@article {2013PASA...30....3D, title = {{GASKAP-The Galactic ASKAP Survey}}, journal = {Publications of the Astronomical Society of Australia}, volume = {30}, year = {2013}, month = {jan}, pages = {3}, abstract = {A survey of the Milky Way disk and the Magellanic System at the wavelengths of the 21-cm atomic hydrogen (HI) line and three 18-cm lines of the OH molecule will be carried out with the Australian Square Kilometre Array Pathfinder telescope. The survey will study the distribution of HI emission and absorption with unprecedented angular and velocity resolution, as well as molecular line thermal emission, absorption, and maser lines. The area to be covered includes the Galactic plane (|b| {\l}t} 10{\deg}) at all declinations south of {$δ$} = +40{\deg}, spanning longitudes 167{\deg} through 360{\deg}to 79{\deg} at b = 0{\deg}, plus the entire area of the Magellanic Stream and Clouds, a total of 13 020 deg$^{2}$. The brightness temperature sensitivity will be very good, typically {$\sigma$}$_{T}${\sime} 1 K at resolution 30 arcsec and 1 km s$^{-1}$. The survey has a wide spectrum of scientific goals, from studies of galaxy evolution to star formation, with particular contributions to understanding stellar wind kinematics, the thermal phases of the interstellar medium, the interaction between gas in the disk and halo, and the dynamical and thermal states of gas at various positions along the Magellanic Stream.}, keywords = {Galaxy: evolution, Galaxy: general, ISM: clouds, ISM: general, ISM: kinematics and dynamics, ISM: molecules}, doi = {10.1017/pasa.2012.003}, url = {http://adsabs.harvard.edu/abs/2013PASA...30....3D}, author = {Dickey, J.~M. and McClure-Griffiths, N. and Gibson, S.~J. and G{\'o}mez, J.~F. and Imai, H. and Jones, P. and Stanimirovi{\'c}, S. and Van Loon, J.~T. and Walsh, A. and Alberdi, A. and Anglada, G. and Uscanga, L. and Arce, H. and Bailey, M. and Begum, A. and Wakker, B. and Bekhti, N.~B. and Kalberla, P. and Winkel, B. and Bekki, K. and For, B.-Q. and Staveley-Smith, L. and Westmeier, T. and Burton, M. and Cunningham, M. and Dawson, J. and Ellingsen, S. and Diamond, P. and Green, J.~A. and Hill, A.~S. and Koribalski, B. and McConnell, D. and Rathborne, J. and Voronkov, M. and Douglas, K.~A. and English, J. and Ford, H.~A. and Lockman, F.~J. and Foster, T. and Gomez, Y. and Green, A. and Bland-Hawthorn, J. and Gulyaev, S. and Hoare, M. and Joncas, G. and Kang, J.-H. and Kerton, C.~R. and Koo, B.-C. and Leahy, D. and Lo, N. and Migenes, V. and Nakashima, J. and Zhang, Y. and Nidever, D. and Peek, J.~E.~G. and Tafoya, D. and Tian, W. and Wu, D.} } @article {2012A\&A...541A..13A, title = {{Morphological and spectral properties of the W51 region measured with the MAGIC telescopes}}, journal = {Astronomy and Astrophysics}, volume = {541}, year = {2012}, month = {may}, pages = {A13}, abstract = {Context. The W51 complex hosts the supernova remnant W51C which is known to interact with the molecular clouds in the star forming region W51B. In addition, a possible pulsar wind nebula CXO J192318.5+140305 was found likely associated with the supernova remnant. Gamma-ray emission from this region was discovered by Fermi/LAT (between 0.2 and 50 GeV) and H.E.S.S. ({\gt}1 TeV). The spatial distribution of the events could not be used to pinpoint the location of the emission among the pulsar wind nebula, the supernova remnant shell and/or the molecular cloud. However, the modeling of the spectral energy distribution presented by the Fermi/LAT collaboration suggests a hadronic emission mechanism. The possibility that the gamma-ray emission from such an object is of hadronic origin can contribute to solvingthe long-standing problem of the contribution to galactic cosmic rays by supernova remnants.
Aims: Our aim is to determine the morphology of the very-high-energy gamma-ray emission of W51 and measure its spectral properties.
Methods: We performed observations of the W51 complex with the MAGIC telescopes for more than 50 h. The energy range accessible with MAGIC extends from 50 GeV to several TeV, allowing for the first spectral measurement at these energies. In addition, the good angular resolution in the medium (few hundred GeV) to high (above 1 TeV) energies allow us to perform morphological studies. We look for underlying structures by means of detailed morphological studies. Multi-wavelength data from this source have been sampled to model the emission with both leptonic and hadronic processes.
Results: We detect an extended emission of very-high-energy gamma rays, with a significance of 11 standard deviations. We extend the spectrum from the highest Fermi/LAT energies to \~{}5 TeV and find that it follows a single power law with an index of 2.58 {\plusmn} 0.07$_{stat}$ {\plusmn} 0.22$_{syst}$. The main part of the emission coincides with the shocked cloud region, while we find a feature extending towards the pulsar wind nebula. The possible contribution of the pulsar wind nebula, assuming a point-like source, shows no dependence on energy and it is about 20\% of the overall emission. The broad band spectral energy distribution can be explained with a hadronic model that implies proton acceleration above 100 TeV. This result, together with the morphology of the source, tentatively suggests that we observe ongoing acceleration of ions in the interaction zone between supernova remnant and cloud.}, keywords = {acceleration of particles, gamma rays: general, gamma rays: ISM, ISM: clouds, ISM: supernova remnants}, doi = {10.1051/0004-6361/201218846}, url = {http://adsabs.harvard.edu/abs/2012A\%26A...541A..13A}, author = {Aleksi{\'c}, J. and Alvarez, E.~A. and Antonelli, L.~A. and Antoranz, P. and Asensio, M. and Backes, M. and Barres de Almeida, U. and Barrio, J.~A. and Bastieri, D. and Becerra Gonz{\'a}lez, J. and Bednarek, W. and Berger, K. and Bernardini, E. and Biland, A. and Blanch, O. and Bock, R.~K. and Boller, A. and Bonnoli, G. and Borla Tridon, D. and Bretz, T. and Ca{\~n}ellas, A. and Carmona, E. and Carosi, A. and Colin, P. and Colombo, E. and Contreras, J.~L. and Cortina, J. and Cossio, L. and Covino, S. and Da Vela, P. and Dazzi, F. and De Angelis, A. and De Caneva, G. and De Cea del Pozo, E. and De Lotto, B. and Delgado Mendez, C. and Diago Ortega, A. and Doert, M. and Dom{\'\i}nguez, A. and Dominis Prester, D. and Dorner, D. and Doro, M. and Eisenacher, D. and Elsaesser, D. and Ferenc, D. and Fonseca, M.~V. and Font, L. and Fruck, C. and Garc{\'\i}a L{\'o}pez, R.~J. and Garczarczyk, M. and Garrido, D. and Giavitto, G. and Godinovi{\'c}, N. and Gonz{\'a}lez Mu{\~n}oz, A. and Gozzini, S.~R. and Hadasch, D. and H{\"a}fner, D. and Herrero, A. and Hildebrand, D. and Hose, J. and Hrupec, D. and Huber, B. and Jankowski, F. and Jogler, T. and Kadenius, V. and Kellermann, H. and Klepser, S. and Kr{\"a}henb{\"u}hl, T. and Krause, J. and La Barbera, A. and Lelas, D. and Leonardo, E. and Lewandowska, N. and Lindfors, E. and Lombardi, S. and L{\'o}pez, M. and L{\'o}pez-Coto, R. and L{\'o}pez-Oramas, A. and Lorenz, E. and Makariev, M. and Maneva, G. and Mankuzhiyil, N. and Mannheim, K. and Maraschi, L. and Mariotti, M. and Mart{\'\i}nez, M. and Mazin, D. and Meucci, M. and Miranda, J.~M. and Mirzoyan, R. and Mold{\'o}n, J. and Moralejo, A. and Munar-Adrover, P. and Niedzwiecki, A. and Nieto, D. and Nilsson, K. and Nowak, N. and Orito, R. and Paiano, S. and Paneque, D. and Paoletti, R. and Pardo, S. and Paredes, J.~M. and Partini, S. and M. A. P{\'e}rez-Torres and Persic, M. and Pilia, M. and Pochon, J. and Prada, F. and Prada Moroni, P.~G. and Prandini, E. and Puerto Gimenez, I. and Puljak, I. and Reichardt, I. and Reinthal, R. and Rhode, W. and Rib{\'o}, M. and Rico, J. and R{\"u}gamer, S. and Saggion, A. and Saito, K. and Saito, T.~Y. and Salvati, M. and Satalecka, K. and Scalzotto, V. and Scapin, V. and Schultz, C. and Schweizer, T. and Shore, S.~N. and Sillanp{\"a}{\"a}, A. and Sitarek, J. and Snidaric, I. and Sobczynska, D. and Spanier, F. and Spiro, S. and Stamatescu, V. and Stamerra, A. and Steinke, B. and Storz, J. and Strah, N. and Sun, S. and Suri{\'c}, T. and Takalo, L. and Takami, H. and Tavecchio, F. and Temnikov, P. and Terzi{\'c}, T. and Tescaro, D. and Teshima, M. and Tibolla, O. and Torres, D.~F. and Treves, A. and Uellenbeck, M. and Vogler, P. and Wagner, R.~M. and Weitzel, Q. and Zabalza, V. and Zandanel, F. and Zanin, R.} }