Publication Date:
2014
abstract:
Rotational transition lines of CO play a major role in molecular radio
astronomy as a mass tracer and in particular in the study of star
formation and Galactic structure. Although a wealth of data exists for
the Galactic plane and some well-known molecular clouds, there is no
available high sensitivity all-sky survey of CO emission to date. Such
all-sky surveys can be constructed using the Planck HFI data because the
three lowest CO rotational transition lines at 115, 230 and 345 GHz
significantly contribute to the signal of the 100, 217 and 353 GHz HFI
channels, respectively. Two different component separation methods are
used to extract the CO maps from Planck HFI data. The maps obtained are
then compared to one another and to existing external CO surveys. From
these quality checks the best CO maps, in terms of signal to noise ratio
and/or residual contamination by other emission, are selected. Three
different sets of velocity-integrated CO emission maps are produced with
different trade-offs between signal-to-noise, angular resolution, and
reliability. Maps for the CO J = 1 --> 0, J = 2 --> 1, and J = 3
--> 2 rotational transitions are presented and described in detail.
They are shown to be fully compatible with previous surveys of parts of
the Galactic plane as well as with undersampled surveys of the high
latitude sky. The Planck HFI velocity-integrated CO maps for the J = 1
--> 0, J = 2 --> 1, and J = 3 -->2 rotational transitions
provide an unprecedented all-sky CO view of the Galaxy. These maps are
also of great interest to monitor potential CO contamination of the
Planck studies of the cosmological microwave background.
astronomy as a mass tracer and in particular in the study of star
formation and Galactic structure. Although a wealth of data exists for
the Galactic plane and some well-known molecular clouds, there is no
available high sensitivity all-sky survey of CO emission to date. Such
all-sky surveys can be constructed using the Planck HFI data because the
three lowest CO rotational transition lines at 115, 230 and 345 GHz
significantly contribute to the signal of the 100, 217 and 353 GHz HFI
channels, respectively. Two different component separation methods are
used to extract the CO maps from Planck HFI data. The maps obtained are
then compared to one another and to existing external CO surveys. From
these quality checks the best CO maps, in terms of signal to noise ratio
and/or residual contamination by other emission, are selected. Three
different sets of velocity-integrated CO emission maps are produced with
different trade-offs between signal-to-noise, angular resolution, and
reliability. Maps for the CO J = 1 --> 0, J = 2 --> 1, and J = 3
--> 2 rotational transitions are presented and described in detail.
They are shown to be fully compatible with previous surveys of parts of
the Galactic plane as well as with undersampled surveys of the high
latitude sky. The Planck HFI velocity-integrated CO maps for the J = 1
--> 0, J = 2 --> 1, and J = 3 -->2 rotational transitions
provide an unprecedented all-sky CO view of the Galaxy. These maps are
also of great interest to monitor potential CO contamination of the
Planck studies of the cosmological microwave background.
Iris type:
1.1 Articolo in rivista
Keywords:
ISM: molecules
List of contributors:
P., Collaboration; P. A., R.; N., Aghanim; M. I., R.; C., Armitage Caplan; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; C., Baccigalupi; A. J., Banday; R. B., Barreiro; J. G., Bartlett; E., Battaner; K., Benabed; A., Beno�t; A., Benoit L�vy; J., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; J. J., Bock; A., Bonaldi; J. R., Bond; J., Borrill; F. R., Bouchet; F., Boulanger; M., Bridges; M., Bucher; C., Burigana; R. C., Butler; J., Cardoso; A., Catalano; A., Chamballu; R., Chary; X., Chen; H. C., Chiang; L., Chiang; P. R., Christensen; S., Church; D. L., Clements; S., Colombi; L. P., L.; C., Combet; F., Couchot; A., Coulais; B. P., Crill; A., Curto; F., Cuttaia; L., Danese; R. D., Davies; P. d., Bernardis; A. d., Rosa; G. d., Zotti; J., Delabrouille; J., Delouis; J. T., Dempsey; F., D�sert; C., Dickinson; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; E., Falgarone; F., Finelli; O., Forni; M., Frailis; E., Franceschi; Y., Fukui; S., Galeotta; K., Ganga; M., Giard; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; T., Handa; F. K., Hansen; D., Hanson; D., Harrison; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; P., Hily Blant; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; G., Hurier; A. H., Jaffe; T. R., Jaffe; J., Jewell; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; A., L�hteenm�ki; J., Lamarre; A., Lasenby; R. J., Laureijs; C. R., Lawrence; R., Leonardi; Tavares, J. Le�n.; J., Lesgourgues; M., Liguori; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; P. M., Lubin; J. F., Mac�as P�rez; B., Maffei; N., Mandolesi; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; F., Matthai; P., Mazzotta; P., Mcgehee; A., Melchiorri; L., Mendes; A., Mennella; M., Migliaccio; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; T. J., T.; G., Morgante; J., Morino; D., Mortlock; D., Munshi; J. A., Murphy; T., Nakajima; P., Naselsky; F., Nati; P., Natoli; C. B., Netterfield; H. U., N�rgaard Nielsen; F., Noviello; D., Novikov; I., Novikov; T., Okuda; S., Osborne; C. A., Oxborrow; F., Paci; L., Pagano; F., Pajot; R., Paladini; D., Paoletti; F., Pasian; G., Patanchon; O., Perdereau; L., Perotto; F., Perrotta; F., Piacentini; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; G., Polenta; N., Ponthieu; L., Popa; T., Poutanen; G. W., Pratt; G., Pr�zeau; S., Prunet; J., Puget; J. P., Rachen; W. T., Reach; R., Rebolo; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; M., Rowan Robinson; Mart�n, J. A. Rubi�o.; B., Rusholme; M., Sandri; D., Santos; G., Savini; D., Scott; M. D., Seiffert; E. P., S.; L. D., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; R., Sunyaev; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; D., Tavagnacco; Terenzi, Luca; H. S., Thomas; L., Toffolatti; M., Tomasi; K., Torii; M., Tristram; M., Tucci; J., Tuovinen; G., Umana; L., Valenziano; J., Valiviita; B. V., Tent; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; I. K., Wehus; H., Yamamoto; T., Yoda; D., Yvon; A., Zacchei; A., Zonca
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