ALBERT

Description: Recent observations of supernova remnants (SNRs) hint that they accelerate cosmic rays to energies close to ~10(15) electron volts. However, the nature of the particles that produce the emission remains ambiguous. We report observations of SNR W44 with the Fermi Large Area Telescope at energies between 2 x 10(8) electron volts and 3 x10(11) electron volts. The detection of a source with a morphology corresponding to the SNR shell implies that the emission is produced by particles accelerated there. The gamma-ray spectrum is well modeled with emission from protons and nuclei. Its steepening above approximately 10(9) electron volts provides a probe with which to study how particle acceleration responds to environmental effects such as shock propagation in dense clouds and how accelerated particles are released into interstellar space.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Abdo, A A -- Ackermann, M -- Ajello, M -- Baldini, L -- Ballet, J -- Barbiellini, G -- Baring, M G -- Bastieri, D -- Baughman, B M -- Bechtol, K -- Bellazzini, R -- Berenji, B -- Blandford, R D -- Bloom, E D -- Bonamente, E -- Borgland, A W -- Bregeon, J -- Brez, A -- Brigida, M -- Bruel, P -- Burnett, T H -- Buson, S -- Caliandro, G A -- Cameron, R A -- Caraveo, P A -- Casandjian, J M -- Cecchi, C -- Celik, O -- Chekhtman, A -- Cheung, C C -- Chiang, J -- Ciprini, S -- Claus, R -- Cognard, I -- Cohen-Tanugi, J -- Cominsky, L R -- Conrad, J -- Cutini, S -- Dermer, C D -- de Angelis, A -- de Palma, F -- Digel, S W -- do Couto e Silva, E -- Drell, P S -- Dubois, R -- Dumora, D -- Espinoza, C -- Farnier, C -- Favuzzi, C -- Fegan, S J -- Focke, W B -- Fortin, P -- Frailis, M -- Fukazawa, Y -- Funk, S -- Fusco, P -- Gargano, F -- Gasparrini, D -- Gehrels, N -- Germani, S -- Giavitto, G -- Giebels, B -- Giglietto, N -- Giordano, F -- Glanzman, T -- Godfrey, G -- Grenier, I A -- Grondin, M-H -- Grove, J E -- Guillemot, L -- Guiriec, S -- Hanabata, Y -- Harding, A K -- Hayashida, M -- Hays, E -- Hughes, R E -- Jackson, M S -- Johannesson, G -- Johnson, A S -- Johnson, T J -- Johnson, W N -- Kamae, T -- Katagiri, H -- Kataoka, J -- Katsuta, J -- Kawai, N -- Kerr, M -- Knodlseder, J -- Kocian, M L -- Kramer, M -- Kuss, M -- Lande, J -- Latronico, L -- Lemoine-Goumard, M -- Longo, F -- Loparco, F -- Lott, B -- Lovellette, M N -- Lubrano, P -- Lyne, A G -- Madejski, G M -- Makeev, A -- Mazziotta, M N -- McEnery, J E -- Meurer, C -- Michelson, P F -- Mitthumsiri, W -- Mizuno, T -- Monte, C -- Monzani, M E -- Morselli, A -- Moskalenko, I V -- Murgia, S -- Nakamori, T -- Nolan, P L -- Norris, J P -- Noutsos, A -- Nuss, E -- Ohsugi, T -- Omodei, N -- Orlando, E -- Ormes, J F -- Paneque, D -- Parent, D -- Pelassa, V -- Pepe, M -- Pesce-Rollins, M -- Piron, F -- Porter, T A -- Raino, S -- Rando, R -- Razzano, M -- Reimer, A -- Reimer, O -- Reposeur, T -- Rochester, L S -- Rodriguez, A Y -- Romani, R W -- Roth, M -- Ryde, F -- Sadrozinski, H F-W -- Sanchez, D -- Sander, A -- Saz Parkinson, P M -- Scargle, J D -- Sgro, C -- Siskind, E J -- Smith, D A -- Smith, P D -- Spandre, G -- Spinelli, P -- Stappers, B W -- Stecker, F W -- Strickman, M S -- Suson, D J -- Tajima, H -- Takahashi, H -- Takahashi, T -- Tanaka, T -- Thayer, J B -- Thayer, J G -- Theureau, G -- Thompson, D J -- Tibaldo, L -- Tibolla, O -- Torres, D F -- Tosti, G -- Tramacere, A -- Uchiyama, Y -- Usher, T L -- Vasileiou, V -- Venter, C -- Vilchez, N -- Vitale, V -- Waite, A P -- Wang, P -- Winer, B L -- Wood, K S -- Yamazaki, R -- Ylinen, T -- Ziegler, M -- New York, N.Y. -- Science. 2010 Feb 26;327(5969):1103-6. doi: 10.1126/science.1182787. Epub 2010 Jan 7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Space Science Division, Naval Research Laboratory, Washington, DC 20375, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20056857" target="_blank"〉PubMed〈/a〉

Description: Pulsars emit from low-frequency radio waves up to high-energy gamma-rays, generated anywhere from the stellar surface out to the edge of the magnetosphere. Detecting correlated mode changes across the electromagnetic spectrum is therefore key to understanding the physical relationship among the emission sites. Through simultaneous observations, we detected synchronous switching in the radio and x-ray emission properties of PSR B0943+10. When the pulsar is in a sustained radio-"bright" mode, the x-rays show only an unpulsed, nonthermal component. Conversely, when the pulsar is in a radio-"quiet" mode, the x-ray luminosity more than doubles and a 100% pulsed thermal component is observed along with the nonthermal component. This indicates rapid, global changes to the conditions in the magnetosphere, which challenge all proposed pulsar emission theories.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hermsen, W -- Hessels, J W T -- Kuiper, L -- van Leeuwen, J -- Mitra, D -- de Plaa, J -- Rankin, J M -- Stappers, B W -- Wright, G A E -- Basu, R -- Alexov, A -- Coenen, T -- Griessmeier, J-M -- Hassall, T E -- Karastergiou, A -- Keane, E -- Kondratiev, V I -- Kramer, M -- Kuniyoshi, M -- Noutsos, A -- Serylak, M -- Pilia, M -- Sobey, C -- Weltevrede, P -- Zagkouris, K -- Asgekar, A -- Avruch, I M -- Batejat, F -- Bell, M E -- Bell, M R -- Bentum, M J -- Bernardi, G -- Best, P -- Birzan, L -- Bonafede, A -- Breitling, F -- Broderick, J -- Bruggen, M -- Butcher, H R -- Ciardi, B -- Duscha, S -- Eisloffel, J -- Falcke, H -- Fender, R -- Ferrari, C -- Frieswijk, W -- Garrett, M A -- de Gasperin, F -- de Geus, E -- Gunst, A W -- Heald, G -- Hoeft, M -- Horneffer, A -- Iacobelli, M -- Kuper, G -- Maat, P -- Macario, G -- Markoff, S -- McKean, J P -- Mevius, M -- Miller-Jones, J C A -- Morganti, R -- Munk, H -- Orru, E -- Paas, H -- Pandey-Pommier, M -- Pandey, V N -- Pizzo, R -- Polatidis, A G -- Rawlings, S -- Reich, W -- Rottgering, H -- Scaife, A M M -- Schoenmakers, A -- Shulevski, A -- Sluman, J -- Steinmetz, M -- Tagger, M -- Tang, Y -- Tasse, C -- ter Veen, S -- Vermeulen, R -- van de Brink, R H -- van Weeren, R J -- Wijers, R A M J -- Wise, M W -- Wucknitz, O -- Yatawatta, S -- Zarka, P -- New York, N.Y. -- Science. 2013 Jan 25;339(6118):436-9. doi: 10.1126/science.1230960.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, Netherlands. w.hermsen@sron.nl〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/23349288" target="_blank"〉PubMed〈/a〉

Description: X-ray binaries are composed of a normal star in orbit around a neutron star or stellar-mass black hole. Radio and x-ray observations have led to the presumption that some x-ray binaries called microquasars behave as scaled-down active galactic nuclei. Microquasars have resolved radio emission that is thought to arise from a relativistic outflow akin to active galactic nuclei jets, in which particles can be accelerated to large energies. Very high energy gamma-rays produced by the interactions of these particles have been observed from several active galactic nuclei. Using the High Energy Stereoscopic System, we find evidence for gamma-ray emission of 〉100 gigaelectron volts from a candidate microquasar, LS 5039, showing that particles are also accelerated to very high energies in these systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Aharonian, F -- Akhperjanian, A G -- Aye, K-M -- Bazer-Bachi, A R -- Beilicke, M -- Benbow, W -- Berge, D -- Berghaus, P -- Bernlohr, K -- Boisson, C -- Bolz, O -- Borrel, V -- Braun, I -- Breitling, F -- Brown, A M -- Bussons Gordo, J -- Chadwick, P M -- Chounet, L-M -- Cornils, R -- Costamante, L -- Degrange, B -- Dickinson, H J -- Djannati-Atai, A -- Drury, L O'c -- Dubus, G -- Emmanoulopoulos, D -- Espigat, P -- Feinstein, F -- Fleury, P -- Fontaine, G -- Fuchs, Y -- Funk, S -- Gallant, Y A -- Giebels, B -- Gillessen, S -- Glicenstein, J F -- Goret, P -- Hadjichristidis, C -- Hauser, M -- Heinzelmann, G -- Henri, G -- Hermann, G -- Hinton, J A -- Hofmann, W -- Holleran, M -- Horns, D -- Jacholkowska, A -- de Jager, O C -- Khelifi, B -- Komin, Nu -- Konopelko, A -- Latham, I J -- Le Gallou, R -- Lemiere, A -- Lemoine-Goumard, M -- Leroy, N -- Lohse, T -- Marcowith, A -- Martin, J-M -- Martineau-Huynh, O -- Masterson, C -- McComb, T J L -- de Naurois, M -- Nolan, S J -- Noutsos, A -- Orford, K J -- Osborne, J L -- Ouchrif, M -- Panter, M -- Pelletier, G -- Pita, S -- Puhlhofer, G -- Punch, M -- Raubenheimer, B C -- Raue, M -- Raux, J -- Rayner, S M -- Reimer, A -- Reimer, O -- Ripken, J -- Rob, L -- Rolland, L -- Rowell, G -- Sahakian, V -- Sauge, L -- Schlenker, S -- Schlickeiser, R -- Schuster, C -- Schwanke, U -- Siewert, M -- Sol, H -- Spangler, D -- Steenkamp, R -- Stegmann, C -- Tavernet, J-P -- Terrier, R -- Theoret, C G -- Tluczykont, M -- Vasileiadis, G -- Venter, C -- Vincent, P -- Volk, H J -- Wagner, S J -- New York, N.Y. -- Science. 2005 Jul 29;309(5735):746-9. Epub 2005 Jul 7.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Kernphysik, Post Office Box 103980, D-69029 Heidelberg, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16002580" target="_blank"〉PubMed〈/a〉

Description: Very high energy gamma-rays probe the long-standing mystery of the origin of cosmic rays. Produced in the interactions of accelerated particles in astrophysical objects, they can be used to image cosmic particle accelerators. A first sensitive survey of the inner part of the Milky Way with the High Energy Stereoscopic System (HESS) reveals a population of eight previously unknown firmly detected sources of very high energy gamma-rays. At least two have no known radio or x-ray counterpart and may be representative of a new class of "dark" nucleonic cosmic ray sources.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Aharonian, F -- Akhperjanian, A G -- Aye, K-M -- Bazer-Bachi, A R -- Beilicke, M -- Benbow, W -- Berge, D -- Berghaus, P -- Bernlohr, K -- Boisson, C -- Bolz, O -- Borgmeier, C -- Braun, I -- Breitling, F -- Brown, A M -- Gordo, J Bussons -- Chadwick, P M -- Chounet, L-M -- Cornils, R -- Costamante, L -- Degrange, B -- Djannati-Atai, A -- Drury, L O'C -- Dubus, G -- Ergin, T -- Espigat, P -- Feinstein, F -- Fleury, P -- Fontaine, G -- Funk, S -- Gallant, Y A -- Giebels, B -- Gillessen, S -- Goret, P -- Hadjichristidis, C -- Hauser, M -- Heinzelmann, G -- Henri, G -- Hermann, G -- Hinton, J A -- Hofmann, W -- Holleran, M -- Horns, D -- de Jager, O C -- Jung, I -- Khelifi, B -- Komin, Nu -- Konopelko, A -- Latham, I J -- Le Gallou, R -- Lemiere, A -- Lemoine, M -- Leroy, N -- Lohse, T -- Marcowith, A -- Masterson, C -- McComb, T J L -- de Naurois, M -- Nolan, S J -- Noutsos, A -- Orford, K J -- Osborne, J L -- Ouchrif, M -- Panter, M -- Pelletier, G -- Pita, S -- Puhlhofer, G -- Punch, M -- Raubenheimer, B C -- Raue, M -- Raux, J -- Rayner, S M -- Redondo, I -- Reimer, A -- Reimer, O -- Ripken, J -- Rob, L -- Rolland, L -- Rowell, G -- Sahakian, V -- Sauge, L -- Schlenker, S -- Schlickeiser, R -- Schuster, C -- Schwanke, U -- Siewert, M -- Sol, H -- Steenkamp, R -- Stegmann, C -- Tavernet, J-P -- Terrier, R -- Theoret, C G -- Tluczykont, M -- van der Walt, D J -- Vasileiadis, G -- Venter, C -- Vincent, P -- Visser, B -- Volk, H J -- Wagner, S J -- New York, N.Y. -- Science. 2005 Mar 25;307(5717):1938-42.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Kernphysik, Post Office Box 103980, D-69029 Heidelberg, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15790849" target="_blank"〉PubMed〈/a〉

Description: The detection of fast variations of the tera-electron volt (TeV) (10(12) eV) gamma-ray flux, on time scales of days, from the nearby radio galaxy M87 is reported. These variations are about 10 times as fast as those observed in any other wave band and imply a very compact emission region with a dimension similar to the Schwarzschild radius of the central black hole. We thus can exclude several other sites and processes of the gamma-ray production. The observations confirm that TeV gamma rays are emitted by extragalactic sources other than blazars, where jets are not relativistically beamed toward the observer.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Aharonian, F -- Akhperjanian, A G -- Bazer-Bachi, A R -- Beilicke, M -- Benbow, W -- Berge, D -- Bernlohr, K -- Boisson, C -- Bolz, O -- Borrel, V -- Braun, I -- Brown, A M -- Buhler, R -- Busching, I -- Carrigan, S -- Chadwick, P M -- Chounet, L-M -- Coignet, G -- Cornils, R -- Costamante, L -- Degrange, B -- Dickinson, H J -- Djannati-Atai, A -- Drury, L O'c -- Dubus, G -- Egberts, K -- Emmanoulopoulos, D -- Espigat, P -- Feinstein, F -- Ferrero, E -- Fiasson, A -- Fontaine, G -- Funk, Seb -- Funk, S -- Fussling, M -- Gallant, Y A -- Giebels, B -- Glicenstein, J F -- Goret, P -- Hadjichristidis, C -- Hauser, D -- Hauser, M -- Heinzelmann, G -- Henri, G -- Hermann, G -- Hinton, J A -- Hoffmann, A -- Hofmann, W -- Holleran, M -- Hoppe, S -- Horns, D -- Jacholkowska, A -- de Jager, O C -- Kendziorra, E -- Kerschhaggl, M -- Khelifi, B -- Komin, Nu -- Konopelko, A -- Kosack, K -- Lamanna, G -- Latham, I J -- Le Gallou, R -- Lemiere, A -- Lemoine-Goumard, M -- Lenain, J-P -- Lohse, T -- Martin, J M -- Martineau-Huynh, O -- Marcowith, A -- Masterson, C -- Maurin, G -- McComb, T J L -- Moulin, E -- de Naurois, M -- Nedbal, D -- Nolan, S J -- Noutsos, A -- Orford, K J -- Osborne, J L -- Ouchrif, M -- Panter, M -- Pelletier, G -- Pita, S -- Puhlhofer, G -- Punch, M -- Ranchon, S -- Raubenheimer, B C -- Raue, M -- Rayner, S M -- Reimer, A -- Ripken, J -- Rob, L -- Rolland, L -- Rosier-Lees, S -- Rowell, G -- Sahakian, V -- Santangelo, A -- Sauge, L -- Schlenker, S -- Schlickeiser, R -- Schroder, R -- Schwanke, U -- Schwarzburg, S -- Schwemmer, S -- Shalchi, A -- Sol, H -- Spangler, D -- Spanier, F -- Steenkamp, R -- Stegmann, C -- Superina, G -- Tam, P H -- Tavernet, J-P -- Terrier, R -- Tluczykont, M -- van Eldik, C -- Vasileiadis, G -- Venter, C -- Vialle, J P -- Vincent, P -- Volk, H J -- Wagner, S J -- Ward, M -- New York, N.Y. -- Science. 2006 Dec 1;314(5804):1424-7. Epub 2006 Oct 26.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Max-Planck-Institut fur Kernphysik, Post Office Box 103980, D 69029 Heidelberg, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17068224" target="_blank"〉PubMed〈/a〉