ALBERT

Description: Long gamma-ray bursts (GRBs) are the most dramatic examples of massive stellar deaths, often associated with supernovae. They release ultra-relativistic jets, which produce non-thermal emission through synchrotron radiation as they interact with the surrounding medium. Here we report observations of the unusual GRB 101225A. Its gamma-ray emission was exceptionally long-lived and was followed by a bright X-ray transient with a hot thermal component and an unusual optical counterpart. During the first 10 days, the optical emission evolved as an expanding, cooling black body, after which an additional component, consistent with a faint supernova, emerged. We estimate its redshift to be z = 0.33 by fitting the spectral-energy distribution and light curve of the optical emission with a GRB-supernova template. Deep optical observations may have revealed a faint, unresolved host galaxy. Our proposed progenitor is a merger of a helium star with a neutron star that underwent a common envelope phase, expelling its hydrogen envelope. The resulting explosion created a GRB-like jet which became thermalized by interacting with the dense, previously ejected material, thus creating the observed black body, until finally the emission from the supernova dominated. An alternative explanation is a minor body falling onto a neutron star in the Galaxy.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Thone, C C -- de Ugarte Postigo, A -- Fryer, C L -- Page, K L -- Gorosabel, J -- Aloy, M A -- Perley, D A -- Kouveliotou, C -- Janka, H T -- Mimica, P -- Racusin, J L -- Krimm, H -- Cummings, J -- Oates, S R -- Holland, S T -- Siegel, M H -- De Pasquale, M -- Sonbas, E -- Im, M -- Park, W-K -- Kann, D A -- Guziy, S -- Garcia, L Hernandez -- Llorente, A -- Bundy, K -- Choi, C -- Jeong, H -- Korhonen, H -- Kubanek, P -- Lim, J -- Moskvitin, A -- Munoz-Darias, T -- Pak, S -- Parrish, I -- England -- Nature. 2011 Nov 30;480(7375):72-4. doi: 10.1038/nature10611.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉IAA - CSIC, Glorieta de la Astronomia s/n, 18008 Granada, Spain. cthoene@iaa.es〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22129726" target="_blank"〉PubMed〈/a〉

Description: Quiescent galaxies with little or no ongoing star formation dominate the population of galaxies with masses above 2 x 10(10) times that of the Sun; the number of quiescent galaxies has increased by a factor of about 25 over the past ten billion years (refs 1-4). Once star formation has been shut down, perhaps during the quasar phase of rapid accretion onto a supermassive black hole, an unknown mechanism must remove or heat the gas that is subsequently accreted from either stellar mass loss or mergers and that would otherwise cool to form stars. Energy output from a black hole accreting at a low rate has been proposed, but observational evidence for this in the form of expanding hot gas shells is indirect and limited to radio galaxies at the centres of clusters, which are too rare to explain the vast majority of the quiescent population. Here we report bisymmetric emission features co-aligned with strong ionized-gas velocity gradients from which we infer the presence of centrally driven winds in typical quiescent galaxies that host low-luminosity active nuclei. These galaxies are surprisingly common, accounting for as much as ten per cent of the quiescent population with masses around 2 x 10(10) times that of the Sun. In a prototypical example, we calculate that the energy input from the galaxy's low-level active supermassive black hole is capable of driving the observed wind, which contains sufficient mechanical energy to heat ambient, cooler gas (also detected) and thereby suppress star formation.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Cheung, Edmond -- Bundy, Kevin -- Cappellari, Michele -- Peirani, Sebastien -- Rujopakarn, Wiphu -- Westfall, Kyle -- Yan, Renbin -- Bershady, Matthew -- Greene, Jenny E -- Heckman, Timothy M -- Drory, Niv -- Law, David R -- Masters, Karen L -- Thomas, Daniel -- Wake, David A -- Weijmans, Anne-Marie -- Rubin, Kate -- Belfiore, Francesco -- Vulcani, Benedetta -- Chen, Yan-mei -- Zhang, Kai -- Gelfand, Joseph D -- Bizyaev, Dmitry -- Roman-Lopes, A -- Schneider, Donald P -- England -- Nature. 2016 May 25;533(7604):504-8. doi: 10.1038/nature18006.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Kavli Institute for the Physics and Mathematics of the Universe (World Premier International Research Center Initiative), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan. ; Sub-department of Astrophysics, Department of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, UK. ; Institut d'Astrophysique de Paris (UMR 7095, CNRS and UPMC), 98 bis Boulevard Arago, F-75014 Paris, France. ; Department of Physics, Faculty of Science, Chulalongkorn University, 254 Phayathai Road, Pathumwan, Bangkok 10330, Thailand. ; Institute for Cosmology and Gravitation, University of Portsmouth, Dennis Sciama Building, Burnaby Road, Portsmouth PO1 3FX, UK. ; Department of Physics and Astronomy, University of Kentucky, 505 Rose Street, Lexington, Kentucky 40506-0055, USA. ; Department of Astronomy, University of Wisconsin-Madison, 475 North Charter Street, Madison, Wisconsin 53706, USA. ; Department of Astrophysical Sciences, Princeton University, Princeton, New Jersey 08544, USA. ; Center for Astrophysical Sciences, Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, Maryland 21218, USA. ; McDonald Observatory, Department of Astronomy, University of Texas at Austin, 1 University Station, Austin, Texas 78712-0259, USA. ; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218, USA. ; Department of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK. ; School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews, Fife KY16 9SS, UK. ; Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA. ; Cavendish Laboratory, University of Cambridge, 19 J. J. Thomson Avenue, Cambridge CB3 0HE, UK. ; Kavli Institute for Cosmology, University of Cambridge, Cambridge CB3 0HE, UK. ; Department of Astronomy, Nanjing University, Nanjing 210093, China. ; New York University Abu Dhabi, PO Box 129188, Abu Dhabi, United Arab Emirates. ; Center for Cosmology and Particle Physics, New York University, Meyer Hall of Physics, 4 Washington Place, New York, New York 10003, USA. ; Apache Point Observatory and New Mexico State University, PO Box 59, Sunspot, New Mexico 88349-0059, USA. ; Sternberg Astronomical Institute, Moscow State University, Moscow, Russia. ; Departamento de Fisica y Astronomia, Facultad de Ciencias, Universidad de La Serena, Cisternas 1200, La Serena, Chile. ; Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, Pennsylvania 16802, USA. ; Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, Pennsylvania 16802, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/27225122" target="_blank"〉PubMed〈/a〉