Data di Pubblicazione:
2013
Abstract:
We perform an analysis of the diffuse low-frequency Galactic components
in the southern part of the Gould Belt system (130� <= l <=
230� and -50� <= b <= -10�). Strong ultra-violet flux
coming from the Gould Belt super-association is responsible for bright
diffuse foregrounds that we observe from our position inside the system
and that can help us improve our knowledge of the Galactic emission.
Free-free emission and anomalous microwave emission (AME) are the
dominant components at low frequencies (nu < 40 GHz), while
synchrotron emission is very smooth and faint. We separated diffuse
free-free emission and AME from synchrotron emission and thermal dust
emission by using Planck data, complemented by ancillary data, using the
correlated component analysis (CCA) component-separation method and we
compared our results with the results of cross-correlation of foreground
templates with the frequency maps. We estimated the electron temperature
Te from Halpha and free-free emission using two methods
(temperature-temperature plot and cross-correlation) and obtained
Te ranging from 3100 to 5200K for an effective fraction of
absorbing dust along the line of sight of 30% (fd = 0.3). We
estimated the frequency spectrum of the diffuse AME and recovered a peak
frequency (in flux density units) of 25.5 � 1.5 GHz. We verified
the reliability of this result with realistic simulations that include
biases in the spectral model for the AME and in the free-free template.
By combining physical models for vibrational and rotational dust
emission and adding the constraints from the thermal dust spectrum from
Planck and IRAS, we are able to present a good description of the AME
frequency spectrum for plausible values of the local density and
radiation field.
Appendices are available in electronic form at
in the southern part of the Gould Belt system (130� <= l <=
230� and -50� <= b <= -10�). Strong ultra-violet flux
coming from the Gould Belt super-association is responsible for bright
diffuse foregrounds that we observe from our position inside the system
and that can help us improve our knowledge of the Galactic emission.
Free-free emission and anomalous microwave emission (AME) are the
dominant components at low frequencies (nu < 40 GHz), while
synchrotron emission is very smooth and faint. We separated diffuse
free-free emission and AME from synchrotron emission and thermal dust
emission by using Planck data, complemented by ancillary data, using the
correlated component analysis (CCA) component-separation method and we
compared our results with the results of cross-correlation of foreground
templates with the frequency maps. We estimated the electron temperature
Te from Halpha and free-free emission using two methods
(temperature-temperature plot and cross-correlation) and obtained
Te ranging from 3100 to 5200K for an effective fraction of
absorbing dust along the line of sight of 30% (fd = 0.3). We
estimated the frequency spectrum of the diffuse AME and recovered a peak
frequency (in flux density units) of 25.5 � 1.5 GHz. We verified
the reliability of this result with realistic simulations that include
biases in the spectral model for the AME and in the free-free template.
By combining physical models for vibrational and rotational dust
emission and adding the constraints from the thermal dust spectrum from
Planck and IRAS, we are able to present a good description of the AME
frequency spectrum for plausible values of the local density and
radiation field.
Appendices are available in electronic form at
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
Galaxy: general; radio continuum: ISM; radiation mechanisms: general
Elenco autori:
P., Collaboration; P. A., R.; N., Aghanim; M. I., R.; M., Arnaud; M., Ashdown; F., Atrio Barandela; J., Aumont; C., Baccigalupi; A., Balbi; A. J., Banday; R. B., Barreiro; J. G., Bartlett; E., Battaner; L., Bedini; K., Benabed; A., Beno�t; J., Bernard; M., Bersanelli; A., Bonaldi; J. R., Bond; J., Borrill; F. R., Bouchet; F., Boulanger; C., Burigana; R. C., Butler; P., Cabella; J., Cardoso; X., Chen; L., Chiang; P. R., Christensen; D. L., Clements; S., Colombi; L. P., L.; A., Coulais; F., Cuttaia; R. D., Davies; R. J., Davis; P. d., Bernardis; G. d., Gasperis; G. d., Zotti; J., Delabrouille; C., Dickinson; J. M., Diego; G., Dobler; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; T. A., En�lin; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; K., Ganga; R. T., G�nova Santos; T., Ghosh; M., Giard; G., Giardino; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; A., Gregorio; A., Gruppuso; F. K., Hansen; D., Harrison; C., Hern�ndez Monteagudo; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; T. R., Jaffe; A. H., Jaffe; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; J., Knoche; M., Kunz; H., Kurki Suonio; G., Lagache; A., L�hteenm�ki; J., Lamarre; A., Lasenby; C. R., Lawrence; S., Leach; R., Leonardi; P. B., Lilje; M., Linden V�rnle; P. M., Lubin; J. F., Mac�as P�rez; B., Maffei; D., Maino; N., Mandolesi; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; P., Mazzotta; A., Melchiorri; A., Mennella; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; D., Munshi; J. A., Murphy; P., Naselsky; F., Nati; P., Natoli; H. U., N�rgaard Nielsen; F., Noviello; D., Novikov; I., Novikov; S., Osborne; C. A., Oxborrow; F., Pajot; R., Paladini; D., Paoletti; M., Peel; L., Perotto; F., Perrotta; F., Piacentini; M., Piat; E., Pierpaoli; D., Pietrobon; S., Plaszczynski; E., Pointecouteau; G., Polenta; L., Popa; T., Poutanen; G. W., Pratt; S., Prunet; J., Puget; J. P., Rachen; W. T., Reach; R., Rebolo; M., Reinecke; C., Renault; S., Ricciardi; I., Ristorcelli; G., Rocha; C., Rosset; Mart�n, J. A. Rubi�o.; B., Rusholme; E., Salerno; M., Sandri; G., Savini; D., Scott; L., Spencer; V., Stolyarov; R., Sudiwala; A., Suur Uski; J., Sygnet; J. A., Tauber; Terenzi, Luca; C. T., Tibbs; L., Toffolatti; M., Tomasi; M., Tristram; L., Valenziano; B. V., Tent; J., Varis; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; N., Ysard; D., Yvon; A., Zacchei; A., Zonca
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