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  • 1
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    Detection of the gravitational lens magnifying a type Ia supernova (2014)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2014-04-26
    Description: Objects of known brightness, like type Ia supernovae (SNIa), can be used to measure distances. If a massive object warps spacetime to form multiple images of a background SNIa, a direct test of cosmic expansion is also possible. However, these lensing events must first be distinguished from other rare phenomena. Recently, a supernova was found to shine much brighter than normal for its distance, which resulted in a debate: Was it a new type of superluminous supernova or a normal SNIa magnified by a hidden gravitational lens? Here, we report that a spectrum obtained after the supernova faded away shows the presence of a foreground galaxy-the first found to strongly magnify a SNIa. We discuss how more lensed SNIa can be found than previously predicted.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Quimby, Robert M -- Oguri, Masamune -- More, Anupreeta -- More, Surhud -- Moriya, Takashi J -- Werner, Marcus C -- Tanaka, Masayuki -- Folatelli, Gaston -- Bersten, Melina C -- Maeda, Keiichi -- Nomoto, Ken'ichi -- New York, N.Y. -- Science. 2014 Apr 25;344(6182):396-9. doi: 10.1126/science.1250903.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Kavli Institute for the Physics and Mathematics of the Universe (WPI), Todai Institutes for Advanced Study, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa-shi, Chiba 277-8583, Japan.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24763586" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 2
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    Hydrogen-poor superluminous stellar explosions (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-06-10
    Description: Supernovae are stellar explosions driven by gravitational or thermonuclear energy that is observed as electromagnetic radiation emitted over weeks or more. In all known supernovae, this radiation comes from internal energy deposited in the outflowing ejecta by one or more of the following processes: radioactive decay of freshly synthesized elements (typically (56)Ni), the explosion shock in the envelope of a supergiant star, and interaction between the debris and slowly moving, hydrogen-rich circumstellar material. Here we report observations of a class of luminous supernovae whose properties cannot be explained by any of these processes. The class includes four new supernovae that we have discovered and two previously unexplained events (SN 2005ap and SCP 06F6) that we can now identify as members of the same class. These supernovae are all about ten times brighter than most type Ia supernova, do not show any trace of hydrogen, emit significant ultraviolet flux for extended periods of time and have late-time decay rates that are inconsistent with radioactivity. Our data require that the observed radiation be emitted by hydrogen-free material distributed over a large radius ( approximately 10(15) centimetres) and expanding at high speeds (〉10(4) kilometres per second). These long-lived, ultraviolet-luminous events can be observed out to redshifts z 〉 4.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Quimby, R M -- Kulkarni, S R -- Kasliwal, M M -- Gal-Yam, A -- Arcavi, I -- Sullivan, M -- Nugent, P -- Thomas, R -- Howell, D A -- Nakar, E -- Bildsten, L -- Theissen, C -- Law, N M -- Dekany, R -- Rahmer, G -- Hale, D -- Smith, R -- Ofek, E O -- Zolkower, J -- Velur, V -- Walters, R -- Henning, J -- Bui, K -- McKenna, D -- Poznanski, D -- Cenko, S B -- Levitan, D -- England -- Nature. 2011 Jun 8;474(7352):487-9. doi: 10.1038/nature10095.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Cahill Center for Astrophysics 249-17, California Institute of Technology, Pasadena, California 91125, USA. quimby@astro.caltech.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21654747" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 3
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    Exclusion of a luminous red giant as a companion star to the progenitor of supernova SN 2011fe (2011)
    Nature Publishing Group (NPG)
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    Publication Date: 2011-12-16
    Description: Type Ia supernovae are thought to result from a thermonuclear explosion of an accreting white dwarf in a binary system, but little is known of the precise nature of the companion star and the physical properties of the progenitor system. There are two classes of models: double-degenerate (involving two white dwarfs in a close binary system) and single-degenerate models. In the latter, the primary white dwarf accretes material from a secondary companion until conditions are such that carbon ignites, at a mass of 1.38 times the mass of the Sun. The type Ia supernova SN 2011fe was recently detected in a nearby galaxy. Here we report an analysis of archival images of the location of SN 2011fe. The luminosity of the progenitor system (especially the companion star) is 10-100 times fainter than previous limits on other type Ia supernova progenitor systems, allowing us to rule out luminous red giants and almost all helium stars as the mass-donating companion to the exploding white dwarf.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Li, Weidong -- Bloom, Joshua S -- Podsiadlowski, Philipp -- Miller, Adam A -- Cenko, S Bradley -- Jha, Saurabh W -- Sullivan, Mark -- Howell, D Andrew -- Nugent, Peter E -- Butler, Nathaniel R -- Ofek, Eran O -- Kasliwal, Mansi M -- Richards, Joseph W -- Stockton, Alan -- Shih, Hsin-Yi -- Bildsten, Lars -- Shara, Michael M -- Bibby, Joanne -- Filippenko, Alexei V -- Ganeshalingam, Mohan -- Silverman, Jeffrey M -- Kulkarni, S R -- Law, Nicholas M -- Poznanski, Dovi -- Quimby, Robert M -- McCully, Curtis -- Patel, Brandon -- Maguire, Kate -- Shen, Ken J -- England -- Nature. 2011 Dec 14;480(7377):348-50. doi: 10.1038/nature10646.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of California, Berkeley, California 94720-3411, USA. weidong@berkeley.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22170681" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 4
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    Supernova SN 2011fe from an exploding carbon-oxygen white dwarf star (2011)
    Nature Publishing Group (NPG)
    Details
    Publication Date: 2011-12-16
    Description: Type Ia supernovae have been used empirically as 'standard candles' to demonstrate the acceleration of the expansion of the Universe even though fundamental details, such as the nature of their progenitor systems and how the stars explode, remain a mystery. There is consensus that a white dwarf star explodes after accreting matter in a binary system, but the secondary body could be anything from a main-sequence star to a red giant, or even another white dwarf. This uncertainty stems from the fact that no recent type Ia supernova has been discovered close enough to Earth to detect the stars before explosion. Here we report early observations of supernova SN 2011fe in the galaxy M101 at a distance from Earth of 6.4 megaparsecs. We find that the exploding star was probably a carbon-oxygen white dwarf, and from the lack of an early shock we conclude that the companion was probably a main-sequence star. Early spectroscopy shows high-velocity oxygen that slows rapidly, on a timescale of hours, and extensive mixing of newly synthesized intermediate-mass elements in the outermost layers of the supernova. A companion paper uses pre-explosion images to rule out luminous red giants and most helium stars as companions to the progenitor.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Nugent, Peter E -- Sullivan, Mark -- Cenko, S Bradley -- Thomas, Rollin C -- Kasen, Daniel -- Howell, D Andrew -- Bersier, David -- Bloom, Joshua S -- Kulkarni, S R -- Kandrashoff, Michael T -- Filippenko, Alexei V -- Silverman, Jeffrey M -- Marcy, Geoffrey W -- Howard, Andrew W -- Isaacson, Howard T -- Maguire, Kate -- Suzuki, Nao -- Tarlton, James E -- Pan, Yen-Chen -- Bildsten, Lars -- Fulton, Benjamin J -- Parrent, Jerod T -- Sand, David -- Podsiadlowski, Philipp -- Bianco, Federica B -- Dilday, Benjamin -- Graham, Melissa L -- Lyman, Joe -- James, Phil -- Kasliwal, Mansi M -- Law, Nicholas M -- Quimby, Robert M -- Hook, Isobel M -- Walker, Emma S -- Mazzali, Paolo -- Pian, Elena -- Ofek, Eran O -- Gal-Yam, Avishay -- Poznanski, Dovi -- England -- Nature. 2011 Dec 14;480(7377):344-7. doi: 10.1038/nature10644.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA. penugent@lbl.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22170680" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0028-0836
    Electronic ISSN: 1476-4687
    Topics: Biology , Chemistry and Pharmacology , Medicine , Natural Sciences in General , Physics
    Published by Nature Publishing Group (NPG)
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  • 5
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    Circumstellar material in type Ia supernovae via sodium absorption features (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-08-13
    Description: Type Ia supernovae are key tools for measuring distances on a cosmic scale. They are generally thought to be the thermonuclear explosion of an accreting white dwarf in a close binary system. The nature of the mass donor is still uncertain. In the single-degenerate model it is a main-sequence star or an evolved star, whereas in the double-degenerate model it is another white dwarf. We show that the velocity structure of absorbing material along the line of sight to 35 type Ia supernovae tends to be blueshifted. These structures are likely signatures of gas outflows from the supernova progenitor systems. Thus, many type Ia supernovae in nearby spiral galaxies may originate in single-degenerate systems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Sternberg, A -- Gal-Yam, A -- Simon, J D -- Leonard, D C -- Quimby, R M -- Phillips, M M -- Morrell, N -- Thompson, I B -- Ivans, I -- Marshall, J L -- Filippenko, A V -- Marcy, G W -- Bloom, J S -- Patat, F -- Foley, R J -- Yong, D -- Penprase, B E -- Beeler, D J -- Allende Prieto, C -- Stringfellow, G S -- New York, N.Y. -- Science. 2011 Aug 12;333(6044):856-9. doi: 10.1126/science.1203836.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Benoziyo Center for Astrophysics, Faculty of Physics, Weizmann Institute of Science, Rehovot 76100, Israel. assaf.sternberg@weizmann.ac.il〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21836010" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 6
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    PTF 11kx: a type Ia supernova with a symbiotic nova progenitor (2012)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2012-08-28
    Description: There is a consensus that type Ia supernovae (SNe Ia) arise from the thermonuclear explosion of white dwarf stars that accrete matter from a binary companion. However, direct observation of SN Ia progenitors is lacking, and the precise nature of the binary companion remains uncertain. A temporal series of high-resolution optical spectra of the SN Ia PTF 11kx reveals a complex circumstellar environment that provides an unprecedentedly detailed view of the progenitor system. Multiple shells of circumstellar material are detected, and the SN ejecta are seen to interact with circumstellar material starting 59 days after the explosion. These features are best described by a symbiotic nova progenitor, similar to RS Ophiuchi.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Dilday, B -- Howell, D A -- Cenko, S B -- Silverman, J M -- Nugent, P E -- Sullivan, M -- Ben-Ami, S -- Bildsten, L -- Bolte, M -- Endl, M -- Filippenko, A V -- Gnat, O -- Horesh, A -- Hsiao, E -- Kasliwal, M M -- Kirkman, D -- Maguire, K -- Marcy, G W -- Moore, K -- Pan, Y -- Parrent, J T -- Podsiadlowski, P -- Quimby, R M -- Sternberg, A -- Suzuki, N -- Tytler, D R -- Xu, D -- Bloom, J S -- Gal-Yam, A -- Hook, I M -- Kulkarni, S R -- Law, N M -- Ofek, E O -- Polishook, D -- Poznanski, D -- New York, N.Y. -- Science. 2012 Aug 24;337(6097):942-5. doi: 10.1126/science.1219164.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Goleta, CA 93117, USA. bdilday@lcogt.net〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22923575" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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  • 7
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    An extremely luminous panchromatic outburst from the nucleus of a distant galaxy (2011)
    American Association for the Advancement of Science (AAAS)
    Details
    Publication Date: 2011-06-18
    Description: Variable x-ray and gamma-ray emission is characteristic of the most extreme physical processes in the universe. We present multiwavelength observations of a unique gamma-ray-selected transient detected by the Swift satellite, accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z = 0.3534. Its high-energy emission has lasted much longer than any gamma-ray burst, whereas its peak luminosity was approximately 100 times higher than bright active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a rare mechanism involving the massive black hole in the nucleus of that galaxy.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Levan, A J -- Tanvir, N R -- Cenko, S B -- Perley, D A -- Wiersema, K -- Bloom, J S -- Fruchter, A S -- Postigo, A de Ugarte -- O'Brien, P T -- Butler, N -- van der Horst, A J -- Leloudas, G -- Morgan, A N -- Misra, K -- Bower, G C -- Farihi, J -- Tunnicliffe, R L -- Modjaz, M -- Silverman, J M -- Hjorth, J -- Thone, C -- Cucchiara, A -- Ceron, J M Castro -- Castro-Tirado, A J -- Arnold, J A -- Bremer, M -- Brodie, J P -- Carroll, T -- Cooper, M C -- Curran, P A -- Cutri, R M -- Ehle, J -- Forbes, D -- Fynbo, J -- Gorosabel, J -- Graham, J -- Hoffman, D I -- Guziy, S -- Jakobsson, P -- Kamble, A -- Kerr, T -- Kasliwal, M M -- Kouveliotou, C -- Kocevski, D -- Law, N M -- Nugent, P E -- Ofek, E O -- Poznanski, D -- Quimby, R M -- Rol, E -- Romanowsky, A J -- Sanchez-Ramirez, R -- Schulze, S -- Singh, N -- van Spaandonk, L -- Starling, R L C -- Strom, R G -- Tello, J C -- Vaduvescu, O -- Wheatley, P J -- Wijers, R A M J -- Winters, J M -- Xu, D -- New York, N.Y. -- Science. 2011 Jul 8;333(6039):199-202. doi: 10.1126/science.1207143. Epub 2011 Jun 16.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, University of Warwick, Coventry, UK. a.j.levan@warwick.ac.uk〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/21680811" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
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  • 8
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    Structure of 5-hydroxymethylcytosine-specific restriction enzyme, AbaSI, in complex with DNA (2014)
    Oxford University Press
    Details
    Publication Date: 2014-07-04
    Description: AbaSI, a member of the PvuRts1I-family of modification-dependent restriction endonucleases, cleaves deoxyribonucleic acid (DNA) containing 5-hydroxymethylctosine (5hmC) and glucosylated 5hmC (g5hmC), but not DNA containing unmodified cytosine. AbaSI has been used as a tool for mapping the genomic locations of 5hmC, an important epigenetic modification in the DNA of higher organisms. Here we report the crystal structures of AbaSI in the presence and absence of DNA. These structures provide considerable, although incomplete, insight into how this enzyme acts. AbaSI appears to be mainly a homodimer in solution, but interacts with DNA in our structures as a homotetramer. Each AbaSI subunit comprises an N-terminal, Vsr-like, cleavage domain containing a single catalytic site, and a C-terminal, SRA-like, 5hmC-binding domain. Two N-terminal helices mediate most of the homodimer interface. Dimerization brings together the two catalytic sites required for double-strand cleavage, and separates the 5hmC binding-domains by ~70 Å, consistent with the known activity of AbaSI which cleaves DNA optimally between symmetrically modified cytosines ~22 bp apart. The eukaryotic SET and RING-associated (SRA) domains bind to DNA containing 5-methylcytosine (5mC) in the hemi-methylated CpG sequence. They make contacts in both the major and minor DNA grooves, and flip the modified cytosine out of the helix into a conserved binding pocket. In contrast, the SRA-like domain of AbaSI, which has no sequence specificity, contacts only the minor DNA groove, and in our current structures the 5hmC remains intra-helical. A conserved, binding pocket is nevertheless present in this domain, suitable for accommodating 5hmC and g5hmC. We consider it likely, therefore, that base-flipping is part of the recognition and cleavage mechanism of AbaSI, but that our structures represent an earlier, pre-flipped stage, prior to actual recognition.
    Print ISSN: 0305-1048
    Electronic ISSN: 1362-4962
    Topics: Biology
    Published by Oxford University Press
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  • 9
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    Rates of superluminous supernovae at z ~ 0.2 (2013)
    Oxford University Press
    Details
    Publication Date: 2013-04-03
    Description: We calculate the volumetric rate of superluminous supernovae (SLSNe) based on five events discovered with the Robotic Optical Transient Search Experiment-IIIb (ROTSE-IIIb) telescope. We gather light curves of 19 events from the literature and our own unpublished data and employ crude k -corrections to constrain the pseudo-absolute magnitude distributions in the rest-frame ROTSE-IIIb (unfiltered) bandpass for both the hydrogen-poor (SLSN-I) and hydrogen-rich (SLSN-II) populations. We find that the peak magnitudes of the available SLSN-I are narrowly distributed ( M  = –21.7 ± 0.4) in our unfiltered band pass and may suggest an even tighter intrinsic distribution when the effects of dust are considered, although the sample may be skewed by selection and publication biases. The presence of O ii features near maximum light may uniquely signal a high-luminosity event, and we suggest further observational and theoretical work is warranted to assess the possible utility of such SN 2005ap-like SLSN-I as distance indicators. Using the pseudo-absolute magnitude distributions derived from the light-curve sample, we measure the SLSN-I rate to be about (32 $ {^{+ 77}_{-26}} $ ) events Gpc –3 yr –1 h 3 71 at a weighted redshift of $\overline{z} = 0.17$ , and the SLSN-II rate to be about (151 $ {^{+ 151}_{-82}} $ ) events Gpc –3 yr –1 h 3 71 at $\overline{z} = 0.15$ . Given that the exact nature and limits of these populations are still unknown, we discuss how it may be difficult to distinguish these rare SLSNe from other transient phenomena such as active galactic nucleus activity and tidal disruption events even when multiband photometry, spectroscopy or even high-resolution imaging are available. Including one spectroscopically peculiar event, we determine a total rate for SLSN-like events of (199 $ {^{+ 137}_{-86}} $ ) events Gpc –3 yr –1 h 3 71 at $\overline{z} = 0.16$ .
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    Illuminating gravitational waves: A concordant picture of photons from a neutron star merger (2017)
    Kasliwal, M. M., Nakar, E., Singer, L. P., Kaplan, D. L., Cook, D. O., Van Sistine, A., Lau, R. M., Fremling, C., Gottlieb, O., Jencson, J. E., Adams, S. M., Feindt, U., Hotokezaka, K., Ghosh, S., Perley, D. A., Yu, P.- C., Piran, T., Allison, J. R., Anupama, G. C., Balasubramanian, A., Bannister, K. W., Bally, J., Barnes, J., Barway, S., Bellm, E., Bhalerao, V., Bhattacharya, D., Blagorodnova, N., Bloom, J. S., Brady, P. R., Cannella, C., Chatterjee, D., Cenko, S. B., Cobb, B. E., Copperwheat, C., Corsi, A., De, K., Dobie, D., Emery, S. W. K., Evans, P. A., Fox, O. D., Frail, D. A., Frohmaier, C., Goobar, A., Hallinan, G., Harrison, F., Helou, G., Hinderer, T., Ho, A. Y. Q., Horesh, A., Ip, W.- H., Itoh, R., Kasen, D., Kim, H., Kuin, N. P. M., Kupfer, T., Lynch, C., Madsen, K., Mazzali, P. A., Miller, A. A., Mooley, K., Murphy, T., Ngeow, C.- C., Nichols, D., Nissanke, S., Nugent, P., Ofek, E. O., Qi, H., Quimby, R. M., Rosswog, S., Rusu, F., Sadler, E. M., Schmidt, P., Sollerman, J., Steele, I., Williamson, A. R., Xu, Y., Yan, L., Yatsu, Y., Zhang, C., Zhao, W.
    American Association for the Advancement of Science (AAAS)
    In: Science
    Details
    Publication Date: 2017-12-22
    Description: Merging neutron stars offer an excellent laboratory for simultaneously studying strong-field gravity and matter in extreme environments. We establish the physical association of an electromagnetic counterpart (EM170817) with gravitational waves (GW170817) detected from merging neutron stars. By synthesizing a panchromatic data set, we demonstrate that merging neutron stars are a long-sought production site forging heavy elements by r-process nucleosynthesis. The weak gamma rays seen in EM170817 are dissimilar to classical short gamma-ray bursts with ultrarelativistic jets. Instead, we suggest that breakout of a wide-angle, mildly relativistic cocoon engulfing the jet explains the low-luminosity gamma rays, the high-luminosity ultraviolet-optical-infrared, and the delayed radio and x-ray emission. We posit that all neutron star mergers may lead to a wide-angle cocoon breakout, sometimes accompanied by a successful jet and sometimes by a choked jet.
    Keywords: Astronomy, Physics
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Geosciences , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science (AAAS)
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