137 results on '"PIAN, Elena"'
Search Results
2. INTEGRAL view of AGN
- Author
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Malizia, Angela, Sazonov, Sergey, Bassani, Loredana, Pian, Elena, Beckmann, Volker, Molina, Manuela, Mereminskiy, Ilya, and Belanger, Guillaume
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- 2020
- Full Text
- View/download PDF
3. Identification of strontium in the merger of two neutron stars
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Watson, Darach, Hansen, Camilla J., Selsing, Jonatan, Koch, Andreas, Malesani, Daniele B., Andersen, Anja C., Fynbo, Johan P. U., Arcones, Almudena, Bauswein, Andreas, Covino, Stefano, Grado, Aniello, Heintz, Kasper E., Hunt, Leslie, Kouveliotou, Chryssa, Leloudas, Giorgos, Levan, Andrew J., Mazzali, Paolo, and Pian, Elena
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- 2019
- Full Text
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4. An Asymmetric Energetic Type Ic Supernova Viewed Off-Axis, and a Link to Gamma Ray Bursts
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Mazzali, Paolo A., Kawabata, Koji S., Maeda, Keiichi, Nomoto, Ken'ichi, Filippenko, Alexei V., Ramirez-Ruiz, Enrico, Benetti, Stefano, Pian, Elena, Deng, Jinsong, Tominaga, Nozomu, Ohyama, Youichi, Iye, Masanori, Foley, Ryan J., Matheson, Thomas, Wang, Lifan, and Gal-Yam, Avishay
- Published
- 2005
5. Decay of the GRB 990123 Optical Afterglow: Implications for the Fireball Model
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Castro-Tirado, Alberto J., Zapatero-Osorio, María Rosa, Caon, Nicola, Cairós, Luz Marina, Hjorth, Jens, Pedersen, Holger, Andersen, Michael I., Gorosabel, Javier, Bartolini, Corrado, Guarnieri, Adriano, Piccioni, Adalberto, Frontera, Filippo, Masetti, Nicola, Palazzi, Eliana, Pian, Elena, Greiner, Jochen, Hudec, Renè, Sagar, Ram, Pandey, Anil K., Mohan, Vinay, Björnsson, Gunnlaugur, Jakobsson, Páll, Burud, Ingunn, Courbin, Frederic, Valentini, Gaetano, Piersimoni, Anna, Aceituno, Jesús, Montoya, Luz María, Pedraz, Santos, Gredel, Roland, Claver, Charles F., Rector, Travis A., Rhoads, James E., Walter, Fabian, Ott, Jürgen, Hippelein, Hans, Sánchez-Béjar, Victor, Gutiérrez, Carlos, Oscoz, Alejandro, Zhu, Jin, Chen, Jiansheng, Zhang, Haotong, Wei, Jianyan, Zhou, Aiying, Guiziy, Sergei, Shlyapnikov, Aleksei, Heise, John, Costa, Enrico, Feroci, Marco, and Piro, Luigi
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- 1999
6. Discovery of a Transient Absorption Edge in the X-ray Spectrum of GRB 990705
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Amati, Lorenzo, Frontera, Filippo, Vietri, Mario, Soffitta, Paolo, Costa, Enrico, Del Sordo, Stefano, Pian, Elena, Piro, Luigi, Antonelli, Lucio A., Fiume, D. Dal, Feroci, Marco, Gandolfi, Giangiacomo, Guidorzi, Cristiano, Heise, John, Kuulkers, Erik, Masetti, Nicola, Montanari, Enrico, Nicastro, Luciano, Orlandini, Mauro, and Palazzi, Eliana
- Published
- 2000
7. Cosmic hadron colliders
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Pian, Elena
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- 2019
- Full Text
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8. Early excess emission in Type Ia supernovae from the interaction between supernova ejecta and their circumstellar wind.
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Moriya, Takashi J, Mazzali, Paolo A, Ashall, Chris, and Pian, Elena
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TYPE I supernovae ,SUPERNOVAE ,LIGHT curves ,CIRCUMSTELLAR matter ,WIND speed ,ULTRAVIOLET radiation - Abstract
The effects of the interaction between Type Ia supernova ejecta and their circumstellar wind on the photometric properties of Type Ia supernovae are investigated. We assume that a hydrogen-rich, dense, and extended circumstellar matter (CSM) is formed by the steady mass-loss of their progenitor systems. The CSM density is assumed to be proportional to r
−2 . When the mass-loss rate is above 10−4 M⊙ yr−1 with a wind velocity of 100 km s−1 , CSM interaction results in an early flux excess in optical light curves within 4 d of explosion. In these cases, the optical colour quickly evolves to the blue. The ultraviolet flux below 3000 Å is found to have a persistent flux excess compared to Type Ia supernovae as long as CSM interaction continues. Type Ia supernovae with progenitor mass-loss rates between 10−4 and 10−3 M⊙ yr−1 may not have a CSM that is dense enough to affect spectra to make them Type Ia CSM, but they may still result in Type Ia supernovae with an early optical flux excess. Because they have a persistent ultraviolet flux excess, ultraviolet light curves around the luminosity peak would be significantly different from those with a low-density CSM. [ABSTRACT FROM AUTHOR]- Published
- 2023
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9. Avery luminous magnetar-powered supernova associated with an ultra-long γ-ray burst
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Greiner, Jochen, Mazzali, Paolo A., Kann, D. Alexander, Kruhler, Thomas, Pian, Elena, Prentice, Simon, E., Felipe Olivares, Rossi, Andrea, Klose, Sylvio, Taubenberger, Stefan, Knust, Fabian, Afonso, Paulo M.J., Ashall, Chris, Bolmer, Jan, Delvaux, Corentin, Diehl, Roland, Elliott, Jonathan, Filgas, Robert, Fynbo, Johan P.U., Graham, John F., Guelbenzu, Ana Nicuesa, Kobayashi, Shiho, Leloudas, Giorgos, Savaglio, Sandra, Schady, Patricia, Schmidl, Sebastian, Schweyer, Tassilo, Sudilovsky, Vladimir, Tanga, Mohit, Updike, Adria C., van Eerten, Hendrik, and Varela, Karla
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Supernovae -- Observations ,Gamma rays -- Observations ,Environmental issues ,Science and technology ,Zoology and wildlife conservation - Abstract
A new class of ultra-long-duration (more than 10,000 seconds) γ-ray bursts has recently been suggested (1-3). They may originate in the explosion of stars with much larger radii than those producing normal long-duration γ-ray bursts (3,4) or in the tidal disruption of a star (3). No clear supernova has yet been associated with an ultra-long-duration γ-ray burst. Here we report that a supernova (SN 2011kl) was associated with the ultra-long-duration γ-ray burst GRB 111209A, at a redshift z of 0.677. This supernova is more than three times more luminous than type Ic supernovae associated with long-duration γ-ray bursts (5-7), and its spectrum is distinctly different. The slope of the continuum resembles those of super-luminous supernovae (8,9), but extends further down into the rest-frame ultraviolet implying a low metal content. The light curve evolves much more rapidly than those of super-luminous supernovae. This combination of high luminosity and low metalline opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae (10)., GRB 111209A was detected by the Swift satellite at 07:12 UT on 9 December 2011. The X-ray and optical counterparts were discovered within minutes (11). The extraordinarily long duration of [...]
- Published
- 2015
10. Kilonova Emission and Heavy Element Nucleosynthesis.
- Author
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Pian, Elena
- Subjects
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HEAVY elements , *NUCLEOSYNTHESIS , *VERY large telescopes , *GAMMA ray bursts , *NEUTRON stars , *GRAVITATIONAL waves , *NEUTRON capture , *RADIO jets (Astrophysics) , *STAR formation - Abstract
The binary neutron star merger observed and localized on 17 August 2017 by the LIGO and Virgo gravitational interferometers and by numerous telescopes on the ground and in orbit linked in an unambiguous way the coalescence of double neutron stars with the formation of a relativistic outflow (short gamma-ray burst GRB170817A) and of a thermal radioactive source (kilonova). The vicinity of the event (40 Mpc) made it possible to monitor the electromagnetic counterpart in detail at all wavelengths and to map its close environment in the outskirts of the lenticular galaxy NGC 4993. Radio VLBI images of GRB170817A allowed the first direct detection of superluminal motion in a GRB afterglow, pointing to a collimated ultra-relativistic jet rather than to a quasi-isotropically, mildly relativistically expanding source. The accurate spectroscopy of the kilonova at ultraviolet-to-infrared wavelengths with the X-Shooter spectrograph of the ESO Very Large Telescope showed the long-sought-after signature of rapid neutron capture process (in short: r-process) nucleosynthesis. Kilonova detection makes gravitational wave sources optimal tracers of heavy element formation sites. [ABSTRACT FROM AUTHOR]
- Published
- 2023
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11. The Metamorphosis of Supernova SN 2008D/XRF 080109: A Link between Supernovae and GRBs/Hypernovae
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Mazzali, Paolo A., Valenti, Stefano, Valle, Massimo Della, Chincarini, Guido, Sauer, Daniel N., Benetti, Stefano, Pian, Elena, Piran, Tsvi, D'Elia, Valerio, Elias-Rosa, Nancy, Margutti, Raffaella, Pasotti, Francesco, Antonelli, L. Angelo, Bufano, Filomena, Campana, Sergio, Cappellaro, Enrico, Covino, Stefano, D'Avanzo, Paolo, Fiore, Fabrizio, Fugazza, Dino, Gilmozzi, Roberto, Hunter, Deborah, Maguire, Kate, Maiorano, Elisabetta, Marziani, Paola, Masetti, Nicola, Mirabel, Felix, Navasardyan, Hripsime, Nomoto, Ken'ichi, Palazzi, Eliana, Pastorello, Andrea, Panagia, Nino, Pellizza, L. J., Sari, Re'em, Smartt, Stephen, Tagliaferri, Gianpiero, Tanaka, Masaomi, Taubenberger, Stefan, Tominaga, Nozomu, Trundle, Carrie, and Turatto, Massimo
- Published
- 2008
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12. Asphericity in Supernova Explosions from Late-Time Spectroscopy
- Author
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Maeda, Keiichi, Kawabata, Koji, Mazzali, Paolo A., Tanaka, Masaomi, Valenti, Stefano, Nomoto, Ken'ichi, Hattori, Takashi, Deng, Jinsong, Pian, Elena, Taubenberger, Stefan, Iye, Masanori, Matheson, Thomas, Filippenko, Alexei V., Aoki, Kentaro, Kosugi, George, Ohyama, Youichi, Sasaki, Toshiyuki, and Takata, Tadafumi
- Published
- 2008
- Full Text
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13. An optical view of BL Lacertae objects
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Falomo, Renato, Pian, Elena, and Treves, Aldo
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- 2014
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14. A very luminous magnetar-powered supernova associated with an ultra-long γ-ray burst
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Greiner, Jochen, Mazzali, Paolo A., Kann, Alexander D., Krühler, Thomas, Pian, Elena, Prentice, Simon, Olivares E., Felipe, Rossi, Andrea, Klose, Sylvio, Taubenberger, Stefan, Knust, Fabian, Afonso, Paulo M. J., Ashall, Chris, Bolmer, Jan, Delvaux, Corentin, Diehl, Roland, Elliott, Jonathan, Filgas, Robert, Fynbo, Johan P. U., Graham, John F., Nicuesa Guelbenzu, Ana, Kobayashi, Shiho, Leloudas, Giorgos, Savaglio, Sandra, Schady, Patricia, Schmidl, Sebastian, Schweyer, Tassilo, Sudilovsky, Vladimir, Tanga, Mohit, Updike, Adria C., van Eerten, Hendrik, and Varela, Karla
- Published
- 2015
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15. Abundance stratification in Type Ia supernovae – VI. The peculiar slow decliner SN 1999aa.
- Author
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Aouad, Charles J, Mazzali, Paolo A, Hachinger, Stephan, Teffs, Jacob, Pian, Elena, Ashall, Chris, Benetti, Stefano, Filippenko, Alexei V, and Tanaka, Masaomi
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TYPE I supernovae ,OPTICAL spectra ,IRON - Abstract
The abundance distribution in the ejecta of the peculiar slowly declining Type Ia supernova (SN Ia) SN 1999aa is obtained by modelling a time series of optical spectra. Similar to SN 1991T, SN 1999aa was characterized by early-time spectra dominated by Fe iii features and a weak Si ii 6355 Å line, but it exhibited a high-velocity Ca ii H&K line and morphed into a spectroscopically normal SN Ia earlier. Three explosion models are investigated, yielding comparable fits. The innermost layers are dominated by ∼0.3 M
⊙ of neutron-rich stable iron-group elements, mostly stable iron. Above that central region lies a56 Ni-dominated shell, extending to |$v \approx 11\, 000$| – |$12\, 000$| km s−1 , with mass ∼0.65 M⊙ . These inner layers are therefore similar to those of normal SNe Ia. However, the outer layers exhibit composition peculiarities similar to those of SN 1991T: The intermediate-mass elements shell is very thin, containing only ∼0.2 M⊙ , and is sharply separated from an outer oxygen-dominated shell, which includes ∼0.22 M⊙ . These results imply that burning suddenly stopped in SN 1999aa. This is a feature SN 1999aa shares with SN 1991T, and explains the peculiarities of both SNe, which are quite similar in nature apart from the different luminosities. The spectroscopic path from normal to SN 1991T-like SNe Ia cannot be explained solely by a temperature sequence. It also involves composition layering differences, suggesting variations in the progenitor density structure or in the explosion parameters. [ABSTRACT FROM AUTHOR]- Published
- 2022
- Full Text
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16. GRIPS - Gamma-Ray Imaging, Polarimetry and Spectroscopy
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Greiner, Jochen, Mannheim, Karl, Aharonian, Felix, Ajello, Marco, Balasz, Lajos G., Barbiellini, Guido, Bellazzini, Ronaldo, Bishop, Shawn, Bisnovatij-Kogan, Gennady S., Boggs, Steven, Bykov, Andrej, DiCocco, Guido, Diehl, Roland, Elsässer, Dominik, Foley, Suzanne, Fransson, Claes, Gehrels, Neil, Hanlon, Lorraine, Hartmann, Dieter, Hermsen, Wim, Hillebrandt, Wolfgang, Hudec, Rene, Iyudin, Anatoli, Jose, Jordi, Kadler, Matthias, Kanbach, Gottfried, Klamra, Wlodek, Kiener, Jürgen, Klose, Sylvio, Kreykenbohm, Ingo, Kuiper, Lucien M., Kylafis, Nikos, Labanti, Claudio, Langanke, Karlheinz, Langer, Norbert, Larsson, Stefan, Leibundgut, Bruno, Laux, Uwe, Longo, Francesco, Maeda, Kei’ichi, Marcinkowski, Radoslaw, Marisaldi, Martino, McBreen, Brian, McBreen, Sheila, Meszaros, Attila, Nomoto, Ken’ichi, Pearce, Mark, Peer, Asaf, Pian, Elena, Prantzos, Nikolas, Raffelt, Georg, Reimer, Olaf, Rhode, Wolfgang, Ryde, Felix, Schmidt, Christian, Silk, Joe, Shustov, Boris M., Strong, Andrew, Tanvir, Nial, Thielemann, Friedrich-Karl, Tibolla, Omar, Tierney, David, Trümper, Joachim, Varshalovich, Dmitry A., Wilms, Jörn, Wrochna, Grzegorz, Zdziarski, Andrzej, and Zoglauer, Andreas
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- 2012
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17. Supernova SN 2011fe from an exploding carbon–oxygen white dwarf star
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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, and Poznanski, Dovi
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- 2011
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18. Kilonova Luminosity Function Constraints based on Zwicky Transient Facility Searches for 13 Neutron Star Mergers
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Kasliwal, Mansi M., Anand, Shreya, Ahumada, Tomas, Stein, Robert, Carracedo, Ana Sagues, Andreoni, Igor, Coughlin, Michael W., Singer, Leo P., Kool, Erik C., De, Kishalay, Kumar, Harsh, AlMualla, Mouza, Yao, Yuhan, Bulla, Mattia, Dobie, Dougal, Reusch, Simeon, Perley, Daniel A., Cenko, S. Bradley, Bhalerao, Varun, Kaplan, David L., Sollerman, Jesper, Goobar, Ariel, Copperwheat, Christopher M., Bellm, Eric C., Anupama, G. C., Corsi, Alessandra, Nissanke, Samaya, Agudo, Ivan, Bagdasaryan, Ashot, Barway, Sudhanshu, Belicki, Justin, Bloom, Joshua S., Bolin, Bryce, Buckley, David A. H., Burdge, Kevin B., Burruss, Rick, Caballero-Garc��a, Maria D., Cannella, Chris, Castro-Tirado, Alberto J., Cook, David O., Cooke, Jeff, Cunningham, Virginia, Dahiwale, Aishwarya, Deshmukh, Kunal, Dichiara, Simone, Duev, Dmitry A., Dutta, Anirban, Feeney, Michael, Franckowiak, Anna, Frederick, Sara, Fremling, Christoffer, Gal-Yam, Avishay, Gatkine, Pradip, Ghosh, Shaon, Goldstein, Daniel A., Golkhou, V. Zach, Graham, Matthew J., Graham, Melissa L., Hankins, Matthew J., Helou, George, Hu, Youdong, Ip, Wing-Huen, Jaodand, Amruta, Karambelkar, Viraj, Kong, Albert K. H., Kowalski, Marek, Khandagale, Maitreya, Kulkarni, S. R., Kumar, Brajesh, Laher, Russ R., Li, K. L., Mahabal, Ashish, Masci, Frank J., Miller, Adam A., Mogotsi, Moses, Mohite, Siddharth, Mooley, Kunal, Mroz, Przemek, Newman, Jeffrey A., Ngeow, Chow-Choong, Oates, Samantha R., Patil, Atharva Sunil, Pandey, Shashi B., Pavana, M., Pian, Elena, Riddle, Reed, Sanchez-Ram��rez, Ruben, Sharma, Yashvi, Singh, Avinash, Smith, Roger, Soumagnac, Maayane T., Taggart, Kirsty, Tan, Hanjie, Tzanidakis, Anastasios, Troja, Eleonora, Valeev, Azamat F., Walters, Richard, Waratkar, Gaurav, Webb, Sara, Yu, Po-Chieh, Zhang, Bin-Bin, Zhou, Rongpu, and Zolkower, Jeffry
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics - Solar and Stellar Astrophysics ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Solar and Stellar Astrophysics (astro-ph.SR) - Abstract
We present a systematic search for optical counterparts to 13 gravitational wave (GW) triggers involving at least one neutron star during LIGO/Virgo's third observing run. We searched binary neutron star (BNS) and neutron star black hole (NSBH) merger localizations with the Zwicky Transient Facility (ZTF) and undertook follow-up with the Global Relay of Observatories Watching Transients Happen (GROWTH) collaboration. The GW triggers had a median localization of 4480 deg^2, median distance of 267 Mpc and false alarm rates ranging from 1.5 to 1e-25 per yr. The ZTF coverage had a median enclosed probability of 39%, median depth of 20.8mag, and median response time of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UVOIR photometric points, 64 OIR spectra, and 3 radio. We find no promising kilonova (radioactivity-powered counterpart) and we convert the upper limits to constrain the underlying kilonova luminosity function. Assuming that all kilonovae are at least as luminous as GW170817 at discovery (-16.1mag), we calculate our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than -16.6mag (extrapolated peak magnitude of GW170817) and fade at 1 mag/day (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations, the joint probability of zero detections, assuming all kilonovae are brighter than -16.6mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, 1e-4 or phi>30deg to be consistent with our limits. (Abridged), Submitted to ApJ
- Published
- 2020
19. A very energetic supernova associated with the γ-ray burst of 29 March 2003
- Author
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Hjorth, Jens, Sollerman, Jesper, Møller, Palle, Fynbo, Johan P. U., Woosley, Stan E., Kouveliotou, Chryssa, Tanvir, Nial R., Greiner, Jochen, Andersen, Michael I., Castro-Tirado, Alberto J., Castro Cerón, José María, Fruchter, Andrew S., Gorosabel, Javier, Jakobsson, Páll, Kaper, Lex, Klose, Sylvio, Masetti, Nicola, Pedersen, Holger, Pedersen, Kristian, Pian, Elena, Palazzi, Eliana, Rhoads, James E., Rol, Evert, van den Heuvel, Edward P. J., Vreeswijk, Paul M., Watson, Darach, and Wijers, Ralph A. M. J.
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- 2003
- Full Text
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20. A neutron-star-driven X-ray flash associated with supernova SN 2006aj
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Mazzali, Paolo A., Deng, Jinsong, Nomoto, Ken'ichi, Sauer, Daniel N., Pian, Elena, Tominaga, Nozomu, Tanaka, Masaomi, Maeda, Keiichi, and Filippenko, Alexei V.
- Published
- 2006
21. A very energetic supernova associated with the [gamma]-ray burst of 29 March 2003
- Author
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Hjorth, Jens, Sollerman, Jesper, Mller, Palle, Fynbo, Johan P. U., Woosley, Stan E., Kouveliotou, Chryssa, Tanvir, Nial R., Greiner, Jochen, Andersen, Michael I., Castro-Tirado, Alberto J., Cerón, José, María, Castro, Fruchter, Andrew S., Gorosabel, Javier, Jakobsson, Páll, Kaper, Lex, Klose, Sylvio, Masetti, Nicola, Pedersen, Holger, Pedersen, Kristian, Pian, Elena, Palazzi, Eliana, Rhoads, James E., Rol, Evert, van den Heuvel, Edward P. J., Vreeswijk, Paul M., Watson, Darach, and Wijers, Ralph A. M. J.
- Published
- 2003
22. GRB 180728A: classification of the associated SN 2018fip
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Selsing, J., Izzo, L., ROSSI, Andrea, Malesani, D. B., Heintz, K. E., Schady, P., Starling, R. L. C., Sollerman, J., Leloudas, G., Cano, Z., Fynbo, J. P. U., Valle, M. D., PIAN, Elena, Kann, D. A., Perley, D. A., PALAZZI, ELIANA, Klose, S., Hjorth, J., COVINO, Stefano, D'Elia, V., Tanvir, N. R., Levan, A. J., Hartmann, D., Kouveliotou, C., ITA, USA, GBR, FRA, DEU, and ESP
- Abstract
No abstract
- Published
- 2018
23. BL-Lacs in X-Ray Outburst
- Author
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Remillard, Ronald A, Urry, C. Megan, Aharonian, Felix, Pian, Elena, Sambruna, Rita, and Coppi, Paolo
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Astronomy - Abstract
We conducted a multifrequency campaign for the TeV blazar Markarian 421 in 1998 April. The campaign started from a pronounced high-amplitude flare recorded by BeppoSAX and Whipple; the Advanced Satellite for Cosmology and Astrophysics (ASCA) observation started three days later. In the X-ray data, we detected multiple flares, occurring on timescales of about one day. ASCA data clearly reveal spectral variability. The comparison of the data from ASCA, the Extreme Ultraviolet Explorer, and the Rossi X-Ray Timing Explorer indicates that the variability amplitudes in the low-energy synchrotron component are larger at higher photon energies. In TeV and gamma-rays, large intraday variations-which were correlated with the X-ray flux-were observed when results from three Cerenkov telescopes were combined. The rms variability of TeV and gamma-rays was similar to that observed in hard X-rays, above ten keV. The X-ray light curve reveals flares that are almost symmetric for most cases, implying that the dominant timescale is the light crossing time through the emitting region. The structure function analysis based on the continuous X-ray light curve of seven days indicates that the characteristic timescale is approx. 0.5 days. The analysis of ASCA light curves in various energy bands appears to show both soft (positive) and hard (negative) lags. These may not be real, as systematic effects could also produce these lags, which are all much smaller than an orbit. If the lags of both signs are real, these imply that the particle acceleration and X-ray cooling timescales are similar.
- Published
- 2000
24. Monitoring Ly-Alpha Emission From the Blazar 3C 279
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Koratkar, Anuradha, Pian, Elena, Urry, C. Megan, and Pesce, Joseph E
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Space Radiation - Abstract
The blazar 3C 279 is well studied and shows frequent large continuum flares from radio to gamma-ray wavelengths. There have been a number of multiwavelength observations of 3C 279, and hence there are extensive ultraviolet data for this object available in the UV archives. In this paper we present Ly-alpha emission line measurements for 3C 279 using all the archival IUE SWP spectra from 1988 to 1996 and all archival Hubble Space Telescope (HST) Faint Object Spectrograph (FOS) G190H spectra from 1992 to 1996. Individual archival IUE spectra of 3C 279 show weak Ly-alpha emission at approximately 1868 A (z = 0.536), which is easily seen in the co-added data. The Ly-alpha emission is observed in all the HST/FOS spectra. The strength of Ly-alpha is nearly constant (approximately 5 x 10(exp -14) erg/sq cm.s), while the 1750 A continuum varies by a factor of approximately 50, from approximately 0.6 to 31.6 x 10(exp -15) ergs/sq cm.s.A. The behavior of the Ly-alpha emission line flux and continuum flux is similar to that of the only other well observed blazar, 3C 273, which shows constant line flux while the continuum varies by a factor of approximately 3. This near-constancy of emission-line flux in the two best-studied blazars suggests that the highly variable beamed continuum is not a significant source of photoionization for the gas. Some other source, such as thermal emission from an accretion disk, must be providing a significant fraction of the photoionizing flux in these objects. The large amplitude variability seen at gamma-ray energies must be due to changes in the energetic electrons in the jet rather than changes in the external photon field.
- Published
- 1998
25. OISTER optical and near-infrared monitoring observations of peculiar radio-loud active galactic nucleus SDSSJ110006.07+442144.3
- Author
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Gandhi, Poshak, Pian, Elena, Mazzali, Paolo, Ali, Gamal B., Essam, Ahmed, Hayashida, Kenzo, Hiratsuka, Yuichiro, Inoue, Kanichiro, Ishibashi, Michiko, Murakami, Kotone, Nagayama, Takahiro, Nishimori, Takafumi, Ohshima, Tomohito, Sakata, Shuichiro, Taddia, Francesco, Urago, Riku, Yamashita, Satoshi, Morokuma, Tomoki, Tanaka, Masaomi, Tanaka, Yasuyuki T., Itoh, Ryosuke, Tominaga, Nozomu, Ohta, Kouji, Matsumoto, Emiko, Shibata, Takumi, Akimoto, Hinako, Akitaya, Hiroshi, Aoki, Tsutomu, Doi, Mamoru, Ebisuda, Nana, Fujisawa, Kenta, Fukushima, Hideo, Goda, Shuhei, Gouda, Yuya, Hanayama, Hidekazu, Hashiba, Yasuhito, Hashimoto, Osamu, Honda, Satoshi, Imai, Masataka, Iwata, Ikuru, Izumiura, Hideyuki, Kanda, Yuka, Kawabata, Miho, Kawaguchi, Kenji, Kawai, Nobuyuki, Kokubo, Mitsuru, Kuroda, Daisuke, Maehara, Hiroyuki, Mito, Hiroyuki, Mitsuda, Kazuma, Miyagawa, Ryota, Miyaji, Takeshi, Miyamoto, Yusuke, Morihana, Kumiko, Moritani, Yuki, Morokuma-Matsui, Kana, Murata, Katsuhiro L., Nakamura, Kazuki, Nakaoka, Tatsuya, Niinuma, Kotaro, Nogami, Daisaku, Oasa, Yumiko, Oda, Tatsunori, Saito, Yoshihiko, Sako, Shigeyuki, Sarugaku, Yuki, Sawada-Satoh, Satoko, Seino, Genta, Sorai, Kazuo, Soyano, Takao, Takahashi, Jun, Takagi, Yuhei, Takaki, Katsutoshi, Takata, Koji, Tarusawa, Ken'ichi, Uemura, Makoto, Ui, Takahiro, Ushioda, Kazutoshi, Watanabe, Jun-ichi, Watanabe, Makoto, Yanagisawa, Kenshi, Yonekura, Yoshinori, and Yoshida, Michitoshi
- Subjects
Active galactic nucleus ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,quasars: individual(SDSS J110006.07+442144.3) ,01 natural sciences ,law.invention ,010309 optics ,law ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Emission spectrum ,010303 astronomy & astrophysics ,QC ,Astrophysics::Galaxy Astrophysics ,QB ,relativistic processes ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,accretion, accretion disks ,Near-infrared spectroscopy ,quasars: supermassive black holes ,Astronomy and Astrophysics ,Light curve ,Astrophysics - Astrophysics of Galaxies ,Galaxy ,Redshift ,Accretion (astrophysics) ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics - High Energy Astrophysical Phenomena ,Flare - Abstract
著者人数: 83名, Accepted: 2017-07-13, 資料番号: SA1170168000
- Published
- 2017
26. A Supernova Candidate at z = 0.092 in XMM–Newton Archival Data.
- Author
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Novara, Giovanni, Esposito, Paolo, Tiengo, Andrea, Vianello, Giacomo, Salvaterra, Ruben, Belfiore, Andrea, De Luca, Andrea, D'Avanzo, Paolo, Greiner, Jochen, Scodeggio, Marco, Rosen, Simon, Delvaux, Corentin, Pian, Elena, Campana, Sergio, Lisini, Gianni, Mereghetti, Sandro, and Israel, G. L.
- Published
- 2020
- Full Text
- View/download PDF
27. iPTF14hls as a variable hyper-wind from a very massive star.
- Author
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Moriya, Takashi J, Mazzali, Paolo A, and Pian, Elena
- Subjects
SUPERGIANT stars ,STELLAR winds ,LIGHT curves ,SUPERNOVAE - Abstract
The origin of iPTF14hls, which had Type IIP supernova-like spectra but kept bright for almost two years with little spectral evolution, is still unclear. We here propose that iPTF14hls was not a sudden outburst like supernovae but rather a long-term outflow similar to stellar winds. The properties of iPTF14hls, which are at odds with a supernova scenario, become natural when interpreted as a stellar wind with variable mass-loss rate. Based on the wind hypothesis, we estimate the mass-loss rates of iPTF14hls in the bright phase. We find that the instantaneous mass-loss rate of iPTF14hls during the 2-yr bright phase was more than a few M
⊙ yr−1 ('hyper-wind') and it reached as much as 10 M⊙ yr−1 . The total mass lost over two years was about 10 M⊙ . Interestingly, we find that the light curve of iPTF14hls has a very similar shape to that of η Carinae during the Great Eruption, which also experienced a similar but less extreme brightening accompanied by extraordinary mass-loss, shedding more than 10 M⊙ in 10 yr. The progenitor of iPTF14hls is less than 150 M⊙ if it still exists, which is similar to η Carinae. The two phenomena may be related to a continuum-driven extreme wind from very massive stars. [ABSTRACT FROM AUTHOR]- Published
- 2020
- Full Text
- View/download PDF
28. Supplement: 'Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914' (2016, ApJS, 225, 8)
- Author
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Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Bodiya, T. P., Goetz, R., Mihara, T., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Miao, H., Gossan, S. E., Walsh, S., Johnson, M. D., Aston, S. M., Tomida, H., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Wang, G., Michel, C., Gray, C., Greco, G., Ueno, S., Johnson, M. W. G., Green, A. C., Astone, P., Groot, P., Grote, H., Grunewald, S., Vikram, V., Guidi, G. M., Guo, X., Nichol, R. C., Gupta, A., Tsunemi, H., Gupta, M. K., Gushwa, K. E., Karliner, I., Gustafson, E. K., Gustafson, R., Wang, H., Aufmuth, P., Hacker, J. J., Hall, B. R., Hall, E. D., Middleton, H., Cavalier, F., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Wang, M., Braginsky, V. B., Hanna, C., Hannam, M. D., Hanson, J., Aulbert, C., Hardwick, T., Cowperthwaite, P. S., Mikhailov, E. E., Haris, K., Harms, J., Wang, X., Harry, G. M., Harry, I. W., Hart, M. J., Kasen, D., Hartman, M. T., Haster, C. -J., Haughian, K., Matsuoka, M., Heidmann, A., Milano, L., Wang, Y., Babak, S., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Kent, S., Heng, I. S., MAXI Collaboration, Hennig, J., Ward, R. L., Heptonstall, A. W., Miller, J., Heurs, M., Hild, S., Bacon, P., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Mason, K., Warner, J., Kessler, R., Holt, K., Holz, D. E., Millhouse, M., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Bader, M. K. M., Howell, E. J., Smith, M., Fraser, M., Croft, S., Hu, Y. M., Huang, S., Kim, A. G., Huerta, E. A., Królak, A., Batch, J. C., Huet, D., Hughey, B., Husa, S., Martini, P., Huttner, S. H., Feng, L., Huynh-Dinh, T., Idrisy, A., Baker, P. T., Indik, N., Ingram, D. R., Carrasco Kind, M., Minenkov, Y., Inta, R., Was, M., Isa, H. N., Isac, J. -M., Franzen, T. M. O., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Baldaccini, F., Jacqmin, T., Weaver, B., Ming, J., Kuehn, K., Jang, H., Gaensler, B. M., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Boer, M., Jones, R., Jonker, R. J. G., Mirshekari, S., Ballardin, G., Johnston-Hollitt, M., Kuropatkin, N., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Wei, L. -W., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Mishra, C., Kaplan, D. L., Katsavounidis, E., Katzman, W., Lahav, O., Ballmer, S. W., Walker, A. R., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Morales, M. F., Nord, B., Keitel, D., Kelley, D. B., Weinert, M., Kells, W., Li, T. S., Kennedy, R., Barayoga, J. C., Key, J. S., Khalaidovski, A., Khalili, F. Y., Tingay, S. J., Khan, I., Mitra, S., Weinstein, A. J., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Lima, M., Kim, C., Kim, J., Barclay, S. E., Crocce, M., Kim, K., Weiss, R., Kim, N., Mitrofanov, V. P., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Branchesi, M., Kleybolte, L., Cavalieri, R., Blackburn, J. K., Welborn, T., Klimenko, S., Koehlenbeck, S. M., Barish, B. C., Mitselmakher, G., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Martin, R. M., Masserot, A., Mittleman, R., Barker, D., Moggi, A., Mohan, M., Baune, C., Mohapatra, S. R. P., Montani, M., Moore, B. C., Nugent, P., Matone, L., Moore, C. J., Wayth, R. B., Moraru, D., Moreno, G., Krueger, C., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Bavigadda, V., Wen, L., Mueller, C. L., Mueller, G., Williams, A., Ogando, R., Muir, A. W., Mukherjee, A., Kuehn, G., Mukherjee, D., Mukherjee, S., Mukund, N., Lord, J. E., Mullavey, A., Munch, J., Murphy, D. J., Murchison Wide-field Array (MWA Collaboration), Bazzan, M., Murray, P. G., Petravick, D., Mytidis, A., Kumar, P., Nardecchia, I., Wessels, P., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Smartt, S. J., Nelemans, G., Neri, M., Neunzert, A., Behnke, B., Plazas, A. A., Westphal, T., Kuo, L., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Chambers, K. C., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Wette, K., Nuttall, L. K., Oberling, J., Kutynia, A., Quataert, E., Bejger, M., Ochsner, E., Smith, K. W., O'Dell, J., Oelker, E., Ogin, G. H., Whelan, J. T., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Maia, M. A. G., Oppermann, P., Roe, N., Huber, M. E., Oram, R. J., Bell, A. S., Bogaert, G., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Lackey, B. D., Pai, A., Young, D. R., Pai, S. A., Thorne, K. S., Allen, W. H., Fernández-Muñoz, R., Romer, A. K., Palamos, J. R., Palashov, O., Bell, C. J., Palliyaguru, N., Palomba, C., Pal-Singh, A., Landry, M., Wright, D. E., Wechsler, R. H., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Affeldt, C., Paoletti, F., Paoli, A., Papa, M. A., Berger, B. K., Paris, H. R., White, D. J., Cunha, C. E., Lange, J., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Briant, T., Patricelli, B., Patrick, Z., Inserra, C., Pearlstone, B. L., Massinger, T. J., Pedraza, M., Lantz, B., Bergman, J., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Whiting, B. F., Roodman, A., Phelps, M., Schultz, A., Piccinni, O., Pichot, M., Lasky, P. D., Piergiovanni, F., Pierro, V., Bergmann, G., Pillant, G., Williams, R. D., Pinard, L., Pinto, I. M., Pitkin, M., Cella, G., Rosell, A. C., Poggiani, R., Popolizio, P., Barone, F., Post, A., Powell, J., Lorenzini, M., Prasad, J., Predoi, V., Berry, C. P. L., Premachandra, S. S., Denneau, L., Prestegard, T., Price, L. R., Rykoff, E. S., Prijatelj, M., Lazzarini, A., Williamson, A. R., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Flewelling, H., Punturo, M., Bersanetti, D., Puppo, P., Pürrer, M., Willis, J. L., Sako, M., Lazzaro, C., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Magnier, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Willke, B., Radkins, H., Bertolini, A., Raffai, P., Leaci, P., Sanchez, E., Raja, S., Rakhmanov, M., Primak, N., Rapagnani, P., Raymond, V., Levine, B. M., Wimmer, M. H., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Leavey, S., Betzwieser, J., Scarpine, V., Rest, A., Rei, L., Winkler, W., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Margutti, R., Robie, R., Sherstyuk, A., Wipf, C. C., Robinet, F., Schindler, R., Bhagwat, S., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Lebigot, E. O., Wittel, H., Stalder, B., Romie, J. H., Rosińska, D., Rowan, S., Yock, P. C., Schubnell, M., Rüdiger, A., Bhandare, R., Ruggi, P., Ryan, K., Kankare, E., Sachdev, S., Stubbs, C. W., Lee, C. H., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Scolnic, D., Samajdar, A., Wester, W., Sammut, L., Bilenko, I. A., Masso-Reid, M., Sanchez, E. J., Lee, H. K., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Bogan, C., Saulson, P. R., Sevilla-Noarbe, I., Sauter, O., D'Andrea, C. B., Savage, R. L., Sawadsky, A., Lee, H. M., Billingsley, G., Schale, P., Schilling, R., Woan, G., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Tonry, J., Brillet, A., Schönbeck, A., Schreiber, E., Lee, K., Schuette, D., Loriette, V., Schutz, B. F., Birch, J., Scott, J., Scott, S. M., Sellers, D., Waters, C., Sentenac, D., Sequino, V., Sheldon, E., Sergeev, A., Worden, J., Lenon, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Birney, R., Cepeda, C. B., Shah, S., Shahriar, M. S., Shaltev, M., Thrane, E., Wright, J. 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L., Sollerman, J., Letendre, N., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Rattenbury, N., Suchyta, E., Yap, M. J., Bizouard, M. A., Tápai, M., Tarabrin, S. P., Matichard, F., Taracchini, A., Levin, Y., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Yanny, B., Thomas, M., Thomas, P., Swanson, M. E. C., Thorne, K. A., Yu, H., Tiwari, S., Lormand, M., Bohe, A., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Kupfer, T., Zendri, J. -P., Zevin, M., Zhang, F., Tiwari, V., Zhang, L., Zuntz, J., Losurdo, G., Zhang, M., Zhang, Y., Bojtos, P., Zhao, C., Harmanen, J., Zhou, M., Zhou, Z., Tokmakov, K. V., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Lough, J. D., Dark Energy Survey Collaboration, LIGO Scientific Collaboration, Virgo Collaboration, Galbany, L., Allison, J., Tomlinson, C., Bond, C., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Lück, H., Harvey-Smith, L., Brisson, V., Le Guillou, L., Tonelli, M., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., Bondu, F., McConnell, D., Murphy, T., Popping, A., Lundgren, A. P., Reynolds, J., Torres, C. V., Cerretani, G., Sault, R. J., Dark Energy Camera GW-EM Collaboration, Voronkov, M. A., Whiting, M. T., Australian Square Kilometer Array Pathfinder (ASKAP Collaboration), Castro-Tirado, A. J., Cunniffe, R., Bonnand, R., Jelínek, M., da Costa, L. N., Barsuglia, M., Lyman, J. D., Tello, J. C., Oates, S. R., Hu, Y. -D., Connaughton, V., Kubánek, P., Guziy, S., Castellón, A., García-Cerezo, A., Tarle, G., Muñoz, V. F., Pérez del Pulgar, C., CASENTINI, CLAUDIO, Maguire, K., Luo, J., Boom, B. A., Castillo-Carrión, S., Castro Cerón, J. M., Hudec, R., Burns, E., Torrie, C. I., Caballero-García, M. D., Páta, P., Vitek, S., Adame, J. A., Lin, H., Konig, S., Matheson, T., Rendón, F., Mateo Sanguino, T. de J., Goldstein, A., Töyrä, D., Querel, R., Briggs, M. 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M., Macleod, D. M., Caragiulo, M., Trozzo, L., CARAVEO, PATRIZIA, Valenti, S., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Boschi, V., Dennefeld, M., Magaña-Sandoval, F., Cominsky, L. R., Gal-Yam, A., Buchanan, C. C., Costanza, F., Cuoco, A., D'AMMANDO, FILIPPO, de Palma, F., Desiante, R., Digel, S. W., Tse, M., Di Lalla, N., Di Mauro, M., Magee, R. M., Jonker, P. G., PESSTO Collaboration, Wang, Ch., Di Venere, L., Domínguez, A., Agathos, M., Buikema, A., Turconi, M., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Ćwiek, A., Mageswaran, M., Fukazawa, Y., Hiriart, D., Funk, S., Thaler, J., Fusco, P., Gargano, F., Gasparrini, D., Bulik, T., Giglietto, N., Giommi, P., Aguiar, O. D., Giordano, F., Barta, D., Giroletti, M., Tuyenbayev, D., Glanzman, T., Lee, W. H., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Mavalvala, N., Bulten, H. J., Guiriec, S., Libson, A., Melchior, P., Hadasch, D., Harding, A. K., Hays, E., Claret, A., Hewitt, J. W., Hill, A. B., Horan, D., Cesarini, E., Jogler, T., Ugolini, D., Jóhannesson, G., Johnson, A. S., Majorana, E., Buonanno, A., Kensei, S., Kocevski, D., Kuss, M., Sánchez-Ramírez, R., La Mura, G., Ćwiok, M., Unnikrishnan, C. S., Larsson, S., Latronico, L., Li, J., Li, L., Maksimovic, I., Longo, F., Loparco, F., Buskulic, D., Lovellette, M. N., Lubrano, P., Blair, D. G., Mankiewicz, L., Pandey, S. B., Magill, J., Maldera, S., Manfreda, A., MARELLI, MARTINO, Malvezzi, V., Mayer, M., Mazziotta, M. N., McEnery, J. E., Urban, A. L., Meyer, M., Opiela, R., Buy, C., Michelson, P. F., Mediavilla, T., Mirabal, N., Mizuno, T., Moiseev, A. A., Man, N., Monzani, M. E., Usman, S. A., Moretti, E., Morselli, A., Diehl, H. T., Moskalenko, I. V., Negro, M., Nuss, E., Byer, R. L., Sabau-Graziati, L., Ohsugi, T., Omodei, N., Anderson, J. P., Mandel, I., Orienti, M., Orlando, E., Zaremba, M., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Vahlbruch, H., BOOTES Collaboration, Cadonati, L., Mandic, V., Porter, T. A., Rowlinson, A., Żarnecki, A. F., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Vajente, G., Reimer, A., Reimer, O., Salvetti, D., Saz Parkinson, P. M., Abbott, T. M. C., Mangano, V., Pi of Sky Collaboration, Sgrò, C., Cagnoli, G., Simone, D., Valdes, G., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Onken, C. A., Mansell, G. L., Bose, S., van Bakel, N., Thompson, D. J., Tibaldo, L., Cahillane, C., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Scalzo, R. A., Wood, K. S., Brinkmann, M., Manske, M., Wood, M., Abdalla, F. B., Zhu, S., Zimmer, S., Fermi LAT Collaboration, Agatsuma, K., Bustillo, J. C., BROCATO, Enzo, Mazumder, N., Littenberg, T. B., CAPPELLARO, Enrico, COVINO, Stefano, Mantovani, M., GRADO, ANIELLO, NICASTRO, LUCIANO, Allam, S., PALAZZI, ELIANA, PIAN, Elena, AMATI, LORENZO, ANTONELLI, Lucio Angelo, van Beuzekom, M., Schmidt, B. P., Capaccioli, M., Callister, T., D'AVANZO, Paolo, Metzger, B. D., D'Elia, V., GETMAN, FEDOR, Giuffrida, G., Annis, J., Iannicola, G., van den Brand, J. F. J., Limatola, L., Wolf, C., LISI, Massimiliano, MARINONI, SILVIA, MARRESE, Paola Maria, MELANDRI, Andrea, Barthelmy, S., Calloni, E., PIRANOMONTE, Silvia, POSSENTI, ANDREA, Van Den Broeck, C., PULONE, Luigi, Armstrong, R., Chakraborty, R., ROSSI, Andrea, STAMERRA, Antonio, Stella, L., Testa, V., TOMASELLA, Lina, Marchesoni, F., Yang, S., Vander-Hyde, D. C., GRAvitational Wave Inaf TeAm (GRAWITA), Camp, J. B., Bazzano, A., Yuan, F., Bozzo, E., Benoit-Lévy, A., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., BOTTICELLA, MARIA TERESA, Marion, F., Kuulkers, E., Laurent, P., MEREGHETTI, Sandro, SkyMapper Collaboration, Roques, J. P., Cannon, K. C., Savchenko, V., Berger, E., Ubertini, P., Blair, R. M., INTEGRAL Collaboration, Kasliwal, M. M., Márka, S., Singer, L. P., Cao, Y., Stappers, B. W., Dietrich, J. P., Duggan, G., Kulkarni, S. R., Bhalerao, V., van der Schaaf, L., Miller, A. A., Cao, J., Bernstein, R. A., Barlow, T., Bellm, E., Márka, Z., Manulis, I., Evans, P. A., Rana, J., Laher, R., van Heijningen, J. V., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Bertin, E., Capano, C. D., Markosyan, A. S., Kennea, J. A., Perley, D., van Veggel, A. A., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Intermediate Palomar Transient Factory (iPTF Collaboration), Hurley, K., Golenetskii, S. V., Aptekar, R. L., Brout, D., Burrows, D. N., Vardaro, M., Maros, E., Frederiks, D. D., Capocasa, E., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., InterPlanetary Network, Vass, S., CAMPANA, Sergio, Abe, F., Martelli, F., Buckley-Geer, E., Doi, M., Fujisawa, K., Carbognani, F., Kawabata, K. S., Morokuma, T., Motohara, K., Lockerbie, N. A., Tanaka, M., Bartos, I., Ohta, K., Yanagisawa, K., Martellini, L., Yoshida, M., Bouffanais, Y., J-GEM Collaboration, Baltay, C., Rabinowitz, D., Thomas, D., Caride, S., Ellman, N., Cenko, S. B., Rostami, S., La Silla-QUEST Survey, Bersier, D. F., Martin, I. W., Bode, M. F., Collins, C. A., Burke, D. L., Vasúth, M., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Marshall, F. E., Gomboc, A., Aggarwal, N., Diaz, J. C., Kobayashi, S., Miller, C. J., Mazzali, P., Vaulin, R., Mundell, C. G., Piascik, A. S., Capozzi, D., Pollacco, Don, Nousek, J., Steele, I. A., Ulaczyk, K., Liverpool Telescope Collaboration, Broderick, J. W., Fender, R. P., Baiardi, L. C., O'Brien, P., Carretero, J., Chalermsongsak, T., Osborne, J. P., Doctor, Z., Palmer, D., PERRI, Matteo, Siegel, M., Mazzolo, G., TAGLIAFERRI, Gianpiero, Vecchio, A., Swift Collaboration, Klotz, A., Wijers, R. A. M. J., Turpin, D., Laugier, R., TAROT Collaboration, Chamberlin, S. J., Drlica-Wagner, A., Zadko Collaboration, Algerian National Observatory, Algerian Collaboration, Vedovato, G., McCarthy, R., C2PU Collaboration, Beroiz, M., Low Frequency Array (LOFAR Collaboration), Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Veitch, J., Drout, M. R., Chan, M., McClelland, D. E., Colazo, C., Lipunov, V., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., Bloemen, S., DePoy, D. L., Padilla, N., Pereyra, N. A., Eifler, T. F., McCormick, S., Gorbovskoy, E., Benacquista, M., Chao, S., TOROS Collaboration, Tanvir, N. R., Veitch, P. J., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Tyurina, N., McGuire, S. C., Estrada, J., Milvang-Jensen, B., Venkateswara, K., Watson, D., Charlton, P., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Bartlett, J., Schulze, S., McIntyre, G., Verkindt, D., de Ugarte Postigo, A., Evrard, A. E., Thoene, C. C., Cano, Z., Rosswog, S., Chassande-Mottin, E., VISTA Collaboration, ASCENZI, STEFANO, Kornilov, V., Barsotti, L., MANGANO, VALERIA, Kowalska, I., McIver, J., MUKHERJEE, DIPANJAN, SALEMI, Filippo, Fernandez, E., SANCHEZ RAMIREZ, RUBEN, DI MAURO, Maria Giuseppina, GIROLETTI, MARCELLO, Balanutsa, P., Vetrano, F., Chen, H. Y., ORIENTI, Monica, Bork, R., STELLA, Luigi, Bradaschia, C., TESTA, Vincenzo, BAZZANO, ANGELA, Chen, Y., Caudill, S., Thomas, R. C., Aiello, L., Cheng, C., Chincarini, A., Chiummo, A., Brau, J. E., Cho, H. S., Cho, M., Chow, J. H., Finley, D. A., Christensen, N., Chen, T. -W., Kuznetsov, A., Chu, Q., Chua, S., Chung, S., Ain, A., Ciani, G., McManus, D. J., Clara, F., Clark, J. A., Cleva, F., Viceré, A., Coccia, E., Buckley, D., Flaugher, B., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Jr., McWilliams, S. T., Ajith, P., Vinciguerra, S., Conte, A., Conti, L., Castander, F. J., Cook, D., Corbitt, T. R., Foley, R. J., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Vine, D. J., Meacher, D., Coughlin, M. W., Coughlin, S. B., Rebolo, R., Allen, B., Coulon, J. -P., Countryman, S. T., Couvares, P., Fong, W. -F., Cowan, E. E., Vinet, J. -Y., Coward, D. M., Cowart, M. J., Bassiri, R., Coyne, D. C., Serra-Ricart, M., Coyne, R., Craig, K., Creighton, J. D. E., Allocca, A., Cripe, J., Vitale, S., Crowder, S. G., Fosalba, P., Cumming, A., Cunningham, L., Meadors, G. D., Israelian, G., Cuoco, E., Dal Canton, T., Danilishin, S. L., D'Antonio, S., Vo, T., Danzmann, K., Darman, N. S., Altin, P. A., Dattilo, V., Fox, D. B., Dave, I., Budnev, N. M., Meidam, J., Daveloza, H. P., Davier, M., Bock, O., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., Anderson, S. B., Martynov, D. V., Frieman, J., Melatos, A., Vocca, H., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., Gress, O., De Rosa, R., Logue, J., DeSalvo, R., Kozak, D. B., Mendell, G., Fryer, C. L., Anderson, W. G., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Ivanov, K., Vorvick, C., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Mendoza-Gandara, D., Dojcinoski, G., Gaztanaga, E., Dolique, V., Arai, K., Donovan, F., DELLA VALLE, Massimo, Poleshuk, V., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Mercer, R. A., Drever, R. W. P., Driggers, J. C., Gerdes, D. W., Voss, D., Du, Z., Tlatov, A., Ducrot, M., Araya, M. C., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Neilsen, E., Eggenstein, H. -B., Tucker, D. L., Ehrens, P., Eichholz, J., Cavagliá, M., Brady, P. R., Eikenberry, S. S., Engels, W., Essick, R. C., Arceneaux, C. C., Etzel, T., Evans, M., Vousden, W. D., Merilh, E., Evans, T. M., Everett, R., Yurkov, V., Factourovich, M., Fafone, V., Goldstein, D. A., Fair, H., Fairhurst, S., Fan, X., Vyatchanin, S. P., Fang, Q., Areeda, J. S., Merzougui, M., Farinon, S., Chornock, R., Farr, B., Farr, W. M., Favata, M., Fays, M., Gruen, D., Wade, A. R., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Meshkov, S., MASTER Collaboration, Ferrini, F., Arnaud, N., Fidecaro, F., Fiori, I., Wade, L. E., Fiorucci, D., Fisher, R. P., Gruendl, R. A., Flaminio, R., Fletcher, M., Fournier, J. -D., Kawai, N., Messenger, C., Franco, S., Frasca, S., Wade, M., Frasconi, F., Arun, K. G., Frei, Z., Freise, A., Frey, R., Gutierrez, G., Frey, V., Serino, M., Fricke, T. T., Basti, A., Walker, M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Ascenzi, S., Gair, J. R., Gammaitoni, L., Marx, J. N., Herner, K., Wallace, L., Gaonkar, S. G., Messick, C., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Negoro, H., Lombardi, A. L., Ashton, G., Gennai, A., Honscheid, K., Kringel, V., Meyers, P. M., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., ELIAS DE LA ROSA, NANCY DEL CARMEN, Nakahira, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Ast, M., Mezzani, F., James, D. J., Glaefke, A., and Goetz, E.
- Abstract
This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.
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- 2016
29. LIGO/Virgo G194575: INAF-TNG/Asiago Telescope follow-up of iPTF15dld
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TOMASELLA, Lina, CAPPELLARO, Enrico, D'AVANZO, Paolo, PIRANOMONTE, Silvia, Branchesi, M., CAMPANA, Sergio, BENETTI, Stefano, BROCATO, Enzo, ANTONELLI, Lucio Angelo, Astone, P., COVINO, Stefano, D'Elia, V., GETMAN, FEDOR, Giuffrida, G., GRADO, ANIELLO, Greco, G., Limatola, L., Lisi, M., Marinoni, S., MARRESE, Paola Maria, MELANDRI, Andrea, NICASTRO, LUCIANO, PALAZZI, ELIANA, PIAN, Elena, PULONE, Luigi, Ricci, F., Stratta, G., TAGLIAFERRI, Gianpiero, TESTA, Vincenzo, Boschin, W., Carosati, D., and Di Fabrizio, L.
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- 2015
30. Discovery of dramatic optical variability in SDSS J1100+4421:A peculiar radio-loud narrow-line Seyfert 1 galaxy?
- Author
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Stawarz, Lukasz, Gandhi, Poshak, Ali, Gamal, Contreras, Carlos, Essam, Ahmad, Hamed, Gamal, Hsiao, Eric Y., Mazzali, Paolo A., Morokuma-Matsui, Kana, Morrell, Nidia, Nagao, Tohru, Nakata, Fumiaki, Noma, Chinami, Phillips, Mark M., Pian, Elena, Richmond, Michael W., Sahu, Devendra, Tanaka, Masaomi, Morokuma, Tomoki, Itoh, Ryosuke, Akitaya, Hiroshi, Tominaga, Nozomu, Saito, Yoshihiko, Tanaka, Yasuyuki T., Aoki, Tsutomu, Doi, Mamoru, Iwata, Ikuru, Kawabata, Koji S., Kawai, Nobuyuki, Kikuchi, Yuki, Kobayashi, Naoto, Kuroda, Daisuke, Maehara, Hiroyuki, Matsumoto, Emiko, Minezaki, Takeo, Mito, Hiroyuki, Miyata, Takashi, Miyazaki, Satoshi, Mori, Kensho, Moritani, Yuki, Nakada, Yoshikazu, Ohsuga, Ken, Okada, Norio, Sako, Shigeyuki, and Sarugaku, Yuki
- Subjects
Active galactic nucleus ,Astrophysics::High Energy Astrophysical Phenomena ,galaxies: active ,jets [galaxies] ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Luminosity ,symbols.namesake ,Astrophysical jet ,Seyfert [galaxies] ,Astrophysics::Solar and Stellar Astrophysics ,galaxies: individual (SDSS J110006.07+442144.3) ,Emission spectrum ,Astrophysics::Galaxy Astrophysics ,QB ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Astronomy and Astrophysics ,galaxies: jets ,Astrophysics - Astrophysics of Galaxies ,galaxies: Seyfert ,Galaxy ,individual (SDSS J110006.07+442144.3) [galaxies] ,Black hole ,Supernova ,Space and Planetary Science ,Astrophysics of Galaxies (astro-ph.GA) ,Eddington luminosity ,active [galaxies] ,symbols ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
著者人数: 58名, Accepted: 2014-09-01, 資料番号: SA1140158000
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- 2014
31. Time delays between Fermi LAT and GBM light curves of GRBs
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Castignani, Gianluca, Guetta, Dafne, Pian, Elena, Amati, Lorenzo, Puccetti, Simonetta, and Dichiara, Simone
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
Most Gamma-Ray Bursts (GRBs) detected by the Fermi Gamma-ray Space Telescope exhibit a delay of up to about 10 seconds between the trigger time of the hard X-ray signal as measured by the Fermi GBM and the onset of the MeV-GeV counterpart detected by the LAT. This delay may hint at important physics, whether it is due to the intrinsic variability of the inner engine or it is related to quantum dispersion effects in the velocity of light propagation from the sources to the observer. It is critical to have a proper assessment of how these time delays affect the overall properties of the light curves. We cross-correlated the 5 brightest GRBs of the 1st Fermi LAT Catalog by means of the continuous correlation function (CCF) and of the Discrete Correlation Function (DCF). A maximum in the DCF suggests the presence of a time lag between the curves, whose value and uncertainty are estimated through a Gaussian fitting of the DCF profile and light curve simulation via a Monte Carlo approach. The cross-correlation of the observed LAT and GBM light curves yields time lags that are mostly similar to those reported in the literature, but they are formally consistent with zero. The cross-correlation of the simulated light curves yields smaller errors on the time lags and more than one time lag for GRBs 090902B and 090926A; for all 5 GRBs, the time lags are significantly different from zero and consistent with those reported in the literature, when only the secondary maxima are considered for those two GRBs. The DCF method evidences the presence of time lags between the LAT and GBM light curves and underlines their complexity. While this suggests that the delays should be ascribed to intrinsic physical mechanisms, more sensitivity and larger statistics are needed to assess whether time lags are universally present in the early GRB emission and which dynamical time scales they trace., 9 pages, 3 figures, accepted for publication in Astronomy & Astrophysics
- Published
- 2014
32. Extending the 'energetic scaling of relativistic jets from black hole systems' to include γ-ray-loud X-ray binaries.
- Author
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Lamb, Gavin P., Kobayashi, Shiho, and Pian, Elena
- Subjects
BLACK holes ,X-ray binaries ,COSMOLOGICAL distances ,ACTIVE galactic nuclei ,DOPPLER effect - Abstract
We show that the jet power Pj and geometrically corrected γ-ray luminosity Lγ for the X-ray binaries (XRBs) Cygnus X-1, Cygnus X-3, and V404 Cygni, and γ-ray upper limits for GRS 1915+105 and GX339-4, follow the universal scaling for the energetics of relativistic jets from black hole (BH) systems found by Nemmen et al. for blazars and GRBs. The observed peak γ-ray luminosity for XRBs is geometrically corrected, and theminimum jet power is estimated from the peak flux density of radio flares and the flare rise time. The Lγ-Pj correlation holds across ~17 orders of magnitude. The correlation suggests a jet origin for the high-energy emission from XRBs, and indicates a common mechanism or efficiency for the high-energy emission 0.1-100 GeV from all relativistic BH systems. [ABSTRACT FROM AUTHOR]
- Published
- 2017
- Full Text
- View/download PDF
33. PTF11eon/SN2011dh: Discovery of a Type IIb Supernova From a Compact Progenitor in the Nearby Galaxy M51
- Author
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Arcavi, Iair, Gal-Yam, Avishay, Yaron, Ofer, Sternberg, Assaf, Rabinak, Itay, Waxman, Eli, Kasliwal, Mansi M., Quimby, Robert M., Ofek, Eran O., Horesh, Assaf, Kulkarni, Shrinivas R., Filippenko, Alexei V., Silverman, Jeffrey M., Cenko, S. Bradley, Li, Weidong, Bloom, Joshua S., Sullivan, Mark, Fox, Derek B., Nugent, Peter E., Poznanski, Dovi, Gorbikov, Evgeny, Riou, Amedee, Lamotte-Bailey, Stephane, Griga, Thomas, Cohen, Judith G., Polishook, David, Xu, Dong, Ben-Ami, Sagi, Manulis, Ilan, Walker, Emma S., Mazzali, Paulo A., Pian, Elena, Matheson, Thomas, Maquire, Kate, Pan, Yen-Chen, Bersier, David, James, Philip, Marchant, Jonathan M., Smith, Robert J., Mottram, Chris J., Barnsley, Robert M., Kandrashoff, Michael T., and Clubb, Kelsey I.
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
On May 31, 2011 UT a supernova (SN) exploded in the nearby galaxy M51 (the Whirlpool Galaxy). We discovered this event using small telescopes equipped with CCD cameras, as well as by the Palomar Transient Factory (PTF) survey, and rapidly confirmed it to be a Type II supernova. Our early light curve and spectroscopy indicates that PTF11eon resulted from the explosion of a relatively compact progenitor star as evidenced by the rapid shock-breakout cooling seen in the light curve, the relatively low temperature in early-time spectra and the prompt appearance of low-ionization spectral features. The spectra of PTF11eon are dominated by H lines out to day 10 after explosion, but initial signs of He appear to be present. Assuming that He lines continue to develop in the near future, this SN is likely a member of the cIIb (compact IIb; Chevalier and Soderberg 2010) class, with progenitor radius larger than that of SN 2008ax and smaller than the eIIb (extended IIb) SN 1993J progenitor. Our data imply that the object identified in pre-explosion Hubble Space Telescope images at the SN location is possibly a companion to the progenitor or a blended source, and not the progenitor star itself, as its radius (~10^13 cm) would be highly inconsistent with constraints from our post-explosion photometric and spectroscopic data.
- Published
- 2011
34. FERMI constraints on the high energy, ~1 GeV, emission of long GRBs
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Guetta, Dafne, Pian, Elena, and Waxman, Eli
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Nuclear Experiment ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
We investigate the constraints imposed on the luminosity function (LF) of long duration Gamma Ray Bursts (LGRBs) by the flux distribution of bursts detected by the GBM at ~1 MeV, and the implications of the non detection of the vast majority, ~95%, of the LGRBs at higher energy, ~1 GeV, by the LAT detector. We find a LF that is consistent with those determined by BATSE and Swift. The non detections by LAT set upper limits on the ratio R of the prompt fluence at ~1 GeV to that at ~1 MeV. The upper limits are more stringent for brighter bursts, with R, Comment: 12 pages, 6 figures. Submitted to A&A
- Published
- 2010
35. INTEGRAL and Swift Observations of Blazars in Outburst
- Author
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Pian, Elena, Foschini, Luigi, and Ghisellini, Gabriele
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Abstract
The blazars 3C 454.3, PKS 0537-441 and PKS 2155-304 are traditionally known to be among the most active sources of this class. They emit at all frequencies, up to the gamma-rays, and are good probes of multiwavelength nuclear variability. The first two have also luminous broad emission line regions. We have recently monitored them with various facilities, including Swift and INTEGRAL, and have interpreted their variations with models of non-thermal radiation from a relativistic jet. In particular, we have tested for the first two sources the hypothesis that the variability is produced within the jet through internal shocks, i.e. collisions of relativistic plasma blobs. This allows a parameterization of all physical quantities as functions of the bulk Lorentz factor. We have made the critical assumption that every flaring episode is characterized by a fixed amount of energy. The model reproduces brilliantly the multiwavelength data and especially the gamma-ray spectra, when available. The model is not applicable to PKS 2155-304, the variability of which is caused by independent variations of few individual parameters., 12 pages, 5 figures, Proceedings of the Frascati Workshop 2007 (Vulcano, May 28 - June 2, 2007)
- Published
- 2007
36. OISTER optical and near-infrared monitoring observations of peculiar radio-loud active galactic nucleus SDSSJ110006.07+442144.3.
- Author
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Tomoki MOROKUMA, Masaomi TANAKA, TANAKA, Yasuyuki T., Ryosuke ITOH, Nozomu TOMINAGA, GANDHI, Poshak, PIAN, Elena, MAZZALI, Paolo, Kouji OHTA, Emiko MATSUMOTO, Takumi SHIBATA, Hinako AKIMOTO, Hiroshi AKITAYA, ALI, Gamal B., Tsutomu AOKI, DOI, Mamoru, EBISUDA, Nana, ESSAM, Ahmed, Kenta FUJISAWA, and Hideo FUKUSHIMA
- Subjects
ACCRETION disks ,QUASARS ,SUPERMASSIVE black holes ,RELATIVISTIC astrophysics ,ACTIVE galactic nuclei ,NEAR infrared radiation ,OPTICAL astronomy - Abstract
We present monitoring campaign observations at optical and near-infrared (NIR) wavelengths for a radio-loud active galactic nucleus (AGN) at z = 0.840, SDSSJ110006.07+442144.3 (hereafter, J1100+4421), which was identified during a flare phase in late 2014 February. The campaigns consist of three intensive observing runs from the discovery to 2015 March, mostly within the scheme of the OISTER collaboration. Optical-NIR light curves and simultaneous spectral energy distributions (SEDs) are obtained. Our measurements show the strongest brightening in 2015 March. We found that the optical-NIR SEDs of J1100+4421 show an almost steady shape despite the large and rapid intranight variability. This constant SED shape is confirmed to extend to ~5μm in the observed frame using the archival WISE data. Given the lack of absorption lines and the steep power-law spectrum of α
ν ~ -1.4, where fν - ναν , synchrotron radiation by a relativistic jet with no or small contributions from the host galaxy and the accretion disk seemsmost plausible as an optical-NIR emission mechanism. The steep optical-NIR spectral shape and the large amplitude of variability are consistent with this object being a low νpeak jet-dominated AGN. In addition, sub-arcsecond resolution optical imaging data taken with Subaru Hyper Suprime-Cam does not show a clear extended component and the spatial scales are significantly smaller than the large extensions detected at radio wavelengths. The optical spectrum of a possible faint companion galaxy does not show any emission lines at the same redshift, and hence a merging hypothesis for this AGN-related activity is not supported by our observations. [ABSTRACT FROM AUTHOR]- Published
- 2017
- Full Text
- View/download PDF
37. Hubble Space Telescope STIS Observations of GRB 000301C: CCD Imaging and Near-Ultraviolet MAMA Spectroscopy
- Author
-
Smette, Alain, Fruchter, Andrew S., Gull, Theodore R., Sahu, Kailash C., Petro, Larry, Ferguson, Henry, Rhoads, James, Lindler, Don J., Gibbons, Rachel, Hogg, David W., Kouveliotou, Chryssa, Livio, Mario, Macchetto, Duccio, Metzger, Mark R., Pedersen, Holger, Pian, Elena, Thorsett, Stephen E., Wijers, Ralph A. M. J., Fynbo, Johan P. U., Gorosabel, Javier, Hjorth, Jens, Jensen, Brian L., Levine, Alan, Smith, Donald A., Cline, Tom, Hurley, Kevin, and Trombka, Jack
- Abstract
We present Space Telescope Imaging Spectrograph observations of the optical transient (OT) counterpart of the γ-ray burster GRB 000301C obtained 5 days after the burst, on 2000 March 6. CCD clear-aperture imaging reveals a R ≃ 21.50 ± 0.15 source with no apparent host galaxy. An 8000 s, 1150 Å < λ < 3300 Å near-ultraviolet MAMA prism spectrum shows a flat or slightly rising continuum (in f_λ) between 2800 and 3300 Å, with a mean flux of (8.7^(+0.8)_(-1.6) ± 2.6) × 10^(-18) ergs s^(-1) cm^(-2)Å^(-1), and a sharp break centered at 2797 ± 25 Å. We interpret this as the H I Lyman break at z = 2.067 ± 0.025, indicating the presence of a cloud with an H I column density log N_(H I(cm^2) > 18 on the line of sight to the OT. This measured redshift is conservatively a lower limit to the GRB redshift. However, as all other GRBs that have deep Hubble Space Telescope images appear to lie on the stellar field of a host galaxy, and as the large H I column density measured here and in later ground-based observations is unlikely on a random line of sight, we believe we are probably seeing absorption from H I in the host galaxy. In any case, this represents the largest direct redshift determination of a γ-ray burster to date. Our data are compatible with an OT spectrum represented by a power law with an intrinsic index α = 1.2 (f_ν ∝ ν^(-α)) and no extinction in the host galaxy, or with α = 0.5 and extinction by SMC-like dust in the OT rest frame with A_V = 0.15. The large N_(H I) and the lack of a detected host are similar to the situation for damped Lyα absorbers at z > 2.
- Published
- 2001
38. Science with IUE and the Growth of an Astrophysical Group in Milan: from X-Ray Binaries to AGN
- Author
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Falomo, Renato, Maraschi, Laura, Pian, Elena, and Treves, Aldo
- Subjects
Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics - Abstract
The contribution of an astrophysics group based in Milan to the science with the IUE satellite during its almost 20 years lifetime has focussed on high energy sources, of both galactic (LMXRB, HMXRB, and black hole candidates) and extragalactic (AGN) nature. The results of this long term research and in particular of the latest multiwavelength campaigns conducted simultaneously with IUE are reviewed here., 15 pages, Latex, 6 PostScript figures, to appear in "UV Astronomy in Italy", Lucio M. Buson and Domitilla De Martino eds., Mem. S.A.It. 1999
- Published
- 1998
39. BeppoSAX Observations of Unprecedented Synchrotron Activity in the BL Lac Object Mkn 501
- Author
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Pian, Elena, Vacanti, Giuseppe, Tagliaferri, Gianpiero, Ghisellini, Gabriele, Maraschi, Laura, Treves, Aldo, Urry, C. Megan, Fiore, Fabrizio, Giommi, Paolo, Palazzi, Eliana, Chiappetti, Lucio, and Sambruna, Rita M.
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics - Abstract
The BL Lac object Mkn 501, one of the only three extragalactic sources (with Mkn 421 and 1ES 2344+514) so far detected at TeV energies, was observed with the BeppoSAX satellite on 7, 11, and 16 April 1997 during a phase of high activity at TeV energies, as monitored with the Whipple, HEGRA and CAT Cherenkov telescopes. Over the whole 0.1-200 keV range the spectrum was exceptionally hard (alpha =< 1, with F_nu ~ nu^{-alpha}) indicating that the X-ray power output peaked at (or above) ~100 keV. This represents a shift of at least two orders of magnitude with respect to previous observations of Mkn 501, a behavior never seen before in this or any other blazar. The overall X-ray spectrum hardens with increasing intensity and, at each epoch, it is softer at larger energies. The correlated variability from soft X-rays to the TeV band points to models in which the same population of relativistic electrons produces the X-ray continuum via synchrotron radiation and the TeV emission by inverse Compton scattering of the synchrotron photons or other seed photons. For the first time in any blazar the synchrotron power is observed to peak at hard X-ray energies. The large shift of the synchrotron peak frequency with respect to previous observations of Mkn 501 implies that intrinsic changes in the relativistic electron spectrum caused the increase in emitted power. Due to the very high electron energies, the inverse Compton process is limited by the Klein-Nishina regime. This implies a quasi-linear (as opposed to quadratic) relation of the variability amplitude in the TeV and hard X-ray ranges (for the SSC model) and an increase of the inverse Compton peak frequency smaller than that of the synchrotron peak frequency., 11 pages, Latex, 4 Postscript figures, to appear in The Astrophysical Journal Letters
- Published
- 1997
40. Multiwavelength Monitoring of the BL Lacertae Object PKS 2155-304 in May 1994. II. The IUE Campaign
- Author
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Pian, Elena, Urry, C. Megan, Treves, Aldo, Maraschi, Laura, Penton, Steve, Shull, J. Michael, Pesce, Joseph E., Grandi, Paola, Kii, Tsuneo, Kollgaard, Ron I., Madejski, Greg, Marshall, Herman, Wamsteker, Willem, Celotti, Annalisa, Courvoisier, Thierry J. -L., Falomo, Renato, Fink, Henner H., George, Ian M., and Ghisellini, Gabriele
- Subjects
Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics - Abstract
PKS 2155-304, the brightest BL Lac object in the ultraviolet sky, was monitored with the IUE satellite at ~1 hour time-resolution for ten nearly uninterrupted days in May 1994. The campaign, which was coordinated with EUVE, ROSAT, and ASCA monitoring, along with optical and radio observations from the ground, yielded the largest set of spectra and the richest short time scale variability information ever gathered for a blazar at UV wavelengths. The source flared dramatically during the first day, with an increase by a factor ~2.2 in an hour and a half. In subsequent days, the flux maintained a nearly constant level for ~5 days, then flared with ~35% amplitude for two days. The same variability was seen in both short- and long-wavelength IUE light curves, with zero formal lag (~, 45 pages, Latex, 11 PostScript figures, to appear in The Astrophysical Journal
- Published
- 1997
41. Multiwavelength Monitoring of the BL Lacertae Object PKS 2155-304 in May 1994. III. Probing the Inner Jet through Multiwavelength Correlations
- Author
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Urry, C. Megan, Treves, Aldo, Maraschi, Laura, Marshall, Herman L., Madejski, Greg, Penton, Steve, Pesce, Joseph E., Pian, Elena, Celotti, Annalisa, Sambruna, R. M., Shull, J. M., Smith, Paul S., Kii, Tsuneo, Fujimoto, Ryuichi, Makino, Fumiyoshi, Otani, Chiko, Sasaki, Koichi, Takahashi, Tadayuki, and Tashiro, M.
- Subjects
PKS 2155-304 ,Physics ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astronomy and Astrophysics ,Astrophysics ,Light curve ,law.invention ,Wavelength ,Amplitude ,Space and Planetary Science ,law ,ROSAT ,Astrophysics::Solar and Stellar Astrophysics ,Blazar ,BL Lac object ,Flare - Abstract
著者人数:19名, Accepted: 1997-04-21, 資料番号: SA1002215000
- Published
- 1997
42. Subaru spectropolarimetry of supernovae.
- Author
-
Tanaka, Masaomi, Kawabata, Koji S., Hattori, Takashi, Aoki, Kentaro, Iye, Masanori, Maeda, Keiichi, Mazzali, Paolo A., Nomoto, Ken'ichi, Pian, Elena, Sasaki, Toshiyuki, and Yamanaka, Masayuki
- Subjects
ASTROPHYSICAL spectropolarimetry ,SUPERNOVAE ,ASTRONOMICAL observations ,TELESCOPES ,SIMULATION methods & models ,RADIATIVE transfer ,COMPARATIVE studies - Abstract
Spectropolarimetry is one of the most powerful methods to study the multi-dimensional geometry of extragalactic supernovae (SNe). We have performed spectropolarimetric observations of Type Ib/c SNe with the Subaru telescope. The data clearly show the "loop" in the Stokes Q - U plane. By performing 3D radiative transfer simulations, we show that the loop is clear evidence for 3D, non-axisymmetric geometry of SNe. We also summarize the properties of the line polarization of Type Ib/c SNe. We find that a stronger line tends to show a higher line polarization. This effect must be corrected to compare the polarization of different lines or different objects. [ABSTRACT FROM AUTHOR]
- Published
- 2012
- Full Text
- View/download PDF
43. Optical Afterglows of Gamma-Ray Bursts.
- Author
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Pian, Elena
- Subjects
- *
AFTERGLOW (Physics) , *GAMMA ray bursts , *TELESCOPES , *REDSHIFT , *EXPLOSIONS , *SUPERNOVAE - Abstract
The advent of the Swift mission for Gamma-Ray Bursts (GRBs) in late 2004 has more than doubled the existing sample of detected optical counterparts. The rapid dissemination of the accurate BAT and XRT localizations has allowed ground-based telescopes, especially the automatic ones, to slew timely to the GRB positions and to scan them efficiently in search of an afterglow. For about 25% of the Swift GRBs, the onboard UVOT instrument has also provided an early counterpart detection in the optical, and occasionally in the near-UV. There are now about 200 detected GRB optical afterglows, of which nearly 100 have a redshift measurement. I will review here some of the highlights in this field during the Swift era, with particular emphasis on the early (minutes to hours after explosion) optical light curves, on the afterglows of short GRBs, and on the supernova-GRB connection. [ABSTRACT FROM AUTHOR]
- Published
- 2007
- Full Text
- View/download PDF
44. Using the Interplanetary Network to Search for SN Ic/GRB Coincidences.
- Author
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Hurley, Kevin and Pian, Elena
- Subjects
- *
GAMMA ray bursts , *ASTRONOMICAL observations , *GAMMA rays , *TYPE I supernovae , *INTERPLANETARY dust , *EMISSIONS (Air pollution) - Abstract
We describe a systematic search, still in progress, for gamma-ray bursts associated with optically identified energetic supernovae. The results (negative so far) can be explained in various ways. It is possible that not all energetic Type Ic supernovae produce gamma-ray bursts. If they do, though, our non-detections can be explained by beaming, soft energy spectra, weak gamma-ray emission, or a combination of these effects. [ABSTRACT FROM AUTHOR]
- Published
- 2007
- Full Text
- View/download PDF
45. Optical observations of GRB 060218/SN 2006aj and its host galaxy.
- Author
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Ferrero, Patrizia, Palazzi, Eliana, Pian, Elena, and Savaglio, Sandra
- Subjects
SPECTRUM analysis ,OPTICAL spectroscopy ,GALAXIES ,STAR formation ,DWARF galaxies - Abstract
The supernova SN 2006aj associated with GRB 060218 is the second-closest GRB-SN observed to date (z=0.033) and is the clearest example of a SN associated with a Swift GRB with the earliest optical spectroscopy. Its optical data showed that this is the fastest evolving and among the least luminous GRB-SNe (70% as luminous as SN1998bw). However, its expansion velocity and a comparison with other stripped-envelope SNe suggest that SN2006aj is an intermediate object between Type Ic GRB-SNe and those not accompained by a GRB. High-resolution optical spectroscopy together with SDSS pre-burst observations revealed that the host galaxy of SN2006aj is a low-luminosity, metal-poor star-forming dwarf galaxy. © 2007 American Institute of Physics [ABSTRACT FROM AUTHOR]
- Published
- 2007
- Full Text
- View/download PDF
46. The REM optical slitless spectrograph (ROSS).
- Author
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Tosti, Gino, Bagaglia, Marco, Campeggi, Carlo, Masetti, Nicola, Monfardini, Alessandro, Nicastro, Luciano, Palazzi, Eliana, Pian, Elena, Sciuto, Giorgio, Zerbi, Filippo M., Chincarini, Guido, Antonelli, Lucio A., Conconi, Paolo, Covino, Stefano, Cutispoto, Giuseppe, Rodono, Marcello, and Molinari, Emilio
- Published
- 2004
- Full Text
- View/download PDF
47. BeppoSAX spectra of five low mass X-ray binaries.
- Author
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Masetti, Nicola, Pian, Elena, Frontera, Filippo, Palazzi, Eliana, Amati, Lorenzo, Orlandini, Mauro, and Dal Fiume, Daniele
- Subjects
- *
X-ray binaries , *SPECTRUM analysis , *ARTIFICIAL satellites - Abstract
Observations of five Low Mass X-ray Binaries (LMXBs) were performed with BeppoSAX in order to investigate emission processes in LMXBs in a wide X-ray energy range and understand the crucial spectral characteristics of compact stellar systems harbouring neutron stars. We find that two thermal components are present in the spectra of both faint and bright LMXBs and that the high energy spectra of the observed LMXBs are systematically softer than those of black hole candidates. We also detect an iron emission line around 6.5 keV in bright LMXBs. [ABSTRACT FROM AUTHOR]
- Published
- 2001
48. GRB 081007 AND GRB 090424: THE SURROUNDING MEDIUM, OUTFLOWS, AND SUPERNOVAE.
- Author
-
ZHI-PING JIN, COVINO, STEFANO, VALLE, MASSIMO DELLA, FERRERO, PATRIZIA, FUGAZZA, DINO, MALESANI, DANIELE, MELANDRI, ANDREA, PIAN, ELENA, SALVATERRA, RUBEN, BERSIER, DAVID, CAMPANA, SERGIO, CANO, ZACH, CASTRO-TIRADO, ALBERTO J., D'AVANZO, PAOLO, FYNBO, JOHAN P. U., GOMBOC, ANDREJA, GOROSABEL, JAVIER, GUIDORZI, CRISTIANO, HAISLIP, JOSHUA B., and HJORTH, JENS
- Subjects
SUPERNOVAE ,SUPERNOVA remnants ,ENERGY dissipation ,SPECTROMETRY ,WAVELENGTHS - Abstract
We discuss the results of the analysis of multi-wavelength data for the afterglows of GRB 081007 and GRB 090424, two bursts detected by Swift. One of them, GRB 081007, also shows a spectroscopically confirmed supernova, SN 2008hw, which resembles SN 1998bw in its absorption features, while the maximum magnitude may be fainter, up to 0.7 mag, than observed in SN 1998bw. Bright optical flashes have been detected in both events, which allows us to derive solid constraints on the circumburst-matter density profile. This is particularly interesting in the case of GRB 081007, whose afterglow is found to be propagating into a constant-density medium, yielding yet another example of a gamma-ray burst (GRB) clearly associated with a massive-star progenitor which did not sculpt the surroundings with its stellar wind. There is no supernova component detected in the afterglow of GRB 090424, likely due to the brightness of the host galaxy, comparable to the Milky Way. We show that the afterglow data are consistent with the presence of both forward- and reverse-shock emission powered by relativistic outflows expanding into the interstellar medium. The absence of optical peaks due to the forward shock strongly suggests that the reverse-shock regions should be mildly magnetized. The initial Lorentz factor of outflow of GRB 081007 is estimated to be Γ ~ 200, while for GRB 090424 a lower limit of Γ > 170 is derived.We also discuss the prompt emission of GRB 081007, which consists of just a single pulse. We argue that neither the external forward-shock model nor the shock-breakout model can account for the prompt emission data and suggest that the single-pulse-like prompt emission may be due to magnetic energy dissipation of a Poynting-flux-dominated outflow or to a dissipative photosphere. [ABSTRACT FROM AUTHOR]
- Published
- 2013
- Full Text
- View/download PDF
49. MULTI-WAVELENGTH OBSERVATIONS OF SUPERNOVA 2011ei: TIME-DEPENDENT CLASSIFICATION OF TYPE IIb AND Ib SUPERNOVAE AND IMPLICATIONS FOR THEIR PROGENITORS.
- Author
-
MILISAVLJEVIC, DAN, MARGUTTI, RAFFAELLA, SODERBERG, ALICIA M., PIGNATA, GIULIANO, CHOMIUK, LAURA, FESEN, ROBERT A., BUFANO, FILOMENA, SANDERS, NATHAN E., PARRENT, JEROD T., PARKER, STUART, MAZZALI, PAOLO, PIAN, ELENA, PICKERING, TIMOTHY, BUCKLEY, DAVID A. H., CRAWFORD, STEVEN M., GULBIS, AMANDA A. S., HETTLAGE, CHRISTIAN, HOOPER, ERIC, NORDSIECK, KENNETH H., and O'DONOGHUE, DARRAGH
- Subjects
TYPE II supernovae ,STELLAR evolution ,X-rays ,WAVELENGTHS ,OPTICAL spectra - Abstract
We present X-ray, UV/optical, and radio observations of the stripped-envelope, core-collapse supernova (SN) 2011ei, one of the least luminous SNe IIb or Ib observed to date. Our observations begin with a discovery within ~1 day of explosion and span several months afterward. Early optical spectra exhibit broad, Type II-like hydrogen Balmer profiles that subside rapidly and are replaced by Type Ib-like He-rich features on a timescale of one week. High-cadence monitoring of this transition suggests absorption attributable to a high-velocity (≳12,000 km s
-1 ) H-rich shell, which is likely present in many Type Ib events. Radio observations imply a shock velocity of v ≈ 0.13 c and a progenitor star average mass-loss rate of M ≈ 1.4 × 10-5 M☉ yr-1 (assuming wind velocity vw = 103 km s-1 ). This is consistent with independent constraints from deep X-ray observations with Swift-XRT and Chandra. Overall, the multi-wavelength properties of SN 2011ei are consistent with the explosion of a lowermass (3-4 M☉), compact (R" ≲ 1 × 1011 cm), He-core star. The star retained a thin hydrogen envelope at the time of explosion, and was embedded in an inhomogeneous circumstellar wind suggestive of modest episodic mass loss. We conclude that SN 2011ei's rapid spectral metamorphosis is indicative of time-dependent classifications that bias estimates of the relative explosion rates for Type IIb and Ib objects, and that important information about a progenitor star's evolutionary state and mass loss immediately prior to SN explosion can be inferred from timely multi-wavelength observations. [ABSTRACT FROM AUTHOR]- Published
- 2013
- Full Text
- View/download PDF
50. DISCOVERY AND EARLY MULTI-WAVELENGTH MEASUREMENTS OF THE ENERGETIC TYPE IC SUPERNOVA PTF12GZK: A MASSIVE-STAR EXPLOSION IN A DWARF HOST GALAXY.
- Author
-
BEN-AMI, SAGI, GAL-YAM, AVISHAY, FILIPPENKO, ALEXEI V., MAZZALI, PAOLO A., MODJAZ, MARYAM, YARON, OFER, ARCAVI, IAIR, CENKO, S. BRADLEY, HORESH, ASSAF, HOWELL, D. ANDREW, GRAHAM, MELISSA L., HORST, J. CHUCK, MYUNSHIN IM, YISEUL JEON, KULKARNI, SHRINIVAS R., LEONARD, DOUGLAS C., PERLEY, DANIEL, PIAN, ELENA, SAND, DAVID J., and SULLIVAN, MARK
- Published
- 2012
- Full Text
- View/download PDF
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