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1. OGLE-2013-BLG-0911Lb: A Secondary on the Brown-dwarf Planet Boundary around an M Dwarf

Author

Shota Miyazaki, Takahiro Sumi, David P. Bennett, Andrzej Udalski, Yossi Shvartzvald, Rachel Street, Valerio Bozza, Jennifer C. Yee, Ian A. Bond, Nicholas Rattenbury, Naoki Koshimoto, Daisuke Suzuki, Akihiko Fukui, F. Abe, A. Bhattacharya, R. Barry, M. Donachie, H. Fujii, Y. Hirao, Y. Itow, Y. Kamei, I. Kondo, M. C. A. Li, C. H. Ling, Y. Matsubara, T. Matsuo, Y. Muraki, M. Nagakane, K. Ohnishi, C Ranc, T. Saito1, A. Sharan, H. Shibai, H. Suematsu, D. J. Sullivan, P. J. Tristram, T. Yamakawa, A. Yonehara, J. Skowron, R. Poleski, P. Mróz, M. K. Szymański, I. Soszyński, P. Pietrukowicz, S. KozŁowski, K. Ulaczyk, Ł. Wyrzykowski, Matan Friedmann, Shai Kaspi, Dan Maoz, M. Albrow, G. Christie, D. L. DePoy, A. Gal-Yam, A. Gould, C.-U. Lee, I. Manulis, J. McCormick, T. Natusch, H. Ngan, R. W. Pogge, I. Porritt, Y. Tsapras, E. Bachelet, M. P. G. Hundertmark, M. Dominik, D. M. Bramich, A. Cassan, R. Figuera Jaimes, K. Horne, R. Schmidt, C. Snodgrass, J. Wambsganss, I. A. Steele, J. Menzies, S. Mao, U. G. Jørgensen, M. J. Burgdorf, S. Ciceri, S. Calchi Novati, G. D’Ago, D. F. Evans, T. C. Hinse, N. Kains, E. Kerins, H. Korhonen, L. Mancini, A. Popovas, M. Rabus, S. Rahvar, G. Scarpetta, J. Skottfelt, J. Southworth, N. Peixinho, and P. Verma

Subjects
Astrophysics, Astronomy
Abstract

We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q 0.03, which differs from that reported in Shvartzvald et al. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ~ 0.15 or s ~ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M dwarf orbited by a massive Jupiter companion at very close (M(host) = 0.30(sup +0.08, sub -0.06)Mʘ, M(comp) = 10.1 (sup +2.9, sub -2.2 M(jup), a(exp) = 0.40 (sup +0.05, sub -0.40)au) or wide (M(host) = 0.28 (sup +0.10, sub -0.80)Mʘ, M(comp) = 9.9 (sup +3.8, sub -3.5)M(jup), a(exp) = 18.0 (sup +3.2, sub -3.2)au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q = 0.03, which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M(Jup). It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ~13M(Jup) in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M dwarfs and even BDs, which is challenging for other exoplanet detection methods.

Published
2020
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2. Observation of inverse Compton emission from a long γ-ray burst

Author

P. Veres, P. N. Bhat, M. S. Briggs, W. H. Cleveland, R. Hamburg, C. M. Hui, B. Mailyan, R. D. Preece, O. J. Roberts, A. von Kienlin, C. A. Wilson-Hodge, D. Kocevski, M. Arimoto, D. Tak, K. Asano, M. Axelsson, G. Barbiellini, E. Bissaldi, F.Fana Dirirsa, R. Gill, J. Granot, J. McEnery, N. Omodei, S. Razzaque, F. Piron, J. L. Racusin, D. J. Thompson, S. Campana, M. G. Bernardini, N. P. M. Kuin, M. H. Siegel, S. B. Cenko, P. O’Brien, M. Capalbi, A. Daì, M. De Pasquale, J. Gropp, N. Klingler, J. P. Osborne, M. Perri, R. L. C. Starling, G. Tagliaferri, A. Tohuvavohu, A. Ursi, M.Tavani, M. Cardillo, C. Casentini, G. Piano, Y. Evangelista, F. Verrecchia, C. Pittori, F. Lucarelli, A. Bulgarelli, N. Parmiggiani, G. E. Anderson, J. P. Anderson, G. Bernardi, J. Bolmer, M. D. Caballero-García, I. M. Carrasco, A. Castellón, N. Castro Segura, A. J. Castro-Tirado, S. V. Cherukuri, A. M. Cockeram, P. D’Avanzo, A. Di Dato, R. Diretse, R. P. Fender, E. Fernández-García, J. P. U. Fynbo, A. S.Fruchter, J. Greiner, M. Gromadzki, K. E. Heintz, I. Heywood, A. J. van der Horst, Y.-D. Hu, C. Inserra, L. Izzo, V. Jaiswal, P. Jakobsson, J. Japelj, E. Kankare, D. A.Kann, C. Kouveliotou, S. Klose, A. J. Levan, X. Y. Li, S. Lotti, K. Maguire, D. B. Malesani, I. Manulis, M. Marongiu, S. Martin, A. Melandri, M. J.Michałowski, J. C. A. Miller-Jones, K. Misra, A. Moin, K. P. Mooley, S. Nasri, M. Nicholl, A. Noschese, G. Novara, S. B. Pandey, E. Peretti, C. J. Pérez del Pulgar, M. A. Pérez-Torres, D. A. Perley, L. Piro, F. Ragosta, L. Resmi, R. Ricci, A. Rossi, R. Sánchez-Ramírez, J. Selsing, S. Schulze, S. J. Smartt, I. A. Smith, V. V. Sokolov, J. Stevens, N. R. Tanvir, C. C. Thöne, A. Tiengo, E. Tremou, E. Troja, A. de Ugarte Postigo, A. F. Valeev, S. D. Vergani, M. Wieringa, P. A. Woudt, D. Xu, O. Yaron, D. R. Young, V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, D. Baack, A. Babić, B. Banerjee, U. Barres de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Ž. Bošnjak, G. Busetto, R. Carosi, G. Ceribella, Y. Chai, A. Chilingaryan, S. Cikota, S. M. Colak, U. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, V. D’Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, D. Depaoli, F. Di Pierro, L. Di Venere, E. Do Souto Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, G. Ferrara, D. Fidalgo, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, R. J. García López, M. Garczarczyk, S.Gasparyan, M. Gaug, N. Giglietto, F. Giordano, N. Godinović, D. Green, D. Guberman, D. Hadasch, A. Hahn, J. Herrera, J. Hoang, D. Hrupec, M. Hütten, T. Inada, S. Inoue, K. Ishio, Y. Iwamura, L. Jouvin, D. Kerszberg, H. Kubo, J. Kushida, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, S. Lombardi, F. Longo, M. López, R. López-Coto, A. López-Oramas, S. Loporchio, B. Machado de Oliveira Fraga, C. Maggio, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, S. Mićanović, D. Miceli, M. Minev, J. M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, D. Morcuende, V. Moreno, E. Moretti, P. Munar-Adrover, V. Neustroev, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, L. Nogués, S. Nozaki, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, P. Peñil, M. Peresano, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, K. Schmidt, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Somero, A. Stamerra, D. Strom, M. Strzys, Y. Suda, T. Surić, M. Takahashi, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, N. Torres-Albà, L. Tosti, V. Vagelli, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, C. F. Vigorito, V. Vitale, I. Vovk, M. Will, D. Zarić, and L. Nava

Subjects
Space Sciences (General)
Abstract

Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission. Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C. Here we report multifrequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10^(−6) to 10^(12) electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.

Published
2019
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3. Physical properties of the trans-Neptunian object (38628) Huya from a multi-chord stellar occultation

Author

P. Santos-Sanz, J. L. Ortiz, B. Sicardy, M. Popescu, G. Benedetti-Rossi, N. Morales, M. Vara-Lubiano, J. I. B. Camargo, C. L. Pereira, F. L. Rommel, M. Assafin, J. Desmars, F. Braga-Ribas, R. Duffard, J. Marques Oliveira, R. Vieira-Martins, E. Fernández-Valenzuela, B. E. Morgado, M. Acar, S. Anghel, E. Atalay, A. Ateş, H. Bakiş, V. Bakis, Z. Eker, O. Erece, S. Kaspi, C. Kayhan, S. E. Kilic, Y. Kilic, I. Manulis, D. A. Nedelcu, M. S. Niaei, G. Nir, E. Ofek, T. Ozisik, E. Petrescu, O. Satir, A. Solmaz, A. Sonka, M. Tekes, O. Unsalan, C. Yesilyaprak, R. Anghel, D. Berteşteanu, L. Curelaru, C. Danescu, V. Dumitrescu, R. Gherase, L. Hudin, A-M. Stoian, J. O. Tercu, R. Truta, V. Turcu, C. Vantdevara, I. Belskaya, T. O. Dementiev, K. Gazeas, S. Karampotsiou, V. Kashuba, Cs. Kiss, N. Koshkin, O. M. Kozhukhov, Y. Krugly, J. Lecacheux, A. Pal, Ç. Püsküllü, R. Szakats, V. Zhukov, D. Bamberger, B. Mondon, C. Perelló, A. Pratt, C. Schnabel, A. Selva, J. P. Teng, K. Tigani, V. Tsamis, C. Weber, G. Wells, S. Kalkan, V. Kudak, A. Marciniak, W. Ogloza, T. Özdemir, E. Pakštiene, V. Perig, M. Żejmo, Ministerio de Ciencia e Innovación (España), European Commission, European Research Council, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Institut Polytechnique des Sciences Avancées (IPSA)

Subjects
Albedo, Kuiper belt objects, FOS: Physical sciences, Density, Huya, methods, photometric, Size, Methods: observational, individual: huya, methods: observational, techniques: photometric, astrophysics - earth and planetary astrophysics, astrophysics - solar and stellar astrophysics [kuiper belt objects], observational, individual, Variability, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Ring, Pluto, Atmosphere, Kuiper belt objects: individual: Huya, Astronomy and Astrophysics, Bodies, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques, Centaur, Orbit, Techniques: photometric, Astrophysics - Earth and Planetary Astrophysics
Abstract

Full list of authors: Santos-Sanz, P.; Ortiz, J. L.; Sicardy, B.; Popescu, M.; Benedetti-Rossi, G.; Morales, N.; Vara-Lubiano, M.; Camargo, J. I. B.; Pereira, C. L.; Rommel, F. L.; Assafin, M.; Desmars, J.; Braga-Ribas, F.; Duffard, R.; Marques Oliveira, J.; Vieira-Martins, R.; Fernández-Valenzuela, E.; Morgado, B. E.; Acar, M.; Anghel, S.; Atalay, E.; Ateş, A.; Bakiş, H.; Bakis, V.; Eker, Z.; Erece, O.; Kaspi, S.; Kayhan, C.; Kilic, S. E.; Kilic, Y.; Manulis, I.; Nedelcu, D. A.; Niaei, M. S.; Nir, G.; Ofek, E.; Ozisik, T.; Petrescu, E.; Satir, O.; Solmaz, A.; Sonka, A.; Tekes, M.; Unsalan, O.; Yesilyaprak, C.; Anghel, R.; Berteşteanu, D.; Curelaru, L.; Danescu, C.; Dumitrescu, V.; Gherase, R.; Hudin, L.; Stoian, A. -M.; Tercu, J. O.; Truta, R.; Turcu, V.; Vantdevara, C.; Belskaya, I.; Dementiev, T. O.; Gazeas, K.; Karampotsiou, S.; Kashuba, V.; Kiss, Cs.; Koshkin, N.; Kozhukhov, O. M.; Krugly, Y.; Lecacheux, J.; Pal, A.; Püsküllü, Ç.; Szakats, R.; Zhukov, V.; Bamberger, D.; Mondon, B.; Perelló, C.; Pratt, A.; Schnabel, C.; Selva, A.; Teng, J. P.; Tigani, K.; Tsamis, V.; Weber, C.; Wells, G.; Kalkan, S.; Kudak, V.; Marciniak, A.; Ogloza, W.; Özdemir, T.; Pakštiene, E.; Perig, V.; Żejmo, M.--This is an Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited., Context. As part of our international program aimed at obtaining accurate physical properties of trans-Neptunian objects (TNOs), we predicted a stellar occultation by the TNO (38628) Huya of the star Gaia DR2 4352760586390566400 (mG = 11.5 mag) on March 18, 2019. After an extensive observational campaign geared at obtaining the astrometric data, we updated the prediction and found it favorable to central Europe. Therefore, we mobilized half a hundred of professional and amateur astronomers in this region and the occultation was finally detected by 21 telescopes located at 18 sites in Europe and Asia. This places the Huya event among the best ever observed stellar occultation by a TNO in terms of the number of chords. Aims. The aim of our work is to determine an accurate size, shape, and geometric albedo for the TNO (38628) Huya by using the observations obtained from a multi-chord stellar occultation. We also aim to provide constraints on the density and other internal properties of this TNO. Methods. The 21 positive detections of the occultation by Huya allowed us to obtain well-separated chords which permitted us to fit an ellipse for the limb of the body at the moment of the occultation (i.e., the instantaneous limb) with kilometric accuracy. Results. The projected semi-major and minor axes of the best ellipse fit obtained using the occultation data are (a′, b′) = (217.6 ± 3.5 km, 194.1 ± 6.1 km) with a position angle for the minor axis of P′ = 55.2° ± 9.1. From this fit, the projected area-equivalent diameter is 411.0 ± 7.3 km. This diameter is compatible with the equivalent diameter for Huya obtained from radiometric techniques (D = 406 ± 16 km). From this instantaneous limb, we obtained the geometric albedo for Huya (pV = 0.079 ± 0.004) and we explored possible three-dimensional shapes and constraints to the mass density for this TNO. We did not detect the satellite of Huya through this occultation, but the presence of rings or debris around Huya was constrained using the occultation data. We also derived an upper limit for a putative Pluto-like global atmosphere of about psurf = 10 nbar. © P. Santos-Sanz et al. 2022., P.S-S. acknowledges financial support by the Spanish grant AYA-RTI2018-098657-J-I00 “LEO-SBNAF” (MCIU/AEI/FEDER, UE). P.S-S., J.L.O., N.M., M.V-L. and R.D. acknowledge financial support from the State Agency for Research of the Spanish MCIU through the “Center of Excellence Severo Ochoa” award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709), they also acknowledge the financial support by the Spanish grants AYA-2017-84637-R and PID2020-112789GB-I00, and the Proyectos de Excelencia de la Junta de Andalucía 2012-FQM1776 and PY20-01309. The research leading to these results has received funding from the European Union’s Horizon 2020 Research and Innovation Programme, under Grant Agreement no. 687378, as part of the project “Small Bodies Near and Far” (SBNAF). Part of the research leading to these results has received funding from the European Research Council under the European Community’s H2020 (2014-2020/ERC Grant Agreement no. 669416 “LUCKY STAR”). Part of the work of M.P. was financed by a grant of the Romanian National Authority for Scientific Research and Innovation, CNCS – UEFISCDI PN-III-P1-1.1-TE-2019-1504. This study was financed in part by the Coordenaçâo de Aperfeiçoamento de Pessoal de Nível Superior – Brasil (CAPES) – Finance Code 001 and the National Institute of Science and Technology of the e-Universe project (INCT do e-Universo, CNPq grant 465376/2014-2). The following authors acknowledge the respective CNPq grants: F.B-R 309578/2017-5; R.V.-M. 304544/2017-5, 401903/2016-8; J.I.B.C. 308150/2016-3 and 305917/2019-6; M.A 427700/2018-3, 310683/2017-3 and 473002/2013-2; B.E.M. 150612/2020-6. G.B.R. thanks the support of CAPES and FAPERJ/PAPDRJ (E26/203.173/2016) grant. J.M.O. acknowledges financial support from the Portuguese Foundation for Science and Technology (FCT) and the European Social Fund (ESF) through the PhD grant SFRH/BD/131700/2017. E.F-V. acknowledges funding through the Preeminant Postdoctoral Program of the University of Central Florida. C.K., A.P. and R.S. have been supported by the grants K-125015 and K-138962 of the National Research, Development and Innovation Office (NKFIH, Hungary). E.P. acknowledges the Europlanet 2024 RI project funded by the European Union’s Horizon 2020 Research and Innovation Programme (Grant agreement No. 871149). We are grateful to the CAHA and OSN staffs. This research is partially based on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by Junta de Andalucía and Consejo Superior de Investigaciones Científicas (IAA-CSIC). This research was also partially based on observation carried out at the Observatorio de Sierra Nevada (OSN) operated by Instituto de Astrofísica de Andalucía (CSIC). This article is also based on observations made in the Observatorios de Canarias del IAC with the Liverpool Telescope operated on the island of La Palma by the Instituto de Astrofísica de Canarias in the Observatorio del Roque de los Muchachos. Part of the results were based on observations taken at Pico dos Dias Observatory of the National Laboratory of Astrophysics (LNA/Brazil). Part of the data were collected during the photometric monitoring observations with the robotic and remotely controlled observatory at the University of Athens Observatory – UOAO (Gazeas 2016). We thank the Adiyaman University Astrophysics Application and Research Center for their support in the acquisition of data with the ADYU60 telescope. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.

Published
2022

4. COMMON ENVELOPE EJECTION FOR A LUMINOUS RED NOVA IN M101.

Author

M. M. Kasliwal, Y. Cao, J. Jencson, S. R. Kulkarni, F. J. Masci, N. Blagorodnova, I. Manulis, P. M. Vreeswijk, P. Nugent, P. Wozniak, M. Fraser, C. Gonzalez-Fernandez, S. Mattila, R. Kotak, J. Polshaw, E. Kankare, K. Smith, G. Terreran, A. M. Cody, and G. B. Doran

Subjects
BINARY stars, CATACLYSMIC variable stars, NOVAE (Astronomy), ASTRONOMICAL photometry
Abstract

We present the results of optical, near-infrared, and mid-infrared observations of M101 OT2015-1 (PSN J14021678+5426205), a luminous red transient in the Pinwheel galaxy (M101), spanning a total of 16 years. The light curve showed two distinct peaks with absolute magnitudes and , on 2014 November 11 and 2015 February 17, respectively. The spectral energy distributions during the second maximum show a cool outburst temperature of K and low expansion velocities ( km s−1) for the H i, Ca ii, Ba ii, and K i lines. From archival data spanning 15–8 years before the outburst, we find a single source consistent with the optically discovered transient, which we attribute to being the progenitor; it has properties consistent with being an F-type yellow supergiant with L ∼ 8.7 L⊙, K, and an estimated mass of M⊙. This star has likely just finished the H-burning phase in the core, started expanding, and is now crossing the Hertzsprung gap. Based on the combination of observed properties, we argue that the progenitor is a binary system, with the more evolved system overfilling the Roche lobe. Comparison with binary evolution models suggests that the outburst was an extremely rare phenomenon, likely associated with the ejection of the common envelope of a massive star. The initial mass of the primary fills the gap between the merger candidates V838 Mon (5−10 M⊙) and NGC 4490-OT (30 M⊙). [ABSTRACT FROM AUTHOR]

Published
2017
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6. FLASH SPECTROSCOPY: EMISSION LINES FROM THE IONIZED CIRCUMSTELLAR MATERIAL AROUND <10-DAY-OLD TYPE II SUPERNOVAE.

Author

D. Khazov, O. Yaron, A. Gal-Yam, I. Manulis, A. Rubin, S. R. Kulkarni, I. Arcavi, M. M. Kasliwal, E. O. Ofek, Y. Cao, D. Perley, J. Sollerman, A. Horesh, M. Sullivan, A. V. Filippenko, P. E. Nugent, D. A. Howell, S. B. Cenko, J. M. Silverman, and H. Ebeling

Subjects
SUPERNOVAE, CIRCUMSTELLAR matter, ELECTRON emission, STELLAR mass, BLACK body (Physics)
Abstract

Supernovae (SNe) embedded in dense circumstellar material (CSM) may show prominent emission lines in their early-time spectra (≤10 days after the explosion), owing to recombination of the CSM ionized by the shock-breakout flash. From such spectra (“flash spectroscopy”), we can measure various physical properties of the CSM, as well as the mass-loss rate of the progenitor during the year prior to its explosion. Searching through the Palomar Transient Factory (PTF and iPTF) SN spectroscopy databases from 2009 through 2014, we found 12 SNe II showing flash-ionized (FI) signatures in their first spectra. All are younger than 10 days. These events constitute 14% of all 84 SNe in our sample having a spectrum within 10 days from explosion, and 18% of SNe II observed at ages <5 days, thereby setting lower limits on the fraction of FI events. We classified as “blue/featureless” (BF) those events having a first spectrum that is similar to that of a blackbody, without any emission or absorption signatures. It is possible that some BF events had FI signatures at an earlier phase than observed, or that they lack dense CSM around the progenitor. Within 2 days after explosion, 8 out of 11 SNe in our sample are either BF events or show FI signatures. Interestingly, we found that 19 out of 21 SNe brighter than an absolute magnitude MR = −18.2 belong to the FI or BF groups, and that all FI events peaked above MR = −17.6 mag, significantly brighter than average SNe II. [ABSTRACT FROM AUTHOR]

Published
2016
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7. Observation of inverse Compton emission from a long γ-ray burst.

Author

Veres P, Bhat PN, Briggs MS, Cleveland WH, Hamburg R, Hui CM, Mailyan B, Preece RD, Roberts OJ, von Kienlin A, Wilson-Hodge CA, Kocevski D, Arimoto M, Tak D, Asano K, Axelsson M, Barbiellini G, Bissaldi E, Dirirsa FF, Gill R, Granot J, McEnery J, Omodei N, Razzaque S, Piron F, Racusin JL, Thompson DJ, Campana S, Bernardini MG, Kuin NPM, Siegel MH, Cenko SB, O'Brien P, Capalbi M, Daì A, De Pasquale M, Gropp J, Klingler N, Osborne JP, Perri M, Starling RLC, Tagliaferri G, Tohuvavohu A, Ursi A, Tavani M, Cardillo M, Casentini C, Piano G, Evangelista Y, Verrecchia F, Pittori C, Lucarelli F, Bulgarelli A, Parmiggiani N, Anderson GE, Anderson JP, Bernardi G, Bolmer J, Caballero-García MD, Carrasco IM, Castellón A, Segura NC, Castro-Tirado AJ, Cherukuri SV, Cockeram AM, D'Avanzo P, Di Dato A, Diretse R, Fender RP, Fernández-García E, Fynbo JPU, Fruchter AS, Greiner J, Gromadzki M, Heintz KE, Heywood I, van der Horst AJ, Hu YD, Inserra C, Izzo L, Jaiswal V, Jakobsson P, Japelj J, Kankare E, Kann DA, Kouveliotou C, Klose S, Levan AJ, Li XY, Lotti S, Maguire K, Malesani DB, Manulis I, Marongiu M, Martin S, Melandri A, Michałowski MJ, Miller-Jones JCA, Misra K, Moin A, Mooley KP, Nasri S, Nicholl M, Noschese A, Novara G, Pandey SB, Peretti E, Del Pulgar CJP, Pérez-Torres MA, Perley DA, Piro L, Ragosta F, Resmi L, Ricci R, Rossi A, Sánchez-Ramírez R, Selsing J, Schulze S, Smartt SJ, Smith IA, Sokolov VV, Stevens J, Tanvir NR, Thöne CC, Tiengo A, Tremou E, Troja E, de Ugarte Postigo A, Valeev AF, Vergani SD, Wieringa M, Woudt PA, Xu D, Yaron O, and Young DR

Abstract

Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission 1,2 . Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands 1-6 . The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock 7-9 . Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C 10,11 . Here we report multi-frequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10 -6 to 10 12 electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.

Published
2019
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8. A kilonova as the electromagnetic counterpart to a gravitational-wave source.

Author

Smartt SJ, Chen TW, Jerkstrand A, Coughlin M, Kankare E, Sim SA, Fraser M, Inserra C, Maguire K, Chambers KC, Huber ME, Krühler T, Leloudas G, Magee M, Shingles LJ, Smith KW, Young DR, Tonry J, Kotak R, Gal-Yam A, Lyman JD, Homan DS, Agliozzo C, Anderson JP, Angus CR, Ashall C, Barbarino C, Bauer FE, Berton M, Botticella MT, Bulla M, Bulger J, Cannizzaro G, Cano Z, Cartier R, Cikota A, Clark P, De Cia A, Della Valle M, Denneau L, Dennefeld M, Dessart L, Dimitriadis G, Elias-Rosa N, Firth RE, Flewelling H, Flörs A, Franckowiak A, Frohmaier C, Galbany L, González-Gaitán S, Greiner J, Gromadzki M, Guelbenzu AN, Gutiérrez CP, Hamanowicz A, Hanlon L, Harmanen J, Heintz KE, Heinze A, Hernandez MS, Hodgkin ST, Hook IM, Izzo L, James PA, Jonker PG, Kerzendorf WE, Klose S, Kostrzewa-Rutkowska Z, Kowalski M, Kromer M, Kuncarayakti H, Lawrence A, Lowe TB, Magnier EA, Manulis I, Martin-Carrillo A, Mattila S, McBrien O, Müller A, Nordin J, O'Neill D, Onori F, Palmerio JT, Pastorello A, Patat F, Pignata G, Podsiadlowski P, Pumo ML, Prentice SJ, Rau A, Razza A, Rest A, Reynolds T, Roy R, Ruiter AJ, Rybicki KA, Salmon L, Schady P, Schultz ASB, Schweyer T, Seitenzahl IR, Smith M, Sollerman J, Stalder B, Stubbs CW, Sullivan M, Szegedi H, Taddia F, Taubenberger S, Terreran G, van Soelen B, Vos J, Wainscoat RJ, Walton NA, Waters C, Weiland H, Willman M, Wiseman P, Wright DE, Wyrzykowski Ł, and Yaron O

Abstract

Gravitational waves were discovered with the detection of binary black-hole mergers and they should also be detectable from lower-mass neutron-star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal. This signal is luminous at optical and infrared wavelengths and is called a kilonova. The gravitational-wave source GW170817 arose from a binary neutron-star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC 4993, which is spatially coincident with GW170817 and with a weak, short γ-ray burst. The transient has physical parameters that broadly match the theoretical predictions of blue kilonovae from neutron-star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 ± 0.01 solar masses, with an opacity of less than 0.5 square centimetres per gram, at a velocity of 0.2 ± 0.1 times light speed. The power source is constrained to have a power-law slope of -1.2 ± 0.3, consistent with radioactive powering from r-process nuclides. (The r-process is a series of neutron capture reactions that synthesise many of the elements heavier than iron.) We identify line features in the spectra that are consistent with light r-process elements (atomic masses of 90-140). As it fades, the transient rapidly becomes red, and a higher-opacity, lanthanide-rich ejecta component may contribute to the emission. This indicates that neutron-star mergers produce gravitational waves and radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements.

Published
2017
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