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@article{Ade:2015:0004-6361/201424955,
author = {Ade, PAR and Aghanim, N and Aniano, G and Arnaud, M and Ashdown, M and Aumont, J and Baccigalupi, C and Banday, AJ and Barreiro, RB and Bartolo, N and Battaner, E and Benabed, K and Benoit-Levy, A and Bernard, J-P and Bersanelli, M and Bielewicz, P and Bonaldi, A and Bonavera, L and Bond, JR and Borrill, J and Bouchet, FR and Boulanger, F and Burigana, C and Butler, RC and Calabrese, E and Cardoso, J-F and Casandjian, JM and Catalano, A and Chamballu, A and Chiang, HC and Christensen, PR and Colombo, LPL and Combet, C and Couchot, F and Crill, BP and Curto, A and Cuttaia, F and Danese, L 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 Digel, SW and Dole, H and Donzelli, S and Dore, O and Douspis, M and Ducout, A and Dupac, X and Efstathiou, G and Elsner, F and Ensslin, TA and Eriksen, HK and Falgarone, E and Finelli, F and Forni, O and Frailis, M and Fraisse, AA and Franceschi, E and },
doi = {0004-6361/201424955},
journal = {ASTRONOMY & ASTROPHYSICS},
title = {Planck intermediate results XXVIII. Interstellar gas and dust in the Chamaeleon clouds as seen by Fermi LAT and Planck},
url = {http://dx.doi.org/10.1051/0004-6361/201424955},
volume = {582},
year = {2015}
}

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TY  - JOUR
AB  - The nearby Chamaeleon clouds have been observed in γ rays by the Fermi Large Area Telescope (LAT) and in thermal dust emission by Planck and IRAS. Cosmic rays and large dust grains, if smoothly mixed with gas, can jointly serve with the H i and 12CO radio data to (i) map the hydrogen column densities, NH, in the different gas phases, in particular at the dark neutral medium (DNM) transition between the H i-bright and CO-bright media; (ii) constrain the CO-to-H2 conversion factor, XCO; and (iii) probe the dust properties per gas nucleon in each phase and map their spatial variations across the clouds. We have separated clouds at local, intermediate, and Galactic velocities in H i and 12CO line emission to model in parallel the γ-ray intensity recorded between 0.4 and 100 GeV; the dust optical depth at 353 GHz, τ353; the thermal radiance of the large grains; and an estimate of the dust extinction, AVQ, empirically corrected for the starlight intensity. The dust and γ-ray models have been coupled to account for the DNM gas. The consistent γ-ray emissivity spectra recorded in the different phases confirm that the GeV–TeV cosmic rays probed by the LAT uniformly permeate all gas phases up to the 12CO cores. The dust and cosmic rays both reveal large amounts of DNM gas, with comparable spatial distributions and twice as much mass as in the CO-bright clouds. We give constraints on the H i-DNM-CO transitions for five separate clouds. CO-dark H2 dominates the molecular columns up to AV  0.9 and its mass often exceeds the one-third of the molecular mass expected by theory. The corrected AVQ extinction largely provides the best fit to the total gas traced by the γ rays. Nevertheless, we find evidence for a marked rise in AVQ/NH with increasing NH and molecular fraction, and with decreasing dust temperature. The rise in τ353/NH is even steeper. We observe variations of lesser amplitude and orderlines
AU  - Ade,PAR
AU  - Aghanim,N
AU  - Aniano,G
AU  - Arnaud,M
AU  - Ashdown,M
AU  - Aumont,J
AU  - Baccigalupi,C
AU  - Banday,AJ
AU  - Barreiro,RB
AU  - Bartolo,N
AU  - Battaner,E
AU  - Benabed,K
AU  - Benoit-Levy,A
AU  - Bernard,J-P
AU  - Bersanelli,M
AU  - Bielewicz,P
AU  - Bonaldi,A
AU  - Bonavera,L
AU  - Bond,JR
AU  - Borrill,J
AU  - Bouchet,FR
AU  - Boulanger,F
AU  - Burigana,C
AU  - Butler,RC
AU  - Calabrese,E
AU  - Cardoso,J-F
AU  - Casandjian,JM
AU  - Catalano,A
AU  - Chamballu,A
AU  - Chiang,HC
AU  - Christensen,PR
AU  - Colombo,LPL
AU  - Combet,C
AU  - Couchot,F
AU  - Crill,BP
AU  - Curto,A
AU  - Cuttaia,F
AU  - Danese,L
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  - Digel,SW
AU  - Dole,H
AU  - Donzelli,S
AU  - Dore,O
AU  - Douspis,M
AU  - Ducout,A
AU  - Dupac,X
AU  - Efstathiou,G
AU  - Elsner,F
AU  - Ensslin,TA
AU  - Eriksen,HK
AU  - Falgarone,E
AU  - Finelli,F
AU  - Forni,O
AU  - Frailis,M
AU  - Fraisse,AA
AU  - Franceschi,E
AU  - Frejsel,A
AU  - Fukui,Y
AU  - Galeotta,S
AU  - Galli,S
AU  - Ganga,K
AU  - Ghosh,T
AU  - Giard,M
AU  - Gjerlow,E
AU  - Gonzalez-Nuevo,J
AU  - Gorski,KM
AU  - Gregorio,A
AU  - Grenier,IA
AU  - Gruppuso,A
AU  - Hansen,FK
AU  - Hanson,D
AU  - Harrison,DL
AU  - Henrot-Versill,S
AU  - Hernandez-Monteagudo,C
AU  - Herranz,D
AU  - Hildebrandt,SR
AU  - Hivon,E
AU  - Hobson,M
AU  - Holmes,WA
AU  - Hovest,W
AU  - Huffenberger,KM
AU  - Hurier,G
AU  - Jaffe,AH
AU  - Jaffe,TR
AU  - Jones,WC
AU  - Juvela,M
AU  - Keihaenen,E
AU  - Keskitalo,R
AU  - Kisner,TS
AU  - Kneissl,R
AU  - Knoche,J
AU  - Kunz,M
AU  - Kurki-Suonio,H
AU  - Lagache,G
AU  - Lamarre,J-M
AU  - Lasenby,A
AU  - Lattanzi,M
AU  - Lawrence,CR
AU  - Leonardi,R
AU  - Levrier,F
AU  - Liguori,M
AU  - Lilje,PB
AU  - Linden-Vornle,M
AU  - Lopez-Caniego,M
AU  - Lubin,PM
AU  - Macias-Perez,JF
AU  - Maffei,B
AU  - Maino,D
AU  - Mandolesi,N
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  - Natoli,P
AU  - Norgaard-Nielsen,HU
AU  - Novikov,D
AU  - Novikov,I
AU  - Oxborrow,CA
AU  - Pagano,L
AU  - Pajot,F
AU  - Paladini,R
AU  - Paoletti,D
AU  - Pasian,F
AU  - Perdereau,O
AU  - Perotto,L
AU  - Perrotta,F
AU  - Pettorino,V
AU  - Piacentini,F
AU  - Piat,M
AU  - Plaszczynski,S
AU  - Pointecouteau,E
AU  - Polenta,G
AU  - Popa,L
AU  - Pratt,GW
AU  - Prunet,S
AU  - Puget,J-L
AU  - Rachen,JP
AU  - Reach,WT
AU  - Rebolo,R
AU  - Reinecke,M
AU  - Remazeilles,M
AU  - Renault,C
AU  - Ristorcelli,I
AU  - Rocha,G
AU  - Roudier,G
AU  - Rusholme
DO  - 0004-6361/201424955
PY  - 2015///
SN  - 1432-0746
TI  - Planck intermediate results XXVIII. Interstellar gas and dust in the Chamaeleon clouds as seen by Fermi LAT and Planck
T2  - ASTRONOMY & ASTROPHYSICS
UR  - http://dx.doi.org/10.1051/0004-6361/201424955
UR  - http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000363538500031&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=1ba7043ffcc86c417c072aa74d649202
UR  - http://hdl.handle.net/10044/1/44006
VL  - 582
ER  -

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