Author: "Castro-Tirado AJ" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Castro-Tirado AJ"' showing total 48 results

Start Over Author "Castro-Tirado AJ"

48 results on '"Castro-Tirado AJ"'

1. Kilonova Luminosity Function Constraints Based on Zwicky Transient Facility Searches for 13 Neutron Star Merger Triggers during O3

Author: Kasliwal, MM, Anand, S, Ahumada, T, Stein, R, Carracedo, AS, Andreoni, I, Coughlin, MW, Singer, LP, Kool, EC, De, K, Kumar, H, Almualla, M, Yao, Y, Bulla, M, Dobie, D, Reusch, S, Perley, DA, Cenko, SB, Bhalerao, V, Kaplan, DL, Sollerman, J, Goobar, A, Copperwheat, CM, Bellm, EC, Anupama, GC, Corsi, A, Nissanke, S, Agudo, I, Bagdasaryan, A, Barway, S, Belicki, J, Bloom, JS, Bolin, B, Buckley, DAH, Burdge, KB, Burruss, R, Caballero-García, MD, Cannella, C, Castro-Tirado, AJ, Cook, DO, Cooke, J, Cunningham, V, Dahiwale, A, Deshmukh, K, Dichiara, S, Duev, DA, Dutta, A, Feeney, M, Franckowiak, A, Frederick, S, Fremling, C, Gal-Yam, A, Gatkine, P, Ghosh, S, Goldstein, DA, Golkhou, VZ, Graham, MJ, Graham, ML, Hankins, MJ, Helou, G, Hu, Y, Ip, WH, Jaodand, A, Karambelkar, V, Kong, AKH, Kowalski, M, Khandagale, M, Kulkarni, SR, Kumar, B, Laher, RR, Li, KL, Mahabal, A, Masci, FJ, Miller, AA, Mogotsi, M, Mohite, S, Mooley, K, Mroz, P, Newman, JA, Ngeow, CC, Oates, SR, Patil, AS, Pandey, SB, Pavana, M, Pian, E, Riddle, R, Sánchez-Ramírez, R, Sharma, Y, Singh, A, Smith, R, Soumagnac, MT, Taggart, K, Tan, H, Tzanidakis, A, Troja, E, Valeev, AF, Walters, R, Waratkar, G, Webb, S, and Yu, PC
Subjects: Neutron stars, Black holes, Gravitational waves, Nucleosynthesis, R-process, Compact objects, Spectroscopy, Sky surveys, Photometry, astro-ph.HE, astro-ph.IM, astro-ph.SR, Astronomy & Astrophysics, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
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 (O3). 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 area of 4480 deg2, a median distance of 267 Mpc, and false-alarm rates ranging from 1.5 to 10-25 yr-1. The ZTF coverage in the g and r bands had a median enclosed probability of 39%, median depth of 20.8 mag, and median time lag between merger and the start of observations of 1.5 hr. The O3 follow-up by the GROWTH team comprised 340 UltraViolet/Optical/InfraRed (UVOIR) photometric points, 64 OIR spectra, and three radio images using 17 different telescopes. We find no promising kilonovae (radioactivity-powered counterparts), and we show how to convert the upper limits to constrain the underlying kilonova luminosity function. Initially, we assume that all GW triggers are bona fide astrophysical events regardless of false-alarm rate and that kilonovae accompanying BNS and NSBH mergers are drawn from a common population; later, we relax these assumptions. Assuming that all kilonovae are at least as luminous as the discovery magnitude of GW170817 (-16.1 mag), we calculate that our joint probability of detecting zero kilonovae is only 4.2%. If we assume that all kilonovae are brighter than-16.6 mag (the extrapolated peak magnitude of GW170817) and fade at a rate of 1 mag day-1 (similar to GW170817), the joint probability of zero detections is 7%. If we separate the NSBH and BNS populations based on the online classifications, the joint probability of zero detections, assuming all kilonovae are brighter than-16.6 mag, is 9.7% for NSBH and 7.9% for BNS mergers. Moreover, no more than 10-4, or φ > 30° to be consistent with our limits. We look forward to searches in the fourth GW observing run; even 17 neutron star mergers with only 50% coverage to a depth of-16 mag would constrain the maximum fraction of bright kilonovae to
Published: 2020

2. GROWTH on S190814bv: Deep Synoptic Limits on the Optical/Near-infrared Counterpart to a Neutron Star-Black Hole Merger

Author: Andreoni, I, Goldstein, DA, Kasliwal, MM, Nugent, PE, Zhou, R, Newman, JA, Bulla, M, Foucart, F, Hotokezaka, K, Nakar, E, Nissanke, S, Raaijmakers, G, Bloom, JS, De, K, Jencson, JE, Ward, C, Ahumada, T, Anand, S, Buckley, DAH, Caballero-García, MD, Castro-Tirado, AJ, Copperwheat, CM, Coughlin, MW, Cenko, SB, Gromadzki, M, Hu, Y, Karambelkar, VR, Perley, DA, Sharma, Y, Valeev, AF, Cook, DO, Fremling, UC, Kumar, H, Taggart, K, Bagdasaryan, A, Cooke, J, Dahiwale, A, Dhawan, S, Dobie, D, Gatkine, P, Golkhou, VZ, Goobar, A, Chaves, AG, Hankins, M, Kaplan, DL, Kong, AKH, Kool, EC, Mohite, S, Sollerman, J, Tzanidakis, A, Webb, S, and Zhang, K
Subjects: astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry, Astronomy & Astrophysics, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural)
Abstract: On 2019 August 14, the Advanced LIGO and Virgo interferometers detected the high-significance gravitational wave (GW) signal S190814bv. The GW data indicated that the event resulted from a neutron star-black hole (NSBH) merger, or potentially a low-mass binary BH merger. Due to the low false-alarm rate and the precise localization (23 deg2 at 90%), S190814bv presented the community with the best opportunity yet to directly observe an optical/near-infrared counterpart to an NSBH merger. To search for potential counterparts, the GROWTH Collaboration performed real-time image subtraction on six nights of public Dark Energy Camera images acquired in the 3 weeks following the merger, covering >98% of the localization probability. Using a worldwide network of follow-up facilities, we systematically undertook spectroscopy and imaging of optical counterpart candidates. Combining these data with a photometric redshift catalog, we ruled out each candidate as the counterpart to S190814bv and placed deep, uniform limits on the optical emission associated with S190814bv. For the nearest consistent GW distance, radiative transfer simulations of NSBH mergers constrain the ejecta mass of S190814bv to be M ej < 0.04 M o˙ at polar viewing angles, or M ej < 0.03 M o˙ if the opacity is κ < 2 cm2g-1. Assuming a tidal deformability for the NS at the high end of the range compatible with GW170817 results, our limits would constrain the BH spin component aligned with the orbital momentum to be χ < 0.7 for mass ratios Q < 6, with weaker constraints for more compact NSs.
Published: 2020

3. A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

Author: Pandey, SB, Hu, Y, Castro-Tirado, AJ, Pozanenko, AS, Sánchez-Ramírez, R, Gorosabel, J, Guziy, S, Jelinek, M, Tello, JC, Jeong, S, Oates, SR, Zhang, BB, Mazaeva, ED, Volnova, AA, Minaev, PY, Van Eerten, HJ, Caballero-García, MD, Pérez-Ramírez, D, Bremer, M, Winters, JM, Park, IH, Nicuesa Guelbenzu, A, Klose, S, Moskvitin, A, Sokolov, VV, Sonbas, E, Ayala, A, Cepa, J, Butler, N, Troja, E, Chernenko, AM, Molkov, SV, Volvach, AE, Inasaridze, RY, Egamberdiyev, SA, Burkhonov, O, Reva, IV, Polyakov, KA, Matkin, AA, Ivanov, AL, Molotov, I, Guver, T, Watson, AM, Kutyrev, A, Lee, WH, Fox, O, Littlejohns, O, Cucchiara, A, Gonzalez, J, Richer, MG, Román-Zúñiga, CG, Tanvir, NR, Bloom, JS, Prochaska, JX, Gehrels, N, Moseley, H, De Diego, JA, Ramírez-Ruiz, E, Klunko, EV, Fan, Y, Zhao, X, Bai, J, Wang, C, Xin, Y, Cui, C, Tungalag, N, Peng, ZK, Kumar, A, Gupta, R, Aryan, A, Kumar, B, Volvach, LN, Lamb, GP, and Valeev, AF
Subjects: gamma-rays: general, X-ray: bursts, techniques: photometric, radiation mechanims : non-thermalonova, astro-ph.HE, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We investigate the prompt emission and the afterglow properties of short-duration gamma-ray burst (sGRB) 130603B and another eight sGRB events during 2012-2015, observed by several multiwavelength facilities including the Gran Canarias Telescope 10.4 m telescope. Prompt emission high energy data of the events were obtained by INTEGRAL-SPI-ACS, Swift-BAT, and Fermi-GBM satellites. The prompt emission data by INTEGRAL in the energy range of 0.1-10 MeV for sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A, and sGRB 151228A do not show any signature of the extended emission or precursor activity and their spectral and temporal properties are similar to those seen in case of other short bursts. For sGRB 130603B, our new afterglow photometric data constrain the pre-jet-break temporal decay due to denser temporal coverage. For sGRB 130603B, the afterglow light curve, containing both our new and previously published photometric data is broadly consistent with the ISM afterglow model. Modeling of the host galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software supports a scenario in which the environment of the burst is undergoing moderate star formation activity. From the inclusion of our late-time data for eight other sGRBs we are able to: place tight constraints on the non-detection of the afterglow, host galaxy, or any underlying 'kilonova' emission. Our late-time afterglow observations of the sGRB 170817A/GW170817 are also discussed and compared with the sub-set of sGRBs.
Published: 2019

4. iPTF16fnl: A Faint and Fast Tidal Disruption Event in an E+A Galaxy

Author: Blagorodnova, N, Gezari, S, Hung, T, Kulkarni, SR, Cenko, SB, Pasham, DR, Yan, L, Arcavi, I, Ben-Ami, S, Bue, BD, Cantwell, T, Cao, Y, Castro-Tirado, AJ, Fender, R, Fremling, C, Gal-Yam, A, Ho, AYQ, Horesh, A, Hosseinzadeh, G, Kasliwal, MM, Kong, AKH, Laher, RR, Leloudas, G, Lunnan, R, Masci, FJ, Mooley, K, Neill, JD, Nugent, P, Powell, M, Valeev, AF, Vreeswijk, PM, Walters, R, and Wozniak, P
Subjects: Space Sciences, Astronomical Sciences, Physical Sciences, accretion, accretion disks, black hole physics, galaxies: nuclei, stars: individual, astro-ph.HE, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract: We present ground-based and Swift observations of iPTF16fnl, a likely tidal disruption event (TDE) discovered by the intermediate Palomar Transient Factory (iPTF) survey at 66.6 Mpc. The light curve of the object peaked at an absolute mag Mg = -17.2. The maximum bolometric luminosity (from optical and UV) was Lp ≃ (1.0 ± 0.15) × 1043erg s-1, an order of magnitude fainter than any other optical TDE discovered so far. The luminosity in the first 60 days is consistent with an exponential decay, with L ∝ e-(t-t0)/τ, where t0 = 57631.0 (MJD) and τ ≃ 15 days. The X-ray shows a marginal detection at LX = 2.41.9-1.1 × 1039 erg s-1 (Swift X-ray Telescope). No radio counterpart was detected down to 3σ, providing upper limits for monochromatic radio luminosities of νLν < 1.7 × 1036 erg s-1 and νLν < 2.3 × 1037 erg s-1 (Very Large Array, 6.1 and 22 GHz). The blackbody temperature, obtained from combined Swift UV and optical photometry, shows a constant value of 19,000 K. The transient spectrum at peak is characterized by broad He ii and Hα emission lines, with FWHMs of about 14,000 km s-1 and 10,000 km s-1, respectively. He i lines are also detected at λλ 5875 and 6678. The spectrum of the host is dominated by strong Balmer absorption lines, which are consistent with a post-starburst (E+A) galaxy with an age of ∼650 Myr and solar metallicity. The characteristics of iPTF16fnl make it an outlier on both luminosity and decay timescales, as compared to other optically selected TDEs. The discovery of such a faint optical event suggests a higher rate of tidal disruptions, as low-luminosity events may have gone unnoticed in previous searches.
Published: 2017

5. XIPE: The X-ray imaging polarimetry explorer

Author: Soffitta, P, Bellazzini, R, Bozzo, E, Burwitz, V, Castro-Tirado, AJ, Costa, E, Courvoisier, T, Feng, H, Gburek, S, Goosmann, R, Karas, V, Matt, G, Muleri, F, Nandra, K, Pearce, M, Poutanen, J, Reglero, V, Sabau Maria, D, Santangelo, A, Tagliaferri, G, Tenzer, C, Vink, J, Weisskopf, MC, Zane, S, Agudo, I, Antonelli, A, Attina, P, Baldini, L, Bykov, A, Carpentiero, R, Cavazzuti, E, Churazov, E, Del Monte, E, De Martino, D, Donnarumma, I, Doroshenko, V, Evangelista, Y, Ferreira, I, Gallo, E, Grosso, N, Kaaret, P, Kuulkers, E, Laranaga, J, Latronico, L, Lumb, DH, Macian, J, Malzac, J, Marin, F, Massaro, E, Minuti, M, Mundell, C, Ness, JU, Oosterbroek, T, Paltani, S, Pareschi, G, Perna, R, Petrucci, PO, Pinazo, HB, Pinchera, M, Rodriguez, JP, Roncadelli, M, Santovincenzo, A, Sazonov, S, Sgro, C, Spiga, D, Svoboda, J, Theobald, C, Theodorou, T, Turolla, R, Wilhelmi De Ona, E, Winter, B, Akbar, AM, Allan, H, Aloisio, R, Altamirano, D, Amati, L, Amato, E, Angelakis, E, Arezu, J, Atteia, JL, Axelsson, M, Bachetti, M, Ballo, L, Balman, S, Bandiera, R, Barcons, X, Basso, S, Baykal, A, Becker, W, Behar, E, Beheshtipour, B, Belmont, R, Berger, E, Bernardini, F, Bianchi, S, Bisnovatyi-Kogan, G, Blasi, P, Blay, P, Bodaghee, A, and Boer, M
Subjects: X-ray Astronomy, Polarimetry, X-ray optics, Gas Pixel Detector
Abstract: XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially-resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.
Published: 2016

6. The Large Observatory for x-ray timing

Author: Feroci, M, Herder, JW den, Bozzo, E, Barret, D, Brandt, S, Hernanz, M, van der Klis, M, Pohl, M, Santangelo, A, Stella, L, Watts, A, Wilms, J, Zane, S, Ahangarianabhari, M, Albertus, C, Alford, M, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Artigues, B, Atteia, J-L, Azzarello, P, Bakala, P, Baldazzi, G, Balman, S, Barbera, M, van Baren, C, Bhattacharyya, S, Baykal, A, Belloni, T, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bodin, P, Bombaci, I, Bidaud, J-M Bonnet, Boutloukos, S, Bradley, L, Braga, J, Brown, E, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jørgensen, C, Cackett, E, Cadoux, FR, Caïs, P, Caliandro, GA, Campana, R, Campana, S, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, AJ, Cavazzuti, E, Cerda-Duran, P, Chakrabarty, D, Château, F, Chenevez, J, Coker, J, Cole, R, Collura, A, Cornelisse, R, Courvoisier, T, Cros, A, Cumming, A, Cusumano, G, D'Ai, A, D'Elia, V, Del Monte, E, de Luca, A, de Martino, D, Dercksen, JPC, de Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Diebold, S, Di Salvo, T, Donnarumma, I, Drago, A, Durant, M, Emmanoulopoulos, D, Erkut, MH, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, and Favre, Y
Subjects: X-ray timing, X-ray spectroscopy, X-ray imaging, compact objects, X-ray detectors, microchannel plates, astro-ph.IM
Abstract: The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final downselection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supranuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m2 effective area, 2-30 keV, 240 eV spectral resolution, 1° collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study.
Published: 2014

7. A possible bright blue supernova in the afterglow of GRB 020305

Author: Gorosabel, J, Fynbo, JPU, Fruchter, A, Levan, A, Hjorth, J, Nugent, P, Castro-Tirado, AJ, Cerón, JM Castro, Rhoads, J, Bersier, D, and Burud, I
Subjects: gamma rays : bursts, techniques : photometric, astro-ph, Astronomical and Space Sciences, Astronomy & Astrophysics
Abstract: We report on ground-based and HST(+STIS) imaging of the afterglow and host galaxy of the Gamma-Ray Burst (GRB) of March 5, 2002. The GRB occurred in a R = 25.17 ± 0.14 galaxy, which apparently is part of an interacting system. The lightcurve of the optical afterglow shows a rebrightening, or at least a plateau, 12-16 days after the gamma-ray event. UBVRIK' multi-band imaging of the afterglow ∼12 days after the GRB reveals a blue spectral energy distribution (SED). The SED is consistent with a power-law with a spectral index of β= -0.63 ± 0.16, but there is tentative evidence for deviations away from a power-law. Unfortunately, a spectroscopic redshift has not been secured for GRB 020305. From the SED we impose a redshift upper limit of z ≲2.8, hence excluding the pseudo redshift of 4.6 reported for this burst. We discuss the possibilities for explaining the lightcurve, SED and host galaxy properties for GRB 020305. The most natural interpretation of the lightcurve and the SED is an associated supernova (SN). Our data can not precisely determine the redshift of the GRB. The most favoured explanation is a low redshift (z ∼ 0.2) SN, but a higher redshift (z ≳ 0.5) SN can not be excluded. We also discuss less likely scenarios not based on SNe, like a burst occurring in a z = 2.5 galaxy with an extinction curve similar to that of the Milky Way. © ESO 2005.
Published: 2005

8. The LOFT mission concept: a status update

Author: Feroci, M, Bozzo, E, Brandt, S, Hernanz, M, Van Der Klis, M, Liu, L, Orleanski, P, Pohl, M, Santangelo, A, Schanne, S, Stella, L, Takahashi, T, Tamura, H, Watts, A, Wilms, J, Zane, S, Zhang, S, Bhattacharyya, S, Agudo, I, Ahangarianabhari, M, Albertus, C, Alford, M, Alpar, A, Altamirano, D, Alvarez, L, Amati, L, Amoros, C, Andersson, N, Antonelli, A, Argan, A, Artigue, R, Artigues, B, Atteia, J, Azzarello, P, Bakala, P, Ballantyne, Dr, Baldazzi, G, Baldo, M, Balman, S, Barbera, M, Van Baren, C, Barret, D, Baykal, A, Begelman, M, Behar, E, Behar, O, Belloni, T, Bellutti, P, Bernardini, F, Bertuccio, G, Bianchi, S, Bianchini, A, Binko, P, Blay, P, Bocchino, F, Bode, M, Bodin, P, Bombaci, I, Bonnet Bidaud, J, Borghi, G, Boutloukos, S, Bouyjou, F, Bradley, L, Braga, J, Briggs, Ms, Brown, E, Buballa, M, Bucciantini, N, Burderi, L, Burgay, M, Bursa, M, Budtz-Jorgensen, C, Cackett, E, Cadoux, Fr, Cais, P, Caliandro, Ga, Campana, R, Campana, S, Cao, X, Capitanio, F, Casares, J, Casella, P, Castro-Tirado, Aj, Cavazzuti, E, Cavechi, Y, Celestin, S, Cerda-Duran, P, Chakrabarty, D, Chamel, N, Chateau, F, Chen, C, Chen, Y, Chenevez, J, Chernyakova, M, Coker, J, Cole, R, Collura, A, Coriat, M, Cornelisse, R, Costamante, L, Cros, A, Cui, W, Cumming, A, Cusumano, G, Czerny, B, D'Ai, A, D'Ammando, F, D'Elia, V, Dai, Z, Del Monte, E, De Luca, A, De Martino, D, Dercksen, Jpc, De Pasquale, M, De Rosa, A, Del Santo, M, Di Cosimo, S, Degenaar, N, Den Herder, Jw, Diebold, S, Di Salvo, T, Dong, Y, Donnarumma, I, Doroshenko, V, Doyle, G, Drake, Sa, Durant, M, Emmanoulopoulos, D, Enoto, T, Erkut, Mh, Esposito, P, Evangelista, Y, Fabian, A, Falanga, M, Favre, Y, Feldman, C, Fender, R, Feng, H, Ferrari, V, Ferrigno, C, Ficorella, F, Finger, M, Finger, Mh, Fraser, Gw, Frericks, M, Fullekrug, M, Fuschino, F, Gabler, M, Galloway, Dk, Galvez Sanchez, Jl, Gandhi, P, Gao, Z, Garcia-Berro, E, Gendre, B, Gevin, O, Gezari, S, Giles, Ab, Gilfanov, M, Giommi, P, Giovannini, G, Giroletti, M, Gogus, E, Goldwurm, A, Goluchova, K, Gotz, D, Gou, L, Gouiffes, C, Grandi, P, Grassi, M, Greiner, J, Grinberg, V, Groot, P, Gschwender, M, Gualtieri, L, Guedel, M, Guidorzi, C, Guy, L, Haas, D, Haensel, P, Hailey, M, Hamuguchi, K, Hansen, F, Hartmann, Dh, Haswell, Ca, Hebeler, K, Heger, A, Hempel, M, Hermsen, W, Homan, J, Hornstrup, A, Hudec, R, Huovelin, J, Huppenkothen, D, Inam, Sc, Ingram, A, In'Tzand, Jjm, Israel, G, Iwasawa, K, Izzo, L, Jacobs, Hm, Jetter, F, Johannsen, T, Jenke, Pa, Jonker, P, Jose, J, Kaaret, P, Kalamkar, M, Kalemci, E, Kanbach, G, Karas, V, Karelin, D, Kataria, D, Keek, L, Kennedy, T, Klochkov, D, Kluzniak, W, Koerding, E, Kokkotas, K, Komossa, S, Korpela, S, Kouveliotou, C, Kowalski, Af, Kreykenbohm, I, Kuiper, Lm, Kunneriath, D, Kurkela, A, Kuvvetli, I, La Franca, F, Labanti, C, Lai, D, Lamb, Fk, Lachaud, C, Laubert, Pp, Lebrun, F, Li, X, Liang, E, Limousin, O, Lin, D, Linares, M, Linder, D, Lodato, G, Longo, F, Lu, F, Lund, N, Maccarone, Tj, Macera, D, Maestre, S, Mahmoodifar, S, Maier, D, Malcovati, P, Malzac, J, Malone, C, Mandel, I, Mangano, V, Manousakis, A, Marelli, M, Margueron, J, Marisaldi, M, Markoff, Sb, Markowitz, A, Marinucci, A, Martindale, A, Martinez, G, Mchardy, Im, Medina-Tanco, G, Mehdipour, M, Melatos, A, Mendez, M, Mereghetti, S, Migliari, S, Mignani, R, Michalska, M, Mihara, T, Miller, Mc, Miller, Jm, Mineo, T, Miniutti, G, Morsink, S, Motch, C, Motta, S, Mouchet, M, Mouret, G, Mulacova, J, Muleri, F, Munoz-Darias, T, Negueruela, I, Neilsen, J, Neubert, T, Norton, Aj, Nowak, M, Nucita, A, O'Brien, P, Oertel, M, Olsen, Peh, Orienti, M, Orio, M, Orlandini, M, Osborne, Jp, Osten, R, Ozel, F, Pacciani, L, Paerels, F, Paltani, S, Paolillo, M, Papadakis, I, Papitto, A, Paragi, Z, Paredes, Jm, Patruno, A, Paul, B, Pederiva, F, Perinati, E, Pellizzoni, A, Penacchioni, Av, Peretz, U, Perez, Ma, Perez-Torres, M, Peterson, Bm, Petracek, V, Picciotto, A, Piemonte, C, Pittori, C, Pons, J, Portell, J, Possenti, A, Postnov, K, Poutanen, J, Prakash, M, Prandoni, I, Le Provost, H, Psaltis, D, Pye, J, Qu, J, Rambaud, D, Ramon, P, Ramsay, G, Rapisarda, M, Rachevski, A, Rashevskaya, I, Ray, Ps, Rea, N, Reddy, S, Reig, P, Reina Aranda, M, Remillard, R, Reynolds, C, Rezzolla, L, Ribo, M, De La Rie, R, Riggio, A, Rios, A, Rischke, Dh, Rodriguez-Gil, P, Rodriguez, J, Rohlfs, R, Romano, P, Rossi, Emr, Rozanska, A, Rousseau, A, Rudak, B, Russell, Dm, Ryde, F, Sabau-Graziati, L, Sakamoto, T, Sala, G, Salvaterra, R, Salvetti, D, Sanna, A, Sandberg, J, Savolainen, T, Scaringi, S, Schaffner-Bielich, J, Schatz, H, Schee, J, Schmid, C, Serino, M, Shakura, N, Shore, S, Schnittman, Jd, Schneider, R, Schwenk, A, Schwope, Ad, Sedrakian, A, Seyler, J, Shearer, A, Slowikowska, A, Sims, M, Smith, A, Smith, Dm, Smith, Pj, Sobolewska, M, Sochora, V, Soffitta, P, Soleri, P, Song, L, Spencer, A, Stamerra, A, Stappers, B, Staubert, R, Steiner, Aw, Stergioulas, N, Stevens, Al, Stratta, G, Strohmayer, Te, Stuchlik, Z, Suchy, S, Suleimanov, V, Tamburini, F, Tauris, T, Tavecchio, F, Tenzer, C, Thielemann, Fk, Tiengo, A, Tolos, L, Tombesi, F, Tomsick, J, Torok, G, Torrejon, Jm, Torres, Df, Torresi, E, Tramacere, A, Traulsen, I, Trois, A, Turolla, R, Turriziani, S, Typel, S, Uter, P, Uttley, P, Vacchi, A, Varniere, P, Vaughan, S, Vercellone, S, Vietri, M, Vincent, Fh, Vrba, V, Walton, D, Wang, J, Wang, Z, Watanabe, S, Wawrzaszek, R, Webb, N, Weinberg, N, Wende, H, Wheatley, P, Wijers, R, Wijnands, R, Wille, M, Wilson-Hodge, Ca, Winter, B, Walk, Sj, Wood, K, Woosley, Se, Wu, X, Xiao, L, Xu, R, Yu, W, Yuan, F, Yuan, W, Yuan, Y, Zampa, G, Zampa, N, Zampieri, L, Zdunik, L, Zdziarski, A, Zech, A, Zhang, B, Zhang, C, Zingale, M, Zorzi, N, Zwart, F, High Energy Astrophys. & Astropart. Phys (API, FNWI), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Icahn School of Medicine at Mount Sinai [New York] (MSSM), Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers), Institut für Astronomie und Astrophysik [Tübingen] (IAAT), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Astrophysique Interprétation Modélisation (AIM (UMR7158 / 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), Dipartimento di Scienze e Tecnologie Chimiche, Università degli Studi di Roma Tor Vergata [Roma], Graduate School of the Natural Science and Technology [Kanazawa], Kanazawa University (KU), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Centre Interdisciplinaire de Nanoscience de Marseille (CINaM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Tampere University of Technology [Tampere] (TUT), University of Maryland [College Park], University of Maryland System, Department of Biological Sciences [Mississippi], University of Southern Mississippi (USM), School of Physics and Astronomy [Southampton], University of Southampton, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), Università di Roma La Sapienza, Università di Roma Tor Vergata, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Swedish Institute of Space Physics [Uppsala] (IRF), INAF - Osservatorio Astronomico di Brera (OAB), Department of Computer Sciences [Scheffield], University of Sheffield [Sheffield], Colgate University, Bibliothèque nationale de France (BnF), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), ARC Centre of Excellence for Environmental Decisions (ARC CEED), The University of Western Australia (UWA)-Australian National University (ANU)-University of Queensland [Brisbane]-Royal Melbourne Institute of Technology University (RMIT University)-School of BioSciences [Melbourne], Faculty of Science [Melbourne], University of Melbourne-University of Melbourne-Faculty of Science [Melbourne], University of Melbourne-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies (CoralCoE), James Cook University (JCU), Lund University [Lund], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse (AMIS), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de synthèse organique (DCSO), École polytechnique (X)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), University of Alabama at Birmingham [ Birmingham] (UAB), INAF - Osservatorio Astronomico di Cagliari (OAC), ELECTRONIQUE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Modèles Statistiques (LPTMS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), School of Geosciences, Monash University [Clayton], Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), 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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-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 d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université libre de Bruxelles (ULB), National Oceanography Centre [Southampton] (NOC), Dublin Institute for Advanced Studies (DIAS), Dublin City University [Dublin] (DCU), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Institut Parisien de Chimie Moléculaire (IPCM), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), China Information Technology Security Evaluation Center (CNITSEC), Department of Applied Mathematics and Computer Science [Lyngby] (DTU Compute), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), PCAS, Anton Pannekoek Institute for Astronomy, Institute of Astronomy [Cambridge], University of Cambridge [UK] (CAM), International Space Science Institute [Bern] (ISSI), Université Grenoble Alpes - UFR Médecine (UGA UFRM), Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), CALVIN research group [Edinburgh], Institute of Perception, Action and Behaviour (IPAB), University of Edinburgh-University of Edinburgh, Department of Electronics and Electrical Engineering [Bath], University of Bath [Bath], United States Geological Survey [Reston] (USGS), Sr. PLM Consultant, AstroParticule et Cosmologie (APC (UMR_7164)), 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, Dept Ind Engn & Informat Techonolgy, Università degli studi di Trieste = University of Trieste, Max-Planck-Institut für Extraterrestrische Physik (MPE), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Matériaux, ingénierie et science [Villeurbanne] (MATEIS), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Wisconsin Regional Primate Research Center, University of Wisconsin-Madison, SRON Netherlands Institute for Space Research (SRON), Opole University of Technology, University of Technology (Opole), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud University [Nijmegen]-Radboud University [Nijmegen], Radboud University [Nijmegen], NASA Goddard Space Flight Center (GSFC), Dept Fis Aplicada, Universidad de Granada = University of Granada (UGR), Victoria University [Melbourne], The Hong Kong Polytechnic University [Hong Kong] (POLYU), Chinese Academy of Sciences [Changchun Branch] (CAS), Department of Physics, Chemistry and Biology [Linköping] (IFM), Linköping University (LIU), Institut de Chimie des Substances Naturelles (ICSN), Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire de Lyon (IPNL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Centre de recherche en Biologie cellulaire de Montpellier (CRBM), Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Institute of Astronomy, University of Zielona Góra, Department of Electronics and Computer Systems, Takushoku University, Instituto Nacional de Pesquisas da Amazônia (INPA), Università degli studi di Catania = University of Catania (Unict), Centre d'Ecologie et des Sciences de la COnservation (CESCO), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Ecologie Alpine (LECA ), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS), HEPL, Solar Physics, Stanford University, Institut des Sciences Moléculaires de Marseille (ISM2), Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Space Telescope Science Institute (STSci), Dipartimento di Scienze Fisiche [Naples], University of Naples Federico II = Università degli studi di Napoli Federico II, Columbia University [New York], Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Department of Anthropology [University of Arkansas], University of Arkansas [Fayetteville], Hu county ventre for disease control and prevention of Shaanxi province, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Istituto Nazionale di Fisica Nucleare (INFN), Institut Jean le Rond d'Alembert (DALEMBERT), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institut de Ciencies de l'Espai [Barcelona] (ICE-CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Reading (UOR), Departamento de Matemática Aplicada, Universidade de Santiago de Compostela [Spain] (USC ), Osservatorio Astrofisico di Catania, Équipe Robotique et InteractionS (LAAS-RIS), Laboratoire d'analyse et d'architecture des systèmes (LAAS), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Centro Euro-Mediterraneo per i Cambiamenti Climatici [Bologna] (CMCC), Institut für Theoretische Physik, Universität Heidelberg [Heidelberg] = Heidelberg University, Augsburg Hospital, Leibniz-Institut für Astrophysik Potsdam (AIP), Daimler Chrysler AG (Daimler), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Montserrat Volcano Observatory (MVO), Institut Armand Frappier (INRS-IAF), Institut National de la Recherche Scientifique [Québec] (INRS)-Réseau International des Instituts Pasteur (RIIP), Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], FICLIT, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Max-Planck-Institut für Radioastronomie (MPIFR), Argelander-Institut für Astronomie (AlfA), Rheinische Friedrich-Wilhelms-Universität Bonn, Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Christian-Albrechts-Universität zu Kiel (CAU), Dipartimento di Fisica e Astronomia 'Galileo Galilei', Università degli Studi di Padova = University of Padua (Unipd), APC - Gravitation (APC-Gravitation), 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)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Cahill Center for Astronomy and Astrophysics, California Institute of Technology (CALTECH), Xinjiang Astronomical Observatory, Mitsubishi Electric Research Laboratories (MERL), Mitsubishi Research Institute, Inc., School of Urban and Regional Planning, University of Southern California (USC), National University of Defense Technology [China], Princeton University, Department of Microtechnology and Nanoscience (MC2), Chalmers University of Technology [Gothenburg, Sweden], Feroci, M., Bozzo, E., Brandt, S., Hernanz, M., van der Klis, M., Liu, L., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Zhang, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, N., Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, E., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, P., Bombaci, I., Bonnet Bidaud, J., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M., Brown, E., Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Cais, P., Caliandro, G., Campana, R., Campana, S., Cao, X., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, C., Chen, Y., Chenevez, J., Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Z., Del Monte, E., De Luca, A., De Martino, D., Dercksen, J., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J., Diebold, S., DI SALVO, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, H., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D., Gálvez Sanchez, J., Gandhi, P., Gao, Z., Garcia Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, F., Hartmann, D., Haswell, C., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jenke, P., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A., Kreykenbohm, I., Kuiper, L., Kunneriath, D., Kurkela, A., Kuvvetli, I., La Franca, F., Labanti, C., Lai, D., Lamb, F., Lachaud, C., Laubert, P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, N., Maccarone, T., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., Mchardy, I., Medina Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Neubert, T., Norton, A., Nowak, M., Nucita, A., O'Brien, P., Oertel, M., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paerels, F., Paltani, S., Paolillo, M., Papadakis, I., Papitto, A., Paragi, Z., Paredes, J., Patruno, A., Paul, B., Pederiva, F., Perinati, E., Pellizzoni, A., Penacchioni, A., Peretz, U., Perez, M., Perez Torres, M., Peterson, B., Petracek, V., Pittori, C., Pons, J., Portell, J., Possenti, A., Postnov, K., Poutanen, J., Prakash, M., Prandoni, I., Le Provost, H., Psaltis, D., Pye, J., Qu, J., Rambaud, D., Ramon, P., Ramsay, G., Rapisarda, M., Rashevski, A., Rashevskaya, I., Ray, P., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., Rozanska, A., Rousseau, A., Rudak, B., Russell, D., Ryde, F., Sabau Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J., Schneider, R., Schwenk, A., Schwope, A., Sedrakian, A., Seyler, J., Shearer, A., Slowikowska, A., Sims, M., Smith, A., Smith, D., Smith, P., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A., Stergioulas, N., Stevens, A., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., Torresi, E., Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F., Vrba, V., Walton, D., Wang, J., Wang, Z., Watanabe, S., Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, M., Wilson Hodge, C., Winter, B., Walk, S., Wood, K., Woosley, S., Wu, X., Xu, R., Yu, W., Yuan, F., Yuan, W., Yuan, Y., Zampa, G., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, B., Zhang, C., Zingale, M., Zwart, F., University of Geneva [Switzerland], Eberhard Karls Universität Tübingen, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Graduate School of the Natural Science and Technology, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), School of BioSciences [Melbourne], University of Melbourne-University of Melbourne-Royal Melbourne Institute of Technology University (RMIT University)-University of Queensland [Brisbane]-Australian National University (ANU)-The University of Western Australia (UWA), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Université Libre de Bruxelles [Bruxelles] (ULB), Dublin City University, Dublin 9, Ireland, Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), China Information Technology Security Evaluation Center, Technical University of Denmark [Lyngby] (DTU), Université Grenoble Alpes (UGA), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), 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), University of Trieste, Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie Intégrative de la Cellule (I2BC), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées de Lyon (INSA Lyon), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Università degli Studi di Roma 'La Sapienza' [Rome], Radboud university [Nijmegen]-Radboud university [Nijmegen], Radboud university [Nijmegen], Universidad de Granada (UGR), Centre National de la Recherche Scientifique (CNRS), Centre de recherche en Biologie Cellulaire (CRBM), Université Montpellier 1 (UM1)-Université Montpellier 2 - Sciences et Techniques (UM2)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Catania [Catania], Laboratoire d'Ecologie Alpine (LECA), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Université du Littoral Côte d'Opale, Stanford University [Stanford], Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Aix Marseille Université (AMU), Università degli studi di Napoli Federico II, IFP Energies nouvelles (IFPEN), National Institute for Nuclear Physics (INFN), Institut Jean Le Rond d'Alembert (DALEMBERT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J), Ingénierie des Matériaux Polymères (IMP), Université de Lyon-Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Jean Monnet [Saint-Étienne] (UJM)-Centre National de la Recherche Scientifique (CNRS), Centro Euro-Mediterraneo per i Cambiamenti Climatici (CMCC), Universität Heidelberg [Heidelberg], Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP)-Institut National de la Recherche Scientifique [Québec] (INRS), Università di Bologna [Bologna] (UNIBO), University of California [Berkeley], University of California-University of California, Universita degli Studi di Padova, 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)-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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Chalmers University of Technology [Göteborg], Astronomy, Jan-Willem A. den Herder, Shouleh Nikzad, Kazuhiro Nakazawa, Van Der Klis, M., Liu, L. -P., Zhang, S. -N., Atteia, J. -L., Ballantyne, D. R., Van Baren, C., Bellutti, P., Bonnet Bidaud, J. -M., Borghi, G., Briggs, M. S., Budtz-Jorgensen, C., Cadoux, F. R., Caliandro, G. A., Castro-Tirado, A. J., Cerda-Duran, P., Chateau, F., D'Ai, A., Dercksen, J. P. C., Den Herder, J. W., Di Salvo, T., Drake, S. A., Erkut, M. H., Ficorella, F., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Garcia-Berro, E., Giles, A. B., Goluchova, K., Gotz, D., Hartmann, D. H., Haswell, C. A., Inam, S. C., In'Tzand, J. J. M., Jacobs, H. M., Jenke, P. A., Jose, J., Kalamkar, M., Kowalski, A. F., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Markoff, S. B., Martinez, G., Mchardy, I. M., Medina-Tanco, G., Miller, M. C., Miller, J. M., Mulacova, J., Munoz-Darias, T., Norton, A. J., Olsen, P. E. H., Osborne, J. P., Paredes, J. M., Penacchioni, A. V., Perez, M. A., Perez-Torres, M., Peterson, B. M., Picciotto, A., Piemonte, C., Rachevski, A., Ray, P. S., De La Rie, R., Rischke, D. H., Rodriguez-Gil, P., Rossi, E. M. R., Russell, D. M., Sabau-Graziati, L., Schaffner-Bielich, J., Schnittman, J. D., Schwope, A. D., Seyler, J. -Y., Smith, D. M., Smith, P. J., Steiner, A. W., Stevens, A. L., Strohmayer, T. E., Thielemann, F. K., Torrejon, J. M., Torres, D. F., Vincent, F. H., Wilson-Hodge, C. A., Walk, S. J., Woosley, S. E., Xiao, L., Zorzi, N., 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), Centre National de la Recherche Scientifique (CNRS)-Aix Marseille Université (AMU), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Institut de Chimie du CNRS (INC)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Montpellier 2 - Sciences et Techniques (UM2)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université Montpellier 1 (UM1), Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Muséum national d'Histoire naturelle (MNHN), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-École Centrale de Marseille (ECM)-Institut de Chimie du CNRS (INC), Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Department of Psychiatry (Icahn School of Medicine at Mount Sinai) ( ISMMS ), Rutgers, The State University of New Jersey [New Brunswick] ( RUTGERS ), Institut fur Astronomie und Astrophysik, Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Kanazawa University ( KU ), Department of Earth Sciences, University of Oxford [Oxford], Centre Interdisciplinaire de Nanoscience de Marseille ( CINaM ), Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Tampere University of Technology [Tampere] ( TUT ), University of Southern Mississippi ( USM ), University of Southampton [Southampton], Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), Istituto Nazionale di Astrofisica ( INAF ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), Osservatorio Astronomico di Brera ( INAF ), Bibliothèque nationale de France ( BnF ), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo ( IASF-Pa ), ARC Centre of Excellence for Environmental Decisions ( ARC CEED ), The University of Western Australia ( UWA ) -Australian National University ( ANU ) -University of Queensland [Brisbane]-RMIT University [Melbourne]-University of Melbourne, ARC Centre of Excellence for Coral Reef Studies ( CoralCoE ), James Cook University ( JCU ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Anthropologie Moléculaire et Imagerie de Synthèse ( AMIS ), PRES Université de Toulouse-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de synthèse organique ( DCSO ), École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Pathology, University of Alabama at Birmingham, University of Alabama at Birmingham Comprehensive Cancer Center, Birmingham, Alabama, INAF-Osservatorio di Cagliari, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique Théorique et Modèles Statistiques ( LPTMS ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Université Libre de Bruxelles [Bruxelles] ( ULB ), Ocean and Earth Sciences, National Oceanography Centre Southampton, Dublin Institute for advanced studies, 31 Fitzwilliam Place, Dublin 2, Ireland, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Institut Parisien de Chimie Moléculaire ( IPCM ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Chinese Academy of Sciences [Beijing] ( CAS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Applied Mathematics and Computer Science [Lyngby] ( DTU Compute ), Technical University of Denmark [Lyngby] ( DTU ), Institut für Astronomie und Astrophysik ( IAAT ), Anton Pannekoek Institute for Astronomy, University of Amsterdam, University of Cambridge [UK] ( CAM ), International Space Science Institute ( ISSI ), Université Grenoble Alpes - UFR Médecine ( UGA UFRM ), Université Grenoble Alpes ( UGA ), Institute of Perception, Action and Behaviour ( IPAB ), United States Geological Survey [Reston] ( USGS ), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux ( ARTEMIS ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Max-Planck-Institut für Extraterrestrische Physik ( MPE ), Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology ( MIT ), Institut de Physique du Globe de Paris ( IPGP ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie Intégrative de la Cellule ( I2BC ), Université Paris-Sud - Paris 11 ( UP11 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Centre National de la Recherche Scientifique ( CNRS ), Matériaux, ingénierie et science [Villeurbanne] ( MATEIS ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ) -Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ), University of Wisconsin-Madison [Madison], SRON Netherlands Institute for Space Research ( SRON ), University of Technology ( Opole ), Institute for Mathematics, Astrophysics and Particle Physics ( IMAPP ), Grp Fis Atmosfera, Ctr Andaluz Medio Ambiente CEAMA, Universidad de Granada ( UGR ), The Hong Kong Polytechnic University [Hong Kong] ( POLYU ), Chinese Academy of Sciences [Changchun Branch] ( CAS ), Department of Physics, Chemistry and Biology, Linköping University ( LIU ), Institut de Chimie des Substances Naturelles ( ICSN ), Centre National de la Recherche Scientifique ( CNRS ), Institut de Physique Nucléaire de Lyon ( IPNL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Astronomical Institute Anton Pannekoek ( AI PANNEKOEK ), University of Amsterdam [Amsterdam] ( UvA ), Erlangen Centre for Astroparticle Physics ( ECAP ), Friedrich-Alexander Universität Erlangen-Nürnberg ( FAU ), Centre de recherches de biochimie macromoléculaire ( CRBM ), Université Montpellier 1 ( UM1 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto Nacional de Pesquisas da Amazônia ( INPA ), Instituto Nacional de Pesquisas da Amazônia, Centre d'Ecologie et des Sciences de la COnservation ( CESCO ), Muséum National d'Histoire Naturelle ( MNHN ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Ecologie Alpine ( LECA ), Université Joseph Fourier - Grenoble 1 ( UJF ) -Université Savoie Mont Blanc ( USMB [Université de Savoie] [Université de Chambéry] ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Physico-Chimie de l'Atmosphère ( LPCA ), Université du Littoral Côte d'Opale-Centre National de la Recherche Scientifique ( CNRS ), Institut des Sciences Moléculaires de Marseille ( ISM2 ), Aix Marseille Université ( AMU ) -Ecole Centrale de Marseille ( ECM ) -Centre National de la Recherche Scientifique ( CNRS ), Space Telescope Science Institute ( STSci ), IFP Energies nouvelles ( IFPEN ), Laboratoire de Biométrie et Biologie Evolutive ( LBBE ), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique ( Inria ) -Centre National de la Recherche Scientifique ( CNRS ), University of Arkansas, Istituto Nazionale di Fisica Nucleare, Sezione di Trieste ( INFN, Sezione di Trieste ), National Institute for Nuclear Physics ( INFN ), Institut Jean Le Rond d'Alembert ( DALEMBERT ), Institut de Ciencies de l'Espai [Barcelona] ( ICE-CSIC ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), University of Reading ( UOR ), Universidade de Santiago de Compostela, Équipe Robotique et InteractionS ( LAAS-RIS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National Polytechnique [Toulouse] ( INP ) -Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Paul Sabatier - Toulouse 3 ( UPS ) -Centre National de la Recherche Scientifique ( CNRS ), Ingénierie des Matériaux Polymères - Site INSA Lyon ( IMP ), Université de Lyon-Université de Lyon-Institut National des Sciences Appliquées de Lyon ( INSA Lyon ), Université de Lyon-Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Université Jean Monnet [Saint-Étienne] ( UJM ) -Centre National de la Recherche Scientifique ( CNRS ), Leibniz-Institut für Astrophysik Potsdam ( AIP ), Daimler Chrysler AG ( Daimler ), Centre d'Etudes Nucléaires de Bordeaux Gradignan ( CENBG ), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Montserrat Volcano Observatory ( MVO ), Institut Armand Frappier ( INRS-IAF ), Institut National de la Recherche Scientifique [Québec] ( INRS ) -Réseau International des Instituts Pasteur ( RIIP ) -Institut Armand Frappier, Università di Bologna [Bologna] ( UNIBO ), Max-Planck-Institut für Radioastronomie, Argelander Institut für Astronomie, Bonn Universität [Bonn], Space Sciences Laboratory [Berkeley] ( SSL ), Christian-Albrechts-Universität zu Kiel ( CAU ), Universita degli Studi di Padova = University of Padua = Université de Padoue, APC - Gravitation ( APC-Gravitation ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Max-Planck-Institut-Max-Planck-Institut, California Institute of Technology ( CALTECH ), Mitsubishi Electric Research Laboratories ( MERL ), Mitsubishi Electric Research Laboratories, Institute for Astronomy, University of Amsterdam, The Netherland, University of Southern California ( USC ), National University of Defense Technology [Changsha], Department of Microtechnology and Nanoscience ( MC2 ), Université Chalmers, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Nice Sophia Antipolis (UNS), Université Paris-Sud - Paris 11 (UP11)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Aix Marseille Université (AMU)-École Centrale de Marseille (ECM)-Centre National de la Recherche Scientifique (CNRS), Den Herder, Jan-Willem A., Bautz, M., den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Liu, L. P., Zhang, S. N., Atteia, J. L., Bonnet Bidaud, J. M., Castro Tirado, A. J., D'Aı, A., den Herder, J. W., Gálvez Sanchez, J. L., In't Zand, J. J. M., Nucita, Achille, Seyler, J. Y., Wilson Hodge, C. A., Baldazzi, Giuseppe, Fuschino, Fabio, Bianchi, Stefano, Casella, Piergiorgio, DE ROSA, Alessandra, Giovannini, Gabriele, LA FRANCA, Fabio, Marinucci, Andrea, Paredes, M. J., Schneider, Raffaella, Vietri, Mario, 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), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), M., Feroci, E., Bozzo, S., Brandt, M., Hernanz, M., van der Kli, L. P., Liu, P., Orleanski, M., Pohl, A., Santangelo, S., Schanne, L., Stella, T., Takahashi, H., Tamura, A., Watt, J., Wilm, S., Zane, S. N., Zhang, S., Bhattacharyya, I., Agudo, M., Ahangarianabhari, C., Albertu, M., Alford, A., Alpar, D., Altamirano, L., Alvarez, L., Amati, C., Amoro, N., Andersson, A., Antonelli, A., Argan, R., Artigue, B., Artigue, J. L., Atteia, P., Azzarello, P., Bakala, D., Ballantyne, G., Baldazzi, M., Baldo, S., Balman, M., Barbera, C., van Baren, D., Barret, A., Baykal, M., Begelman, E., Behar, O., Behar, T., Belloni, F., Bernardini, G., Bertuccio, S., Bianchi, A., Bianchini, P., Binko, P., Blay, F., Bocchino, M., Bode, P., Bodin, I., Bombaci, J. M., Bonnet Bidaud, S., Boutlouko, F., Bouyjou, L., Bradley, J., Braga, M. S., Brigg, E., Brown, M., Buballa, N., Bucciantini, L., Burderi, M., Burgay, M., Bursa, C., Budtz Jørgensen, E., Cackett, F., Cadoux, P., Cai, G. A., Caliandro, R., Campana, S., Campana, X., Cao, F., Capitanio, J., Casare, P., Casella, A. J., Castro Tirado, E., Cavazzuti, Y., Cavechi, S., Celestin, P., Cerda Duran, D., Chakrabarty, N., Chamel, F., Château, C., Chen, Y., Chen, J., Chenevez, M., Chernyakova, J., Coker, R., Cole, A., Collura, M., Coriat, R., Cornelisse, L., Costamante, A., Cro, W., Cui, A., Cumming, G., Cusumano, B., Czerny, A., D'Aì, F., D'Ammando, V., D'Elia, Z., Dai, E., Del Monte, A., De Luca, D., De Martino, J. P. C., Dercksen, M., De Pasquale, A., De Rosa, M., Del Santo, S., Di Cosimo, N., Degenaar, J. W., den Herder, S., Diebold, T., Di Salvo, Y., Dong, I., Donnarumma, V., Doroshenko, G., Doyle, S. A., Drake, M., Durant, D., Emmanoulopoulo, T., Enoto, M. H., Erkut, P., Esposito, Y., Evangelista, A., Fabian, M., Falanga, Y., Favre, C., Feldman, R., Fender, H., Feng, V., Ferrari, C., Ferrigno, M., Finger, M. H., Finger, G. W., Fraser, M., Frerick, M., Fullekrug, F., Fuschino, M., Gabler, D. K., Galloway, J. L., Gálvez Sanchez, P., Gandhi, Z., Gao, E., Garcia Berro, B., Gendre, O., Gevin, S., Gezari, A. B., Gile, M., Gilfanov, P., Giommi, G., Giovannini, M., Giroletti, E., Gogu, A., Goldwurm, K., Goluchová, D., Götz, L., Gou, C., Gouiffe, P., Grandi, M., Grassi, J., Greiner, V., Grinberg, P., Groot, M., Gschwender, L., Gualtieri, M., Guedel, C., Guidorzi, L., Guy, D., Haa, P., Haensel, M., Hailey, K., Hamuguchi, F., Hansen, D. H., Hartmann, C. A., Haswell, K., Hebeler, A., Heger, M., Hempel, W., Hermsen, J., Homan, A., Hornstrup, R., Hudec, J., Huovelin, D., Huppenkothen, S. C., Inam, A., Ingram, J. J. M., In't Zand, G., Israel, K., Iwasawa, L., Izzo, H. M., Jacob, F., Jetter, T., Johannsen, P. A., Jenke, P., Jonker, J., Josè, P., Kaaret, K., Kalamkar, E., Kalemci, G., Kanbach, V., Kara, D., Karelin, D., Kataria, L., Keek, T., Kennedy, D., Klochkov, W., Kluzniak, E., Koerding, K., Kokkota, S., Komossa, S., Korpela, C., Kouveliotou, A. F., Kowalski, I., Kreykenbohm, L. M., Kuiper, D., Kunneriath, A., Kurkela, I., Kuvvetli, F., La Franca, C., Labanti, D., Lai, F. K., Lamb, C., Lachaud, P. P., Laubert, F., Lebrun, X., Li, E., Liang, O., Limousin, D., Lin, M., Linare, D., Linder, G., Lodato, F., Longo, F., Lu, N., Lund, T. J., Maccarone, D., Macera, S., Maestre, S., Mahmoodifar, D., Maier, P., Malcovati, J., Malzac, C., Malone, I., Mandel, V., Mangano, A., Manousaki, M., Marelli, J., Margueron, M., Marisaldi, S. B., Markoff, A., Markowitz, A., Marinucci, A., Martindale, G., Martínez, I. M., Mchardy, G., Medina Tanco, M., Mehdipour, A., Melato, M., Mendez, S., Mereghetti, S., Migliari, R., Mignani, M., Michalska, T., Mihara, M. C., Miller, J. M., Miller, T., Mineo, G., Miniutti, S., Morsink, C., Motch, S., Motta, M., Mouchet, G., Mouret, J., Mulačová, F., Muleri, T., Muñoz Daria, I., Negueruela, J., Neilsen, T., Neubert, A. J., Norton, M., Nowak, A., Nucita, P., O'Brien, M., Oertel, P. E. H., Olsen, M., Orienti, M., Orio, M., Orlandini, J. P., Osborne, R., Osten, F., Ozel, L., Pacciani, F., Paerel, S., Paltani, Paolillo, Maurizio, I., Papadaki, A., Papitto, Z., Paragi, J. M., Parede, A., Patruno, B., Paul, F., Pederiva, E., Perinati, A., Pellizzoni, A. V., Penacchioni, U., Peretz, M. A., Perez, M., Perez Torre, B. M., Peterson, V., Petracek, C., Pittori, J., Pon, J., Portell, A., Possenti, K., Postnov, J., Poutanen, M., Prakash, I., Prandoni, H., Le Provost, D., Psalti, J., Pye, J., Qu, D., Rambaud, P., Ramon, G., Ramsay, M., Rapisarda, A., Rashevski, I., Rashevskaya, P. S., Ray, N., Rea, S., Reddy, P., Reig, M., Reina Aranda, R., Remillard, C., Reynold, L., Rezzolla, M., Ribo, R., de la Rie, A., Riggio, A., Rio, D. H., Rischke, P., Rodríguez Gil, J., Rodriguez, R., Rohlf, P., Romano, E. M. R., Rossi, A., Rozanska, A., Rousseau, B., Rudak, D. M., Russell, F., Ryde, L., Sabau Graziati, T., Sakamoto, G., Sala, R., Salvaterra, D., Salvetti, A., Sanna, J., Sandberg, T., Savolainen, S., Scaringi, J., Schaffner Bielich, H., Schatz, J., Schee, C., Schmid, M., Serino, N., Shakura, S., Shore, J. D., Schnittman, R., Schneider, A., Schwenk, A. D., Schwope, A., Sedrakian, J. Y., Seyler, A., Shearer, A., Slowikowska, M., Sim, A., Smith, D. M., Smith, P. J., Smith, M., Sobolewska, V., Sochora, P., Soffitta, P., Soleri, L., Song, A., Spencer, A., Stamerra, B., Stapper, R., Staubert, A. W., Steiner, N., Stergioula, A. L., Steven, G., Stratta, T. E., Strohmayer, Z., Stuchlik, S., Suchy, V., Suleimanov, F., Tamburini, T., Tauri, F., Tavecchio, C., Tenzer, F. K., Thielemann, A., Tiengo, L., Tolo, F., Tombesi, J., Tomsick, G., Torok, J. M., Torrejon, D. F., Torre, E., Torresi, A., Tramacere, I., Traulsen, A., Troi, R., Turolla, S., Turriziani, S., Typel, P., Uter, P., Uttley, A., Vacchi, P., Varniere, S., Vaughan, S., Vercellone, M., Vietri, F. H., Vincent, V., Vrba, D., Walton, J., Wang, Z., Wang, S., Watanabe, R., Wawrzaszek, N., Webb, N., Weinberg, H., Wende, P., Wheatley, R., Wijer, R., Wijnand, M., Wille, C. A., Wilson Hodge, B., Winter, S. J., Walk, K., Wood, S. E., Woosley, X., Wu, R., Xu, W., Yu, F., Yuan, W., Yuan, Y., Yuan, G., Zampa, N., Zampa, L., Zampieri, L., Zdunik, A., Zdziarski, A., Zech, B., Zhang, C., Zhang, S., Zhang, M., Zingale, and F., Zwart
Subjects: X-ray timing, [ SDU.ASTR.GA ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Field of view, Astrophysics, 01 natural sciences, law.invention, law, Observatory, timing, 010303 astronomy & astrophysics, QB, Physics, microchannel plates. PROPORTIONAL COUNTER ARRAY, CALIBRATION, X-ray astronomy, Electronic, Optical and Magnetic Material, Applied Mathematics, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, X-ray detectors, Condensed Matter Physics, compact objects, X-ray spectroscopy, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], spectroscopy, Cosmic Vision, [ INFO ] Computer Science [cs], Silicon detector, Astrophysics::High Energy Astrophysical Phenomena, Condensed Matter Physic, Telescope, X-ray, Silicon detectors, Electronic, Optical and Magnetic Materials, Electrical and Electronic Engineering, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Electronic, [INFO]Computer Science [cs], Optical and Magnetic Materials, Spectral resolution, DETECTOR, ta115, X-ray astronomy, Silicon detectors, timing, spectroscopy, 010308 nuclear & particles physics, X-ray imaging, Applied Mathematic, Neutron star, QB460-466 Astrophysics, Large Observatory For x-ray Timing (LOFT), Large Area Detector (LAD), Wide Field Monitor (WFM), Large Area Silicon Drift Detectors (SDD), Gamma-ray burst
Abstract: The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, >8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission. © (2016) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
Published: 2016

9. BeppoSAX observations of GRS 1915+105

Author: Feroci M, Casella P, Costa E, Massaro E, Soffitta P, Belloni T, Castro Tirado AJ, Dhawan V, Frontera F, Harmon A, Mirabel F, Pooley G, Tavani M., MATT, Giorgio, Feroci, M, Casella, P, Costa, E, Massaro, E, Soffitta, P, Matt, Giorgio, Belloni, T, Castro Tirado, Aj, Dhawan, V, Frontera, F, Harmon, A, Mirabel, F, Pooley, G, and Tavani, M.
Abstract: The galactic superluminal source GRS 1915+105 was observed by BeppoSAX at several occasions from October 1996 to April 2000. In April 1999 the 2-10 keV light curve showed a long series of quasi regular pulses with a recurrence time of about 50 s. Some preliminary results of a spectral analysis are presented.
Published: 2001

10. The origin of the early time optical emission of Swift GRB 080310

Author: Littlejohns, OM, Willingale, R, O'Brien, PT, Beardmore, AP, Covino, S, Perley, DA, Tanvir, NR, Rol, E, Yuan, F, Akerlof, C, D'Avanzo, P, Bersier, DF, Castro-Tirado, AJ, Christian, P, Cobb, BE, Evans, PA, Filippenko, AV, Flewelling, H, Fugazza, D, Hoversten, EA, Kamble, AP, Kobayashi, S, Li, W, Morgan, AN, Mundell, CG, Page, K, Palazzi, E, Quimby, RM, Schulze, S, Steele, IA, Postigo, ADU, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, QC, QB
Abstract: We present broadband multi-wavelength observations of GRB 080310 at redshift z = 2.43. This burst was bright and long-lived, and unusual in having extensive optical and near IR follow-up during the prompt phase. Using these data we attempt to simultaneously model the gamma-ray, X-ray, optical and IR emission using a series of prompt pulses and an afterglow component. Initial attempts to extrapolate the high energy model directly to lower energies for each pulse reveal that a spectral break is required between the optical regime and 0.3 keV to avoid over predicting the optical flux. We demonstrate that afterglow emission alone is insufficient to describe all morphology seen in the optical and IR data. Allowing the prompt component to dominate the early-time optical and IR and permitting each pulse to have an independent low energy spectral indices we produce an alternative scenario which better describes the optical light curve. This, however, does not describe the spectral shape of GRB 080310 at early times. The fit statistics for the prompt and afterglow dominated models are nearly identical making it difficult to favour either. However one enduring result is that both models require a low energy spectral index consistent with self absorption for at least some of the pulses identified in the high energy emission model., 24 pages, 12 figures, 12 tables. Accepted to MNRAS
Published: 2012

11. Optical observations of the bright long duration peculiar GRB 021004 afterglow

Author: Pandey, SB, Sahu, DK, Resmi, L, Sagar, R, Anupama, GC, Bhattacharya, D, Mohan, V, Prabhu, TP, Bhatt, BC, Pandey, JC, Parihar, Padmaker, and Castro-Tirado, AJ
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Joint Astronomy Programme, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The CCD magnitudes in Johnson $B,V$ and Cousins $R$ and $I$ photometric passbands are determined for the bright long duration GRB 021004 afterglow from 2002 October 4 to 16 starting $\sim$ 3 hours after the $\gamma-$ray burst. Light curves of the afterglow emission in $B$,$V$,$R$ and $I$ passbands are obtained by combining these measurements with other published data. The earliest optical emission appears to originate in a revese shock. Flux decay of the afterglow shows a very uncommon variation relative to other well-observed GRBs. Rapid light variations, especially during early times ($\Delta t < 2$ days) is superposed on an underlying broken power law decay typical of a jetted afterglow. The flux decay constants at early and late times derived from least square fits to the light curve are $0.99\pm0.05$ and $2.0\pm0.2$ respectively, with a jet break at around 7 day. Comparison with a standard fireball model indicates a total extinction of $E(B-V)=0.20$ mag in the direction of the burst. Our low-resolution spectra corrected for this extinction provide a spectral slope $\beta = 0.6\pm0.02$. This value and the flux decay constants agree well with the electron energy index $p\sim 2.27$ used in the model. The derived jet opening angle of about $7^{\circ}$ implies a total emitted gamma-ray energy $E_{\gamma} = 3.5\times10^{50}$ erg at a cosmological distance of about 20 Gpc. Multiwavelength observations indicate association of this GRB with a star forming region, supporting the case for collapsar origin of long duration GRBs., Comment: 19 pages, 3 figures, BASI, 31, 19
Published: 2002

12. Discovery of the optical counterpart and early optical observations of GRB 990712

Author: Sahu, KC, Bakos, G, Menzies, JW, Bragaglia, A, Frontera, F, Piro, L, Albrow, MD, Bond, IA, Bower, R, Caldwell, JAR, Castro-Tirado, AJ, Courbin, F, Dominik, M, Fynbo, JU, Galama, T, Glazebrook, K, Greenhill, J, Gorosabel, J, Hearnshaw, J, Hill, K, Hjorth, J, Kane, S, Kilmartin, PM, Kouveliotou, C, Martin, R, Masetti, N, Maxted, P, Minniti, D, Moller, P, Muraki, Y, Nakamura, T, Noda, S, Ohnishi, K, Palazzi, E, van Paradijs, J, Pian, E, Pollard, KR, Rattenbury, NJ, Reid, M, Rol, E, Saito, T, Sackett, PD, Saizar, P, Tinney, C, Vermaak, P, Watson, R, Williams, A, Yock, P, Dar, A, and Kapteyn Astronomical Institute
Subjects: Astrophysics::High Energy Astrophysical Phenomena, GRB-970508, 28 FEBRUARY 1997, Astrophysics::Cosmology and Extragalactic Astrophysics, HUBBLE-SPACE-TELESCOPE, ERROR BOX, GAMMA-RAY BURST, GALAXY, cosmology : observations, AFTERGLOW, gamma rays : bursts, Astrophysics::Solar and Stellar Astrophysics, 25 APRIL 1998, EMISSION, Astrophysics::Galaxy Astrophysics, SUPERNOVA
Abstract: We present the discovery observations of the optical counterpart of the gamma-ray burst GRB 990712 taken 4.16 hr after the outburst and discuss its light curve observed in the V, R, and I bands during the first similar to 35 days after the outburst. The observed light curves were fitted with a power-law decay for the optical transient (OT), plus an additional component that was treated in two different ways. First, the additional component was assumed to be an underlying galaxy of constant brightness. The resulting slope of the decay is 0.97(-0.02)(+0.05), and the magnitudes of the underlying galaxy are V = 22.3 +/- 0.05, R = 21.75 +/- 0.05, and I = 21.35 +/- 0.05. Second, the additional component was assumed to be a galaxy plus an underlying supernova with a time-variable brightness identical to that of GRB 980425, appropriately scaled to the redshift of GRB 990712. The resulting slope of the decay is similar, but the goodness of fit is worse, which would imply that either this GRB is not associated with an underlying supernova or the underlying supernova is much fainter than the supernova associated with GRB 980425. The galaxy in this case is fainter: V = 22.7 +/- 0.05, R = 22.25 +/- 0.05, and I = 22.15 +/- 0.05, and the OT plus the underlying supernova at a given time is brighter. Measurements of the brightnesses of the OT and the galaxy by late-time Hubble Space Telescope observation and ground-based observations can thus assess the presence of an underlying supernova.
Published: 2000

13. Properties of Swift's intermediate bursts

Author: Veres, P, de Ugarte Postigo, A, Horvath, I, Bagoly, Z, Kann, D, Thöne, C, Balazs, L, D'Avanzo, P, Aloy, M, Foley, S, Campana, S, Mao, J, Jakobsson, P, Covino, S, Fynbo, J, Gorosabel, J, Castro Tirado, A, Nardini, M, Amati, L, Kann, DA, Thöne, CC, Balazs, LG, Aloy, MA, Fynbo, JPU, Castro Tirado, AJ, Amati, L., NARDINI, MARCO, Veres, P, de Ugarte Postigo, A, Horvath, I, Bagoly, Z, Kann, D, Thöne, C, Balazs, L, D'Avanzo, P, Aloy, M, Foley, S, Campana, S, Mao, J, Jakobsson, P, Covino, S, Fynbo, J, Gorosabel, J, Castro Tirado, A, Nardini, M, Amati, L, Kann, DA, Thöne, CC, Balazs, LG, Aloy, MA, Fynbo, JPU, Castro Tirado, AJ, Amati, L., and NARDINI, MARCO
Abstract: Based on their prompt, high-energy emission, gamma-ray bursts are usually classified into short-duration and long-duration classes. A third intermediate group has been identified on statistical grounds but its individual properties have not yet been studied in detail. Using the large sample of follow-up observations of GRBs produced during the Swift era we analyze the individual characteristics of this group. We find that intermediate bursts are significantly different from short GRBs but share many properties with long bursts, probably pointing to a common progenitor type. However, we find that intermediate bursts are significantly dimmer and have on average lower redshifts., Based on their prompt, high-energy emission, gamma-ray bursts are usually classified into short-duration and long-duration classes. A third intermediate group has been identified on statistical grounds but its individual properties have not yet been studied in detail. Using the large sample of follow-up observations of GRBs produced during the Swift era we analyze the individual characteristics of this group. We find that intermediate bursts are significantly different from short GRBs but share many properties with long bursts, probably pointing to a common progenitor type. However, we find that intermediate bursts are significantly dimmer and have on average lower redshifts. © 2011 American Institute of Physics.
Published: 2011

14. The effect of magnetic fields on gamma-ray bursts inferred from multi-wavelength observations of the burst of 23 January 1999

Author: Galama, TJ, Briggs, MS, Wijers, RAMJ, Rol, E, Band, D, van Paradijs, J, Kouveliotou, C, Preece, RD, Smith, IA, Tilanus, RPJ, de Bruyn, AG, Strom, RG, Pooley, G, Castro-Tirado, AJ, Tanvir, N, Robinson, C, Hurley, K, Heise, J, Telting, J, Rutten, RGM, Packham, C, Swaters, R, Fassia, A, Green, SF, Foster, MJ, Sagar, R, Pandey, AK, Nilakshi, [No Value], Yadav, RKS, Ofek, EO, Leibowitz, E, Ibbetson, P, Rhoads, J, Falco, E, Petry, C, Impey, C, Geballe, TR, Bhattacharya, D, and Kapteyn Astronomical Institute
Subjects: RADIO TELESCOPE, AFTERGLOW, Astrophysics::High Energy Astrophysical Phenomena, BATSE OBSERVATIONS, PHOTOMETRY, SPECTRA, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Gamma-ray bursts (GRBs) are thought to arise when an extremely relativistic outflow of particles from a massive explosion (the nature of which is still unclear) Interacts with material surrounding the site of the explosion. observations of the evolving changes in emission at many wavelengths allow us to Investigate the origin of the photons, and so potentially determine the nature of the explosion. Here we report the results of gamma-ray, optical, Infrared, submillimetre, millimetre and radio observations of the burst GRB990123 and Its afterglow. Our Interpretation of the data Indicates that the initial and afterglow emissions are associated with three distinct regions In the fireball. The peak flux of the afterglow, one day after the burst, has a lower frequency than observed for other bursts; this explains tbe short-lived radio emission. We suggest that the differences between bursts reflect variations In the magnetic-field strength in the afterglow-emitting regions.
Published: 1999

15. Properties of Swift's intermediate bursts

Author: de Ugarte Postigo, A, Horváth, I, Veres, P, Bagoly, Z, Kann, D, Thöne, C, Balazs, L, D'Avanzo, P, Aloy, M, Foley, S, Campana, S, Mao, J, Jakobsson, P, Covino, S, Fynbo, J, Gorosabel, J, Castro Tirado, A, Amati, L, Nardini, M, Kann, DA, Thöne, CC, Balazs, LG, Aloy, MA, Fynbo, JPU, Castro Tirado, AJ, NARDINI, MARCO, de Ugarte Postigo, A, Horváth, I, Veres, P, Bagoly, Z, Kann, D, Thöne, C, Balazs, L, D'Avanzo, P, Aloy, M, Foley, S, Campana, S, Mao, J, Jakobsson, P, Covino, S, Fynbo, J, Gorosabel, J, Castro Tirado, A, Amati, L, Nardini, M, Kann, DA, Thöne, CC, Balazs, LG, Aloy, MA, Fynbo, JPU, Castro Tirado, AJ, and NARDINI, MARCO
Abstract: Gamma-ray bursts are usually classified through their high-energy emission into short-duration and long-duration bursts. A third intermediate group has been identified on statistical grounds but its individual properties have not yet been studied in detail. Using the large sample of follow-up observations of GRBs produced during the Swift era we analyze the individual characteristics of this group. We find that intermediate bursts are significantly different from short GRBs but share many properties with long bursts, probably pointing to a common progenitor type. However, we find that intermediate bursts are significantly dimmer and have on average lower redshifts. © 2010 American Institute of Physics.
Published: 2010

16. Searching for differences in Swift’s intermediate GRBs

Author: de Ugarte Postigo, A, Horváth, I, Veres, P, Bagoly, Z, Kann, D, Thöne, C, Balazs, L, D’Avanzo, P, Aloy, M, Foley, S, Campana, S, Mao, J, Jakobsson, P, Covino, S, Fynbo, J, Gorosabel, J, Castro Tirado, A, Amati, L, Nardini, M, Kann, DA, Thöne, CC, Balazs, LG, Aloy, MA, Fynbo, JPU, Castro Tirado, AJ, NARDINI, MARCO, de Ugarte Postigo, A, Horváth, I, Veres, P, Bagoly, Z, Kann, D, Thöne, C, Balazs, L, D’Avanzo, P, Aloy, M, Foley, S, Campana, S, Mao, J, Jakobsson, P, Covino, S, Fynbo, J, Gorosabel, J, Castro Tirado, A, Amati, L, Nardini, M, Kann, DA, Thöne, CC, Balazs, LG, Aloy, MA, Fynbo, JPU, Castro Tirado, AJ, and NARDINI, MARCO
Abstract: Context. Gamma-ray bursts are usually classified in terms their high-energy emission into either short-duration or long-duration bursts, which presumably reflect two different types of progenitors. However, it has been shown on statistical grounds that a third, intermediate population is needed in this classification scheme, although an extensive study of the properties of this class has so far not been performed. The large amount of follow-up studies generated during the Swift era allows us to have a sufficient sample to attempt a study of this third population through the properties of their prompt emission and their afterglows. Aims. To understand the differences of the intermediate population, we study a sample of GRBs observed by Swift during its first four years of operation. The sample contains only bursts with measured redshifts since these data help us to derive intrinsic properties. Methods. We search for differences in the properties of the three groups of bursts, which we quantify using a Kolmogorov-Smirnov test whenever possible. Results. Intermediate bursts are found to be less energetic and have dimmer afterglows than long GRBs, especially when considering the X-ray light curves, which are on average one order of magnitude fainter than long bursts. There is a less significant trend in the redshift distribution that places intermediate bursts closer than long bursts. Except for this, intermediate bursts show similar properties to long bursts. In particular, they follow the Epeak versus Eiso correlation and have, on average, positive spectral lags with a distribution similar to that of long bursts. As for long GRBs, they normally have an associated supernova, although some intermediate bursts have been found to contain no supernova component. Conclusions. This study shows that intermediate bursts differ from short bursts, but exhibit no significant differences from long bursts apart from their lower brightness. We suggest that the physical difference be
Published: 2010

17. SUPPLEMENT: 'lOCALIZATION and BROADBAND FOLLOW-UP of the GRAVITATIONAL-WAVE TRANSIENT GW150914' (2016, ApJL, 826, L13)

Author: Abbott, BP, Abbott, R, Abbott, TD, Abernathy, MR, Acernese, F, Ackley, K, Adams, C, Adams, T, Addesso, P, Adhikari, RX, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, B, Allocca, A, Altin, PA, Anderson, SB, Anderson, WG, Arai, K, Araya, MC, Arceneaux, CC, Areeda, JS, Arnaud, N, Arun, KG, Ascenzi, S, Ashton, G, Ast, M, Aston, SM, Astone, P, Aufmuth, P, Aulbert, C, Babak, S, Bacon, P, Bader, MKM, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Barayoga, JC, Barclay, SE, Barish, BC, Barker, D, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Barthelmy, S, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Batch, JC, Baune, C, Bavigadda, V, Bazzan, M, Behnke, B, Bejger, M, Bell, AS, Bell, CJ, Berger, BK, Bergman, J, Bergmann, G, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhagwat, S, Bhandare, R, Bilenko, IA, Billingsley, G, Birch, J, Birney, R, Biscans, S, Bisht, A, Bitossi, M, Biwer, C, Bizouard, MA, Blackburn, JK, Blair, CD, Blair, DG, Blair, RM, Bloemen, S, Bock, O, Bodiya, TP, Boer, M, Bogaert, G, Bogan, C, Bohe, A, Bojtos, P, Bond, C, Bondu, F, Bonnand, R, Boom, BA, Bork, R, Boschi, V, Bose, S, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, PR, Braginsky, VB, Branchesi, M, Brau, JE, Briant, T, Brillet, A, Brinkmann, M, Brisson, V, Brockill, P, Brooks, AF, Brown, DA, Brown, DD, Brown, NM, Buchanan, CC, Buikema, A, Bulik, T, Bulten, HJ, Buonanno, A, Buskulic, D, Buy, C, Byer, RL, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, JC, Callister, T, Calloni, E, Camp, JB, Cannon, KC, Cao, J, Capano, CD, Capocasa, E, Carbognani, F, Caride, S, Diaz, JC, Casentini, C, Caudill, S, Cavaglia, M, Cavalier, F, Cavalieri, R, Cella, G, Cepeda, CB, Baiardi, LC, Cerretani, G, Cesarini, E, Chakraborty, R, Chalermsongsak, T, Chamberlin, SJ, Chan, M, Chao, S, Charlton, P, Chassande-Mottin, E, Chen, HY, Chen, Y, Cheng, C, Chincarini, A, Chiummo, A, Cho, HS, Cho, M, Chow, JH, Christensen, N, Chu, Q, Chua, S, Chung, S, Ciani, G, Clara, F, Clark, JA, Cleva, F, Coccia, E, Cohadon, P-F, Colla, A, Collette, CG, Cominsky, L, Jr, Constancio M, Conte, A, Conti, L, Cook, D, Corbitt, TR, Cornish, N, Corsi, A, Cortese, S, Costa, CA, Coughlin, MW, Coughlin, SB, Coulon, J-P, Countryman, ST, Couvares, P, Cowan, EE, Coward, DM, Cowart, MJ, Coyne, DC, Coyne, R, Craig, K, Creighton, JDE, Cripe, J, Crowder, SG, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Danilishin, SL, D'Antonio, S, Danzmann, K, Darman, NS, Dattilo, V, Dave, I, Daveloza, HP, Davier, M, Davies, GS, Daw, EJ, Day, R, DeBra, D, Debreczeni, G, Degallaix, J, De Laurentis, M, Deleglise, S, Del Pozzo, W, Denker, T, Dent, T, Dereli, H, Dergachev, V, DeRosa, RT, De Rosa, R, DeSalvo, R, Dhurandhar, S, Diaz, MC, Di Fiore, L, Di Giovanni, M, Di Lieto, A, Di Pace, S, Di Palma, I, Di Virgilio, A, Dojcinoski, G, Dolique, V, Donovan, F, Dooley, KL, Doravari, S, Douglas, R, Downes, TP, Drago, M, Drever, RWP, Driggers, JC, Du, Z, Ducrot, M, Dwyer, SE, Edo, TB, Edwards, MC, Effler, A, Eggenstein, H-B, Ehrens, P, Eichholz, J, Eikenberry, SS, Engels, W, Essick, RC, Etzel, T, Evans, M, Evans, TM, Everett, R, Factourovich, M, Fafone, V, Fair, H, Fairhurst, S, Fan, X, Fang, Q, Farinon, S, Farr, B, Farr, WM, Favata, M, Fays, M, Fehrmann, H, Fejer, MM, Ferrante, I, Ferreira, EC, Ferrini, F, Fidecaro, F, Fiori, I, Fiorucci, D, Fisher, RP, Flaminio, R, Fletcher, M, Fournier, J-D, Franco, S, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fricke, TT, Fritschel, P, Frolov, VV, Fulda, P, Fyffe, M, Gabbard, HAG, Gair, JR, Gammaitoni, L, Gaonkar, SG, Garufi, F, Gatto, A, Gaur, G, Gehrels, N, Gemme, G, Gendre, B, Genin, E, Gennai, A, George, J, Gergely, L, Germain, V, Ghosh, A, Ghosh, S, Giaime, JA, Giardina, KD, Giazotto, A, Gill, K, Glaefke, A, Goetz, E, Goetz, R, Gondan, L, Gonzalez, G, Castro, JMG, Gopakumar, A, Gordon, NA, Gorodetsky, ML, Gossan, SE, Gosselin, M, Gouaty, R, Graef, C, Graff, PB, Granata, M, Grant, A, Gras, S, Gray, C, Greco, G, Green, AC, Groot, P, Grote, H, Grunewald, S, Guidi, GM, Guo, X, Gupta, A, Gupta, MK, Gushwa, KE, Gustafson, EK, Gustafson, R, Hacker, JJ, Hall, BR, Hall, ED, Hammond, G, Haney, M, Hanke, MM, Hanks, J, Hanna, C, Hannam, MD, Hanson, J, Hardwick, T, Haris, K, Harms, J, Harry, GM, Harry, IW, Hart, MJ, Hartman, MT, Haster, C-J, Haughian, K, Heidmann, A, Heintze, MC, Heitmann, H, Hello, P, Hemming, G, Hendry, M, Heng, IS, Hennig, J, Heptonstall, AW, Heurs, M, Hild, S, Hoak, D, Hodge, KA, Hofman, D, Hollitt, SE, Holt, K, Holz, DE, Hopkins, P, Hosken, DJ, Hough, J, Houston, EA, Howell, EJ, Hu, YM, Huang, S, Huerta, EA, Huet, D, Hughey, B, Husa, S, Huttner, SH, Huynh-Dinh, T, Idrisy, A, Indik, N, Ingram, DR, Inta, R, Isa, HN, Isac, J-M, Isi, M, Islas, G, Isogai, T, Iyer, BR, Izumi, K, Jacqmin, T, Jang, H, Jani, K, Jaranowski, P, Jawahar, S, Jimenez-Forteza, F, Johnson, WW, Jones, DI, Jones, R, Jonker, RJG, Ju, L, Kalaghatgi, CV, Kalogera, V, Kandhasamy, S, Kang, G, Kanner, JB, Karki, S, Kasprzack, M, Katsavounidis, E, Katzman, W, Kaufer, S, Kaur, T, Kawabe, K, Kawazoe, F, Kefelian, F, Kehl, MS, Keitel, D, Kelley, DB, Kells, W, Kennedy, R, Key, JS, Khalaidovski, A, Khalili, FY, Khan, I, Khan, S, Khan, Z, Khazanov, EA, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, N, Kim, Y-M, King, EJ, King, PJ, Kinzel, DL, Kissel, JS, Kleybolte, L, Klimenko, S, Koehlenbeck, SM, Kokeyama, K, Koley, S, Kondrashov, V, Kontos, A, Korobko, M, Korth, WZ, Kowalska, I, Kozak, DB, Kringel, V, Krolak, A, Krueger, C, Kuehn, G, Kumar, P, Kuo, L, Kutynia, A, Lackey, BD, Landry, M, Lange, J, Lantz, B, Lasky, PD, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lebigot, EO, Lee, CH, Lee, HK, Lee, HM, Lee, K, Lenon, A, Leonardi, M, Leong, JR, Leroy, N, Letendre, N, Levin, Y, Levine, BM, Li, TGF, Libson, A, Littenberg, TB, Lockerbie, NA, Logue, J, Lombardi, AL, Lord, JE, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, JD, Lueck, H, Lundgren, P, Luo, J, Lynch, R, Ma, Y, MacDonald, T, Machenschalk, B, MacInnis, M, Macleod, DM, Magana-Sandoval, F, Magee, RM, Mageswaran, M, Majorana, E, Maksimovic, I, Malvezzi, V, Man, N, Mandel, I, Mandic, V, Mangano, V, Mansell, GL, Manske, M, Mantovani, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markosyan, AS, Maros, E, Martelli, F, Martellini, L, Martin, IW, Martin, RM, Martynov, DV, Marx, JN, Mason, K, Masserot, A, Massinger, TJ, Masso-Reid, M, Matichard, F, Matone, L, Mavalvala, N, Mazumder, N, Mazzolo, G, McCarthy, R, McClelland, DE, McCormick, S, McGuire, SC, McIntyre, G, McIver, J, McManus, DJ, McWilliams, ST, Meacher, D, Meadors, GD, Meidam, J, Melatos, A, Mendell, G, Mendoza-Gandara, D, Mercer, RA, Merilh, E, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Meyers, PM, Mezzani, F, Miao, H, Michel, C, Middleton, H, Mikhailov, EE, Milano, L, Miller, J, Millhouse, M, Minenkov, Y, Ming, J, Mirshekari, S, Mishra, C, Mitra, S, Mitrofanov, VP, Mitselmakher, G, Mittleman, R, Moggi, A, Mohan, M, Mohapatra, SRP, Montani, M, Moore, BC, Moore, CJ, Moraru, D, Moreno, G, Morriss, SR, Mossavi, K, Mours, B, Mow-Lowry, CM, Mueller, CL, Mueller, G, Muir, AW, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Murphy, DJ, Murray, PG, Mytidis, A, Nardecchia, I, Naticchioni, L, Nayak, RK, Necula, V, Nedkova, K, Nelemans, G, Neri, M, Neunzert, A, Newton, G, Nguyen, TT, Nielsen, AB, Nissanke, S, Nitz, A, Nocera, F, Nolting, D, Normandin, MEN, Nuttall, LK, Oberling, J, Ochsner, E, O'Dell, J, Oelker, E, Ogin, GH, Oh, JJ, Oh, SH, Ohme, F, Oliver, M, Oppermann, P, Oram, RJ, O'Reilly, B, O'Shaughnessy, R, Ottaway, DJ, Ottens, RS, Overmier, H, Owen, BJ, Pai, A, Pai, SA, Palamos, JR, Palashov, O, Palliyaguru, N, Palomba, C, Pal-Singh, A, Pan, H, Pankow, C, Pannarale, F, Pant, BC, Paoletti, F, Paoli, A, Papa, MA, Paris, HR, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patricelli, B, Patrick, Z, Pearlstone, BL, Pedraza, M, Pedurand, R, Pekowsky, L, Pele, A, Penn, S, Perreca, A, Phelps, M, Piccinni, O, Pichot, M, Piergiovanni, F, Pierro, V, Pillant, G, Pinard, L, Pinto, IM, Pitkin, M, Poggiani, R, Popolizio, P, Post, A, Powell, J, Prasad, J, Predoi, V, Premachandra, SS, Prestegard, T, Price, LR, Prijatelj, M, Principe, M, Privitera, S, Prodi, GA, Prokhorov, L, Puncken, O, Punturo, M, Puppo, P, Puerrer, M, Qi, H, Qin, J, Quetschke, V, Quintero, EA, Quitzow-James, R, Raab, FJ, Rabeling, DS, Radkins, H, Raffai, P, Raja, S, Rakhmanov, M, Rapagnani, P, Raymond, V, Razzano, M, Re, V, Read, J, Reed, CM, Regimbau, T, Rei, L, Reid, S, Reitze, DH, Rew, H, Reyes, SD, Ricci, F, Riles, K, Robertson, NA, Robie, R, Robinet, F, Rocchi, A, Rolland, L, Rollins, JG, Roma, VJ, Romano, R, Romanov, G, Romie, JH, Rosinska, D, Rowan, S, Ruediger, A, Ruggi, P, Ryan, K, Sachdev, S, Sadecki, T, Sadeghian, L, Salconi, L, Saleem, M, Salemi, F, Samajdar, A, Sammut, L, Sanchez, EJ, Sandberg, V, Sandeen, B, Sanders, JR, Sassolas, B, Sathyaprakash, BS, Saulson, PR, Sauter, O, Savage, RL, Sawadsky, A, Schale, P, Schilling, R, Schmidt, J, Schmidt, P, Schnabel, R, Schofield, RMS, Schoenbeck, A, Schreiber, E, Schuette, D, Schutz, BF, Scott, J, Scott, SM, Sellers, D, Sentenac, D, Sequino, V, Sergeev, A, Serna, G, Setyawati, Y, Sevigny, A, Shaddock, DA, Shah, S, Shahriar, MS, Shaltev, M, Shao, Z, Shapiro, B, Shawhan, P, Sheperd, A, Shoemaker, DH, Shoemaker, DM, Siellez, K, Siemens, X, Sigg, D, Silva, AD, Simakov, D, Singer, A, Singh, A, Singh, R, Singhal, A, Sintes, AM, Slagmolen, BJJ, Smith, JR, Smith, ND, Smith, RJE, Son, EJ, Sorazu, B, Sorrentino, F, Souradeep, T, Srivastava, AK, Staley, A, Steinke, M, Steinlechner, J, Steinlechner, S, Steinmeyer, D, Stephens, BC, Stone, R, Strain, KA, Straniero, N, Stratta, G, Strauss, NA, Strigin, S, Sturani, R, Stuver, AL, Summerscales, TZ, Sun, L, Sutton, PJ, Swinkels, BL, SzczepaNczyk, MJ, Tacca, M, Talukder, D, Tanner, DB, Tpai, M, Tarabrin, SP, Taracchini, A, Taylor, R, Theeg, T, Thirugnanasambandam, P, Thomas, EG, Thomas, M, Thomas, P, Thorne, KA, Thorne, KS, Thrane, E, Tiwari, S, Tiwari, V, Tokmakov, KV, Tomlinson, C, Tonelli, M, Torres, CV, Torrie, CI, Tyr, D, Travasso, F, Traylor, G, Trifiro, D, Tringali, MC, Trozzo, L, Tse, M, Turconi, M, Tuyenbayev, D, Ugolini, D, Unnikrishnan, CS, Urban, AL, Usman, SA, Vahlbruch, H, Vajente, G, Valdes, G, van Bakel, N, van Beuzekom, M, van den Brand, JFJ, Van den Broeck, C, Vander-Hyde, DC, van der Schaaf, L, van Heijningen, JV, van Veggel, AA, Vardaro, M, Vass, S, Vasuth, M, Vaulin, R, Vecchio, A, Vedovato, G, Veitch, J, Veitch, PJ, Venkateswara, K, Verkindt, D, Vetrano, F, Vicere, A, Vinciguerra, S, Vine, DJ, Vinet, J-Y, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Voss, D, Vousden, WD, Vyatchanin, SP, Wade, AR, Wade, LE, Wade, M, Walker, M, Wallace, L, Walsh, S, Wang, G, Wang, H, Wang, M, Wang, X, Wang, Y, Ward, RL, Warner, J, Was, M, Weaver, B, Wei, L-W, Weinert, M, Weinstein, AJ, Weiss, R, Welborn, T, Wen, L, Wessels, P, Westphal, T, Wette, K, Whelan, JT, White, DJ, Whiting, BF, Williams, RD, Williamson, AR, Willis, JL, Willke, B, Wimmer, MH, Winkler, W, Wipf, CC, Wittel, H, Woan, G, Worden, J, Wright, JL, Wu, G, Yablon, J, Yam, W, Yamamoto, H, Yancey, CC, Yap, MJ, Yu, H, Yvert, M, Zadrozny, A, Zangrando, L, Zanolin, M, Zendri, J-P, Zevin, M, Zhang, F, Zhang, L, Zhang, M, Zhang, Y, Zhao, C, Zhou, M, Zhou, Z, Zhu, XJ, Zucker, ME, Zuraw, SE, Zweizig, J, Allison, J, Bannister, K, Bell, ME, Chatterjee, S, Chippendale, AP, Edwards, PG, Harvey-Smith, L, Heywood, Ian, Hotan, A, Indermuehle, B, Marvil, J, McConnell, D, Murphy, T, Popping, A, Reynolds, J, Sault, RJ, Voronkov, MA, Whiting, MT, Castro-Tirado, AJ, Cunniffe, R, Jelinek, M, Tello, JC, Oates, SR, Hu, Y-D, Kubanek, P, Guziy, S, Castellon, A, Garcia-Cerezo, A, Munoz, VF, Perez del Pulgar, C, Castillo-Carrion, S, Castro Ceron, JM, Hudec, R, Caballero-Garcia, MD, Pata, P, Vitek, S, Adame, JA, Konig, S, Rendon, F, Mateo Sanguino, T de J, Fernandez-Munoz, R, Yock, PC, Rattenbury, N, Allen, WH, Querel, R, Jeong, S, Park, IH, Bai, J, Cui, Ch, Fan, Y, Wang, Ch, Hiriart, D, Lee, WH, Claret, A, Sanchez-Ramirez, R, Pandey, SB, Mediavilla, T, Sabau-Graziati, L, Abbott, TMC, Abdalla, FB, Allam, S, Annis, J, Armstrong, R, Benoit-Levy, A, Berger, E, Bernstein, RA, Bertin, E, Brout, D, Buckley-Geer, E, Burke, DL, Capozzi, D, Carretero, J, Castander, FJ, Chornock, R, Cowperthwaite, PS, Crocce, M, Cunha, CE, D'Andrea, CB, da Costa, LN, Desai, S, Diehl, HT, Dietrich, JP, Doctor, Z, Drlica-Wagner, A, Drout, MR, Eifler, TF, Estrada, J, Evrard, AE, Fernandez, E, Finley, DA, Flaugher, B, Foley, RJ, Fong, W-F, Fosalba, P, Fox, DB, Frieman, J, Fryer, CL, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gutierrez, G, Herner, K, Honscheid, K, James, DJ, Johnson, MD, Johnson, MWG, Karliner, I, Kasen, D, Kent, S, Kessler, R, Kim, AG, Kind, MC, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Lin, H, Maia, MAG, Margutti, R, Marriner, J, Martini, P, Matheson, T, Melchior, P, Metzger, BD, Miller, CJ, Miquel, R, Neilsen, E, Nichol, RC, Nord, B, Nugent, P, Ogando, R, Petravick, D, Plazas, AA, Quataert, E, Roe, N, Romer, AK, Roodman, A, Rosell, AC, Rykoff, ES, Sako, M, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Scolnic, D, Sevilla-Noarbe, I, Sheldon, E, Smith, N, Smith, RC, Soares-Santos, M, Sobreira, F, Stebbins, A, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Thomas, RC, Tucker, DL, Vikram, V, Walker, AR, Wechsler, RH, Wester, W, Yanny, B, Zuntz, J, Connaughton, V, Burns, E, Goldstein, A, Briggs, MS, Zhang, B-B, Hui, CM, Jenke, P, Wilson-Hodge, CA, Bhat, PN, Bissaldi, E, Cleveland, W, Fitzpatrick, G, Giles, MM, Gibby, MH, Greiner, J, von Kienlin, A, Kippen, RM, McBreen, S, Mailyan, B, Meegan, CA, Paciesas, WS, Preece, RD, Roberts, O, Sparke, L, Stanbro, M, Toelge, K, Veres, P, Yu, H-F, Blackburn, L, Ackermann, M, Ajello, M, Albert, A, Anderson, B, Atwood, WB, Axelsson, M, Baldini, L, Barbiellini, G, Bastieri, D, Bellazzini, R, Blandford, RD, Bloom, ED, Bonino, R, Bottacini, E, Brandt, TJ, Bruel, P, Buson, S, Caliandro, GA, Cameron, RA, Caragiulo, M, Caraveo, PA, Cavazzuti, E, Charles, E, Chekhtman, A, Chiang, J, Chiaro, G, Ciprini, S, Cohen-Tanugi, J, Cominsky, LR, Costanza, F, Cuoco, A, D'Ammando, F, de Palma, F, Desiante, R, Digel, SW, Di Lalla, N, Di Mauro, M, Di Venere, L, Dominguez, A, Drell, PS, Dubois, R, Favuzzi, C, Ferrara, EC, Franckowiak, A, Fukazawa, Y, Funk, S, Fusco, P, Gargano, F, Gasparrini, D, Giglietto, N, Giommi, P, Giordano, F, Giroletti, M, Glanzman, T, Godfrey, G, Gomez-Vargas, GA, Green, D, Grenier, IA, Grove, JE, Guiriec, S, Hadasch, D, Harding, AK, Hays, E, Hewitt, JW, Hill, AB, Horan, D, Jogler, T, Johannesson, G, Johnson, AS, Kensei, S, Kocevski, D, Kuss, M, La Mura, G, Larsson, S, Latronico, L, Li, J, Li, L, Longo, F, Loparco, F, Lovellette, MN, Lubrano, P, Magill, J, Maldera, S, Manfreda, A, Marelli, M, Mayer, M, Mazziotta, MN, McEnery, JE, Meyer, M, Michelson, PF, Mirabal, N, Mizuno, T, Moiseev, AA, Monzani, ME, Moretti, E, Morselli, A, Moskalenko, IV, Negro, M, Nuss, E, Ohsugi, T, Omodei, N, Orienti, M, Orlando, E, Ormes, JF, Paneque, D, Perkins, JS, Pesce-Rollins, M, Piron, F, Pivato, G, Porter, TA, Racusin, JL, Raino, S, Rando, R, Razzaque, S, Reimer, A, Reimer, O, Salvetti, D, Parkinson, PM Saz, Sgro, C, Simone, D, Siskind, EJ, Spada, F, Spandre, G, Spinelli, P, Suson, DJ, Tajima, H, Thayer, JB, Thompson, DJ, Tibaldo, L, Torres, DF, Troja, E, Uchiyama, Y, Venters, TM, Vianello, G, Wood, KS, Wood, M, Zhu, S, Zimmer, S, Brocato, E, Cappellaro, E, Covino, S, Grado, A, Nicastro, L, Palazzi, E, Pian, E, Amati, L, Antonelli, LA, Capaccioli, M, D'Avanzo, P, D'Elia, V, Getman, F, Giuffrida, G, Iannicola, G, Limatola, L, Lisi, M, Marinoni, S, Marrese, P, Melandri, A, Piranomonte, S, Possenti, A, Pulone, L, Rossi, A, Stamerra, A, Stella, L, Testa, V, Tomasella, L, Yang, S, Bazzano, A, Bozzo, E, Brandt, S, Courvoisier, TJ-L, Ferrigno, C, Hanlon, L, Kuulkers, E, Laurent, P, Mereghetti, S, Roques, JP, Savchenko, V, Ubertini, P, Kasliwal, MM, Singer, LP, Cao, Y, Duggan, G, Kulkarni, SR, Bhalerao, V, Miller, AA, Barlow, T, Bellm, E, Manulis, I, Rana, J, Laher, R, Masci, F, Surace, J, Rebbapragada, U, Van Sistine, A, Sesar, B, Perley, D, Ferreti, R, Prince, T, Kendrick, R, Horesh, A, Hurley, K, Golenetskii, SV, Aptekar, RL, Frederiks, DD, Svinkin, DS, Rau, A, Zhang, X, Smith, DM, Cline, T, Krimm, H, Abe, F, Doi, M, Fujisawa, K, Kawabata, KS, Morokuma, T, Motohara, K, Tanaka, M, Ohta, K, Yanagisawa, K, Yoshida, M, Baltay, C, Rabinowitz, D, Ellman, N, Rostami, S, Bersier, DF, Bode, MF, Collins, CA, Copperwheat, CM, Darnley, MJ, Galloway, DK, Gomboc, A, Kobayashi, S, Mazzali, P, Mundell, CG, Piascik, AS, Pollacco, Don, Steele, IA, Ulaczyk, K, Broderick, JW, Fender, RP, Jonker, PG, Rowlinson, A, Stappers, BW, Wijers, RAMJ, Lipunov, V, Gorbovskoy, E, Tyurina, N, Kornilov, V, Balanutsa, P, Kuznetsov, A, Buckley, D, Rebolo, R, Serra-Ricart, M, Israelian, G, Budnev, NM, Gress, O, Ivanov, K, Poleshuk, V, Tlatov, A, Yurkov, V, Kawai, N, Serino, M, Negoro, H, Nakahira, S, Mihara, T, Tomida, H, Ueno, S, Tsunemi, H, Matsuoka, M, Croft, S, Feng, L, Franzen, TMO, Gaensler, BM, Johnston-Hollitt, M, Kaplan, DL, Morales, MF, Tingay, SJ, Wayth, RB, Williams, A, Smartt, SJ, Chambers, KC, Smith, KW, Huber, ME, Young, DR, Wright, DE, Schultz, A, Denneau, L, Flewelling, H, Magnier, EA, Primak, N, Rest, A, Sherstyuk, A, Stalder, B, Stubbs, CW, Tonry, J, Waters, C, Willman, M, Olivares E, F, Campbell, H, Kotak, R, Sollerman, J, Smith, M, Dennefeld, M, Anderson, JP, Botticella, MT, Chen, T-W, Valle, MD, Elias-Rosa, N, Fraser, M, Inserra, C, Kankare, E, Kupfer, T, Harmanen, J, Galbany, L, Le Guillou, L, Lyman, JD, Maguire, K, Mitra, A, Nicholl, M, Razza, A, Terreran, G, Valenti, S, Gal-Yam, A, Cwiek, A, Cwiok, M, Mankiewicz, L, Opiela, R, Zaremba, M, Zarnecki, AF, Onken, CA, Scalzo, RA, Schmidt, BP, Wolf, C, Yuan, F, Evans, PA, Kennea, JA, Burrows, DN, Campana, S, Cenko, SB, Marshall, FE, Nousek, J, O'Brien, P, Osborne, JP, Palmer, D, Perri, M, Siegel, M, Tagliaferri, G, Klotz, A, Turpin, D, Laugier, R, Beroiz, M, Penuela, T, Macri, LM, Oelkers, RJ, Lambas, DG, Vrech, R, Cabral, J, Colazo, C, Dominguez, M, Sanchez, B, Gurovich, S, Lares, M, Marshall, JL, Depoy, DL, Padilla, N, Pereyra, NA, Benacquista, M, Tanvir, NR, Wiersema, K, Levan, AJ, Steeghs, D, Hjorth, J, Fynbo, JPU, Malesani, D, Milvang-Jensen, B, Watson, D, Irwin, M, Fernandez, CG, McMahon, RG, Banerji, M, Gonzalez-Solares, E, Schulze, S, Postigo, A de U, Thoene, CC, Cano, Z, Rosswog, S, Colla, LIGO Sci Collaboration Virgo, Collaboration, ASKAP, Collaboration, BOOTES, Collaboration, Dark Energy Survey, Collabor, Dark Energy Camera GW-EM, Collaboration, Fermi GBM, Collaboration, FERMILAT, GRAWI, GRAvitational Wave Inaf TeAm, Collaboration, INTEGRAL, Collaboration, IPTF, Network, InterPlanetary, Collaboration, J-GEM, Survey, LA Silla-QUEST, Collaboration, Liverpool Telescope, Collabo, Low Frequency Array LOFAR, Collaboration, MASTER, Collaboration, MAXI, Collaboration, MWA, Collaboration, Pan-STARRS, Collaboration, PESSTO, Collaboration, Pi Sky, Collaboration, SkyMapper, Collaboration, Swift, Tarot, Zadko Algerian Natl Observ C, Collaboration, TOROS, Collaboration, VISTA, (Astro)-Particles Physics, 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., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, Enrico, Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavagliá, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. F., Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., Debra, D., Debreczeni, G., Degallaix, J., DE LAURENTIS, Martina, Deléglise, S., Pozzo, W. Del, Denker, T., Dent, T., Dereli, H., Dergachev, V., Derosa, R. T., DE ROSA, Rosario, Desalvo, R., Dhurandhar, S., Díaz, M. C., Fiore, L. Di, Giovanni, M. Di, Lieto, A. Di, Pace, S. Di, Palma, I. Di, Virgilio, A. Di, Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, Fabio, Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., Macdonald, T., Machenschalk, B., Macinnis, M., Macleod, D. M., Magaña Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcguire, S. C., Mcintyre, G., Mciver, J., Mcmanus, D. J., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, Leopoldo, Miller, J., Millhouse, M., Minenkov, Y., Ming, J., Mirshekari, S., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moggi, A., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, B. C., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mossavi, K., Mours, B., Mow Lowry, C. M., Mueller, C. L., Mueller, G., Muir, A. W., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Murphy, D. J., Murray, P. G., Mytidis, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Necula, V., Nedkova, K., Nelemans, G., Neri, M., Neunzert, A., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., O'Dell, J., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palliyaguru, N., Palomba, C., Pal Singh, A., Pan, H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Paris, H. R., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Patrick, Z., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perreca, A., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Predoi, V., Premachandra, S. S., Prestegard, T., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Qin, J., Quetschke, V., Quintero, E. A., Quitzow James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Reed, C. M., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Ricci, F., Riles, K., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romanov, G., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sanchez, E. J., Sandberg, V., Sandeen, B., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Schilling, R., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Scott, J., Scott, S. M., Sellers, D., Sentenac, D., Sequino, V., Sergeev, A., Serna, G., Setyawati, Y., Sevigny, A., Shaddock, D. A., Shah, S., Shahriar, M. S., Shaltev, M., Shao, Z., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sigg, D., Silva, A. D., Simakov, D., Singer, A., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, J. R., Smith, N. D., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strauss, N. A., Strigin, S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., Tápai, M., Tarabrin, S. P., Taracchini, A., Taylor, R., Theeg, T., Thirugnanasambandam, M. P., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Tomlinson, C., Tonelli, M., Torres, C. V., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Trifirò, D., Tringali, M. C., Trozzo, L., Tse, M., Turconi, M., Tuyenbayev, D., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Den Broeck, C., Vander Hyde, D. C., Van Der Schaaf, L., Van Heijningen, J. V., Van Veggel, A. A., Vardaro, M., Vass, S., Vasúth, M., Vaulin, R., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Verkindt, D., Vetrano, F., Viceré, A., Vinciguerra, S., Vine, D. J., Vinet, J. Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D., Vousden, W. D., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, M., Wang, X., Wang, Y., Ward, R. L., Warner, J., Was, M., Weaver, B., Wei, L. W., Weinert, M., Weinstein, A. J., Weiss, R., Welborn, T., Wen, L., Wessels, P., Westphal, T., Wette, K., Whelan, J. T., White, D. J., Whiting, B. F., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Worden, J., Wright, J. L., Wu, G., Yablon, J., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, H., Yvert, M., Zadrożny, A., Zangrando, L., Zanolin, M., Zendri, J. P., Zevin, M., Zhang, F., Zhang, L., Zhang, M., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zuraw, S. E., Zweizig, J., Allison, J., Bannister, K., Bell, M. E., Chatterjee, S., Chippendale, A. P., Edwards, P. G., Harvey Smith, L., Heywood, Ian, Hotan, A., Indermuehle, B., Marvil, J., Mcconnell, D., Murphy, T., Popping, A., Reynolds, J., Sault, R. J., Voronkov, M. A., Whiting, M. T., Castro Tirado, A. J., Cunniffe, R., Jelínek, M., Tello, J. C., Oates, S. R., Hu, Y. D., Kubánek, P., Guziy, S., Castellón, A., García Cerezo, A., Muñoz, V. F., Pérez Del Pulgar, C., Castillo Carrión, S., Castro Cerón, J. M., Hudec, R., Caballero García, M. D., Páta, P., Vitek, S., Adame, J. A., Konig, S., Rendón, F., Mateo Sanguino, T. De J., Fernández Muñoz, R., Yock, P. C., Rattenbury, N., Allen, W. H., Querel, R., Jeong, S., Park, I. H., Bai, J., Cui, C. h., Fan, Y., Wang, C. h., Hiriart, D., Lee, W. H., Claret, A., Sánchez Ramírez, R., Pandey, S. B., Mediavilla, T., Sabau Graziati, L., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Armstrong, R., Benoit Lévy, A., Berger, E., Bernstein, R. A., Bertin, E., Brout, D., Buckley Geer, E., Burke, D. L., Capozzi, D., Carretero, J., Castander, F. J., Chornock, R., Cowperthwaite, P. S., Crocce, M., Cunha, C. E., D'Andrea, C. B., Da Costa, L. N., Desai, S., Diehl, H. T., Dietrich, J. P., Doctor, Z., Drlica Wagner, A., Drout, M. R., Eifler, T. F., Estrada, J., Evrard, A. E., Fernandez, E., Finley, D. A., Flaugher, B., Foley, R. J., Fong, W. F., Fosalba, P., Fox, D. B., Frieman, J., Fryer, C. L., Gaztanaga, E., Gerdes, D. W., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Herner, K., Honscheid, K., James, D. J., Johnson, M. D., Johnson, M. W. G., Karliner, I., Kasen, D., Kent, S., Kessler, R., Kim, A. G., Kind, M. C., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Lin, H., Maia, M. A. G., Margutti, R., Marriner, J., Martini, P., Matheson, T., Melchior, P., Metzger, B. D., Miller, C. J., Miquel, R., Neilsen, E., Nichol, R. C., Nord, B., Nugent, P., Ogando, R., Petravick, D., Plazas, A. A., Quataert, E., Roe, N., Romer, A. K., Roodman, A., Rosell, A. C., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla Noarbe, I., Sheldon, E., Smith, N., Smith, R. C., Soares Santos, M., Sobreira, F., Stebbins, A., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Thomas, R. C., Tucker, D. L., Vikram, V., Walker, A. R., Wechsler, R. H., Wester, W., Yanny, B., Zuntz, J., Connaughton, V., Burns, E., Goldstein, A., Briggs, M. S., Zhang, B. B., Hui, C. M., Jenke, P., Wilson Hodge, C. A., Bhat, P. N., Bissaldi, E., Cleveland, W., Fitzpatrick, G., Giles, M. M., Gibby, M. H., Greiner, J., Kienlin, A. Von, Kippen, R. M., Mcbreen, S., Mailyan, B., Meegan, C. A., Paciesas, W. S., Preece, R. D., Roberts, O., Sparke, L., Stanbro, M., Toelge, K., Veres, P., Yu, H. F., Blackburn, L., Ackermann, M., Ajello, M., Albert, A., Anderson, B., Atwood, W. B., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Caliandro, G. A., Cameron, R. A., Caragiulo, M., Caraveo, P. A., Cavazzuti, E., Charles, E., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Cohen Tanugi, J., Cominsky, L. R., Costanza, F., Cuoco, A., D'Ammando, F., Palma, F. De, Desiante, R., Digel, S. W., Lalla, N. Di, Mauro, M. Di, Di Venere, L., Domínguez, A., Drell, P. S., Dubois, R., Favuzzi, C., Ferrara, E. C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., Mura, G. La, Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., Mcenery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Von Kienlin, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, Duncan K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., Olivares, E. F., Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. W., Valle, M. D., Elias Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., Depoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., Mcmahon, R. G., Banerji, M., Gonzalez Solares, E., Schulze, S., De Postigo, A. U., Thoene, C. C., Cano, Z., Rosswog, S., Calloni, E., De Laurentis, M., De Rosa, R., Garufi, F., Milano, L., Longo, Francesco, High Energy Astrophys. & Astropart. Phys (API, FNWI), CALTECH, Louisiana State Univ, Univ Salerno, Ist Nazl Fis Nucl, Univ Florida, LIGO Livingston Observ, Univ Savoie Mt Blanc, Max Planck Inst Gravitat Phys, Nikhef, MIT, Inst Nacl Pesquisas Espaciais, Interuniv Ctr Astron & Astrophys, Tata Inst Fundamental Res, Univ Wisconsin Milwaukee, Leibniz Univ Hannover, Univ Pisa, Australian Natl Univ, Univ Mississippi, Calif State Univ Fullerton, Univ Paris 11, Chennai Math Inst, Univ Roma Tor Vergata, Univ Southampton, Univ Hamburg, INFN, Universidade de São Paulo (USP), Montana State Univ, Univ Perugia, EGO, Syracuse Univ, Univ Glasgow, LIGO Hanford Observ, Wigner RCP, NASA, Columbia Univ, Stanford Univ, Univ Padua, CAMK PAN, Univ Birmingham, Univ Genoa, RRCAT, Lomonosov Moscow State Univ, Univ West Scotland, Univ Western Australia, Radboud Univ Nijmegen, Univ Cote dAzur, MTA Eotvos Univ, Univ Rennes 1, Washington State Univ, Univ Urbino Carlo Bo, Univ Oregon, UPMC, Warsaw Univ, Vrije Univ Amsterdam, Univ Maryland, Georgia Inst Technol, Univ Lyon 1, Univ Lyon, Univ Illes Balears, Univ Naples Federico II, Univ Toronto, Tsinghua Univ, Texas Tech Univ, Penn State Univ, Natl Tsing Hua Univ, Charles Sturt Univ, Univ Chicago, Caltech CaRT, Korea Inst Sci & Technol Informat, Carleton Coll, Univ Roma La Sapienza, Univ Brussels, Sonoma State Univ, Northwestern Univ, Univ Minnesota, Univ Melbourne, Univ Sheffield, Univ Sannio Benevento, Montclair State Univ, Univ Trento, Cardiff Univ, Natl Astron Observ Japan, Univ Edinburgh, Indian Inst Technol, Inst Plasma Res, Univ Szeged, Embry Riddle Aeronaut Univ, Univ Michigan, Amer Univ, Univ Massachusetts Amherst, Univ Adelaide, West Virginia Univ, Univ Bialystok, Univ Strathclyde, IISER TVM, Inst Appl Phys, Pusan Natl Univ, Hanyang Univ, NCBJ, IM PAN, Rochester Inst Technol, Monash Univ, Seoul Natl Univ, Univ Alabama, CNRS, Univ Camerino, Southern Univ, A&M Coll, Coll William & Mary, Universidade Estadual Paulista (Unesp), Univ Cambridge, IISER Kolkata, Rutherford Appleton Lab, Whitman Coll, Natl Inst Math Sci, Hobart & William Smith Coll, Univ Zielona Gora, Andrews Univ, Univ Siena, Trinity Univ, Univ Washington, Kenyon Coll, Abilene Christian Univ, CSIRO Astron & Space Sci, ARC Ctr Excellence All Sky Astrophys CAASTRO, Cornell Ctr Astrophys & Planetary Sci, Rhodes Univ, Univ Sydney, CSIC, Univ Malaga, Acad Sci Czech Republ, Nikolaev Natl Univ, ISDEFE SMOS FOS ESA ESAC, Czech Tech Univ, Estn Sondeos Atmosfer ESAt) El Arenosillo CEDEA I, Univ Huelva, IHSM UMA CSIC, Univ Auckland, Vintage Lane Observ, Natl Inst Water & Atmospher Res NIWA, Sungkyunkwan Univ SKKU, Chinese Acad Sci, Univ Nacl Autonoma Mexico, Aryabhatta Res Inst Observat Sci, Univ Cadiz, INTA, Natl Opt Astron Observ, UCL, Fermilab Natl Accelerator Lab, Princeton Univ, Univ Paris 06, Harvard Smithsonian Ctr Astrophys, Carnegie Observ, Univ Penn, SLAC Natl Accelerator Lab, Univ Portsmouth, IEEC CSIC, Barcelona Inst Sci & Technol, Ohio Univ, Lab Interinst E Astron LIneA, Excellence Cluster Univ, Univ Munich, Univ Illinois, Univ Arizona, Los Alamos Natl Lab, Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Natl Ctr Supercomp Applicat, Ohio State Univ, Australian Astron Observ, Texas A&M Univ, NYU, Columbia Astrophys Lab, Inst Catalana Recerca & Estudis Avancats, Univ Sussex, CIEMAT, Brookhaven Natl Lab, Argonne Natl Lab, Univ Manchester, Univ Space Res Assoc, Jacobs Technol Inc, Max Planck Inst Extraterr Phys, Univ Coll Dublin, NASA Headquarters, Tech Univ Munich, Deutsch Elektronen Synchrotron DESY, Clemson Univ, Stockholm Univ, AlbaNova, Univ Calif Santa Cruz, KTH Royal Inst Technol, Tokyo Metropolitan Univ, Univ Trieste, Univ Torino, CNRS IN2P3, Univ Maryland Baltimore Cty, CRESST, CIFS, Univ Bari, Politecn Bari, INAF Ist Astrofis Spaziale & Fis Cosm, ASI, George Mason Univ, Naval Res Lab, Univ Montpellier, INAF Ist Radioastron, Univ Bologna, Univ Telemat Pegaso, Univ Udine, Hiroshima Univ, Erlangen Ctr Astroparticle Phys, Pontificia Univ Catolica Chile, Univ Innsbruck, Univ North Florida, Univ Iceland, Max Planck Inst Phys & Astrophys, Univ Denver, Univ Johannesburg, Univ Hong Kong, NYCB Real Time Comp Inc, Purdue Univ Calumet, Nagoya Univ, Max Planck Inst Kernphys, ICREA, Dept Phys, INAF Osservatorio Astron Roma, INAF Osservatorio Astron Padova, INAF Osservatorio Astron Brera, INAF Osservatorio Astron Capodimonte, INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Scuola Normale Super Pisa, ASI Sci Data Ctr, INAF ORA Osservatorio Astron Cagliari, INAF Osservatorio Astron Torino, INAF Inst Space Astrophys & Planetol, Univ Geneva, Natl Space Inst Elektrovej, ESAC, INAF, Univ Toulouse, UPS OMP, IRAP, Weizmann Inst Sci, Max Planck Inst Astron, Niels Bohr Inst, Lockheed Martin Space Syst Co, Ioffe Phys Tech Inst, Univ Tokyo, Yamaguchi Univ, Kyoto Univ, Yale Univ, Liverpool JMU, Univ Nova Gorica, Univ Ljubljana, Univ Bath, Univ Warwick, Netherlands Inst Radio Astron, Univ Oxford, SRON Netherlands Inst Space Res, Univ Amsterdam, South African Astron Observ, Inst Astrofis Canarias, Irkutsk State Univ, RAS, Blagoveschensk State Pedag Univ, Tokyo Inst Technol, RIKEN, Nihon Univ, Japan Aerosp Explorat Agcy, Japan Aerosp Explorat Agcy JAXA, Osaka Univ, Eureka Sci Inc, Curtin Univ, Victoria Univ Wellington, Ist Nazl Astrofis, Queens Univ Belfast, Univ Hawaii Manoa, Space Telescope Sci Inst, Harvard Univ, Millennium Inst Astrophys, Univ Andres Bello, European Southern Observ, Univ Turku, Univ Chile, Las Cumbres Observ Global Telescope Network, Univ Calif Santa Barbara, Univ Warsaw, Polish Acad Sci, Univ Leicester, CNRS UMR 5277 UPS, Univ Texas San Antonio, Univ Nacl Cordoba, The LIGO Scientific Collaboration, The Virgo Collaboration, The Australian Square Kilometer Array, Pathfinder (ASKAP) Collaboration, The BOOTES Collaboration, The Dark Energy Survey and the Dark Energy Camera GW-EM Collaborations, The Fermi GBM Collaboration, The Fermi LAT Collaboration, The GRAvitational Wave Inaf TeAm (GRAWITA), The Intermediate Palomar Transient Factory (iPTF) Collaboration, The InterPlanetary Network, The J-GEM Collaboration, The La Silla--QUEST Survey, The Liverpool Telescope Collaboration, The Low Frequency Array (LOFAR) Collaboration, The MASTER Collaboration, The MAXI Collaboration, The Murchison Wide-field Array (MWA) Collaboration, The Pan-STARRS Collaboration, The PESSTO Collaboration, The Pi of the Sky Collaboration, The SkyMapper Collaboration, The Swift Collaboration, The TAROT, Zadko, Algerian National Observatory, C2PU Collaboration, The TOROS Collaboration, The VISTA Collaboration, Abbott BP, Abbott R, Abbott TD, Abernathy MR, Acernese F, Ackley K, Adams C, Adams T, Addesso P, Adhikari RX, Adya VB, Affeldt C, Agathos M, Agatsuma K, Aggarwal N, Aguiar OD, Aiello L, Ain A, Ajith P, Allen B, Allocca A, Altin PA, Anderson SB, Anderson WG, Arai K, Araya MC, Arceneaux CC, Areeda JS, Arnaud N, Arun KG, Ascenzi S, Ashton G, Ast M, Aston SM, Astone P, Aufmuth P, Aulbert C, Babak S, Bacon P, Bader MKM, Baker PT, Baldaccini F, Ballardin G, Ballmer SW, Barayoga JC, Barclay SE, Barish BC, Barker D, Barone F, Barr B, Barsotti L, Barsuglia M, Barta D, Barthelmy S, Bartlett J, Bartos I, Bassiri R, Basti A, Batch JC, Baune C, Bavigadda V, Bazzan M, Behnke B, Bejger M, Bell AS, Bell CJ, Berger BK, Bergman J, Bergmann G, Berry CPL, Bersanetti D, Bertolini A, Betzwieser J, Bhagwat S, Bhandare R, Bilenko IA, Billingsley G, Birch J, Birney R, Biscans S, Bisht A, Bitossi M, Biwer C, Bizouard MA, Blackburn JK, Blair CD, Blair DG, Blair RM, Bloemen S, Bock O, Bodiya TP, Boer M, Bogaert G, Bogan C, Bohe A, Bojtos P, Bond C, Bondu F, Bonnand R, Boom BA, Bork R, Boschi V, Bose S, Bouffanais Y, Bozzi A, Bradaschia C, Brady PR, Braginsky VB, Branchesi M, Brau JE, Briant T, Brillet A, Brinkmann M, Brisson V, Brockill P, Brooks AF, Brown DA, Brown DD, Brown NM, Buchanan CC, Buikema A, Bulik T, Bulten HJ, Buonanno A, Buskulic D, Buy C, Byer RL, Cadonati L, Cagnoli G, Cahillane C, Bustillo JC, Callister T, Calloni E, Camp JB, Cannon KC, Cao J, Capano CD, Capocasa E, Carbognani F, Caride S, Diaz JC, Casentini C, Caudill S, Cavaglia M, Cavalier F, Cavalieri R, Cella G, Cepeda CB, Baiardi LC, Cerretani G, Cesarini E, Chakraborty R, Chalermsongsak T, Chamberlin SJ, Chan M, Chao S, Charlton P, Chassande-Mottin E, Chen HY, Chen Y, Cheng C, Chincarini A, Chiummo A, Cho HS, Cho M, Chow JH, Christensen N, Chu Q, Chua S, Chung S, Ciani G, Clara F, Clark JA, Cleva F, Coccia E, Cohadon PF, Colla A, Collette CG, Cominsky L, Constancio M, Conte A, Conti L, Cook D, Corbitt TR, Cornish N, Corsi A, Cortese S, Costa CA, Coughlin MW, Coughlin SB, Coulon JP, Countryman ST, Couvares P, Cowan EE, Coward DM, Cowart MJ, Coyne DC, Coyne R, Craig K, Creighton JDE, Cripe J, Crowder SG, Cumming A, Cunningham L, Cuoco E, Dal Canton T, Danilishin SL, D'Antonio S, Danzmann K, Darman NS, Dattilo V, Dave I, Daveloza HP, Davier M, Davies GS, Daw EJ, Day R, DeBra D, Debreczeni G, Degallaix J, De Laurentis M, Deleglise S, Del Pozzo W, Denker T, Dent T, Dereli H, Dergachev V, DeRosa RT, De Rosa R, DeSalvo R, Dhurandhar S, Diaz MC, Di Fiore L, Di Giovanni M, Di Lieto A, Di Pace S, Di Palma I, Di Virgilio A, Dojcinoski G, Dolique V, Donovan F, Dooley KL, Doravari S, Douglas R, Downes TP, Drago M, Drever RWP, Driggers JC, Du Z, Ducrot M, Dwyer SE, Edo TB, Edwards MC, Effler A, Eggenstein HB, Ehrens P, Eichholz J, Eikenberry SS, Engels W, Essick RC, Etzel T, Evans M, Evans TM, Everett R, Factourovich M, Fafone V, Fair H, Fairhurst S, Fan X, Fang Q, Farinon S, Farr B, Farr WM, Favata M, Fays M, Fehrmann H, Fejer MM, Ferrante I, Ferreira EC, Ferrini F, Fidecaro F, Fiori I, Fiorucci D, Fisher RP, Flaminio R, Fletcher M, Fournier JD, Franco S, Frasca S, Frasconi F, Frei Z, Freise A, Frey R, Frey V, Fricke TT, Fritschel P, Frolov VV, Fulda P, Fyffe M, Gabbard HAG, Gair JR, Gammaitoni L, Gaonkar SG, Garufi F, Gatto A, Gaur G, Gehrels N, Gemme G, Gendre B, Genin E, Gennai A, George J, Gergely L, Germain V, Ghosh A, Ghosh S, Giaime JA, Giardina KD, Giazotto A, Gill K, Glaefke A, Goetz E, Goetz R, Gondan L, Gonzalez G, Castro JMG, Gopakumar A, Gordon NA, Gorodetsky ML, Gossan SE, Gosselin M, Gouaty R, Graef C, Graff PB, Granata M, Grant A, Gras S, Gray C, Greco G, Green AC, Groot P, Grote H, Grunewald S, Guidi GM, Guo X, Gupta A, Gupta MK, Gushwa KE, Gustafson EK, Gustafson R, Hacker JJ, Hall BR, Hall ED, Hammond G, Haney M, Hanke MM, Hanks J, Hanna C, Hannam MD, Hanson J, Hardwick T, Haris K, Harms J, Harry GM, Harry IW, Hart MJ, Hartman MT, Haster CJ, Haughian K, Heidmann A, Heintze MC, Heitmann H, Hello P, Hemming G, Hendry M, Heng IS, Hennig J, Heptonstall AW, Heurs M, Hild S, Hoak D, Hodge KA, Hofman D, Hollitt SE, Holt K, Holz DE, Hopkins P, Hosken DJ, Hough J, Houston EA, Howell EJ, Hu YM, Huang S, Huerta EA, Huet D, Hughey B, Husa S, Huttner SH, Huynh-Dinh T, Idrisy A, Indik N, Ingram DR, Inta R, Isa HN, Isac JM, Isi M, Islas G, Isogai T, Iyer BR, Izumi K, Jacqmin T, Jang H, Jani K, Jaranowski P, Jawahar S, Jimenez-Forteza F, Johnson WW, Jones DI, Jones R, Jonker RJG, Ju L, Kalaghatgi CV, Kalogera V, Kandhasamy S, Kang G, Kanner JB, Karki S, Kasprzack M, Katsavounidis E, Katzman W, Kaufer S, Kaur T, Kawabe K, Kawazoe F, Kefelian F, Kehl MS, Keitel D, Kelley DB, Kells W, Kennedy R, Key JS, Khalaidovski A, Khalili FY, Khan I, Khan S, Khan Z, Khazanov EA, Kijbunchoo N, Kim C, Kim J, Kim K, Kim N, Kim YM, King EJ, King PJ, Kinzel DL, Kissel JS, Kleybolte L, Klimenko S, Koehlenbeck SM, Kokeyama K, Koley S, Kondrashov V, Kontos A, Korobko M, Korth WZ, Kowalska I, Kozak DB, Kringel V, Krolak A, Krueger C, Kuehn G, Kumar P, Kuo L, Kutynia A, Lackey BD, Landry M, Lange J, Lantz B, Lasky PD, Lazzarini A, Lazzaro C, Leaci P, Leavey S, Lebigot EO, Lee CH, Lee HK, Lee HM, Lee K, Lenon A, Leonardi M, Leong JR, Leroy N, Letendre N, Levin Y, Levine BM, Li TGF, Libson A, Littenberg TB, Lockerbie NA, Logue J, Lombardi AL, Lord JE, Lorenzini M, Loriette V, Lormand M, Losurdo G, Lough JD, Luck H, Lundgren P, Luo J, Lynch R, Ma Y, MacDonald T, Machenschalk B, MacInnis M, Macleod DM, Magana-Sandoval F, Magee RM, Mageswaran M, Majorana E, Maksimovic I, Malvezzi V, Man N, Mandel I, Mandic V, Mangano V, Mansell GL, Manske M, Mantovani M, Marchesoni F, Marion F, Marka S, Marka Z, Markosyan AS, Maros E, Martelli F, Martellini L, Martin IW, Martin RM, Martynov DV, Marx JN, Mason K, Masserot A, Massinger TJ, Masso-Reid M, Matichard F, Matone L, Mavalvala N, Mazumder N, Mazzolo G, McCarthy R, McClelland DE, McCormick S, McGuire SC, McIntyre G, McIver J, McManus DJ, McWilliams ST, Meacher D, Meadors GD, Meidam J, Melatos A, Mendell G, Mendoza-Gandara D, Mercer RA, Merilh E, Merzougui M, Meshkov S, Messenger C, Messick C, Meyers PM, Mezzani F, Miao H, Michel C, Middleton H, Mikhailov EE, Milano L, Miller J, Millhouse M, Minenkov Y, Ming J, Mirshekari S, Mishra C, Mitra S, Mitrofanov VP, Mitselmakher G, Mittleman R, Moggi A, Mohan M, Mohapatra SRP, Montani M, Moore BC, Moore CJ, Moraru D, Moreno G, Morriss SR, Mossavi K, Mours B, Mow-Lowry CM, Mueller CL, Mueller G, Muir AW, Mukherjee A, Mukherjee D, Mukherjee S, Mukund N, Mullavey A, Munch J, Murphy DJ, Murray PG, Mytidis A, Nardecchia I, Naticchioni L, Nayak RK, Necula V, Nedkova K, Nelemans G, Neri M, Neunzert A, Newton G, Nguyen TT, Nielsen AB, Nissanke S, Nitz A, Nocera F, Nolting D, Normandin MEN, Nuttall LK, Oberling J, Ochsner E, O'Dell J, Oelker E, Ogin GH, Oh JJ, Oh SH, Ohme F, Oliver M, Oppermann P, Oram RJ, O'Reilly B, O'Shaughnessy R, Ottaway DJ, Ottens RS, Overmier H, Owen BJ, Pai A, Pai SA, Palamos JR, Palashov O, Palliyaguru N, Palomba C, Pal-Singh A, Pan H, Pankow C, Pannarale F, Pant BC, Paoletti F, Paoli A, Papa MA, Paris HR, Parker W, Pascucci D, Pasqualetti A, Passaquieti R, Passuello D, Patricelli B, Patrick Z, Pearlstone BL, Pedraza M, Pedurand R, Pekowsky L, Pele A, Penn S, Perreca A, Phelps M, Piccinni O, Pichot M, Piergiovanni F, Pierro V, Pillant G, Pinard L, Pinto IM, Pitkin M, Poggiani R, Popolizio P, Post A, Powell J, Prasad J, Predoi V, Premachandra SS, Prestegard T, Price LR, Prijatelj M, Principe M, Privitera S, Prodi GA, Prokhorov L, Puncken O, Punturo M, Puppo P, Purrer M, Qi H, Qin J, Quetschke V, Quintero EA, Quitzow-James R, Raab FJ, Rabeling DS, Radkins H, Raffai P, Raja S, Rakhmanov M, Rapagnani P, Raymond V, Razzano M, Re V, Read J, Reed CM, Regimbau T, Rei L, Reid S, Reitze DH, Rew H, Reyes SD, Ricci F, Riles K, Robertson NA, Robie R, Robinet F, Rocchi A, Rolland L, Rollins JG, Roma VJ, Romano R, Romanov G, Romie JH, Rosinska D, Rowan S, Rudiger A, Ruggi P, Ryan K, Sachdev S, Sadecki T, Sadeghian L, Salconi L, Saleem M, Salemi F, Samajdar A, Sammut L, Sanchez EJ, Sandberg V, Sandeen B, Sanders JR, Sassolas B, Sathyaprakash BS, Saulson PR, Sauter O, Savage RL, Sawadsky A, Schale P, Schilling R, Schmidt J, Schmidt P, Schnabel R, Schofield RMS, Schonbeck A, Schreiber E, Schuette D, Schutz BF, Scott J, Scott SM, Sellers D, Sentenac D, Sequino V, Sergeev A, Serna G, Setyawati Y, Sevigny A, Shaddock DA, Shah S, Shahriar MS, Shaltev M, Shao Z, Shapiro B, Shawhan P, Sheperd A, Shoemaker DH, Shoemaker DM, Siellez K, Siemens X, Sigg D, Silva AD, Simakov D, Singer A, Singh A, Singh R, Singhal A, Sintes AM, Slagmolen BJJ, Smith JR, Smith ND, Smith RJE, Son EJ, Sorazu B, Sorrentino F, Souradeep T, Srivastava AK, Staley A, Steinke M, Steinlechner J, Steinlechner S, Steinmeyer D, Stephens BC, Stone R, Strain KA, Straniero N, Stratta G, Strauss NA, Strigin S, Sturani R, Stuver AL, Summerscales TZ, Sun L, Sutton PJ, Swinkels BL, SzczepaNczyk MJ, Tacca M, Talukder D, Tanner DB, Tpai M, Tarabrin SP, Taracchini A, Taylor R, Theeg T, Thirugnanasambandam P, Thomas EG, Thomas M, Thomas P, Thorne KA, Thorne KS, Thrane E, Tiwari S, Tiwari V, Tokmakov KV, Tomlinson C, Tonelli M, Torres CV, Torrie CI, Tyr D, Travasso F, Traylor G, Trifiro D, Tringali MC, Trozzo L, Tse M, Turconi M, Tuyenbayev D, Ugolini D, Unnikrishnan CS, Urban AL, Usman SA, Vahlbruch H, Vajente G, Valdes G, van Bakel N, van Beuzekom M, van den Brand JFJ, Van den Broeck C, Vander-Hyde DC, van der Schaaf L, van Heijningen JV, van Veggel AA, Vardaro M, Vass S, Vasuth M, Vaulin R, Vecchio A, Vedovato G, Veitch J, Veitch PJ, Venkateswara K, Verkindt D, Vetrano F, Vicere A, Vinciguerra S, Vine DJ, Vinet JY, Vitale S, Vo T, Vocca H, Vorvick C, Voss D, Vousden WD, Vyatchanin SP, Wade AR, Wade LE, Wade M, Walker M, Wallace L, Walsh S, Wang G, Wang H, Wang M, Wang X, Wang Y, Ward RL, Warner J, Was M, Weaver B, Wei LW, Weinert M, Weinstein AJ, Weiss R, Welborn T, Wen L, Wessels P, Westphal T, Wette K, Whelan JT, White DJ, Whiting BF, Williams RD, Williamson AR, Willis JL, Willke B, Wimmer MH, Winkler W, Wipf CC, Wittel H, Woan G, Worden J, Wright JL, Wu G, Yablon J, Yam W, Yamamoto H, Yancey CC, Yap MJ, Yu H, Yvert M, Zadrozny A, Zangrando L, Zanolin M, Zendri JP, Zevin M, Zhang F, Zhang L, Zhang M, Zhang Y, Zhao C, Zhou M, Zhou Z, Zhu XJ, Zucker ME, Zuraw SE, Zweizig J, Allison J, Bannister K, Bell ME, Chatterjee S, Chippendale AP, Edwards PG, Harvey-Smith L, Heywood I, Hotan A, Indermuehle B, Marvil J, McConnell D, Murphy T, Popping A, Reynolds J, Sault RJ, Voronkov MA, Whiting MT, Castro-Tirado AJ, Cunniffe R, Jelinek M, Tello JC, Oates SR, Hu YD, Kubanek P, Guziy S, Castellon A, Garcia-Cerezo A, Munoz VF, del Pulgar CP, Castillo-Carrion S, Ceron JMC, Hudec R, Caballero-Garcia MD, Pata P, Vitek S, Adame JA, Konig S, Rendon F, Sanguino TDM, Fernandez-Munoz R, Yock PC, Rattenbury N, Allen WH, Querel R, Jeong S, Park IH, Bai J, Cui C, Fan Y, Wang C, Hiriart D, Lee WH, Claret A, Sanchez-Ramirez R, Pandey SB, Mediavilla T, Sabau-Graziati L, Abbott TMC, Abdalla FB, Allam S, Annis J, Armstrong R, Benoit-Levy A, Berger E, Bernstein RA, Bertin E, Brout D, Buckley-Geer E, Burke DL, Capozzi D, Carretero J, Castander FJ, Chornock R, Cowperthwaite PS, Crocce M, Cunha CE, D'Andrea CB, da Costa LN, Desai S, Diehl HT, Dietrich JP, Doctor Z, Drlica-Wagner A, Drout MR, Eifler TF, Estrada J, Evrard AE, Fernandez E, Finley DA, Flaugher B, Foley RJ, Fong WF, Fosalba P, Fox DB, Frieman J, Fryer CL, Gaztanaga E, Gerdes DW, Goldstein DA, Gruen D, Gruendl RA, Gutierrez G, Herner K, Honscheid K, James DJ, Johnson MD, Johnson MWG, Karliner I, Kasen D, Kent S, Kessler R, Kim AG, Kind MC, Kuehn K, Kuropatkin N, Lahav O, Li TS, Lima M, Lin H, Maia MAG, Margutti R, Marriner J, Martini P, Matheson T, Melchior P, Metzger BD, Miller CJ, Miquel R, Neilsen E, Nichol RC, Nord B, Nugent P, Ogando R, Petravick D, Plazas AA, Quataert E, Roe N, Romer AK, Roodman A, Rosell AC, Rykoff ES, Sako M, Sanchez E, Scarpine V, Schindler R, Schubnell M, Scolnic D, Sevilla-Noarbe I, Sheldon E, Smith N, Smith RC, Soares-Santos M, Sobreira F, Stebbins A, Suchyta E, Swanson MEC, Tarle G, Thaler J, Thomas D, Thomas RC, Tucker DL, Vikram V, Walker AR, Wechsler RH, Wester W, Yanny B, Zuntz J, Connaughton V, Burns E, Goldstein A, Briggs MS, Zhang BB, Hui CM, Jenke P, Wilson-Hodge CA, Bhat PN, Bissaldi E, Cleveland W, Fitzpatrick G, Giles MM, Gibby MH, Greiner J, von Kienlin A, Kippen RM, McBreen S, Mailyan B, Meegan CA, Paciesas WS, Preece RD, Roberts O, Sparke L, Stanbro M, Toelge K, Veres P, Yu HF, Blackburn L, Ackermann M, Ajello M, Albert A, Anderson B, Atwood WB, Axelsson M, Baldini L, Barbiellini G, Bastieri D, Bellazzini R, Blandford RD, Bloom ED, Bonino R, Bottacini E, Brandt TJ, Bruel P, Buson S, Caliandro GA, Cameron RA, Caragiulo M, Caraveo PA, Cavazzuti E, Charles E, Chekhtman A, Chiang J, Chiaro G, Ciprini S, Cohen-Tanugi J, Cominsky LR, Costanza F, Cuoco A, DAmmando F, de Palma F, Desiante R, Digel SW, Di Lalla N, Di Mauro M, Di Venere L, Dominguez A, Drell PS, Dubois R, Favuzzi C, Ferrara EC, Franckowiak A, Fukazawa Y, Funk S, Fusco P, Gargano F, Gasparrini D, Giglietto N, Giommi P, Giordano F, Giroletti M, Glanzman T, Godfrey G, Gomez-Vargas GA, Green D, Grenier IA, Grove JE, Guiriec S, Hadasch D, Harding AK, Hays E, Hewitt JW, Hill AB, Horan D, Jogler T, Johannesson G, Johnson AS, Kensei S, Kocevski D, Kuss M, La Mura G, Larsson S, Latronico L, Li J, Li L, Longo F, Loparco F, Lovellette MN, Lubrano P, Magill J, Maldera S, Manfreda A, Marelli M, Mayer M, Mazziotta MN, McEnery JE, Meyer M, Michelson PF, Mirabal N, Mizuno T, Moiseev AA, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Negro M, Nuss E, Ohsugi T, Omodei N, Orienti M, Orlando E, Ormes JF, Paneque D, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Porter TA, Racusin JL, Raino S, Rando R, Razzaque S, Reimer A, Reimer O, Salvetti D, Parkinson PMS, Sgro C, Simone D, Siskind EJ, Spada F, Spandre G, Spinelli P, Suson DJ, Tajima H, Thayer JB, Thompson DJ, Tibaldo L, Torres DF, Troja E, Uchiyama Y, Venters TM, Vianello G, Wood KS, Wood M, Zhu S, Zimmer S, Brocato E, Cappellaro E, Covino S, Grado A, Nicastro L, Palazzi E, Pian E, Amati L, Antonelli LA, Capaccioli M, D'Avanzo P, D'Elia V, Getman F, Giuffrida G, Iannicola G, Limatola L, Lisi M, Marinoni S, Marrese P, Melandri A, Piranomonte S, Possenti A, Pulone L, Rossi A, Stamerra A, Stella L, Testa V, Tomasella L, Yang S, Bazzano A, Bozzo E, Brandt S, Courvoisier TJL, Ferrigno C, Hanlon L, Kuulkers E, Laurent P, Mereghetti S, Roques JP, Savchenko V, Ubertini P, Kasliwal MM, Singer LP, Cao Y, Duggan G, Kulkarni SR, Bhalerao V, Miller AA, Barlow T, Bellm E, Manulis I, Rana J, Laher R, Masci F, Surace J, Rebbapragada U, Van Sistine A, Sesar B, Perley D, Ferreti R, Prince T, Kendrick R, Horesh A, Hurley K, Golenetskii SV, Aptekar RL, Frederiks DD, Svinkin DS, Rau A, Zhang X, Smith DM, Cline T, Krimm H, Abe F, Doi M, Fujisawa K, Kawabata KS, Morokuma T, Motohara K, Tanaka M, Ohta K, Yanagisawa K, Yoshida M, Baltay C, Rabinowitz D, Ellman N, Rostami S, Bersier DF, Bode MF, Collins CA, Copperwheat CM, Darnley MJ, Galloway DK, Gomboc A, Kobayashi S, Mazzali P, Mundell CG, Piascik AS, Pollacco D, Steele IA, Ulaczyk K, Broderick JW, Fender RP, Jonker PG, Rowlinson A, Stappers BW, Wijers RAMJ, Lipunov V, Gorbovskoy E, Tyurina N, Kornilov V, Balanutsa P, Kuznetsov A, Buckley D, Rebolo R, Serra-Ricart M, Israelian G, Budnev NM, Gress O, Ivanov K, Poleshuk V, Tlatov A, Yurkov V, Kawai N, Serino M, Negoro H, Nakahira S, Mihara T, Tomida H, Ueno S, Tsunemi H, Matsuoka M, Croft S, Feng L, Franzen TMO, Gaensler BM, Johnston-Hollitt M, Kaplan DL, Morales MF, Tingay SJ, Wayth RB, Williams A, Smartt SJ, Chambers KC, Smith KW, Huber ME, Young DR, Wright DE, Schultz A, Denneau L, Flewelling H, Magnier EA, Primak N, Rest A, Sherstyuk A, Stalder B, Stubbs CW, Tonry J, Waters C, Willman M, Olivares F, Campbell H, Kotak R, Sollerman J, Smith M, Dennefeld M, Anderson JP, Botticella MT, Chen TW, Valle MD, Elias-Rosa N, Fraser M, Inserra C, Kankare E, Kupfer T, Harmanen J, Galbany L, Le Guillou L, Lyman JD, Maguire K, Mitra A, Nicholl M, Razza A, Terreran G, Valenti S, Gal-Yam A, Cwiek A, Cwiok M, Mankiewicz L, Opiela R, Zaremba M, Zarnecki AF, Onken CA, Scalzo RA, Schmidt BP, Wolf C, Yuan F, Evans PA, Kennea JA, Burrows DN, Campana S, Cenko SB, Marshall FE, Nousek J, O'Brien P, Osborne JP, Palmer D, Perri M, Siegel M, Tagliaferri G, Klotz A, Turpin D, Laugier R, Beroiz M, Penuela T, Macri LM, Oelkers RJ, Lambas DG, Vrech R, Cabral J, Colazo C, Dominguez M, Sanchez B, Gurovich S, Lares M, Marshall JL, Depoy DL, Padilla N, Pereyra NA, Benacquista M, Tanvir NR, Wiersema K, Levan AJ, Steeghs D, Hjorth J, Fynbo JPU, Malesani D, Milvang-Jensen B, Watson D, Irwin M, Fernandez CG, McMahon RG, Banerji M, Gonzalez-Solares E, Schulze S, Postigo AD, Thoene CC, Cano Z, and Rosswog S
Subjects: TELESCOPE, gravitational waves – methods: observational, Astronomy, media_common.quotation_subject, observational [methods], GW150914, ADVANCED LIGO, supplement, 01 natural sciences, localization, SEARCH, Computer Science::Multimedia, 0103 physical sciences, Broadband, EM follow-up, 010303 astronomy & astrophysics, gravitational wave, QC, media_common, QB, Physics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Gravitational waves, methods: observational, Space and Planetary Science, Astronomy and Astrophysic, Computational physics, GW150914, localization, EM follow-up, supplement, gravitational waves, Sky, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, DARK ENERGY, Transient (oscillation), Current (fluid), SYSTEM
Abstract: Made available in DSpace on 2018-11-26T16:56:32Z (GMT). No. of bitstreams: 0 Previous issue date: 2016-07-01 United States National Science Foundation (NSF) Science and Technology Facilities Council (STFC) of the United Kingdom Max-Planck Society State of Niedersachsen/Germany Australian Research Council Netherlands Organisation for Scientific Research EGO consortium Council of Scientific and Industrial Research of India Department of Science and Technology, India Science & Engineering Research Board (SERB), India Ministry of Human Resource Development, India Spanish Ministerio de Economia y Competitividad Conselleria d'Economia i Competitivitat and Conselleria d'Educacio Cultura i Universitats of the Govern de les Illes Balears National Science Centre of Poland European Commission Royal Society Scottish Funding Council Scottish Universities Physics Alliance Hungarian Scientific Research Fund (OTKA) Lyon Institute of Origins (LIO) National Research Foundation of Korea Industry Canada Province of Ontario through Ministry of Economic Development and Innovation National Science and Engineering Research Council Canada Canadian Institute for Advanced Research Brazilian Ministry of Science, Technology, and Innovation Russian Foundation for Basic Research Leverhulme Trust Research Corporation Ministry of Science and Technology (MOST), Taiwan Kavli Foundation Australian Government National Collaborative Research Infrastructure Strategy Government of Western Australia United States Department of Energy United States National Science Foundation Ministry of Science and Education of Spain Science and Technology Facilities Council of the United Kingdom Higher Education Funding Council for England National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign Kavli Institute of Cosmological Physics at the University of Chicago Center for Cosmology and Astro-Particle Physics at the Ohio State University Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University Financiadora de Estudos e Projetos Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ) Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq) Ministerio da Ciencia, Tecnologia e Inovacao Deutsche Forschungsgemeinschaft Collaborating Institutions in the Dark Energy Survey National Science Foundation MINECO Centro de Excelencia Severo Ochoa European Research Council under European Union's Seventh Framework Programme ERC NASA (United States) DOE (United States) IN2P3/CNRS (France) CEA/Irfu (France) ASI (Italy) INFN (Italy) MEXT (Japan) KEK (Japan) JAXA (Japan) Wallenberg Foundation Swedish Research Council National Space Board (Sweden) NASA in the United States DRL in Germany INAF for the project Gravitational Wave Astronomy with the first detections of adLIGO and adVIRGO experiments ESA (Denmark) ESA (France) ESA (Germany) ESA (Italy) ESA (Switzerland) ESA (Spain) German INTEGRAL through DLR grant US under NASA Grant National Science Foundation PIRE program grant Hubble Fellowship KAKENHI of MEXT Japan JSPS Optical and Near-Infrared Astronomy Inter-University Cooperation Program - MEXT UK Science and Technology Facilities Council ERC Advanced Investigator Grant Lomonosov Moscow State University Development programm Moscow Union OPTICA Russian Science Foundation National Research Foundation of South Africa Australian Government Department of Industry and Science and Department of Education (National Collaborative Research Infrastructure Strategy: NCRIS) NVIDIA at Harvard University University of Hawaii National Aeronautics and Space Administration's Planetary Defense Office Queen's University Belfast National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate European Research Council under European Union's Seventh Framework Programme/ERC STFC grants European Union FP7 programme through ERC STFC through an Ernest Rutherford Fellowship FONDECYT Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) NASA in the US 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. UK Space Agency in the UK Agenzia Spaziale Italiana (ASI) in Italy Ministerio de Ciencia y Tecnologia (MinCyT) Consejo Nacional de Investigaciones Cientificas y Tecnologicas (CONICET) from Argentina USA NSF PHYS NSF ICREA Science and Technology Facilities Council UK Space Agency CALTECH, LIGO, Pasadena, CA 91125 USA Louisiana State Univ, Baton Rouge, LA 70803 USA Univ Salerno, I-84084 Salerno, Italy Ist Nazl Fis Nucl, Sez Napoli, Complesso Univ Monte S Angelo, I-80126 Naples, Italy Univ Florida, Gainesville, FL 32611 USA LIGO Livingston Observ, Livingston, LA 70754 USA Univ Savoie Mt Blanc, CNRS IN2P3, Lab Annecy le Vieux Phys Particules LAPP, F-74941 Annecy Le Vieux, France Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany Nikhef, Sci Pk, NL-1098 XG Amsterdam, Netherlands MIT, LIGO, 77 Massachusetts Ave, Cambridge, MA 02139 USA Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, SP, Brazil Ist Nazl Fis Nucl, Gran Sasso Sci Inst, I-67100 Laquila, Italy Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-00133 Rome, Italy Interuniv Ctr Astron & Astrophys, Pune 411007, Maharashtra, India Tata Inst Fundamental Res, Int Ctr Theoret Sci, Bangalore 560012, Karnataka, India Univ Wisconsin Milwaukee, Milwaukee, WI 53201 USA Leibniz Univ Hannover, D-30167 Hannover, Germany Univ Pisa, I-56127 Pisa, Italy Ist Nazl Fis Nucl, Sez Pisa, I-56127 Pisa, Italy Australian Natl Univ, GPO Box 4, Canberra, ACT 0200, Australia Univ Mississippi, University, MS 38677 USA Calif State Univ Fullerton, Fullerton, CA 92831 USA Univ Paris 11, Univ Paris Saclay, CNRS, LAL,IN2P3, Orsay, France Chennai Math Inst, Chennai, Tamil Nadu, India Univ Roma Tor Vergata, I-00133 Rome, Italy Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England Univ Hamburg, D-22761 Hamburg, Germany INFN, Sez Roma, I-00185 Rome, Italy Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Potsdam, Germany Univ Paris Diderot, Sorbonne Paris Cite, Observ Paris, APC,CNRS,IN2P3,CEA,Irfu, F-75205 Paris 13, France Montana State Univ, Bozeman, MT 59717 USA Univ Perugia, I-06123 Perugia, Italy Ist Nazl Fis Nucl, Sez Perugia, I-06123 Perugia, Italy EGO, I-56021 Pisa, Italy Syracuse Univ, Syracuse, NY 13244 USA Univ Glasgow, SUPA, Glasgow G12 8QQ, Lanark, Scotland LIGO Hanford Observ, Richland, WA 99352 USA Wigner RCP, RMKI, Konkoly Thege Miklos Ut 29-33, H-1121 Budapest, Hungary NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA Columbia Univ, New York, NY 10027 USA Stanford Univ, Stanford, CA 94305 USA Univ Padua, Dipartimento Fis & Astron, I-35131 Padua, Italy INFN, Sez Padova, I-35131 Padua, Italy CAMK PAN, PL-00716 Warsaw, Poland Univ Birmingham, Birmingham B15 2TT, W Midlands, England Univ Genoa, I-16146 Genoa, Italy INFN, Sez Genova, I-16146 Genoa, Italy RRCAT, Indore 452013, MP, India Lomonosov Moscow State Univ, Fac Phys, Moscow 119991, Russia Univ West Scotland, SUPA, Paisley PA1 2BE, Renfrew, Scotland Univ Western Australia, Crawley, WA 6009, Australia Radboud Univ Nijmegen, IMAPP, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands Univ Cote dAzur, CNRS, Observ Cote dAzur, Artemis, CS 34229, Nice 4, France MTA Eotvos Univ, Lendulet Astrophys Res Grp, H-1117 Budapest, Hungary Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France Washington State Univ, Pullman, WA 99164 USA Univ Urbino Carlo Bo, I-61029 Urbino, Italy INFN, Sez Firenze, I-50019 Florence, Italy Univ Oregon, Eugene, OR 97403 USA UPMC, Sorbonne Univ, PSL Res Univ, CNRS,ENS,Coll France,Lab Kastler Brossel, F-75005 Paris, France Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands Univ Maryland, College Pk, MD 20742 USA Georgia Inst Technol, Ctr Relativist Astrophys, Atlanta, GA 30332 USA Georgia Inst Technol, Sch Phys, Atlanta, GA 30332 USA Univ Lyon 1, UMR CNRS 5306, Inst Lumiere Mat, F-69622 Villeurbanne, France Univ Lyon, IN2P3 CNRS, LMA, F-69622 Villeurbanne, France Univ Illes Balears, IEEC IAC3, E-07122 Palma De Mallorca, Spain Univ Naples Federico II, Complesso Univ Monte S Angelo, I-80126 Naples, Italy Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada Tsinghua Univ, Beijing 100084, Peoples R China Texas Tech Univ, Lubbock, TX 79409 USA Penn State Univ, University Pk, PA 16802 USA Natl Tsing Hua Univ, Hsinchu 30013, Taiwan Charles Sturt Univ, Wagga Wagga, NSW 2678, Australia Univ Chicago, Chicago, IL 60637 USA Caltech CaRT, Pasadena, CA 91125 USA Korea Inst Sci & Technol Informat, Daejeon 305806, South Korea Carleton Coll, Northfield, MN 55057 USA Univ Roma La Sapienza, I-00185 Rome, Italy Univ Brussels, B-1050 Brussels, Belgium Sonoma State Univ, Rohnert Pk, CA 94928 USA Northwestern Univ, Evanston, IL 60208 USA Univ Minnesota, Minneapolis, MN 55455 USA Univ Melbourne, Parkville, Vic 3010, Australia Univ Sheffield, Sheffield S10 2TN, S Yorkshire, England Univ Sannio Benevento, I-82100 Benevento, Italy Ist Nazl Fis Nucl, Sez Napoli, I-80100 Naples, Italy Montclair State Univ, Montclair, NJ 07043 USA Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy Ist Nazl Fis Nucl, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy Cardiff Univ, Cardiff CF24 3AA, S Glam, Wales Natl Astron Observ Japan, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan Univ Edinburgh, Sch Math, Edinburgh EH9 3FD, Midlothian, Scotland Indian Inst Technol, Ahmadabad 382424, Gujarat, India Inst Plasma Res, Bhat 382428, Gandhinagar, India Univ Szeged, Dom Ter 9, H-6720 Szeged, Hungary Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA Univ Michigan, Ann Arbor, MI 48109 USA Tata Inst Fundamental Res, Mumbai 400005, Maharashtra, India Amer Univ, Washington, DC 20016 USA Univ Massachusetts Amherst, Amherst, MA 01003 USA Univ Adelaide, Adelaide, SA 5005, Australia West Virginia Univ, Morgantown, WV 26506 USA Univ Bialystok, PL-15424 Bialystok, Poland Univ Strathclyde, SUPA, Glasgow G1 1XQ, Lanark, Scotland IISER TVM, CET Campus, Trivandrum 695016, Kerala, India Inst Appl Phys, Nizhnii Novgorod 603950, Russia Pusan Natl Univ, Busan 609735, South Korea Hanyang Univ, Seoul 133791, South Korea NCBJ, PL-05400 Otwock, Poland IM PAN, PL-00956 Warsaw, Poland Rochester Inst Technol, Rochester, NY 14623 USA Monash Univ, Clayton, Vic 3800, Australia Seoul Natl Univ, Seoul 151742, South Korea Univ Alabama, Huntsville, AL 35899 USA CNRS, ESPCI, F-75005 Paris, France Univ Camerino, Dipartimento Fis, I-62032 Camerino, Italy Southern Univ, Baton Rouge, LA 70813 USA A&M Coll, Baton Rouge, LA 70813 USA Coll William & Mary, Williamsburg, VA 23187 USA Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil Univ Cambridge, Cambridge CB2 1TN, England IISER Kolkata, Mohanpur 741252, W Bengal, India Rutherford Appleton Lab, HSIC, Didcot OX11 0QX, Oxon, England Whitman Coll, 345 Boyer Ave, Walla Walla, WA 99362 USA Natl Inst Math Sci, Daejeon 305390, South Korea Hobart & William Smith Coll, Geneva, NY 14456 USA Univ Zielona Gora, Janusz Gil Inst Astron, PL-65265 Zielona Gora, Poland Andrews Univ, Berrien Springs, MI 49104 USA Univ Siena, I-53100 Siena, Italy Trinity Univ, San Antonio, TX 78212 USA Univ Washington, Seattle, WA 98195 USA Kenyon Coll, Gambier, OH 43022 USA Abilene Christian Univ, Abilene, TX 79699 USA CSIRO Astron & Space Sci, POB 76, Epping, NSW 1710, Australia ARC Ctr Excellence All Sky Astrophys CAASTRO, Sydney, NSW, Australia Cornell Ctr Astrophys & Planetary Sci, Ithaca, NY 14853 USA Rhodes Univ, Dept Phys & Elect, POB 94, ZA-6140 Grahamstown, South Africa CSIRO Astron & Space Sci, 26 Dick Perry Ave,Technol Pk, Kensington, WA 6151, Australia Univ Sydney, Sch Phys, Sydney Inst Astron, Sydney, NSW 2006, Australia Univ Western Australia, ICRAR, M468,35 Stirling Highway, Perth, WA 6009, Australia CSIC, IAA, POB 03004, E-18080 Granada, Spain Univ Malaga, Unidad Asociada CSIC, Escuela Ingn, Dept Ingn Sistemas & Automat, E-29071 Malaga, Spain Acad Sci Czech Republ, Inst Astron, CS-25165 Ondrejov, Czech Republic Acad Sci Czech Republ, Inst Phys, Slovance 1999-2, Prague 18221 8, Czech Republic Nikolaev Natl Univ, Nikolska Str 24, UA-54030 Nikolayev, Ukraine Univ Malaga, Fac Ciencias, Blvd Louis Pasteur, E-29010 Malaga, Spain Univ Malaga, Ensenanza Virtual & Labs Tecnol, Jimenez Fraud 10, E-29071 Malaga, Spain ISDEFE SMOS FOS ESA ESAC, E-28692 Villanueva De La Canada, Madrid, Spain Czech Tech Univ, Fac Elect Engn, Dept Radioelect, Tech 2, Prague 16627, Czech Republic Acad Sci Czech Republ, Inst Astron, Bocni 2 1401, CZ-14100 Prague 4, Czech Republic Estn Sondeos Atmosfer ESAt) El Arenosillo CEDEA I, E-21130 Mazagon, Huelva, Spain Univ Huelva, ETSI La Rabida, Dept Ingn Elect Sistemas Informat & Automat, E-21819 Palos De La Frontera, Huelva, Spain IHSM UMA CSIC, Inst Hortofruticultura Subtrop & Mediterranea La, E-29750 Algarrobo Costa, Malaga, Spain Univ Auckland, Dept Phys, Private Bag 92019, Auckland 1, New Zealand Vintage Lane Observ, RD3, Blenheim 7273, New Zealand Natl Inst Water & Atmospher Res NIWA, Lauder, New Zealand Sungkyunkwan Univ SKKU, Dept Phys, Suwon, South Korea Chinese Acad Sci, Yunnan Astron Observ, Kunming 650011, Yunnan, Peoples R China Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China Univ Nacl Autonoma Mexico, Inst Astron, Ensenada 22800, Baja California, Mexico Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70-264, Mexico City 04510, DF, Mexico Aryabhatta Res Inst Observat Sci, Manora Peak 263002, Nainital, India Univ Cadiz, Escuela Politecn Super, Avda Ramon Puyol, E-11202 Algeciras, Cadiz, Spain INTA, Div Ciencias Espacio, E-28850 Torrejon De Ardoz, Madrid, Spain Natl Opt Astron Observ, Cerro Tololo Interamer Observ, Casilla 603, La Serena, Chile UCL, Dept Phys & Astron, Gower St, London WC1E 6BT, England Fermilab Natl Accelerator Lab, POB 500, Batavia, IL 60510 USA Princeton Univ, Dept Astrophys Sci, Peyton Hall, Princeton, NJ 08544 USA CNRS, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France Univ Paris 06, Sorbonne Univ, UMR 7095, Inst Astrophys Paris, F-75014 Paris, France Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA Carnegie Observ, 813 Santa Barbara St, Pasadena, CA 91101 USA Univ Penn, Dept Phys & Astron, Philadelphia, PA 19104 USA Stanford Univ, Kavli Inst Particle Astrophys & Cosmol, POB 2450, Stanford, CA 94305 USA SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA Univ Portsmouth, Inst Cosmol & Gravitat, Portsmouth PO1 3FX, Hants, England IEEC CSIC, Inst Ciencies Espai, Campus UAB,Carrer Can Magrans S-N, E-08193 Barcelona, Spain Barcelona Inst Sci & Technol, IFAE, Campus UAB, E-08193 Bellaterra, Barcelona, Spain Ohio Univ, Inst Astrophys, Dept Phys & Astron, Clippinger Lab 251B, Athens, OH 45701 USA Lab Interinst E Astron LIneA, Rua Gal Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ, Brazil Excellence Cluster Univ, Boltzmannstr 2, D-85748 Garching, Germany Univ Munich, Fac Phys, Scheinerstr 1, D-81679 Munich, Germany Univ Chicago, Kavli Inst Cosmol Phys, Chicago, IL 60637 USA CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA Univ Illinois, Dept Phys, 1110 W Green St, Urbana, IL 61801 USA Univ Arizona, Steward Observ, 933 N Cherry Ave, Tucson, AZ 85721 USA Penn State Univ, Ctr Particle & Gravitat Astrophys, Dept Astron & Astrophys, University Pk, PA 16802 USA Penn State Univ, Ctr Theoret & Observat Cosmol, University Pk, PA 16802 USA Los Alamos Natl Lab, CCS Div, Los Alamos, NM 87545 USA Univ Michigan, Dept Phys, Ann Arbor, MI 48109 USA Univ Calif Berkeley, Dept Astron, 501 Campbell Hall, Berkeley, CA 94720 USA Lawrence Berkeley Natl Lab, 1 Cyclotron Rd, Berkeley, CA 94720 USA Natl Ctr Supercomp Applicat, 1205 West Clark St, Urbana, IL 61801 USA Ohio State Univ, Ctr Cosmol & Astroparticle Phys, Columbus, OH 43210 USA Ohio State Univ, Dept Phys, Columbus, OH 43210 USA Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA Univ Calif Berkeley, Dept Astron, 601 Campbell Hall, Berkeley, CA 94720 USA Australian Astron Observ, N Ryde, NSW 2113, Australia Texas A&M Univ, George P & Cynthia Woods Mitchell Inst Fundamenta, College Stn, TX 77843 USA Texas A&M Univ, Dept Phys & Astron, College Stn, TX 77843 USA Univ Sao Paulo, Inst Fis, Dept Fis Matemat, CP 66318, BR-05314970 Sao Paulo, SP, Brazil NYU, Ctr Cosmol & Particle Phys, 4 Washington Pl, New York, NY 10003 USA Ohio State Univ, Dept Astron, Columbus, OH 43210 USA Natl Opt Astron Observ, 950 North Cherry Ave, Tucson, AZ 85719 USA Columbia Astrophys Lab, Pupin Hall, New York, NY 10027 USA Univ Michigan, Dept Astron, Ann Arbor, MI 48109 USA Inst Catalana Recerca & Estudis Avancats, E-08010 Barcelona, Spain Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA Univ Calif Berkeley, Theoret Astrophys Ctr, Berkeley, CA 94720 USA Univ Sussex, Dept Phys & Astron, Pevensey Bldg, Brighton BN1 9QH, E Sussex, England CIEMAT, Madrid, Spain Brookhaven Natl Lab, Bldg 510, Upton, NY 11973 USA Argonne Natl Lab, 9700 South Cass Ave, Argonne, IL 60439 USA Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Oxford Rd, Manchester M13 9PL, Lancs, England Univ Space Res Assoc, 320 Sparkman Dr, Huntsville, AL 35806 USA Univ Alabama, Dept Phys, 320 Sparkman Dr, Huntsville, AL 35899 USA NASA, Marshall Space Flight Ctr, Astrophys Off, ZP12, Huntsville, AL 35812 USA Univ Alabama, Dept Space Sci, 320 Sparkman Dr, Huntsville, AL 35899 USA Univ Alabama, CSPAR, 320 Sparkman Dr, Huntsville, AL 35899 USA Ist Nazl Fis Nucl, Sez Bari, I-70126 Bari, Italy Jacobs Technol Inc, Huntsville, AL USA Max Planck Inst Extraterr Phys, Giessenbachstr 1, D-85748 Garching, Germany Los Alamos Natl Lab, Los Alamos, NM 87545 USA Univ Coll Dublin, Sch Phys, Stillorgan Rd, Dublin 4, Ireland NASA Headquarters, Washington, DC USA Tech Univ Munich, Excellence Cluster Universe, Boltzmannstr 2, D-85748 Garching, Germany Deutsch Elektronen Synchrotron DESY, D-15738 Zeuthen, Germany Clemson Univ, Kinard Lab Phys, Dept Phys & Astron, Clemson, SC 29634 USA Stanford Univ, Dept Phys, Kavli Inst Particle Astrophys & Cosmol, WW Hansen Expt Phys Lab, Stanford, CA 94305 USA Stanford Univ, SLAC Natl Accelerator Lab, Stanford, CA 94305 USA Stockholm Univ, AlbaNova, Dept Phys, SE-10691 Stockholm, Sweden AlbaNova, Oskar Klein Ctr Cosmoparticle Phys, SE-10691 Stockholm, Sweden Univ Calif Santa Cruz, Dept Phys, Santa Cruz Inst Particle Phys, Santa Cruz, CA 95064 USA Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA KTH Royal Inst Technol, Dept Phys, AlbaNova, SE-10691 Stockholm, Sweden Tokyo Metropolitan Univ, Dept Phys, Minami Osawa 1-1, Hachioji, Tokyo 1920397, Japan Ist Nazl Fis Nucl, Sez Trieste, I-34127 Trieste, Italy Univ Trieste, Dipartimento Fis, I-34127 Trieste, Italy Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy Ist Nazl Fis Nucl, Sez Torino, I-10125 Turin, Italy Univ Torino, Dipartimento Fis Gen Amadeo Avogadro, I-10125 Turin, Italy CNRS IN2P3, Ecole Polytech, Lab Leprince Ringuet, Palaiseau, France Univ Maryland Baltimore Cty, Dept Phys, Baltimore, MD 21250 USA Univ Maryland Baltimore Cty, Ctr Space Sci & Technol, Baltimore, MD 21250 USA CRESST, Greenbelt, MD 20771 USA CIFS, I-10133 Turin, Italy Univ Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy Politecn Bari, Dipartimento Fis M Merlin, I-70126 Bari, Italy INAF Ist Astrofis Spaziale & Fis Cosm, I-20133 Milan, Italy ASI, Sci Data Ctr, I-00133 Rome, Italy George Mason Univ, Coll Sci, Fairfax, VA 22030 USA Naval Res Lab, Washington, DC 20375 USA Univ Montpellier, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France Sonoma State Univ, Dept Phys & Astron, Rohnert Pk, CA 94928 USA INAF Ist Radioastron, I-40129 Bologna, Italy Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy Univ Telemat Pegaso, Piazza Trieste & Trento 48, I-80132 Naples, Italy Univ Udine, I-33100 Udine, Italy Hiroshima Univ, Dept Phys Sci, Hiroshima 7398526, Japan Erlangen Ctr Astroparticle Phys, D-91058 Erlangen, Germany Pontificia Univ Catolica Chile, Fac Fis, Inst Astrofis, Casilla 306, Santiago 22, Chile Univ Maryland, Dept Phys, College Pk, MD 20742 USA Univ Maryland, Dept Astron, College Pk, MD 20742 USA Univ Paris Diderot, Serv Astrophys, CEA Saclay, Lab AIM,CEA IRFU,CNRS, F-91191 Gif Sur Yvette, France Naval Res Lab, Div Space Sci, Washington, DC 20375 USA Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria Univ Innsbruck, Inst Theoret Phys, A-6020 Innsbruck, Austria Univ North Florida, Dept Phys, 1 UNF Dr, Jacksonville, FL 32224 USA Univ Iceland, Inst Sci, IS-107 Reykjavik, Iceland IEEC CSIC, Inst Space Sci, Campus UAB, E-08193 Barcelona, Spain Hiroshima Univ, Hiroshima Astrophys Sci Ctr, Hiroshima 7398526, Japan Max Planck Inst Phys & Astrophys, D-80805 Munich, Germany Univ Denver, Dept Phys & Astron, Denver, CO 80208 USA Univ Johannesburg, Dept Phys, POB 524, ZA-2006 Auckland Pk, South Africa Univ Hong Kong, Dept Phys, Pokfulam Rd, Hong Kong, Hong Kong, Peoples R China Univ Hong Kong, Lab Space Res, Hong Kong, Hong Kong, Peoples R China NYCB Real Time Comp Inc, Lattingtown, NY 11560 USA Purdue Univ Calumet, Dept Chem & Phys, Hammond, IN 46323 USA Nagoya Univ, Solar Terr Environm Lab, Nagoya, Aichi 4648601, Japan Max Planck Inst Kernphys, D-69029 Heidelberg, Germany ICREA, Barcelona, Spain Dept Phys, Toshima Ku, 3-34-1 Nishi Ikebukuro, Tokyo 1718501, Japan INAF Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, RM, Italy INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy INAF Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy INAF Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy INAF Ist Astrofis Spaziale & Fis Cosm Bologna, Via Gobetti 101, I-40129 Bologna, Italy Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy ASI Sci Data Ctr, Via Politecn Snc, I-00133 Rome, Italy Univ Naples Federico II, CU Monte St Angelo, Dip Fis Ettore Pancini, Via Cinthia, I-80126 Naples, Italy INAF ORA Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy INAF Osservatorio Astron Torino, Str Osservatorio 20, I-10025 Pino Torinese, To, Italy INAF Inst Space Astrophys & Planetol, Via Fosso del Cavaliere 100, I-00133 Rome, Italy Univ Geneva, Dept Astron, ISDC, Chemin Ecogia 16, CH-1290 Versoix, Switzerland Natl Space Inst Elektrovej, DTU Space, Bldg 327, DK-2800 Lyngby, Denmark Univ Coll Dublin, Sch Phys, Space Sci Grp, Dublin 4, Ireland ESAC, ESA, Sci Operat Dept, E-28691 Madrid, Spain Univ Paris Diderot, CNRS IN2P3, Sorbonne Paris Cite, APC,CEA Irfu,Observ Paris, 10 Rue Alice Domont & Leonie Duquet, F-75205 Paris 13, France INAF, IASF Milano, Via E Bassini 15, I-20133 Milan, Italy Univ Toulouse, 9 Ave Roche,BP 44346, F-31028 Toulouse, France UPS OMP, 9 Ave Roche,BP 44346, F-31028 Toulouse, France CNRS, 9 Ave Roche,BP 44346, F-31028 Toulouse, France IRAP, 9 Ave Roche,BP 44346, F-31028 Toulouse, France Univ Paris Diderot, CNRS IN2P3, Sorbonne Paris Cite, Francois Arago Ctr,APC,CEA Irfu,Observ Paris, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France CALTECH, Cahill Ctr Astrophys, Pasadena, CA 91125 USA Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark Stockholm Univ, AlbaNova, Dept Astron, SE-10691 Stockholm, Sweden Stockholm Univ, AlbaNova, Oskar Klein Ctr, SE-10691 Stockholm, Sweden Lockheed Martin Space Syst Co, Palo Alto, CA 94304 USA Univ Calif Berkeley, Space Sci Lab, 7 Gauss Way, Berkeley, CA 94720 USA Ioffe Phys Tech Inst, Politekhnicheskaya 26, St Petersburg 194021, Russia Univ Space Res Assoc, 7178 Columbia Gateway Dr, Columbia, MD 21046 USA Nagoya Univ, Inst Space Earth Environm Res, Chikusa Ku, Furo Cho, Nagoya, Aichi 4648601, Japan Univ Tokyo, Inst Astron, Grad Sch Sci, Mitaka, Tokyo 1810015, Japan Yamaguchi Univ, Res Inst Time Studies, Yamaguchi, Yamaguchi 7538511, Japan Natl Astron Observ Japan, Div Theoret Astron, Mitaka, Tokyo 1818588, Japan Kyoto Univ, Dept Astron, Kyoto, Kyoto 6068502, Japan Natl Astron Observ Japan, Okayama Astrophys Observ, Okayama 7190232, Japan Yale Univ, Dept Phys, New Haven, CT 06520 USA Liverpool JMU, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia Univ Nova Gorica, Vipavska 13, Nova Gorica 5000, Slovenia Univ Ljubljana, Fac Math & Phys, Jadranska 19, Ljubljana 1000, Slovenia Univ Bath, Dept Phys, Bath BA2 7AY, Avon, England Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England Netherlands Inst Radio Astron, ASTRON, Postbus 2, NL-7990 AA Dwingeloo, Netherlands Univ Oxford, Dept Phys, Astrophys, Keble Rd, Oxford OX1 3RH, England SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands Univ Amsterdam, Astron Inst Anton Pannekoek, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands Lomonosov Moscow State Univ, Sternberg Astron Inst, 13 Univ Skiy Prospekt, Moscow 119234, Russia South African Astron Observ, POB 9, ZA-7935 Cape Town, South Africa Inst Astrofis Canarias, Calle Via Lactea S-N, E-38200 Tenerife, Spain Irkutsk State Univ, Inst Appl Phys, 20 Gagarin Blvd, Irkutsk 664003, Russia RAS, Kislovodsk Solar Stn Main Pulkovo Observ, POB 45,Ul Gagarina 100, Kislovodsk 357700, Russia Blagoveschensk State Pedag Univ, Lenin Str 104, Blagoveshchensk 675000, Amur Region, Russia Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528851, Japan RIKEN, MAXI Team, 2-1 Hirosawa, Wako, Saitama 3510198, Japan Nihon Univ, Dept Phys, Chiyoda Ku, 1-8-14 Kanda Surugadai, Tokyo 1018308, Japan Japan Aerosp Explorat Agcy, Human Spaceflight Technol Directorate, JEM Mission Operat & Integrat Ctr, 2-1-1 Sengen, Tsukuba, Ibaraki 3058505, Japan Japan Aerosp Explorat Agcy JAXA, ISAS, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 2525210, Japan Osaka Univ, Dept Earth & Space Sci, 1-1 Machikaneyama, Toyonaka, Osaka 5600043, Japan Univ Calif Berkeley, Dept Astron, 501 Campbell Hall 3411, Berkeley, CA 94720 USA Eureka Sci Inc, 2452 Delmer St Suite 100, Oakland, CA 94602 USA MIT, Kavli Inst Astrophys & Space Res, 77 Massachusetts Ave, Cambridge, MA 02139 USA Curtin Univ, Int Ctr Radio Astron Res, Bentley, WA 6102, Australia Univ Toronto, Dunlap Inst Astron & Astrophys, Toronto, ON M5S 3H4, Canada Victoria Univ Wellington, Sch Chem & Phys Sci, POB 600, Wellington 6140, New Zealand Ist Nazl Astrofis, Osservatorio Radio Astron, I-40123 Bologna, Italy Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA Harvard Univ, Dept Phys, Cambridge, MA 02138 USA Millennium Inst Astrophys, Casilla 36-D, Santiago, Chile Univ Andres Bello, Dept Ciencias Fis, Avda Republ 252, Santiago, Chile Univ Cambridge, Inst Astron, Madingley Rd, Cambridge CB3 0HA, England CNRS, Inst Astrophys Paris, 98 Bis Blvd Arago, F-75014 Paris, France Univ Paris 06, 98 Bis Blvd Arago, F-75014 Paris, France European Southern Observ, Alonso de Cordova 3107, Santiago, Chile Univ Turku, Dept Phys & Astron, Tuorla Observ, Vaialantie 20, FI-21500 Piikkio, Finland Univ Chile, Dept Astron, Camino El Observ 1515, Santiago, Chile Univ Paris 06, Sorbonne Univ, UMR 7585, LPNHE, F-75005 Paris, France CNRS, UMR 7585, Lab Phys Nucl & Hautes Energies, 4 Pl Jussieu, F-75005 Paris, France Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA Weizmann Inst Sci, Benoziyo Ctr Astrophys, IL-76100 Rehovot, Israel Univ Warsaw, Fac Phys, PL-02093 Warsaw, Poland Polish Acad Sci, Ctr Theoret Phys, PL-02668 Warsaw, Poland Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England Univ Maryland, Joint Space Sci Inst, College Pk, MD 20742 USA Los Alamos Natl Lab, B244, Los Alamos, NM 87545 USA CNRS UMR 5277 UPS, Inst Rech Astrophys & Planetol, 14 Ave Edouard Belin, F-31400 Toulouse, France Univ Texas San Antonio, San Antonio, TX USA Univ Munich, Fac Phys, Schellingstr 4, D-80799 Munich, Germany Texas A&M Univ, Dept Phys & Astron, Mitchell Inst Fundamental Phys & Astron, 4242 TAMU, College Stn, TX 77843 USA Univ Nacl Cordoba, IATE, Laprida 854, Cordoba, Argentina Pontificia Univ Catolica Chile, Inst Astrofis, Ave Vicuna Mackenna 4860, Santiago, Chile CSIC, Inst Astrofis Andalucia, Glorieta Astron S-N, E-18008 Granada, Spain Univ Iceland, Inst Sci, Ctr Astrophys & Cosmol, IS-107 Reykjavik, Iceland Univ Estadual Paulista, ICTP South Amer Inst Fundamental Res, Inst Fis Teor, BR-01140070 Sao Paulo, SP, Brazil National Science Foundation: AST-1138766 National Science Foundation: AST-1238877 MINECO: AYA2012-39559 MINECO: ESP2013-48274 MINECO: FPA2013-47986 Centro de Excelencia Severo Ochoa: SEV-2012-0234 ERC: 240672 ERC: 291329 ERC: 306478 German INTEGRAL through DLR grant: 50 OG 1101 US under NASA Grant: NNX15AU74G National Science Foundation PIRE program grant: 1545949 Hubble Fellowship: HST-HF-51325.01 KAKENHI of MEXT Japan: 24103003 KAKENHI of MEXT Japan: 15H00774 KAKENHI of MEXT Japan: 15H00788 JSPS: 15H02069 JSPS: 15H02075 ERC Advanced Investigator Grant: 267697 Russian Science Foundation: 16-12-00085 Russian Science Foundation: RFBR15-02-07875 National Aeronautics and Space Administration's Planetary Defense Office: NNX14AM74G National Aeronautics and Space Administration through Planetary Science Division of the NASA Science Mission Directorate: NNX08AR22G European Research Council under European Union's Seventh Framework Programme/ERC: 291222 STFC grants: ST/I001123/1 STFC grants: ST/L000709/1 European Union FP7 programme through ERC: 320360 FONDECYT: 3140326 Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO): CE110001020 USA NSF PHYS: 1156600 NSF: 1242090 Science and Technology Facilities Council: Gravitational Waves Science and Technology Facilities Council: ST/L000946/1 Science and Technology Facilities Council: ST/K005014/1 Science and Technology Facilities Council: ST/N000668/1 Science and Technology Facilities Council: ST/M000966/1 Science and Technology Facilities Council: ST/I006269/1 Science and Technology Facilities Council: ST/L000709/1 Science and Technology Facilities Council: ST/J00166X/1 Science and Technology Facilities Council: ST/K000845/1 Science and Technology Facilities Council: ST/K00090X/1 Science and Technology Facilities Council: ST/N000633/1 Science and Technology Facilities Council: ST/H001972/1 Science and Technology Facilities Council: ST/L000733/1 Science and Technology Facilities Council: ST/N000757/1 Science and Technology Facilities Council: ST/M001334/1 Science and Technology Facilities Council: ST/J000019/1 Science and Technology Facilities Council: ST/M003035/1 Science and Technology Facilities Council: ST/I001123/1 Science and Technology Facilities Council: ST/N00003X/1 Science and Technology Facilities Council: ST/I006269/1 Gravitational Waves Science and Technology Facilities Council: ST/N000072/1 Science and Technology Facilities Council: ST/L003465/1 UK Space Agency: ST/P002196/1

18. BART - Recent status

Author: Jelinek, M., Hudec, R., Kubanek, P., Nekola, M., Soldan, A., Ivana Orlitova, Topinka, A., Smida, A., Sveda, L., Hroch, F., Polcar, J., Castro-Tirado, Aj, Ricker, Gr, and Vanderspek, Rk

19. RTS2 - Remote telescope system, 2(nd) version

Author: Petr Kubánek, Jelinek, M., Nekola, M., Topinka, M., Strobl, J., Hudec, R., Sanguino, Tdm, Postigo, Ad, Castro-Tirado, Aj, Fenimore, Ee, and Galassi, M.

20. BOOTES: Recent technical developments and scientific results

Author: Sanguino, Tjm, La Morena, Ba, Riera, Jt, Castro-Tirado, Aj, Postigo, Adu, Gorosabel, J., Ceron, Jcm, Dabo, Ceg, Galiano, Jab, Pata, P., Vitek, S., Bernas, M., Jelinek, M., Petr Kubánek, Hudec, R., Mcbreen, S., Soria, T., Feroci, M., Frontera, F., Masetti, N., and Piro, L.

21. The BOOTES experiment in support of the Gran Telescopio Canarias (GTC) in the study of the high energy universe

Author: Ceron, Jmc, Postigo, Ad, Garcia-Dabo, Ce, Sanguino, Tjm, Pata, P., Bernas, M., Jelinek, M., Hudec, R., Berna, Ja, Gorosabel, J., J. Miguel Mas-Hesse, Castro-Tirado, Aj, and UNAM

22. Ground-based support for space telescopes

Author: Hudec, R., Jelinek, M., Soldan, J., Nekola, M., Petr Kubánek, Castro-Tirado, Aj, and Battrick, B.

23. BOOTES: A stereoscopic and robotic ground-support facility for the integral era

Author: Castro-Tirado, Aj, Sanguino, Tjm, Postigo, Adu, Ceron, Jmc, Jelinek, M., Petr Kubánek, Hudec, R., Vitek, S., Pata, P., Bernas, M., Berna, Ja, Soldan, J., Gorosabel, J., Soria, T., La Morena, B., Reglero, V., Torres, J., and Battrick, B.

24. Recent developments in the BOOTES experiment

Author: Postigo, Ad, Sanguino, Tjm, Ceron, Jmc, Pata, P., Bernas, M., Jelinek, M., Hudec, R., Mcbreen, S., Berna, Ja, Dabo, Ceg, Gorosabel, J., J. Miguel Mas-Hesse, Soria, T., La Morena, Ba, Riera, Jt, Castro-Tirado, Aj, Ricker, Gr, and Vanderspek, Rk

25. BOOTES: Technological developments and scientific results by a stereoscopic system with two stations spaced by 240 km

Author: Sanguino, Tdm, Castro-Tirado, Aj, Postigo, Ad, Palomo, Mtf, Ceron, Jmc, Galiano, Jab, Pata, P., Soldan, Pj, Bernas, M., Hudec, R., Jelinek, M., Vitek, S., Petr Kubánek, Mcbreen, S., Gorosabel, J., Dabo, Ceg, Soria, T., Carretero, Badl, Riera, Jt, Fenimore, Ee, and Galassi, M.

26. A shock flash breaking out of a dusty red supergiant.

Author: Li G, Hu M, Li W, Yang Y, Wang X, Yan S, Hu L, Zhang J, Mao Y, Riise H, Gao X, Sun T, Liu J, Xiong D, Wang L, Mo J, Iskandar A, Xi G, Xiang D, Wang L, Sun G, Zhang K, Chen J, Lin W, Guo F, Liu Q, Cai G, Zhou W, Zhao J, Chen J, Zheng X, Li K, Zhang M, Xu S, Lyu X, Castro-Tirado AJ, Chufarin V, Potapov N, Ionov I, Korotkiy S, Nazarov S, Sokolovsky K, Hamann N, and Herman E
Abstract: Shock-breakout emission is light that arises when a shockwave, generated by the core-collapse explosion of a massive star, passes through its outer envelope. Hitherto, the earliest detection of such a signal was at several hours after the explosion 1 , although a few others had been reported 2-7 . The temporal evolution of early light curves should provide insights into the shock propagation, including explosion asymmetry and environment in the vicinity, but this has been hampered by the lack of multiwavelength observations. Here we report the instant multiband observations of a type II supernova (SN 2023ixf) in the galaxy M101 (at a distance of 6.85 ± 0.15 Mpc; ref. 8 ), beginning at about 1.4 h after the explosion. The exploding star was a red supergiant with a radius of about 440 solar radii. The light curves evolved rapidly, on timescales of 1-2 h, and appeared unusually fainter and redder than predicted by the models 9-11 within the first few hours, which we attribute to an optically thick dust shell before it was disrupted by the shockwave. We infer that the breakout and perhaps the distribution of the surrounding dust were not spherically symmetric., (© 2023. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2024
Full Text: View/download PDF

27. A lanthanide-rich kilonova in the aftermath of a long gamma-ray burst.

Author: Yang YH, Troja E, O'Connor B, Fryer CL, Im M, Durbak J, Paek GSH, Ricci R, Bom CR, Gillanders JH, Castro-Tirado AJ, Peng ZK, Dichiara S, Ryan G, van Eerten H, Dai ZG, Chang SW, Choi H, De K, Hu Y, Kilpatrick CD, Kutyrev A, Jeong M, Lee CU, Makler M, Navarete F, and Pérez-García I
Abstract: Observationally, kilonovae are astrophysical transients powered by the radioactive decay of nuclei heavier than iron, thought to be synthesized in the merger of two compact objects 1-4 . Over the first few days, the kilonova evolution is dominated by a large number of radioactive isotopes contributing to the heating rate 2,5 . On timescales of weeks to months, its behaviour is predicted to differ depending on the ejecta composition and the merger remnant 6-8 . Previous work has shown that the kilonova associated with gamma-ray burst 230307A is similar to kilonova AT2017gfo (ref. 9 ), and mid-infrared spectra revealed an emission line at 2.15 micrometres that was attributed to tellurium. Here we report a multi-wavelength analysis, including publicly available James Webb Space Telescope data 9 and our own Hubble Space Telescope data, for the same gamma-ray burst. We model its evolution up to two months after the burst and show that, at these late times, the recession of the photospheric radius and the rapidly decaying bolometric luminosity (L bol ∝ t -2.7±0.4 , where t is time) support the recombination of lanthanide-rich ejecta as they cool., (© 2024. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2024
Full Text: View/download PDF

28. A nearby long gamma-ray burst from a merger of compact objects.

Author: Troja E, Fryer CL, O'Connor B, Ryan G, Dichiara S, Kumar A, Ito N, Gupta R, Wollaeger RT, Norris JP, Kawai N, Butler NR, Aryan A, Misra K, Hosokawa R, Murata KL, Niwano M, Pandey SB, Kutyrev A, van Eerten HJ, Chase EA, Hu YD, Caballero-Garcia MD, and Castro-Tirado AJ
Subjects: Stars, Celestial
Abstract: Gamma-ray bursts (GRBs) are flashes of high-energy radiation arising from energetic cosmic explosions. Bursts of long (greater than two seconds) duration are produced by the core-collapse of massive stars 1 , and those of short (less than two seconds) duration by the merger of compact objects, such as two neutron stars 2 . A third class of events with hybrid high-energy properties was identified 3 , but never conclusively linked to a stellar progenitor. The lack of bright supernovae rules out typical core-collapse explosions 4-6 , but their distance scales prevent sensitive searches for direct signatures of a progenitor system. Only tentative evidence for a kilonova has been presented 7,8 . Here we report observations of the exceptionally bright GRB 211211A, which classify it as a hybrid event and constrain its distance scale to only 346 megaparsecs. Our measurements indicate that its lower-energy (from ultraviolet to near-infrared) counterpart is powered by a luminous (approximately 10 42 erg per second) kilonova possibly formed in the ejecta of a compact object merger., (© 2022. The Author(s).)
Published: 2022
Full Text: View/download PDF

29. Very-high-frequency oscillations in the main peak of a magnetar giant flare.

Author: Castro-Tirado AJ, Østgaard N, Göǧüş E, Sánchez-Gil C, Pascual-Granado J, Reglero V, Mezentsev A, Gabler M, Marisaldi M, Neubert T, Budtz-Jørgensen C, Lindanger A, Sarria D, Kuvvetli I, Cerdá-Durán P, Navarro-González J, Font JA, Zhang BB, Lund N, Oxborrow CA, Brandt S, Caballero-García MD, Carrasco-García IM, Castellón A, Castro Tirado MA, Christiansen F, Eyles CJ, Fernández-García E, Genov G, Guziy S, Hu YD, Nicuesa Guelbenzu A, Pandey SB, Peng ZK, Pérez Del Pulgar C, Reina Terol AJ, Rodríguez E, Sánchez-Ramírez R, Sun T, Ullaland K, and Yang S
Subjects: Atmosphere, Stars, Celestial
Abstract: Magnetars are strongly magnetized, isolated neutron stars 1-3 with magnetic fields up to around 10 15 gauss, luminosities of approximately 10 31 -10 36 ergs per second and rotation periods of about 0.3-12.0 s. Very energetic giant flares from galactic magnetars (peak luminosities of 10 44 -10 47 ergs per second, lasting approximately 0.1 s) have been detected in hard X-rays and soft γ-rays 4 , and only one has been detected from outside our galaxy 5 . During such giant flares, quasi-periodic oscillations (QPOs) with low (less than 150 hertz) and high (greater than 500 hertz) frequencies have been observed 6-9 , but their statistical significance has been questioned 10 . High-frequency QPOs have been seen only during the tail phase of the flare 9 . Here we report the observation of two broad QPOs at approximately 2,132 hertz and 4,250 hertz in the main peak of a giant γ-ray flare 11 in the direction of the NGC 253 galaxy 12-17 , disappearing after 3.5 milliseconds. The flare was detected on 15 April 2020 by the Atmosphere-Space Interactions Monitor instrument 18,19 aboard the International Space Station, which was the only instrument that recorded the main burst phase (0.8-3.2 milliseconds) in the full energy range (50 × 10 3 to 40 × 10 6 electronvolts) without suffering from saturation effects such as deadtime and pile-up. Along with sudden spectral variations, these extremely high-frequency oscillations in the burst peak are a crucial component that will aid our understanding of magnetar giant flares., (© 2021. The Author(s), under exclusive licence to Springer Nature Limited.)
Published: 2021
Full Text: View/download PDF

30. No pulsed radio emission during a bursting phase of a Galactic magnetar.

Author: Lin L, Zhang CF, Wang P, Gao H, Guan X, Han JL, Jiang JC, Jiang P, Lee KJ, Li D, Men YP, Miao CC, Niu CH, Niu JR, Sun C, Wang BJ, Wang ZL, Xu H, Xu JL, Xu JW, Yang YH, Yang YP, Yu W, Zhang B, Zhang BB, Zhou DJ, Zhu WW, Castro-Tirado AJ, Dai ZG, Ge MY, Hu YD, Li CK, Li Y, Li Z, Liang EW, Jia SM, Querel R, Shao L, Wang FY, Wang XG, Wu XF, Xiong SL, Xu RX, Yang YS, Zhang GQ, Zhang SN, Zheng TC, and Zou JH
Abstract: Fast radio bursts (FRBs) are millisecond-duration radio transients of unknown physical origin observed at extragalactic distances 1-3 . It has long been speculated that magnetars are the engine powering repeating bursts from FRB sources 4-13 , but no convincing evidence has been collected so far 14 . Recently, the Galactic magnetar SRG 1935+2154 entered an active phase by emitting intense soft γ-ray bursts 15 . One FRB-like event with two peaks (FRB 200428) and a luminosity slightly lower than the faintest extragalactic FRBs was detected from the source, in association with a soft γ-ray/hard-X-ray flare 18-21 . Here we report an eight-hour targeted radio observational campaign comprising four sessions and assisted by multi-wavelength (optical and hard-X-ray) data. During the third session, 29 soft-γ-ray repeater (SGR) bursts were detected in γ-ray energies. Throughout the observing period, we detected no single dispersed pulsed emission coincident with the arrivals of SGR bursts, but unfortunately we were not observing when the FRB was detected. The non-detection places a fluence upper limit that is eight orders of magnitude lower than the fluence of FRB 200428. Our results suggest that FRB-SGR burst associations are rare. FRBs may be highly relativistic and geometrically beamed, or FRB-like events associated with SGR bursts may have narrow spectra and characteristic frequencies outside the observed band. It is also possible that the physical conditions required to achieve coherent radiation in SGR bursts are difficult to satisfy, and that only under extreme conditions could an FRB be associated with an SGR burst.
Published: 2020
Full Text: View/download PDF

31. 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
Full Text: View/download PDF

32. A peculiar low-luminosity short gamma-ray burst from a double neutron star merger progenitor.

Author: Zhang BB, Zhang B, Sun H, Lei WH, Gao H, Li Y, Shao L, Zhao Y, Hu YD, Lü HJ, Wu XF, Fan XL, Wang G, Castro-Tirado AJ, Zhang S, Yu BY, Cao YY, and Liang EW
Abstract: Double neutron star (DNS) merger events are promising candidates of short gamma-ray burst (sGRB) progenitors as well as high-frequency gravitational wave (GW) emitters. On August 17, 2017, such a coinciding event was detected by both the LIGO-Virgo gravitational wave detector network as GW170817 and Gamma-Ray Monitor on board NASA's Fermi Space Telescope as GRB 170817A. Here, we show that the fluence and spectral peak energy of this sGRB fall into the lower portion of the distributions of known sGRBs. Its peak isotropic luminosity is abnormally low. The estimated event rate density above this luminosity is at least [Formula: see text] Gpc -3 yr -1 , which is close to but still below the DNS merger event rate density. This event likely originates from a structured jet viewed from a large viewing angle. There are similar faint soft GRBs in the Fermi archival data, a small fraction of which might belong to this new population of nearby, low-luminosity sGRBs.
Published: 2018
Full Text: View/download PDF

33. A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni.

Author: Dallilar Y, Eikenberry SS, Garner A, Stelter RD, Gottlieb A, Gandhi P, Casella P, Dhillon VS, Marsh TR, Littlefair SP, Hardy L, Fender R, Mooley K, Walton DJ, Fuerst F, Bachetti M, Castro-Tirado AJ, Charcos M, Edwards ML, Lasso-Cabrera NM, Marin-Franch A, Raines SN, Ackley K, Bennett JG, Cenarro AJ, Chinn B, Donoso HV, Frommeyer R, Hanna K, Herlevich MD, Julian J, Miller P, Mullin S, Murphey CH, Packham C, Varosi F, Vega C, Warner C, Ramaprakash AN, Burse M, Punnadi S, Chordia P, Gerarts A, de Paz Martín H, Calero MM, Scarpa R, Acosta SF, Hernández Sánchez WM, Siegel B, Pérez FF, Viera Martín HD, Rodríguez Losada JA, Nuñez A, Tejero Á, Martín González CE, Rodríguez CC, Molgó J, Rodriguez JE, Cáceres JIF, Rodríguez García LA, Lopez MH, Dominguez R, Gaggstatter T, Lavers AC, Geier S, Pessev P, and Sarajedini A
Abstract: Observations of binary stars containing an accreting black hole or neutron star often show x-ray emission extending to high energies (>10 kilo--electron volts), which is ascribed to an accretion disk corona of energetic particles akin to those seen in the solar corona. Despite their ubiquity, the physical conditions in accretion disk coronae remain poorly constrained. Using simultaneous infrared, optical, x-ray, and radio observations of the Galactic black hole system V404 Cygni, showing a rapid synchrotron cooling event in its 2015 outburst, we present a precise 461 ± 12 gauss magnetic field measurement in the corona. This measurement is substantially lower than previous estimates for such systems, providing constraints on physical models of accretion physics in black hole and neutron star binary systems., (Copyright © 2017 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.)
Published: 2017
Full Text: View/download PDF

34. Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger.

Author: Pian E, D'Avanzo P, Benetti S, Branchesi M, Brocato E, Campana S, Cappellaro E, Covino S, D'Elia V, Fynbo JPU, Getman F, Ghirlanda G, Ghisellini G, Grado A, Greco G, Hjorth J, Kouveliotou C, Levan A, Limatola L, Malesani D, Mazzali PA, Melandri A, Møller P, Nicastro L, Palazzi E, Piranomonte S, Rossi A, Salafia OS, Selsing J, Stratta G, Tanaka M, Tanvir NR, Tomasella L, Watson D, Yang S, Amati L, Antonelli LA, Ascenzi S, Bernardini MG, Boër M, Bufano F, Bulgarelli A, Capaccioli M, Casella P, Castro-Tirado AJ, Chassande-Mottin E, Ciolfi R, Copperwheat CM, Dadina M, De Cesare G, Di Paola A, Fan YZ, Gendre B, Giuffrida G, Giunta A, Hunt LK, Israel GL, Jin ZP, Kasliwal MM, Klose S, Lisi M, Longo F, Maiorano E, Mapelli M, Masetti N, Nava L, Patricelli B, Perley D, Pescalli A, Piran T, Possenti A, Pulone L, Razzano M, Salvaterra R, Schipani P, Spera M, Stamerra A, Stella L, Tagliaferri G, Testa V, Troja E, Turatto M, Vergani SD, and Vergani D
Abstract: The merger of two neutron stars is predicted to give rise to three major detectable phenomena: a short burst of γ-rays, a gravitational-wave signal, and a transient optical-near-infrared source powered by the synthesis of large amounts of very heavy elements via rapid neutron capture (the r-process). Such transients, named 'macronovae' or 'kilonovae', are believed to be centres of production of rare elements such as gold and platinum. The most compelling evidence so far for a kilonova was a very faint near-infrared rebrightening in the afterglow of a short γ-ray burst at redshift z = 0.356, although findings indicating bluer events have been reported. Here we report the spectral identification and describe the physical properties of a bright kilonova associated with the gravitational-wave source GW170817 and γ-ray burst GRB 170817A associated with a galaxy at a distance of 40 megaparsecs from Earth. Using a series of spectra from ground-based observatories covering the wavelength range from the ultraviolet to the near-infrared, we find that the kilonova is characterized by rapidly expanding ejecta with spectral features similar to those predicted by current models. The ejecta is optically thick early on, with a velocity of about 0.2 times light speed, and reaches a radius of about 50 astronomical units in only 1.5 days. As the ejecta expands, broad absorption-like lines appear on the spectral continuum, indicating atomic species produced by nucleosynthesis that occurs in the post-merger fast-moving dynamical ejecta and in two slower (0.05 times light speed) wind regions. Comparison with spectral models suggests that the merger ejected 0.03 to 0.05 solar masses of material, including high-opacity lanthanides.
Published: 2017
Full Text: View/download PDF

35. Compact low resolution spectrograph, an imaging and long slit spectrograph for robotic telescopes.

Author: Rabaza O, Jelinek M, Castro-Tirado AJ, Cunniffe R, Zeman J, Hudec R, Sabau-Graziati L, and Ruedas-Sánchez J
Abstract: The COmpact LOw REsolution Spectrograph (COLORES) is a compact and lightweight (13 kg) f/8 imaging spectrograph designed for robotic telescopes, now installed and operating on the TELMA, a rapid-slewing 60 cm telescope of the BOOTES-2 observatory in Málaga (Spain). COLORES is a multi-mode instrument that enables the observer to seamlessly switch between low-dispersion spectroscopy and direct imaging modes during an observation. In this paper, we describe the instrument and its development, from the initial scientific requirements through the optical design process to final configuration with theoretical performance calculations. The mechanical and electronic design is described, methods of calibration are discussed and early laboratory and scientific results are shown.
Published: 2013
Full Text: View/download PDF

36. Slewing Mirror Telescope optics for the early observation of UV/optical photons from Gamma-Ray Bursts.

Author: Jeong S, Nam JW, Ahn KB, Park IH, Kim SW, Lee J, Lim H, Brandt S, Budtz-Jørgensen C, Castro-Tirado AJ, Chen P, Cho MH, Choi JN, Grossan B, Huang MA, Jung A, Kim JE, Kim MB, Kim YW, Linder EV, Min KW, Na GW, Panasyuk MI, Ripa J, Reglero V, Smoot GF, Suh JE, Svertilov S, Vedenkin N, and Yashin I
Subjects: Equipment Design, Equipment Failure Analysis, Gamma Rays, Photons, Ultraviolet Rays, Lenses, Radiometry instrumentation, Spacecraft instrumentation, Telescopes
Abstract: We report on design, manufacture, and testing of a Slewing Mirror Telescope (SMT), the first of its kind and a part of Ultra-Fast Flash Observatory-pathfinder (UFFO-p) for space-based prompt measurement of early UV/optical light curves from Gamma-Ray Bursts (GRBs). Using a fast slewing mirror of 150 mm diameter mounted on a 2 axis gimbal stage, SMT can deliver the images of GRB optical counterparts to the intensified CCD detector within 1.5~1.8 s over ± 35 degrees in the slewing field of view. Its Ritchey-Chrétien telescope of 100 mm diameter provides a 17 × 17 arcmin² instantaneous field of view. Technical details of design, construction, the laboratory performance tests in space environments for this unique SMT are described in conjunction with the plan for in-orbit operation onboard the Lomonosov satellite in 2013.
Published: 2013
Full Text: View/download PDF

37. A Pluto-like radius and a high albedo for the dwarf planet Eris from an occultation.

Author: Sicardy B, Ortiz JL, Assafin M, Jehin E, Maury A, Lellouch E, Hutton RG, Braga-Ribas F, Colas F, Hestroffer D, Lecacheux J, Roques F, Santos-Sanz P, Widemann T, Morales N, Duffard R, Thirouin A, Castro-Tirado AJ, Jelínek M, Kubánek P, Sota A, Sánchez-Ramírez R, Andrei AH, Camargo JI, da Silva Neto DN, Gomes AR Jr, Martins RV, Gillon M, Manfroid J, Tozzi GP, Harlingten C, Saravia S, Behrend R, Mottola S, Melendo EG, Peris V, Fabregat J, Madiedo JM, Cuesta L, Eibe MT, Ullán A, Organero F, Pastor S, de Los Reyes JA, Pedraz S, Castro A, de la Cueva I, Muler G, Steele IA, Cebrián M, Montañés-Rodríguez P, Oscoz A, Weaver D, Jacques C, Corradi WJ, Santos FP, Reis W, Milone A, Emilio M, Gutiérrez L, Vázquez R, and Hernández-Toledo H
Abstract: The dwarf planet Eris is a trans-Neptunian object with an orbital eccentricity of 0.44, an inclination of 44 degrees and a surface composition very similar to that of Pluto. It resides at present at 95.7 astronomical units (1 AU is the Earth-Sun distance) from Earth, near its aphelion and more than three times farther than Pluto. Owing to this great distance, measuring its size or detecting a putative atmosphere is difficult. Here we report the observation of a multi-chord stellar occultation by Eris on 6 November 2010 UT. The event is consistent with a spherical shape for Eris, with radius 1,163 ± 6 kilometres, density 2.52 ± 0.05 grams per cm(3) and a high visible geometric albedo, Pv = 0.96(+0.09)(-0.04). No nitrogen, argon or methane atmospheres are detected with surface pressure larger than ∼1 nanobar, about 10,000 times more tenuous than Pluto's present atmosphere. As Pluto's radius is estimated to be between 1,150 and 1,200 kilometres, Eris appears as a Pluto twin, with a bright surface possibly caused by a collapsed atmosphere, owing to its cold environment. We anticipate that this atmosphere may periodically sublimate as Eris approaches its perihelion, at 37.8 astronomical units from the Sun.
Published: 2011
Full Text: View/download PDF

38. An extremely luminous panchromatic outburst from the nucleus of a distant galaxy.

Author: Levan AJ, Tanvir NR, Cenko SB, Perley DA, Wiersema K, Bloom JS, Fruchter AS, Postigo Ade U, O'Brien PT, Butler N, van der Horst AJ, Leloudas G, Morgan AN, Misra K, Bower GC, Farihi J, Tunnicliffe RL, Modjaz M, Silverman JM, Hjorth J, Thöne C, Cucchiara A, Cerón JM, Castro-Tirado AJ, Arnold JA, Bremer M, Brodie JP, Carroll T, Cooper MC, Curran PA, Cutri RM, Ehle J, Forbes D, Fynbo J, Gorosabel J, Graham J, Hoffman DI, Guziy S, Jakobsson P, Kamble A, Kerr T, Kasliwal MM, Kouveliotou C, Kocevski D, Law NM, Nugent PE, Ofek EO, Poznanski D, Quimby RM, Rol E, Romanowsky AJ, Sánchez-Ramírez R, Schulze S, Singh N, van Spaandonk L, Starling RL, Strom RG, Tello JC, Vaduvescu O, Wheatley PJ, Wijers RA, Winters JM, and Xu D
Abstract: Variable x-ray and γ-ray emission is characteristic of the most extreme physical processes in the universe. We present multiwavelength observations of a unique γ-ray-selected transient detected by the Swift satellite, accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z = 0.3534. Its high-energy emission has lasted much longer than any γ-ray burst, whereas its peak luminosity was ∼100 times higher than bright active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a rare mechanism involving the massive black hole in the nucleus of that galaxy.
Published: 2011
Full Text: View/download PDF

39. A gamma-ray burst at a redshift of z approximately 8.2.

Author: Tanvir NR, Fox DB, Levan AJ, Berger E, Wiersema K, Fynbo JP, Cucchiara A, Krühler T, Gehrels N, Bloom JS, Greiner J, Evans PA, Rol E, Olivares F, Hjorth J, Jakobsson P, Farihi J, Willingale R, Starling RL, Cenko SB, Perley D, Maund JR, Duke J, Wijers RA, Adamson AJ, Allan A, Bremer MN, Burrows DN, Castro-Tirado AJ, Cavanagh B, de Ugarte Postigo A, Dopita MA, Fatkhullin TA, Fruchter AS, Foley RJ, Gorosabel J, Kennea J, Kerr T, Klose S, Krimm HA, Komarova VN, Kulkarni SR, Moskvitin AS, Mundell CG, Naylor T, Page K, Penprase BE, Perri M, Podsiadlowski P, Roth K, Rutledge RE, Sakamoto T, Schady P, Schmidt BP, Soderberg AM, Sollerman J, Stephens AW, Stratta G, Ukwatta TN, Watson D, Westra E, Wold T, and Wolf C
Abstract: Long-duration gamma-ray bursts (GRBs) are thought to result from the explosions of certain massive stars, and some are bright enough that they should be observable out to redshifts of z > 20 using current technology. Hitherto, the highest redshift measured for any object was z = 6.96, for a Lyman-alpha emitting galaxy. Here we report that GRB 090423 lies at a redshift of z approximately 8.2, implying that massive stars were being produced and dying as GRBs approximately 630 Myr after the Big Bang. The burst also pinpoints the location of its host galaxy.
Published: 2009
Full Text: View/download PDF

40. Flares from a candidate Galactic magnetar suggest a missing link to dim isolated neutron stars.

Author: Castro-Tirado AJ, de Ugarte Postigo A, Gorosabel J, Jelínek M, Fatkhullin TA, Sokolov VV, Ferrero P, Kann DA, Klose S, Sluse D, Bremer M, Winters JM, Nuernberger D, Pérez-Ramírez D, Guerrero MA, French J, Melady G, Hanlon L, McBreen B, Leventis K, Markoff SB, Leon S, Kraus A, Aceituno FJ, Cunniffe R, Kubánek P, Vítek S, Schulze S, Wilson AC, Hudec R, Durant M, González-Pérez JM, Shahbaz T, Guziy S, Pandey SB, Pavlenko L, Sonbas E, Trushkin SA, Bursov NN, Nizhelskij NA, Sánchez-Fernández C, and Sabau-Graziati L
Abstract: Magnetars are young neutron stars with very strong magnetic fields of the order of 10(14)-10(15) G. They are detected in our Galaxy either as soft gamma-ray repeaters or anomalous X-ray pulsars. Soft gamma-ray repeaters are a rare type of gamma-ray transient sources that are occasionally detected as bursters in the high-energy sky. No optical counterpart to the gamma-ray flares or the quiescent source has yet been identified. Here we report multi-wavelength observations of a puzzling source, SWIFT J195509+261406. We detected more than 40 flaring episodes in the optical band over a time span of three days, and a faint infrared flare 11 days later, after which the source returned to quiescence. Our radio observations confirm a Galactic nature and establish a lower distance limit of approximately 3.7 kpc. We suggest that SWIFT J195509+261406 could be an isolated magnetar whose bursting activity has been detected at optical wavelengths, and for which the long-term X-ray emission is short-lived. In this case, a new manifestation of magnetar activity has been recorded and we can consider SWIFT J195509+261406 to be a link between the 'persistent' soft gamma-ray repeaters/anomalous X-ray pulsars and dim isolated neutron stars.
Published: 2008
Full Text: View/download PDF

41. An optical supernova associated with the X-ray flash XRF 060218.

Author: Pian E, Mazzali PA, Masetti N, Ferrero P, Klose S, Palazzi E, Ramirez-Ruiz E, Woosley SE, Kouveliotou C, Deng J, Filippenko AV, Foley RJ, Fynbo JP, Kann DA, Li W, Hjorth J, Nomoto K, Patat F, Sauer DN, Sollerman J, Vreeswijk PM, Guenther EW, Levan A, O'Brien P, Tanvir NR, Wijers RA, Dumas C, Hainaut O, Wong DS, Baade D, Wang L, Amati L, Cappellaro E, Castro-Tirado AJ, Ellison S, Frontera F, Fruchter AS, Greiner J, Kawabata K, Ledoux C, Maeda K, Møller P, Nicastro L, Rol E, and Starling R
Abstract: Long-duration gamma-ray bursts (GRBs) are associated with type Ic supernovae that are more luminous than average and that eject material at very high velocities. Less-luminous supernovae were not hitherto known to be associated with GRBs, and therefore GRB-supernovae were thought to be rare events. Whether X-ray flashes--analogues of GRBs, but with lower luminosities and fewer gamma-rays--can also be associated with supernovae, and whether they are intrinsically 'weak' events or typical GRBs viewed off the axis of the burst, is unclear. Here we report the optical discovery and follow-up observations of the type Ic supernova SN 2006aj associated with X-ray flash XRF 060218. Supernova 2006aj is intrinsically less luminous than the GRB-supernovae, but more luminous than many supernovae not accompanied by a GRB. The ejecta velocities derived from our spectra are intermediate between these two groups, which is consistent with the weakness of both the GRB output and the supernova radio flux. Our data, combined with radio and X-ray observations, suggest that XRF 060218 is an intrinsically weak and soft event, rather than a classical GRB observed off-axis. This extends the GRB-supernova connection to X-ray flashes and fainter supernovae, implying a common origin. Events such as XRF 060218 are probably more numerous than GRB-supernovae.
Published: 2006
Full Text: View/download PDF

42. Long gamma-ray bursts and core-collapse supernovae have different environments.

Author: Fruchter AS, Levan AJ, Strolger L, Vreeswijk PM, Thorsett SE, Bersier D, Burud I, Castro Cerón JM, Castro-Tirado AJ, Conselice C, Dahlen T, Ferguson HC, Fynbo JP, Garnavich PM, Gibbons RA, Gorosabel J, Gull TR, Hjorth J, Holland ST, Kouveliotou C, Levay Z, Livio M, Metzger MR, Nugent PE, Petro L, Pian E, Rhoads JE, Riess AG, Sahu KC, Smette A, Tanvir NR, Wijers RA, and Woosley SE
Abstract: When massive stars exhaust their fuel, they collapse and often produce the extraordinarily bright explosions known as core-collapse supernovae. On occasion, this stellar collapse also powers an even more brilliant relativistic explosion known as a long-duration gamma-ray burst. One would then expect that these long gamma-ray bursts and core-collapse supernovae should be found in similar galactic environments. Here we show that this expectation is wrong. We find that the gamma-ray bursts are far more concentrated in the very brightest regions of their host galaxies than are the core-collapse supernovae. Furthermore, the host galaxies of the long gamma-ray bursts are significantly fainter and more irregular than the hosts of the core-collapse supernovae. Together these results suggest that long-duration gamma-ray bursts are associated with the most extremely massive stars and may be restricted to galaxies of limited chemical evolution. Our results directly imply that long gamma-ray bursts are relatively rare in galaxies such as our own Milky Way.
Published: 2006
Full Text: View/download PDF

43. A photometric redshift of z = 6.39 +/- 0.12 for GRB 050904.

Author: Haislip JB, Nysewander MC, Reichart DE, Levan A, Tanvir N, Cenko SB, Fox DB, Price PA, Castro-Tirado AJ, Gorosabel J, Evans CR, Figueredo E, MacLeod CL, Kirschbrown JR, Jelinek M, Guziy S, de Ugarte Postigo A, Cypriano ES, LaCluyze A, Graham J, Priddey R, Chapman R, Rhoads J, Fruchter AS, Lamb DQ, Kouveliotou C, Wijers RA, Bayliss MB, Schmidt BP, Soderberg AM, Kulkarni SR, Harrison FA, Moon DS, Gal-Yam A, Kasliwal MM, Hudec R, Vitek S, Kubanek P, Crain JA, Foster AC, Clemens JC, Bartelme JW, Canterna R, Hartmann DH, Henden AA, Klose S, Park HS, Williams GG, Rol E, O'Brien P, Bersier D, Prada F, Pizarro S, Maturana D, Ugarte P, Alvarez A, Fernandez AJ, Jarvis MJ, Moles M, Alfaro E, Ivarsen KM, Kumar ND, Mack CE, Zdarowicz CM, Gehrels N, Barthelmy S, and Burrows DN
Abstract: Gamma-ray bursts (GRBs) and their afterglows are the most brilliant transient events in the Universe. Both the bursts themselves and their afterglows have been predicted to be visible out to redshifts of z approximately 20, and therefore to be powerful probes of the early Universe. The burst GRB 000131, at z = 4.50, was hitherto the most distant such event identified. Here we report the discovery of the bright near-infrared afterglow of GRB 050904 (ref. 4). From our measurements of the near-infrared afterglow, and our failure to detect the optical afterglow, we determine the photometric redshift of the burst to be z = 6.39 - 0.12 + 0.11 (refs 5-7). Subsequently, it was measured spectroscopically to be z = 6.29 +/- 0.01, in agreement with our photometric estimate. These results demonstrate that GRBs can be used to trace the star formation, metallicity, and reionization histories of the early Universe.
Published: 2006
Full Text: View/download PDF

44. A very energetic supernova associated with the gamma-ray burst of 29 March 2003.

Author: Hjorth J, Sollerman J, Møller P, Fynbo JP, Woosley SE, Kouveliotou C, Tanvir NR, Greiner J, Andersen MI, Castro-Tirado AJ, Castro Cerón JM, Fruchter AS, Gorosabel J, Jakobsson P, Kaper L, Klose S, Masetti N, Pedersen H, Pedersen K, Pian E, Palazzi E, Rhoads JE, Rol E, van den Heuvel EP, Vreeswijk PM, Watson D, and Wijers RA
Abstract: Over the past five years evidence has mounted that long-duration (>2 s) gamma-ray bursts (GRBs)-the most luminous of all astronomical explosions-signal the collapse of massive stars in our Universe. This evidence was originally based on the probable association of one unusual GRB with a supernova, but now includes the association of GRBs with regions of massive star formation in distant galaxies, the appearance of supernova-like 'bumps' in the optical afterglow light curves of several bursts and lines of freshly synthesized elements in the spectra of a few X-ray afterglows. These observations support, but do not yet conclusively demonstrate, the idea that long-duration GRBs are associated with the deaths of massive stars, presumably arising from core collapse. Here we report evidence that a very energetic supernova (a hypernova) was temporally and spatially coincident with a GRB at redshift z = 0.1685. The timing of the supernova indicates that it exploded within a few days of the GRB, strongly suggesting that core-collapse events can give rise to GRBs, thereby favouring the 'collapsar' model.
Published: 2003
Full Text: View/download PDF

45. Polarimetric constraints on the optical afterglow emission from GRB 990123

Author: Hjorth J, Bjornsson G, Andersen MI, Caon N, Cairos LM, Castro-Tirado AJ, Osorio MR, Pedersen H, and Costa E
Abstract: Polarization of the optical emission from GRB 990123 was measured on 24.17 January 1999 universal time with the Nordic Optical Telescope. An upper limit of 2.3% on the linear polarization was found. Accurate polarization measurements provide important clues to the blast wave geometry and magnetic field structure of gamma-ray bursts (GRBs). The lack of detectable polarization for GRB 990123 indicates that the optical afterglow was produced by a blast wave of unknown geometry with an insignificant coherent magnetic field or by a beamed outflow at high Lorentz factor seen at a small viewing angle. Such a collimated jet would help solve the problem of energy release in this exceptionally luminous cosmological burst.
Published: 1999
Full Text: View/download PDF

46. Decay of the GRB 990123 optical afterglow: implications for the fireball model

Author: Castro-Tirado AJ, Zapatero-Osorio MR, Caon N, Cairos LM, Hjorth J, Pedersen H, Andersen MI, Gorosabel J, Bartolini C, Guarnieri A, Piccioni A, Frontera F, Masetti N, Palazzi E, Pian E, Greiner J, Hudec R, Sagar R, Pandey AK, Mohan V V, Yadav RK, Nilakshi, Bjornsson C, Jakobsson P, Burud I I, Courbin F, Valentini G, Piersimoni A, Aceituno J, Montoya LM, Pedraz S, Gredel R, Claver CF, Rector TA, Rhoads JE, Walter F, Ott J, Hippelein H, Sàsnchez-Bèjar V, Gutiérrez C, Wei J, Zhou A, Guziy S, Shlyapnikov A, Heise J, Costa E, Feroci M, and Piro L
Abstract: Broad-band (ultraviolet to near-infrared) observations of the intense gamma ray burst GRB 990123 started approximately 8.5 hours after the event and continued until 18 February 1999. When combined with other data, in particular from the Robotic Telescope and Transient Source Experiment (ROTSE) and the Hubble Space Telescope (HST), evidence emerges for a smoothly declining light curve, suggesting some color dependence that could be related to a cooling break passing the ultraviolet-optical band at about 1 day after the high-energy event. The steeper decline rate seen after 1.5 to 2 days may be evidence for a collimated jet pointing toward the observer.
Published: 1999
Full Text: View/download PDF

47. Spectroscopic limits on the distance and energy release of GRB 990123

Author: Andersen MI, Castro-Tirado AJ, Hjorth J, Moller P, Pedersen H, Caon N, Cairos LM, Korhonen H, Osorio MR, Perez E, and Frontera F
Abstract: An optical spectrum of the afterglow from the unusually bright gamma-ray burst GRB 990123 obtained on 24.25 January 1999 universal time showed an absorption system at a redshift of z = 1.600. The absence of a hydrogen Lyman alpha forest sets an upper limit of z < 2.17, whereas ultraviolet photometry indicates an upper limit of z < 2.05. The probability of intersecting an absorption system as strong as the one observed along a random line of sight out to this z is at most a few percent, implying that GRB 990123 was probably at z = 1. 600. Currently favored cosmological parameters imply that an isotropic energy release equivalent to the rest mass of 1.8 neutron stars (4.5 x 10(54) erg) was emitted in gamma rays. Nonisotropic emission, such as intrinsic beaming, may resolve this energy problem.
Published: 1999
Full Text: View/download PDF

48. Photometry and spectroscopy of the GRB 970508 optical counterpart

Author: Castro-Tirado AJ, Gorosabel J, Benitez N, Wolf C, Fockenbrock R, Martinez-Gonzalez E, Kristen H, Broeils A, Pedersen H, Greiner J, Costa E, Feroci M, Piro L, Frontera F, Nicastro L, Palazzi E, Bartolini C, Guarnieri A, Masetti N, Piccioni A, Mignoli M, Wold M, Lacy M, Birkle K, Broadhurst T, Brandt S, and Lund N
Abstract: An optical transient within the error box of the gamma ray burst GRB 970508 was imaged 4 hours after the event. It displayed a strong ultraviolet excess, and reached maximum brightness 2 days later. The optical spectra did not show any emission lines, and no variations on time scales of minutes were observed for 1 hour during the decline phase. According to the fireball and afterglow models, the intensity should rise monotonically before the observed optical maximum, but the data indicate that another physical mechanism may be responsible for the constant phase seen during the first hours after the burst.
Published: 1998
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Database

Publisher

48 results on '"Castro-Tirado AJ"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources