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1. Implications For The Origin Of GRB 051103 From LIGO Observations

Author: The LIGO Scientific Collaboration, Abadie, J., Abbott, B. P., Abbott, T. D., Abbott, R., Abernathy, M., Adams, C., Adhikari, R., Affeldt, C., Ajith, P., Allen, B., Allen, G. S., Ceron, E. Amador, Amariutei, D., Amin, R. S., Anderson, S. B., Anderson, W. G., Arai, K., Arain, M. A., Araya, M. C., Aston, S. M., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballmer, S., Barker, D., Barnum, S., Barr, B., Barriga, P., Barsotti, L., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauchrowitz, J., Behnke, B., Bell, A. S., Belopolski, I., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Biswas, R., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Bock, O., Bodiya, T. P., Bogan, C., Bondarescu, R., Bork, R., Born, M., Bose, S., Boyle, M., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brinkmann, M., Britzger, M., Brooks, A. F., Brown, D. A., Brummitt, A., Buonanno, A., Burguet-Castell, J., Burmeister, O., Byer, R. L., Cadonati, L., Camp, J. B., Campsie, P., Cannizzo, J., Cannon, K., Cao, J., Capano, C., Caride, S., Caudill, S., Cavaglia, M., Cepeda, C., Chalermsongsak, T., Chalkley, E., Charlton, P., Chelkowski, S., Chen, Y., Christensen, N., Chua, S. S. Y., Chung, S., Chung, C. T. Y., Clara, F., Clark, D., Clark, J., Clayton, J. H., Conte, R., Cook, D., Corbitt, T. R. C., Cornish, N., Costa, C. A., Coughlin, M., Coward, D. M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Cumming, A., Cunningham, L., Culter, R. M., Dahl, K., Danilishin, S. L., Dannenberg, R., Danzmann, K., Das, K., Daudert, B., Daveloza, H., Davies, G., Daw, E. J., Dayanga, T., DeBra, D., Degallaix, J., Dent, T., Dergachev, V., DeRosa, R., DeSalvo, R., Dhurandhar, S., Di Palma, I., Diaz, M., Donovan, F., Dooley, K. L., Dorsher, S., Douglas, E. S. D., Drever, R. W. P., Driggers, J. C., Dumas, J. -C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Engel, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Finn, L. S., Flanigan, M., Foley, S., Forsi, E., Fotopoulos, N., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Garcia, J., Garofoli, J. A., Gholami, I., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Gill, C., Goetz, E., Goggin, L. M., Gonzalez, G., Gorodetsky, M. L., Gossler, S., Graef, C., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Grosso, R., Grote, H., Grunewald, S., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Heefner, J., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Hong, T., Hooper, S., Hosken, D. J., Hough, J., Howell, E. J., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Katzman, W., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Kelner, M., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, N., Kim, H., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Korth, W. Z., Kozak, D., Kringel, V., Krishnamurthy, S., Krishnan, B., Kuehn, G., Kumar, R., Kwee, P., Landry, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Li, J., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lormand, M., Lu, P., Luan, J., Lubinski, M., Luck, H., Lundgren, A. P., Macdonald, E., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Mandel, I., Mandic, V., Marandi, A., Marka, S., Marka, Z., Maros, E., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McIver, J., McKechan, D. J. A., Meadors, G., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Miller, J., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Moesta, P., Mohanty, S. D., Moraru, D., Moreno, G., Mossavi, K., Mow-Lowry, C. M., Mueller, G., Mukherjee, S., Mullavey, A., Muller-Ebhardt, H., Munch, J., Murphy, D., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Newton, G., Nishizawa, A., Nolting, D., Nuttall, L., O'Reilly, B., O'Shaughnessy, R., Ochsner, E., O'Dell, J., Ogin, G. H., Oldenburg, R. G., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pan, Y., Pankow, C., Papa, M. A., Patel, P., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Phelps, M., Pickenpack, M., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Podkaminer, J., Pold, J., Postiglione, F., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prokhorov, L., Puncken, O., Quetschke, V., Raab, F. J., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C. R., Rankins, B., Mohapatra, S. R. P., Raymond, V., Redwine, K., Reed, C. M., Reed, T., Reid, S., Reitze, D. H., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinson, C., Robinson, E. L., Roddy, S., Rollins, J., Romano, J. D., Romie, J. H., Rover, C., Rowan, S., Rudiger, A., Ryan, K., Sakata, S., Sakosky, M., Salemi, F., Salit, M., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., SantamarÌa, L., Santiago-Prieto, I., Santostasi, G., Saraf, S., Sathyaprakash, B. S., Sato, S., Saulson, P. R., Savage, R., Schilling, R., Schlamminger, S., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Weerathunga, T. Shihan, Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, R., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Soto, J., Speirits, F. C., Stein, A. J., Steinlechner, J., Steinlechner, S., Steplewski, S., Stefszky, M., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A. S., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Szokoly, G. P., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thuring, A., Tokmakov, K. V., Torres, C., Torrie, C. I., Traylor, G., Trias, M., Tseng, K., Ugolini, D., Urbanek, K., Vahlbruch, H., Vaishnav, B., Vallisneri, M., Broeck, C. Van Den, van der Sluys, M. V., van Veggel, A. A., Vass, S., Vaulin, R., Vecchio, A., Veitch, J., Veitch, P. J., Veltkamp, C., Villar, A. E., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, K., Yamamoto, H., Yang, H., Yeaton-Massey, D., Yoshida, S., Yu, P., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Bizouard, M. A., Dietz, A., Guidi, G. M., and Was, M.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present the results of a LIGO search for gravitational waves (GWs) associated with GRB 051103, a short-duration hard-spectrum gamma-ray burst (GRB) whose electromagnetically determined sky position is coincident with the spiral galaxy M81, which is 3.6 Mpc from Earth. Possible progenitors for short-hard GRBs include compact object mergers and soft gamma repeater (SGR) giant flares. A merger progenitor would produce a characteristic GW signal that should be detectable at the distance of M81, while GW emission from an SGR is not expected to be detectable at that distance. We found no evidence of a GW signal associated with GRB 051103. Assuming weakly beamed gamma-ray emission with a jet semi-angle of 30 deg we exclude a binary neutron star merger in M81 as the progenitor with a confidence of 98%. Neutron star-black hole mergers are excluded with > 99% confidence. If the event occurred in M81 our findings support the the hypothesis that GRB 051103 was due to an SGR giant flare, making it the most distant extragalactic magnetar observed to date., Comment: 8 pages, 3 figures. For a repository of data used in the publication, go to: https://dcc.ligo.org/cgi-bin/DocDB/ShowDocument?docid=15166 . Also see the announcement for this paper on ligo.org at: http://www.ligo.org/science/Publication-GRB051103/index.php
Published: 2012
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2. Super-solar Metal Abundances in Two Galaxies at z ~ 3.57 revealed by the GRB 090323 Afterglow Spectrum

Author: Savaglio, S., Rau, A., Greiner, J., Krühler, T., McBreen, S., Hartmann, D. H., Updike, A. C., Filgas, R., Klose, S., Afonso, P., Clemens, C., Yoldaş, A. Küpcü, E., F. Olivares, Sudilovsky, V., and Szokoly, G.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report on the surprisingly high metallicity measured in two absorption systems at high redshift, detected in the Very Large Telescope spectrum of the afterglow of the gamma-ray burst GRB 090323. The two systems, at redshift z=3.5673 and z=3.5774 (separation Delta v ~ 660 km/s), are dominated by the neutral gas in the interstellar medium of the parent galaxies. From the singly ionized zinc and sulfur, we estimate oversolar metallicities of [Zn/H] =+0.29+/-0.10 and [S/H] = +0.67+/- 0.34, in the blue and red absorber, respectively. These are the highest metallicities ever measured in galaxies at z>3. We propose that the two systems trace two galaxies in the process of merging, whose star formation and metallicity are heightened by the interaction. This enhanced star formation might also have triggered the birth of the GRB progenitor. As typically seen in star-forming galaxies, the fine-structure absorption SiII* is detected, both in G0 and G1. From the rest-frame UV emission in the GRB location, we derive a relatively high, not corrected for dust extinction, star-formation rate SFR ~ 6 Msun/yr. These properties suggest a possible connection between some high-redshift GRB host galaxies and high-z massive sub-millimeter galaxies, which are characterized by disturbed morphologies and high metallicities. Our result provides additional evidence that the dispersion in the chemical enrichment of the Universe at high redshift is substantial, with the existence of very metal rich galaxies less than two billion years after the Big Bang., Comment: accepted for publication in MNRAS
Published: 2011
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3. Directional limits on persistent gravitational waves using LIGO S5 science data

Author: Abbott, B. P., Abbott, R., Abernathy, M., Accadia, T., Acernese, F., Adams, C., Adhikari, R., Ajith, P., Allen, B., Allen, G. S., Ceron, E. Amador, Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Arain, M. A., Araya, M. C., Aronsson, M., Arun, K. G., Aso, Y., Aston, S. M., Astone, P., Atkinson, D., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, D., Barnum, S., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauchrowitz, J., Bauer, Th. S., Behnke, B., Beker, M. G., Belletoile, A., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birch, J., Birindelli, S., Biswas, R., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Boccara, C., Bock, O., Bodiya, T. P., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Bose, S., Bosi, L., Bouhou, B., Boyle, M., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Budzyński, R., Bulik, T., Bulten, H. J., Buonanno, A., Burguet--Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cain, J., Calloni, E., Camp, J. B., Campagna, E., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C., Carbognani, F., Caride, S., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coulon, J. -P., Coward, D. M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., Dannenberg, R., D'Antonio, S., Danzmann, K., Das, K., Dattilo, V., Daudert, B., Davier, M., Davies, G., Davis, A., Daw, E. J., Day, R., Dayanga, T., De Rosa, R., DeBra, D., Degallaix, J., del Prete, M., Dergachev, V., DeRosa, R., DeSalvo, R., Devanka, P., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Di Palma, I., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Dorsher, S., Douglas, E. S. D., Drago, M., Drever, R. W. P., Driggers, J. C., Dueck, J., Dumas, J. -C., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Engel, R., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flanigan, M., Flasch, K., Foley, S., Forrest, C., Forsi, E., Fotopoulos, N., Fournier, J. -D., Franc, J., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoni, L., Garofoli, J. A., Garufi, F., Gemme, G., Genin, E., Gennai, A., Gholami, I., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gill, C., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grosso, R., Grote, H., Grunewald, S., Guidi, G. M., Gustafson, E. K., Gustafson, R., Hage, B., Hall, P., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Hayau, J. -F., Hayler, T., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A. W., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Howell, E. J., Hoyland, D., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh--Dinh, T., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Jaranowski, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, H., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krause, T., Kringel, V., Krishnamurthy, S., Krishnan, B., Królak, A., Kuehn, G., Kullman, J., Kumar, R., Kwee, P., Landry, M., Lang, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Leroy, N., Letendre, N., Li, J., Li, T. G. F., Liguori, N., Lin, H., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Luan, J., Lubinski, M., Lucianetti, A., Lück, H., Lundgren, A. D., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Majorana, E., Mak, C., Maksimovic, I., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McIvor, G., McKechan, D. J. A., Meadors, G., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Mercer, R. A., Merill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mino, Y., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moraru, D., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., Mow--Lowry, C. M., Mueller, G., Mukherjee, S., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Nolting, D., Ochsner, E., O'Dell, J., Ogin, G. H., Oldenburg, R. G., O'Reilly, B., O'Shaughnessy, R., Osthelder, C., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pagliaroli, G., Palladino, L., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Pardi, S., Pareja, M., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichetti, G., Pichot, M., Pickenpack, M., Piergiovanni, F., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabeling, D. S., Radke, T., Radkins, H., Raffai, P., Rakhmanov, M., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Röver, C., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sakata, S., Sakosky, M., Salemi, F., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., Santamaría, L., Santostasi, G., Saraf, S., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shaddock, D. A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Speirits, F. C., Sperandio, L., Stein, A. J., Stein, L. C., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szokoly, G. P., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thüring, A., Titsler, C., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torre, O., Torres, C., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Trummer, J., Tseng, K., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vaishnav, B., Vajente, G., Vallisneri, M., Brand, J. F. J. van den, Broeck, C. Van Den, van der Putten, S., van der Sluys, M. V., van Veggel, A. A., Vass, S., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A. E., Vinet, J. -Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Was, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - Galaxy Astrophysics
Abstract: The gravitational-wave (GW) sky may include nearby pointlike sources as well as astrophysical and cosmological stochastic backgrounds. Since the relative strength and angular distribution of the many possible sources of GWs are not well constrained, searches for GW signals must be performed in a model-independent way. To that end we perform two directional searches for persistent GWs using data from the LIGO S5 science run: one optimized for pointlike sources and one for arbitrary extended sources. The latter result is the first of its kind. Finding no evidence to support the detection of GWs, we present 90% confidence level (CL) upper-limit maps of GW strain power with typical values between 2-20x10^-50 strain^2 Hz^-1 and 5-35x10^-49 strain^2 Hz^-1 sr^-1 for pointlike and extended sources respectively. The limits on pointlike sources constitute a factor of 30 improvement over the previous best limits. We also set 90% CL limits on the narrow-band root-mean-square GW strain from interesting targets including Sco X-1, SN1987A and the Galactic Center as low as ~7x10^-25 in the most sensitive frequency range near 160 Hz. These limits are the most constraining to date and constitute a factor of 5 improvement over the previous best limits., Comment: 10 pages, 4 figures
Published: 2011
Full Text: View/download PDF

4. Beating the spin-down limit on gravitational wave emission from the Vela pulsar

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abadie, J., Abbott, B. P., Abbott, R., Abernathy, M., Accadia, T., Acernese, F., Adams, C., Adhikari, R., Affeldt, C., Allen, B., Allen, G. S., Ceron, E. Amador, Amariutei, D., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Arai, K., Arain, M. A., Araya, M. C., Aston, S. M., Astone, P., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, D., Barnum, S., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Basti, A., Bauchrowitz, J., Bauer, Th. S., Behnke, B., Bejger, M., Beker, M. G., Bell, A. S., Belletoile, A., Belopolski, I., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Birindelli, S., Biswas, R., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Bock, O., Bodiya, T. P., Bogan, C., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, S., Bosi, L., Bouhou, B., Boyle, M., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Brummit, A., Budzyński, R., Bulik, T., Bulten, H. J., Buonanno, A., Burguet--Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cain, J., Calloni, E., Camp, J. B., Campagna, E., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C., Carbognani, F., Caride, S., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chaibi, O., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Chung, S., Clara, F., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coughlin, M., Coulon, J. -P., Coward, D. M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., Dannenberg, R., D'Antonio, S., Danzmann, K., Das, K., Dattilo, V., Daudert, B., Daveloza, H., Davier, M., Davies, G., Daw, E. J., Day, R., Dayanga, T., De Rosa, R., DeBra, D., Debreczeni, G., Degallaix, J., del Prete, M., Dent, T., Dergachev, V., DeRosa, R., DeSalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Di Palma, I., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Dorsher, S., Douglas, E. S. D., Drago, M., Drever, R. W. P., Driggers, J. C., Dumas, J. -C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Engel, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flanigan, M., Foley, S., Forsi, E., Forte, L. A., Fotopoulos, N., Fournier, J. -D., Franc, J., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoni, L., Garcia, J., Garofoli, J. A., Garufi, F., Gáspár, M. E., Gemme, G., Genin, E., Gennai, A., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gill, C., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grosso, R., Grote, H., Grunewald, S., Guidi, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Hayau, J. -F., Hayler, T., Heefner, J., Heitmann, H., Hello, P., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Hong, T., Hooper, S., Hosken, D. J., Hough, J., Howell, E. J., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Jaranowski, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Katzman, W., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Kelner, M., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, H., Kim, N., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Korth, W. Z., Kowalska, I., Kozak, D., Kringel, V., Krishnamurthy, S., Krishnan, B., Królak, A., Kuehn, G., Kumar, R., Kwee, P., Landry, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Leroy, N., Letendre, N., Li, J., Li, T. G. F., Liguori, N., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Luan, J., Lubinski, M., Lück, H., Lundgren, A. P., Macdonald, E., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Majorana, E., Maksimovic, I., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marandi, A., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McKechan, D. J. A., Meadors, G., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Mercer, R. A., Merill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Moesta, P., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morgia, A., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., Mow--Lowry, C. M., Mueller, G., Mukherjee, S., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Neri, I., Newton, G., Nishida, E., Nishizawa, A., Nocera, F., Nolting, D., Ochsner, E., O'Dell, J., Ogin, G. H., Oldenburg, R. G., O'Reilly, B., O'Shaughnessy, R., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pagliaroli, G., Palladino, L., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameswaran, A., Pardi, S., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichetti, G., Phelps, M., Pichot, M., Pickenpack, M., Piergiovanni, F., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Podkaminer, J., Poggiani, R., Pöld, J., Postiglione, F., Prato, M., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabeling, D. S., Rácz, I., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C. R., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Redwine, K., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sakata, S., Sakosky, M., Salemi, F., Salit, M., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., Santamaría, L., Santiago-Prieto, I., Santostasi, G., Saraf, S., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schlamminger, S., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Weerathunga, T. Shihan, Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Smith, R., Somiya, K., Sorazu, B., Soto, J., Speirits, F. C., Sperandio, L., Stefszky, M., Stein, A. J., Steinlechner, J., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szokoly, G. P., Tacca, M., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thüring, A., Titsler, C., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torre, O., Torres, C., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Tseng, K., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vaishnav, B., Vajente, G., Vallisneri, M., Brand, J. F. J. van den, Broeck, C. Van Den, van der Putten, S., van der Sluys, M. V., van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A. E., Vinet, J. -Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Was, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yang, H., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Buchner, S., Hotan, A., and Palfreyman, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present direct upper limits on continuous gravitational wave emission from the Vela pulsar using data from the Virgo detector's second science run. These upper limits have been obtained using three independent methods that assume the gravitational wave emission follows the radio timing. Two of the methods produce frequentist upper limits for an assumed known orientation of the star's spin axis and value of the wave polarization angle of, respectively, $1.9\ee{-24}$ and $2.2\ee{-24}$, with 95% confidence. The third method, under the same hypothesis, produces a Bayesian upper limit of $2.1\ee{-24}$, with 95% degree of belief. These limits are below the indirect {\it spin-down limit} of $3.3\ee{-24}$ for the Vela pulsar, defined by the energy loss rate inferred from observed decrease in Vela's spin frequency, and correspond to a limit on the star ellipticity of $\sim 10^{-3}$. Slightly less stringent results, but still well below the spin-down limit, are obtained assuming the star's spin axis inclination and the wave polarization angles are unknown., Comment: 37 pages, 6 figures corrected typo in the Authors field
Published: 2011
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5. Optical and infrared properties of active galactic nuclei in the Lockman Hole

Author: Rovilos, E., Fotopoulou, S., Salvato, M., Burwitz, V., Egami, E., Hasinger, G., and Szokoly, G.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the observed-frame optical, near- and mid-infrared properties of X-ray selected AGN in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogues, we assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalogue. Accurate photometry was collected for all the sources from U to 24um. We used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN. We used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, we identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared colour-colour diagrams. More specifically, the AGN dominated sources show a clear trend in the f_x/f_R vs. R-K and f_24um/f_R vs. R-K diagrams, while the hosts follow the behaviour of non X-ray detected galaxies. In the optical-near-infrared colour-magnitude diagram we see that the known trend of redder objects being more obscured in X-rays is stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN contaminating the overall colours than any evolutionary effects. Finally, we find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays., Comment: Accepted for publication in A&A
Published: 2011
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6. Search for gravitational waves from binary black hole inspiral, merger and ringdown

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abadie, J., Abbott, B. P., Abbott, R., Abernathy, M., Accadia, T., Acernese, F., Adams, C., Adhikari, R., Ajith, P., Allen, B., Allen, G. S., Ceron, E. Amador, Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Arain, M. A., Araya, M. C., Aronsson, M., Aso, Y., Aston, S. M., Astone, P., Atkinson, D., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballinger, T., Ballmer, S., Barker, D., Barnum, S., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauchrowitz, J., Bauer, Th. S., Behnke, B., Beker, M. G., Belletoile, A., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Birindelli, S., Biswas, R., Bitossi, M., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Boccara, C., Bock, O., Bodiya, T. P., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Boschi, V., Bose, S., Bosi, L., Bouhou, B., Boyle, M., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Budzyński, R., Bulik, T., Bulten, H. J., Buonanno, A., Burguet-Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cain, J., Calloni, E., Camp, J. B., Campagna, E., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C., Carbognani, F., Caride, S., Caudill, S., Cavaglia`, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chaibi, O., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Costa, C. A., Coulon, J. -P., Coward, D. M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., Dannenberg, R., D'Antonio, S., Danzmann, K., Das, K., Dattilo, V., Daudert, B., Davier, M., Davies, G., Davis, A., Daw, E. J., Day, R., Dayanga, T., De Rosa, R., DeBra, D., Debreczeni, G., Degallaix, J., del Prete, M., Dergachev, V., DeRosa, R., DeSalvo, R., Devanka, P., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Di Palma, I., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Dorsher, S., Douglas, E. S. D., Drago, M., Drever, R. W. P., Driggers, J. C., Dueck, J., Dumas, J. -C., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Ely, G., Engel, R., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flanigan, M., Flasch, K., Foley, S., Forrest, C., Forsi, E., Forte, L. A., Fotopoulos, N., Fournier, J. -D., Franc, J., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoni, L., Garofoli, J. A., Garufi, F., Gáspár, M. E., Gemme, G., Genin, E., Gennai, A., Gholami, I., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Gill, C., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grosso, R., Grote, H., Grunewald, S., Guidi, G. M., Gustafson, E. K., Gustafson, R., Hage, B., Hall, P., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Hayau, J. -F., Hayler, T., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A. W., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Howell, E. J., Hoyland, D., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Jaranowski, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, H., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krause, T., Kringel, V., Krishnamurthy, S., Krishnan, B., Królak, A., Kuehn, G., Kullman, J., Kumar, R., Kwee, P., Landry, M., Lang, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Leroy, N., Letendre, N., Li, J., Li, T. G. F., Liguori, N., Lin, H., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Luan, J., Lubinski, M., Lucianetti, A., Lück, H., Lundgren, A. D., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Majorana, E., Mak, C., Maksimovic, I., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McIvor, G., McKechan, D. J. A., Meadors, G., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Mercer, R. A., Merill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mino, Y., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moraru, D., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., Mow-Lowry, C. M., Mueller, G., Mukherjee, S., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Nolting, D., Ochsner, E., O'Dell, J., Ogin, G. H., Oldenburg, R. G., O'Reilly, B., O'Shaughnessy, R., Osthelder, C., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pagliaroli, G., Palladino, L., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Pardi, S., Pareja, M., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichetti, G., Pichot, M., Pickenpack, M., Piergiovanni, F., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabeling, D. S., Rácz, I., Radke, T., Radkins, H., Raffai, P., Rakhmanov, M., Rankins, B., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sakata, S., Sakosky, M., Salemi, F., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., Santamaría, L., Santostasi, G., Saraf, S., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shaddock, D. A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Speirits, F. C., Sperandio, L., Stein, A. J., Stein, L. C., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A. S., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szokoly, G. P., Tacca, M., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thüring, A., Titsler, C., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torre, O., Torres, C., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Tseng, K., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vaishnav, B., Vajente, G., Vallisneri, M., Brand, J. F. J. van den, Broeck, C. Van Den, van der Putten, S., van der Sluys, M. V., van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A. E., Vinet, J. -Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Was, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., and Zweizig, J.
Subjects: General Relativity and Quantum Cosmology
Abstract: We present the first modeled search for gravitational waves using the complete binary black hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched approximately 2 years of LIGO data taken between November 2005 and September 2007 for systems with component masses of 1-99 solar masses and total masses of 25-100 solar masses. We did not detect any plausible gravitational-wave signals but we do place upper limits on the merger rate of binary black holes as a function of the component masses in this range. We constrain the rate of mergers for binary black hole systems with component masses between 19 and 28 solar masses and negligible spin to be no more than 2.0 per Mpc^3 per Myr at 90% confidence., Comment: 19 pages, 3 figures
Published: 2011
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7. Search for Gravitational Wave Bursts from Six Magnetars

Author: Abadie, J., Abbott, B. P., Abbott, R., Abernathy, M., Accadia, T., Acerneseac, F., Adams, C., Adhikari, R., Affeldt, C., Allen, B., Allen, G. S., Ceron, E. Amador, Amariutei, D., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonuccia, F., Arai, K., Arain, M. A., Araya, M. C., Aston, S. M., Astonea, P., Atkinson, D., Aufmuth, P., Aulbert, C., Aylott, B. E., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, D., Barnum, S., Baroneac, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bastiab, A., Bauchrowitz, J., Bauera, Th. S., Behnke, B., Bekera, M. G., Bell, A. S., Belletoile, A., Belopolski, I., Benacquista, M., Bertolini, A., Betzwieser, J., Beveridge, N., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Birch, J., Birindellia, S., Biswas, R., Bitossia, M., Bizouarda, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Bloma, M., Bock, O., Bodiya, T. P., Bogan, C., Bondarescu, R., Bondub, F., Bonelliab, L., Bonnand, R., Bork, R., Born, M., Boschia, V., Bose, S., Bosia, L., Bouhou, B., Boyle, M., Braccinia, S., Bradaschiaa, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brilleta, A., Brinkmann, M., Brissona, V., Britzger, M., Brooks, A. F., Brown, D. A., Brummit, A., Budzyńskib, R., Bulikbc, T., Bultenab, H. J., Buonanno, A., Burguet--Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnolia, G., Cain, J., Calloniab, E., Camp, J. B., Campagnaab, E., Campsie, P., Cannizzo, J., Cannon, K., Canuel, B., Cao, J., Capano, C., Carbognani, F., Caride, S., Caudill, S., Cavaglià, M., Cavaliera, F., Cavalieri, R., Cellaa, G., Cepeda, C., Cesarinib, E., Chaibia, O., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Chung, S., Clara, F., Clark, D., Clark, J., Clayton, J. H., Clevaa, F., Cocciaab, E., Colacinoab, C. N., Colas, J., Collaab, A., Colombinib, M., Conte, R., Cook, D., Corbitt, T. R., Cornish, N., Corsia, A., Costa, C. A., Coughlin, M., Coulona, J. -P., Coward, D. M., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., Dannenberg, R., D'Antonioa, S., Danzmann, K., Das, K., Dattilo, V., Daudert, B., Daveloza, H., Daviera, M., Davies, G., Daw, E. J., Day, R., Dayanga, T., De Rosaab, R., DeBra, D., Debreczeni, G., Degallaix, J., del Preteac, M., Dent, T., Dergachev, V., DeRosa, R., DeSalvo, R., Dhurandhar, S., Di Fiorea, L., Di Lietoab, A., Di Palma, I., Emilioac, M. Di Paolo, Di Virgilioa, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Dorsher, S., Douglas, E. S. D., Dragocd, M., Drever, R. W. P., Driggers, J. C., Dumas, J. -C., Dwyer, S., Eberle, T., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Engel, R., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafoneab, V., Fairhurst, S., Fan, Y., Farr, B. F., Fazi, D., Fehrmann, H., Feldbaum, D., Ferranteab, I., Fidecaroab, F., Finn, L. S., Fiori, I., Flaminio, R., Flanigan, M., Foley, S., Forsi, E., Fortea, L. A., Fotopoulos, N., Fourniera, J. -D., Franc, J., Frascaab, S., Frasconia, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoniab, L., Garcia, J., Garofoli, J. A., Garufiab, F., Gáspár, M. E., Gemme, G., Genin, E., Gennaia, A., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazottoa, A., Gill, C., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Greveriea, C., Grosso, R., Grote, H., Grunewald, S., Guidiab, G. M., Guido, C., Gupta, R., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G., Hanks, J., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Hartman, M. T., Haughian, K., Hayama, K., Hayaub, J. -F., Hayler, T., Heefner, J., Heitmann, H., Helloa, P., Hendry, M. A., Heng, I. S., Heptonstall, A. W., Herrera, V., Hewitson, M., Hild, S., Hoak, D., Hodge, K. A., Holt, K., Hong, T., Hooper, S., Hosken, D. J., Hough, J., Howell, E. J., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Inta, R., Isogai, T., Ivanov, A., Jaranowskid, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J. B., Katsavounidis, E., Katzman, W., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Kelner, M., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khazanov, E. A., Kim, H., Kim, N., King, P. J., Kinzel, D. L., Kissel, J. S., Klimenko, S., Kondrashov, V., Kopparapu, R., Koranda, S., Korth, W. Z., Kowalskab, I., Kozak, D., Kringel, V., Krishnamurthy, S., Krishnan, B., Królakae, A., Kuehn, G., Kumar, R., Kwee, P., Landry, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Leong, J., Leonor, I., Leroya, N., Letendre, N., Li, J., Lia, T. G. F., Liguoriab, N., Lindquist, P. E., Lockerbie, N. A., Lodhia, D., Lorenzinia, M., Lorietteb, V., Lormand, M., Losurdoa, G., Lu, P., Luan, J., Lubinski, M., Lück, H., Lundgren, A. P., Macdonald, E., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Majoranaa, E., Maksimovicb, I., Mana, N., Mandel, I., Mandic, V., Mantovaniac, M., Marandi, A., Marchesonia, F., Marion, F., Márka, S., Márka, Z., Maros, E., Marque, J., Martelliab, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McKechan, D. J. A., Meadors, G., Mehmet, M., Meier, T., Melatos, A., Melissinos, A. C., Mendell, G., Mercer, R. A., Merill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milanoab, L., Miller, J., Minenkova, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Moesta, P., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moraru, D., Moreno, G., Morgado, N., Morgiaab, A., Moscaab, S., Moscatellia, V., Mossavi, K., Mours, B., Mow--Lowry, C. M., Mueller, G., Mukherjee, S., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Neriab, I., Newton, G., Nishida, E., Nishizawa, A., Nocera, F., Nolting, D., Ochsner, E., O'Dell, J., Ogin, G. H., Oldenburg, R. G., O'Reilly, B., O'Shaughnessy, R., Osthelder, C., Ott, C. D., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pagliaroliac, G., Palladinoac, L., Palombaa, C., Pan, Y., Pankow, C., Paolettia, F., Papa, M. A., Parameswaran, A., Pardiab, S., Parisiab, M., Pasqualetti, A., Passaquietiab, R., Passuelloa, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichettiab, G., Phelps, M., Pichota, M., Pickenpack, M., Piergiovanniab, F., Pietkad, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Podkaminer, J., Poggianiab, R., Pöld, J., Postiglione, F., Prato, M., Predoi, V., Price, L. R., Prijatelj, M., Principe, M., Privitera, S., Prix, R., Prodiab, G. A., Prokhorov, L., Puncken, O., Punturoa, M., Puppoa, P., Quetschke, V., Raab, F. J., Rabelingab, D. S., Rácz, I., Radkins, H., Raffai, P., Rakhmanov, M., Ramet, C. R., Rankins, B., Rapagnaniab, P., Raymond, V., Reab, V., Redwine, K., Reed, C. M., Reed, T., Regimbaua, T., Reid, S., Reitze, D. H., Ricciab, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robineta, F., Robinson, C., Robinson, E. L., Rocchia, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romanoac, R., Romie, J. H., Rosińskacf, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sakata, S., Sakosky, M., Salemi, F., Salit, M., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., Santamaría, L., Santiago-Prieto, I., Santostasi, G., Saraf, S., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schlamminger, S., Schnabel, R., Schofield, R. M. S., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shaddock, D. A., Shaltev, M., Shapiro, B., Shawhan, P., Weerathunga, T. Shihan, Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Singer, A., Singer, L., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Smith, R., Somiya, K., Sorazu, B., Soto, J., Speirits, F. C., Sperandioab, L., Stefszky, M., Stein, A. J., Steinlechner, J., Steinlechner, S., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A. S., Sturaniab, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szokoly, G. P., Tacca, M., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thomas, P., Thorne, K. A., Thorne, K. S., Thrane, E., Thüring, A., Titsler, C., Tokmakov, K. V., Toncelliab, A., Tonelliab, M., Torreac, O., Torres, C., Torrie, C. I., Tournefier, E., Travassoab, F., Traylor, G., Trias, M., Tseng, K., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vaishnav, B., Vajenteab, G., Vallisneri, M., Brandab, J. F. J. van den, Broeck, C. Van Den, van der Puttena, S., van der Sluys, M. V., van Veggel, A. A., Vass, S., Vasuth, M., Vaulin, R., Vavoulidisa, M., Vecchio, A., Vedovatoc, G., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetranoab, F., Viceréab, A., Villar, A. E., Vineta, J. -Y., Voccaa, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Wasa, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., White, D., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yablon, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yang, H., Yeaton-Massey, D., Yoshida, S., Yu, P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Aptekar, R. L., Boynton, W. V., Briggs, M. S., Cline, T. L., Connaughton, V., Frederiks, D. D., Gehrels, N., Goldsten, J. O, Golovin, D., van der Horst, A. J., Hurley, K. C., Kaneko, Y., von Kienlin, A., Kouveliotou, C., Krimm, H. A., Lin, L., Mitrofanov, I., Ohno, M., Palshin, V. D., Rau, A., Sanin, A., Tashiro, M. S., Terada, Y., and Yamaoka, K.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely ~1 kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >10^{44} erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between November 2006 and June 2009, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band- and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090 Hz), are 3.0x10^{44} d_1^2 erg and 1.4x10^{47} d_1^2 erg respectively, where d_1 = d_{0501} / 1 kpc and d_{0501} is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time., Comment: 9 pages, 3 figures; v2 minor clarifications and new references
Published: 2010
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8. A search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar

Author: The LIGO Scientific Collaboration, Abadie, J., Abbott, B. P., Abbott, R., Adhikari, R., Ajith, P., Allen, B., Allen, G., Ceron, E. Amador, Amin, R. S., Anderson, S. B., Anderson, W. G., Arain, M. A., Araya, M., Aso, Y., Aston, S., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballmer, S., Barker, D., Barr, B., Barriga, P., Barsotti, L., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Behnke, B., Benacquista, M., Bennett, M. F., Betzwieser, J., Beyersdorf, P. T., Bilenko, I. A., Billingsley, G., Biswas, R., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Bock, O., Bodiya, T. P., Bondarescu, R., Bork, R., Born, M., Bose, S., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brinkmann, M., Britzger, M., Brooks, A. F., Brown, D. A., Buchner, S., Bullington, A., Buonanno, A., Burmeister, O., Byer, R. L., Cadonati, L., Cain, J., Camp, J. B., Cannizzo, J., Cannon, K. C., Cao, J., Capano, C., Cardenas, L., Caudill, S., Cavaglià, M., Cepeda, C., Chalermsongsak, T., Chalkley, E., Charlton, P., Chatterji, S., Chelkowski, S., Chen, Y., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Conte, R., Cook, D., Corbitt, T. R. C., Cornish, N., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Dahl, K., Danilishin, S. L., Danzmann, K., Daudert, B., Davies, G., Daw, E. J., Dayanga, T., DeBra, D., Degallaix, J., Dergachev, V., DeSalvo, R., Dhurandhar, S., Díaz, M., Donovan, F., Dooley, K. L., Doomes, E. E., Drever, R. W. P., Driggers, J., Dueck, J., Duke, I., Dumas, J. -C., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Etzel, T., Evans, M., Evans, T., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Finn, L. S., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Garofoli, J. A., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Goetz, E., Goggin, L. M., González, G., Goßler, S., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Grosso, R., Grote, H., Grunewald, S., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Hayler, T., Heefner, J., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Howell, E., Hoyland, D., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Isogai, T., Ivanov, A., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., Kim, H., King, P. J., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kozak, D., Kringel, V., Krishnan, B., Kuehn, G., Kullman, J., Kumar, R., Kwee, P., Lam, P. K., Landry, M., Lang, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Lei, M., Leindecker, N., Leonor, I., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Lormand, M., Lu, P., Lubinski, M., Lucianetti, A., Lück, H., Lundgren, A., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Mak, C., Mandel, I., Mandic, V., Márka, S., Márka, Z., Markosyan, A., Markowitz, J., Maros, E., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McKechan, D. J. A., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Mercer, R. A., Merrill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Miller, J., Mino, Y., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohanty, S. D., Mohapatra, S. R. P., Moreno, G., Mors, K., Mossavi, K., MowLowry, C., Mueller, G., Müller-Ebhardt, H., Mukherjee, S., Mullavey, A., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Newton, G., Nishida, E., Nishizawa, A., O'Dell, J., O'Reilly, B., O'Shaughnessy, R., Ochsner, E., Ogin, G. H., Oldenburg, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pan, Y., Pankow, C., Papa, M. A., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Pickenpack, M., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Postiglione, F., Principe, M., Prix, R., Prokhorov, L., Puncken, O., Quetschke, V., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rakhmanov, M., Raymond, V., Reed, C. M., Reed, T., Rehbein, H., Reid, S., Reitze, D. H., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinson, C., Robinson, E. L., Roddy, S., Röver, C., Rollins, J., Romano, J. D., Romie, J. H., Rowan, S., Rüdiger, A., Ryan, K., Sakata, S., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., Santamaría, L., Santostasi, G., Saraf, S., Sarin, P., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schnabel, R., Schofield, R., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sergeev, A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Speirits, F., Stein, A. J., Stein, L. C., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Szokoly, G. P., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thorne, K. A., Thorne, K. S., Thüring, A., Titsler, C., Tokmakov, K. V., Torres, C., Torrie, C. I., Traylor, G., Trias, M., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vallisneri, M., Broeck, C. Van Den, van der Sluys, M. V., van Veggel, A. A., Vass, S., Vaulin, R., Vecchio, A., Veitch, J., Veitch, P. J., Veltkamp, C., Villar, A., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Wilmut, I., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yeaton-Massey, D., Yoshida, S., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., and Zweizig, J.
Subjects: General Relativity and Quantum Cosmology, Astrophysics - Solar and Stellar Astrophysics
Abstract: The physical mechanisms responsible for pulsar timing glitches are thought to excite quasi-normal mode oscillations in their parent neutron star that couple to gravitational wave emission. In August 2006, a timing glitch was observed in the radio emission of PSR B0833-45, the Vela pulsar. At the time of the glitch, the two co-located Hanford gravitational wave detectors of the Laser Interferometer Gravitational-wave observatory (LIGO) were operational and taking data as part of the fifth LIGO science run (S5). We present the first direct search for the gravitational wave emission associated with oscillations of the fundamental quadrupole mode excited by a pulsar timing glitch. No gravitational wave detection candidate was found. We place Bayesian 90% confidence upper limits of 6.3e-21 to 1.4e-20 on the peak intrinsic strain amplitude of gravitational wave ring-down signals, depending on which spherical harmonic mode is excited. The corresponding range of energy upper limits is 5.0e44 to 1.3e45 erg., Comment: 13 pages, 5 figures
Published: 2010
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9. The Extended Chandra Deep Field-South Survey: Optical spectroscopy of faint X-ray sources with the VLT and Keck

Author: Silverman, J. D., Mainieri, V., Salvato, M., Hasinger, G., Bergeron, J., Capak, P., Szokoly, G., Finoguenov, A., Gilli, R., Rosati, P., Tozzi, P., Vignali, C., Alexander, D. M., Brandt, W. N., Lehmer, B. D., Luo, B., Rafferty, D., Xue, Y. Q., Balestra, I., Bauer, F. E., Brusa, M., Comastri, A., Kartaltepe, J., Koekemoer, A. M., Miyaji, T., Schneider, D. P., Treister, E., Wisotski, L., and Schramm, M.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results of a program to acquire high-quality optical spectra of X-ray sources detected in the E-CDF-S and its central area. New spectroscopic redshifts are measured for 283 counterparts to Chandra sources with deep exposures (t~2-9 hr per pointing) using multi-slit facilities on both the VLT and Keck thus bringing the total number of spectroscopically-identified X-ray sources to over 500 in this survey field. We provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, and redshifts (both spectroscopic and photometric) that incorporate published spectroscopic catalogs thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. We demonstrate the remarkable coverage of the Lx-z plane now accessible from our data while emphasizing the detection of AGNs that contribute to the faint end of the luminosity function at 1.5
Published: 2010
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10. The Swift/Fermi GRB 080928 from 1 eV to 150 keV

Author: Rossi, A., Schulze, S., Klose, S., Kann, D. A., Rau, A., Krimm, H. A., Jóhannesson, G., Panaitescu, A., Yuan, F., Ferrero, P., Krühler, T., Greiner, J., Schady, P., Pandey, S. B., Amati, L., Afonso, P. M. J., Akerlof, C. W., Arnold, L., Clemens, C., Filgas, R., Hartmann, D. H., Yoldaş, A. Küpcü, McBreen, S., McKay, T. A., Guelbenzu, A. Nicuesa, E., F. Olivares, Paciesas, B., Rykoff, E. S., Szokoly, G., Updike, A. C., and Yoldaş, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present the results of a comprehensive study of the gamma-ray burst 080928 and of its afterglow. GRB 080928 was a long burst detected by Swift/BAT and Fermi/GBM. It is one of the exceptional cases where optical emission had already been detected when the GRB itself was still radiating in the gamma-ray band. For nearly 100 seconds simultaneous optical, X-ray and gamma-ray data provide a coverage of the spectral energy distribution of the transient source from about 1 eV to 150 keV. In particular, we show that the SED during the main prompt emission phase agrees with synchrotron radiation. We constructed the optical/near-infrared light curve and the spectral energy distribution based on Swift/UVOT, ROTSE-IIIa (Australia), and GROND (La Silla) data and compared it to the X-ray light curve retrieved from the Swift/XRT repository. We show that its bumpy shape can be modeled by multiple energy-injections into the forward shock.Furthermore, we investigate whether the temporal and spectral evolution of the tail emission of the first strong flare seen in the early X-ray light curve can be explained by large-angle emission (LAE). We find that a nonstandard LAE model is required to explain the observations. Finally, we report on the results of our search for the GRB host galaxy, for which only a deep upper limit can be provided., Comment: A&A, in press (including revisions according to the language editor), 14 pages, 11 figures, 7 tables; Online Appendix: 4 pages, 1 figure, 4 tables; v4: final journal version to be published soon
Published: 2010
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11. Optical and near-infrared follow-up observations of four Fermi/LAT GRBs : Redshifts, afterglows, energetics and host galaxies

Author: McBreen, S., Krühler, T., Rau, A., Greiner, J., Kann, D. A., Savaglio, S., Afonso, P., Clemens, C., Filgas, R., Klose, S., Yoldas, A. Küpüc, E., F. Olivares, Rossi, A., Szokoly, G. P., Updike, A., and Yoldas, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Fermi can measure the spectral properties of gamma-ray bursts over a very large energy range and is opening a new window on the prompt emission of these energetic events. Localizations by the instruments on Fermi in combination with follow-up by Swift provide accurate positions for observations at longer wavelengths leading to the determination of redshifts, the true energy budget, host galaxy properties and facilitate comparison with pre-Fermi bursts. Multi-wavelength follow-up observations were performed on the afterglows of four bursts with high energy emission detected by Fermi/LAT : GRB090323, GRB090328, GRB090510 and GRB090902B. They were obtained in the optical/near-infrared bands with GROND mounted at the MPG/ESO 2.2m telescope and additionally of GRB090323 in the optical with the 2 m telescope in Tautenburg, Germany. Three of the events are classified as long bursts while GRB090510 is a well localized short GRB with GeV emission. In addition, host galaxies were detected for three of the four bursts. Spectroscopic follow-up was initiated with the VLT for GRB090328 and GRB090510. The afterglow observations in 7 bands are presented for all bursts and their host galaxies are investigated. Knowledge of the distance and the local dust extinction enables comparison of the afterglows of LAT-detected GRBs with the general sample. The spectroscopic redshifts of GRB090328 and GRB090510 were determined to be z=0.7354+/-0.0003 and z=0.903 +/- 0.001 and dust corrected star-formation rates of 4.8 Mdot yr^-1 and 0.60 M_dot yr^-1 were derived for their host galaxies, respectively. The afterglows of long bursts exhibit power-law decay indices alpha from less than 1 to ~2.3 and spectral indices (beta) values from 0.65 to ~1.2 which are fairly standard for GRB afterglows. Constraints are placed on the jet half opening angles of less than 2.1 deg to greater than 6.4 deg which allows limits to be placed on the beaming corrected energies. These range from less than 5x10^50 erg to the one of the highest values ever recorded, greater than 2.2x10^52 erg for GRB090902B, and are not consistent with a standard candle. The extremely energetic long Fermi bursts have optical afterglows which lie in the top half of the brightness distribution of all optical afterglows detected in the Swift era or even in the top 5% if incompleteness is considered. The properties of the host galaxies of these LAT detected bursts in terms of extinction, star formation rates and masses do not appear to differ from previous samples., Comment: Accepted for publication in Astronomy and Astrophysics. 16 pages, 14 figures.
Published: 2010
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12. Search for gravitational-wave inspiral signals associated with short Gamma-Ray Bursts during LIGO's fifth and Virgo's first science run

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abadie, J., Abbott, B. P., Abbott, R., Accadia, T., Acernese, F., Adhikari, R., Ajith, P., Allen, B., Allen, G., Ceron, E. Amador, Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Aoudia, S., Arain, M. A., Araya, M., Arun, K. G., Aso, Y., Aston, S., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, D., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauer, Th. S., Behnke, B., Beker, M. G., Belletoile, A., Benacquista, M., Betzwieser, J., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birindelli, S., Biswas, R., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Blom, M., Boccara, C., Bock, O., Bodiya, T. P., Bondarescu, R., Bondu, F., Bonelli, L., Bonnand, R., Bork, R., Born, M., Bose, S., Bosi, L., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Breyer, J., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Britzger, M., Brooks, A. F., Brown, D. A., Budzyński, R., Bulik, T., Bullington, A., Bulten, H. J., Buonanno, A., Burguet-Castell, J., Burmeister, O., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cain, J., Calloni, E., Camp, J. B., Campagna, E., Cannizzo, J., Cannon, K. C., Canuel, B., Cao, J., Capano, C. D., Carbognani, F., Cardenas, L., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chatterji, S., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chua, S. S. Y., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R. C., Cornish, N., Corsi, A., Coulon, J. -P., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Dahl, K., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dattilo, V., Daudert, B., Davier, M., Davies, G., Daw, E. J., Day, R., Dayanga, T., De Rosa, R., DeBra, D., Degallaix, J., del Prete, M., Dergachev, V., DeSalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Drago, M., Drever, R. W. P., Driggers, J., Dueck, J., Duke, I., Dumas, J. -C., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Fournier, J. -D., Franc, J., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T. T., Friedrich, D., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Galimberti, M., Gammaitoni, L., Garofoli, J. A., Garufi, F., Gemme, G., Genin, E., Gennai, A., Ghosh, S., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Goetz, E., Goggin, L. M., González, G., Goßler, S., Gouaty, R., Granata, M., Grant, A., Gras, S., Gray, C., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grosso, R., Grote, H., Grunewald, S., Guidi, G. M., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Hayler, T., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Howell, E., Hoyland, D., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Ingram, D. R., Isogai, T., Ivanov, A., Jaranowski, P., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., Kim, H., King, P. J., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Kringel, V., Krishnan, B., Królak, A., Kuehn, G., Kullman, J., Kumar, R., Kwee, P., Lam, P. K., Landry, M., Lang, M., Lantz, B., Lastzka, N., Lazzarini, A., Leaci, P., Lei, M., Leindecker, N., Leonor, I., Leroy, N., Letendre, N., Li, T. G. F., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Lubinski, M., Lucianetti, A., Lück, H., Lundgren, A., Machenschalk, B., MacInnis, M., Mageswaran, M., Mailand, K., Majorana, E., Mak, C., Maksimovic, I., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Markowitz, J., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McIntyre, G., McKechan, D. J. A., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Mercer, R. A., Merill, L., Meshkov, S., Messenger, C., Meyer, M. S., Miao, H., Michel, C., Milano, L., Miller, J., Minenkov, Y., Mino, Y., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., MowLowry, C., Mueller, G., Mukherjee, S., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Nash, T., Nawrodt, R., Nelson, J., Neri, I., Newton, G., Nishida, E., Nishizawa, A., Nocera, F., Ochsner, E., O'Dell, J., Ogin, G. H., Oldenburg, R., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Page, A., Pagliaroli, G., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Pardi, S., Parisi, M., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pathak, D., Pedraza, M., Pekowsky, L., Penn, S., Peralta, C., Perreca, A., Persichetti, G., Pichot, M., Pickenpack, M., Piergiovanni, F., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Predoi, V., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rakhmanov, M., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Rehbein, H., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Röver, C., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Rowan, S., Rüdiger, A., Ruggi, P., Ryan, K., Sakata, S., Salemi, F., Sammut, L., de la Jordana, L. Sancho, Sandberg, V., Sannibale, V., Santamaría, L., Santostasi, G., Saraf, S., Sarin, P., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Schilling, R., Schnabel, R., Schofield, R., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sintes, A. M., Skelton, G., Slagmolen, B. J. J., Slutsky, J., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Stein, A. J., Stein, L. C., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sung, M., Susmithan, S., Sutton, P. J., Swinkels, B., Szokoly, G. P., Talukder, D., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Thorne, K. A., Thorne, K. S., Thüring, A., Titsler, C., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torres, C., Torrie, C. I., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Trummer, J., Turner, L., Ugolini, D., Urbanek, K., Vahlbruch, H., Vajente, G., Vallisneri, M., Brand, J. F. J. van den, Broeck, C. Van Den, van der Putten, S., van der Sluys, M. V., Vass, S., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., van Veggel, A. A., Veitch, J., Veitch, P. J., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A., Vinet, J. -Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Wanner, A., Ward, R. L., Was, M., Wei, P., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wessels, P., West, M., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Wilmut, I., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Yakushin, I., Yamamoto, H., Yamamoto, K., Yeaton-Massey, D., Yoshida, S., Yu, P. P., Yvert, M., Zanolin, M., Zhang, L., Zhang, Z., Zhao, C., Zotov, N., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Progenitor scenarios for short gamma-ray bursts (short GRBs) include coalescenses of two neutron stars or a neutron star and black hole, which would necessarily be accompanied by the emission of strong gravitational waves. We present a search for these known gravitational-wave signatures in temporal and directional coincidence with 22 GRBs that had sufficient gravitational-wave data available in multiple instruments during LIGO's fifth science run, S5, and Virgo's first science run, VSR1. We find no statistically significant gravitational-wave candidates within a [-5, +1) s window around the trigger time of any GRB. Using the Wilcoxon-Mann-Whitney U test, we find no evidence for an excess of weak gravitational-wave signals in our sample of GRBs. We exclude neutron star-black hole progenitors to a median 90% CL exclusion distance of 6.7 Mpc., Comment: 8 pages, 2 figures, Accepted by ApJ
Published: 2010
Full Text: View/download PDF

13. Searches for gravitational waves from known pulsars with S5 LIGO data

Author: The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Acernese, F., Adhikari, R., Ajith, P., Allen, B., Allen, G., Alshourbagy, M., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Aoudia, S., Arain, M. A., Araya, M., Armandula, H., Armor, P., Arun, K. G., Aso, Y., Aston, S., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, C., Barker, D., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauer, Th. S., Behnke, B., Beker, M., Benacquista, M., Betzwieser, J., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birindelli, S., Biswas, R., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Boccara, C., Bodiya, T. P., Bogue, L., Bondu, F., Bonelli, L., Bork, R., Boschi, V., Bose, S., Bosi, L., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Broeck, C. Van Den, Brooks, A. F., Brown, D. A., Brummit, A., Brunet, G., Budzynski, R., Bulik, T., Bullington, A., Bulten, H. J., Buonanno, A., Burmeister, O., Buskulic, D., Byer, R. L., Cadonati, L., Cagnoli, G., Calloni, E., Camp, J. B., Campagna, E., Cannizzo, J., Cannon, K. C., Canuel, B., Cao, J., Carbognani, F., Cardenas, L., Caride, S., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chatterji, S., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Cokelaer, T., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R. C., Corda, C., Cornish, N., Corsi, A., Coulon, J. -P., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dari, A., Dattilo, V., Daudert, B., Davier, M., Davies, G., Daw, E. J., Day, R., De Rosa, R., DeBra, D., Degallaix, J., del Prete, M., Dergachev, V., Desai, S., DeSalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Drago, M., Drever, R. W. P., Dueck, J., Duke, I., Dumas, J. -C., Dwyer, J. G., Echols, C., Edgar, M., Effler, A., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Fournier, J. -D., Franc, J., Franzen, A., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T., Fritschel, P., Frolov, V. V., Fyffe, M., Galdi, V., Gammaitoni, L., Garofoli, J. A., Garufi, F., Gemme, G., Genin, E., Gennai, A., Gholami, I., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Goda, K., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goßler, S., Gouaty, R., Granata, M., Granata, V., Grant, A., Gras, S., Gray, C., Gray, M., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grimaldi, F., Grosso, R., Grote, H., Grunewald, S., Guenther, M., Guidi, G., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Hoyland, D., Huet, D., Hughey, B., Huttner, S. H., Ingram, D. R., Isogai, T., Ito, M., Ivanov, A., Jaranowski, P., Johnson, B., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., de la Jordana, L. Sancho, Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Kasprzyk, D., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., King, P., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krishnan, B., Królak, A., Kumar, R., Kwee, P., La Penna, P., Lam, P. K., Landry, M., Lantz, B., Lazzarini, A., Lei, H., Lei, M., Leindecker, N., Leonor, I., Leroy, N., Letendre, N., Li, C., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Longo, M., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Lubinski, M., Lucianetti, A., Lück, H., Machenschalk, B., MacInnis, M., Mackowski, J. -M., Mageswaran, M., Mailand, K., Majorana, E., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Markowitz, J., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McHugh, M., McIntyre, G., McKechan, D. J. A., McKenzie, K., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Menzinger, F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Michel, C., Milano, L., Miller, J., Minelli, J., Minenkov, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., MowLowry, C., Mueller, G., Muhammad, D., Mühlen, H. zur, Mukherjee, S., Mukhopadhyay, H., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Myers, E., Myers, J., Nash, T., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Numata, K., Ochsner, E., O'Dell, J., Ogin, G. H., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pagliaroli, G., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameshwaraiah, V., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Pichot, M., Piergiovanni, F., Pierro, V., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabaste, O., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rainer, N., Rakhmanov, M., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Rehbein, H., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Rivera, B., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosinska, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Russell, P., Ryan, K., Sakata, S., Salemi, F., Sandberg, V., Sannibale, V., Santamaría, L., Saraf, S., Sarin, P., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Savov, P., Scanlan, M., Schilling, R., Schnabel, R., Schofield, R., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Sears, B., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sinha, S., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., van der Sluys, M. V., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Stein, A., Stein, L. C., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, K. -X., Sung, M., Sutton, P. J., Swinkels, B., Szokoly, G. P., Talukder, D., Tang, L., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Terenzi, R., Thacker, J., Thorne, K. A., Thorne, K. S., Thüring, A., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torres, C., Torrie, C., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Trummer, J., Ugolini, D., Ulmen, J., Urbanek, K., Vahlbruch, H., Vajente, G., Vallisneri, M., Brand, J. F. J. van den, van der Putten, S., Vass, S., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., van Veggel, A. A., Veitch, J., Veitch, P., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A., Vinet, J. -Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Ward, R. L., Was, M., Weidner, A., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Wilmut, I., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Wu, W., Yakushin, I., Yamamoto, H., Yan, Z., Yoshida, S., Yvert, M., Zanolin, M., Zhang, J., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., Zweizig, J., Bégin, S., Corongiu, A., D'Amico, N., Freire, P. C. C., Hessels, J. W. T., Hobbs, G. B., Kramer, M., Lyne, A. G., Manchester, R. N., Marshall, F. E., Middleditch, J., Possenti, A., Ransom, S. M., Stairs, I. H., and Stappers, B.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Galaxy Astrophysics, General Relativity and Quantum Cosmology
Abstract: We present a search for gravitational waves from 116 known millisecond and young pulsars using data from the fifth science run of the LIGO detectors. For this search ephemerides overlapping the run period were obtained for all pulsars using radio and X-ray observations. We demonstrate an updated search method that allows for small uncertainties in the pulsar phase parameters to be included in the search. We report no signal detection from any of the targets and therefore interpret our results as upper limits on the gravitational wave signal strength. The most interesting limits are those for young pulsars. We present updated limits on gravitational radiation from the Crab pulsar, where the measured limit is now a factor of seven below the spin-down limit. This limits the power radiated via gravitational waves to be less than ~2% of the available spin-down power. For the X-ray pulsar J0537-6910 we reach the spin-down limit under the assumption that any gravitational wave signal from it stays phase locked to the X-ray pulses over timing glitches, and for pulsars J1913+1011 and J1952+3252 we are only a factor of a few above the spin-down limit. Of the recycled millisecond pulsars several of the measured upper limits are only about an order of magnitude above their spin-down limits. For these our best (lowest) upper limit on gravitational wave amplitude is 2.3x10^-26 for J1603-7202 and our best (lowest) limit on the inferred pulsar ellipticity is 7.0x10^-8 for J2124-3358., Comment: 39 pages, 5 figures, Accepted in The Astrophysical Journal
Published: 2009
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14. Deep U-B-V imaging of the Lockman Hole with the LBT. Observations and number counts

Author: Rovilos, E., Burwitz, V., Szokoly, G., Hasinger, G., Egami, E., Bouche, N., Berta, S., Salvato, M., Lutz, D., and Genzel, R.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We used the large binocular camera (LBC) mounted on the large binocular telescope (LBT) to observe the Lockman Hole in the U, B, and V bands. Our observations cover an area of 925 sq.arcmin. We reached depths of 26.7, 26.3, and 26.3 mag(AB) in the three bands, respectively, in terms of 50% source detection efficiency, making this survey the deepest U-band survey and one of the deepest B and V band surveys with respect to its covered area. We extracted a large number of sources (~89000), detected in all three bands and examined their surface density, comparing it with models of galaxy evolution. We find good agreement with previous claims of a steep faint-end slope of the luminosity functions, caused by late-type and irregular galaxies at z>1.5. A population of dwarf star-forming galaxies at 1.5
Published: 2009
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15. Search for gravitational-wave bursts associated with gamma-ray bursts using data from LIGO Science Run 5 and Virgo Science Run 1

Author: LIGO Scientific Collaboration, Virgo Collaboration, Abbott, B. P., Abbott, R., Acernese, F., Adhikari, R., Ajith, P., Allen, B., Allen, G., Alshourbagy, M., Amin, R. S., Anderson, S. B., Anderson, W. G., Antonucci, F., Aoudia, S., Arain, M. A., Araya, M., Armandula, H., Armor, P., Arun, K. G., Aso, Y., Aston, S., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Baker, P., Ballardin, G., Ballmer, S., Barker, C., Barker, D., Barone, F., Barr, B., Barriga, P., Barsotti, L., Barsuglia, M., Barton, M. A., Bartos, I., Bassiri, R., Bastarrika, M., Bauer, Th. S., Behnke, B., Beker, M., Benacquista, M., Betzwieser, J., Beyersdorf, P. T., Bigotta, S., Bilenko, I. A., Billingsley, G., Birindelli, S., Biswas, R., Bizouard, M. A., Black, E., Blackburn, J. K., Blackburn, L., Blair, D., Bland, B., Boccara, C., Bodiya, T. P., Bogue, L., Bondu, F., Bonelli, L., Bork, R., Boschi, V., Bose, S., Bosi, L., Braccini, S., Bradaschia, C., Brady, P. R., Braginsky, V. B., Brau, J. E., Bridges, D. O., Brillet, A., Brinkmann, M., Brisson, V., Broeck, C. Van Den, Brooks, A. F., Brown, D. A., Brummit, A., Brunet, G., Budzyński, R., Bulik, T., Bullington, A., Bulten, H. J., Buonanno, A., Burmeister, O., Buskulic, D., Byer, R. L., Cadonati, L., Cagnoli, G., Calloni, E., Camp, J. B., Campagna, E., Cannizzo, J., Cannon, K. C., Canuel, B., Cao, J., Carbognani, F., Cardenas, L., Caride, S., Castaldi, G., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cesarini, E., Chalermsongsak, T., Chalkley, E., Charlton, P., Chassande-Mottin, E., Chatterji, S., Chelkowski, S., Chen, Y., Chincarini, A., Christensen, N., Chung, C. T. Y., Clark, D., Clark, J., Clayton, J. H., Cleva, F., Coccia, E., Cokelaer, T., Colacino, C. N., Colas, J., Colla, A., Colombini, M., Conte, R., Cook, D., Corbitt, T. R. C., Corda, C., Cornish, N., Corsi, A., Coulon, J. -P., Coward, D., Coyne, D. C., Creighton, J. D. E., Creighton, T. D., Cruise, A. M., Culter, R. M., Cumming, A., Cunningham, L., Cuoco, E., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dari, A., Dattilo, V., Daudert, B., Davier, M., Davies, G., Daw, E. J., Day, R., De Rosa, R., DeBra, D., Degallaix, J., del Prete, M., Dergachev, V., Desai, S., DeSalvo, R., Dhurandhar, S., Di Fiore, L., Di Lieto, A., Emilio, M. Di Paolo, Di Virgilio, A., Díaz, M., Dietz, A., Donovan, F., Dooley, K. L., Doomes, E. E., Drago, M., Drever, R. W. P., Dueck, J., Duke, I., Dumas, J. -C., Dwyer, J. G., Echols, C., Edgar, M., Edwards, M., Effler, A., Ehrens, P., Espinoza, E., Etzel, T., Evans, M., Evans, T., Fafone, V., Fairhurst, S., Faltas, Y., Fan, Y., Fazi, D., Fehrmann, H., Ferrante, I., Fidecaro, F., Finn, L. S., Fiori, I., Flaminio, R., Flasch, K., Foley, S., Forrest, C., Fotopoulos, N., Fournier, J. -D., Franc, J., Franzen, A., Frasca, S., Frasconi, F., Frede, M., Frei, M., Frei, Z., Freise, A., Frey, R., Fricke, T., Fritschel, P., Frolov, V. V., Fyffe, M., Galdi, V., Gammaitoni, L., Garofoli, J. A., Garufi, F., Gemme, G., Genin, E., Gennai, A., Gholami, I., Giaime, J. A., Giampanis, S., Giardina, K. D., Giazotto, A., Goda, K., Goetz, E., Goggin, L. M., González, G., Gorodetsky, M. L., Goeßzetler, S., Goßler, S., Gouaty, R., Granata, M., Granata, V., Grant, A., Gras, S., Gray, C., Gray, M., Greenhalgh, R. J. S., Gretarsson, A. M., Greverie, C., Grimaldi, F., Grosso, R., Grote, H., Grunewald, S., Guenther, M., Guidi, G., Gustafson, E. K., Gustafson, R., Hage, B., Hallam, J. M., Hammer, D., Hammond, G. D., Hanna, C., Hanson, J., Harms, J., Harry, G. M., Harry, I. W., Harstad, E. D., Haughian, K., Hayama, K., Heefner, J., Heitmann, H., Hello, P., Heng, I. S., Heptonstall, A., Hewitson, M., Hild, S., Hirose, E., Hoak, D., Hodge, K. A., Holt, K., Hosken, D. J., Hough, J., Hoyland, D., Huet, D., Hughey, B., Huttner, S. H., Ingram, D. R., Isogai, T., Ito, M., Ivanov, A., Jaranowski, P., Johnson, B., Johnson, W. W., Jones, D. I., Jones, G., Jones, R., de la Jordana, L. Sancho, Ju, L., Kalmus, P., Kalogera, V., Kandhasamy, S., Kanner, J., Kasprzyk, D., Katsavounidis, E., Kawabe, K., Kawamura, S., Kawazoe, F., Kells, W., Keppel, D. G., Khalaidovski, A., Khalili, F. Y., Khan, R., Khazanov, E., King, P., Kissel, J. S., Klimenko, S., Kokeyama, K., Kondrashov, V., Kopparapu, R., Koranda, S., Kowalska, I., Kozak, D., Krishnan, B., Królak, A., Kumar, R., Kwee, P., La Penna, P., Lam, P. K., Landry, M., Lantz, B., Lazzarini, A., Lei, H., Lei, M., Leindecker, N., Leonor, I., Leroy, N., Letendre, N., Li, C., Lin, H., Lindquist, P. E., Littenberg, T. B., Lockerbie, N. A., Lodhia, D., Longo, M., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lu, P., Lubinski, M., Lucianetti, A., Lück, H., Machenschalk, B., MacInnis, M., Mackowski, J. -M., Mageswaran, M., Mailand, K., Majorana, E., Man, N., Mandel, I., Mandic, V., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A., Markowitz, J., Maros, E., Marque, J., Martelli, F., Martin, I. W., Martin, R. M., Marx, J. N., Mason, K., Masserot, A., Matichard, F., Matone, L., Matzner, R. A., Mavalvala, N., McCarthy, R., McClelland, D. E., McGuire, S. C., McHugh, M., McIntyre, G., McKechan, D. J. A., McKenzie, K., Mehmet, M., Melatos, A., Melissinos, A. C., Mendell, G., Menéndez, D. F., Menzinger, F., Mercer, R. A., Meshkov, S., Messenger, C., Meyer, M. S., Michel, C., Milano, L., Miller, J., Minelli, J., Minenkov, Y., Mino, Y., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Miyakawa, O., Moe, B., Mohan, M., Mohanty, S. D., Mohapatra, S. R. P., Moreau, J., Moreno, G., Morgado, N., Morgia, A., Morioka, T., Mors, K., Mosca, S., Moscatelli, V., Mossavi, K., Mours, B., MowLowry, C., Mueller, G., Muhammad, D., Mühlen, H. zur, Mukherjee, S., Mukhopadhyay, H., Mullavey, A., Müller-Ebhardt, H., Munch, J., Murray, P. G., Myers, E., Myers, J., Nash, T., Nelson, J., Neri, I., Newton, G., Nishizawa, A., Nocera, F., Numata, K., Ochsner, E., O'Dell, J., Ogin, G. H., O'Reilly, B., O'Shaughnessy, R., Ottaway, D. J., Ottens, R. S., Overmier, H., Owen, B. J., Pagliaroli, G., Palomba, C., Pan, Y., Pankow, C., Paoletti, F., Papa, M. A., Parameshwaraiah, V., Pardi, S., Pasqualetti, A., Passaquieti, R., Passuello, D., Patel, P., Pedraza, M., Penn, S., Perreca, A., Persichetti, G., Pichot, M., Piergiovanni, F., Pierro, V., Pietka, M., Pinard, L., Pinto, I. M., Pitkin, M., Pletsch, H. J., Plissi, M. V., Poggiani, R., Postiglione, F., Prato, M., Principe, M., Prix, R., Prodi, G. A., Prokhorov, L., Punken, O., Punturo, M., Puppo, P., Quetschke, V., Raab, F. J., Rabaste, O., Rabeling, D. S., Radkins, H., Raffai, P., Raics, Z., Rainer, N., Rakhmanov, M., Rapagnani, P., Raymond, V., Re, V., Reed, C. M., Reed, T., Regimbau, T., Rehbein, H., Reid, S., Reitze, D. H., Ricci, F., Riesen, R., Riles, K., Rivera, B., Roberts, P., Robertson, N. A., Robinet, F., Robinson, C., Robinson, E. L., Rocchi, A., Roddy, S., Rolland, L., Rollins, J., Romano, J. D., Romano, R., Romie, J. H., Rosińska, D., Röver, C., Rowan, S., Rüdiger, A., Ruggi, P., Russell, P., Ryan, K., Sakata, S., Salemi, F., Sandberg, V., Sannibale, V., Santamaría, L., Saraf, S., Sarin, P., Sassolas, B., Sathyaprakash, B. S., Sato, S., Satterthwaite, M., Saulson, P. R., Savage, R., Savov, P., Scanlan, M., Schilling, R., Schnabel, R., Schofield, R., Schulz, B., Schutz, B. F., Schwinberg, P., Scott, J., Scott, S. M., Searle, A. C., Sears, B., Seifert, F., Sellers, D., Sengupta, A. S., Sentenac, D., Sergeev, A., Shapiro, B., Shawhan, P., Shoemaker, D. H., Sibley, A., Siemens, X., Sigg, D., Sinha, S., Sintes, A. M., Slagmolen, B. J. J., Slutsky, J., van der Sluys, M. V., Smith, J. R., Smith, M. R., Smith, N. D., Somiya, K., Sorazu, B., Stein, A., Stein, L. C., Steplewski, S., Stochino, A., Stone, R., Strain, K. A., Strigin, S., Stroeer, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, K. -X., Sung, M., Sutton, Patrick J., Swinkels, B., Szokoly, G. P., Talukder, D., Tang, L., Tanner, D. B., Tarabrin, S. P., Taylor, J. R., Taylor, R., Terenzi, R., Thacker, J., Thorne, K. A., Thorne, K. S., Thüring, A., Tokmakov, K. V., Toncelli, A., Tonelli, M., Torres, C., Torrie, C., Tournefier, E., Travasso, F., Traylor, G., Trias, M., Trummer, J., Ugolini, D., Ulmen, J., Urbanek, K., Vahlbruch, H., Vajente, G., Vallisneri, M., Brand, J. F. J. van den, van der Putten, S., Vass, S., Vaulin, R., Vavoulidis, M., Vecchio, A., Vedovato, G., van Veggel, A. A., Veitch, J., Veitch, P., Veltkamp, C., Verkindt, D., Vetrano, F., Viceré, A., Villar, A., Vinet, J. -Y., Vocca, H., Vorvick, C., Vyachanin, S. P., Waldman, S. J., Wallace, L., Ward, R. L., Was, M., Weidner, A., Weinert, M., Weinstein, A. J., Weiss, R., Wen, L., Wen, S., Wette, K., Whelan, J. T., Whitcomb, S. E., Whiting, B. F., Wilkinson, C., Willems, P. A., Williams, H. R., Williams, L., Willke, B., Wilmut, I., Winkelmann, L., Winkler, W., Wipf, C. C., Wiseman, A. G., Woan, G., Wooley, R., Worden, J., Wu, W., Yakushin, I., Yamamoto, H., Yan, Z., Yoshida, S., Yvert, M., Zanolin, M., Zhang, J., Zhang, L., Zhao, C., Zotov, N., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We present the results of a search for gravitational-wave bursts associated with 137 gamma-ray bursts (GRBs) that were detected by satellite-based gamma-ray experiments during the fifth LIGO science run and first Virgo science run. The data used in this analysis were collected from 2005 November 4 to 2007 October 1, and most of the GRB triggers were from the Swift satellite. The search uses a coherent network analysis method that takes into account the different locations and orientations of the interferometers at the three LIGO-Virgo sites. We find no evidence for gravitational-wave burst signals associated with this sample of GRBs. Using simulated short-duration (<1 s) waveforms, we set upper limits on the amplitude of gravitational waves associated with each GRB. We also place lower bounds on the distance to each GRB under the assumption of a fixed energy emission in gravitational waves, with typical limits of D ~ 15 Mpc (E_GW^iso / 0.01 M_o c^2)^1/2 for emission at frequencies around 150 Hz, where the LIGO-Virgo detector network has best sensitivity. We present astrophysical interpretations and implications of these results, and prospects for corresponding searches during future LIGO-Virgo runs., Comment: 16 pages, 3 figures. Updated references. To appear in ApJ.
Published: 2009
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16. The bright optical/NIR afterglow of the faint GRB 080710 - Evidence for a jet viewed off axis

Author: Krühler, T., Greiner, J., Afonso, P., Burlon, D., Clemens, C., Filgas, R., Kann, D. A., Klose, S., Yoldas, A. Küpcü, McBreen, S., Olivares, F., Rau, A., Rossi, A., Schulze, S., Szokoly, G. P., Updike, A., and Yoldas, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We investigate the optical/near-infrared light curve of the afterglow of GRB 080710 in the context of rising afterglows. Optical and near-infrared photometry was performed using the seven channel imager GROND and the Tautenburg Schmidt telescope. X-ray data were provided by the X-ray Telescope onboard the Swift satellite. The optical/NIR light curve of the afterglow of GRB 080710 is dominated by an initial increase in brightness, which smoothly turns over into a shallow power law decay. The initially rising achromatic light curve of the afterglow of GRB 080710 can be accounted for with a model of a burst viewed off-axis or a single jet in its pre deceleration phase and in an on-axis geometry. An unified picture of the afterglow light curve and prompt emission properties can be obtained with an off-axis geometry, suggesting that late and shallow rising optical light curves of GRB afterglows might be produced by geometric effects., Comment: 9 pages, 4 figures, accepted by A and A
Published: 2009
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17. Rise and fall of the X-ray flash 080330: an off-axis jet?

Author: Guidorzi, C., Clemens, C., Kobayashi, S., Granot, J., Melandri, A., D'Avanzo, P., Kuin, N. P. M., Klotz, A., Fynbo, J. P. U., Covino, S., Greiner, J., Malesani, D., Mao, J., Mundell, C. G., Steele, I. A., Jakobsson, P., Margutti, R., Bersier, D., Campana, S., Chincarini, G., D'Elia, V., Fugazza, D., Genet, F., Gomboc, A., Kruehler, T., Yoldacs, A. Kupcu, Moretti, A., Mottram, C. J., O'Brien, P. T., Smith, R. J., Szokoly, G., Tagliaferri, G., Tanvir, N. R., and Gehrels, N.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: X-ray flashes (XRFs) are a class of gamma-ray bursts (GRBs) with the peak energy of the time-integrated spectrum, Ep, below 30 keV, whereas classical GRBs have Ep of a few hundreds keV. Apart from Ep and the lower luminosity, the properties of XRFs are typical of the classical GRBs. Yet, the nature of XRFs and the differences from that of GRBs are not understood. In addition, there is no consensus on the interpretation of the shallow decay phase observed in most X-ray afterglows of both XRFs and GRBs. We examine in detail the case of XRF 080330 discovered by Swift at the redshift of 1.51. This burst is representative of the XRF class and exhibits an X-ray shallow decay. The rich and broadband (from NIR to UV) photometric data set we collected across this phase makes it an ideal candidate to test the off-axis jet interpretation proposed to explain both the softness of XRFs and the shallow decay phase. We present prompt gamma-ray, early and late IR/visible/UV and X-ray observations of the XRF 080330. We derive a SED from NIR to X-ray bands across the plateau phase with a power-law index of 0.79 +- 0.01 and negligible rest-frame dust extinction. The multi-wavelength evolution of the afterglow is achromatic from ~10^2 s out to ~8x10^4 s. We describe the temporal evolution of the multi-wavelength afterglow within the context of the standard afterglow model and show that a single-component jet viewed off-axis explains the observations (abriged)., Comment: accepted to A&A, 19 pages, 11 figures
Published: 2009
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18. Correlated optical and X-ray flares in the afterglow of XRF 071031

Author: Krühler, T., Greiner, J., McBreen, S., Klose, S., Rossi, A., Afonso, P., Clemens, C., Filgas, R., Yoldas, A. Küpcü, Szokoly, G. P., and Yoldas, A.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract: We present a densely sampled early light curve of the optical/near-infrared (NIR) afterglow of the X-Ray Flash (XRF) 071031 at z=2.692. Simultaneous and continuous observations in seven photometric bands from g' to K with GROND at the 2.2 m MPI/ESO telescope on LaSilla were performed between 4 minutes and 7 hours after the burst. The light curve consists of 547 individual points which allows us to study the early evolution of the optical transient associated with XRF 071031 in great detail. The optical/NIR light curve is dominated by an early increase in brightness which can be attributed to the apparent onset of the forward shock emission. There are several bumps which are superimposed onto the overall rise and decay. Significant flaring is also visible in the Swift X-Ray Telescope (XRT) light curve from early to late times. The availability of high quality, broadband data enables detailed studies of the connection between the X-ray and optical/NIR afterglow and its colour evolution during the first night post burst. We find evidence of spectral hardening in the optical bands contemporaneous with the emergence of the bumps from an underlying afterglow component. The bumps in the optical/NIR light curve can be associated with flares in the X-ray regime suggesting late central engine activity as the common origin., Comment: Accepted for publication in ApJ
Published: 2009
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19. The redshift and afterglow of the extremely energetic gamma-ray burst GRB 080916C

Author: Greiner, J., Clemens, C., Kruehler, T., Kienlin, A. v., Rau, A., Sari, R., Fox, D. B., Kawai, N., Afonso, P., Ajello, M., Berger, E., Cenko, S. B., Cucchiara, A., Filgas, R., Klose, S., Yoldas, A. Kuepue, Lichti, G. G., Loew, S., McBreen, S., Nagayama, T., Rossi, A., Sato, S., Szokoly, G., Yoldas, A., and Zhang, X. -L.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: The detection of GeV photons from gamma-ray bursts (GRBs) has important consequences for the interpretation and modelling of these most-energetic cosmological explosions. The full exploitation of the high-energy measurements relies, however, on the accurate knowledge of the distance to the events. Here we report on the discovery of the afterglow and subsequent redshift determination of GRB 080916C, the first GRB detected by the Fermi Gamma-Ray Space Telescope with high significance detection of photons at >0.1 GeV. Observations were done with 7-channel imager GROND at the 2.2m MPI/ESO telescope, the SIRIUS instrument at the Nagoya-SAAO 1.4m telescope in South Africa, and the GMOS instrument at Gemini-S. The afterglow photometric redshift of z=4.35+-0.15, based on simultaneous 7-filter observations with the Gamma-Ray Optical and Near-infrared Detector (GROND), places GRB 080916C among the top 5% most distant GRBs, and makes it the most energetic GRB known to date. The detection of GeV photons from such a distant event is rather surprising. The observed gamma-ray variability in the prompt emission together with the redshift suggests a lower limit for the Lorentz factor of the ultra-relativistic ejecta of Gamma > 1090. This value rivals any previous measurements of Gamma in GRBs and strengthens the extreme nature of GRB 080916C., Comment: 6 pages, 5 figures; subm. to A&A
Published: 2009
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20. Discovery of the Most-Distant Double-Peaked Emitter at z=1.369

Author: Luo, B., Brandt, W. N., Silverman, J. D., Strateva, I. V., Bauer, F. E., Capak, P., Kartaltepe, J., Lehmer, B. D., Mainieri, V., Salvato, M., Szokoly, G., Schneider, D. P., and Vignali, C.
Subjects: Astrophysics - Galaxy Astrophysics, Astrophysics - Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We report the discovery of the most-distant double-peaked emitter, CXOECDFS J033115.0-275518, at z=1.369. A Keck/DEIMOS spectrum shows a clearly double-peaked broad Mg II $\lambda2799$ emission line, with FWHM 11000 km/s for the line complex. The line profile can be well fit by an elliptical relativistic Keplerian disk model. This is one of a handful of double-peaked emitters known to be a luminous quasar, with excellent multiwavelength coverage and a high-quality X-ray spectrum. CXOECDFS J033115.0-275518 is a radio-loud quasar with two radio lobes (FR II morphology) and a radio loudness of f_{5 GHz}/f_{4400 \AA}~429. The X-ray spectrum can be modeled by a power law with photon index 1.72 and no intrinsic absorption; the rest-frame 0.5-8.0 keV luminosity is $5.0\times10^{44}$ erg/s. The spectral energy distribution (SED) of CXOECDFS J033115.0-275518 has a shape typical for radio-loud quasars and double-peaked emitters at lower redshift. The local viscous energy released from the line-emitting region of the accretion disk is probably insufficient to power the observed line flux, and external illumination of the disk appears to be required. The presence of a big blue bump in the SED along with the unexceptional X-ray spectrum suggest that the illumination cannot arise from a radiatively inefficient accretion flow., Comment: 6 pages, 5 figures, ApJ in press
Published: 2009
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21. A strong optical flare before the rising afterglow of GRB 080129

Author: Greiner, J., Krühler, T., McBreen, S., Ajello, M., Giannos, D., Schwarz, R., Savaglio, S., Yoldas, A. Küpcü, Clemens, C., Stefanescu, A., Sala, G., Bertoldi, F., Szokoly, G., and Klose, S.
Subjects: Astrophysics
Abstract: We report on GROND observations of a 40 sec duration (rest-frame) optical flare from GRB 080129 at redshift 4.349. The rise- and decay time follow a power law with indices +12 and -8, respectively, inconsistent with a reverse shock and a factor 10$^5$ faster than variability caused by ISM interaction. While optical flares have been seen in the past (e.g. GRB 990123, 041219B, 060111B and 080319B), for the first time, our observations not only resolve the optical flare into sub-components, but also provide a spectral energy distribution from the optical to the near-infrared once every minute. The delay of the flare relative to the GRB, its spectral energy distribution as well as the ratio of pulse widths suggest it to arise from residual collisions in GRB outflows \cite{liw08}.If this interpretation is correct and can be supported by more detailed modelling or observation in further GRBs, the delay measurement provides an independent, determination of the Lorentz factor of the outflow., Comment: accepted for publ. in ApJ, 5 Figs
Published: 2008
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22. GRB 080913 at redshift 6.7

Author: Greiner, J., Kruehler, T., Fynbo, J. P. U., Rossi, A., Schwarz, R., Klose, S., Savaglio, S., Tanvir, N. R., McBreen, S., Totani, T., Zhang, B. B., Wu, X. F., Watson, D., Barthelmy, S. D., Beardmore, A. P., Ferrero, P., Gehrels, N., Kann, D. A., Kawai, N., Yoldas, A. Kuepcue, Meszaros, P., Milvang-Jensen, B., Oates, S. R., Pierini, D., Schady, P., Toma, K., Vreeswijk, P. M., Yoldas, A., Zhang, B., Afonso, P., Aoki, K., Burrows, D. N., Clemens, C., Filgas, R., Haiman, Z., Hartmann, D. H., Hasinger, G., Hjorth, J., Jehin, E., Levan, A. J., Liang, E. W., Malesani, D., Pyo, T. -S., Schulze, S., Szokoly, G., Terada, H., and Wiersema, K.
Subjects: Astrophysics
Abstract: We report on the detection by Swift of GRB 080913, and subsequent optical/near-infrared follow-up observations by GROND which led to the discovery of its optical/NIR afterglow and the recognition of its high-z nature via the detection of a spectral break between the i' and z' bands. Spectroscopy obtained at the ESO-VLT revealed a continuum extending down to lambda = 9400 A, and zero flux for 7500 A < lambda<9400 A, which we interpret as the onset of a Gunn-Peterson trough at z=6.695+-0.025 (95.5% conf. level), making GRB 080913 the highest redshift GRB to date, and more distant than the highest-redshift QSO. We note that many redshift indicators which are based on promptly available burst or afterglow properties have failed for GRB 080913. We report on our follow-up campaign and compare the properties of GRB 080913 with bursts at lower redshift. In particular, since the afterglow of this burst is fainter than typical for GRBs, we show that 2m-class telescopes can identify most high-redshift GRBs., Comment: 14 pages, 7 figures, ApJ (subm)
Published: 2008
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23. A photometric redshift of $z=1.8^{+0.4}_{-0.3}$ for the \agile GRB 080514B

Author: Rossi, A., Postigo, A. de Ugarte, Ferrero, P., Kann, D. A., Klose, S., Schulze, S., Greiner, J., Schady, P., Filgas, R., Gonsalves, E. E., Yoldaş, A. Küpcü, Krühler, T., Szokoly, G., Yoldaş, A., Afonso, P. M. J., Clemens, C., Bloom, J. S., Perley, D. A., Fynbo, J. P. U., Castro-Tirado, A. J., Gorosabel, J., Kubánek, P., Updike, A. C., Hartmann, D. H., Giuliani, A., Holland, S. T., Hanlon, L., Bremer, M., and García-Hernández, A.
Subjects: Astrophysics
Abstract: Aims: The AGILE gamma-ray burst GRB 080514B is the first burst with detected emission above 30 MeV and an optical afterglow. However, no spectroscopic redshift for this burst is known. Methods: We compiled ground-based photometric optical/NIR and millimeter data from several observatories, including the multi-channel imager GROND, as well as ultraviolet \swift UVOT and X-ray XRT observations. The spectral energy distribution of the optical/NIR afterglow shows a sharp drop in the \swift UVOT UV filters that can be utilized for the estimation of a redshift. Results: Fitting the SED from the \swift UVOT $uvw2$ band to the $H$ band, we estimate a photometric redshift of $z=1.8^{+0.4}_{-0.3}$, consistent with the pseudo redshift reported by Pelangeon & Atteia (2008) based on the gamma-ray data. Conclusions: The afterglow properties of GRB 080514B do not differ from those exhibited by the global sample of long bursts, supporting the view that afterglow properties are basically independent of prompt emission properties., Comment: submitted to A&A letters
Published: 2008
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24. The 2175 A dust feature in a Gamma Ray Burst afterglow at redshift 2.45

Author: Krühler, T., Yoldaş, A. Küpcü, Greiner, J., Clemens, C., McBreen, S., Primak, N., Savaglio, S., Yoldaş, A., and Szokoly, G. P.
Subjects: Astrophysics
Abstract: We present optical and near-infrared photometry of the afterglow of the long Gamma-Ray Burst GRB 070802 at redshift 2.45 obtained with the ESO/MPI 2.2 m telescope equipped with the multi-channel imager GROND. Follow-up observations in g'r'i'z' and JHK_S bands started ~17 min and extended up to 28 h post burst. We find an increase in brightness of the afterglow at early times, which can be explained by the superposition of reverse and forward shock (FS) emission or the onset of the afterglow FS. Additionally, we detect a strong broad-band absorption feature in the i' band, which we interpret as extinction from the redshifted 2175 A bump in the GRB host galaxy. This is one of the first and clearest detections of the 2175 A feature at high redshift. It is strong evidence for a carbon rich environment, indicating that Milky Way or Large Magellanic Cloud like dust was already formed in substantial amounts in a galaxy at z=2.45., Comment: 21 pages, 3 figures, accepted for publication by ApJ
Published: 2008
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25. GROND - a 7-channel imager

Author: Greiner, J., Bornemann, W., Clemens, C., Deuter, M., Hasinger, G., Honsberg, M., Huber, H., Huber, S., Krauss, M., Krühler, T., Yoldaş, A. Küpcü, Mayer-Hasselwander, H., Mican, B., Primak, N., Schrey, F., Steiner, I., Szokoly, G., Thöne, C. C., Yoldaş, A., Klose, S., Laux, U., and Winkler, J.
Subjects: Astrophysics
Abstract: We describe the construction of GROND, a 7-channel imager, primarily designed for rapid observations of gamma-ray burst afterglows. It allows simultaneous imaging in the Sloan g'r'i'z' and near-infrared $JHK$ bands. GROND was commissioned at the MPI/ESO 2.2m telescope at La Silla (Chile) in April 2007, and first results of its performance and calibration are presented., Comment: 25 pages, 21 figs, PASP (subm); version with full-resolution figures at http://www.mpe.mpg.de/~jcg/GROND/grond_pasp.pdf
Published: 2008
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26. XMM-Newton observations of the Lockman Hole: X-ray source catalogue and number counts

Author: Brunner, H., Cappelluti, N., Hasinger, G., Barcons, X., Fabian, A. C., Mainieri, V., and Szokoly, G.
Subjects: Astrophysics
Abstract: The Lockman Hole field represents the sky area of lowest Galactic line-of-sight column density N_H=5.7X10^19 cm^-2. It was observed by the XMM-Newton X-ray observatory in 18 pointings for a total of 1.16 Msec (raw EPIC pn observing time) constituting the deepest XMM-Newton exposure so far. We present a catalogue of the X-ray sources detected in the central 0.196 deg^2 of the field and discuss the derived number counts and X-ray colours. In the 0.5--2.0 keV band, a sensitivity limit (defined as the faintest detectable source)of 1.9X10^-16 erg cm^-2 s^-1 was reached. The 2.0--10.0 keV band and 5.0--10.0 keV band sensitivity limits were 9X10^-16 erg cm^-2 s^-1 and 1.8X10^-15 erg cm^-2 s^-1, respectively.A total of 409 sources above a detection likelihood of 10 (3.9 sigma) were found within a radius of 15' off the field centre, of which 340, 266, and 98 sources were detected in the soft, hard, and very hard bands, respectively. The number counts in each energy band are in close agreement with results from previous surveys and with the synthesis models of the X-ray background. A 6% of Compton-thick source candidates have been selected from the X-ray colour-colour diagram. This fraction is consistent with the most recent predictions of X-ray background population synthesis models at our flux limits. We also estimated, for the first time, the logN-logS relation for Compton-thick AGN., Comment: 20 pages, 12 figures, source catalogue. Some figures compressed. Accepted by Astronomy and Astrophysics on 11/27/2007. Machine readable version on Vizie-R
Published: 2007
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27. The XMM-Newton Serendipitous Survey V. Optical identification of the XMM-Newton Medium sensitivity Survey (XMS)

Author: Barcons, X., Carrera, F. J., Ceballos, M. T., Page, M. J., Bussons-Gordo, J., Corral, A., Ebrero, J., Mateos, S., Tedds, J. A., Watson, M. G., Birkinshaw, M., Boller, T., Borisov, N., Bremer, M., Bromage, G. E., Brunner, H., Caccianiga, A., Crawford, C. S., Cropper, M. S., Della Ceca, R., Derry, P., Fabian, A. C., Guillout, P., Hashimoto, Y., Hasinger, G., Hassall, B. J. M., Lamer, G., Loaring, N. S., Maccacaro, T., Mason, K. O., McMahon, R. G., Mirioni, L., Mittaz, J. P. D., Motch, C., Negueruela, I., Osborne, J. P., Panessa, F., Perez-Fournon, I., Pye, J. P., Roberts, T. P., Rosen, S., Schartel, N., Schurch, N., Schwope, A., Severgnini, P., Sharp, R., Stewart, G. C., Szokoly, G., Ullan, A., Ward, M. J., Warwick, R. S., Wheatley, P. J., Webb, N. A., Worrall, D., Yuan, W., and Ziaeepour, H.
Subjects: Astrophysics
Abstract: We present the XMM-Newton Medium sensitivity Survey (XMS), including a total of 318 X-ray sources found among the serendipitous content of 25 XMM-Newton target fields. The XMS comprises four largely overlapping source samples selected at soft (0.5-2 keV), intermediate (0.5-4.5 keV), hard (2-10 keV) and ultra-hard (4.5-7.5 keV) bands, the first three of them being flux-limited. We report on the optical identification of the XMS samples, complete to 85-95%. At the intermediate flux levels sampled by the XMS we find that the X-ray sky is largely dominated by Active Galactic Nuclei. The fraction of stars in soft X-ray selected samples is below 10%, and only a few per cent for hard selected samples. We find that the fraction of optically obscured objects in the AGN population stays constant at around 15-20% for soft and intermediate band selected X-ray sources, over 2 decades of flux. The fraction of obscured objects amongst the AGN population is larger (~35-45%) in the hard or ultra-hard selected samples, and constant across a similarly wide flux range. The distribution in X-ray-to-optical flux ratio is a strong function of the selection band, with a larger fraction of sources with high values in hard selected samples. Sources with X-ray-to-optical flux ratios in excess of 10 are dominated by obscured AGN, but with a significant contribution from unobscured AGN., Comment: A&A, accepted
Published: 2007
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28. The Evolution of AGN Host Galaxies: From Blue to Red and the Influence of Large-Scale Structures

Author: Silverman, J. D., Mainieri, V., Lehmer, B. D., Alexander, D. M., Bauer, F. E., Bergeron, J., Brandt, W. N., Gilli, R., Hasinger, G., Schneider, D. P., Tozzi, P., Vignali, C., Koekemoer, A. M., Miyaji, T., Popesso, P., Rosati, P., and Szokoly, G.
Subjects: Astrophysics
Abstract: We present an analysis of 109 moderate-luminosity (41.9 < Log L{0.5-8.0 keV} < 43.7) AGN in the Extended Chandra Deep Field-South survey, which is drawn from 5,549 galaxies from the COMBO-17 and GEMS surveys having 0.4 < z < 1.1. These obscured or optically-weak AGN facilitate the study of their host galaxies since the AGN provide an insubstantial amount of contamination to the galaxy light. We find that the color distribution of AGN host galaxies is highly dependent upon (1) the strong color-evolution of luminous (M_V < -20.7) galaxies, and (2) the influence of ~10 Mpc scale structures. When excluding galaxies within the redshift range 0.63 < z < 0.76, a regime dominated by sources in large-scale structures at z=0.67 and z=0.73, we observe a bimodality in the host galaxy colors. Galaxies hosting AGN at z > 0.8 preferentially have bluer (rest-frame U-V < 0.7) colors than their z <~ 0.6 counterparts (many of which fall along the red sequence). The fraction of galaxies hosting AGN peaks in the ``green valley'' (0.5 < U-V < 1.0); this is primarily due to enhanced AGN activity in the redshift interval 0.63 < z < 0.76. The AGN fraction in this redshift and color interval is 12.8% (compared to its `field' value of 7.8%) and reaches a maximum of 14.8% at U-V~0.8. We further find that blue, bulge-dominated (Sersic index n>2.5) galaxies have the highest fraction of AGN (21%) in our sample. We explore the scenario that the evolution of AGN hosts is driven by galaxy mergers and illustrate that an accurate assessment requires a larger area survey since only three hosts may be undergoing a merger with timescales <1 Gyr following a starburst phase., Comment: Published in ApJ, 2008, 675, 1025; 17 pages, 14 figures
Published: 2007
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29. Most hard X-ray selected quasars in Chandra Deep Fields are obscured

Author: Wang, J. X., Jiang, P., Zheng, Z. Y., Tozzi, P., Norman, C., Giacconi, R., Gilli, R., Hasinger, G., Kewley, L., Mainieri, V., Nonino, M., Rosati, P., Streblyanska, A., Szokoly, G., Zirm, A., and Zheng, W.
Subjects: Astrophysics
Abstract: Measuring the population of obscured quasars is one of the key issues to understand the evolution of active galactic nuclei (AGNs). With a redshift completeness of 99%, the X-ray sources detected in Chandra Deep Field South (CDF-S) provide the best sample for this issue. In this letter we study the population of obscured quasars in CDF-S by choosing the 4 -- 7 keV selected sample, which is less biased by the intrinsic X-ray absorption. The 4 -- 7 keV band selected samples also filter out most of the X-ray faint sources with too few counts, for which the measurements of N_H and L_X have very large uncertainties. Simply adopting the best-fit L_2-10keV and N_H, we find 71% (20 out of 28) of the quasars (with intrinsic L_2-10keV > 10^44 erg/s) are obscured with N_H > 10^22 cm^-2. Taking account of the uncertainties in the measurements of both N_H and L_X, conservative lower and upper limits of the fraction are 54% (13 out 24) and 84% (31 out 37). In Chandra Deep Field North, the number is 29%, however, this is mainly due to the redshift incompleteness. We estimate a fraction of ~ 50% - 63% after correcting the redshift incompleteness with a straightforward approach. Our results robustly confirm the existence of a large population of obscured quasars., Comment: 18 pages, including 6 figures and 1 table, ApJ accepted (submitted on Apr. 10)
Published: 2006
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30. X-ray spectral properties of AGN in the Chandra Deep Field South

Author: Tozzi, P., Gilli, R., Mainieri, V., Norman, C., Risaliti, G., Rosati, P., Bergeron, J., Borgani, S., Giacconi, R., Hasinger, G., Nonino, M., Streblyanska, A., Szokoly, G., Wang, J. X., and Zheng, W.
Subjects: Astrophysics
Abstract: We present a detailed X-ray spectral analysis of the sources in the 1Ms catalog of the Chandra Deep Field South (CDFS) taking advantage of optical spectroscopy and photometric redshifts for 321 sources. As a default spectral model, we adopt a power law with slope Gamma with an intrinsic redshifted absorption N_H, a fixed Galactic absorption and an unresolved Fe emission line. For 82 X-ray bright sources, we perform the X-ray spectral analysis leaving both Gamma and N_H free. The weighted mean value is ~ 1.75+-0.02, with an intrinsic dispersion of sigma~0.30. We do not find hints of a correlation between Gamma and the N_H. We detect the presence of a scattered component at soft energies in 8 sources, and a pure reflection spectrum, typical of Compton-thick AGN, in 14 sources (Compton-thick AGN candidates). The intrinsic N_H distribution shows a lognormal shape, peaking around log(N_H)~23.1 and with sigma~1.1. We find that the fraction of absorbed sources (with N_H>10^{22} cm^{-2}) in the sample is constant (at the level of about 75%) or moderately increasing with redshift. Finally, we compare the optical classification to the X-ray spectral properties, confirming that the correspondence of unabsorbed (absorbed) X-ray sources to optical Type I (Type II) AGN is accurate for at least 80% of the sources with spectral identification (1/3 of the total X-ray sample)., Comment: 86 pages, A&A accepted, full version available at http://adlibitum.oat.ts.astro.it/tozzi/spectral_CDFS/paper_1Mspec.ps
Published: 2006
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31. Relativistic outflow in CXO CDFS J033260.0-274748

Author: Wang, J. X., Wang, T. G., Tozzi, P., Giacconi, R., Hasinger, G., Kewley, L., Mainieri, V., Nonino, M., Norman, C., Streblyanska, A., Szokoly, G., Yaqoob, T., and Zirm, A.
Subjects: Astrophysics
Abstract: In this letter we report the detection of a strong and extremely blueshifted X-ray absorption feature in the 1 Ms Chandra spectrum of CXO CDFS J033260.0-274748, a quasar at z = 2.579 with L_2-10keV ~ 4x10^44 ergs/s. The broad absorption feature at ~ 6.3 keV in the observed frame can be fitted either as an absorption edge at 20.9 keV or as a broad absorption line at 22.2 keV rest frame. The absorber has to be extremely ionized with an ionization parameter \xi ~ 10^4, and a high column density N_H >5x10^23 cm^-2. We reject the possibility of a statistical or instrumental artifact. The most likely interpretation is an extremely blueshifted broad absorption line or absorption edge, due to H or He--like iron in a relativistic jet-like outflow with bulk velocity of ~ 0.7-0.8 c. Similar relativistic outflows have been reported in the X-ray spectra of several other AGNs in the past few years., Comment: ApJ letter accepted
Published: 2005
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32. Optimal slit orientation for long multi-object spectroscopic exposures

Author: Szokoly, G. P.
Subjects: Astrophysics
Abstract: Historically, long-slit spectroscopic observations were carried out using the parallactic angle for the slit orientation if slit loss was an important consideration (either to maximize the signal-to-noise or to do spectrophotometry). This requires periodic realignment of the slit position angle as the parallactic angle changes. This is not possible for multi-slit observations where one slit position angle must be chosen for the entire exposure. Common wisdom suggests using the parallactic angle at the meridian (HA=0). In this paper, I examine what the best strategy is for long, multi-slit exposures. I find that in extreme cases (very long exposure time) the best choice is to orient the slit \emph{perpendicular} to the parallactic angle at the meridian. There are two effects to consider: the increasing dispersion with increasing airmass and the changing angle between the parallactic angle and the slit. In the case of \emph{traditional} slit orientation, the two effects amplify each other, thus rendering a significant fraction of the observation useless. Using the perpendicular orientation, the two processes work against each other, thus most of the observation remains useful. I will use, as an example, our 8 hour Lockman Hole observations using the Keck telescope, but generic methods are given to evaluate a particular observation. I also make the tools available to the community., Comment: Accepted by A&A (20/06/2005)
Published: 2005
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33. The Extended Chandra Deep Field-South Survey. Chandra Point-Source Catalogs

Author: Lehmer, B. D., Brandt, W. N., Alexander, D. M., Bauer, F. E., Schneider, D. P., Tozzi, P., Bergeron, J., Garmire, G. P., Giacconi, R., Gilli, R., Hasinger, G., Hornschemeier, A. E., Koekemoer, A. M., Mainieri, V., Miyaji, T., Nonino, M., Rosati, P., Silverman, J. D., Szokoly, G., and Vignali, C.
Subjects: Astrophysics
Abstract: We present Chandra point-source catalogs for the Extended Chandra Deep Field-South (E-CDF-S) survey. The E-CDF-S consists of four contiguous 250 ks Chandra observations covering an approximately square region of total solid angle ~0.3 deg^2, which flank the existing ~1 Ms Chandra Deep Field-South (CDF-S). The survey reaches sensitivity limits of 1.1 X 10^-16 erg/cm^2/s and 6.7 X 10^-16 erg/cm^2/s for the 0.5-2.0 keV and 2-8 keV bands, respectively. We detect 762 distinct X-ray point sources within the E-CDF-S exposure; 589 of these sources are new (i.e., not previously detected in the ~1 Ms CDF-S). This brings the total number of X-ray point sources detected in the E-CDF-S region to 915 (via the E-CDF-S and ~1 Ms CDF-S observations). Source positions are determined using matched-filter and centroiding techniques; the median positional uncertainty is ~0.35". The basic X-ray and optical properties of these sources indicate a variety of source types, although absorbed active galactic nuclei (AGNs) seem to dominate. In addition to our main Chandra catalog, we constructed a supplementary source catalog containing 33 lower significance X-ray point sources that have bright optical counterparts (R<23). These sources generally have X-ray-to-optical flux ratios expected for normal and starburst galaxies, which lack a strong AGN component. We present basic number-count results for our main Chandra catalog and find good agreement with the ~1 Ms CDF-S for sources with 0.5-2.0 keV and 2-8 keV fluxes greater than 3 X 10^-16 erg/cm^2/s and 1 X 10^-15 erg/cm^2/s, respectively. Furthermore, three extended sources are detected in the 0.5-2.0 keV band, which are found to be likely associated with galaxy groups or poor clusters at z ~ 0.1-0.7; these have typical rest-frame 0.5-2.0 keV luminosities of (1-5) X 10^42 erg/s., Comment: Accepted for publcation in ApJS (44 pages, 20 figures); version with all figures and catalogs available at http://www.astro.psu.edu/users/niel/ecdfs/ecdfs-chandra.html
Published: 2005
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34. The Chandra Deep Field South/GOODS survey. Optically faint X-ray sources

Author: Mainieri, V., Rosati, P., Tozzi, P., Bergeron, J., Gilli, R., Hasinger, G., Nonino, M., Lehmann, I., Alexander, D. M., Idzi, R., Koekemoer, A. M., Norman, C., Szokoly, G., and Zheng, W.
Subjects: Astrophysics
Abstract: We provide important new constraints on the nature and redshift distribution of optically faint (R>25) X-ray sources in the Chandra Deep Field South Survey. We show that we can derive accurate photometric redshifts for the spectroscopically unidentified sources thus maximizing the redshift completeness for the whole X-ray sample. Our new redshift distribution for the X-ray source population is in better agreement with that predicted by X-ray background synthesis models; however, we still find an overdensity of low redshift (z<1) sources. The optically faint sources are mainly X-ray absorbed AGN, as determined from direct X-ray spectral analysis and other diagnostics. Many of these optically faint sources have high (>10) X-ray-to-optical flux ratios. We also find that ~71% of them are well fitted with the SED of an early-type galaxy with ~1.9 and the remaining 29% with irregular or starburst galaxies mainly at z_phot>3. We estimate that 23% of the optically faint sources are X-ray absorbed QSOs. The overall population of X-ray absorbed QSOs contributes a ~15% fraction of the [2-10] keV X-ray Background (XRB) whereas current XRB synthesis models predict a ~38% contribution., Comment: 29 pages, 13 figures. Accepted for publication in Astronomy & Astrophysics. Full resolution preprint available at the CDF-S web page http://www.mpe.mpg.de/~mainieri/cdfs_pub/
Published: 2005
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35. The Galaxy Populations of Double Cluster RX J1053.7+5735 at z=1.13

Author: Hashimoto, Yasuhiro, Henry, J. Patrick, Hasinger, Guenther, Szokoly, G., Schmidt, M., and Lehmann, Ingo
Subjects: Astrophysics
Abstract: We present a study of the galaxy population in the cluster RX J1053.7+5735, one of the most distant X-ray selected clusters of galaxies, which also shows an unusual double-lobed X-ray morphology, indicative of a possible equal-mass cluster merger. Using Keck-DEIMOS spectroscopic observations of galaxies in the 2x1.5 arcmin region surrounding RX J1053.7+5735, we secured redshifts for six galaxies in the range 1.129 < z < 1.139, with a mean redshift =1.134. The mean redshift agrees well with the cluster X-ray redshift previously estimated from the cluster X-ray Fe-K line, confirming the presence of a cluster at z~1.135. Galaxies with concordant redshifts are located in both eastern and western sub-clusters of the double cluster structure, indicating that both sub-clusters are at similar redshifts. This result is also consistent with a previous claim that both eastern and western X-ray lobes have similar X-ray redshifts. Based on their separation of ~ 250 kpc/h, these results support the interpretation that RX J1053.7+5735 is an equal-mass cluster merger taken place at z ~ 1, although further direct evidence for dynamical state of the cluster is needed for a more definitive statement about the cluster merging state. The six galaxies have a line-of-sight velocity dispersion = 650 km/s. All six galaxies show clear absorption features of CaII H & K, and several Balmer lines, typical of early galaxies at the present epoch, in agreement with their I-K colors. A color-magnitude diagram, constructed from deep optical/NIR observations of the RX J1053.7+5735 field, shows a clear red color sequence. There is an indication that the red sequence in RX J1053.7+5735 lies ~ 0.3 to the blue of the Coma line, qualitatively consistent with previous studies investigating other clusters at z ~ 1., Comment: Accepted for publication in A&A. 5 pages, 4 figures
Published: 2005
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36. Candidate Type II Quasars from the SDSS: III. Spectropolarimetry Reveals Hidden Type I Nuclei

Author: Zakamska, Nadia L., Schmidt, Gary D., Smith, Paul S., Strauss, Michael A., Krolik, Julian H., Hall, P. B., Richards, G. T., Schneider, D. P., Brinkmann, J., and Szokoly, G. P.
Subjects: Astrophysics
Abstract: We have conducted spectropolarimetry of 12 type II (obscured) quasar candidates selected from the spectroscopic database of the Sloan Digital Sky Survey based on their emission line properties. Polarization was detected in all objects, with nine being highly polarized (> 3%) and with polarization reaching as high as 17% in two objects. Broad lines were detected in the polarized spectra of five objects. These observations prove beyond a reasonable doubt that the objects in our sample are indeed type II quasars, in that they harbor luminous UV-excess AGNs in their centers and that the direct view to the AGN is highly obscured. For three of the objects in this paper, we have obtained HST images in three bands. The HST observations, combined with the spectropolarimetry data, imply that scattering off material outside the obscuration plane is the dominant polarization mechanism. In all three objects the sizes of scattering regions are a few kpc. For one object, the extent of the scattering region, coupled with the characteristics of the polarized spectrum, argue strongly that dust scattering rather than electron scattering dominates the polarized light. Our observations are well-described by the basic orientation-based unification model of toroidal obscuration and off-plane scattering, implying that the model can be extended to include at least some high-luminosity AGNs., Comment: 31 pages including 4 b/w pictures, 1 color HST image and 2 tables. Submitted to AJ on Sept 26, accepted for March 2005. Minor modifications to match the accepted version
Published: 2004
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37. The spatial clustering of X-ray selected AGN and galaxies in the Chandra Deep Field South and North

Author: Gilli, R., Daddi, E., Zamorani, G., Tozzi, P., Borgani, S., Bergeron, J., Giacconi, R., Hasinger, G., Mainieri, V., Norman, C., Rosati, P., Szokoly, G., and Zheng, W.
Subjects: Astrophysics
Abstract: We investigate the spatial clustering of X-ray selected sources in the two deepest X-ray fields to date, namely the 2Msec Chandra Deep Field North (CDFN) and the 1Msec Chandra Deep Field South (CDFS). The projected correlation function w(r_p), measured on scales ~0.2-10 h^-1 Mpc for a sample of 240 sources with spectroscopic redshift in the CDFN and 124 sources in the CDFS at a median redshift of z~0.8, is used to constrain the amplitude and slope of the real space correlation function xi(r)=(r/r0)^-gamma. The clustering signal is detected at high confidence (>~ 7 sigma) in both fields. The amplitude of the correlation is found to be significantly different in the two fields, the correlation length r0 being 8.6 +- 1.2 h^-1 Mpc in the CDFS and 4.2 +- 0.4 h^-1 Mpc in the CDFN, while the correlation slope gamma is found to be flat in both fields: gamma=1.33 +- 0.11 in the CDFS and gamma=1.42 +- 0.07 in the CDFN (a flat Universe with Omega_m=0.3 and Omega_L=0.7 is assumed; 1 sigma Poisson error estimates are considered). The correlation function has been also measured separately for sources classified as AGN or galaxies. In both fields AGN have a median redshift of z~0.9 and a median 0.5-10 keV luminosity of L_x~10^43 erg s^-1, i.e. they are generally in the Seyfert luminosity regime. As in the case of the total samples, we found a significant difference in the AGN clustering amplitude between the two fields, the best fit correlation parameters being r0=10.3 +- 1.7 h^-1 Mpc, gamma=1.33 +- 0.14 in the CDFS, and r0=5.5 +- 0.6 h^-1 Mpc, gamma=1.50 +- 0.12 in the CDFN. Within each field no statistically significant difference is found between soft and hard X-ray selected sources or between type 1 and type 2 AGN. (abridged), Comment: 16 pages, 15 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2004
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38. Photometric Redshift of X-Ray Sources in the Chandra Deep Field South

Author: Zheng, W., Mikles, V. J., Mainieri, V., Hasinger, G., Rosati, P., Wolf, C., Norman, C., Szokoly, G., Gilli, R., Tozzi, P., Wang, J. X., Zirm, A., and Giacconi, R.
Subjects: Astrophysics
Abstract: Based on the photometry of 10 near-UV, optical, and near-infrared bands of the Chandra Deep Field South, we estimate the photometric redshifts for 342 X-ray sources, which constitute ~99% of all the detected X-ray sources in the field. The models of spectral energy distribution are based on galaxies and a combination of power-law continuum and emission lines. Color information is useful for source classifications: Type-I AGN show non-thermal spectral features that are distinctive from galaxies and Type-II AGN. The hardness ratio in X-ray and the X-ray-to-optical flux ratio are also useful discriminators. Using rudimentary color separation techniques, we are able to further refine our photometric redshift estimations. Among these sources, 137 have reliable spectroscopic redshifts, which we use to verify the accuracy of photometric redshifts and to modify the model inputs. The average relative dispersion in redshift distribution is ~8%, among the most accurate for photometric surveys. The high reliability of our results is attributable to the high quality and broad coverage of data as well as the applications of several independent methods and a careful evaluation of every source. We apply our redshift estimations to study the effect of redshift on broadband colors and to study the redshift distribution of AGN. Our results show that both the hardness ratio and U-K color decline with redshift, which may be the result of a K-correction. The number of Type-II AGN declines significantly at z>2 and that of galaxies declines at z>1. However, the distribution of Type-I AGN exhibits less redshift dependence. As well, we observe a significant peak in the redshift distribution at z=0.6. We demonstrate that our photometric redshift estimation produces a reliable database for the study of X-ray luminosity of galaxies and AGN., Comment: 40 pages, 11 figures. Accepted for publication in the Astrophysical Journal
Published: 2004
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39. A catalogue of the Chandra Deep Field South with multi-colour classification and photometric redshifts from COMBO-17

Author: Wolf, C., Meisenheimer, K., Kleinheinrich, M., Borch, A., Dye, S., Gray, M., Wisotzki, L., Bell, E. F., Rix, H. -W., Cimatti, A., Hasinger, G., and Szokoly, G.
Subjects: Astrophysics
Abstract: We present the COMBO-17 object catalogue of the Chandra Deep Field South for public use, covering a field which is 31.5' x 30' in size. This catalogue lists astrometry, photometry in 17 passbands from 350 to 930 nm, and ground-based morphological data for 63,501 objects. The catalogue also contains multi-colour classification into the categories 'Star', 'Galaxy' and 'Quasar' as well as photometric redshifts. We include restframe luminosities in Johnson, SDSS and Bessell passbands and estimated errors. The redshifts are most reliable at R<24, where the sample contains approximately 100 quasars, 1000 stars and 10000 galaxies. We use nearly 1000 spectroscopically identified objects in conjunction with detailed simulations to characterize the performance of COMBO-17. We show that the selection of quasars, more generally type-1 AGN, is nearly complete and minimally contaminated at z=[0.5,5] for luminosities above M_B=-21.7. Their photometric redshifts are accurate to roughly 5000 km/sec. Galaxy redshifts are accurate to 1% in dz/(1+z) at R<21. They degrade in quality for progressively fainter galaxies, reaching accuracies of 2% for galaxies with R~222 and of 10% for galaxies with R>24. The selection of stars is complete to R~23, and deeper for M stars. We also present an updated discussion of our classification technique with maps of survey completeness, and discuss possible failures of the statistical classification in the faint regime at R>24., Comment: submitted to Astronomy & Astrophysics, public data set available at http://www.mpia.de/COMBO/combo_index.html
Published: 2004
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40. The Chandra Deep Field South: Optical Spectroscopy I

Author: Szokoly, G. P., Bergeron, J., Hasinger, G., Lehmann, I., Kewley, L., Mainieri, V., Nonino, M., Rosati, P., Giacconi, R., Gilli, R., Gilmozzi, R., Norman, C., Romaniello, M., Schreier, E., Tozzi, P., Wang, J. X., Zheng, W., and Zirm, A.
Subjects: Astrophysics
Abstract: We present the results of our spectroscopic follow-up program of the X-ray sources detected in the 942 ks exposure of the Chandra Deep Field South (CDFS). 288 possible counterparts were observed at the VLT with the FORS1/FORS2 spectrographs for 251 of the 349 Chandra sources (including three additional faint X-ray sources). Spectra and R-band images are shown for all the observed sources and R-K colours are given for most of them. Spectroscopic redshifts were obtained for 168 X-ray sources, of which 137 have both reliable optical identification and redshift estimate (including 16 external identifications). The R<24 observed sample comprises 161 X-ray objects (181 optical counterparts) and 126 of them have unambiguous spectroscopic identification. We introduce a new classification based solely on X-ray properties, HR and X-ray luminosity, consistent with the unified AGN model. This X-ray classification uncovers a large fraction of optically obscured, X-ray luminous AGNs missed by the classical optical classification., Comment: Accepted for publication in ApJ supplement. Full version is available from http://www.mpe.mpg.de/~mainieri/cdfs_pub/
Published: 2003
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41. A serendipitous survey for galaxy clusters by the XMM-Newton Survey Science Center

Author: Schwope, A. D., Lamer, G., Burke, D., Elvis, M., Watson, M. G., Schulze, M. P., Szokoly, G., and Urrutia, T.
Subjects: Astrophysics
Abstract: We describe the initial results of a programme to detect and identify extended X-ray sources found serendipitously in XMM-Newton observations. We have analysed 186 EPIC-PN images at high galactic latitude with a limiting flux of $1\times 10^{-14}$ \ergcms and found 62 cluster candidates. Thanks to the enhanced sensitivity of the XMM-Newton telescopes, the new clusters found in this pilot study are on the average fainter, more compact, and more distant than those found in previous X-ray surveys. At our survey limit the surface density of clusters is about 5 deg$^{-2}$. We also present the first results of an optical follow-up programme aiming at the redshift measurement of a large sample of clusters. The results of this pilot study give a first glimpse on the potential of serendipitous cluster science with XMM-Newton based on real data. The largest, yet to be fulfilled promise is the identification of a large number of high-redshift clusters for cosmological studies up to $z=1$ or 1.5., Comment: Proc World Space Conf. Houston, October 2002, Adv. Space Res., in press
Published: 2003
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42. A Puzzling X-Ray Source Found in the chandra Deep Field South

Author: Wang, J., Yaqoob, T., Szokoly, G., Gilli, R., Kewley, L., Mainieri, V., Nonino, M., Rosati, P., Tozzi, P., Zheng, W., Zirm, A., and Norman, C.
Subjects: Astrophysics
Abstract: In this letter we report the detection of an extremely strong X-ray emission line in the 940ks chandra ACIS-I spectrum of CXO CDFS J033225.3-274219. The source was identified as a Type1 AGN at redshift of z = 1.617, with 2.0 -- 10.0 keV rest frame X-ray luminosity of ~ 10^44 ergs s^-1. The emission line was detected at 6.2^{+0.2}_{-0.1} keV, with an equivalent width (EW) of 4.4^{+3.2}_{-1.4} keV, both quantities referring to the observed frame. In the rest frame, the line is at 16.2^{+0.4}_{-0.3} keV with an EW of 11.5^{+8.3}_{-3.7} keV. An X-ray emission line at similar energy (~ 17 keV, rest frame) in QSO PKS 2149-306 was discovered before using ASCA data. We reject the possibility that the line is due to a statistical or instrumental artifact. The line is most likely due to blueshifted Fe-K emission from an relativistic outflow, probably an inner X-ray jet, with velocities of the order of ~ 0.6-0.7c. Other possible explanations are also discussed.
Published: 2003
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43. Tracing the large scale structure in the Chandra Deep Field South

Author: Gilli, R., Cimatti, A., Daddi, E., Hasinger, G., Rosati, P., Szokoly, G., Tozzi, P., Bergeron, J., Borgani, S., Giacconi, R., Kewley, L., Mainieri, V., Mignoli, M., Nonino, M., Norman, C., Wang, J., Zamorani, G., Zheng, W., and Zirm, A.
Subjects: Astrophysics
Abstract: We report the discovery of large scale structures of X-ray sources in the 1Msec observation of the Chandra Deep Field South. Two main structures appear as narrow (Delta_z < 0.02) spikes in the source redshift distribution at z=0.67 and z=0.73, respectively. Their angular distribution spans a region at least ~ 17 arcmin wide, corresponding to a physical size of 7.3 h_{70}^{-1} Mpc at a redshift of z ~ 0.7 (Omega_m=0.3, Omega_{Lambda}=0.7). These spikes are populated by 19 sources each, which are mainly identified as Active Galactic Nuclei (AGN). Two sources in each spike are extended in X-rays, corresponding to galaxy groups/clusters embedded in larger structures. The X-ray source redshift distribution shows other spikes, the most remarkable at z=1.04, 1.62 and 2.57. This is one of the first evidences for large scale structure traced by X-ray sources and for spatial clustering of X-ray selected AGN. The X-ray data have been complemented with the spectroscopic data from the K20 near infrared survey (Cimatti et al. 2002), which covers ~1/10 of the X-ray field. Also in this survey the source redshift distribution shows several spikes. Two narrow structures at z=0.67 and z=0.73 (again with Delta_z ~ 0.02) are the most significant features, containing 24 and 47 galaxies, respectively. While the K20 structure at z=0.73 is dominated by a standard galaxy cluster with a significant concentration around a central cD galaxy and morphological segregation, the galaxies at z=0.67 constitute a loose structure rather uniformly distributed along the K20 field.[abridged], Comment: 18 pages, 3 figures. Accepted by The Astrophysical Journal. A high resolution version of Fig.2 can be found at http://www.arcetri.astro.it/~gilli/f2_col.eps
Published: 2003
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44. The nature of X-ray selected EROs

Author: Stevens, J. A., Page, M. J., Ivison, R. J., Smail, Ian, Lehmann, I., Hasinger, G., and Szokoly, G.
Subjects: Astrophysics
Abstract: We report on the X-ray, optical, near-infrared, submillimetre and radio properties of five Extremely Red Objects (EROs) selected at X-ray wavelengths by XMM-Newton in the Lockman Hole field. They all have enough counts in the X-ray band to allow spectral fitting: four are most probably obscured, Compton-thin AGN with redshift dependent absorbing column densities of 10^22 - 10^24 cm-2, whilst the fifth is best fitted by a thermal spectrum and is likely to be a massive elliptical galaxy in a deep gravitational potential. Their optical/near-infrared colours and sizes suggest that X-ray selected EROs comprise a mixture of dusty 'starburst' galaxies and non-dusty galaxies that are dominated by either star-light or light from an active nucleus. The colour diagnostics are supported by the submillimetre and radio data: the two AGN with 'starburst' colours have submillimetre or radio flux densities that imply large star-formation rates, whilst those with 'elliptical' colours do not. The one source detected in the submillimetre waveband has narrow emission lines at a redshift of 1.45. Although the bulk of its radio emission originates from processes other than star formation, it is most probably a radio-quiet ultraluminous infrared galaxy., Comment: MNRAS, in press, 10 pages, 7 figures
Published: 2003
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45. A deep VLA survey at 6 cm in the Lockman Hole

Author: Ciliegi, P., Zamorani, G., Hasinger, G., Lehmann, I., Szokoly, G. P., and Wilson, G.
Subjects: Astrophysics
Abstract: We have obtained a deep radio image with the Very Large Array at 6 cm in the Lockman Hole. The noise level in the central part of the field is about 11 microJy. From these data we have extracted a catalogue of 63 radio sources. The analysis of the radio spectral index suggests a flattening of the average radio spectra and an increase of the population of flat spectrum radio sources in the faintest flux bin. Cross correlation with the ROSAT/XMM X-ray sources list yields 13 reliable radio/X-ray associations, corresponding to about 21 per cent of the radio sample. Most of these associations (8 out of 13) are classified as Type II AGN. Using optical CCD (V and I) and K' band data we found an optical identification for 58 of the 63 radio sources. This corresponds to an identification rate of about 92 per cent, one of the highest percentages so far available. From the analysis of the colour-colour diagram and of the radio flux - optical magnitude diagram we have been able to select a subsample of radio sources whose optical counterparts are likely to be high redshift (z>0.5) early-type galaxies, hosting an Active Galactic Nucleus responsible of the radio activity. We also find evidence that at these faint radio limits a large fraction (about 60 per cent) of the faintest optical counterparts (i.e. sources in the magnitude range 22.54., Comment: 20 pages, Astronomy and Astrophysics, accepted
Published: 2002
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46. XMM-Newton observation of the Lockman Hole II. Spectral analysis

Author: Mainieri, V., Bergeron, J., Hasinger, G., Lehmann, I., Rosati, P., Schmidt, M., Szokoly, G., and Della Ceca, R.
Subjects: Astrophysics
Abstract: We present the results of the X-ray spectral analysis of the first deep X-ray survey with the XMM-Newton observatory during Performance Verification. We restrict the analysis to the sample of 98 sources with more than 70 net counts (flux limit in the [0.5-7] keV band of 1.6 10^{-15} erg cm^{-2} s^{-1}) of which 61 have redshift identification. We find no correlation between the spectral index Gamma and the intrinsic absorption column density N_H and, for both the Type-1 and Type-2 AGN populations, we obtain ~2. The progressive hardening of the mean X-ray source spectrum with decreasing flux is essentially due to an increase in intrinsic absorption. The marked separation between the two AGN populations in several diagnostics diagrams, involving X-ray colour, X-ray flux, optical/near IR colour and optical brightness, is also a consequence of different absorption column densities and enables the classification of optically faint obscured AGN. About 27% of the subsample with R-K' colour are EROs (R-K>5) and most of these 18 X-ray selected EROs contain anobscured AGN as revealed by their high X-ray-to-optical/near IR flux ratios. There are six sources in our sample with L_X[0.5-10]>10^44 erg s^{-1} and log(N_H)>10^22 cm^{-2}: which are likely Type-2 QSOs and we thus derive a density of ~69 objects of this class per square degree., Comment: Accepted by Astronomy & Astrophysics, 15 pages, 10 figures
Published: 2002
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47. The XMM-Newton SSC Survey of the Galactic Plane

Author: Motch, C., Barcons, X., Carrera, F., Guillout, P., Hands, A., Hassal, B. J. M., Herent, O., Lamer, G., Schwope, A., Szokoly, G., Warwick, R., Watson, M., Webb, N., and Wheatley, P.
Subjects: Astrophysics
Abstract: The XMM-Newton Survey Science Center is currently conducting an optical identification programme of serendipitous EPIC sources at low galactic latitudes. The aim of this study is to quantify the various populations contributing to the overall X-ray emission of the Galaxy and elaborate identification rules that can be later applied to the bulk of the low galactic latitude EPIC detections. We report here on preliminary results from an optical campaign performed in two very low b XMM-Newton fields and discuss the contributions of the various X-ray populations. This paper is presented on behalf of the Survey Science Center and of the AXIS collaboration., Comment: 4 pages 3 figures. To appear in the Proceedings of the Symposium on `New Visions of the X-ray Universe in the XMM-Newton and Chandra Era', 26-30 November 2001, ESTEC, The Netherlands
Published: 2002

48. VLT observations of the z=6.28 quasar SDSS 1030+0524

Author: Pentericci, L., Fan, X., Rix, H. W., Strauss, M. A., Narayanan, V. K., Richards, G T., Schneider, D. P., Krolik, J., Heckman, T., Brinkmann, J., Lamb, D. Q., and Szokoly, G. P.
Subjects: Astrophysics
Abstract: We present new VLT spectroscopic observations of the most distant quasar known, SDSS J1030+0524 at z=6.28 which was recently discovered by the Sloan Digital Sky Survey. We confirm the presence of a complete Gunn-Peterson trough caused by neutral hydrogen in the intergalactic medium. There is no detectable flux over the wavelength range from 8450 to 8710 A. We set an improved limit on the drop of the flux level blueward of the Ly alpha line: a factor of > 200. Below 8450 A the spectrum shows a rise in flux, with a large fraction (> 60 %) of the total emission produced by few narrow features of transmitted flux. We discuss the obvious proximity effect around this quasar, with the presence of transmitted flux with many absorption features in a region of about 23h^{-1} comoving Mpc. If assuming the surrounding medium were completely neutral, the size of this region would imply a quasar lifetime of \~1.3x10^7 years. We also present near-IR spectroscopy of both SDSS J1030+0524 and of SDSS J1306+05, the second most distant quasar known at redshift 6.0. We combine measurements of the CIV line and limits on the HeII emission with the NV line measurements from the optical spectra to derive line ratios, and by implication the abundances of these early quasar environments. The results are indistinguishable from those of lower redshift quasars and indicate little or no evolution in the abundances from z ~ 6 to z ~ 2. The line ratios suggest supersolar metallicities, implying that the first stars around the quasars must have formed at least a few hundreds of Myrs prior to the observation, i.e. at redshift higher than 8., Comment: Accepted by the Astronomical Journal (scheduled for May 2002). Proximity effect section revised
Published: 2001
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49. The Chandra Deep Field South: the 1 Million Second

Author: Rosati, P., Tozzi, P., Giacconi, R., Gilli, R., Hasinger, G., Kewley, L., Mainieri, V., Nonino, M., Norman, C., Szokoly, G., Wang, J. X., Zirm, A., Bergeron, J., Borgani, S., Gilmozzi, R., Grogin, N., Koekemoer, A., Schreier, E., and Zheng, W.
Subjects: Astrophysics
Abstract: We present the main results from our 940 ksec observation of the Chandra Deep Field South (CDFS), using the source catalog described in an accompanying paper (Giacconi et al. 2001). We extend the measurement of source number counts to 5.5e-17 erg/cm^2/s in the soft 0.5-2 keV band and 4.5e-16 erg/cm^2/s in the hard 2-10 keV band. The hard band LogN-LogS shows a significant flattening (slope~=0.6) below ~1e-14 erg/cm^2/s, leaving at most 10-15% of the X-ray background (XRB) to be resolved, the main uncertainty lying in the measurement of the total flux of the XRB. On the other hand, the analysis in the very hard 5-10 keV band reveals a relatively steep LogN-LogS (slope ~=1.3) down to 1e-15 erg/cm^2/s. Together with the evidence of a progressive flattening of the average X-ray spectrum near the flux limit, this indicates that there is still a non negligible population of faint hard sources to be discovered at energies not well probed by Chandra, which possibly contribute to the 30 keV bump in the spectrum of the XRB. We use optical redshifts and identifications, obtained with the VLT, for one quarter of the sample to characterize the combined optical and X-ray properties of the CDFS sample. Different source types are well separated in a parameter space which includes X-ray luminosity, hardness ratio and R-K color. Type II objects, while redder on average than the field population, have colors which are consistent with being hosted by a range of galaxy types. Type II AGN are mostly found at z<~1, in contrast with predictions based on AGN population synthesis models, thus suggesting a revision of their evolutionary parameters., Comment: Accepted by The Astrophysical Journal, 24 pages, 8 figures, 1 color jpg plate (fig.1)
Published: 2001
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50. The XMM-Newton Serendipitous Survey. II. First results from the AXIS high galactic latitude medium sensitivity survey

Author: Barcons, X., Carrera, F. J., Watson, M. G., McMahon, R. G., Aschenbach, B., Freyberg, M. J., Page, K., Page, M. J., Roberts, T. P., Turner, M. J. L., Barret, D., Brunner, H., Ceballos, M. T., Della Ceca, R., Guillout, P., Hasinger, G., Maccacaro, T., Mateos, S., Motch, C., Negueruela, I., Osborne, J. P., Perez-Fournon, I., Schwope, A., Severgnini, P., Szokoly, G. P., Webb, N. A., Wheatley, P. J., and Worrall, D. M.
Subjects: Astrophysics
Abstract: We present the first results on the identifications of a medium sensitivity survey (X-ray flux limit 2E-14 erg/cm2/s in the 0.5-4.5 keV band) at high galactic latitude (|b|>20 deg) carried out with the XMM-Newton X-ray observatory within the AXIS observing programme. This study is being conducted as part of the XMM-Newton Survey Science Centre activities towards the identification of the sources in the X-ray serendipitous sky survey. The sample contains 29 X-ray sources in a solid angle of 0.26deg2 (source density 113 +/- 21 sources/deg2), out of which 27 (93%) have been identified. The majority of the sources are broad-line AGN (19), followed by narrow emission line X-ray emitting galaxies (6, all of which turn out to be AGN), 1 nearby non-emission line galaxy (NGC 4291) and 1 active coronal star. Among the identified sources we find 2 broad-absorption line QSOs (z~1.8 and z~1.9), which constitute ~10% of the AGN population at this flux level, similar to optically selected samples. Identifications of a further 10 X-ray sources fainter than our survey limit are also presented., Comment: 14 pages, 13 eps figures included. New version, including new figure. Accepted in A&A
Published: 2001
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