenes,M-A
AU  - Moneti,A
AU  - Montier,L
AU  - Morgante,G
AU  - Mortlock,D
AU  - Munshi,D
AU  - Murphy,JA
AU  - Naselsky,P
AU  - Nati,F
AU  - Noviello,E
AU  - Novikov,D
AU  - Novikov,I
AU  - Oppermann,N
AU  - Oxborrow,CA
AU  - Pagano,L
AU  - Pajot,F
AU  - Paladini,R
AU  - Pasian,F
AU  - Peel,M
AU  - Perdereau,O
AU  - Perrotta,F
AU  - Piacentini,F
AU  - Piat,M
AU  - Pietrobon,D
AU  - Plaszczynski,S
AU  - Pointecouteau,E
AU  - Polenta,G
AU  - Popa,L
AU  - Pratt,GW
AU  - Puget,J-L
AU  - Rachen,JP
AU  - Reach,WT
AU  - Reich,W
AU  - Reinecke,M
AU  - Remazeilles,M
AU  - Renault,C
AU  - Rho,J
AU  - Ricciardi,S
AU  - Riller,T
AU  - Ristorcelli,I
AU  - Rocha,G
AU  - Rosset,C
AU  - Roudier,G
AU  - Rusholme,B
AU  - Sandri,M
AU  - Savini,G
AU  - Scott,D
AU  - Stolyarov,V
AU  - Sutton,D
AU  - Suur-Uski,A-S
AU  - Sygnet,J-F
AU  - Tauber,JA
AU  - Terenzi,L
AU  - Toffolatti,L
AU  - Tomasi,M
AU  - Tristram,M
AU  - Tucci,M
AU  - Umana,G
AU  - Valenziano,L
AU  - Valiviita,J
AU  - Van,Tent B
AU  - Vielva,P
AU  - Villa,F
AU  - Wade,LA
AU  - Yvon,D
AU  - Zacchei,A
AU  - Zonca,A
DO  - 0004-6361/201425022
PY  - 2016///
SN  - 1432-0746
TI  - Planck intermediate results XXXI. Microwave survey of Galactic supernova remnants
T2  - Astronomy & Astrophysics
UR  - http://dx.doi.org/10.1051/0004-6361/201425022
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000369715900144&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/44007
VL  - 586
ER  -

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