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112 results on '"Assaf Horesh"'

101. IPTF14yb: The first discovery of a gamma-ray burst afterglow independent of a high-energy trigger

Author

S. Bradley Cenko, Alex L. Urban, Daniel A. Perley, Assaf Horesh, Alessandra Corsi, Derek B. Fox, Yi Cao, Mansi M. Kasliwal, Amy Lien, Iair Arcavi, Joshua S. Bloom, Nat R. Butler, Antonino Cucchiara, José A. de Diego, Alexei V. Filippenko, Avishay Gal-Yam, Neil Gehrels, Leonid Georgiev, J. Jesús González, John F. Graham, Jochen Greiner, D. Alexander Kann, Christopher R. Klein, Fabian Knust, S. R. Kulkarni, Alexander Kutyrev, Russ Laher, William H. Lee, Peter E. Nugent, J. Xavier Prochaska, Enrico Ramirez-Ruiz, Michael G. Richer, Adam Rubin, Yuji Urata, Karla Varela, Alan M. Watson, and Przemek R. Wozniak

Subjects
Swift Gamma-Ray Burst Mission, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, general [gamma-ray burst], Astronomy & Astrophysics, 01 natural sciences, Affordable and Clean Energy, 0103 physical sciences, education, 010303 astronomy & astrophysics, QC, QB, Physics, astro-ph.HE, education.field_of_study, 010308 nuclear & particles physics, Astronomy and Astrophysics, Redshift, Afterglow, 13. Climate action, Space and Planetary Science, flare [stars], Gamma-ray burst, general [supernovae], Energy (signal processing), Astronomical and Space Sciences
Abstract

We report here the discovery by the Intermediate Palomar Transient Factory (iPTF) of iPTF14yb, a luminous(Mr ≈ -27.8 mag), cosmological (redshift 1.9733), rapidly fading optical transient. We demonstrate, based onprobabilistic arguments and a comparison with the broader population, that iPTF14yb is the optical afterglow ofthe long-duration gamma-ray burst GRB 140226A. This marks the first unambiguous discovery of a GRBafterglow prior to (and thus entirely independent of) an associated high-energy trigger. We estimate the rate ofiPTF14yb-like sources (i.e., cosmologically distant relativistic explosions) based on iPTF observations, inferringan all-sky value of Rrel = 610 yr?1 (68% confidence interval of 1102000 yr?1). Our derived rate is consistent(within the large uncertainty) with the all-sky rate of on-axis GRBs derived by the Swift satellite. Finally, webriefly discuss the implications of the nondetection to date of bona fide orphan afterglows (i.e., those lackingdetectable high-energy emission) on GRB beaming and the degree of baryon loading in these relativistic jets. © 2015. The American Astronomical Society. All rights reserved.

102. Is supernova SN 2020faa an iPTF14hls look-alike?

Author

Shan Yang, P. E. Nugent, Nora L. Strotjohann, Assaf Horesh, Ragnhild Lunnan, Mansi M. Kasliwal, Frank J. Masci, E. C. Kool, Thomas Kupfer, Reed Riddle, Daniel A. Perley, Jesper Sollerman, A. A. Mahabal, B. Rusholme, Steve Schulze, Tao Chen, and Y. Sharma

Subjects
FOS: Physical sciences, Context (language use), Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Luminosity, Spectral evolution, 0103 physical sciences, 010303 astronomy & astrophysics, QC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, individual: ZTF20aatqesi [supernovae], individual: iPTF14hls [supernovae], 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Light curve, Type II supernova, Optical spectra, individual: SN 2020faa [supernovae], Supernova, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, general [supernovae], Astronomical and Space Sciences
Abstract

We present observations of SN 2020faa. This Type II supernova displays a luminous light curve that started to rebrighten from an initial decline. We investigate this in relation to the famous supernova iPTF14hls, which received a lot of attention and multiple interpretations in the literature, however whose nature and source of energy still remains unknown. We demonstrate the great similarity between SN 2020faa and iPTF14hls during the first 6 months, and use this comparison both to forecast the evolution of SN 2020faa and to reflect on the less well observed early evolution of iPTF14hls. We present and analyse our observational data, consisting mainly of optical light curves from the Zwicky Transient Facility in the gri bands as well as a sequence of optical spectra. We construct colour curves, a bolometric light curve, compare ejecta-velocity and Black-body radius evolutions for the two supernovae, as well as for more typical Type II supernovae. The light curves show a great similarity with those of iPTF14hls over the first 6 months, in luminosity, timescale and colours. Also the spectral evolution of SN 2020faa is that of a Type II supernova, although it probes earlier epochs than those available for iPTF14hls. The similar light curve behaviour is suggestive of SN 2020faa being a new iPTF14hls. We present these observations now to advocate follow-up observations, since most of the more striking evolution of supernova iPTF14hls came later, with light curve undulations and a spectacular longevity. On the other hand, for SN 2020faa we have better constraints on the explosion epoch than we had for iPTF14hls, and we have been able to spectroscopically monitor it from earlier phases than was done for the more famous sibling., Comment: 14 pages, 12 figures, submitted to A&A

103. GRB 160625B: Evidence for a Gaussian-shaped Jet

Author

Antonino Cucchiara, Judith Racusin, S. Bradley Cenko, Geoffrey Ryan, Stuart N. Vogel, Andrew S. Fruchter, Alessandra Corsi, Virginia Cunningham, Daniel A. Perley, Tuomas Kangas, Assaf Horesh, and Daniel Kocevski

Subjects
010504 meteorology & atmospheric sciences, Gaussian, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, symbols.namesake, Astrophysical jet, 0103 physical sciences, 010303 astronomy & astrophysics, QC, 0105 earth and related environmental sciences, QB, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), Astronomy and Astrophysics, Markov chain Monte Carlo, Viewing angle, Afterglow, Space and Planetary Science, symbols, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Order of magnitude
Abstract

We present multiwavelength modeling of the afterglow from the long gamma-ray burst GRB 160625B using Markov Chain Monte Carlo (MCMC) techniques of the afterglowpy Python package. GRB 160625B is an extremely bright burst with a rich set of observations spanning from radio to gamma-ray frequencies. These observations range from ~0.1 days to >1000 days, thus making this event extremely well-suited to such modeling. In this work we compare top-hat and Gaussian jet structure types in order to find best fit values for the GRB jet collimation angle, viewing angle, and other physical parameters. We find that a Gaussian-shaped jet is preferred (2.7-5.3 sigma) over the traditional top-hat model. Our estimate for the opening angle of the burst ranges from 1.26 to 3.90 degrees, depending on jet shape model. We also discuss the implications that assumptions on jet shape, viewing angle, and particularly the participation fraction of electrons have on the final estimation of GRB intrinsic energy release and the resulting energy budget of the relativistic outflow. Most notably, allowing the participation fraction to vary results in an estimated total relativistic energy of ~$10^{53}$ erg. This is two orders of magnitude higher than when the total fraction is assumed to be unity, thus this parameter has strong relevance for placing constraints on long GRB central engines, details of the circumburst media, and host environment., 29 pages, 10 figures, accepted by ApJ

104. SPIRITS 16tn in NGC 3556: A Heavily Obscured and Low-luminosity Supernova at 8.8 Mpc.

Author

Jacob E. Jencson, Mansi M. Kasliwal, Scott M. Adams, Howard E. Bond, Ryan M. Lau, Joel Johansson, Assaf Horesh, Kunal P. Mooley, Robert Fender, Kishalay De, Dónal O’Sullivan, Frank J. Masci, Ann Marie Cody, Nadia Blagorodnova, Ori D. Fox, Robert D. Gehrz, Peter A. Milne, Daniel A. Perley, Nathan Smith, and Schuyler D. Van Dyk

Subjects
LUMINOSITY, SUPERNOVAE, LIGHT curves, STAR formation, DISKS (Astrophysics), INFRARED spectroscopy
Abstract

We present the discovery by the SPitzer InfraRed Intensive Transients Survey (SPIRITS) of a likely supernova (SN) in NGC 3556 (M108) at only 8.8 Mpc that was not detected by optical searches. A luminous infrared (IR) transient at M[4.5] = −16.7 mag (Vega), SPIRITS 16tn is coincident with a dust lane in the inclined, star-forming disk of the host. Using observations in the IR, optical, and radio, we attempt to determine the nature of this event. We estimate AV ≈ 8–9 mag of extinction, placing it among the three most highly obscured IR-discovered SNe. The [4.5] light curve declined at a rate of 0.013 mag day−1, and the [3.6]–[4.5] color increased from 0.7 to ≳1.0 mag by 184.7 days post discovery. Optical/IR spectroscopy shows a red continuum but no clearly discernible features, preventing a definitive spectroscopic classification. Radio observations constrain the radio luminosity of SPIRITS 16tn to Lν ≲ 1024 erg s−1 Hz−1 between 3 and 15 GHz, excluding many varieties of core-collapse SNe. An SN Ia is ruled out by the observed IR color and lack of spectroscopic features from Fe-peak elements. SPIRITS 16tn was fainter at [4.5] than typical stripped-envelope SNe by ≈1 mag. Comparison of the spectral energy distribution to SNe II suggests that SPIRITS 16tn was both highly obscured and intrinsically dim, possibly akin to the low-luminosity SN 2005cs. We infer the presence of an IR dust echo powered by an initial peak luminosity of the transient of 5 × 1040 erg s−1 ≲ Lpeak ≲ 4 × 1043 erg s−1, consistent with the observed range for SNe II. This discovery illustrates the power of IR surveys to overcome the compounding effects of visible extinction and optically subluminous events in completing the inventory of nearby SNe. [ABSTRACT FROM AUTHOR]

Published
2018
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105. Black holes, gravitational waves and fundamental physics: a roadmap

Author

Leor Barack, Vitor Cardoso, Samaya Nissanke, Thomas P Sotiriou, Abbas Askar, Chris Belczynski, Gianfranco Bertone, Edi Bon, Diego Blas, Richard Brito, Tomasz Bulik, Clare Burrage, Christian T Byrnes, Chiara Caprini, Masha Chernyakova, Piotr Chruściel, Monica Colpi, Valeria Ferrari, Daniele Gaggero, Jonathan Gair, Juan García-Bellido, S F Hassan, Lavinia Heisenberg, Martin Hendry, Ik Siong Heng, Carlos Herdeiro, Tanja Hinderer, Assaf Horesh, Bradley J Kavanagh, Bence Kocsis, Michael Kramer, Alexandre Le Tiec, Chiara Mingarelli, Germano Nardini, Gijs Nelemans, Carlos Palenzuela, Paolo Pani, Albino Perego, Edward K Porter, Elena M Rossi, Patricia Schmidt, Alberto Sesana, Ulrich Sperhake, Antonio Stamerra, Leo C Stein, Nicola Tamanini, Thomas M Tauris, L Arturo Urena-López, Frederic Vincent, Marta Volonteri, Barry Wardell, Norbert Wex, Kent Yagi, Tiziano Abdelsalhin, Miguel Ángel Aloy, Pau Amaro-Seoane, Lorenzo Annulli, Manuel Arca-Sedda, Ibrahima Bah, Enrico Barausse, Elvis Barakovic, Robert Benkel, Charles L Bennett, Laura Bernard, Sebastiano Bernuzzi, Christopher P L Berry, Emanuele Berti, Miguel Bezares, Jose Juan Blanco-Pillado, Jose Luis Blázquez-Salcedo, Matteo Bonetti, Mateja Bošković, Zeljka Bosnjak, Katja Bricman, Bernd Brügmann, Pedro R Capelo, Sante Carloni, Pablo Cerdá-Durán, Christos Charmousis, Sylvain Chaty, Aurora Clerici, Andrew Coates, Marta Colleoni, Lucas G Collodel, Geoffrey Compère, William Cook, Isabel Cordero-Carrión, Miguel Correia, Álvaro de la Cruz-Dombriz, Viktor G Czinner, Kyriakos Destounis, Kostas Dialektopoulos, Daniela Doneva, Massimo Dotti, Amelia Drew, Christopher Eckner, James Edholm, Roberto Emparan, Recai Erdem, Miguel Ferreira, Pedro G Ferreira, Andrew Finch, Jose A Font, Nicola Franchini, Kwinten Fransen, Dmitry Gal’tsov, Apratim Ganguly, Davide Gerosa, Kostas Glampedakis, Andreja Gomboc, Ariel Goobar, Leonardo Gualtieri, Eduardo Guendelman, Francesco Haardt, Troels Harmark, Filip Hejda, Thomas Hertog, Seth Hopper, Sascha Husa, Nada Ihanec, Taishi Ikeda, Amruta Jaodand, Philippe Jetzer, Xisco Jimenez-Forteza, Marc Kamionkowski, David E Kaplan, Stelios Kazantzidis, Masashi Kimura, Shiho Kobayashi, Kostas Kokkotas, Julian Krolik, Jutta Kunz, Claus Lämmerzahl, Paul Lasky, José P S Lemos, Jackson Levi Said, Stefano Liberati, Jorge Lopes, Raimon Luna, Yin-Zhe Ma, Elisa Maggio, Alberto Mangiagli, Marina Martinez Montero, Andrea Maselli, Lucio Mayer, Anupam Mazumdar, Christopher Messenger, Brice Ménard, Masato Minamitsuji, Christopher J Moore, David Mota, Sourabh Nampalliwar, Andrea Nerozzi, David Nichols, Emil Nissimov, Martin Obergaulinger, Niels A Obers, Roberto Oliveri, George Pappas, Vedad Pasic, Hiranya Peiris, Tanja Petrushevska, Denis Pollney, Geraint Pratten, Nemanja Rakic, Istvan Racz, Miren Radia, Fethi M Ramazanoğlu, Antoni Ramos-Buades, Guilherme Raposo, Marek Rogatko, Roxana Rosca-Mead, Dorota Rosinska, Stephan Rosswog, Ester Ruiz-Morales, Mairi Sakellariadou, Nicolás Sanchis-Gual, Om Sharan Salafia, Anuradha Samajdar, Alicia Sintes, Majda Smole, Carlos Sopuerta, Rafael Souza-Lima, Marko Stalevski, Nikolaos Stergioulas, Chris Stevens, Tomas Tamfal, Alejandro Torres-Forné, Sergey Tsygankov, Kıvanç İ Ünlütürk, Rosa Valiante, Maarten van de Meent, José Velhinho, Yosef Verbin, Bert Vercnocke, Daniele Vernieri, Rodrigo Vicente, Vincenzo Vitagliano, Amanda Weltman, Bernard Whiting, Andrew Williamson, Helvi Witek, Aneta Wojnar, Kadri Yakut, Haopeng Yan, Stoycho Yazadjiev, Gabrijela Zaharijas, Miguel Zilhão, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut des Hautes Etudes Scientifiques (IHES), IHES, Laboratoire Univers et Théories (LUTH (UMR_8102)), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut des Hautes Études Scientifiques (IHES), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Barack, L., Cardoso, V., Nissanke, S., Sotiriou, T. P., Askar, A., Belczynski, C., Bertone, G., Bon, E., Blas, D., Brito, R., Bulik, T., Burrage, C., Byrnes, C. T., Caprini, C., Chernyakova, M., Chrusciel, P., Colpi, M., Ferrari, V., Gaggero, D., Gair, J., Garcia-Bellido, J., Hassan, S. F., Heisenberg, L., Hendry, M., Heng, I. S., Herdeiro, C., Hinderer, T., Horesh, A., Kavanagh, B. J., Kocsis, B., Kramer, M., Le Tiec, A., Mingarelli, C., Nardini, G., Nelemans, G., Palenzuela, C., Pani, P., Perego, A., Porter, E. K., Rossi, E. M., Schmidt, P., Sesana, A., Sperhake, U., Stamerra, A., Stein, L. C., Tamanini, N., Tauris, T. M., Urena-Lopez, L. A., Vincent, F., Volonteri, M., Wardell, B., Wex, N., Yagi, K., Abdelsalhin, T., Aloy, M. A., Amaro-Seoane, P., Annulli, L., Arca-Sedda, M., Bah, I., Barausse, E., Barakovic, E., Benkel, R., Bennett, C. L., Bernard, L., Bernuzzi, S., Berry, C. P. L., Berti, E., Bezares, M., Blanco-Pillado, J. J., Blazquez-Salcedo, J. L., Bonetti, M., Boskovic, M., Bosnjak, Z., Bricman, K., Brugmann, B., Capelo, P. R., Carloni, S., Cerda-Duran, P., Charmousis, C., Chaty, S., Clerici, A., Coates, A., Colleoni, M., Collodel, L. G., Compere, G., Cook, W., Cordero-Carrion, I., Correia, M., De La Cruz-Dombriz, A., Czinner, V. G., Destounis, K., Dialektopoulos, K., Doneva, D., Dotti, M., Drew, A., Eckner, C., Edholm, J., Emparan, R., Erdem, R., Ferreira, M., Ferreira, P. G., Finch, A., Font, J. A., Franchini, N., Fransen, K., Gal'Tsov, D., Ganguly, A., Gerosa, D., Glampedakis, K., Gomboc, A., Goobar, A., Gualtieri, L., Guendelman, E., Haardt, F., Harmark, T., Hejda, F., Hertog, T., Hopper, S., Husa, S., Ihanec, N., Ikeda, T., Jaodand, A., Jetzer, P., Jimenez-Forteza, X., Kamionkowski, M., Kaplan, D. E., Kazantzidis, S., Kimura, M., Kobayashi, S., Kokkotas, K., Krolik, J., Kunz, J., Lammerzahl, C., Lasky, P., Lemos, J. P. S., Levi Said, J., Liberati, S., Lopes, J., Luna, R., Ma, Y. -Z., Maggio, E., Mangiagli, A., Montero, M. M., Maselli, A., Mayer, L., Mazumdar, A., Messenger, C., Menard, B., Minamitsuji, M., Moore, C. J., Mota, D., Nampalliwar, S., Nerozzi, A., Nichols, D., Nissimov, E., Obergaulinger, M., Obers, N. A., Oliveri, R., Pappas, G., Pasic, V., Peiris, H., Petrushevska, T., Pollney, D., Pratten, G., Rakic, N., Racz, I., Radia, M., Ramazanoglu, F. M., Ramos-Buades, A., Raposo, G., Rogatko, M., Rosca-Mead, R., Rosinska, D., Rosswog, S., Ruiz-Morales, E., Sakellariadou, M., Sanchis-Gual, N., Sharan Salafia, O., Samajdar, A., Sintes, A., Smole, M., Sopuerta, C., Souza-Lima, R., Stalevski, M., Stergioulas, N., Stevens, C., Tamfal, T., Torres-Forne, A., Tsygankov, S., I Unluturk, Ki., Valiante, R., Van De Meent, M., Velhinho, J., Verbin, Y., Vercnocke, B., Vernieri, D., Vicente, R., Vitagliano, V., Weltman, A., Whiting, B., Williamson, A., Witek, H., Wojnar, A., Yakut, K., Yan, H., Yazadjiev, S., Zaharijas, G., Zilhao, M., Gravitation and Astroparticle Physics Amsterdam, GRAPPA (ITFA, IoP, FNWI), IoP (FNWI), High Energy Astrophys. & Astropart. Phys (API, FNWI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Sperhake, Ulrich [0000-0002-3134-7088], Drew, Amelia [0000-0001-8252-602X], Radia, Miren [0000-0001-8861-2025], Apollo - University of Cambridge Repository, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Ege Üniversitesi, Barack, L, Cardoso, V, Nissanke, S, Sotiriou, T, Askar, A, Belczynski, C, Bertone, G, Bon, E, Blas, D, Brito, R, Bulik, T, Burrage, C, Byrnes, C, Caprini, C, Chernyakova, M, Chruściel, P, Colpi, M, Ferrari, V, Gaggero, D, Gair, J, García-Bellido, J, Hassan, S, Heisenberg, L, Hendry, M, Heng, I, Herdeiro, C, Hinderer, T, Horesh, A, Kavanagh, B, Kocsis, B, Kramer, M, Le Tiec, A, Mingarelli, C, Nardini, G, Nelemans, G, Palenzuela, C, Pani, P, Perego, A, Porter, E, Rossi, E, Schmidt, P, Sesana, A, Sperhake, U, Stamerra, A, Stein, L, Tamanini, N, Tauris, T, Urena-López, L, Vincent, F, Volonteri, M, Wardell, B, Wex, N, Yagi, K, Abdelsalhin, T, Aloy, M, Amaro-Seoane, P, Annulli, L, Arca-Sedda, M, Bah, I, Barausse, E, Barakovic, E, Benkel, R, Bennett, C, Bernard, L, Bernuzzi, S, Berry, C, Berti, E, Bezares, M, Blanco-Pillado, J, Blázquez-Salcedo, J, Bonetti, M, Bošković, M, Bosnjak, Z, Bricman, K, Brügmann, B, Capelo, P, Carloni, S, Cerdá-Durán, P, Charmousis, C, Chaty, S, Clerici, A, Coates, A, Colleoni, M, Collodel, L, Compère, G, Cook, W, Cordero-Carrión, I, Correia, M, de la Cruz-Dombriz, Á, Czinner, V, Destounis, K, Dialektopoulos, K, Doneva, D, Dotti, M, Drew, A, Eckner, C, Edholm, J, Emparan, R, Erdem, R, Ferreira, M, Ferreira, P, Finch, A, Font, J, Franchini, N, Fransen, K, Gal’Tsov, D, Ganguly, A, Gerosa, D, Glampedakis, K, Gomboc, A, Goobar, A, Gualtieri, L, Guendelman, E, Haardt, F, Harmark, T, Hejda, F, Hertog, T, Hopper, S, Husa, S, Ihanec, N, Ikeda, T, Jaodand, A, Jetzer, P, Jimenez-Forteza, X, Kamionkowski, M, Kaplan, D, Kazantzidis, S, Kimura, M, Kobayashi, S, Kokkotas, K, Krolik, J, Kunz, J, Lämmerzahl, C, Lasky, P, Lemos, J, Levi Said, J, Liberati, S, Lopes, J, Luna, R, Ma, Y, Maggio, E, Mangiagli, A, Montero, M, Maselli, A, Mayer, L, Mazumdar, A, Messenger, C, Ménard, B, Minamitsuji, M, Moore, C, Mota, D, Nampalliwar, S, Nerozzi, A, Nichols, D, Nissimov, E, Obergaulinger, M, Obers, N, Oliveri, R, Pappas, G, Pasic, V, Peiris, H, Petrushevska, T, Pollney, D, Pratten, G, Rakic, N, Racz, I, Radia, M, Ramazanoğlu, F, Ramos-Buades, A, Raposo, G, Rogatko, M, Rosca-Mead, R, Rosinska, D, Rosswog, S, Ruiz-Morales, E, Sakellariadou, M, Sanchis-Gual, N, Sharan Salafia, O, Samajdar, A, Sintes, A, Smole, M, Sopuerta, C, Souza-Lima, R, Stalevski, M, Stergioulas, N, Stevens, C, Tamfal, T, Torres-Forné, A, Tsygankov, S, İ Ünlütürk, K, Valiante, R, van de Meent, M, Velhinho, J, Verbin, Y, Vercnocke, B, Vernieri, D, Vicente, R, Vitagliano, V, Weltman, A, Whiting, B, Williamson, A, Witek, H, Wojnar, A, Yakut, K, Yan, H, Yazadjiev, S, Zaharijas, G, and Zilhão, M

Subjects
High Energy Physics - Theory, cosmological model, Physics and Astronomy (miscellaneous), Event horizon, Astronomy, 01 natural sciences, General Relativity and Quantum Cosmology, Cosmology, Physics, Particles & Fields, Gravitation, High Energy Physics::Theory, black hole: formation, Vacuum energy, black hole, general relativity, NEUTRON-STAR, GENERAL-RELATIVITY, dark energy, STAR CLUSTER SIMULATIONS, gravitational wave, QC, QB, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, Quantum Science & Technology, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, source modelling, BRANS-DICKE THEORY, fundamental physic, gravitational waves, QUASI-NORMAL MODES, Physical Sciences, birth and evolution of black holes, black holes, fundamental physics, gravitational-wave astronomy, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], HIGH-REDSHIFT FORMATION, Astrophysics - High Energy Astrophysical Phenomena, SCALAR-TENSOR THEORIES, General relativity, media_common.quotation_subject, gr-qc, Physics, Multidisciplinary, birth and evolution of black hole, FOS: Physical sciences, ST/R00045X/1, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, gravitational radiation: direct detection, horizon, vacuum state: energy, Theoretical physics, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, inflation, 010306 general physics, STFC, Science & Technology, 010308 nuclear & particles physics, Gravitational wave, Physique, gravitational radiation, RCUK, ST/P000703/1, R-PROCESS NUCLEOSYNTHESIS, Astronomie, singularity, Universe, High Energy Physics - Theory (hep-th), gravitation, black hole: model, TIMING ARRAY LIMITS, Dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], X-RAY BINARIES
Abstract

The grand challenges of contemporary fundamental physics-dark matter, dark energy, vacuum energy, inflation and early universe cosmology, singularities and the hierarchy problem-all involve gravity as a key component. And of all gravitational phenomena, black holes stand out in their elegant simplicity, while harbouring some of the most remarkable predictions of General Relativity: event horizons, singularities and ergoregions. The hitherto invisible landscape of the gravitational Universe is being unveiled before our eyes: the historical direct detection of gravitational waves by the LIGO-Virgo collaboration marks the dawn of a new era of scientific exploration. Gravitational-wave astronomy will allow us to test models of black hole formation, growth and evolution, as well as models of gravitational-wave generation and propagation. It will provide evidence for event horizons and ergoregions, test the theory of General Relativity itself, and may reveal the existence of new fundamental fields. The synthesis of these results has the potential to radically reshape our understanding of the cosmos and of the laws of Nature. The purpose of this work is to present a concise, yet comprehensive overview of the state of the art in the relevant fields of research, summarize important open problems, and lay out a roadmap for future progress. This write-up is an initiative taken within the framework of the European Action on 'Black holes, Gravitational waves and Fundamental Physics'., SCOPUS: re.j, info:eu-repo/semantics/published

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106. TYPE II SUPERNOVA ENERGETICS AND COMPARISON OF LIGHT CURVES TO SHOCK-COOLING MODELS.

Author

Adam Rubin, Avishay Gal-Yam, Annalisa De Cia, Assaf Horesh, Danny Khazov, Eran O. Ofek, S. R. Kulkarni, Iair Arcavi, Ilan Manulis, Ofer Yaron, Paul Vreeswijk, Mansi M. Kasliwal, Sagi Ben-Ami, Daniel A. Perley, Yi Cao, S. Bradley Cenko, Umaa D. Rebbapragada, P. R. Woźniak, Alexei V. Filippenko, and K. I. Clubb

Subjects
SUPERNOVAE, LIGHT curves, CATACLYSMIC variable stars, GALACTIC X-ray sources, ASTRONOMICAL spectroscopy
Abstract

During the first few days after explosion, Type II supernovae (SNe) are dominated by relatively simple physics. Theoretical predictions regarding early-time SN light curves in the ultraviolet (UV) and optical bands are thus quite robust. We present, for the first time, a sample of 57 R-band SN II light curves that are well-monitored during their rise, with detections during the first 10 days after discovery, and a well-constrained time of explosion to within 1–3 days. We show that the energy per unit mass (E/M) can be deduced to roughly a factor of five by comparing early-time optical data to the 2011 model of Rabinak & Waxman, while the progenitor radius cannot be determined based on R-band data alone. We find that SN II explosion energies span a range of E/M = (0.2–20) × 1051 erg/(10 ), and have a mean energy per unit mass of erg/(10 ), corrected for Malmquist bias. Assuming a small spread in progenitor masses, this indicates a large intrinsic diversity in explosion energy. Moreover, E/M is positively correlated with the amount of 56Ni produced in the explosion, as predicted by some recent models of core-collapse SNe. We further present several empirical correlations. The peak magnitude is correlated with the decline rate (), the decline rate is weakly correlated with the rise time, and the rise time is not significantly correlated with the peak magnitude. Faster declining SNe are more luminous and have longer rise times. This limits the possible power sources for such events. [ABSTRACT FROM AUTHOR]

Published
2016
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108. THE UNUSUAL RADIO AFTERGLOW OF THE ULTRA-LONG GAMMA-RAY BURST GRB 130925A.

Author

Assaf Horesh, S. Bradley Cenko, S. R. Kulkarni, Gregg Hallinan, Eric Bellm, and Daniel A. Perley

Subjects
*GAMMA ray bursts, *X-ray emission spectroscopy, *ELECTRON accelerators, *ELECTRON energy states, *ASTROPHYSICS research
Abstract

GRB 130925A is one of the recent additions to the growing family of ultra-long gamma-ray bursts (GRBs; T90 ≳1000 s). While the X-ray emission of ultra-long GRBs have been studied extensively in the past, no comprehensive radio data set has been obtained so far. We report here the early discovery of an unusual radio afterglow associated with the ultra-long GRB 130925A. The radio emission peaks at low-frequencies (∼7 GHz) at early times, only 2.2 days after the burst occurred. More notably, the radio spectrum at frequencies above 10 GHz exhibits a rather steep cut-off, compared to other long GRB radio afterglows. This cut-off can be explained if the emitting electrons are either mono-energetic or originate from a rather steep, dN/dE ∝ E−4, power-law energy distribution. An alternative electron acceleration mechanism may be required to produce such an electron energy distribution. Furthermore, the radio spectrum exhibits a secondary underlying and slowly varying component. This may hint that the radio emission we observed is comprised of emission from both a reverse and a forward shock. We discuss our results in comparison with previous works that studied the unusual X-ray spectrum of this event and discuss the implications of our findings on progenitor scenarios. [ABSTRACT FROM AUTHOR]

Published
2015
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109. THE NEEDLE IN THE 100 deg2 HAYSTACK: UNCOVERING AFTERGLOWS OF FERMI GRBs WITH THE PALOMAR TRANSIENT FACTORY.

Author

Leo P. Singer, Mansi M. Kasliwal, S. Bradley Cenko, Daniel A. Perley, Gemma E. Anderson, G. C. Anupama, Iair Arcavi, Varun Bhalerao, Brian D. Bue, Yi Cao, Valerie Connaughton, Alessandra Corsi, Antonino Cucchiara, Rob P. Fender, Derek B. Fox, Neil Gehrels, Adam Goldstein, J. Gorosabel, Assaf Horesh, and Kevin Hurley

Subjects
GAMMA-ray scattering, SPACE telescopes, GAMMA ray bursts, METAPHYSICAL cosmology, ASTRONOMY
Abstract

The Fermi Gamma-ray Space Telescope has greatly expanded the number and energy window of observations of gamma-ray bursts (GRBs). However, the coarse localizations of tens to a hundred square degrees provided by the Fermi GRB Monitor instrument have posed a formidable obstacle to locating the bursts’ host galaxies, measuring their redshifts, and tracking their panchromatic afterglows. We have built a target-of-opportunity mode for the intermediate Palomar Transient Factory in order to perform targeted searches for Fermi afterglows. Here, we present the results of one year of this program: 8 afterglow discoveries out of 35 searches. Two of the bursts with detected afterglows (GRBs 130702A and 140606B) were at low redshift (z = 0.145 and 0.384, respectively) and had spectroscopically confirmed broad-line Type Ic supernovae. We present our broadband follow-up including spectroscopy as well as X-ray, UV, optical, millimeter, and radio observations. We study possible selection effects in the context of the total Fermi and Swift GRB samples. We identify one new outlier on the Amati relation. We find that two bursts are consistent with a mildly relativistic shock breaking out from the progenitor star rather than the ultra-relativistic internal shock mechanism that powers standard cosmological bursts. Finally, in the context of the Zwicky Transient Facility, we discuss how we will continue to expand this effort to find optical counterparts of binary neutron star mergers that may soon be detected by Advanced LIGO and Virgo. [ABSTRACT FROM AUTHOR]

Published
2015
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110. A MULTIWAVELENGTH STUDY OF THE RELATIVISTIC TIDAL DISRUPTION CANDIDATE SWIFT J2058.4+0516 AT LATE TIMES.

Author

Dheeraj R. Pasham, S. Bradley Cenko, Andrew J. Levan, Geoffrey C. Bower, Assaf Horesh, Gregory C. Brown, Stephen Dolan, Klaas Wiersema, Alexei V. Filippenko, Andrew S. Fruchter, Jochen Greiner, Paul T. O’Brien, Kim L. Page, Arne Rau, and Nial R. Tanvir

Subjects
ACCRETION disks, ASTROMETRY, BLACK holes, RELATIVISTIC astrophysics, X-ray research
Abstract

We report a multiwavelength (X-ray, ultraviolet/optical/infrared (UVOIR), radio) analysis of the relativistic tidal disruption event (TDE) candidate Sw J2058+05 from 3 months to 3 yr post-discovery in order to study its properties and compare its behavior with that of Sw J1644+57. Our main results are as follows: (1) The long-term X-ray light curve of Sw J2058+05 shows a remarkably similar trend to that of Sw J1644+57. After a prolonged power-law decay, the X-ray flux drops off rapidly by a factor of ≳160 within a span of Δt/ . Associating this sudden decline with the transition from super-Eddington to sub-Eddington accretion, we estimate the black hole mass to be in the range of 104–6M. (2) We detect rapid (≲500 s) X-ray variability before the drop-off, suggesting that, even at late times, the X-rays originate from close to the black hole (ruling out a forward-shock origin). (3) We confirm using Hubble Space Telescope and Very Long Baseline Array astrometry that the location of the source coincides with the galaxy’s center to within ≲400 pc (in projection). (4) We modeled Sw J2058+05's UVOIR spectral energy distribution with a single-temperature blackbody and find that while the radius remains more or less constant at a value of 63.4 ± 4.5 AU ( cm) at all times during the outburst, the blackbody temperature drops significantly from ∼30,000 K at early times to a value of ∼15,000 K at late times (before the X-ray drop-off). Our results strengthen Sw J2058+05's interpretation as a TDE similar to Sw J1644+57. [ABSTRACT FROM AUTHOR]

Published
2015
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112. ULTRAVIOLET SPECTROSCOPY OF TYPE IIB SUPERNOVAE: DIVERSITY AND THE IMPACT OF CIRCUMSTELLAR MATERIAL.

Author

Sagi Ben-Ami, Stephan Hachinger, Avishay Gal-Yam, Paolo A. Mazzali, Alexei V. Filippenko, Assaf Horesh, Thomas Matheson, Maryam Modjaz, Daniel N. Sauer, Jeffrey M. Silverman, Nathan Smith, and Ofer Yaron

Subjects
ULTRAVIOLET spectra, STELLAR photospheres, SOLAR photosphere, CIRCUMSTELLAR matter
Abstract

We present new Hubble Space Telescope (HST) multi-epoch ultraviolet (UV) spectra of the bright Type IIb SN 2013df, and undertake a comprehensive analysis of the set of four SNe IIb for which HST UV spectra are available (SN 1993J, SN 2001ig, SN 2011dh, and SN 2013df). We find strong diversity in both continuum levels and line features among these objects. We use radiative-transfer models that fit the optical part of the spectrum well, and find that in three of these four events we see a UV continuum flux excess, apparently unaffected by line absorption. We hypothesize that this emission originates above the photosphere, and is related to interaction with circumstellar material (CSM) located in close proximity to the SN progenitor. In contrast, the spectra of SN 2001ig are well fit by single-temperature models, display weak continuum and strong reverse-fluorescence features, and are similar to spectra of radioactive 56Ni-dominated SNe Ia. A comparison of the early shock-cooling components in the observed light curves with the UV continuum levels which we assume trace the strength of CSM interaction suggests that events with slower cooling have stronger CSM emission. The radio emission from events having a prominent UV excess is perhaps consistent with slower blast-wave velocities, as expected if the explosion shock was slowed down by the CSM that is also responsible for the strong UV, but this connection is currently speculative as it is based on only a few events. [ABSTRACT FROM AUTHOR]

Published
2015
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