Planck intermediate results: IX. Detection of the galactic haze with planck

P. A.R. Ade; N. Aghanim; M. Arnaud; M. Ashdown; F. Atrio-Barandela; J. Aumont; C. Baccigalupi; A. Balbi; A. J. Banday; R. B. Barreiro; J. G. Bartlett; E. Battaner; K. Benabed; A. Benoît; J. P. Bernard; M. Bersanelli; A. Bonaldi; J. R. Bond; J. Borrill; F. R. Bouchet; C. Burigana; P. Cabella; J. F. Cardoso; A. Catalano; L. Cayón; R. R. Chary; L. Y. Chiang; P. R. Christensen; D. L. Clements; L. P.L. Colombo; A. Coulais; B. P. Crill; F. Cuttaia; L. Danese; O. D'Arcangelo; R. J. Davis; P. De Bernardis; G. De Gasperis; A. De Rosa; G. De Zotti; J. Delabrouille; C. Dickinson; J. M. Diego; G. Dobler; H. Dole; S. Donzelli; O. Doré; U. Dörl; M. Douspis; X. Dupac; G. Efstathiou; T. A. Enßlin; H. K. Eriksen; F. Finelli; O. Forni; M. Frailis; E. Franceschi; S. Galeotta; K. Ganga; M. Giard; G. Giardino; J. González-Nuevo; K. M. Górski; S. Gratton; A. Gregorio; A. Gruppuso; F. K. Hansen; D. Harrison; G. Helou; S. Henrot-Versillé; C. Hernández-Monteagudo; S. R. Hildebrandt; E. Hivon; M. Hobson; W. A. Holmes; A. Hornstrup; W. Hovest; K. M. Huffenberger; T. R. Jaffe; T. Jagemann; J. Jewell; W. C. Jones; M. Juvela; E. Keihänen; J. Knoche; L. Knox; M. Kunz; H. Kurki-Suonio; G. Lagache; A. Lähteenmäki; J. M. Lamarre; A. Lasenby; C. R. Lawrence; S. Leach; R. Leonardi; P. B. Lilje; M. Linden-Vørnle; M. López-Caniego; P. M. Lubin; J. F. MacÍas-Pérez; B. Maffei; D. Maino; N. Mandolesi; M. Maris; D. J. Marshall; P. G. Martin; E. Martínez-González; S. Masi; M. Massardi; S. Matarrese; F. Matthai; P. Mazzotta; P. R. Meinhold; A. Melchiorri; L. Mendes; A. Mennella; S. Mitra; A. Moneti; L. Montier; G. Morgante; D. Munshi; J. A. Murphy; P. Naselsky; P. Natoli; H. U. Nørgaard-Nielsen; F. Noviello; D. Novikov; I. Novikov; S. Osborne; F. Pajot; R. Paladini; D. Paoletti; B. Partridge; T. J. Pearson; O. Perdereau; 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; S. Prunet; J. L. Puget; J. P. Rachen; R. Rebolo; M. Reinecke; C. Renault; S. Ricciardi; T. Riller; I. Ristorcelli; G. Rocha; C. Rosset; J. A. Rubiño-Martín; B. Rusholme; M. Sandri; G. Savini; B. M. Schaefer; D. Scott; G. F. Smoot; L. Spencer; F. Stivoli; R. Sudiwala; A. S. Suur-Uski; J. F. Sygnet; J. A. Tauber; L. Terenzi; L. Toffolatti; M. Tomasi; M. Tristram; M. Türler; G. Umana; L. Valenziano; B. Van Tent; P. Vielva; F. Villa; N. Vittorio; L. A. Wade; B. D. Wandelt; M. White; D. Yvon; A. Zacchei; A. Zonca

doi:10.1051/0004-6361/201220271

Planck intermediate results: IX. Detection of the galactic haze with planck

P. A.R. Ade, N. Aghanim, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J. P. Bernard, M. Bersanelli, A. Bonaldi, J. R. Bond, J. Borrill, F. R. BouchetC. Burigana, P. Cabella, J. F. Cardoso, A. Catalano, L. Cayón, R. R. Chary, L. Y. Chiang, P. R. Christensen, D. L. Clements, L. P.L. Colombo, A. Coulais, B. P. Crill, F. Cuttaia, L. Danese, O. D'Arcangelo, R. J. Davis, P. De Bernardis, G. De Gasperis, A. De Rosa, G. De Zotti, J. Delabrouille, C. Dickinson, J. M. Diego, G. Dobler, H. Dole, S. Donzelli, O. Doré, U. Dörl, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, G. Giardino, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Harrison, G. Helou, S. Henrot-Versillé, C. Hernández-Monteagudo, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, W. Hovest, K. M. Huffenberger, T. R. Jaffe, T. Jagemann, J. Jewell, W. C. Jones, M. Juvela, E. Keihänen, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. M. Lamarre, A. Lasenby, C. R. Lawrence, S. Leach, R. Leonardi, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. MacÍas-Pérez, B. Maffei, D. Maino, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, F. Matthai, P. Mazzotta, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, S. Mitra, A. Moneti, L. Montier, G. Morgante, D. Munshi, J. A. Murphy, P. Naselsky, P. Natoli, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, F. Pajot, R. Paladini, D. Paoletti, B. Partridge, T. J. Pearson, O. Perdereau, 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, S. Prunet, J. L. Puget, J. P. Rachen, R. Rebolo, M. Reinecke, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, J. A. Rubiño-Martín, B. Rusholme, M. Sandri, G. Savini, B. M. Schaefer, D. Scott, G. F. Smoot, L. Spencer, F. Stivoli, R. Sudiwala, A. S. Suur-Uski, J. F. Sygnet, J. A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Türler, G. Umana, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, M. White, D. Yvon, A. Zacchei, A. Zonca

Physics

Research output: Contribution to journal › Article › peer-review

68 Scopus citations

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	https://doi.org/10.1051/0004-6361/201220271
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

Access to Document

10.1051/0004-6361/201220271

Cite this

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., ... Zonca, A. (2013). Planck intermediate results: IX. Detection of the galactic haze with planck. Astronomy and Astrophysics, 554, [A139]. https://doi.org/10.1051/0004-6361/201220271

@article{8f3e5b7b31fe452d82652bbac150a372,

title = "Planck intermediate results: IX. Detection of the galactic haze with planck",

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.",

keywords = "Galaxy: nucleus, ISM: bubbles, ISM: structure, Radio continuum: ISM",

author = "Ade, {P. A.R.} and N. Aghanim and M. Arnaud and M. Ashdown and F. Atrio-Barandela and J. Aumont and C. Baccigalupi and A. Balbi and Banday, {A. J.} and Barreiro, {R. B.} and Bartlett, {J. G.} and E. Battaner and K. Benabed and A. Beno{\^i}t and Bernard, {J. P.} and M. Bersanelli and A. Bonaldi and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and C. Burigana and P. Cabella and Cardoso, {J. F.} and A. Catalano and L. Cay{\'o}n and Chary, {R. R.} and Chiang, {L. Y.} and Christensen, {P. R.} and Clements, {D. L.} and Colombo, {L. P.L.} and A. Coulais and Crill, {B. P.} and F. Cuttaia and L. Danese and O. D'Arcangelo and Davis, {R. J.} and {De Bernardis}, P. and {De Gasperis}, G. and {De Rosa}, A. and {De Zotti}, G. and J. Delabrouille and C. Dickinson and Diego, {J. M.} and G. Dobler and H. Dole and S. Donzelli and O. Dor{\'e} and U. D{\"o}rl and M. Douspis and X. Dupac and G. Efstathiou and En{\ss}lin, {T. A.} and Eriksen, {H. K.} and F. Finelli and O. Forni and M. Frailis and E. Franceschi and S. Galeotta and K. Ganga and M. Giard and G. Giardino and J. Gonz{\'a}lez-Nuevo and G{\'o}rski, {K. M.} and S. Gratton and A. Gregorio and A. Gruppuso and Hansen, {F. K.} and D. Harrison and G. Helou and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and Hildebrandt, {S. R.} and E. Hivon and M. Hobson and Holmes, {W. A.} and A. Hornstrup and W. Hovest and Huffenberger, {K. M.} and Jaffe, {T. R.} and T. Jagemann and J. Jewell and Jones, {W. C.} and M. Juvela and E. Keih{\"a}nen and J. Knoche and L. Knox and M. Kunz and H. Kurki-Suonio and G. Lagache and A. L{\"a}hteenm{\"a}ki and Lamarre, {J. M.} and A. Lasenby and Lawrence, {C. R.} and S. Leach and R. Leonardi and Lilje, {P. B.} and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and Lubin, {P. M.} and Mac{\'I}as-P{\'e}rez, {J. F.} and B. Maffei and D. Maino and N. Mandolesi and M. Maris and Marshall, {D. J.} and Martin, {P. G.} and E. Mart{\'i}nez-Gonz{\'a}lez and S. Masi and M. Massardi and S. Matarrese and F. Matthai and P. Mazzotta and Meinhold, {P. R.} and A. Melchiorri and L. Mendes and A. Mennella and S. Mitra and A. Moneti and L. Montier and G. Morgante and D. Munshi and Murphy, {J. A.} and P. Naselsky and P. Natoli and N{\o}rgaard-Nielsen, {H. U.} and F. Noviello and D. Novikov and I. Novikov and S. Osborne and F. Pajot and R. Paladini and D. Paoletti and B. Partridge and Pearson, {T. J.} and O. Perdereau and F. Perrotta and F. Piacentini and M. Piat and E. Pierpaoli and D. Pietrobon and S. Plaszczynski and E. Pointecouteau and G. Polenta and N. Ponthieu and L. Popa and T. Poutanen and Pratt, {G. W.} and S. Prunet and Puget, {J. L.} and Rachen, {J. P.} and R. Rebolo and M. Reinecke and C. Renault and S. Ricciardi and T. Riller and I. Ristorcelli and G. Rocha and C. Rosset and Rubi{\~n}o-Mart{\'i}n, {J. A.} and B. Rusholme and M. Sandri and G. Savini and Schaefer, {B. M.} and D. Scott and Smoot, {G. F.} and L. Spencer and F. Stivoli and R. Sudiwala and Suur-Uski, {A. S.} and Sygnet, {J. F.} and Tauber, {J. A.} and L. Terenzi and L. Toffolatti and M. Tomasi and M. Tristram and M. T{\"u}rler and G. Umana and L. Valenziano and {Van Tent}, B. and P. Vielva and F. Villa and N. Vittorio and Wade, {L. A.} and Wandelt, {B. D.} and M. White and D. Yvon and A. Zacchei and A. Zonca",

note = "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 (G{\'o}rski et al. 2005) package.",

year = "2013",

doi = "10.1051/0004-6361/201220271",

language = "English (US)",

volume = "554",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Ade, PAR, Aghanim, N, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Balbi, A, Banday, AJ, Barreiro, RB, Bartlett, JG, Battaner, E, Benabed, K, Benoît, A, Bernard, JP, Bersanelli, M, Bonaldi, A, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Cabella, P, Cardoso, JF, Catalano, A, Cayón, L, Chary, RR, Chiang, LY, Christensen, PR, Clements, DL, Colombo, LPL, Coulais, A, Crill, BP, Cuttaia, F, Danese, L, D'Arcangelo, O, Davis, RJ, De Bernardis, P, De Gasperis, G, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Dobler, G, Dole, H, Donzelli, S, Doré, O, Dörl, U, Douspis, M, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Galeotta, S, Ganga, K, Giard, M, Giardino, G, González-Nuevo, J, Górski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Hansen, FK, Harrison, D, Helou, G, Henrot-Versillé, S, Hernández-Monteagudo, C, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Hovest, W, Huffenberger, KM, Jaffe, TR, Jagemann, T, Jewell, J, Jones, WC, Juvela, M, Keihänen, E, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, JM, Lasenby, A, Lawrence, CR, Leach, S, Leonardi, R, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, MacÍas-Pérez, JF, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marshall, DJ, Martin, PG, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Meinhold, PR, Melchiorri, A, Mendes, L, Mennella, A, Mitra, S, Moneti, A, Montier, L, Morgante, G, Munshi, D, Murphy, JA, Naselsky, P, Natoli, P, Nørgaard-Nielsen, HU, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pearson, TJ, 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, GW, Prunet, S, Puget, JL, Rachen, JP, Rebolo, R, Reinecke, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rubiño-Martín, JA, Rusholme, B, Sandri, M, Savini, G, Schaefer, BM, Scott, D, Smoot, GF, Spencer, L, Stivoli, F, Sudiwala, R, Suur-Uski, AS, Sygnet, JF, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Türler, M, Umana, G, Valenziano, L, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wade, LA, Wandelt, BD, White, M, Yvon, D, Zacchei, A & Zonca, A 2013, 'Planck intermediate results: IX. Detection of the galactic haze with planck', Astronomy and Astrophysics, vol. 554, A139. https://doi.org/10.1051/0004-6361/201220271

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 -

Planck intermediate results: IX. Detection of the galactic haze with planck

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