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22 results on '"Procopio, P."'

1. Galactic synchrotron emissivity measurements between 250° < l < 355° from the GLEAM survey with the MWA

Author

Su, H., Hurley-Walker, N., Jackson, C. A., McClure-Griffiths, N. M., Tingay, S. J., Hindson, L., Hancock, P., Wayth, R. B., Gaensler, B. M., Staveley-Smith, L., Morgan, J., Johnston-Hollitt, M., Lenc, E., Bell, M. E., Callingham, J. R., Dwarkanath, K. S., For, B. Q., Kapi��ska, A. D., McKinley, B., Offringa, A. R., Procopio, P., Wu, C., and Zheng, Q.

Subjects
Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Synchrotron emission pervades the Galactic plane at low radio frequencies, originating from cosmic ray electrons interacting with the Galactic magnetic field. Using a low-frequency radio telescope, the Murchison Widefield Array (MWA), we measure the free-free absorption of this Galactic synchrotron emission by intervening HII regions along the line of sight. These absorption measurements allow us to calculate the Galactic cosmic-ray electron emissivity behind and in front of 47 detected HII regions in the region $250^\circ < l < 355^\circ$, $|b| < 2^\circ$. We find that all average emissivities between the HII regions and the Galactic edge along the line of sight ($��_b$) are in the range of 0.24$\,\,\sim\,\,$0.70$\,\,$K$\,\,$pc$^{-1}$ with a mean of 0.40$\,\,$K$\,\,$pc$^{-1}$ and a variance of 0.10$\,\,$K$\,\,$pc$^{-1}$ at 88$\,\,$MHz. Our best model, the Two-circle model, divides the Galactic disk into three regions using two circles centring on the Galactic centre. It shows a high emissivity region near the Galactic centre, a low emissivity region near the Galactic edge, and a medium emissivity region between these two regions, contrary to the trend found by previous studies., 12 pages, 8 figures. Published on MNRAS. A conversion factor is corrected in this version. For the original published version, see https://academic.oup.com/mnras/article-abstract/465/3/3163/2544366/Galactic-synchrotron-emissivity-measurements?redirectedFrom=fulltext For its erratum, see https://academic.oup.com/mnras/article-abstract/472/1/828/4083643/Erratum-Galactic-synchrotron-emissivity

Published
2017

2. Erratum: Galactic synchrotron emissivity measurements between 250° < l < 355° from the GLEAM survey with the MWA [MNRAS, 472, (2017), (828-834)] doi:10.1093/mnras/stx2129

Author

Su, H, Hurley-Walker, N, Jackson, CA, McClure-Griffiths, NM, Tingay, SJ, Hindson, L, Hancock, P, Wayth, RB, Gaensler, BM, Staveley-Smith, L, Morgan, J, Johnston-Hollitt, M, Lenc, E, Bell, ME, Callingham, JR, Dwarkanath, KS, For, BQ, Kapińska, AD, McKinley, B, Offringa, AR, Procopio, P, Wu, C, and Zheng, Q

Subjects
Astronomy & Astrophysics
Abstract

© 2017 The Authors. This is an erratum to the paper 'Galactic synchrotron emissivity measurements between 250° < l < 355° from the GLEAM survey with the MWA', published in MNRAS, 465, 3163 (2017).

Published
2017

3. A large-scale, low-frequency murchison widefield array survey of galactic H II regions between 260 < l < 340

Author

Hindson, L, Johnston-Hollitt, M, Hurley-Walker, N, Callingham, JR, Su, H, Morgan, J, Bell, M, Bernardi, G, Bowman, JD, Briggs, F, Cappallo, RJ, Deshpande, AA, Dwarakanath, KS, For, BQ, Gaensler, BM, Greenhill, LJ, Hancock, P, Hazelton, BJ, Kapinska, AD, Kaplan, DL, Lenc, E, Lonsdale, CJ, Mckinley, B, McWhirter, SR, Mitchell, DA, Morales, MF, Morgan, E, Oberoi, D, Offringa, A, Ord, SM, Procopio, P, Prabu, T, Udaya Shankar, N, Srivani, KS, Staveley-Smith, L, Subrahmanyan, R, Tingay, SJ, Wayth, RB, Webster, RL, Williams, A, Williams, CL, Wu, C, and Zheng, Q

Subjects
Astronomy & Astrophysics
Abstract

© Astronomical Society of Australia 2016. We have compiled a catalogue of H ii regions detected with the Murchison Widefield Array between 72 and 231 MHz. The multiple frequency bands provided by the Murchison Widefield Array allow us identify the characteristic spectrum generated by the thermal Bremsstrahlung process in H ii regions. We detect 306 H ii regions between 260◦ < l < 340◦ and report on the positions, sizes, peak, integrated flux density, and spectral indices of these H ii regions. By identifying the point at which H ii regions transition from the optically thin to thick regime, we derive the physical properties including the electron density, ionised gas mass, and ionising photon flux, towards 61 H ii regions. This catalogue of H ii regions represents the most extensive and uniform low frequency survey of H ii regions in the Galaxy to date.

Published
2016

4. The MWA GLEAM 4Jy Sample; a new large, bright radio source sample at 151 MHz

Author

Jackson, C. A., Franzen, T. M. O., Seymour, N., White, S. V., Murphy, Tara, Sadler, E. M., Joseph Callingham, Hunstead, R. W., Hughes, J., Wall, J. V., Bell, M. E., Dwarakanath, K. S., For, B-Q, Gaensler, B. M., Hancock, P. J., Hindson, L., Hurley-Walker, N., Johnston-Hollitt, M., Kapinska, A. D., Lenc, E., Mckinley, B., Morgan, J., Offringa, A. R., Procopio, P., Staveley-Smith, L., Wayth, R. B., Wu, C., and Zheng, Q.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This paper outlines how the new GaLactic and Extragalactic All-sky MWA Survey (GLEAM, Wayth et al. 2015), observed by the Murchison Widefield Array covering the frequency range 72 - 231 MHz, allows identification of a new large, complete, sample of more than 2000 bright extragalactic radio sources selected at 151 MHz. With a flux density limit of 4 Jy this sample is significantly larger than the canonical fully-complete sample, 3CRR (Laing, Riley & Longair 1983). In analysing this small bright subset of the GLEAM survey we are also providing a first user check of the GLEAM catalogue ahead of its public release (Hurley-Walker et al. in prep). Whilst significant work remains to fully characterise our new bright source sample, in time it will provide important constraints to evolutionary behaviour, across a wide redshift and intrinsic radio power range, as well as being highly complementary to results from targeted, small area surveys., Conference Proceedings: The many facets of radio galaxies, Bologna, October 2015

Published
2016
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5. A Large Scale, Low Frequency Murchison Widefield Array Survey of Galactic HII regions between 260< l

Author

Hindson, L., Johnston-Hollitt, M., Hurley-Walker, N., Callingham, J. R., Su, H., Morgan, J., Bell, M., Bernardi, G., Bowman, J. D., Briggs, F., Cappallo, R. J., Deshpande, A. A., Dwarakanath, K. S., For, B. -Q, Gaensler, B. M., Greenhill, L. J., Hancock, P., Hazelton, B. J., Kapinska, A. D., Kaplan, D. L., Lenc, E., Lonsdale, C. J., Mckinley, B., McWhirter, S. R., Mitchell, D. A., Morales, M. F., Morgan, E., Oberoi, D., Offringa, A., Ord, S. M., Procopio, P., Prabu, T., UdayaShankar, N., Srivani, K. S., Staveley-Smith, L., Subrahmanyan, R., Tingay, S. J., Wayth, R. B., Webster, R. L., Williams, A., Williams, C. L., Wu, C., and Zheng, Q.

Subjects
Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract

We have compiled a catalogue of HII regions detected with the Murchison Widefield Array (MWA) between 72 and 231MHz. The multiple frequency bands provided by the MWA allow us identify the characteristic spectrum generated by the thermal Bremsstrahlung process in HII regions. We detect 302 HII regions between 260 < l < 340 and report on the positions, sizes, peak, integrated flux density, and spectral indices of these HII regions. By identifying the point at which HII regions transition from the optically thin to thick regime we derive the physical properties including the electron density, ionised gas mass and ionising photon flux, towards 61 HII regions. This catalogue of HII regions represents the most extensive and uniform low frequency survey of HII regions in the Galaxy to date., 20 pages, 9 figures, 3 tables

Published
2016
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6. An analysis of the halo and relic radio emission from Abell 3376 from Murchison Widefield Array observations

Author

George, Lijo T., Dwarakanath, K. S., Johnston-Hollitt, M., Hurley-Walker, N., Hindson, L., Kapińska, A. D., Tingay, S. J., Bell, M., Callingham, J. R., For, Bi-Qing, Hancock, P. J., Lenc, E., McKinley, B., Morgan, J., Offringa, A., Procopio, P., Staveley-Smith, L., Wayth, R. B., Wu, Chen, Zheng, Q., Bernardi, G., Bowman, J. D., Briggs, F., Cappallo, R. J., Corey, B. E., Deshpande, A. A., Emrich, D., Goeke, R., Greenhill, L. J., Hazelton, B. J., Kaplan, D. L., Kasper, J. C., Kratzenberg, E., Lonsdale, C. J., Lynch, M. J., McWhirter, S. R., Mitchell, D. A., Morales, M. F., Morgan, E., Oberoi, D., Ord, S. M., Prabu, T., Rogers, A. E. E., Roshi, A., Shankar, N. Udaya, Srivani, K. S., Subrahmanyan, R., Waterson, M., Whitney, R. L. Webster A. R., Williams, A., and Williams, C. L.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract

We have carried out multiwavelength observations of the near-by ($z=0.046$) rich, merging galaxy cluster Abell 3376 with the Murchison Widefield Array (MWA). As a part of the GaLactic and Extragalactic All-sky MWA survey (GLEAM), this cluster was observed at 88, 118, 154, 188 and 215 MHz. The known radio relics, towards the eastern and western peripheries of the cluster, were detected at all the frequencies. The relics, with a linear extent of $\sim$ 1 Mpc each, are separated by $\sim$ 2 Mpc. Combining the current observations with those in the literature, we have obtained the spectra of these relics over the frequency range 80 -- 1400 MHz. The spectra follow power laws, with $\alpha$ = $-1.17\pm0.06$ and $-1.37\pm0.08$ for the west and east relics, respectively ($S \propto \nu^{\alpha}$). Assuming the break frequency to be near the lower end of the spectrum we estimate the age of the relics to be $\sim$ 0.4 Gyr. No diffuse radio emission from the central regions of the cluster (halo) was detected. The upper limit on the radio power of any possible halo that might be present in the cluster is a factor of 35 lower than that expected from the radio power and X-ray luminosity correlation for cluster halos. From this we conclude that the cluster halo is very extended ($>$ 500 kpc) and/or most of the radio emission from the halo has decayed. The current limit on the halo radio power is a factor of ten lower than the existing upper limits with possible implications for models of halo formation., Comment: 10 pages, 6 figures

Published
2015
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7. Planck early results. XX. New light on anomalous microwave emission from spinning dust grains

Author

Lähteenmäki, A., Poutanen, T., Natoli, P., Polenta, G., Bartlett, J.G., Bucher, M., Cardoso, J.-F., Catalano, A., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Patanchon, G., Piat, M., Rosset, C., Smoot, G.F., Stompor, R., Ashdown, M., Hobson, M., Lasenby, A., Stolyarov, V., Bhatia, R., Kneissl, R., Bond, J.R., Miville-Deschênes, M.-A., Banday, A.J., Bernard, J.-P., Forni, O., Giard, M., Jaffe, T.R., Marshall, D.J., Montier, L., Pointecouteau, E., Ristorcelli, I., Bock, J.J., Doré, O., Helou, G., Hildebrandt, S.R., Paladini, R., Pearson, T.J., Prézeau, G., Rocha, G., Seiffert, M.D., Lilje, P.B., Challinor, A., Shellard, P., Starck, J.-L., Yvon, D., Linden-Vørnle, Michael, Nørgaard-Nielsen, Hans Ulrik, Toffolatti, L., Netterfield, C.B., Scott, D., Juvela, M., Keihänen, E., Keskitalo, R., Kurki-Suonio, H., Ysard, N., Chiang, C., Jones, W.C., Cayón, L., Knox, L., Leonardi, R., Lubin, P.M., Meinhold, P.R., Zonca, A., Wandelt, B.D., Matarrese, S., De Bernardis, P., Masi, S., Melchiorri, A., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Balbi, A., Cabella, P., De Gasperis, G., Mazzotta, P., Vittorio, N., Christensen, P.R., Naselsky, P., Génova-Santos, R.T., Rebolo, R., Rubiño-Martín, J.A., Dupac, X., Mendes, L., Giardino, G., Laureijs, R.J., Tauber, J.A., Partridge, B., Umana, G., Bonaldi, A., De Zotti, G., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Zacchei, A., Burigana, C., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Mandolesi, N., Morgante, G., Procopio, P., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Cappellini, B., Donzelli, S., Stivoli, F., Chamballu, A., Clements, D.L., Jaffe, A.H., Mortlock, D., Novikov, D., Rowan-Robinson, M., Chary, R.-R., Chen, X., McGehee, P., Rusholme, B., Benoît, A., Aghanim, N., Aumont, J., Boulanger, F., Douspis, M., Lagache, G., Noviello, F., Pajot, F., Ponthieu, N., Puget, J.-L., Torre, J.-P., Verstraete, L., Benabed, K., Bouchet, F.R., Colombi, S., Delouis, J.-M., Hivon, E., Moneti, A., Prunet, S., Sygnet, J.-F., Chiang, L.-Y., Efstathiou, G., Gratton, S., Harrison, D., Munshi, D., Eriksen, H.K., Hansen, F.K., Hoyland, R.J., Barreiro, R.B., Herranz, D., López-Caniego, M., Martínez-González, E., Vielva, P., Platania, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Mitra, S., O'Dwyer, I.J., Wade, L.A., Davies, R.D., Davis, R.J., Dickinson, C., Maffei, B., Peel, M., Watson, R., Wilkinson, A., MacTavish, C.J., Coulais, A., Lamarre, J.-M., Arnaud, M., MacÍas-Pérez, J.F., Perotto, L., Renault, C., Santos, D., Couchot, F., Henrot-Versillé, S., Perdereau, O., Plaszczynski, S., Tristram, M., Borrill, J., Kisner, T.S., Dörl, U., Enßlin, T.A., Hovest, W., Matthai, F., Reinecke, M., Riller, T., Reich, W., Tuovinen, J., Varis, J., Murphy, A., Novikov, I., Savini, G., Baccigalupi, C., Danese, L., González-Nuevo, J., Leach, S., Perrotta, F., Mann, R., Ade, P.A.R., Sudiwala, R., Osborne, S., Casassus, S., Reach, W.T., Battaner, E., Huffenberger, K.M., Department of Physics, Helsinki Institute of Physics, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., 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., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Cabella, P., Cappellini, B., Cardoso, J. F., Casassus, S., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. R., Chen, X., Chiang, L. Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Dickinson, C., 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., Génova Santos, R. T., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Hansen, F. K., Harrison, D., Helou, G., Henrot Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, T. R., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Lilje, P. B., Linden Vornle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Mactavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marshall, D. J., Martínez González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Mcgehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Norgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Procopio, P., Prunet, S., Puget, J. L., Reach, W. T., Rebolo, R., Reich, W., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan Robinson, M., Rubino Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Varis, J., Verstraete, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, R., Wilkinson, A., Ysard, N., Yvon, D., Zacchei, A., Zonca, A., APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Universidad de Cantabria, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)

Subjects
Experimental Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cosmic microwave background, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, CMB physic, ISM: general – Galaxy: general – radiation mechanisms: general – radio continuum: ISM – submillimeter: ISM, CMB physics, Astrophysics::Solar and Stellar Astrophysics, submillimeter, radio continuum: ism, ism: general, radiation mechanisms: general, submillimeter: ism, galaxy: general, 010303 astronomy & astrophysics, QB, general [Radiation mechanisms], Physics, general [ISM], Spinning dust, Planck ESA mission, ISM: general, Galaxy: general, radio continuum: ISM, submillimeter: ISM, ISM [Submillimeter], symbols, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Cosmology and Nongalactic Astrophysics, general – Galaxy: general – radiation mechanisms: general – radio continuum: ISM – submillimeter: ISM [ISM], Cosmology and Nongalactic Astrophysics (astro-ph.CO), education, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, radio continuum, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Thermal, Radio continuum: ISM, Planck, Submillimeter: ISM, ISM, Astrophysics::Galaxy Astrophysics, general [Galaxy], 010308 nuclear & particles physics, Molecular cloud, Astronomy and Astrophysics, Radiation mechanisms: general, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, ISM [Radio continuum], Dipole, Galaxy, radiation mechanisms, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], 13. Climate action, Space and Planetary Science, general, Astrophysics of Galaxies (astro-ph.GA)
Abstract

17 páginas, 14 figuras, 4 tablas.-- Planck Collaboration: et al., Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range ~10–60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and ρ Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20–40 GHz and are detected at high significances of 17.1σ for Perseus and 8.4σ for ρ Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In ρ Ophiuchi, the ~30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50–100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. We present spectra for two of the candidates; S140 and S235 are bright Hii regions that show evidence for AME, and are well fitted by spinning dust models., The Planck Collaboration acknowledges the support of: 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).

Published
2011

8. Planck intermediate results. XVIII The millimetre and sub-millimetre emission from planetary nebulae

Author

Planck Collaboration, Arnaud, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit-L��vy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Buemi, C. S., Burigana, C., Cardoso, J. -F., Casassus, S., Catalano, A., Cerrigone, L., Chamballu, A., Chiang, H. C., Colombi, S., Colombo, L. P. L., Couchot, F., Crill, B. P., Curto, A., Cuttaia, F., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Donzelli, S., Dor��, O., Dupac, X., En��lin, T. A., Eriksen, H. K., Finelli, F., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Gonz��lez-Nuevo, J., G��rski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D. L., Hildebrandt, S. R., Hivon, E., Holmes, W. A., Hora, J. L., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, T. R., Jones, W. C., Juvela, M., Keih��nen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Kunz, M., Kurki-Suonio, H., L��hteenm��ki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Leto, P., Lilje, P. B., Linden-V��rnle, M., L��pez-Caniego, M., Mac��as-P��rez, J. F., Maffei, B., Maino, D., Mandolesi, N., Martin, P. G., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., Mendes, L., Mennella, A., Migliaccio, M., Miville-Desch��nes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Noviello, F., Novikov, D., Novikov, I., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Peel, M., Perdereau, O., Perrotta, F., Piacentini, F., Piat, M., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Popa, L., Pratt, G. W., Procopio, P., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rubi��o-Mart��n, J. A., Rusholme, B., Sandri, M., Savini, G., Scott, D., Spencer, L. D., Stolyarov, V., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Trigilio, C., Tristram, M., Trombetti, T., Tucci, M., Umana, G., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Zacchei, A., Zijlstra, A., and Zonca, A.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Late stages of stellar evolution are characterized by copious mass-loss events whose signature is the formation of circumstellar envelopes (CSE). Planck multi-frequency measurements have provided relevant information on a sample of Galactic planetary nebulae (PNe) in the important and relatively unexplored observational band between 30 and 857GHz. Planck enables the assembly of comprehensive PNe spectral energy distributions (SEDs) from radio {\bf to} far-infrared frequencies. Modelling of the derived SEDs provides us with information on physical properties of CSEs and the mass content of both main components: ionised gas, traced by the free-free emission at cm--mm waves; and thermal dust, traced by the millimetre and far-IR emission. In particular, the amount of ionised gas and dust has been derived here. Such quantities have also been estimated for the very young PN CRL618, where the strong variability observed in its radio and millimetre emission has previously prevented the construction of its SED. A morphological study of the Helix Nebula has also been performed. Planck maps reveal, for the first time, the spatial distribution of the dust inside the envelope, allowing us to identify different components, the most interesting of which is a very extended component (up to 1pc) that may be related to a region where the slow expanding envelope is interacting with the surrounding interstellar medium., 18 pages, 14 figures; accepted for publication in A&A

Published
2014
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9. A 20 GHz Bright Sample for Delta > 72 deg - II. Multi-frequency Follow-up

Author

Ricci, R., Righini, S., Verma, R., Prandoni, I., Carretti, E., Mack, K. -H., Massardi, M., Procopio, P., Zanichelli, A., Gregorini, L., Mantovani, F., Gawronski, M. P., and Peel, M. W.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present follow-up observations at 5, 8 and 30 GHz of the K-band Northern Wide Survey (KNoWS) 20 GHz Bright Sample, performed with the 32-m Medicina Radio Telescope and the 32-m Torun Radio Telescope. The KNoWS sources were selected in the Northern Polar Cap (Delta > 72 deg) and have a flux density limit S(20GHz) = 115 mJy. We include NVSS 1.4 GHz measurements to derive the source radio spectra between 1.4 and 30 GHz. Based on optical identifications, 68 per cent of the sources are QSOs, and 27 per cent are radio galaxies. A redshift measurement is available for 58 per cent of the sources. The radio spectral properties of the different source populations are found to be in agreement with those of other high-frequency selected samples., 14 pages, 6 figures, 7 tables. Accepted for publication on MNRAS

Published
2013
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10. A 20 GHz bright sample for �� > +72��: I. Catalogue

Author

Righini, S., Carretti, E., Ricci, R., Zanichelli, A., Mack, K. -H., Massardi, M., Prandoni, I., Procopio, P., Verma, R., L��pez-Caniego, M., Gregorini, L., and Mantovani, F.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

During 2010-2011, the Medicina 32-m dish hosted the 7-feed 18-26.5 GHz receiver built for the Sardinia Radio Telescope, with the goal to perform its commissioning. This opportunity was exploited to carry out a pilot survey at 20 GHz over the area for �� > + 72.3��. This paper describes all the phases of the observations, as they were performed using new hardware and software facilities. The map-making and source extraction procedures are illustrated. A customised data reduction tool was used during the follow-up phase, which produced a list of 73 confirmed sources down to a flux density of 115 mJy. The resulting catalogue, here presented, is complete above 200 mJy. Source counts are in agreement with those provided by the AT20G survey. This pilot activity paves the way to a larger project, the K-band Northern Wide Survey (KNoWS), whose final aim is to survey the whole Northern Hemisphere down to a flux limit of 50 mJy (5��)., 10 pages, 10 figures. Accepted by MNRAS

Published
2012
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11. Mining the Herschel-ATLAS: submillimeter-selected blazars in equatorial fields

Author

López-Caniego, M., González-Nuevo, J., Massardi, M., Bonavera, L., Herranz, D., Negrello, M., De Zotti, G., Carrera, F. J., Danese, L., Fleuren, S., Hardcastle, M., Jarvis, M. J., Klöckner, H. -R., Mauch, T., Procopio, P., Righini, S., Sutherland, W., Auld, R., Baes, M., Buttiglione, S., Clark, C. J. R., Cooray, A., Dariush, A., Dunne, L., Dye, S., Eales, S., Hopwood, R., Hoyos, C., Ibar, E., Ivison, R. J., Maddox, S., and Valiante, E.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Herschel Astrophysical Terahertz Large Area Survey (H-ATLAS) provides an unprecedented opportunity to search for blazars at sub-mm wavelengths. We cross-matched the FIRST radio source catalogue with the 11655 sources brighter than 35 mJy at 500{\mu}m in the \sim 135 square degrees of the sky covered by the H-ATLAS equatorial fields at 9 h and 15 h, plus half of the field at 12 h. We found that 379 of the H-ATLAS sources have a FIRST counterpart within 10 arcsec, including 8 catalogued blazars (plus one known blazar that was found at the edge of one the H-ATLAS maps). To search for additional blazar candidates we have devised new diagnostic diagrams and found that known blazars occupy a region of the log(S500{\mu}m/S350{\mu}m) vs. log(S500{\mu}m/S1.4GHz) plane separated from that of the other sub-mm sources with radio counterparts. Using this diagnostic we have selected 12 further candidates that turn out to be scattered in the (r-z) vs. (u-r) plane or in the WISE colour-colour diagram proposed by Massaro et al. (2012), where known blazars are concentrated in well defined strips. This suggests that the majority of them either are not blazars or have spectral energy distributions contaminated by their host galaxies. A significant fraction of true blazars are found to be hosted by star-forming galaxies. This finding, supported by an analysis of blazars detected in Planck 545 and 857 GHz bands, is at odds with the notion that blazar hosts are passive ellipticals and indicates that the sub-mm selection is providing a novel prospect on blazar properties. Based on an inspection of the available photometric data, including the WISE all-sky survey, the unpublished VIKING survey and new radio observations, we tentatively estimate that there are 11 blazars with synchrotron flux density S500{\mu}m > 35mJy over the considered area. This result already allows us to constrain blazar evolution models., Comment: 13 pages, 5 figures, 5 tables. Submitted to MNRAS

Published
2012
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13. The Simultaneous Medicina-Planck Experiment (SiMPlE): data acquisition, reduction and first results

Author

Procopio, P., Massardi, M., Righini, S., Zanichelli, A., Ricciardi, S., Libardi, P., Burigana, C., Cuttaia, F., Mack, K. -H., Terenzi, L., Villa, F., Bonavera, L., Morgante, G., Trigilio, C., Trombetti, T., and Umana, G.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Simultaneous Medicina-{\it Planck} Experiment (SiMPlE) is aimed at observing a selected sample of 263 extragalactic and Galactic sources with the Medicina 32-m single dish radio telescope in the same epoch as the Planck satellite observations. The data acquired with a frequency coverage down to 5 GHz, also combined with Planck at frequencies above 30 GHz, will constitute a useful reference catalogue of bright sources over the whole Northern hemisphere. Furthermore, source observations performed in different epochs and comparison with other catalogues allow the investigation of source variabilities on different timescales. In this work, we describe the sample selection, the on-going data acquisition campaign, the data reduction procedures, the developed tools, and the comparison with other data-sets. We present the data at 5 and 8.3 GHz for the SiMPlE Northern Sample consisting of 79 sources with $\delta \geq 45^\circ$ selected in our catalogue and observed during the first 6 months of the project. A first analysis of their spectral behaviour and long-term variability is also presented., Comment: 16 pages, 14 figures, submitted to MNRAS

Published
2011
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14. VizieR Online Data Catalog: GaLactic and Extragalactic All-sky MWA survey (Hurley-Walker+, 2016)

Author

Hurley-Walker, N., Joseph Callingham, Hancock, P. J., Franzen, T. M. O., Hindson, L., Kapinska, A. D., Morgan, J., Offringa, A. R., Wayth, R. B., Wu, C., Zheng, Q., Murphy, T., Bell, M. E., Dwarakanath, K. S., For, B., Gaensler, B. M., Johnston-Hollitt, M., Lenc, E., Procopio, P., Staveley-Smith, L., Ekers, R., Bowman, J. D., Briggs, F., Cappallo, R. J., Deshpande, A. A., Greenhill, L., Hazelton, B. J., Kaplan, D. L., Lonsdale, C. J., Mcwhirter, S. R., Mitchell, D. A., Morales, M. F., Morgan, E., Oberoi, D., Ord, S. M., Prabu, T., Udaya Shankar, N., Srivani, K. S., Subrahmanyan, R., Tingay, S. J., Webster, R. L., Williams, A., and Williams, C. L.

15. VizieR Online Data Catalog: 180MHz Murchison Commissioning Survey (MWACS) (Hurley-Walker+, 2014)

Author

Hurley-Walker, N., Morgan, J., Wayth, R. B., Hancock, P. J., Bell, M. E., Bernardi, G., Bhat, N. D. R., Briggs, F., Deshpande, A. A., Ewall-Wice, A., Feng, L., Hazelton, B. J., Hindson, L., Jacobs, D. C., Kaplan, D. L., Kudryavtseva, N., Lenc, E., Mckinley, B., Mitchell, D., Pindor, B., Procopio, P., Oberoi, D., Offringa, A., Ord, S., Riding, J., Bowman, J. D., Cappallo, R., Corey, B., Emrich, D., Gaensler, B. M., Goeke, R., Greenhill, L., Hewitt, J., Johnston-Hollitt, M., Justin Kasper, Kratzenberg, E., Lonsdale, C., Lynch, M., Mcwhirter, R., Morales, M. F., Morgan, E., Prabu, T., Rogers, A., Roshi, A., Shankar, U., Srivani, K., Subrahmanyan, R., Tingay, S., Waterson, M., Webster, R., Whitney, A., Williams, A., and Williams, C.

16. WSClean: Widefield interferometric imager

Author

Offringa, A. R., Mckinley, B., Hurley-Walker, N., Briggs, F. H., Wayth, R. B., Kaplan, D. L., Bell, M. E., Feng, L., Neben, A. R., Hughes, J. D., Rhee, J., Murphy, T., Bhat, N. D. R., Bernardi, G., Bowman, J. D., Cappallo, R. J., Corey, B. E., Deshpande, A. A., Emrich, D., Ewall-Wice, A., Gaensler, B. M., Goeke, R., Greenhill, L. J., Hazelton, B. J., Hindson, L., Johnston-Hollitt, M., Jacobs, D. C., Justin Kasper, Kratzenberg, E., Lenc, E., Lonsdale, C. J., Lynch, M. J., Mcwhirter, S. R., Mitchell, D. A., Morales, M. F., Morgan, E., Kudryavtseva, N., Oberoi, D., Ord, S. M., Pindor, B., Procopio, P., Prabu, T., Riding, J., Roshi, D. A., Shankar, N. Udaya, Srivani, K. S., Subrahmanyan, R., Tingay, S. J., Waterson, M., Webster, R. L., Whitney, A. R., Williams, A., and Williams, C. L.

17. The Planck mission

Author

Mandolesi, N., Burigana, C., Alessandro Gruppuso, Procopio, P., Ricciardi, S., and Planck Collaboration

19. The Planck mission

Author

Mandolesi, N., Burigana, C., Gruppuso, A., Procopio, P., and Sara Ricciardi

20. First Look Murchison Widefield Array observations of Abell 3667

Author

Hindson, L., Johnston-Hollitt, M., Hurley-Walker, N., Morgan, J., Buckley, K., Carretti, E., Dwarakanath, K. S., Bell, M., Bernardi, G., Bhat, R., Briggs, F., Deshpande, A. A., Ewall-Wice, A., Feng, L., Hazeltonm, B., Jacobs, D., Kaplan, D., Kudryavtseva, N., Lenc, E., Mckinley, B., Mitchell, D., Pindor, B., Procopio, P., Oberoi, D., Offringa, A. R., Ord, S., Riding, J., Bowman, J. D., Cappallo, R., Corey, B., David Emrich, Gaensler, B. M., Goeke, R., Greenhill, L., Kasper, I., Kratzenberg, E., Lonsdale, C., Lynch, M., Mcwhirter, R., Morales, M., Morgan, E., Prabu, T., Rogers, A., Roshi, A., Shankar, U., Srivani, K., Subrahmanyan, R., Tingay, S., Waterson, M., Webster, R., Whitney, A., Williams, A., Williams, C., and IEEE

Subjects
Physics, Murchison meteorite, Spectral index, Astronomy, Flux, FOS: Physical sciences, Murchison Widefield Array, Astrophysics, Low frequency, Astrophysics - Astrophysics of Galaxies, Radio telescope, Interferometry, Radio relics, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The Murchison Widefield Array (MWA) is a new low frequency interferometric radio telescope, operating in the remote Murchison Radio Observatory in Western Australia. In this paper we present the first MWA observations of the well known radio relics in Abell 3667 (A3667) between 120 and 226 MHz. We clearly detect the radio relics in A3667 and present flux estimates and spectral indices for these features. The average spectral index of the north-west (NW) and south-east (SE) relics is -0.9 +/- 0.1 between 120 and 1400 MHz. We are able to resolve spatial variation in the spectral index of the NW relic from -1.7 to -0.4, which is consistent with results found at higher frequencies., Comment: 4 pages, 4 figures, accepted for the 31st URSI General Assembly Proceedings to be published in IEEE Xplore

21. A 20 GHz bright sample for > 72 - II. Multifrequency follow-up

Author

F. Mantovani, Marcin P. Gawronski, Isabella Prandoni, Simona Righini, L. Gregorini, Roberto Ricci, Ettore Carretti, Pietro Procopio, A. Zanichelli, Michael W. Peel, Karl-Heinz Mack, R. Verma, Marcella Massardi, Ricci R., Righini S., Verma R., Prandoni I., Carretti E., Mack K.-H., Massardi M., Procopio P., Zanichelli A., Gregorini L., Mantovani F., Gawroński M. P., and Peel M. W.

Subjects
Physics, QSOS, Radio galaxy, RADIO CONTINUUM: GENERAL, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Spectral properties, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Sample (graphics), Redshift, Spectral line, Radio telescope, Space and Planetary Science, RADIO CONTINUUM: GALAXIES, Polar cap, Astrophysics::Galaxy Astrophysics
Abstract

We present follow-up observations at 5, 8 and 30 GHz of the K-band Northern Wide Survey (KNoWS) 20 GHz Bright Sample, performed with the 32-m Medicina radio telescope and the 32-m Toruń radio telescope. The KNoWS sources were selected in the Northern Polar Cap (δ > 72°) and have a flux density limit S20 GHz = 115 mJy. We include NRAO-VLA Sky Survey 1.4 GHz measurements to derive the source radio spectra between 1.4 and 30 GHz. Based on optical identifications, 68 per cent of the sources are quasars and 27 per cent are radio galaxies. A redshift measurement is available for 58 per cent of the sources. The radio spectral properties of the different source populations are found to be in agreement with those of other high-frequency-selected samples.

Published
2013

22. Simultaneous Planck, Swift, and Fermi observations of X-ray and gamma-ray selected blazars

Author

Thomas P. Krichbaum, Carlo Burigana, C. Monte, L. Toffolatti, Anthony Lasenby, F. D'Ammando, M. López-Caniego, G. Polenta, Jingwen Wu, Andrea Tramacere, E. Keihänen, M. Perri, Andrei Berdyugin, S. Cutini, E. Cavazzuti, M. Capalbi, A. Sillanpää, T. J. Pearson, R. Reinthal, G. Tagliaferri, P. Giommi, Mn Mazziotta, P. F. Michelson, Vasiliki Pavlidou, D. J. Thompson, M. Frailis, Laura Bonavera, Luigi Costamante, I. Nestoras, Walter Max-Moerbeck, C. Leto, N. Gehrels, S. Ricciardi, Jörg P. Rachen, A. Reimer, Emmanouil Angelakis, G. de Zotti, L. Fuhrmann, David N. Burrows, G. Tosti, H. Ungerechts, Joni Tammi, D. Gasparrini, Francesco Giordano, M. Turunen, Corrado Trigilio, Anna Sajina, R. Reeves, F. Villa, A. C. S. Readhead, S. Colafrancesco, Marcella Massardi, Charles R. Lawrence, Jonathan León-Tavares, N. Mandolesi, G. Umana, Marcello Giroletti, F. Verrecchia, Yu. V. Sotnikova, O. King, Xu Zhou, F. Gargano, E. Nieppola, A. Sievers, Kari Nilsson, B. Partridge, N. Lavonen, Jari Saarinen, D. Bastieri, Andrea Zacchei, Pietro Procopio, D. Riquelme, D. Tavagnacco, Nicola Giglietto, Luca Terenzi, J. González-Nuevo, J. A. Zensus, G. Chincarini, F. Cuttaia, L. O. Takalo, M. F. Aller, Anna Bonaldi, Anne Lähteenmäki, Mark Stevenson, S. Galeotta, S. Buson, M. Sandri, Hugh D. Aller, J. L. Richards, M. G. Mingaliev, Elina Lindfors, S. Rainò, Paolo Natoli, Merja Tornikoski, P. Savolainen, Giommi P, Polenta G, Lahteenmaki A, Thompson DJ, Capalbi M, Cutini S, Gasparrini D, Gonzalez-Nuevo J, Leon-Tavares J, Lopez-Caniego M, Mazziotta MN, Monte C, Perri M, Raino S, Tosti G, Tramacere A, Verrecchia F, Aller HD, Aller MF, Angelakis E, Bastieri D, Berdyugin A, Bonaldi A, Bonavera L, Burigana C, Burrows DN, Buson S, Cavazzuti E, Chincarini G, Colafrancesco S, Costamante L, Cuttaia F, DAmmando F, de Zotti G, Frailis M, Fuhrmann L, Galeotta S, Gargano F, Gehrels N, Giglietto N, Giordano F, Giroletti M, Keihanen E, King O, Krichbaum TP, Lasenby A, Lavonen N, Lawrence CR, Leto C, Lindfors E, Mandolesi N, Massardi M, Max-Moerbeck W, Michelson PF, Mingaliev M, Natoli P, Nestoras I, Nieppola E, Nilsson K, Partridge B, Pavlidou V, Pearson TJ, Procopio P, Rachen JP, Readhead A, Reeves R, Reimer A, Reinthal R, Ricciardi S, Richards J, Riquelme D, Saarinen J, Sajina A, Sandri M, Savolainen P, Sievers A, Sillanpaa A, Sotnikova Y, Stevenson M, Tagliaferri G, Takalo L, Tammi J, Tavagnacco D, Terenzi L, Toffolatti L, Tornikoski M, Trigilio C, Turunen M, Umana G, Ungerechts H, Villa F, Wu J, Zacchei A, Zensus JA, Zhou X, Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, European Space Agency, Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Consiglio Nazionale delle Ricerche, Istituto Nazionale di Astrofisica, Agenzia Spaziale Italiana, National Aeronautics and Space Administration (US), Department of Energy (US), Science and Technology Facilities Council (UK), UK Space Agency, Ministerio de Ciencia e Innovación (España), Junta de Andalucía, Consejo Superior de Investigaciones Científicas (España), Academy of Finland, Center for Science (Finland), German Centre for Air and Space Travel, Max Planck Society, DTU Space (Denmark), Swiss Space Office, Research Council of Norway, Science Foundation Ireland, and Fundação para a Ciência e a Tecnologia (Portugal)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, education, galaxies: active, Flux, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Spectral line, Luminosity, symbols.namesake, quasars: general, Planck, Blazar, relativistic processes, Physics, general [quasars], general [BL Lacertae objects], Gamma ray, Astronomy and Astrophysics, Quasar, BL Lacertae objects: general, relativistic processes, BL Lacertae objects: general, quasars: general, galaxies: active, Space and Planetary Science, active [galaxies], symbols, relativistic processes, BL Lacertae objects: general,quasars: general, galaxies: active, Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

Planck Collaboration et al., We present simultaneous Planck, Swift, Fermi, and ground-based data for 105 blazars belonging to three samples with flux limits in the soft X-ray, hard X-ray, and γ-ray bands, with additional 5GHz flux-density limits to ensure a good probability of a Planck detection. We compare our results to those of a companion paper presenting simultaneous Planck and multi-frequency observations of 104 radio-loud northern active galactic nuclei selected at radio frequencies. While we confirm several previous results, our unique data set allows us to demonstrate that the selection method strongly influences the results, producing biases that cannot be ignored. Almost all the BL Lac objects have been detected by the Fermi Large AreaTelescope (LAT), whereas 30% to 40% of the flat-spectrum radio quasars (FSRQs) in the radio, soft X-ray, and hard X-ray selected samples are still below the γ-ray detection limit even after integrating 27 months of Fermi-LAT data. The radio to sub-millimetre spectral slope of blazars is quite flat, with α ~ 0 up to about 70GHz, above which it steepens to α ~-0.65. The BL Lacs have significantly flatter spectra than FSRQs at higher frequencies. The distribution of the rest-frame synchrotron peak frequency (ν peak S) in the spectral energy distribution (SED) of FSRQs is the same in all the blazar samples with ν peak S = 10 13.1 ± 0.1 Hz, while the mean inverse Compton peak frequency, ν peak IC, ranges from 10 21 to 10 22 Hz. The distributions of ν peak S and ν peak IC of BL Lacs are much broader and are shifted to higher energies than those of FSRQs; their shapes strongly depend on the selection method. The Compton dominance of blazars, defined as the ratio of the inverse Compton to synchrotron peak luminosities, ranges from less than 0.2 to nearly 100, with only FSRQs reaching values larger than about 3. Its distribution is broad and depends strongly on the selection method, with γ-ray selected blazars peaking at ~7 or more, and radio-selected blazars at values close to 1, thus implying that the common assumption that the blazar power budget is largely dominated by high-energy emission is a selection effect. A comparison of our multi-frequency data with theoretical predictions shows that simple homogeneous SSC models cannot explain the simultaneous SEDs of most of the γ-ray detected blazars in all samples. The SED of the blazars that were not detected by Fermi-LAT may instead be consistent with SSC emission. Our data challenge the correlation between bolometric luminosity and ν peak S predicted by the blazar sequence. © 2012 ESO., The Planck Collaboration acknowledges the support of: 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).

Published
2012

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