Abstract
Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterise the emission from the Galactic "haze" at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to | b | ∼ 35-50 in Galactic latitude and | l | ∼ 15-20 in longitude. By combining the Planck data with observations from the Wilkinson Microwave Anisotropy Probe, we were able to determine the spectrum of this emission to high accuracy, unhindered by the strong systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of-2.56 ± 0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE ∞ E-2.1. At Galactic latitudes | b | < 30, the microwave haze morphology is consistent with that of the Fermi gamma-ray "haze" or "bubbles", while at b ∼-50 we have identified an edge in the microwave haze that is spatially coincident with the edge in the gamma-ray bubbles. Taken together, this indicates that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new astrophysical mechanism for cosmic-ray acceleration in the inner Galaxy is implied.
| Original language | English (US) |
|---|---|
| Article number | A139 |
| Journal | Astronomy and Astrophysics |
| Volume | 554 |
| DOIs | |
| State | Published - 2013 |
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
Keywords
- Galaxy: nucleus
- ISM: bubbles
- ISM: structure
- Radio continuum: ISM
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Planck intermediate results : IX. Detection of the galactic haze with planck. / Ade, P. A.R.; Aghanim, N.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Bernard, J. P.; Bersanelli, M.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Burigana, C.; Cabella, P.; Cardoso, J. F.; Catalano, A.; Cayón, L.; Chary, R. R.; Chiang, L. Y.; Christensen, P. R.; Clements, D. L.; Colombo, L. P.L.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; D'Arcangelo, O.; Davis, R. J.; De Bernardis, P.; De Gasperis, G.; De Rosa, A.; De Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dobler, G.; Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, T. R.; Jagemann, T.; Jewell, J.; Jones, W. C.; Juvela, M.; Keihänen, E.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. M.; Lasenby, A.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; MacÍas-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Mitra, S.; Moneti, A.; Montier, L.; Morgante, G.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.; Pearson, T. J.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.; Puget, J. L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Schaefer, B. M.; Scott, D.; Smoot, G. F.; Spencer, L.; Stivoli, F.; Sudiwala, R.; Suur-Uski, A. S.; Sygnet, J. F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Türler, M.; Umana, G.; Valenziano, L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
In: Astronomy and Astrophysics, Vol. 554, A139, 2013.Research output: Contribution to journal › Article › peer-review
TY - JOUR
T1 - Planck intermediate results
T2 - IX. Detection of the galactic haze with planck
AU - Ade, P. A.R.
AU - Aghanim, N.
AU - Arnaud, M.
AU - Ashdown, M.
AU - Atrio-Barandela, F.
AU - Aumont, J.
AU - Baccigalupi, C.
AU - Balbi, A.
AU - Banday, A. J.
AU - Barreiro, R. B.
AU - Bartlett, J. G.
AU - Battaner, E.
AU - Benabed, K.
AU - Benoît, A.
AU - Bernard, J. P.
AU - Bersanelli, M.
AU - Bonaldi, A.
AU - Bond, J. R.
AU - Borrill, J.
AU - Bouchet, F. R.
AU - Burigana, C.
AU - Cabella, P.
AU - Cardoso, J. F.
AU - Catalano, A.
AU - Cayón, L.
AU - Chary, R. R.
AU - Chiang, L. Y.
AU - Christensen, P. R.
AU - Clements, D. L.
AU - Colombo, L. P.L.
AU - Coulais, A.
AU - Crill, B. P.
AU - Cuttaia, F.
AU - Danese, L.
AU - D'Arcangelo, O.
AU - Davis, R. J.
AU - De Bernardis, P.
AU - De Gasperis, G.
AU - De Rosa, A.
AU - De Zotti, G.
AU - Delabrouille, J.
AU - Dickinson, C.
AU - Diego, J. M.
AU - Dobler, G.
AU - Dole, H.
AU - Donzelli, S.
AU - Doré, O.
AU - Dörl, U.
AU - Douspis, M.
AU - Dupac, X.
AU - Efstathiou, G.
AU - Enßlin, T. A.
AU - Eriksen, H. K.
AU - Finelli, F.
AU - Forni, O.
AU - Frailis, M.
AU - Franceschi, E.
AU - Galeotta, S.
AU - Ganga, K.
AU - Giard, M.
AU - Giardino, G.
AU - González-Nuevo, J.
AU - Górski, K. M.
AU - Gratton, S.
AU - Gregorio, A.
AU - Gruppuso, A.
AU - Hansen, F. K.
AU - Harrison, D.
AU - Helou, G.
AU - Henrot-Versillé, S.
AU - Hernández-Monteagudo, C.
AU - Hildebrandt, S. R.
AU - Hivon, E.
AU - Hobson, M.
AU - Holmes, W. A.
AU - Hornstrup, A.
AU - Hovest, W.
AU - Huffenberger, K. M.
AU - Jaffe, T. R.
AU - Jagemann, T.
AU - Jewell, J.
AU - Jones, W. C.
AU - Juvela, M.
AU - Keihänen, E.
AU - Knoche, J.
AU - Knox, L.
AU - Kunz, M.
AU - Kurki-Suonio, H.
AU - Lagache, G.
AU - Lähteenmäki, A.
AU - Lamarre, J. M.
AU - Lasenby, A.
AU - Lawrence, C. R.
AU - Leach, S.
AU - Leonardi, R.
AU - Lilje, P. B.
AU - Linden-Vørnle, M.
AU - López-Caniego, M.
AU - Lubin, P. M.
AU - MacÍas-Pérez, J. F.
AU - Maffei, B.
AU - Maino, D.
AU - Mandolesi, N.
AU - Maris, M.
AU - Marshall, D. J.
AU - Martin, P. G.
AU - Martínez-González, E.
AU - Masi, S.
AU - Massardi, M.
AU - Matarrese, S.
AU - Matthai, F.
AU - Mazzotta, P.
AU - Meinhold, P. R.
AU - Melchiorri, A.
AU - Mendes, L.
AU - Mennella, A.
AU - Mitra, S.
AU - Moneti, A.
AU - Montier, L.
AU - Morgante, G.
AU - Munshi, D.
AU - Murphy, J. A.
AU - Naselsky, P.
AU - Natoli, P.
AU - Nørgaard-Nielsen, H. U.
AU - Noviello, F.
AU - Novikov, D.
AU - Novikov, I.
AU - Osborne, S.
AU - Pajot, F.
AU - Paladini, R.
AU - Paoletti, D.
AU - Partridge, B.
AU - Pearson, T. J.
AU - Perdereau, O.
AU - Perrotta, F.
AU - Piacentini, F.
AU - Piat, M.
AU - Pierpaoli, E.
AU - Pietrobon, D.
AU - Plaszczynski, S.
AU - Pointecouteau, E.
AU - Polenta, G.
AU - Ponthieu, N.
AU - Popa, L.
AU - Poutanen, T.
AU - Pratt, G. W.
AU - Prunet, S.
AU - Puget, J. L.
AU - Rachen, J. P.
AU - Rebolo, R.
AU - Reinecke, M.
AU - Renault, C.
AU - Ricciardi, S.
AU - Riller, T.
AU - Ristorcelli, I.
AU - Rocha, G.
AU - Rosset, C.
AU - Rubiño-Martín, J. A.
AU - Rusholme, B.
AU - Sandri, M.
AU - Savini, G.
AU - Schaefer, B. M.
AU - Scott, D.
AU - Smoot, G. F.
AU - Spencer, L.
AU - Stivoli, F.
AU - Sudiwala, R.
AU - Suur-Uski, A. S.
AU - Sygnet, J. F.
AU - Tauber, J. A.
AU - Terenzi, L.
AU - Toffolatti, L.
AU - Tomasi, M.
AU - Tristram, M.
AU - Türler, M.
AU - Umana, G.
AU - Valenziano, L.
AU - Van Tent, B.
AU - Vielva, P.
AU - Villa, F.
AU - Vittorio, N.
AU - Wade, L. A.
AU - Wandelt, B. D.
AU - White, M.
AU - Yvon, D.
AU - Zacchei, A.
AU - Zonca, A.
N1 - Funding Information: The development of Planck has been supported by ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.rssd.esa.int/Planck . Part of the research described in this publication was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. G. Dobler has been supported by the Harvey L. Karp Discovery Award. Some of the results in this paper have been derived using the HEALPix (Górski et al. 2005) package.
PY - 2013
Y1 - 2013
N2 - Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterise the emission from the Galactic "haze" at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to | b | ∼ 35-50 in Galactic latitude and | l | ∼ 15-20 in longitude. By combining the Planck data with observations from the Wilkinson Microwave Anisotropy Probe, we were able to determine the spectrum of this emission to high accuracy, unhindered by the strong systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of-2.56 ± 0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE ∞ E-2.1. At Galactic latitudes | b | < 30, the microwave haze morphology is consistent with that of the Fermi gamma-ray "haze" or "bubbles", while at b ∼-50 we have identified an edge in the microwave haze that is spatially coincident with the edge in the gamma-ray bubbles. Taken together, this indicates that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new astrophysical mechanism for cosmic-ray acceleration in the inner Galaxy is implied.
AB - Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterise the emission from the Galactic "haze" at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to | b | ∼ 35-50 in Galactic latitude and | l | ∼ 15-20 in longitude. By combining the Planck data with observations from the Wilkinson Microwave Anisotropy Probe, we were able to determine the spectrum of this emission to high accuracy, unhindered by the strong systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of-2.56 ± 0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE ∞ E-2.1. At Galactic latitudes | b | < 30, the microwave haze morphology is consistent with that of the Fermi gamma-ray "haze" or "bubbles", while at b ∼-50 we have identified an edge in the microwave haze that is spatially coincident with the edge in the gamma-ray bubbles. Taken together, this indicates that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new astrophysical mechanism for cosmic-ray acceleration in the inner Galaxy is implied.
KW - Galaxy: nucleus
KW - ISM: bubbles
KW - ISM: structure
KW - Radio continuum: ISM
UR - http://www.scopus.com/inward/record.url?scp=84879244760&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84879244760&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201220271
DO - 10.1051/0004-6361/201220271
M3 - Article
AN - SCOPUS:84879244760
VL - 554
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
SN - 0004-6361
M1 - A139
ER -