Author: "Strom, R." - Searchworks@Jio Institute Digital Library Search Results

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1,137 results on '"Strom, R."'

1. Periodic and Phase-locked Modulation in PSR B1929+10 Observed with FAST

Author: Kou, F. F., Yan, W. M., Peng, B., Lu, J. G., Liu, K., Zhang, C. M., Strom, R. G., Wang, L., Yuan, J. P., Yuen, Rai, Yu, Y. Z., Yao, J. M., Liu, B., Yan, J., Jiang, P., Jin, C. J., Li, D., Qian, L., Yue, Y. L., and Zhu, Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a detailed single-pulse analysis for PSR B1929+10 based on observations with the Five-hundred-meter Aperture Spherical radio Telescope (FAST). The main pulse and interpulse are found to be modulated with a periodicity of $\sim12$ times the pulsar's rotational period ($P$). The $\sim12P$ modulation is confirmed as a periodic amplitude modulation instead of systematic drifting. The periodic amplitude modulation in the IP is found to be anti-correlated with that in the weak preceding component of the MP (MP_I), but correlated with that in the first two components of the MP (MP_II), which implies that the modulation patterns in the IP and the MP are phase-locked. What is more interesting is that the modulation in MP_II is delayed that in the IP by about 1P. Furthermore, high sensitivity observations by FAST reveal that weak emission exists between the MP and the IP. In addition, we confirm that the separation between the IP and the MP is independent of radio frequency. The above results are a conundrum for pulsar theories and cannot be satisfactorily explained by the current pulsar models. Therefore, our results observed with FAST provide an opportunity to probe the structure of pulsar emission and the neutron star's magnetosphere., Comment: 13 pages 12 figures
Published: 2020
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2. Mechanisms and dynamics of the NH+2+ H+and NH++ H++ H fragmentation channels upon single-photon double ionization of NH3

Author: Larsen, KA, Rescigno, TN, Streeter, ZL, Iskandar, W, Heck, S, Gatton, A, Champenois, EG, Severt, T, Strom, R, Jochim, B, Reedy, D, Call, D, Moshammer, R, Dörner, R, Landers, AL, Williams, JB, Mccurdy, CW, Lucchese, RR, Ben-Itzhak, I, Slaughter, DS, and Weber, T
Subjects: photoionization, photodissociation, COLTRIMS, double ionization, intersystem crossing, non-adiabatic dynamics, autoionization, physics.chem-ph, physics.atom-ph, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Optical Physics, Theoretical and Computational Chemistry, General Physics, Atomic, Molecular, Nuclear, Particle and Plasma Physics
Abstract: We present state-selective measurements on the NH2+ + H+ and NH+ + H+ + H dissociation channels following single-photon double ionization at 61.5 eV of neutral NH3, where the two photoelectrons and two cations are measured in coincidence using 3D momentum imaging. Three dication electronic states are identified to contribute to the NH2+ + H+ dissociation channel, where the excitation in one of the three states undergoes intersystem crossing prior to dissociation, producing a cold NH2+ fragment. In contrast, the other two states directly dissociate, producing a ro-vibrationally excited NH2+ fragment with roughly 1 eV of internal energy. The NH+ + H+ + H channel is fed by direct dissociation from three intermediate dication states, one of which is shared with the NH2+ + H+ channel. We find evidence of autoionization contributing to each of the double ionization channels. The distributions of the relative emission angle between the two photoelectrons, as well as the relative angle between the recoil axis of the molecular breakup and the polarization vector of the ionizing field, are also presented to provide insight on both the photoionization and photodissociation mechanisms for the different dication states.
Published: 2020

3. Photoelectron and fragmentation dynamics of the H++ H+ dissociative channel in NH3 following direct single-photon double ionization

Author: Larsen, KA, Rescigno, TN, Severt, T, Streeter, ZL, Iskandar, W, Heck, S, Gatton, A, Champenois, EG, Strom, R, Jochim, B, Reedy, D, Call, D, Moshammer, R, Dörner, R, Landers, AL, Williams, JB, McCurdy, CW, Lucchese, RR, Ben-Itzhak, I, Slaughter, DS, and Weber, T
Subjects: physics.chem-ph, physics.atom-ph
Abstract: We report measurements on the H++H+ fragmentation channel following direct single-photon double ionization of neutral NH3 at 61.5 eV, where the two photoelectrons and two protons are measured in coincidence using three-dimensional (3D) momentum imaging. We identify four dication electronic states that contribute to H++H+ dissociation, based on our multireference configuration-interaction calculations of the dication potential energy surfaces. The extracted branching ratios between these four dication electronic states are presented. Of the four dication electronic states, three dissociate in a concerted process, while the fourth undergoes a sequential fragmentation mechanism. We find evidence that the neutral NH fragment or intermediate NH+ ion is markedly rovibrationally excited. We also identify differences in the relative emission angle between the two photoelectrons as a function of their energy sharing for the four different dication states, which bare some similarities to previous observations made on atomic targets.
Published: 2020

4. Symmetry breaking in the body-fixed electron emission pattern due to electron-retroaction in the photodissociation of H2+ and D2+ close to threshold

Author: Heck, S, Gatton, A, Larsen, KA, Iskandar, W, Champenois, EG, Strom, R, Landers, A, Reedy, D, Dailey, C, Williams, JB, Severt, T, Jochim, B, Ben-Itzhak, I, Moshammer, R, Dörner, R, Slaughter, DS, and Weber, T
Abstract: We present an experimental investigation of symmetry breaking of H2 and D2 molecules after single photoionization due to the Coulomb field of the emitted slow electron interacting with the parent cation during dissociation. The experiments were carried out by measuring the three-dimensional momentum vectors of the photoelectron and recoiling ion in coincidence using a reaction microscope. For photon energies close to threshold, the low-energy photoelectron influences the dissociation process, which results in an asymmetric molecular frame photoelectron angular distribution. This can be explained by the retroaction of the Coulomb field of the photoelectron on its parent ion and has been recently experimentally demonstrated by M. Waitz et al. [Phys. Rev. Lett. 116, 043001 (2016)PRLTAO0031-900710.1103/PhysRevLett.116.043001], confirming theoretical predictions by V. V. Serov and A. S. Kheifets [Phys. Rev. A 89, 031402(R) (2014)PLRAAN1050-294710.1103/PhysRevA.89.031402]. High-momentum resolution and a new series of photon energies just above the dissociation threshold enable the observation of a strong influence of the electron energy and nuclear kinetic energy on the electron localization process for energies below ∼100 meV, which so far has neither been observed nor discussed by theory. Exploring the limitations of the retroaction mechanism at our lowest photon energy, we are able to single out a sensitive testbed and present data of non-Born-Oppenheimer dynamics of the simplest molecular system for future benchmark computational treatments.
Published: 2019

5. Investigation of the cosmic ray population and magnetic field strength in the halo of NGC 891

Author: Mulcahy, D. D., Horneffer, A., Beck, R., Krause, M., Schmidt, P., Basu, A., Chyzy, K. T., Dettmar, R. -J., Haverkorn, M., Heald, G., Heesen, V., Horellou, C., Iacobelli, M., Nikiel-Wroczynski, B., Paladino, R., Scaife, A. M. M., Sridhar, Sarrvesh S., Strom, R. G., Tabatabaei, F. S., Cantwel, T., Carey, S. H., Grainge, K., Hickish, J., Perrot, Y., Razavi-Ghods, N., Scott, P., and Titterington, D.
Subjects: Astrophysics - Astrophysics of Galaxies, J.2
Abstract: Low-frequency radio continuum observations of edge-on galaxies are ideal to study cosmic-ray electrons (CREs) in halos via radio synchrotron emission and to measure magnetic field strengths. We obtained new observations of the edge-on spiral galaxy NGC 891 at 129-163 MHz with the LOw Frequency ARray (LOFAR) and at 13-18 GHz with the Arcminute Microkelvin Imager (AMI) and combine them with recent high-resolution Very Large Array (VLA) observations at 1-2 GHz, enabling us to study the radio continuum emission over two orders of magnitude in frequency. The spectrum of the integrated nonthermal flux density can be fitted by a power law with a spectral steepening towards higher frequencies or by a curved polynomial. Spectral flattening at low frequencies due to free-free absorption is detected in star-forming regions of the disk. The mean magnetic field strength in the halo is 7 +- 2 $\mu$G. The scale heights of the nonthermal halo emission at 146 MHz are larger than those at 1.5 GHz everywhere, with a mean ratio of 1.7 +- 0.3, indicating that spectral ageing of CREs is important and that diffusive propagation dominates. The halo scale heights at 146 MHz decrease with increasing magnetic field strengths which is a signature of dominating synchrotron losses of CREs. On the other hand, the spectral index between 146 MHz and 1.5 GHz linearly steepens from the disk to the halo, indicating that advection rather than diffusion is the dominating CRE transport process. This issue calls for refined modelling of CRE propagation., Comment: Accepted for publication in Astronomy & Astrophysics
Published: 2018
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6. Search for High-energy Neutrinos from Gravitational Wave Event GW151226 and Candidate LVT151012 with ANTARES and IceCube

Author: Albert, A., Andre, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J. -J., Avgitas, T., Baret, B., Barrios-Marti, J., Basa, S., Bertin, V., Biagi, S., Bormuth, R., Bourret, S., Bouwhuis, M. C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Deschamps, A., De Bonis, G., Distefano, C., Di Palma, I., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Bojaddaini, I. El, Elsasser, D., Enzenhofer, A., Felis, I., Fusco, L. A., Galata, S., Gay, P., Giordano, V., Glotin, H., Gregoire, T., Ruiz, R. Gracia, Graf, K., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hoessl, J., Hofestadt, J., Hugon, C., Illuminati, G., James, C. W., de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Kiessling, D., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mathieu, A., Mele, R., Melis, K., Michael, T., Migliozzi, P., Moussa, A., Nezri, E., Pavalas, G. E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Riccobene, G., Sanchez-Losa, A., Saldana, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schussler, F., Sieger, C., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Turpin, D., Tonnis, C., Vallage, B., Vallee, C., Van Elewyck, V., Versari, F., Vivolo, D., Vizzoca, A., Wilms, J., Zornoza, J. D., Zuniga, J., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Samarai, I. Al, Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Archinger, M., Arguelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H., BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Bos, F., Bose, D., Boser, S., Botner, O., Bradascio, F., Braun, J., Brayeur, L., Bretz, H. -P., Bron, S., Burgman, A., Carver, T., Casier, M., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Cowen, D. F., Cross, R., Day, M., de Andre, J. P. A. M., De Clercq, C., Rosendo, E. del Pino, Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Diaz-Velez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Euler, S., Evenson, P. A., Fahey, S., Fazely, A. R., Feintzeig, J., Felde, J., Filimonov, K., Finley, C., Flis, S., Fosig, C. -C., Franckowiak, A., Friedman, E., Fuchs, T., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Giang, W., Gladstone, L., Glauch, T., Glusenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Gri_th, Z., Haack, C., Hallgren, A., Halzen, F., Hansen, E., Hansmann, T., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., In, S., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kang, W., Kappes, A., Karg, T., Karle, A., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Kohnen, G., Koirala, R., Kolanoski, H., Konietz, R., Kopke, L., Kopper, C., Kopper, S., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Kruckl, G., Kruger, C., Kunnen, J., Kunwar, S., Kurahashi, N., Kuwabara, T., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lennarz, D., Lesiak-Bzdak, M., Leuermann, M., Lu, L., Lunemann, J., Madsen, J., Maggi, G., Mahn, K. B. M., Mancina, S., Maruyama, R., Mase, K., Maunu, R., McNally, F., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Moment_e, G., Montaruli, T., Moulai, M., Nahnhauer, R., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Penek, O., Pepper, J. A., Heros, C. P_erez de los, Pieloth, D., Pinat, E., Price, P. B., Przybylski, G. T., Quinnan, M., Raab, C., Radel, L., Rameez, M., Rawlins, K., Reimann, R., Relethford, B., Relich, M., Resconi, E., Rhode, W., Richman, M., Riedel, B., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Sabbatini, L., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Sarkar, S., Satalecka, K., Schlunder, P., Schmidt, T., Schoenen, S., Schoneberg, S., Schumacher, L., Seckel, D., Seunarine, S., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stanev, T., Stasik, A., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stossl, A., Strom, R., Strotjohann, N. L., Sullivan, G. W., Sutherland, M., Taavola, H., Taboada, I., Tatar, J., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tesic, G., Tilav, S., Toale, P. A., Tobin, M. N., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Unger, E., Usner, M., Vandenbroucke, J., van Eijndhoven, N., Vanheule, S., van Rossem, M., van Santen, J., Vehring, M., Voge, M., Vogel, E., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandkowsky, N., Waza, A., Weaver, Ch., Weiss, M. J., Wendt, C., Westerhoff, S., Whelan, B. J., Wickmann, S., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, T. R., Woolsey, E., Woschnagg, K., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Zoll, M., 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., A_eldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Avila-Alvarez, A., 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., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Beer, C., Bejger, M., Belahcene, I., Belgin, M., Bell, A. S., Berger, B. K., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bou_anais, 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., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder_on, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavagli_a, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. Cerboni, Cerretani, G., Cesarini, E., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Cheeseboro, B. D., Chen, H. Y., Chen, Y., Cheng, H. -P., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conti, L., Cooper, S. J., 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., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Dattilo, V., Dave, I., Davier, M., Davies, G. S., Davis, D., Daw, E. J., Day, B., Day, R., De, S., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Del_eglise, S., Del Pozzo, W., Denker, T., Dent, T., Dergachev, V., De Rosa, R., DeRosa, R. T., DeSalvo, R., Devine, R. C., Dhurandhar, S., D__az, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Virgilio, A., Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Alvarez, M. Dovale, 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., E_er, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Etienne, Z., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Galiana, A. Fern_andez, Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fong, H., Forsyth, S. S., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fy_e, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garu_, F., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., Gonz_alez, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., 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., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Henry, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jim_enez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Karvinen, K. S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kefelian, F., Keitel, D., Kelley, D. B., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, Whansun, Kim, W., Kim, Y. -M., Kimbrell, S. J., King, E. J., King, P. J., Kirchhoff, R., Kissel, J. S., Klein, B., Kleybolte, L., Klimenko, S., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kramer, C., Kringel, V., Krolak, A., Kuehn, G., Kumar, P., Kumar, R., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Libson, A., Littenberg, T. B., Liu, J., Lockerbie, N. A., Lombardi, A. L., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lovelace, G., Luck, H., Lundgren, A. P., Lynch, R., Ma, Y., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Magana-Sandoval, F., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., M_arka, S., M_arka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martynov, D. V., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D. E., McCormick, S., McGrath, C., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Mezzani, F., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Miller, B. B., 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., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E. A. M., Murray, P. G., Mytidis, A., Napier, K., Nardecchia, I., Naticchioni, L., Nelemans, G., Nelson, T. J. N., Neri, M., Nery, M., Neunzert, A., Newport, J. M., Newton, G., Nguyen, T. T., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., Normandin, M. E. N., Nuttall, L. K., Oberling, J., Ochsner, E., Oelker, E., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., 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., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfei_er, H. P., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Predoi, V., Prestegard, T., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Purrer, M., Qi, H., Qin, J., Qiu, S., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Ra_ai, P., Raja, S., Rajan, C., Rakhmanov, M., Rapagnani, P., Raymond, V., Razzano, M., Re, V., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rew, H., Reyes, S. D., Rhoades, E., Ricci, F., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, R., Romie, J. H., Rosi_nska, D., Rowan, S., Rudiger, A., Ruggi, P., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sandberg, V., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheuer, J., Schmidt, E., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schonbeck, A., Schreiber, E., Schuette, D., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Sha_er, T. J., Shahriar, M. S., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, A., Singer, L. P., Singh, A., Singh, R., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, B., Smith, J. R., Smith, R. J. E., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stephens, B. C., Stevenson, S. P., Stone, R., Strain, K. A., Straniero, N., Stratta, G., Strigin, S. E., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Sutton, P. J., Swinkels, B. L., Szczepa_nczyk, M. J., Tacca, M., Talukder, D., Tanner, D. B., T_apai, M., Taracchini, A., Taylor, R., Theeg, T., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tippens, T., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tomlinson, C., Tonelli, M., Tornasi, Z., Torrie, C. I., Toyra, D., Travasso, F., Traylor, G., Trifiro, D., Trinastic, J., Tringali, M. C., Trozzo, L., Tse, M., Tso, R., 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., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vas_uth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicere, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Voss, D. V., 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, Y., Ward, R. L., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., We_els, P., Westphal, T., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Worden, J., Wright, J. L., Wu, D. S., Wu, G., Yam, W., Yamamoto, H., Yancey, C. C., Yap, M. J., Yu, Hang, Yu, Haocun, Yvert, M., Zadrozny, A., Zangrando, L., Zanolin, M., Zendri, J. -P., Zevin, M., Zhang, L., Zhang, M., Zhang, T., Zhang, Y., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Advanced LIGO observatories detected gravitational waves from two binary black hole mergers during their first observation run (O1). We present a high-energy neutrino follow-up search for the second gravitational wave event, GW151226, as well as for gravitational wave candidate LVT151012. We find 2 and 4 neutrino candidates detected by IceCube, and 1 and 0 detected by ANTARES, within $\pm500$ s around the respective gravitational wave signals, consistent with the expected background rate. None of these neutrino candidates are found to be directionally coincident with GW151226 or LVT151012. We use non-detection to constrain isotropic-equivalent high-energy neutrino emission from GW151226 adopting the GW event's 3D localization, to less than $2\times 10^{51}-2\times10^{54}$ erg., Comment: 7 pages (+ author list), 4 figures
Published: 2017
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7. Resonance signatures in the body-frame valence photoionization of CF 4

Author: Larsen, KA, Trevisan, CS, Lucchese, RR, Heck, S, Iskandar, W, Champenois, E, Gatton, A, Moshammer, R, Strom, R, Severt, T, Jochim, B, Reedy, D, Weller, M, Landers, AL, Williams, JB, Ben-Itzhak, I, Dörner, R, Slaughter, D, McCurdy, CW, Weber, Th, and Rescigno, TN
Subjects: Physical Sciences, Chemical Sciences, Atomic, Molecular and Optical Physics, Physical Chemistry, Chemical Physics
Abstract: We present a combined experimental and theoretical investigation of the electron dynamics and body-frame angular dependence of valence photo-single ionization of CF4 and subsequent dissociation into CF3+ and F. Ionization from a valence t2 orbital shows overlapping shape resonances close to threshold that couple to the same total symmetry, leading to striking changes in the photoelectron angular distributions when viewed in the body-frame.
Published: 2018

8. Very High-Energy Gamma-Ray Follow-Up Program Using Neutrino Triggers from IceCube

Author: IceCube Collaboration, Aartsen, M. G., Abraham, K., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Archinger, M., Arguelles, C., Auffenberg, J., Axani, S., Bai, X., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Becker-Tjus, J., Becker, K. -H., BenZvi, S., Berley, D., Bernardini, E., Bernhard, A., Besson, D. Z., Binder, G., Bindig, D., Bissok, M., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Bos, F., Bose, D., Boser, S., Botner, O., Braun, J., Brayeur, L., Bretz, H. -P., Bron, S., Burgman, A., Carver, T., Casier, M., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Cross, D. F. Cowen R., Day, M., de Andre, J. P. A. M., De Clercq, C., Rosendo, E. del Pino, Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Diaz-Velez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Euler, S., Evenson, P. A., Fahey, S., Fazely, A. R., Feintzeig, J., Felde, J., Filimonov, K., Finley, C., Flis, S., Fosig, C. -C., Franckowiak, A., Franke, R., Friedman, E., Fuchs, T., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Giang, W., Gladstone, L., Glauch, T., Glusenkamp, T., Goldschmidt, A., Golup, G., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Ismail, A. Haj, Hallgren, A., Halzen, F., Hansen, E., Hansmann, T., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Holzapfel, K., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., In, S., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Jurkovic, M., Kappes, A., Karg, T., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Kohnen, G., Koirala, R., Kolanoski, H., Konietz, R., Kopke, L., Kopper, C., Kopper, S., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Kruckl, G., Kruger, C., Kunnen, J., Kunwar, S., Kurahashi, N., Kuwabara, T., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lennarz, D., Lesiak-Bzdak, M., Leuermann, M., Lu, L., Lunemann, J., Madsen, J., Maggi, G., Mahn, K. B. M., Mancina, S., Mandelartz, M., Maruyama, R., Mase, K., Maunu, R., McNally, F., Meagher, K., Medici, M., Meier, M., Meli, A., Menne, T., Merino, G., Meures, T., Miarecki, S., Mohrmann, L., Montaruli, T., Moulai, M., Nahnhauer, R., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Penek, O., Pepper, J. A., Heros, C. Perez de los, Pieloth, D., Pinat, E., Price, P. B., Przybylski, G. T., Quinnan, M., Raab, C., Radel, L., Rameez, M., Rawlins, K., Reimann, R., Relethford, B., Relich, M., Resconi, E., Rhode, W., Richman, M., Riedel, B., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Sabbatini, L., Sanchez-Herrera, S. E., Sandrock, A., Sandroos, J., Sarkar, S., Satalecka, K., Schlunder, P., Schmidt, T., Schoenen, S., Schoneberg, S., Schumacher, L., Seckel, D., Seunarine, S., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stanev, T., Stasik, A., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stossl, A., Strom, R., Strotjohann, N. L., Sullivan, G. W., Sutherland, M., Taavola, H., Taboada, I., Tatar, J., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tevsic, G., Tilav, S., Toale, P. A., Tobin, M. N., Toscano, S., Tosi, D., Tselengidou, M., Turcati, A., Unger, E., Usner, M., Vandenbroucke, J., van Eijndhoven, N., Vanheule, S., van Rossem, M., van Santen, J., Veenkamp, J., Vehring, M., Voge, M., Vogel, E., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandkowsky, N., Weaver, Ch., Weiss, M. J., Wendt, C., Westerhoff, S., Whelan, B. J., Wickmann, S., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, T. R., Woolsey, E., Woschnagg, K., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Collaboration, M. Zoll MAGIC, Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Antoranz, P., Babic, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J. A., Gonzalez, J. Becerra, Bednarek, W., Berti, A., Biasuzzi, B., Biland, A., Blanch, O., Bonnefoy, S., Bonnoli, G., Borracci, F., Bretz, T., Buson, S., Carosi, A., Chatterjee, A., Clavero, R., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Wilhelmi, E. de Ona, Di Pierro, F., Doert, M., Dominguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Einecke, S., Glawion, D. Eisenacher, Elsaesser, D., Engelkemeier, M., Ramazani, V. Fallah, Fernandez-Barral, A., Fidalgo, D., Fonseca, M. V., Font, L., Frantzen, K., Fruck, C., Galindo, D., Lopez, R. J. Garcia, Garczarczyk, M., Terrats, D. Garrido, Gaug, M., Giammaria, P., Godinovic, N., Munoz, A. Gonzalez, Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hanabata, Y., Hayashida, M., Herrera, J., Hose, J., Hrupec, D., Hughes, G., Idec, W., Kodani, K., Konno, Y., Kubo, H., Kushida, J., La Barbera, A., Lelas, D., Lindfors, E., Lombardi, S., Longo, F., Lopez, M., Lopez-Coto, R., Majumdar, P., Makariev, M., Mallot, K., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Marcote, B., Mariotti, M., Martinez, M., Mazin, D., Menzel, U., Miranda, J. M., Mirzoyan, R., Moralejo, A., Moretti, E., Nakajima, D., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nilsson, K., Nishijima, K., Noda, K., Nogues, L., Overkemping, A., Paiano, S., Palacio, J., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Paredes-Fortuny, X., Pedaletti, G., Peresano, M., Perri, L., Persic, M., Poutanen, J., Moroni, P. G. Prada, Prandini, E., Puljak, I., Reichardt, I., Ribo, M., Rico, J., Garcia, J. Rodriguez, Saito, T., Schroeder, S., Schultz, C., Schweizer, T., Sillanpaa, A., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Steinbring, T., Strzys, M., Suric, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzic, T., Tescaro, D., Teshima, M., Thaele, J., Torres, D. F., Toyama, T., Treves, A., Vanzo, G., Verguilov, V., Vovk, I., Ward, J. E., Will, M., Wu, M. H., Collaboration, R. Zanin VERITAS, Abeysekara, A. U., Archambault, S., Archer, A., Benbow, W., Bird, R., Bourbeau, E., Buchovecky, M., Bugaev, V., Byrum, K., Cardenzana, J. V, Cerruti, M., Ciupik, L., Connolly, M. P., Cui, W., Dickinson, H. J., Dumm, J., Eisch, J. D., Errando, M., Falcone, A., Feng, Q., Finley, J. P., Fleischhack, H., Flinders, A., Fortson, L., Furniss, A., Gillanders, G. H., Griffin, S., Grube, J., Hutten, M., Haakansson, N., Hervet, O., Holder, J., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kelley-Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Maier, G., McArthur, S., McCann, A., Moriarty, P., Mukherjee, R., Nguyen, T., Nieto, D., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Pohl, M., Popkow, A., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rulten, C., Sadeh, I., Santander, M., Sembroski, G. H., Shahinyan, K., Staszak, D., Telezhinsky, I., Tucci, J. V., Tyler, J., Wakely, S. P., Weinstein, A., Wilcox, P., Wilhelm, A., Williams, D. A., and Zitzer, B.
Subjects: High Energy Physics - Experiment, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Instrumentation and Detectors
Abstract: We describe and report the status of a neutrino-triggered program in IceCube that generates real-time alerts for gamma-ray follow-up observations by atmospheric-Cherenkov telescopes (MAGIC and VERITAS). While IceCube is capable of monitoring the whole sky continuously, high-energy gamma-ray telescopes have restricted fields of view and in general are unlikely to be observing a potential neutrino-flaring source at the time such neutrinos are recorded. The use of neutrino-triggered alerts thus aims at increasing the availability of simultaneous multi-messenger data during potential neutrino flaring activity, which can increase the discovery potential and constrain the phenomenological interpretation of the high-energy emission of selected source classes (e.g. blazars). The requirements of a fast and stable online analysis of potential neutrino signals and its operation are presented, along with first results of the program operating between 14 March 2012 and 31 December 2015., Comment: accepted for publication in JINST
Published: 2016
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9. THE RESURFACING HISTORY OF VENUS

Author: BASILEVSKY, A. T., primary, HEAD, J. W., additional, SCHABER, G. G., additional, and STROM, R. G., additional
Published: 2022
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10. Detailed Afterglow Modeling and Host Galaxy Properties of the Dark GRB 111215A

Author: van der Horst, A. J., Levan, A. J., Pooley, G. G., Wiersema, K., Kruhler, T., Perley, D. A., Starling, R. L. C., Curran, P. A., Tanvir, N. R., Wijers, R. A. M. J., Strom, R. G., Kouveliotou, C., Hartoog, O. E., Xu, D., Fynbo, J. P. U., and Jakobsson, P.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Gamma-ray burst (GRB) 111215A was bright at X-ray and radio frequencies, but not detected in the optical or near-infrared (nIR) down to deep limits. We have observed the GRB afterglow with the Westerbork Synthesis Radio Telescope and Arcminute Microkelvin Imager at radio frequencies, with the William Herschel Telescope and Nordic Optical Telescope in the nIR/optical, and with the Chandra X-ray Observatory. We have combined our data with the Swift X-Ray Telescope monitoring, and radio and millimeter observations from the literature to perform broadband modeling, and determined the macro- and microphysical parameters of the GRB blast wave. By combining the broadband modeling results with our nIR upper limits we have put constraints on the extinction in the host galaxy. This is consistent with the optical extinction we have derived from the excess X-ray absorption, and higher than in other dark bursts for which similar modeling work has been performed. We also present deep imaging of the host galaxy with the Keck I telescope, Spitzer Space Telescope, and Hubble Space Telescope (HST), which resulted in a well-constrained photometric redshift, giving credence to the tentative spectroscopic redshift we obtained with the Keck II telescope, and estimates for the stellar mass and star formation rate of the host. Finally, our high resolution HST images of the host galaxy show that the GRB afterglow position is offset from the brightest regions of the host galaxy, in contrast to studies of optically bright GRBs., Comment: 11 pages, 4 figures, 4 tables; accepted for publication in MNRAS
Published: 2014
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11. A Comprehensive Radio View of the Extremely Bright Gamma-Ray Burst 130427A

Author: van der Horst, A. J., Paragi, Z., de Bruyn, A. G., Granot, J., Kouveliotou, C., Wiersema, K., Starling, R. L. C., Curran, P. A., Wijers, R. A. M. J., Rowlinson, A., Anderson, G. A., Fender, R. P., Yang, J., and Strom, R. G.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: GRB 130427A was extremely bright as a result of occurring at low redshift whilst the energetics were more typical of high-redshift gamma-ray bursts (GRBs). We collected well-sampled light curves at 1.4 and 4.8 GHz of GRB 130427A with the Westerbork Synthesis Radio Telescope (WSRT); and we obtained its most accurate position with the European Very Long Baseline Interferometry Network (EVN). Our flux density measurements are combined with all the data available at radio, optical and X-ray frequencies to perform broadband modeling in the framework of a reverse-forward shock model and a two-component jet model, and we discuss the implications and limitations of both models. The low density inferred from the modeling implies that the GRB 130427A progenitor is either a very low-metallicity Wolf-Rayet star, or a rapidly rotating, low-metallicity O star. We also find that the fraction of the energy in electrons is evolving over time, and that the fraction of electrons participating in a relativistic power-law energy distribution is less than 15%. We observed intraday variability during the earliest WSRT observations, and the source sizes inferred from our modeling are consistent with this variability being due to interstellar scintillation effects. Finally, we present and discuss our limits on the linear and circular polarization, which are among the deepest limits of GRB radio polarization to date., Comment: 14 pages, 5 figures, 6 tables; accepted for publication in MNRAS
Published: 2014
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12. Measurement of the Atmospheric $\nu_e$ flux in IceCube

Author: IceCube Collaboration, Aartsen, M. G., Abbasi, R., Abdou, Y., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Altmann, D., Andeen, K., Auffenberg, J., Bai, X., Baker, M., Barwick, S. W., Baum, V., Bay, R., Beattie, K., Beatty, J. J., Bechet, S., Tjus, J. Becker, Becker, K. -H., Bell, M., Benabderrahmane, M. L., BenZvi, S., Berdermann, J., Berghaus, P., Berley, D., Bernardini, E., Bertrand, D., Besson, D. Z., Bindig, D., Bissok, M., Blaufuss, E., Blumenthal, J., Boersma, D. J., Bohaichuk, S., Bohm, C., Bose1, D., Boser, S., Botner, O., Brayeur, L., Brown, A. M., Bruijn, R., Brunner, J., Buitink, S., Carson, M., Casey, J., Casier, M., Chirkin, D., Christy, B., Clark, K., Clevermann, F., Cohen, S., Cowen, D. F., Silva, A. H. Cruz, Danninger, M., Daughhetee, J., Davis, J. C., De Clercq, C., De Ridder, S., Descamps, F., Desiati, P., de Vries-Uiterweerd, G., DeYoung, T., Diaz-Velez, J. C., Dreyer, J., Dumm, J. P., Dunkman, M., Eagan, R., Eberhardt, B., Eisch, J., Ellsworth, R. W., Engdegard, O., Euler, S., Evenson, P. A., Fadiran, O., Fazely, A. R., Fedynitch, A., Feintzeig, J., Feusels, T., Filimonov, K., Finley, C., Fischer-Wasels, T., Flis, S., Franckowiak, A., Franke, R., Frantzen, K., Fuchs, T., Gaisser, T. K., Gallagher, J., Gerhardt, L., Gladstone, L., Glusenkamp, T., Goldschmidt, A., Golup, G., Goodman, J. A., Gora, D., Grant, D., Gross, A., Grullon, S., Gurtner, M., Ha, C., Ismail, A. Haj, Hallgren, A., Halzen, F., Hanson, K., Heereman, D., Heimann, P., Heinen, D., Helbing, K., Hellauer, R., Hickford, S., Hill, G. C., Hoffman, K. D., Hoffmann, R., Homeier, A., Hoshina, K., Huelsnitz, W., Hulth, P. O., Hultqvist, K., Hussain, S., Ishihara, A., Jacobi, E., Jacobsen, J., Japaridze, G. S., Jlelati, O., Kappes, A., Karg, T., Karle, A., Kiryluk, J., Kislat, F., Klas, J., Klein, S. R., Kohne, J. -H., Kohnen, G., Kolanoski, H., Kopke, L., Kopper, C., Kopper, S., Koskinen, D. J., Kowalski, M., Krasberg, M., Kroll, G., Kunnen, J., Kurahashi, N., Kuwabara, T., Labare, M., Landsman, H., Larson, M. J., Lauer, R., Lesiak-Bzdak, M., Lunemann, J., Madsen, J., Maruyama, R., Mase, K., Matis, H. S., McNally, F., Meagher, K., Merck, M., Meszaros, P., Meures, T., Miarecki, S., Middell, E., Milke, N., Miller, J., Mohrmann, L., Montaruli, T., Morse, R., Nahnhauer, R., Naumann, U., Nowicki, S. C., Nygren, D. R., Obertacke, A., Odrowski, S., Olivas, A., Olivo, M., O'Murchadha, A., Panknin, S., Paul, L., Pepper, J. A., Heros, C. Perez de los, Pieloth, D., Pirk, N., Posselt, J., Price, P. B., Przybylski, G. T., Radel, L., Rawlins, K., Redl, P., Resconi, E., Rhode, W., Ribordy, M., Richman, M., Riedel, B., Rodrigues, J. P., Rott, C., Ruhe, T., Ruzybayev, B., Ryckbosch, D., Saba, S. M., Salameh, T., Sander, H. -G., Santander, M., Sarkar, S., Schatto, K., Scheel, M., Scheriau, F., Schmidt, T., Schmitz, M., Schoenen, S., Schoneberg, S., Schonherr, L., Schonwald, A., Schukraft, A., Schulte, L., Schulz, O., Seckel, D., Seo, S. H., Sestayo, Y., Seunarine, S., Sheremata, C., Smith, M. W. E., Soiron, M., Soldin, D., Spiczak, G. M., Spiering, C., Stamatikos, M., Stanev, T., Stasik, A., Stezelberger, T., Stokstad, R. G., Stoss, A., Strahler, E. A., Strom, R., Sullivan, G. W., Taavola, H., Taboada, I., Tamburro, A., Ter-Antonyan, S., Tilav, S., Toale, P. A., Toscano, S., Usner, M., van der Drift, D., van Eijndhoven, N., Van Overloop, A., van Santen, J., Vehring, M., Voge1, M., Vraeghe, M., Walck, C., Waldenmaier, T., Wallraff, M., Walter, M., Wasserman, R., Weaver, Ch., Wendt, C., Westerhoff, S., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Williams, D. R., Wissing, H., Wolf, M., Wood, T. R., Woschnagg, K., Xu, C., Xu, D. L., Xu, X. W., Yanez, J. P., Yodh, G., Yoshida, S., Zarzhitsky, P., Ziemann, J., Zierke, S., Zilles, A., and Zoll, M.
Subjects: High Energy Physics - Experiment, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the first measurement of the atmospheric electron neutrino flux in the energy range between approximately 80 GeV and 6 TeV, using data recorded during the first year of operation of IceCube's DeepCore low energy extension. Techniques to identify neutrinos interacting within the DeepCore volume and veto muons originating outside the detector are demonstrated. A sample of 1029 events is observed in 281 days of data, of which 496 $\pm$ 66(stat.) $\pm$ 88(syst.) are estimated to be cascade events, including both electron neutrino and neutral current events. The rest of the sample includes residual backgrounds due to atmospheric muons and charged current interactions of atmospheric muon neutrinos. The flux of the atmospheric electron neutrinos is consistent with models of atmospheric neutrinos in this energy range. This constitutes the first observation of electron neutrinos and neutral current interactions in a very large volume neutrino telescope optimized for the TeV energy range., Comment: 7 pages, 4 figures (accepted by PRL)
Published: 2012
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13. An extremely luminous panchromatic outburst from the nucleus of a distant galaxy

Author: Levan, A. J., Tanvir, N. R., Cenko, S. B., Perley, D. A., Wiersema, K., Bloom, J. S., Fruchter, A. S., Postigo, A. de Ugarte, O'Brien, P. T., Butler, N., van der Horst, A. J., Leloudas, G., Morgan, A. N., Misra, K., Bower, G., Farihi, J., Tunnicliffe, R. L., Modjaz, M., Silverman, J. M., Hjorth, J., Thoene, C., Cucchiara, A., Ceron, J. M. Castro, Castro-Tirado, A., Arnold, J. A., Bremer, M., Brodie, J. P., Carroll, T., Cooper, M. C., Curran, P. A., Cutri, R. M., Ehle, J., Forbes, D., Fynbo, J., Gorosabel, J., Graham, J., Guizy, S., Hoffman, D. I., Jakobsson, P., Kamble, A., Kerr, T., Kasliwal, M. M., Kouveliotou, C., Kocesvki, D., Law, N. M., Nugent, P. E., Ofek, E. O., Poznanski, D., Quimby, R. M., Rol, E., Romanowsky, A. J., Sanchez-Ramirez, R., Schulze, S., Singh, N., Starling, R. L. C., Strom, R. G., Wheatley, P. J., Wijers, R. A. M. J., Winters, J. M., Wold, T., and Xu, D.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Variable X-ray and gamma-ray emission is characteristic of the most extreme physical processes in the Universe, and studying the sources of these energetic photons has been a major driver in astronomy for the past 50 years. Here we present multiwavelength observations of a unique gamma-ray selected transient, discovered by Swift, which was accompanied by bright emission across the electromagnetic spectrum, and whose properties are unlike any previously observed source. We pinpoint the event to the center of a small, star-forming galaxy at redshift z=0.3534. Its high-energy emission has lasted much longer than any gamma-ray burst, while its peak luminosity was about 100 times higher than the brightest active galactic nuclei. The association of the outburst with the center of its host galaxy suggests that this phenomenon has its origin in a new, rare mechanism associated with a massive black hole in the nucleus of a galaxy.
Published: 2011
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14. A tale of two GRB-SNe at a common redshift of z = 0.54

Author: Cano, Z., Bersier, D., Guidorzi, C., Margutti, R., Svensson, K. M, Kobayashi, S., Melandri, A., Wiersema, K., Pozanenko, A., van der Horst, A. J., Pooley, G. G., Fernandez-Soto, A., Castro-Tirado, A. J., Postigo, A. de Ugarte, Im, M., Kamble, A. P., Sahu, D., Alonso-Lorite, J., Anupama, G., Bibby, J. L., Burgdorf, M. J., Clay, N., Curran, P. A., Fatkhullin, T. A., Fruchter, A. S., Garnavich, P., Gomboc, A., Gorosabel, J., Graham, J. F., Gurugubelli, U., Haislip, J., Huang, K., Huxor, A., Ibrahimov, M., Jeon, Y., Jeon, Y-B., Ivarsen, K., Kasen, D., Klunko, E., Kouveliotou, C., LaCluyze, A., Levan, A. J., Loznikov, V., Mazzali, P. A., Moskvitin, A. S., Mottram, C., Mundell, C. G., Nugent, P. E., Nysewander, M., O'Brien, P. T., Park, W. -K., Peris, V., Pian, E., Reichart, D., Rhoads, J. E., Rol, E., Rumyantsev, V., Scowcroft, V., Shakhovskoy, D., Small, E., Smith, R. J., Sokolov, V. V., Starling, R. L. C., Steele, I., Strom, R. G., Tanvir, N. R., Tsapras, Y., Urata, Y., Vaduvescu, O., Volnova, A., Volvach, A., Wijers, R. A. M. J., Woosley, S. E., and Young, D. R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present ground-based and HST optical observations of the optical transients (OTs) of long-duration Gamma Ray Bursts (GRBs) 060729 and 090618, both at a redshift of z = 0.54. For GRB 060729, bumps are seen in the optical light curves (LCs), and the late-time broadband spectral energy distributions (SEDs) of the OT resemble those of local type Ic supernovae (SNe). For GRB 090618, the dense sampling of our optical observations has allowed us to detect well-defined bumps in the optical LCs, as well as a change in colour, that are indicative of light coming from a core-collapse SN. The accompanying SNe for both events are individually compared with SN1998bw, a known GRB-supernova, and SN1994I, a typical type Ic supernova without a known GRB counterpart, and in both cases the brightness and temporal evolution more closely resemble SN1998bw. We also exploit our extensive optical and radio data for GRB 090618, as well as the publicly-available SWIFT -XRT data, and discuss the properties of the afterglow at early times. In the context of a simple jet-like model, the afterglow of GRB 090618 is best explained by the presence of a jet-break at t-to > 0.5 days. We then compare the rest-frame, peak V -band absolute magnitudes of all of the GRB and X-Ray Flash (XRF)-associated SNe with a large sample of local type Ibc SNe, concluding that, when host extinction is considered, the peak magnitudes of the GRB/XRF-SNe cannot be distinguished from the peak magnitudes of non-GRB/XRF SNe., Comment: Accepted for publication in MNRAS on Dec 07, 2010. 18 pages, 12 figures, 9 tables
Published: 2010
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15. Detailed Radio View on Two Stellar Explosions and Their Host Galaxy: XRF080109/SN2008D and SN2007uy in NGC2770

Author: van der Horst, A. J., Kamble, A. P., Paragi, Z., Sage, L. J., Pal, S., Taylor, G. B., Kouveliotou, C., Granot, J., Ramirez-Ruiz, E., Ishwara-Chandra, C. H., Oosterloo, T. A., Wijers, R. A. M. J., Wiersema, K., Strom, R. G., Bhattacharya, D., Rol, E., Starling, R. L. C., Curran, P. A., and Garrett, M. A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The galaxy NGC2770 hosted two core-collapse supernova explosions, SN2008D and SN2007uy, within 10 days of each other and 9 years after the first supernova of the same type, SN1999eh, was found in that galaxy. In particular SN2008D attracted a lot of attention due to the detection of an X-ray outburst, which has been hypothesized to be caused by either a (mildly) relativistic jet or the supernova shock breakout. We present an extensive study of the radio emission from SN2008D and SN2007uy: flux measurements with the Westerbork Synthesis Radio Telescope and the Giant Metrewave Radio Telescope, covering ~600 days with observing frequencies ranging from 325 MHz to 8.4 GHz. The results of two epochs of global Very Long Baseline Interferometry observations are also discussed. We have examined the molecular gas in the host galaxy NGC2770 with the Arizona Radio Observatory 12-m telescope, and present the implications of our observations for the star formation and seemingly high SN rate in this galaxy. Furthermore, we discuss the near-future observing possibilities of the two SNe and their host galaxy at low radio frequencies with the Low Frequency Array., Comment: 13 pages, 6 figures, 3 tables; accepted for publication in ApJ
Published: 2010
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16. Constraints on the flux of Ultra-High Energy neutrinos from WSRT observations

Author: Buitink, S., Scholten, O., Bacelar, J., Braun, R., de Bruyn, A. G., Falcke, H., Singh, K., Stappers, B., Strom, R. G., and Yahyaoui, R. al
Subjects: Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract: Ultra-high energy (UHE) neutrinos and cosmic rays initiate particle cascades underneath the Moon's surface. These cascades have a negative charge excess and radiate Cherenkov radio emission in a process known as the Askaryan effect. The optimal frequency window for observation of these pulses with radio telescopes on the Earth is around 150 MHz. By observing the Moon with the Westerbork Synthesis Radio Telescope array we are able to set a new limit on the UHE neutrino flux. The PuMa II backend is used to monitor the Moon in 4 frequency bands between 113 and 175 MHz with a sampling frequency of 40 MHz. The narrowband radio interference is digitally filtered out and the dispersive effect of the Earth's ionosphere is compensated for. A trigger system is implemented to search for short pulses. By inserting simulated pulses in the raw data, the detection efficiency for pulses of various strength is calculated. With 47.6 hours of observation time, we are able to set a limit on the UHE neutrino flux. This new limit is an order of magnitude lower than existing limits. In the near future, the digital radio array LOFAR will be used to achieve an even lower limit., Comment: 13 pages, 17 figures, accepted for publication in Astronomy & Astrophysics
Published: 2010
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17. Improved flux limits for neutrinos with energies above 10$^{22}$ eV from observations with the Westerbork Synthesis Radio Telescope

Author: Scholten, O., Buitink, S., Bacelar, J., Braun, R., de Bruyn, A. G., Falcke, H., Singh, K., Stappers, B., Strom, R. G., and Yahyaoui, R. al
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Particle cascades initiated by ultra-high energy (UHE) neutrinos in the lunar regolith will emit an electromagnetic pulse with a time duration of the order of nano seconds through a process known as the Askaryan effect. It has been shown that in an observing window around 150 MHz there is a maximum chance for detecting this radiation with radio telescopes commonly used in astronomy. In 50 hours of observation time with the Westerbork Synthesis Radio Telescope array we have set a new limit on the flux of neutrinos, summed over all flavors, with energies in excess of $4\times10^{22}$ eV., Comment: Submitted to Phys. Rev. Lett
Published: 2009
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18. Status report of the NuMoon experiment

Author: Scholten, O., Buitink, S., Bacelar, J., Braun, R., de Bruyn, A. G., Falcke, H., Singh, K., Stappers, B., Strom, R. G., and Yahyaoui, R. al
Subjects: Astrophysics
Abstract: We show that at wavelengths comparable to the length of the shower produced by an Ultra-High Energy cosmic ray or neutrino, radio signals are an extremely efficient way to detect these particles. First results are presented of an analysis of 20 hours of observation data for NuMoon project using the Westerbork Synthesis Radio Telescope to search for short radio pulses from the Moon. A limit on the neutrino flux is set that is a factor four better than the current one (based on FORTE)., Comment: Contribution to the Arena 2008 conference, Rome, 25-27 June 2008
Published: 2008

19. Testing the inverse-Compton catastrophe scenario in the intra-day variable blazar S5 0716+71, III. Rapid and correlated flux density variability from radio to sub-mm bands

Author: Fuhrmann, L., Krichbaum, T. P., Witzel, A., Kraus, A., Britzen, S., Bernhart, S., Impellizzeri, C. M. V., Agudo, I., Klare, J., Sohn, B. W., Angelakis, E., Bach, U., Gab'anyi, K. 'E., K"ording, E., Pagels, A., Zensus, J. A., Wagner, S. J., Ostorero, L., Ungerechts, H., Grewing, M., Tornikoski, M., Apponi, A. J., Vila-Vilar'o, B., Ziurys, L. M., and Strom, R. G.
Subjects: Astrophysics
Abstract: The BL Lac object S5 0716+71 was observed in a global multi-frequency campaign to search for rapid and correlated flux density variability and signatures of an inverse-Compton (IC) catastrophe during the states of extreme apparent brightness temperatures. The observing campaign involved simultaneous monitoring at radio to IR/optical wavelengths centered around a 500-ks INTEGRAL pointing (November 10-17, 2003). We present the combined analysis and results of the cm- to sub-mm observations including a detailed study of the inter- to intra-day variability and spectral characteristics of 0716+714. We further constrain the variability brightness temperatures (T_B) and Doppler factors (delta) comparing the radio-bands with the hard X-ray emission (3-200 keV). 0716+714 was in an exceptionally high state (outburst) and different (slower) phase of short-term variability. The flux density variability in the cm- to mm-bands is dominated by a correlated, ~4 day time scale amplitude increase of up to ~35% systematically more pronounced towards shorter wavelengths. This contradicts expectations from standard interstellar scintillation (ISS) and suggests a source-intrinsic origin of the variability. The derived lower limits to T_B exceed the 10^12 K IC-limit by up to 3-4 orders of magnitude. Assuming relativistic boosting, we obtain robust and self-consistent lower limits of delta >= 5-33, in good agreement with delta_VLBI obtained from VLBI studies and the IC-Doppler factors delta_IC > 14-16 obtained from the INTEGRAL data. Since a strong contribution from ISS can be excluded and a simultaneous IC catastrophe was not observed, we conclude that relativistic Doppler boosting naturally explains the apparent violation of the theoretical limits within standard synchrotron-self-Compton (SSC) jet models of AGN., Comment: 20 pages, accepted for publication in A&A
Published: 2008
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20. The NuMoon experiment: first results

Author: Buitink, S., Bacelar, J., Braun, R., de Bruyn, G., Falcke, H., Scholten, O., Singh, K., Stappers, B., Strom, R., and Yahyaoui, R. al
Subjects: Astrophysics
Abstract: The NuMoon project uses the Westerbork Synthesis Radio Telescope to search for short radio pulses from the Moon. These pulses are created when an ultra high energy cosmic ray or neutrino initiates a particle cascade inside the Moon's regolith. The cascade has a negative charge excess and moves faster than the local speed of light, which causes coherent Cherenkov radiation to be emitted. With 100 hours of data, a limit on the neutrino flux can be set that is an order of magnitude better than the current one (based on FORTE). We present an analysis of the first 10 hours of data., Comment: 8 pages, 8 figures, proceedings of XXth rencontres de Blois, 2008
Published: 2008

21. GRB 080319B: A Naked-Eye Stellar Blast from the Distant Universe

Author: Racusin, J. L., Karpov, S. V., Sokolowski, M., Granot, J., Wu, X. F., Pal'shin, V., Covino, S., van der Horst, A. J., Oates, S. R., Schady, P., Smith, R. J., Cummings, J., Starling, R. L. C., Piotrowski, L. W., Zhang, B., Evans, P. A., Holland, S. T., Malek, K., Page, M. T., Vetere, L., Margutti, R., Guidorzi, C., Kamble, A., Curran, P. A., Beardmore, A., Kouveliotou, C., Mankiewicz, L., Melandri, A., O'Brien, P. T., Page, K. L., Piran, T., Tanvir, N. R., Wrochna, G., Aptekar, R. L., Bartolini, C., Barthelmy, S., Beskin, G. M., Bondar, S., Campana, S., Cucchiara, A., Cwiok, M., D'Avanzo, P., D'Elia, V., Della Valle, M., Dominik, W., Falcone, A., Fiore, F., Fox, D. B., Frederiks, D. D., Fruchter, A. S., Fugazza, D., Garrett, M., Gehrels, N., Golenetskii, S., Gomboc, A., Greco, G., Guarnieri, A., Immler, S., Kasprowicz, G., Levan, A. J., Mazets, E. P., Molinari, E., Moretti, A., Nawrocki, K., Oleynik, P. P., Osborne, J. P., Pagani, C., Paragi, Z., Perri, M., Piccioni, A., Ramirez-Ruiz, E., Roming, P. W. A., Steele, I. A., Strom, R. G., Testa, V., Tosti, G., Ulanov, M. V., Wiersema, K., Wijers, R. A. M. J., Zarnecki, A. F., Zerbi, F., Meszaros, P., Chincarini, G., and Burrows, D. N.
Subjects: Astrophysics
Abstract: Long duration gamma-ray bursts (GRBs) release copious amounts of energy across the entire electromagnetic spectrum, and so provide a window into the process of black hole formation from the collapse of a massive star. Over the last forty years, our understanding of the GRB phenomenon has progressed dramatically; nevertheless, fortuitous circumstances occasionally arise that provide access to a regime not yet probed. GRB 080319B presented such an opportunity, with extraordinarily bright prompt optical emission that peaked at a visual magnitude of 5.3, making it briefly visible with the naked eye. It was captured in exquisite detail by wide-field telescopes, imaging the burst location from before the time of the explosion. The combination of these unique optical data with simultaneous gamma-ray observations provides powerful diagnostics of the detailed physics of this explosion within seconds of its formation. Here we show that the prompt optical and gamma-ray emissions from this event likely arise from different spectral components within the same physical region located at a large distance from the source, implying an extremely relativistic outflow. The chromatic behaviour of the broadband afterglow is consistent with viewing the GRB down the very narrow inner core of a two-component jet that is expanding into a wind-like environment consistent with the massive star origin of long GRBs. These circumstances can explain the extreme properties of this GRB., Comment: 43 pages, 18 figures, 3 tables, submitted to Nature May 11, 2008
Published: 2008
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22. GRB 030329: three years of radio afterglow monitoring

Author: van der Horst, A. J., Kamble, A., Wijers, R. A. M. J., Resmi, L., Bhattacharya, D., Rol, E., Strom, R., Kouveliotou, C., Oosterloo, T., and Ishwara-Chandra, C. H.
Subjects: Astrophysics
Abstract: Radio observations of gamma-ray burst (GRB) afterglows are essential for our understanding of the physics of relativistic blast waves, as they enable us to follow the evolution of GRB explosions much longer than the afterglows in any other wave band. We have performed a three-year monitoring campaign of GRB 030329 with the Westerbork Synthesis Radio Telescopes (WSRT) and the Giant Metrewave Radio Telescope (GMRT). Our observations, combined with observations at other wavelengths, have allowed us to determine the GRB blast wave physical parameters, such as the total burst energy and the ambient medium density, as well as investigate the jet nature of the relativistic outflow. Further, by modeling the late-time radio light curve of GRB 030329, we predict that the Low Frequency Array (LOFAR, 30-240 MHz) will be able to observe afterglows of similar GRBs, and constrain the physics of the blast wave during its non-relativistic phase., Comment: 2 pages, to appear in Nuovo Cimento B, proceedings of the Congress "Swift and GRBs: Unveiling the Relativistic Universe", Venice, June 2006
Published: 2007
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23. GRB 030329: 3 years of radio afterglow monitoring

Author: van der Horst, A. J., Kamble, A., Wijers, R. A. M. J., Resmi, L., Bhattacharya, D., Rol, E., Strom, R., Kouveliotou, C., Oosterloo, T., and Ishwara-Chandra, C. H.
Subjects: Astrophysics
Abstract: Radio observations of gamma-ray burst (GRB) afterglows are essential for our understanding of the physics of relativistic blast waves, as they enable us to follow the evolution of GRB explosions much longer than the afterglows in any other wave band. We have performed a three-year monitoring campaign of GRB 030329 with the Westerbork Synthesis Radio Telescopes (WSRT) and the Giant Metrewave Radio Telescope (GMRT). Our observations, combined with observations at other wavelengths, have allowed us to determine the GRB blast wave physical parameters, such as the total burst energy and the ambient medium density, as well as investigate the jet nature of the relativistic outflow. Further, by modeling the late-time radio light curve of GRB 030329, we predict that the Low-Frequency Array (LOFAR, 30-240 MHz) will be able to observe afterglows of similar GRBs, and constrain the physics of the blast wave during its non-relativistic phase., Comment: 5 pages, 2 figures, Phil. Trans. R. Soc. A, vol.365, p.1241, proceedings of the Royal Society Scientific Discussion Meeting, London, September 2006
Published: 2007
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24. Detailed study of the GRB 030329 radio afterglow deep into the non-relativistic phase

Author: van der Horst, A. J., Kamble, A., Resmi, L., Wijers, R. A. M. J., Bhattacharya, D., Scheers, B., Rol, E., Strom, R., Kouveliotou, C., Oosterloo, T., and Ishwara-Chandra, C. H.
Subjects: Astrophysics
Abstract: We explore the physics behind one of the brightest radio afterglows ever, GRB 030329, at late times when the jet is non-relativistic. We determine the physical parameters of the blast wave and its surroundings, in particular the index of the electron energy distribution, the energy of the blast wave, and the density (structure) of the circumburst medium. We then compare our results with those from image size measurements. We observed the GRB 030329 radio afterglow with the Westerbork Synthesis Radio Telescope and the Giant Metrewave Radio Telescope at frequencies from 325 MHz to 8.4 GHz, spanning a time range of 268-1128 days after the burst. We modeled all the available radio data and derived the physical parameters. The index of the electron energy distribution is p=2.1, the circumburst medium is homogeneous, and the transition to the non-relativistic phase happens at t_NR ~ 80 days. The energy of the blast wave and density of the surrounding medium are comparable to previous findings. Our findings indicate that the blast wave is roughly spherical at t_NR, and they agree with the implications from the VLBI studies of image size evolution. It is not clear from the presented dataset whether we have seen emission from the counter jet or not. We predict that the Low Frequency Array will be able to observe the afterglow of GRB 030329 and many other radio afterglows, constraining the physics of the blast wave during its non-relativistic phase even further., Comment: 9 pages, 2 figures; accepted for publication in Astronomy & Astrophysics after minor revisions; small changes in GMRT fluxes at 1280 MHz
Published: 2007
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25. Detecting UHE Cosmics & Neutrinos off the Moon; an Optimal Radio Window

Author: Scholten, O., Bacelar, J., Braun, R., de Bruyn, A. G., Falcke, H., Stappers, B., and Strom, R. G.
Subjects: Astrophysics
Abstract: We show that at wavelengths comparable to the length of the shower produced by an Ultra-High Energy cosmic ray or neutrino, radio signals are an extremely efficient way to detect these particles. Through an example it is shown that this new approach offers, for the first time, the realistic possibility of measuring UHE neutrino fluxes below the Waxman-Bahcall limit. It is shown that in only one month of observing with the upcoming LOFAR radio telescope, cosmic-ray events can be measured beyond the GZK-limit, at a sensitivity level of two orders of magnitude below the extrapolated values., Comment: ARENA 2006 proceedings, to be published in Journal of Physics (Conference Series (JPCS))
Published: 2006

26. Prompt and Afterglow Emission Properties of Gamma-Ray Bursts with Spectroscopically Identified Supernovae

Author: Kaneko, Y., Ramirez-Ruiz, E., Granot, J., Kouveliotou, C., Woosley, S. E., Patel, S. K., Rol, E., Zand, J. J. M. in't, van der Horst, A. J., Wijers, R. A. M. J., and Strom, R.
Subjects: Astrophysics
Abstract: We present a detailed spectral analysis of the prompt and afterglow emission of four nearby long-soft gamma-ray bursts (GRBs 980425, 030329, 031203, and 060218) that were spectroscopically found to be associated with type Ic supernovae, and compare them to the general GRB population. For each event, we investigate the spectral and luminosity evolution, and estimate the total energy budget based upon broadband observations. The observational inventory for these events has become rich enough to allow estimates of their energy content in relativistic and sub-relativistic form. The result is a global portrait of the effects of the physical processes responsible for producing long-soft GRBs. In particular, we find that the values of the energy released in mildly relativistic outflows appears to have a significantly smaller scatter than those found in highly relativistic ejecta. This is consistent with a picture in which the energy released inside the progenitor star is roughly standard, while the fraction of that energy that ends up in highly relativistic ejecta outside the star can vary dramatically between different events., Comment: 55 pages including 23 figures and 8 tables. Accepted for publication in ApJ. Replaced with the accepted version
Published: 2006
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27. Optimal Radio Window for the Detection of Ultra-High-Energy Cosmic Rays and Neutrinos off the Moon

Author: Scholten, O., Bacelar, J., Braun, R., de Bruyn, A. G., Falcke, H., Stappers, B., and Strom, R. G.
Subjects: Astrophysics
Abstract: When high-energy cosmic rays impinge on a dense dielectric medium, radio waves are produced through the Askaryan effect. We show that at wavelengths comparable to the length of the shower produced by an Ultra-High Energy cosmic ray or neutrino, radio signals are an extremely efficient way to detect these particles. Through an example it is shown that this new approach offers, for the first time, the realistic possibility of measuring UHE neutrino fluxes below the Waxman-Bahcall limit. It is shown that in only one month of observing with the upcoming LOFAR radio telescope, cosmic-ray events can be measured beyond the GZK-limit, at a sensitivity level of two orders of magnitude below the extrapolated values., Comment: Submitted to Astroparticle Physics
Published: 2005
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28. The radio afterglow of GRB 030329 at centimeter wavelengths: evidence for a structured jet or non-relativistic expansion

Author: van der Horst, A. J., Rol, E., Wijers, R. A. M. J., Strom, R., Kaper, L., and Kouveliotou, C.
Subjects: Astrophysics
Abstract: We present our centimeter wavelength (1.4, 2.3 and 4.8 GHz) light curves of the afterglow of GRB 030329, which were obtained with the Westerbork Synthesis Radio Telescope. Modeling the data according to a collimated afterglow results in a jet-break time of 10 days. This is in accordance with earlier results obtained at higher radio frequencies. However, with respect to the afterglow model, some additional flux at the lower frequencies is present when these light curves reach their maximum after 40-80 days. We show that this additional flux can be modeled with two or more components with progressively later jet breaks. From these results we infer that the jet is in fact a structured or a layered jet, where the ejecta with lower Lorentz factors produce additional flux that becomes visible at late times in the lowest frequency bands. We show that a transition to non-relativistic expansion of the fireball at late times can also account for the observed flux excess, except for the lowest frequency (1.4 GHz) data., Comment: 7 pages, 2 figures, accepted for publication in ApJ
Published: 2005
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29. What is the primary beam response of an interferometer with unequal elements?

Author: Strom, R. G.
Subjects: Astrophysics
Abstract: The EVN stations encompass elements with a range of diameters, even including an interferometer (the Westerbork Telescope, with up to 14 elements used together as a tied array). In combination, the various station pairs will each produce their own primary beam envelopes, with which the interferometer pattern is modulated. People sometimes forget that in the case of unequal elements, this combined primary beam envelope is different from the beam of each element separately. The reason for this is reviewed, the results for a number of station pairs are summarized, and some of the practical consequences are discussed. The increased interest in wide-field applications, as illustrated by several recent results, underlines the need for a proper determination of the interferometer beam envelope., Comment: 2 pages. no figures. Proceedings of the 7th European VLBI Network Symposium held in Toledo, Spain on October 12-15, 2004. Editors: R. Bachiller, F. Colomer, J.-F. Desmurs, P. de Vicente (Observatorio Astronomico Nacional), p. 273-274. Needs evn2004.cls
Published: 2004

30. Proper Motion Measurements of Pulsar B1951+32 in the Supernova Remnant CTB 80

Author: Migliazzo, J. M., Gaensler, B. M., Backer, D. C., Stappers, B. W., van der Swaluw, E., and Strom, R. G.
Subjects: Astrophysics
Abstract: Using the Very Large Array and the Pie Town antenna, we have measured the position of the radio pulsar B1951+32 relative to nearby background radio sources at four epochs between 1989 and 2000. These data show a clear motion for the pulsar of (25 +/- 4) milliarcsec/yr at a position angle (252 +/- 7) degrees (north through east), corresponding to a transverse velocity (240 +/- 40) km/s for a distance to the source of 2 kpc. The measured direction of motion confirms that the pulsar is moving away from the center of its associated supernova remnant, the first time that such a result has been demonstrated. Independent of assumptions made about the pulsar birth-place, we show that the measured proper motion implies an age for the pulsar of (64 +/- 18) kyr, somewhat less than its characteristic age of 107 kyr. This discrepancy can be explained if the initial spin period of the pulsar was (27 +/- 6) ms., Comment: 5 pages, 2 embedded EPS figures. Accepted to ApJ Letters
Published: 2002
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31. Radio Emission from the Composite Supernova Remnant G326.3-1.8 (MSH15-56)

Author: Dickel, J., Milne, D., and Strom, R.
Subjects: Astrophysics
Abstract: High resolution radio observations of the composite supernova remnant (SNR) G326.3-1.8 or MSH 15-56 with the Australia Telescope Compact Array show details of both the shell and the bright plerion which is offset about 1/3 of the distance from the center of the SNR to the shell. The shell appears to be composed of thin filaments, typical of older shell SNRs. The central part of the elongated plerion is composed of a bundle of parallel ridges which bulge out at the ends and form a distinct ring structure on the northwestern end. The magnetic field with a strength of order 45 microGauss, is directed along the axis of the ridges but circles around the northwestern ring. This plerion is large and bright in the radio but is not detected in x-ray or optical wavelengths. There is, however, a faint hard x-ray feature closer to the shell outside the plerion. Perhaps if the supernova explosion left a rapidly moving magnetar with large energy input but initially rapid decay of both relativistic particles and magnetic field, the observed differences with wavelength could be explained., Comment: 15 pages, 10 figures, accepted by ApJ
Published: 2000
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32. Spectral Energy Distributions and Light Curves of GRB 990123 and its Afterglow

Author: Galama, T. J., Briggs, M. S., Wijers, R. A. M. J., Vreeswijk, P. M., Rol, E., Band, D., van Paradijs, J., Kouveliotou, C., Preece, R. D., Bremer, M., Smith, I. A., Tilanus, R. P. J., de Bruyn, A. G., Strom, R. G., Pooley, G., Castro-Tirado, A. J., Tanvir, N., Robinson, C., Hurley, K., Heise, J., Telting, J., Rutten, R. G. M., Packham, C., Swaters, R., Davies, J. K., Fassia, A., Green, S. F., Foster, M. J., Sagar, R., Pandey, A. K., Nilakshi, Yadav, R. K. S., Ofek, E. O., Leibowitz, E., Ibbetson, P., Rhoads, J., Falco, E., Petry, C., Impey, C., Geballe, T. R., and Bhattacharya, D.
Subjects: Astrophysics
Abstract: Gamma-ray bursts (GRBs) are thought to result from the interaction of an extremely relativistic outflow interacting with a small amount of material surrounding the site of the explosion. Multi-wavelength observations covering the gamma-ray to radio wavebands allow investigations of this `fireball' model. On 23 January 1999 optical emission was detected while the gamma-ray burst was still underway. Here we report the results of gamma-ray, optical/infra-red, sub-mm, mm and radio observations of this burst and its afterglow, which indicate that the prompt and afterglow emissions from GRB 990123 are associated with three distinct regions in the fireball. The afterglow one day after the burst has a much lower peak frequency than those of previous bursts; this explains the short-lived nature of the radio emission, which is not expected to reappear. We suggest that such differences reflect variations in the magnetic-field strengths in the afterglow emitting regions., Comment: Accepted for publication in Nature. Under press embargo
Published: 1999

33. Microfinance Financial and Social Performance: An Introduction

Author: Mersland, Roy, Strøm, R. Øystein, Mersland, Roy, editor, and Strøm, R. Øystein, editor
Published: 2014
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34. Measuring Microfinance Performance

Author: Mersland, Roy, Strøm, R. Øystein, Mersland, Roy, editor, and Strøm, R. Øystein, editor
Published: 2014
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35. Discovery of the peculiar supernova 1998bw in the error box of GRB980425

Author: Galama, T. J., Vreeswijk, P. M., van Paradijs, J., Kouveliotou, C., Augusteijn, T., Hainaut, O. R., Patat, F., Boehnhardt, H., Brewer, J., Doublier, V., Gonzalez, J. -F., Lidman, C., Leibundgut, B., Heise, J., Zand, J. in 't, Groot, P. J., Strom, R. G., Mazzali, P., Iwamoto, K., Nomoto, K., Umeda, H., Nakamura, T., Koshut, T., Kippen, M., Robinson, C., de Wildt, P., Wijers, R. A. M. J., Tanvir, N., Greiner, J., Pian, E., Palazzi, E., Frontera, F., Masetti, N., Nicastro, L., Malozzi, E., Feroci, M., Costa, E., Piro, L., Peterson, B. A., Tinney, C., Boyle, B., Cannon, R., Stathakis, R., Begam, M. C., and Ianna, P.
Subjects: Astrophysics
Abstract: The discovery of X-ray, optical and radio afterglows of gamma-ray bursts (GRBs) and the measurements of the distances to some of them have established that these events come from Gpc distances and are the most powerful photon emitters known in the Universe, with peak luminosities up to 10^52 erg/s. We here report the discovery of an optical transient, in the BeppoSAX Wide Field Camera error box of GRB980425, which occurred within about a day of the gamma-ray burst. Its optical light curve, spectrum and location in a spiral arm of the galaxy ESO 184-G82, at a redshift z = 0.0085, show that the transient is a very luminous type Ic supernova, SN1998bw. The peculiar nature of SN1998bw is emphasized by its extraordinary radio properties which require that the radio emitter expand at relativistical speed. Since SN1998bw is very different from all previously observed afterglows of GRBs, our discovery raises the possibility that very different mechanisms may give rise to GRBs, which differ little in their gamma-ray properties., Comment: Under press embargo at Nature (submitted June 10, 1998)
Published: 1998
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36. The radio to X-ray spectrum of GRB 970508 on May 21.0 UT

Author: Galama, T. J., Wijers, R. A. M. J., Bremer, M., Groot, P. J., Strom, R. G., Kouveliotou, C., and van Paradijs, J.
Subjects: Astrophysics
Abstract: We have reconstructed the spectrum of the afterglow of GRB 970508, on May 21.0 UT (12.1 days after the GRB), on the basis of observations spanning the X-ray to radio range. The low-frequency power law index of the spectrum, $\alpha=0.44\pm0.07$ ($F_\nu\propto\nu^\alpha$), is in agreement with the expected value $\alpha=1/3$ for optically thin synchrotron radiation. The 1.4 GHz emission is self-absorbed. We infer constraints on the break frequecies $\nu_{c}$ and $\nu_{m}$ on May 21.0 UT from a spectral transition from $F_{\nu} \sim \nu^{-0.6}$ to $F_{\nu} \sim \nu^{-1.1}$ in the optical passband around 1.4 days. A model of an adiabatically expanding blast wave, emitting synchrotron radiation, in which a significant fraction of the electrons cool rapidly provides a successful and consistent description of the afterglow observations over nine decades in frequency, ranging in time from trigger until several months later., Comment: Paper II. Accepted for publication in the Astrophysical Journal Letters
Published: 1998
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37. The 1.4 GHz light curve of GRB 970508

Author: Galama, T. J., Wijers, R. A. M. J., Bremer, M., Groot, P. J., Strom, R. G., de Bruyn, A. G., Kouveliotou, C., Robinson, C. R., and van Paradijs, J.
Subjects: Astrophysics
Abstract: We report on Westerbork 1.4 GHz radio observations of the radio counterpart to $\gamma$-ray burst GRB~970508, between 0.80 and 138 days after this event. The 1.4 GHz light curve shows a transition from optically thick to thin emission between 39 and 54 days after the event. We derive the slope $p$ of the spectrum of injected electrons ($dN/d\gamma_{e}\propto\gamma_{e}^{-p}$) in two independent ways which yield values very close to $p=2.2$. This is in agreement with a relativistic dynamically near-adiabatic blast wave model whose emission is dominated by synchrotron radiation and in which a significant fraction of the electrons cool fast., Comment: Paper I. Accepted for publication in the Astrophysical Journal Letters
Published: 1998
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38. Optical follow-up of GRB 970508

Author: Galama, T. J., Groot, P. J., van Paradijs, J., Kouveliotou, C., Strom, R. G., Wijers, R. A. M. J., Tanvir, N., Bloom, J., Centurion, M., Telting, J., Rutten, R. G. M., Smith, P., Mackey, C., Smartt, S., Benn, C., Heise, J., and Zand, J. in 't
Subjects: Astrophysics
Abstract: We report on the results of optical follow-up observations of the counterpart of GRB 970508, starting 7 hours after the event. Multi-color U, B, V, R$_{c}$ and I$_{c}$ band observations were obtained during the first three consecutive nights. The counterpart was monitored regularly in R$_{c}$ until $\sim$ 4 months after the burst. The light curve after the maximum follows a decline that can be fitted with a power law with exponent $\alpha$ = --1.141 $\pm$ 0.014. Deviations from a smooth power law decay are moderate (r.m.s. = 0.15 magnitude). We find no flattening of the light curve at late times. The optical afterglow fluence is a significant fraction, $\sim$ 5%, of the GRB fluence. The optical energy distribution can be well represented by a power law, the slope of which changed at the time of the maximum (the spectrum became redder)., Comment: Accepted for publication in the Astrophysical Journal Letters, 10 pages including 3 figures
Published: 1998
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39. Radio and Optical Follow-up Observations and Improved IPN Position of GRB 970111

Author: Galama, T. J., Groot, P. J., Strom, R. G., van Paradijs, J., Hurley, K., Kouveliotou, C., Fishman, G. J., Meegan, C. A., Heise, J., Zand, J. J. M. in 't, de Bruyn, A. G., Hanlon, L. O., Bennett, K., Telting, J. H., and Rutten, R. G. M.
Subjects: Astrophysics
Abstract: We report on Westerbork 840 MHz, 1.4 and 5 GHz radio observations of the improved IPN-WFC error box of the gamma-ray burst GRB 970111, between 26.4 hours and 120 days after the event onset. In the ~ 13 sq arcmin area defined by the IPN (BATSE and Ulysses) annulus and the published refined BeppoSAX Wide Field Camera error box we detected no steady sources brighter than 0.56 mJy (4 sigma), and no varying radio emission, down to 1.0 mJy (4 sigma). We also report on B, V, R and I band observations of the error box with the 4.2 m William Herschel Telescope at La Palma., Comment: 19 pages including 4 figures, Latex, accepted for APJL
Published: 1997
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40. Gender discrimination before mandated quotas? Evidence from Norway: 1989–2002

Author: Øystein Strøm, R.
Published: 2015
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41. Enhanced Optical Emission during Crab Giant Radio Pulses

Author: Shearer, A., Stappers, B., O'Connor, P., Golden, A., Strom, R., Redfern, M., and Ryan, O.
Published: 2003

42. Bovine lactoferrin and its tryptic peptides: Antibacterial activity against different species

Author: Lizzi, A. R., Carnicelli, V., Clarkson, M. M., Nazzicone, C., Segatore, B., Celenza, G., Aschi, M., Dolo, V., Strom, R., and Amicosante, G.
Published: 2016
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43. The impact of entrepreneur-CEOs in microfinance institutions: a global survey

Author: Randoy, Trond, Strom, R. Oystein, and Mersland, Roy
Subjects: Microfinance -- Surveys, Chief executive officers -- Surveys, Entrepreneurship -- Surveys, Business enterprises -- Growth -- Surveys -- Finance, Businesspeople -- Surveys, Company growth, Company financing, Business, general, Business
Abstract: Microfinance is a global high-growth industry, in which entrepreneurship is prevalent and substantial. Based on the theoretical argument that microfinance entrepreneur-chief executive officers (CEOs) are 'motivated agents' with a unique [...]
Published: 2015
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44. Radio Spectral Monitoring Campaign at Proposed SKA Sites in China

Author: Peng, Bo, Li, Jianbin, Piao, Tingyi, Sun, Jianmin, and Strom, R. G.
Published: 2008
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45. Personal digital assistants and pagers : a model for parent collaboration in school discipline.

Author: Strom, P. S. and Strom, R. D.
Published: 2002

46. Microfinance Mission Drift?

Author: Mersland, Roy and Strøm, R. Øystein
Published: 2010
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47. S-Adenosylhomocysteine Hydrolase Activity in Erythrocytes from HIV-Infected Patients

Author: Bozzi, A., Leonardi, F., De Rinaldis, M. L., Ferrazzi, M., Strom, R., Harkness, R. Angus, editor, Elion, Gertrude B., editor, and Zöllner, Nepomuk, editor
Published: 1991
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48. Performance and governance in microfinance institutions

Author: Mersland, Roy and Øystein Strøm, R.
Published: 2009
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49. Voyager 2 at Neptune: Imaging Science Results

Author: Smith, B. A., Soderblom, L. A., Banfield, D., Barnet, C., Basilevksy, A. T., Beebe, R. F., Bollinger, K., Boyce, J. M., Brahic, A., Briggs, G. A., Brown, R. H., Chyba, C., Collins, S. A., Colvin, T., Cook, A. F., Crisp, D., Croft, S. K., Cruikshank, D., Cuzzi, J. N., Danielson, G. E., Davies, M. E., De Jong, E., Dones, L., Godfrey, D., Goguen, J., Grenier, I., Haemmerle, V. R., Hammel, H., Hansen, C. J., Helfenstein, C. P., Howell, C., Hunt, G. E., Ingersoll, A. P., Johnson, T. V., Kargel, J., Kirk, R., Kuehn, D. I., Limaye, S., Masursky, H., McEwen, A., Morrison, D., Owen, T., Owen, W., Pollack, J. B., Porco, C. C., Rages, K., Rogers, P., Rudy, D., Sagan, C., Schwartz, J., Shoemaker, E. M., Showalter, M., Sicardy, B., Simonelli, D., Spencer, J., Sromovsky, L. A., Stoker, C., Strom, R. G., Suomi, V. E., Synott, S. P., Terrile, R. J., Thomas, P., Thompson, W. R., Verbiscer, A., and Veverka, J.
Published: 1989

50. Voyager 2 in the Uranian System: Imaging Science Results

Author: Smith, B. A., Soderblom, L. A., Beebe, R., Bliss, D., Boyce, J. M., Brahic, A., Briggs, G. A., Brown, R. H., Collins, S. A., Cook, A. F., Croft, S. K., Cuzzi, J. N., Danielson, G. E., Davies, M. E., Dowling, T. E., Godfrey, D., Hansen, C. J., Harris, C., Hunt, G. E., Ingersoll, A. P., Johnson, T. V., Krauss, R. J., Masursky, H., Morrison, D., Owen, T., Plescia, J. B., Pollack, J. B., Porco, C. C., Rages, K., Sagan, C., Shoemaker, E. M., Sromovsky, L. A., Stoker, C., Strom, R. G., Suomi, V. E., Synnott, S. P., Terrile, R. J., Thomas, P., Thompson, W. R., and Veverka, J.
Published: 1986

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