ALBERT

Description: Corrigendum: A large light-mass component of cosmic rays at 1017–1017.5 electronvolts from radio observations Nature 537, 7621 (2016). doi:10.1038/nature18936 Authors: S. Buitink, A. Corstanje, H. Falcke, J. R. Hörandel, T. Huege, A. Nelles, J. P. Rachen, L. Rossetto, P. Schellart, O. Scholten, S. ter Veen, S. Thoudam, T. N. G. Trinh, J. Anderson, A. Asgekar, I. M. Avruch, M. E. Bell, M. J. Bentum, G. Bernardi, P. Best, A. Bonafede, F. Breitling, J. W. Broderick, W. N. Brouw, M. Brüggen, H. R. Butcher, D. Carbone, B. Ciardi, J. E. Conway, F. de Gasperin, E. de Geus, A. Deller, R.-J. Dettmar, G. van Diepen, S. Duscha, J. Eislöffel, D. Engels, J. E. Enriquez, R. A. Fallows, R. Fender, C. Ferrari, W. Frieswijk, M. A. Garrett, J. M. Grießmeier, A. W. Gunst, M. P. van Haarlem, T. E. Hassall, G. Heald, J. W. T. Hessels, M. Hoeft, A. Horneffer, M. Iacobelli, H. Intema, E. Juette, A. Karastergiou, V. I. Kondratiev, M. Kramer, M. Kuniyoshi, G. Kuper, J. van Leeuwen, G. M. Loose, P. Maat, G. Mann, S. Markoff, R. McFadden, D. McKay-Bukowski, J. P. McKean, M. Mevius, D. D. Mulcahy, H. Munk, M. J. Norden, E. Orru, H. Paas, M. Pandey-Pommier, V. N. Pandey, M. Pietka, R. Pizzo, A. G. Polatidis, W. Reich, H. J. A. Röttgering, A. M. M. Scaife, D. J. Schwarz, M. Serylak, J. Sluman, O. Smirnov, B. W. Stappers, M. Steinmetz, A. Stewart, J. Swinbank, M. Tagger, Y. Tang, C. Tasse, M. C. Toribio, R. Vermeulen, C. Vocks, C. Vogt, R. J. van Weeren, R. A. M. J. Wijers, S. J. Wijnholds, M. W. Wise, O. Wucknitz, S. Yatawatta, P. Zarka & J. A. Zensus Nature531, 70–73 (2016); doi:10.1038/nature16976In this Letter, we omitted to cite preliminary results from the low-energy extension of the Pierre Auger Observatory, as presented at the International Cosmic Ray Conference 2015 (ref. 1). Figure 1

Description: A large light-mass component of cosmic rays at 1017–1017.5 electronvolts from radio observations Nature 531, 7592 (2016). doi:10.1038/nature16976 Authors: S. Buitink, A. Corstanje, H. Falcke, J. R. Hörandel, T. Huege, A. Nelles, J. P. Rachen, L. Rossetto, P. Schellart, O. Scholten, S. ter Veen, S. Thoudam, T. N. G. Trinh, J. Anderson, A. Asgekar, I. M. Avruch, M. E. Bell, M. J. Bentum, G. Bernardi, P. Best, A. Bonafede, F. Breitling, J. W. Broderick, W. N. Brouw, M. Brüggen, H. R. Butcher, D. Carbone, B. Ciardi, J. E. Conway, F. de Gasperin, E. de Geus, A. Deller, R.-J. Dettmar, G. van Diepen, S. Duscha, J. Eislöffel, D. Engels, J. E. Enriquez, R. A. Fallows, R. Fender, C. Ferrari, W. Frieswijk, M. A. Garrett, J. M. Grießmeier, A. W. Gunst, M. P. van Haarlem, T. E. Hassall, G. Heald, J. W. T. Hessels, M. Hoeft, A. Horneffer, M. Iacobelli, H. Intema, E. Juette, A. Karastergiou, V. I. Kondratiev, M. Kramer, M. Kuniyoshi, G. Kuper, J. van Leeuwen, G. M. Loose, P. Maat, G. Mann, S. Markoff, R. McFadden, D. McKay-Bukowski, J. P. McKean, M. Mevius, D. D. Mulcahy, H. Munk, M. J. Norden, E. Orru, H. Paas, M. Pandey-Pommier, V. N. Pandey, M. Pietka, R. Pizzo, A. G. Polatidis, W. Reich, H. J. A. Röttgering, A. M. M. Scaife, D. J. Schwarz, M. Serylak, J. Sluman, O. Smirnov, B. W. Stappers, M. Steinmetz, A. Stewart, J. Swinbank, M. Tagger, Y. Tang, C. Tasse, M. C. Toribio, R. Vermeulen, C. Vocks, C. Vogt, R. J. van Weeren, R. A. M. J. Wijers, S. J. Wijnholds, M. W. Wise, O. Wucknitz, S. Yatawatta, P. Zarka & J. A. Zensus Cosmic rays are the highest-energy particles found in nature. Measurements of the mass composition of cosmic rays with energies of 1017–1018 electronvolts are essential to understanding whether they have galactic or extragalactic sources. It has also been proposed that the astrophysical neutrino signal comes from accelerators capable of producing cosmic rays of these energies. Cosmic rays initiate air showers—cascades of secondary particles in the atmosphere—and their masses can be inferred from measurements of the atmospheric depth of the shower maximum (Xmax; the depth of the air shower when it contains the most particles) or of the composition of shower particles reaching the ground. Current measurements have either high uncertainty, or a low duty cycle and a high energy threshold. Radio detection of cosmic rays is a rapidly developing technique for determining Xmax (refs 10, 11) with a duty cycle of, in principle, nearly 100 per cent. The radiation is generated by the separation of relativistic electrons and positrons in the geomagnetic field and a negative charge excess in the shower front. Here we report radio measurements of Xmax with a mean uncertainty of 16 grams per square centimetre for air showers initiated by cosmic rays with energies of 1017–1017.5 electronvolts. This high resolution in Xmax enables us to determine the mass spectrum of the cosmic rays: we find a mixed composition, with a light-mass fraction (protons and helium nuclei) of about 80 per cent. Unless, contrary to current expectations, the extragalactic component of cosmic rays contributes substantially to the total flux below 1017.5 electronvolts, our measurements indicate the existence of an additional galactic component, to account for the light composition that we measured in the 1017–1017.5 electronvolt range.

Description: We have detected an x-ray nebula around the binary millisecond pulsar B1957+20. A narrow tail, corresponding to the shocked pulsar wind, is seen interior to the known Halpha bow shock and proves the long-held assumption that the rotational energy of millisecond pulsars is dissipated through relativistic winds. Unresolved x-ray emission likely represents the shock where the winds of the pulsar and its companion collide. This emission indicates that the efficiency with which relativistic particles are accelerated in the postshock flow is similar to that for young pulsars, despite the shock proximity and much weaker surface magnetic field of this millisecond pulsar.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Stappers, B W -- Gaensler, B M -- Kaspi, V M -- van der Klis, M -- Lewin, W H G -- New York, N.Y. -- Science. 2003 Feb 28;299(5611):1372-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Stichting ASTRON, 7990 Dwingeloo, Netherlands. stappers@astron.nl〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/12610299" target="_blank"〉PubMed〈/a〉

Description: Binary pulsar systems are superb probes of stellar and binary evolution and the physics of extreme environments. In a survey with the Arecibo telescope, we have found PSR J1903+0327, a radio pulsar with a rotational period of 2.15 milliseconds in a highly eccentric (e = 0.44) 95-day orbit around a solar mass (M(middle dot in circle)) companion. Infrared observations identify a possible main-sequence companion star. Conventional binary stellar evolution models predict neither large orbital eccentricities nor main-sequence companions around millisecond pulsars. Alternative formation scenarios involve recycling a neutron star in a globular cluster, then ejecting it into the Galactic disk, or membership in a hierarchical triple system. A relativistic analysis of timing observations of the pulsar finds its mass to be 1.74 +/- 0.04 M solar symbol, an unusually high value.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Champion, David J -- Ransom, Scott M -- Lazarus, Patrick -- Camilo, Fernando -- Bassa, Cees -- Kaspi, Victoria M -- Nice, David J -- Freire, Paulo C C -- Stairs, Ingrid H -- van Leeuwen, Joeri -- Stappers, Ben W -- Cordes, James M -- Hessels, Jason W T -- Lorimer, Duncan R -- Arzoumanian, Zaven -- Backer, Don C -- Bhat, N D Ramesh -- Chatterjee, Shami -- Cognard, Ismael -- Deneva, Julia S -- Faucher-Giguere, Claude-Andre -- Gaensler, Bryan M -- Han, Jinlin -- Jenet, Fredrick A -- Kasian, Laura -- Kondratiev, Vlad I -- Kramer, Michael -- Lazio, Joseph -- McLaughlin, Maura A -- Venkataraman, Arun -- Vlemmings, Wouter -- New York, N.Y. -- Science. 2008 Jun 6;320(5881):1309-12. doi: 10.1126/science.1157580. Epub 2008 May 15.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, McGill University, Montreal, QC H3A 2T8, Canada. David.Champion@atnf.csiro.au〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18483399" target="_blank"〉PubMed〈/a〉

Description: Pulsars are born with subsecond spin periods and slow by electromagnetic braking for several tens of millions of years, when detectable radiation ceases. A second life can occur for neutron stars in binary systems. They can acquire mass and angular momentum from their companions, to be spun up to millisecond periods and begin radiating again. We searched Fermi Large Area Telescope data for pulsations from all known millisecond pulsars (MSPs) outside of globular clusters, using rotation parameters from radio telescopes. Strong gamma-ray pulsations were detected for eight MSPs. The gamma-ray pulse profiles and spectral properties resemble those of young gamma-ray pulsars. The basic emission mechanism seems to be the same for MSPs and young pulsars, with the emission originating in regions far from the neutron star surface.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Abdo, A A -- Ackermann, M -- Ajello, M -- Atwood, W B -- Axelsson, M -- Baldini, L -- Ballet, J -- Barbiellini, G -- Baring, M G -- Bastieri, D -- Baughman, B M -- Bechtol, K -- Bellazzini, R -- Berenji, B -- Bignami, G F -- Blandford, R D -- Bloom, E D -- Bonamente, E -- Borgland, A W -- Bregeon, J -- Brez, A -- Brigida, M -- Bruel, P -- Burnett, T H -- Caliandro, G A -- Cameron, R A -- Camilo, F -- Caraveo, P A -- Carlson, P -- Casandjian, J M -- Cecchi, C -- Celik, O -- Charles, E -- Chekhtman, A -- Cheung, C C -- Chiang, J -- Ciprini, S -- Claus, R -- Cognard, I -- Cohen-Tanugi, J -- Cominsky, L R -- Conrad, J -- Corbet, R -- Cutini, S -- Dermer, C D -- Desvignes, G -- de Angelis, A -- de Luca, A -- de Palma, F -- Digel, S W -- Dormody, M -- do Couto e Silva, E -- Drell, P S -- Dubois, R -- Dumora, D -- Edmonds, Y -- Farnier, C -- Favuzzi, C -- Fegan, S J -- Focke, W B -- Frailis, M -- Freire, P C C -- Fukazawa, Y -- Funk, S -- Fusco, P -- Gargano, F -- Gasparrini, D -- Gehrels, N -- Germani, S -- 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 -- Hobbs, G -- Hughes, R E -- Johannesson, G -- Johnson, A S -- Johnson, R P -- Johnson, T J -- Johnson, W N -- Johnston, S -- Kamae, T -- Katagiri, H -- Kataoka, 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 -- Madejski, G M -- Makeev, A -- Manchester, R N -- Marelli, M -- Mazziotta, M N -- McConville, W -- McEnery, J E -- McLaughlin, M A -- Meurer, C -- Michelson, P F -- Mitthumsiri, W -- Mizuno, T -- Moiseev, A A -- Monte, C -- Monzani, M E -- Morselli, A -- Moskalenko, I V -- Murgia, S -- Nolan, P L -- Norris, J P -- Nuss, E -- Ohsugi, T -- Omodei, N -- Orlando, E -- Ormes, J F -- Paneque, D -- Panetta, J H -- Parent, D -- Pelassa, V -- Pepe, M -- Pesce-Rollins, M -- Piron, F -- Porter, T A -- Raino, S -- Rando, R -- Ransom, S M -- Ray, P S -- Razzano, M -- Rea, N -- Reimer, A -- Reimer, O -- Reposeur, T -- Ritz, S -- 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 -- Schalk, T L -- Sgro, C -- Siskind, E J -- Smith, D A -- Smith, P D -- Spandre, G -- Spinelli, P -- Stappers, B W -- Starck, J L -- Striani, E -- Strickman, M S -- Suson, D J -- Tajima, H -- Takahashi, H -- Tanaka, T -- Thayer, J B -- Thayer, J G -- Theureau, G -- Thompson, D J -- Thorsett, S E -- Tibaldo, L -- Torres, D F -- Tosti, G -- Tramacere, A -- Uchiyama, Y -- Usher, T L -- Van Etten, A -- Vasileiou, V -- Venter, C -- Vilchez, N -- Vitale, V -- Waite, A P -- Wallace, E -- Wang, P -- Watters, K -- Webb, N -- Weltevrede, P -- Winer, B L -- Wood, K S -- Ylinen, T -- Ziegler, M -- New York, N.Y. -- Science. 2009 Aug 14;325(5942):848-52. doi: 10.1126/science.1176113.〈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/19574349" target="_blank"〉PubMed〈/a〉

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: Einstein@Home aggregates the computer power of hundreds of thousands of volunteers from 192 countries to mine large data sets. It has now found a 40.8-hertz isolated pulsar in radio survey data from the Arecibo Observatory taken in February 2007. Additional timing observations indicate that this pulsar is likely a disrupted recycled pulsar. PSR J2007+2722's pulse profile is remarkably wide with emission over almost the entire spin period; the pulsar likely has closely aligned magnetic and spin axes. The massive computing power provided by volunteers should enable many more such discoveries.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Knispel, B -- Allen, B -- Cordes, J M -- Deneva, J S -- Anderson, D -- Aulbert, C -- Bhat, N D R -- Bock, O -- Bogdanov, S -- Brazier, A -- Camilo, F -- Champion, D J -- Chatterjee, S -- Crawford, F -- Demorest, P B -- Fehrmann, H -- Freire, P C C -- Gonzalez, M E -- Hammer, D -- Hessels, J W T -- Jenet, F A -- Kasian, L -- Kaspi, V M -- Kramer, M -- Lazarus, P -- van Leeuwen, J -- Lorimer, D R -- Lyne, A G -- Machenschalk, B -- McLaughlin, M A -- Messenger, C -- Nice, D J -- Papa, M A -- Pletsch, H J -- Prix, R -- Ransom, S M -- Siemens, X -- Stairs, I H -- Stappers, B W -- Stovall, K -- Venkataraman, A -- New York, N.Y. -- Science. 2010 Sep 10;329(5997):1305. doi: 10.1126/science.1195253. Epub 2010 Aug 12.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik, D-30167 Hannover, Germany. benjamin.knispel@aei.mpg.de〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20705813" 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: A repeating fast radio burst Nature 531, 7593 (2016). doi:10.1038/nature17168 Authors: L. G. Spitler, P. Scholz, J. W. T. Hessels, S. Bogdanov, A. Brazier, F. Camilo, S. Chatterjee, J. M. Cordes, F. Crawford, J. Deneva, R. D. Ferdman, P. C. C. Freire, V. M. Kaspi, P. Lazarus, R. Lynch, E. C. Madsen, M. A. McLaughlin, C. Patel, S. M. Ransom, A. Seymour, I. H. Stairs, B. W. Stappers, J. van Leeuwen & W. W. Zhu Fast radio bursts are millisecond-duration astronomical radio pulses of unknown physical origin that appear to come from extragalactic distances. Previous follow-up observations have failed to find additional bursts at the same dispersion measure (that is, the integrated column density of free electrons between source and telescope) and sky position as the original detections. The apparent non-repeating nature of these bursts has led to the suggestion that they originate in cataclysmic events. Here we report observations of ten additional bursts from the direction of the fast radio burst FRB 121102. These bursts have dispersion measures and sky positions consistent with the original burst. This unambiguously identifies FRB 121102 as repeating and demonstrates that its source survives the energetic events that cause the bursts. Additionally, the bursts from FRB 121102 show a wide range of spectral shapes that appear to be predominantly intrinsic to the source and which vary on timescales of minutes or less. Although there may be multiple physical origins for the population of fast radio bursts, these repeat bursts with high dispersion measure and variable spectra specifically seen from the direction of FRB 121102 support an origin in a young, highly magnetized, extragalactic neutron star.

Description: In recent years, millisecond-duration radio signals originating in distant galaxies appear to have been discovered in the so-called fast radio bursts. These signals are dispersed according to a precise physical law and this dispersion is a key observable quantity, which, in tandem with a redshift measurement, can be used for fundamental physical investigations. Every fast radio burst has a dispersion measurement, but none before now have had a redshift measurement, because of the difficulty in pinpointing their celestial coordinates. Here we report the discovery of a fast radio burst and the identification of a fading radio transient lasting ~6 days after the event, which we use to identify the host galaxy; we measure the galaxy's redshift to be z = 0.492 +/- 0.008. The dispersion measure and redshift, in combination, provide a direct measurement of the cosmic density of ionized baryons in the intergalactic medium of OmegaIGM = 4.9 +/- 1.3 per cent, in agreement with the expectation from the Wilkinson Microwave Anisotropy Probe, and including all of the so-called 'missing baryons'. The ~6-day radio transient is largely consistent with the radio afterglow of a short gamma-ray burst, and its existence and timescale do not support progenitor models such as giant pulses from pulsars, and supernovae. This contrasts with the interpretation of another recently discovered fast radio burst, suggesting that there are at least two classes of bursts.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Keane, E F -- Johnston, S -- Bhandari, S -- Barr, E -- Bhat, N D R -- Burgay, M -- Caleb, M -- Flynn, C -- Jameson, A -- Kramer, M -- Petroff, E -- Possenti, A -- van Straten, W -- Bailes, M -- Burke-Spolaor, S -- Eatough, R P -- Stappers, B W -- Totani, T -- Honma, M -- Furusawa, H -- Hattori, T -- Morokuma, T -- Niino, Y -- Sugai, H -- Terai, T -- Tominaga, N -- Yamasaki, S -- Yasuda, N -- Allen, R -- Cooke, J -- Jencson, J -- Kasliwal, M M -- Kaplan, D L -- Tingay, S J -- Williams, A -- Wayth, R -- Chandra, P -- Perrodin, D -- Berezina, M -- Mickaliger, M -- Bassa, C -- England -- Nature. 2016 Feb 25;530(7591):453-6. doi: 10.1038/nature17140.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Square Kilometre Array Organisation, Jodrell Bank Observatory, SK11 9DL, UK. ; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Mail H29, PO Box 218, Victoria 3122, Australia. ; Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia. ; Commonwealth Science and Industrial Research Organisation (CSIRO), Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, New South Wales 1710, Australia. ; International Centre for Radio Astronomy Research, Curtin University, Bentley, Western Australia 6102, Australia. ; Instituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Cagliari, Via della Scienza 5, I-09047 Selargius (CA), Italy. ; Research School of Astronomy and Astrophysics, Australian National University, Canberra, Australian Capital Territory 2611, Australia. ; Max-Planck-Institut fur Radioastronomie (MPIfR), Auf dem Hugel 69, D-53121 Bonn, Germany. ; Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK. ; National Radio Astronomy Observatory, Socorro, New Mexico, USA. ; Department of Astronomy, the University of Tokyo, Hongo, Tokyo 113-0033, Japan. ; National Astronomical Observatory of Japan, 2 Chome-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan. ; Department of Astronomical Science, SOKENDAI (Graduate University for the Advanced Study), Osawa, Mitaka 181-8588, Japan. ; Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, Hawaii 96720, USA. ; Institute of Astronomy, Graduate School of Science, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan. ; Kavli Institute for the Physics and Mathematics of the Universe (WPI), Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan. ; Department of Physics, Faculty of Science and Engineering, Konan University, 8-9-1 Okamoto, Kobe, Hyogo 658-8501, Japan. ; Cahill Center for Astrophysics, California Institute of Technology, 1200 East California Boulevard, Pasadena, California 91125, USA. ; Department of Physics, University of Wisconsin-Milwaukee, Milwaukee, Wisconsin 53201, USA. ; National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus, Ganeshkhind, Pune 411 007, India. ; ASTRON, the Netherlands Institute for Radio Astronomy, Postbus 2, NL-7990 AA Dwingeloo, The Netherlands.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26911781" target="_blank"〉PubMed〈/a〉