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976 results on '"Litvak, M"'

4. The Second Catalog of Interplanetary Network Localizations of Konus Short Duration Gamma-Ray Bursts

Author

Svinkin, D., Hurley, K., Ridnaia, A., Lysenko, A., Frederiks, D., Golenetskii, S., Tsvetkova, A., Ulanov, M., Kokomov, A., Cline, T. L., Mitrofanov, I., Golovin, D., Kozyrev, A., Litvak, M., Sanin, A., Goldstein, A., Briggs, M. S., Wilson-Hodge, C., Burns, E., von Kienlin, A., Zhang, X. -L., Rau, A., Savchenko, V., Bozzo, E., Ferrigno, C., Barthelmy, S., Cummings, J., Krimm, H., Palmer, D. M., Tohuvavohu, A., Yamaoka, K., Ohno, M., Fukazawa, Y., Hanabata, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Boynton, W., Fellows, C. W., Harshman, K. P., Enos, H., Starr, R., Goldsten, J., Gold, R., Ursi, A., Tavani, M., Bulgarelli, A., Casentini, C., Del Monte, E., Evangelista, Y., Galli, M., Longo, F., Marisaldi, M., Parmiggiani, N., Pittori, C., Romani, M., Verrecchia, F., Smith, D. M., Hajdas, W., Xiao, S., Cai, C., Yi, Q. B., Zhang, Y. Q., Xiong, S. L., Li, X. B., Huang, Y., Li, C. K., Zhang, S. N., Song, L. M., Liu, C. Z., Li, X. Q., Peng, W. X., and Martinez-Castellanos, I.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the catalog of Interplanetary Network (IPN) localizations for 199 short-duration gamma-ray bursts (sGRBs) detected by the Konus-Wind (KW) experiment between 2011 January 1 and 2021 August 31, which extends the initial sample of IPN localized KW sGRBs (arXiv:1301.3740) to 495 events. We present the most comprehensive IPN localization data on these events, including probability sky maps in HEALPix format., Comment: Published in ApJS

Published
2022
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6. A bright gamma-ray flare interpreted as a giant magnetar flare in NGC 253

Author

Svinkin, D., Frederiks, D., Hurley, K., Aptekar, R., Golenetskii, S., Lysenko, A., Ridnaia, A. V., Tsvetkova, A., Ulanov, M., Cline, T. L., Mitrofanov, I., Golovin, D., Kozyrev, A., Litvak, M., Sanin, A., Goldstein, A., Briggs, M. S., Wilson-Hodge, C., von Kienlin, A., Zhang, X. -L., Rau, A., Savchenko, V., Bozzo, E., Ferrigno, C., Ubertini, P., Bazzano, A., Rodi, J. C., Barthelmy, S., Cummings, J., Krimm, H., Palmer, D. M., Boynton, W., Fellows, C. W., Harshman, K. P., Enos, H., and Starr, R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Magnetars are young, highly magnetized neutron stars that produce extremely rare giant flares of gamma-rays, the most luminous astrophysical phenomena in our Galaxy. The detection of these flares from outside the Local Group of galaxies has been predicted, with just two candidates so far. Here we report on the extremely bright gamma-ray flare GRB 200415A of April 15, 2020, which we localize, using the Interplanetary Network, to a tiny (20 sq. arcmin) area on the celestial sphere, that overlaps the central region of the Sculptor galaxy at 3.5 Mpc from the Milky Way. From the Konus-Wind detections, we find a striking similarity between GRB 200415A and GRB 051103, the even more energetic flare that presumably originated from the M81/M82 group of galaxies at nearly the same distance (3.6 Mpc). Both bursts display a sharp, millisecond-scale, hard-spectrum initial pulse, followed by an approximately 0.2 s long steadily fading and softening tail. Apart from the huge initial pulses of magnetar giant flares, no astrophysical signal with this combination of temporal and spectral properties and implied energy has been reported previously. At the inferred distances, the energy released in both flares is on par with that of the December 27, 2004 superflare from the Galactic magnetar SGR 1806-20, but with a higher peak luminosity. Taken all together, this makes GRB 200415A and its twin GRB 051103 the most significant candidates for extragalactic magnetar giant flares, both a factor of five more luminous than the brightest Galactic magnetar flare observed previously, thus providing an important step towards a better understanding of this fascinating phenomenon., Comment: Preprint version of Nature paper

Published
2021
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7. Representativeness of Eddy-Covariance flux footprints for areas surrounding AmeriFlux sites

Author

Chu, H, Luo, X, Ouyang, Z, Chan, WS, Dengel, S, Biraud, SC, Torn, MS, Metzger, S, Kumar, J, Arain, MA, Arkebauer, TJ, Baldocchi, D, Bernacchi, C, Billesbach, D, Black, TA, Blanken, PD, Bohrer, G, Bracho, R, Brown, S, Brunsell, NA, Chen, J, Chen, X, Clark, K, Desai, AR, Duman, T, Durden, D, Fares, S, Forbrich, I, Gamon, JA, Gough, CM, Griffis, T, Helbig, M, Hollinger, D, Humphreys, E, Ikawa, H, Iwata, H, Ju, Y, Knowles, JF, Knox, SH, Kobayashi, H, Kolb, T, Law, B, Lee, X, Litvak, M, Liu, H, Munger, JW, Noormets, A, Novick, K, Oberbauer, SF, Oechel, W, Oikawa, P, Papuga, SA, Pendall, E, Prajapati, P, Prueger, J, Quinton, WL, Richardson, AD, Russell, ES, Scott, RL, Starr, G, Staebler, R, Stoy, PC, Stuart-Haëntjens, E, Sonnentag, O, Sullivan, RC, Suyker, A, Ueyama, M, Vargas, R, Wood, JD, and Zona, D

Subjects
Flux footprint, Spatial representativeness, Landsat EVI, Land cover, Sensor location bias, Model-data benchmarking, Meteorology & Atmospheric Sciences, Earth Sciences, Biological Sciences, Agricultural and Veterinary Sciences
Abstract

Large datasets of greenhouse gas and energy surface-atmosphere fluxes measured with the eddy-covariance technique (e.g., FLUXNET2015, AmeriFlux BASE) are widely used to benchmark models and remote-sensing products. This study addresses one of the major challenges facing model-data integration: To what spatial extent do flux measurements taken at individual eddy-covariance sites reflect model- or satellite-based grid cells? We evaluate flux footprints—the temporally dynamic source areas that contribute to measured fluxes—and the representativeness of these footprints for target areas (e.g., within 250–3000 m radii around flux towers) that are often used in flux-data synthesis and modeling studies. We examine the land-cover composition and vegetation characteristics, represented here by the Enhanced Vegetation Index (EVI), in the flux footprints and target areas across 214 AmeriFlux sites, and evaluate potential biases as a consequence of the footprint-to-target-area mismatch. Monthly 80% footprint climatologies vary across sites and through time ranging four orders of magnitude from 103 to 107 m2 due to the measurement heights, underlying vegetation- and ground-surface characteristics, wind directions, and turbulent state of the atmosphere. Few eddy-covariance sites are located in a truly homogeneous landscape. Thus, the common model-data integration approaches that use a fixed-extent target area across sites introduce biases on the order of 4%–20% for EVI and 6%–20% for the dominant land cover percentage. These biases are site-specific functions of measurement heights, target area extents, and land-surface characteristics. We advocate that flux datasets need to be used with footprint awareness, especially in research and applications that benchmark against models and data products with explicit spatial information. We propose a simple representativeness index based on our evaluations that can be used as a guide to identify site-periods suitable for specific applications and to provide general guidance for data use.

Published
2021

9. Search for gravitational-wave signals associated with gamma-ray bursts during the second observing run of Advanced LIGO and Advanced Virgo

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Aronson, S. M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baird, J., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Bals, A., Banagiri, S., Barayoga, J. C., Barbieri, C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Benjamin, M. G., Berger, B. K., Bergmann, G., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Biggs, E., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., 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. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chiadini, F., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Cieślar, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D., Colleoni, M., Collette, C. G., Collins, C., Colpi, M., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corezzi, S., Corley, K. R., Cornish, N., Corre, D., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., 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., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., D'Angelo, B., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., DeMarchi, L. M., Demos, N., Dent, T., De Pietri, R., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Díaz, M. C., Dietrich, T., Di Fiore, L., DiFronzo, C., Di Giorgio, C., Di Giovanni, F., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Divakarla, A. K., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Durante, O., Dwyer, S. E., Easter, P. J., Eddolls, G., Edo, T. B., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Errico, L., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fittipaldi, R., Fitz-Axen, M., Fiumara, V., Flaminio, R., Fletcher, M., Floden, E., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Vivanco, Francisco Hernandez, Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fronzè, G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gill, K., Glover, L., Gniesmer, J., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gossan, S. E., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Grimaldi, A., Grimm, S. J., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, Anchal, Gupta, P., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hasskew, R. K., Haster, C. J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hellman, F., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heurs, M., Hild, S., Hinderer, T., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Huang, Y., Hübner, M. T., Huerta, E. A., Huet, D., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, J. D., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kéfélian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khazanov, E. A., Khetan, N., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kovalam, M., Kozak, D. B., Krämer, C., Kringel, V., Krishnendu, N., Królak, A., Krupinski, N., Kuehn, G., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Laghi, D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., 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., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A. K., Leroy, N., Letendre, N., Levin, Y., Li, A., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Llorens-Monteagudo, M., Lo, R. K. L., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., MacInnis, M., Macleod, D. M., Macquet, A., Hernandez, I. Magaña, Magaña-Sandoval, F., Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, V., Martynov, D. V., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., McCann, J. J., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIsaac, C., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Villa, E. Mejuto, Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Messina, F., Metzdorff, R., Meyers, P. M., Meylahn, F., Miani, A., Miao, H., Michel, C., Middleton, H., Milano, L., Miller, A. L., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. J., Moraru, D., Morawski, F., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Muciaccia, F., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukherjee, Subroto, Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Ng, K. Y., Ng, S., Nguyen, C., Nguyen, P., Nichols, D., Nichols, S. A., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., Oganesyan, G., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, H., Panda, P. K., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Payne, E., Pearlstone, B. L., Pechsiri, T. C., Pedersen, A. J., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perego, A., Perez, C. J., Périgois, C., Perreca, A., Petermann, J., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Plastino, W., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Principe, M., Prodi, G. A., Prokhorov, L., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rettegno, P., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riemenschneider, G., Riles, K., Rizzo, M., Robertson, N. A., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, C. A., Rose, D., Rose, K., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salafia, O. S., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Santiago, K. A., Santos, E., Sarin, N., Sassolas, B., Sathyaprakash, B. S., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Sharma, A., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shukla, K., ShyamSundar, S., Siellez, K., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Soni, S., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Spera, M., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Tanner, D. B., Tao, D., Tápai, M., Tapia, A., Tasson, J. D., Taylor, R., Tenorio, R., Terkowski, L., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Töyrä, D., Travasso, F., Traylor, G., Tringali, M. C., Tripathee, A., Trovato, A., Trozzo, L., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tsutsui, T., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., Valentini, M., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van der Schaaf, L., VanHeijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Viceré, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, H., Wang, J. Z., Wang, S., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Weßels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Xu, R., Yamamoto, H., Yancey, C. C., Yang, L., Yang, Y., Yang, Z., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Zadrożny, A. K., Zadrożny, A., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhao, G., Zhou, M., Zhou, Z., Zhu, X. J., Zucker, M. E., Zweizig, J., Collaboration, The LIGO Scientific, Collaboration, the Virgo, Aptekar, R. L., Boynton, W. V., Frederiks, D. D., Golenetskii, S. V., Golovin, D. V., Hurley, K., Kozlova, A. V., Litvak, M. L., Mitrofanov, I. G., Sanin, A. B., Svinkin, D. S., Collaboration, IPN, Carotenuto, Francesco, and Krishnan, Badri

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

We present the results of targeted searches for gravitational-wave transients associated with gamma-ray bursts during the second observing run of Advanced LIGO and Advanced Virgo, which took place from 2016 November to 2017 August. We have analyzed 98 gamma-ray bursts using an unmodeled search method that searches for generic transient gravitational waves and 42 with a modeled search method that targets compact-binary mergers as progenitors of short gamma-ray bursts. Both methods clearly detect the previously reported binary merger signal GW170817, with p-values of $<9.38 \times 10^{-6}$ (modeled) and $3.1 \times 10^{-4}$ (unmodeled). We do not find any significant evidence for gravitational-wave signals associated with the other gamma-ray bursts analyzed, and therefore we report lower bounds on the distance to each of these, assuming various source types and signal morphologies. Using our final modeled search results, short gamma-ray burst observations, and assuming binary neutron star progenitors, we place bounds on the rate of short gamma-ray bursts as a function of redshift for $z \leq 1$. We estimate 0.07-1.80 joint detections with Fermi-GBM per year for the 2019-20 LIGO-Virgo observing run and 0.15-3.90 per year when current gravitational-wave detectors are operating at their design sensitivities.

Published
2019
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15. Radio, Hard X-Ray, and Gamma-Ray Emissions Associated with a Far-Side Solar Event

Author

Grechnev, V. V., Kiselev, V. I., Kashapova, L. K., Kochanov, A. A., Zimovets, I. V., Uralov, A. M., Nizamov, B. A., Grigorieva, I. Yu., Golovin, D. V., Litvak, M. L., Mitrofanov, I. G., and Sanin, A. B.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The SOL2014-09-01 far-side solar eruptive event produced hard electromagnetic and radio emissions observed with detectors at near-Earth vantage points. Especially challenging was a long-duration >100 MeV $\gamma$-ray burst probably produced by accelerated protons exceeding 300 MeV. This observation raised a question of how high-energy protons could reach the Earth-facing solar surface. Some preceding studies discussed a scenario in which protons accelerated by a CME-driven shock high in the corona return to the solar surface. We continue with the analysis of this challenging event, involving radio images from the Nan\c{c}ay Radioheliograph and hard X-ray data from the High Energy Neutron Detector (HEND) of the Gamma-Ray Spectrometer onboard the Mars Odyssey space observatory located near Mars. HEND recorded unocculted flare emission. The results indicate that the emissions observed from the Earth's direction were generated by flare-accelerated electrons and protons trapped in static long coronal loops. Their reacceleration is possible in these loops by a shock wave, which was excited by the eruption, being initially not CME-driven. The results highlight the ways to address remaining questions., Comment: 36 pages, 11 figures. For associated movie file, see http://ssrt.iszf.irk.ru/~grechnev/papers/2014-09-01/ Accepted for publication in Solar Physics

Published
2018
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16. New estimation of non-thermal electron energetics in the giant solar flare on 28 October 2003 based on Mars Odyssey observations

Author

Nizamov, B. A., Zimovets, I. V., Golovin, D. V., Sanin, A. B., Litvak, M. L., Tretyakov, V. I., Mitrofanov, I. G., and Kozyrev, A. S.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

A new estimation of the total number and energy of the non-thermal electrons produced in the giant ($>\text{X}17$) solar flare on 2003 October 28 is presented based on the analysis of the observations of the hard X-ray (HXR) emission by the High Energy Neutron Detector (HEND) onboard the Mars Odyssey spacecraft orbiting Mars. Previous estimations of the non-thermal electron energy based on the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) data were incomplete since RHESSI missed the peak of the flare impulsive phase. In contrast, HEND observed the whole flare. We used two models to estimate the energy of the non-thermal electrons: the cold thick target model and the warm thick target model. We found that, depending on the model used and the low-energy cutoff ($E_\mathrm{c}$) of the non-thermal electrons, the estimate of their total energy in the entire flare can vary from $2.3 \times 10^{32}$ to $6.2 \times 10^{33}$ ergs. The lowest estimate, $2.3 \times 10^{32}$ ergs, obtained within the cold thick target model and fixed $E_\mathrm{c}=43$ keV, is consistent with the previous estimate. In this case, non-thermal electrons accelerated in the peak of the flare impulsive phase missed by RHESSI contained approximately $40\%$ of the total energy of non-thermal electrons of the entire flare. The highest value, $6.2 \times 10^{33}$ ergs, obtained with the cold thick target model and fixed $E_\mathrm{c}=10$ keV, looks abnormally high, since it exceeds the total non-potential magnetic energy of the parent active region and the total bolometric energy radiated in the flare. Our estimates also show that the total number and energetics of the HXR-producing electrons in the flare region is a few orders of magnitude higher than of the population of energetic electrons injected into interplanetary space., Comment: Accepted to Journal of Atmospheric and Solar-Terrestrial Physics

Published
2018
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20. Catalog of Hard X-ray Solar Flares Detected with Mars Odyssey/HEND from the Mars Orbit in 2001-2016

Author

Livshits, M. A., Zimovets, I. V., Golovin, D. V., Nizamov, B. A., Vybornov, V. I., Mitrofanov, I. G., Kozyrev, A. S., Litvak, M. L., Sanin, A. B., and Tretyakov, V. I.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The study of nonstationary processes in the Sun is of great interest, and lately, multiwavelength observations and registration of magnetic fields are carried out by means of both ground-based telescopes and several specialized spacecraft (SC) on near-Earth orbits. However the acquisition of the new reliable information on their hard X-ray radiation remains demanded, in particular if the corresponding SC provide additional information, e.g. in regard to the flare observations from the directions other than the Sun-Earth direction. In this article we present a catalog of powerful solar flares registered by the High Energy Neutron Detector (HEND) device designed in the Space Research Institute (IKI) of Russian Academy of Sciences. HEND is mounted onboard the 2001 Mars Odyssey spacecraft. It worked successfully during the flight to Mars and currently operates in the near-Mars orbit. Besides neutrons, the HEND instrument is sensitive to the hard X-ray and gamma radiation. This radiation is registered by two scintillators: the outer one is sensitive to the photons above 40 keV and the inner one to the photons above 200 keV. The catalog was created with the new procedure of the data calibration. For most powerful 60 solar flares on the visible and on the far sides of the Sun (in respect to a terrestrial observer), we provide time profiles of flare radiation, summed over all the channels of X-ray and in some cases of gamma-ray bands as well as the spectra and characteristics of their power law approximation. We briefly discuss the results of the previous articles on the study of the Sun with HEND instrument and the potential of the further use of these data., Comment: 11 pages. Accepted by Astronomy Reports. The supplementary material will be published online with the electronic version of the journal article

Published
2017
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21. Search for Gravitational Waves Associated with Gamma-Ray Bursts During the First Advanced LIGO Observing Run and Implications for the Origin of GRB 150906B

Author

LIGO Scientific Collaboration, Virgo Collaboration, IPN Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., 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., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., 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, D'alya, G., 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., Devenson, J., Devine, R. C., Dhurandhar, S., D'iaz, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., 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., Effler, 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., Fyffe, M., Gabbard, H., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, 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., 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., K'ef'elian, 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., Kr"amer, C., Kringel, V., Krishnan, B., Kr'olak, 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., L"uck, 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., Pfeiffer, 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., P"urrer, M., Qi, H., Qin, J., Qiu, S., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, 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., R"udiger, 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., Sch"onbeck, 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., Shaffer, 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., T"oyr"a, D., Travasso, F., Traylor, G., Trifir`o, 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., Vicer'e, 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., Wessels, 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., zny, A. Zadro., 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., Zweizig, J., Aptekar, R. L., Frederiks, D. D., Golenetskii, S. V., Golovin, D. V., Hurley, K., Litvak, M. L., Mitrofanov, I. G., Rau, A., Sanin, A. B., Svinkin, D. S., von Kienlin, A., and Zhang, X.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

We present the results of the search for gravitational waves (GWs) associated with $\gamma$-ray bursts detected during the first observing run of the Advanced Laser Interferometer Gravitational-Wave Observatory (LIGO). We find no evidence of a GW signal for any of the 41 $\gamma$-ray bursts for which LIGO data are available with sufficient duration. For all $\gamma$-ray bursts, we place lower bounds on the distance to the source using the optimistic assumption that GWs with an energy of $10^{-2}M_\odot c^2$ were emitted within the $16$-$500\,$Hz band, and we find a median 90% confidence limit of 71$\,$Mpc at 150$\,$Hz. For the subset of 19 short/hard $\gamma$-ray bursts, we place lower bounds on distance with a median 90% confidence limit of 90$\,$Mpc for binary neutron star (BNS) coalescences, and 150 and 139$\,$Mpc for neutron star-black hole coalescences with spins aligned to the orbital angular momentum and in a generic configuration, respectively. These are the highest distance limits ever achieved by GW searches. We also discuss in detail the results of the search for GWs associated with GRB 150906B, an event that was localized by the InterPlanetary Network near the local galaxy NGC 3313, which is at a luminosity distance of 54$\,$Mpc ($z=0.0124$). Assuming the $\gamma$-ray emission is beamed with a jet half-opening angle $\leq 30^{\circ}$, we exclude a BNS and a neutron star-black hole in NGC 3313 as the progenitor of this event with confidence $>99$%. Further, we exclude such progenitors up to a distance of 102$\,$Mpc and 170$\,$Mpc, respectively., Comment: 18 pages, 6 figures, 3 tables

Published
2016
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26. The Financial Narrative Summarisation Shared Task (FNS 2023)

Author

He, Jingrui, Palpanas, Themis, Hu, Xiaohua, Cuzzocrea, Alfredo, Dou, Dejing, Slezak, Dominik, Wang, Wei, Gruca, Aleksandra, Lin, Jerry Chun-Wei, Agrawal, Rakesh, Zavitsanos, E., Kosmopoulos, A., Giannakopoulos, G., Litvak, M., Carbajo-Coronado, B., Moreno-Sandoval, A., El-Haj, M., He, Jingrui, Palpanas, Themis, Hu, Xiaohua, Cuzzocrea, Alfredo, Dou, Dejing, Slezak, Dominik, Wang, Wei, Gruca, Aleksandra, Lin, Jerry Chun-Wei, Agrawal, Rakesh, Zavitsanos, E., Kosmopoulos, A., Giannakopoulos, G., Litvak, M., Carbajo-Coronado, B., Moreno-Sandoval, A., and El-Haj, M.

Abstract

This paper presents the results and findings of the Financial Narrative Summarisation Shared Task on summarising UK, Greek, and Spanish annual reports. The shared task was organised as part of the 5th Financial Narrative Processing Workshop (FNP 2023). The Financial Narrative summarisation Shared Task (FNS 2023) has been running since 2020 as part of the Financial Narrative Processing (FNP) workshop series [15–20]. The shared task included one main challenge, which is the use of either abstractive or extractive automatic summarisers to summarise long documents in terms of UK, Greek, and Spanish financial annual reports. This shared task is the fourth to target financial documents. The data for the shared task was created and collected from publicly available annual reports published by firms listed on the Stock Exchanges of the UK, Greece, and Spain. A total number of 6 systems from 3 different teams participated in the shared task.

Published
2024

27. A Semi‐Mechanistic Model for Partitioning Evapotranspiration Reveals Transpiration Dominates the Water Flux in Drylands.

Author

Reich, E. G., Samuels‐Crow, K., Bradford, J. B., Litvak, M., Schlaepfer, D. R., and Ogle, K.

Subjects
HUMIDITY, EDDY flux, ARID regions climate, ENVIRONMENTAL engineering, VAPOR pressure, EVAPOTRANSPIRATION
Abstract

Popular evapotranspiration (ET) partitioning methods make assumptions that might not be well‐suited to dryland ecosystems, such as high sensitivity of plant water‐use efficiency (WUE) to vapor pressure deficit (VPD). Our objectives were to (a) create an ET partitioning model that can produce fine‐scale estimates of transpiration (T) in drylands, and (b) use this approach to evaluate how climate controls T and WUE across ecosystem types and timescales along a dryland aridity gradient. We developed a novel, semi‐mechanistic ET partitioning method using a Bayesian approach that constrains abiotic evaporation using process‐based models, and loosely constrains time‐varying WUE within an autoregressive framework. We used this method to estimate daily T and weekly WUE across seven dryland ecosystem types and found that T dominates ET across the aridity gradient. Then, we applied cross‐wavelet coherence analysis to evaluate the temporal coherence between focal response variables (WUE and T/ET) and environmental variables. At yearly scales, we found that WUE at less arid, higher elevation sites was primarily limited by atmospheric moisture demand, and WUE at more arid, lower elevation sites was primarily limited by moisture supply. At sub‐yearly timescales, WUE and VPD were sporadically correlated. Hence, ecosystem‐scale dryland WUE is not always sensitive to changes in VPD at short timescales, despite this being a common assumption in many ET partitioning models. This new ET partitioning method can be used in dryland ecosystems to better understand how climate influences physically and biologically driven water fluxes. Plain Language Summary: We developed a new model to better understand how plants use and lose water in drylands and applied it to seven dryland sites. Our model partitions evapotranspiration—the total water lost to the atmosphere from the Earth's surface— into its components. Evapotranspiration consists of both evaporation from wet surfaces, such as wet soil, and the water lost from plants when they photosynthesize. Currently, models assume a strong relationship between the efficiency with which plants use water ("water‐use efficiency") and the dryness of the atmosphere, but this violates what we know about how plants function in drylands. For example, in drylands many plants are adapted to very dry conditions and their water use can be less sensitive to increasing atmospheric dryness compared to plants from wet environments. Using this new model, we found that plant water‐use efficiency is only correlated with atmospheric dryness some of the time and that evapotranspiration is primary controlled by water lost from plants. This model allows us to better understand the importance of timescale and ecosystem type in governing plant water‐use dynamics and more accurately assess the potential impact of changing climate conditions on dryland water fluxes and ecosystem processes. Key Points: A new evapotranspiration partitioning model (DEPART) was developed using eddy covariance flux tower measurements in a Bayesian frameworkThis method produces daily estimates of transpiration and weekly estimates of plant water‐use efficiency at the ecosystem scaleThis method reveals water‐use efficiency is limited by moisture supply in more arid climates and moisture demand in less arid climates [ABSTRACT FROM AUTHOR]

Published
2024
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30. A Missing-Link in the Supernova-GRB Connection: The Case of SN 2012ap

Author

Chakraborti, Sayan, Soderberg, Alicia, Chomiuk, Laura, Kamble, Atish, Yadav, Naveen, Ray, Alak, Hurley, Kevin, Margutti, Raffaella, Milisavljevic, Dan, Bietenholz, Michael, Brunthaler, Andreas, Pignata, Giuliano, Pian, Elena, Mazzali, Paolo, Fransson, Claes, Bartel, Norbert, Hamuy, Mario, Levesque, Emily, MacFadyen, Andrew, Dittmann, Jason, Krauss, Miriam, Briggs, M. S., Connaughton, V., Yamaoka, K., Takahashi, T., Ohno, M., Fukazawa, Y., Tashiro, M., Terada, Y., Murakami, T., Goldsten, J., Barthelmy, S., Gehrels, N., Cummings, J., Krimm, H., Palmer, D., Golenetskii, S., Aptekar, R., Frederiks, D., Svinkin, D., Cline, T., Mitrofanov, I. G., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Enos, H., von Kienlin, A., Rau, A., Zhang, X., and Savchenko, V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Gamma Ray Bursts (GRBs) are characterized by ultra-relativistic outflows, while supernovae are generally characterized by non-relativistic ejecta. GRB afterglows decelerate rapidly usually within days, because their low-mass ejecta rapidly sweep up a comparatively larger mass of circumstellar material. However supernovae, with heavy ejecta, can be in nearly free expansion for centuries. Supernovae were thought to have non-relativistic outflows except for few relativistic ones accompanied by GRBs. This clear division was blurred by SN 2009bb, the first supernova with a relativistic outflow without an observed GRB. Yet the ejecta from SN 2009bb was baryon loaded, and in nearly-free expansion for a year, unlike GRBs. We report the first supernova discovered without a GRB, but with rapidly decelerating mildly relativistic ejecta, SN 2012ap. We discovered a bright and rapidly evolving radio counterpart driven by the circumstellar interaction of the relativistic ejecta. However, we did not find any coincident GRB with an isotropic fluence of more than a sixth of the fluence from GRB 980425. This shows for the first time that central engines in type Ic supernovae, even without an observed GRB, can produce both relativistic and rapidly decelerating outflows like GRBs., Comment: 8 pages, 5 figures, 1 table, accepted for publication in ApJ

Published
2014
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32. The ultraluminous GRB 110918A

Author

Frederiks, D. D., Hurley, K., Svinkin, D. S., Pal'shin, V. D., Mangano, V., Oates, S., Aptekar, R. L., Golenetskii, S. V., Mazets, E. P., Oleynik, Ph. P., Tsvetkova, A. E., Ulanov, M. V., Kokomov, A. V., Cline, T. L., Burrows, D. N., Krimm, H. A., Pagani, C., Sbarufatti, B., Siegel, M. H., Mitrofanov, I. G., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Enos, H., Starr, R., von Kienlin, A., Rau, A., Zhang, X., and Goldstein, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

GRB 110918A is the brightest long GRB detected by Konus-WIND during its 19 years of continuous observations and the most luminous GRB ever observed since the beginning of the cosmological era in 1997. We report on the final IPN localization of this event and its detailed multiwavelength study with a number of space-based instruments. The prompt emission is characterized by a typical duration, a moderare $E_{peak}$ of the time-integrated spectrum, and strong hard-to-soft evolution. The high observed energy fluence yields, at z=0.984, a huge isotropic-equivalent energy release $E_{iso}=(2.1\pm0.1)\times10^{54}$ erg. The record-breaking energy flux observed at the peak of the short, bright, hard initial pulse results in an unprecedented isotropic-equivalent luminosity $L_{iso}=(4.7\pm0.2)\times10^{54}$erg s$^{-1}$. A tail of the soft gamma-ray emission was detected with temporal and spectral behavior typical of that predicted by the synchrotron forward-shock model. Swift/XRT and Swift/UVOT observed the bright afterglow from 1.2 to 48 days after the burst and revealed no evidence of a jet break. The post-break scenario for the afterglow is preferred from our analysis, with a hard underlying electron spectrum and ISM-like circumburst environment implied. We conclude that, among multiple reasons investigated, the tight collimation of the jet must have been a key ingredient to produce this unusually bright burst. The inferred jet opening angle of 1.7-3.4 deg results in reasonable values of the collimation-corrected radiated energy and the peak luminosity, which, however, are still at the top of their distributions for such tightly collimated events. We estimate a detection horizon for a similar ultraluminous GRB of $z\sim7.5$ for Konus-WIND, and $z\sim12$ for Swift/BAT, which stresses the importance of GRBs as probes of the early Universe., Comment: 22 pages, 20 figures, accepted for publication in ApJ

Published
2013
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37. Influence of ENSO and the NAO on terrestrial carbon uptake in the Texas-northern Mexico region

Author

Parazoo, NC, Barnes, E, Worden, J, Harper, AB, Bowman, KB, Frankenberg, C, Wolf, S, Litvak, M, and Keenan, TF

Subjects
Meteorology & Atmospheric Sciences, Atmospheric Sciences, Geochemistry, Oceanography
Abstract

Climate extremes such as drought and heat waves can cause substantial reductions in terrestrial carbon uptake. Advancing projections of the carbon uptake response to future climate extremes depends on (1) identifying mechanistic links between the carbon cycle and atmospheric drivers, (2) detecting and attributing uptake changes, and (3) evaluating models of land response and atmospheric forcing. Here, we combine model simulations, remote sensing products, and ground observations to investigate the impact of climate variability on carbon uptake in the Texas-northern Mexico region. Specifically, we (1) examine the relationship between drought, carbon uptake, and variability of El Niño-Southern Oscillation (ENSO) and the North Atlantic Oscillation (NAO) using the Joint UK Land-Environment Simulator (JULES) biosphere simulations from 1950-2012, (2) quantify changes in carbon uptake during record drought conditions in 2011, and (3) evaluate JULES carbon uptake and soil moisture in 2011 using observations from remote sensing and a network of flux towers in the region. Long-term simulations reveal systematic decreases in regional-scale carbon uptake during negative phases of ENSO and NAO, including amplified reductions of gross primary production (GPP) (-0.42 ± 0.18 Pg C yr-1) and net ecosystem production (NEP) (-0.14 ± 0.11 Pg C yr-1) during strong La Niña years. The 2011 megadrought caused some of the largest declines of GPP (-0.50 Pg C yr-1) and NEP (-0.23 Pg C yr-1) in our simulations. In 2011, consistent declines were found in observations, including high correlation of GPP and surface soil moisture (r = 0.82 ± 0.23, p = 0.012) in remote sensing-based products. These results suggest a large-scale response of carbon uptake to ENSO and NAO, and highlight a need to improve model predictions of ENSO and NAO in order to improve predictions of future impacts on the carbon cycle and the associated feedbacks to climate change.

Published
2015

38. Pervasive drought legacies in forest ecosystems and their implications for carbon cycle models

Author

Anderegg, WRL, Schwalm, C, Biondi, F, Camarero, JJ, Koch, G, Litvak, M, Ogle, K, Shaw, JD, Shevliakova, E, Williams, AP, Wolf, A, Ziaco, E, and Pacala, S

Subjects
Climate Action, Carbon Cycle, Climate Change, Droughts, Europe, Forests, Models, Theoretical, Trees, United States, General Science & Technology
Abstract

The impacts of climate extremes on terrestrial ecosystems are poorly understood but important for predicting carbon cycle feedbacks to climate change. Coupled climate-carbon cycle models typically assume that vegetation recovery from extreme drought is immediate and complete, which conflicts with the understanding of basic plant physiology. We examined the recovery of stem growth in trees after severe drought at 1338 forest sites across the globe, comprising 49,339 site-years, and compared the results with simulated recovery in climate-vegetation models. We found pervasive and substantial "legacy effects" of reduced growth and incomplete recovery for 1 to 4 years after severe drought. Legacy effects were most prevalent in dry ecosystems, among Pinaceae, and among species with low hydraulic safety margins. In contrast, limited or no legacy effects after drought were simulated by current climate-vegetation models. Our results highlight hysteresis in ecosystem-level carbon cycling and delayed recovery from climate extremes.

Published
2015

39. Soil moisture response to snowmelt timing in mixed-conifer subalpine forests

Author

Harpold, AA, Molotch, NP, Musselman, KN, Bales, RC, Kirchner, PB, Litvak, M, and Brooks, PD

Subjects
snowmelt, soil moisture, snow-vegetation interactions, cross-site comparison, Environmental Engineering, Physical Geography and Environmental Geoscience, Civil Engineering
Abstract

Western US forest ecosystems and downstream water supplies are reliant on seasonal snowmelt. Complex feedbacks govern forest-snow interactions in which forests influence the distribution of snow and the timing of snowmelt but are also sensitive to snow water availability. Notwithstanding, few studies have investigated the influence of forest structure on snow distribution, snowmelt and soil moisture response. Using a multi-year record from co-located observations of snow depth and soil moisture, we evaluated the influence of forest-canopy position on snow accumulation and snow depth depletion, and associated controls on the timing of soil moisture response at Boulder Creek, Colorado, Jemez River Basin, New Mexico, and the Wolverton Basin, California. Forest-canopy controls on snow accumulation led to 12-42cm greater peak snow depths in open versus under-canopy positions. Differences in accumulation and melt across sites resulted in earlier snow disappearance in open positions at Jemez and earlier snow disappearance in under-canopy positions at Boulder and Wolverton sites. Irrespective of net snow accumulation, we found that peak annual soil moisture was nearly synchronous with the date of snow disappearance at all sites with an average deviation of 12, 3 and 22days at Jemez, Boulder and Wolverton sites, respectively. Interestingly, sites in the Sierra Nevada showed peak soil moisture prior to snow disappearance at both our intensive study site and the nearby snow telemetry stations. Our results imply that the duration of soil water stress may increase as regional warming or forest disturbance lead to earlier snow disappearance and soil moisture recession in subalpine forests.

Published
2015

40. GRB 080407: an ultra-long burst discovered by the IPN

Author

Pal'shin, V., Hurley, K., Goldsten, J., Mitrofanov, I. G., Boynton, W., von Kienlin, A., Cummings, J., Feroci, M., Aptekar, R., Frederiks, D., Golenetskii, S., Mazets, E., Svinkin, D., Golovin, D., Litvak, M. L., Sanin, A. B., Fellows, C., Harshman, K., Starr, R., Rau, A., Savchenko, V., Zhang, X., Barthelmy, S., Gehrels, N., Krimm, H., Palmer, D., Del Monte, E., and Marisaldi, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present observations of the extremely long GRB 080704 obtained with the instruments of the Interplanetary Network (IPN). The observations reveal two distinct emission episodes, separated by a ~1500 s long period of quiescence. The total burst duration is about 2100 s. We compare the temporal and spectral characteristics of this burst with those obtained for other ultra-long GRBs and discuss these characteristics in the context of different models., Comment: 5 pages, 2 figures, 3 tables. Proceedings of the Gamma-Ray Bursts 2012 Conference (GRB 2012) held in Munich, Germany, May 7-11, 2012. Published online at http://pos.sissa.it/cgi-bin/reader/conf.cgi?confid=152

Published
2013

41. Extremely long hard bursts observed by Konus-Wind

Author

Pal'shin, V., Aptekar, R., Frederiks, D., Golenetskii, S., Il'Inskii, V., Mazets, E., Yamaoka, K., Ohno, M., Hurley, K., Sakamoto, T., Oleynik, P., Ulanov, M., Mitrofanov, I. G., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Shinohara, C., and Starr, R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report the observations of the prompt emission of the extremely long hard burst, GRB 060814B, discovered by Konus-Wind and localized by the IPN. The observations reveal a smooth, hard, ~40-min long pulse followed by weaker emission seen several hours after the burst onset. We also present the Konus-Wind data on similar burst, GRB 971208, localized by BATSE/IPN. And finally we discuss the different possible origins of these unusual events., Comment: 4 pages, 2 figures, 2 tables. Proceedings of the "Gamma-Ray Bursts 2007" conference held in Santa Fe, New Mexico, November 5-9, 2007. The published article may be found at http://link.aip.org/link/?apc/1000/117

Published
2013
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42. IPN localizations of Konus short gamma-ray bursts

Author

Pal'shin, V. D., Hurley, K., Svinkin, D. S., Aptekar, R. L., Golenetskii, S. V., Frederiks, D. D., Mazets, E. P., Oleynik, P. P., Ulanov, M. V., Cline, T., Mitrofanov, I. G., Golovin, D. V., Kozyrev, A. S., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Trombka, J., McClanahan, T., Starr, R., Goldsten, J., Gold, R., Rau, A., von Kienlin, A., Savchenko, V., Smith, D. M., Hajdas, W., Barthelmy, S. D., Cummings, J., Gehrels, N., Krimm, H., Palmer, D., Yamaoka, K., Ohno, M., Fukazawa, Y., Hanabata, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Briggs, M. S., Kippen, R. M., Kouveliotou, C., Meegan, C., Fishman, G., Connaughton, V., Boer, M., Guidorzi, C., Frontera, F., Montanari, E., Rossi, F., Feroci, M., Amati, L., Nicastro, L., Orlandini, M., Del Monte, E., Costa, E., Donnarumma, I., Evangelista, Y., Lapshov, I., Lazzarotto, F., Pacciani, L., Rapisarda, M., Soffitta, P., Di Cocco, G., Fuschino, F., Galli, M., Labanti, C., Marisaldi, M., Atteia, J. -L., Vanderspek, R., and Ricker, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Between the launch of the \textit{GGS Wind} spacecraft in 1994 November and the end of 2010, the Konus-\textit{Wind} experiment detected 296 short-duration gamma-ray bursts (including 23 bursts which can be classified as short bursts with extended emission). During this period, the IPN consisted of up to eleven spacecraft, and using triangulation, the localizations of 271 bursts were obtained. We present the most comprehensive IPN localization data on these events. The short burst detection rate, $\sim$18 per year, exceeds that of many individual experiments., Comment: Published version

Published
2013
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43. The Interplanetary Network Supplement to the Fermi GBM Catalog of Cosmic Gamma-Ray Bursts

Author

Hurley, K., Pal'shin, V. D., Aptekar, R. L., Golenetskii, S. V., Frederiks, D. D., Mazets, E. P., Svinkin, D. S., Briggs, M. S., Connaughton, V., Meegan, C., Goldsten, J., Boynton, W., Fellows, C., Harshman, K., Mitrofanov, I. G., Golovin, D. V., Kozyrev, A. S., Litvak, M. L., Sanin, A. B., Rau, A., von Kienlin, A., Zhang, X., Yamaoka, K., Fukazawa, Y., Hanabata, Y., Ohno, M., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Barthelmy, S., Cline, T., Gehrels, N., Cummings, J., Krimm, H. A., Smith, D. M., Del Monte, E., Feroci, M., and Marisaldi, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present Interplanetary Network (IPN) data for the gamma-ray bursts in the first Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 491 bursts in that catalog, covering 2008 July 12 to 2010 July 11, 427 were observed by at least one other instrument in the 9-spacecraft IPN. Of the 427, the localizations of 149 could be improved by arrival time analysis (or triangulation). For any given burst observed by the GBM and one other distant spacecraft, triangulation gives an annulus of possible arrival directions whose half-width varies between about 0.4' and 32 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. We find that the IPN localizations intersect the 1 sigma GBM error circles in only 52% of the cases, if no systematic uncertainty is assumed for the latter. If a 6 degree systematic uncertainty is assumed and added in quadrature, the two localization samples agree about 87% of the time, as would be expected. If we then multiply the resulting error radii by a factor of 3, the two samples agree in slightly over 98% of the cases, providing a good estimate of the GBM 3 sigma error radius. The IPN 3 sigma error boxes have areas between about 1 square arcminute and 110 square degrees, and are, on the average, a factor of 180 smaller than the corresponding GBM localizations. We identify two bursts in the IPN/GBM sample that did not appear in the GBM catalog. In one case, the GBM triggered on a terrestrial gamma flash, and in the other, its origin was given as uncertain. We also discuss the sensitivity and calibration of the IPN., Comment: 52 pages, 12 figures, 4 tables. Revised version, resubmitted to the Astrophysical Journal Supplement Series following refereeing. Figures of the localizations in Table 3 may be found on the IPN website, at ssl.berkeley.edu/ipn3/YYMMDD, where YY, MM, and DD are the year, month, and day of the burst, sometimes with suffixes A or B

Published
2013
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45. Mars Science Laboratory Dynamic Albedo of Neutrons passive mode data and results from sols 753 to 1292: Pahrump Hills to Naukluft Plateau

Author

Tate, C.G., Moersch, J., Mitrofanov, I., Litvak, M., Bellutta, P., Boynton, W.V., Cagle, N., Ehresmann, B., Fedosov, F., Golovin, D., Hardgrove, C., Harshman, K., Hassler, D.M., Jun, I., Kozyrev, A.S., Lisov, D., Malakhov, A., Mischna, M., Nikiforov, S., Sanin, A.B., Starr, R., Vostrukhin, A., and Zeitlin, C.

Published
2019
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46. Inverse Compton X-ray Emission from Supernovae with Compact Progenitors: Application to SN2011fe

Author

Margutti, R., Soderberg, A. M., Chomiuk, L., Chevalier, R., Hurley, K., Milisavljevic, D., Foley, R. J., Hughes, J. P., Slane, P., Fransson, C., Moe, M., Barthelmy, S., Boynton, W., Briggs, M., Connaughton, V., Costa, E., Cummings, J., Del Monte, E., Enos, H., Fellows, C., Feroci, M., Fukazawa, Y., Gehrels, N., Goldsten, J., Golovin, D., Hanabata, Y., Harshman, K., Krimm, H., Litvak, M. L., Makishima, K., Marisaldi, M., Mitrofanov, I. G., Murakami, T., Ohno, M., Palmer, D. M., Sanin, A. B., Starr, R., and Svinkin, D.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present a generalized analytic formalism for the inverse Compton X-ray emission from hydrogen-poor supernovae and apply this framework to SN2011fe using Swift-XRT, UVOT and Chandra observations. We characterize the optical properties of SN2011fe in the Swift bands and find them to be broadly consistent with a "normal" SN Ia, however, no X-ray source is detected by either XRT or Chandra. We constrain the progenitor system mass loss rate to be lower than 2x10^-9 M_sun/yr (3sigma c.l.) for wind velocity v_w=100 km/s. Our result rules out symbiotic binary progenitors for SN2011fe and argues against Roche-lobe overflowing subgiants and main sequence secondary stars if >1% of the transferred mass is lost at the Lagrangian points. Regardless of the density profile, the X-ray non-detections are suggestive of a clean environment (particle density < 150 cm-3) for (2x10^15

Published
2012
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47. THE INTERPLANETARY NETWORK

Author

Hurley, K., primary, Mitrofanov, I. G., additional, Golovin, D., additional, Litvak, M. L., additional, Sanin, A. B., additional, Boynton, W., additional, Fellows, C., additional, Harshman, K., additional, Starr, R., additional, Golenetskii, S., additional, Aptekar, R., additional, Mazets, E., additional, Palshin, V., additional, Frederiks, D., additional, Svinkin, D., additional, Smith, D. M., additional, Hajdas, W., additional, Kienlin, A. von, additional, Zhang, X., additional, Rau, A., additional, Yamaoka, K., additional, Takahashi, T., additional, Ohno, M., additional, Hanabata, Y., additional, Fukazawa, Y., additional, Tashiro, M., additional, Terada, Y., additional, Murakami, T., additional, Makishima, K., additional, Cline, T., additional, Barthelmy, S., additional, Cummings, J., additional, Gehrels, N., additional, Krimm, H., additional, Palmer, D., additional, Goldsten, J., additional, Del Monte, E., additional, Feroci, M., additional, Marisaldi, M., additional, Connaughton, V., additional, Briggs, M. S., additional, and Meegan, C., additional

Published
2020
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48. The Interplanetary Network Supplement to the Fermi GBM Catalog - An AO-2 and AO-3 Guest Investigator Project

Author

Hurley, K., Briggs, M., Connaughton, V., Meegan, C., von Kienlin, A., Rau, A., Zhang, X., Golenetskii, S., Aptekar, R., Mazets, E., Pal'shin, V., Frederiks, D., Barthelmy, S., Cline, T., Cummings, J., Gehrels, N., Krimm, H. A., Mitrofanov, I. G., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Starr, R., Smith, D. M., Hajdas, W., Yamaoka, K., Ohno, M., Fukazawa, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Palmer, D. M., Goldsten, J., Del Monte, E., Feroci, M., and Marisaldi, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

In the first two years of operation of the Fermi GBM, the 9-spacecraft Interplanetary Network (IPN) detected 158 GBM bursts with one or two distant spacecraft, and triangulated them to annuli or error boxes. Combining the IPN and GBM localizations leads to error boxes which are up to 4 orders of magnitude smaller than those of the GBM alone. These localizations comprise the IPN supplement to the GBM catalog, and they support a wide range of scientific investigations., Comment: 2011 Fermi Symposium proceedings - eConf C110509

Published
2011

49. The Interplanetary Network Supplement to the BeppoSAX Gamma-Ray Burst Catalogs

Author

Hurley, K., Guidorzi, C., Frontera, F., Montanari, E., Rossi, F., Feroci, M., Mazets, E., Golenetskii, S., Frederiks, D. D., Pal'shin, V. D., Aptekar, R. L., Cline, T., Trombka, J., McClanahan, T., Starr, R., Atteia, J. -L., Barraud, C., Pelangeon, A., Boer, M., Vanderspek, R., Ricker, G., Mitrofanov, I. G., Golovin, D. V., Kozyrev, A. S., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Goldsten, J., Gold, R., Smith, D. M., Wigger, C., and Hajdas, W.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Between 1996 July and 2002 April, one or more spacecraft of the interplanetary network detected 787 cosmic gamma-ray bursts that were also detected by the Gamma-Ray Burst Monitor and/or Wide-Field X-Ray Camera experiments aboard the BeppoSAX spacecraft. During this period, the network consisted of up to six spacecraft, and using triangulation, the localizations of 475 bursts were obtained. We present the localization data for these events., Comment: 89 pages, 3 figures. Submitted to the Astrophysical Journal Supplement Series

Published
2010
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50. Integrating the Fermi Gamma-Ray Burst Monitor into the 3rd Interplanetary Network

Author

Hurley, K., Briggs, M., Connaughton, V., Meegan, C., Cline, T., Mitrofanov, I., Golovin, D., Litvak, M. L., Sanin, A. B., Boynton, W., Fellows, C., Harshman, K., Starr, R., Golenetskii, S., Aptekar, R., Mazets, E., Pal'shin, V., Frederiks, D., Smith, D. M., Wigger, C., Rau, A., von Kienlin, A., Yamaoka, K., Ohno, M., Fukazawa, Y., Takahashi, T., Tashiro, M., Terada, Y., Murakami, T., Makishima, K., Barthelmy, S., Cummings, J., Gehrels, N., Krimm, H., Goldsten, J., Del Monte, E., Feroci, M., and Marisaldi, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We are integrating the Fermi Gamma-Ray Burst Monitor (GBM) into the Interplanetary Network (IPN) of Gamma-Ray Burst (GRB) detectors. With the GBM, the IPN will comprise 9 experiments. This will 1) assist the Fermi team in understanding and reducing their systematic localization uncertainties, 2) reduce the sizes of the GBM and Large Area Telescope (LAT) error circles by 1 to 4 orders of magnitude, 3) facilitate the identification of GRB sources with objects found by ground- and space-based observatories at other wavelengths, from the radio to very high energy gamma-rays, 4) reduce the uncertainties in associating some LAT detections of high energy photons with GBM bursts, and 5) facilitate searches for non-electromagnetic GRB counterparts, particularly neutrinos and gravitational radiation. We present examples and demonstrate the synergy between Fermi and the IPN. This is a Fermi Cycle 2 Guest Investigator project., Comment: 5 pages, 11 figures. 2009 Fermi Symposium. eConf Proceedings C091122

Published
2009

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