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Astronomy and Space Physics Astronomy and Space Science 1. Abadie, J., and 711 colleagues, 'TOPICAL REVIEW: Predictions for the rates of compact binary coalescences observable by ground-based gravitational- wave detectors', CQG 27, 173001, 2010 2. Abadie, J., and 711 colleagues, 'Search for gravitational waves from compact binary coalescence in LIGO and Virgo data from S5 and VSR1', PhRvD 82, 102001, 2010 3. Abadie, J., and 723 colleagues, 'Search for gravitational waves from binary black hole inspiral, merger, and ringdown', PhRvD 83, 122005, 2011 4. Abadie, J., and 544 colleagues, 'Calibration of the LIGO gravitational wave detectors in the fifth science run', NIMPA 624, 223, 2010 5. Abadie, J., and 539 colleagues, 'First Search for Gravitational Waves from the Youngest Known Neutron Star', ApJ 722, 1504, 2010 6. Abadie, J., and 667 colleagues, 'Search for Gravitational-wave Inspiral Signals Associated with Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First Science Run', ApJ 715, 1453, 2010 7. Abadie, J., and 668 colleagues, 'All-sky search for gravitational-wave bursts in the first joint LIGO-GEO-Virgo run', PhRvD 81, 102001, 2010 8. Abadie, J., and 500 colleagues, 'Publisher's Note: Search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar [Phys. Rev. D 83, 042001 (2011)]', PhRvD 83, 069902, 2011 9. Abbott, B. P., and 667 colleagues, 'Search For Gravitational-wave Bursts Associated with Gamma-ray Bursts using Data from LIGO Science Run 5 and Virgo Science Run 1', ApJ 715, 1438, 2010 10. Abbott, B. P., and 680 colleagues, 'Searches for Gravitational Waves from Known Pulsars with Science Run 5 LIGO Data', ApJ 713, 671, 2010 11. Accadia, T., and 173 colleagues, 'Virgo calibration and reconstruction of the gravitationnal wave strain during VSR1', JPhCS 228, 012015, 2010 12. Accadia, T., and 177 colleagues, 'Calibration and sensitivity of the Virgo detector during its second science run', CQG 28, 025005, 2011 13. Accadia, T., and 176 colleagues, 'Automatic Alignment system during the second science run of the Virgo interferometer', APh 34, 327, 2011 14. Accadia, T., and 178 colleagues, 'Performance of the Virgo interferometer longitudinal control system during the second science run', APh 34, 521, 2011 15. Accadia, T., and 171 colleagues, 'Noise from scattered light in Virgo's second science run data', CQG 27, 194011, 2010 16. Allevato, V., Finoguenov, A., Cappelluti, N., Miyaji, T., Hasinger, G., Salvato, M., Brusa, M., Gilli, R., Zamorani, G., Shankar, F., James, J. B., McCracken, H. J., Bongiorno, A., Merloni, A., Peacock, J. A., Silverman, J., and Comastri, A., 'The XMM-Newton Wide Field Survey in the COSMOS Field: Redshift Evolution of AGN Bias and Subdominant Role of Mergers in Triggering Moderate-luminosity AGNs at Redshifts up to 2.2', ApJ 736, 99, 2011 17. Alsubai, K. A., Parley, N. R., Bramich, D. M., West, R. G., Sorensen, P. M., Collier Cameron, A., Latham, D. W., Horne, K., Anderson, D. R., Brown, D. J. A., Buchhave, L. A., Esquerdo, G. A., Everett, M. E., Furesz, G., Hellier, C., Miller, G. M., Pollacco, D., Quinn, S. N., Smith, J. C., Stefanik, R. P., and Szentgyorgyi, A., 'Qatar-1b: a hot Jupiter orbiting a metal-rich K dwarf star', arXiv:1012.3027, 2010 18. Amara, A. and Kitching, T. D., 'Figures of merit for testing standard models: application to dark energy experiments in cosmology', MNRAS 413, 1505, 2011 19. Amblard, A., and 71 colleagues, 'Herschel-ATLAS: Dust temperature and redshift distribution of SPIRE and PACS detected sources using submillimetre colours', A&A 518, L9, 2010 20. Anderson, D. R., Hellier, C., Gillon, M., Triaud, A. H. M. J., Smalley, B., Hebb, L., Collier Cameron, A., Maxted, P. F. L., Queloz, D., West, R. G., Bentley, S. J., Enoch, B., Horne, K., Lister, T. A., Mayor, M., Parley, N. R., Pepe, F., Pollacco, D., Segransan, D., Udry, S., and Wilson, D. M., 'Wasp- 17b: An Ultra-Low Density Planet in a Probable Retrograde Orbit', ApJ 709, 159, 2010 21. Antonucci, F., and 100 colleagues, 'From laboratory experiments to LISA Pathfinder: achieving LISA geodesic motion', CQG 28, 094002, 2011 22. Antonucci, F., and 99 colleagues, 'LISA Pathfinder: mission and status', CQG 28, 094001, 2011 23. Antonucci, F., and 95 colleagues, 'LISA Pathfinder data analysis', CQG 28, 094006, 2011 24. Argiroffi, C., Flaccomio, E., Bouvier, J., Donati, J.-F., Getman, K. V., Gregory, S. G., Hussain, G. A. J., Jardine, M. M., Skelly, M. B., and Walter, F. M., 'Variable X-ray emission from the accretion shock in the classical T Tauri star V2129 Ophiuchi', A&A 530, A1, 2011 25. Arzoumanian, D., Jardine, M., Donati, J.-F., Morin, J., and Johnstone, C., 'The contribution of star-spots to coronal structure', MNRAS 410, 2472, 2011 26. Audley, H., and 102 colleagues, 'The LISA Pathfinder interferometry - hardware and system testing', CQG 28, 094003, 2011 27. Austermann, J. E., Dunlop, J. S., Perera, T. A., Scott, K. S., Wilson, G. W., Aretxaga, I., Hughes, D. H., Almaini, O., Chapin, E. L., Chapman, S. C., Cirasuolo, M., Clements, D. L., Coppin, K. E. K., Dunne, L., Dye, S., Eales, S. A., Egami, E., Farrah, D., Ferrusca, D., Flynn, S., Haig, D., Halpern, M., Ibar, E., Ivison, R. J., van Kampen, E., Kang, Y., Kim, S., Lacey, C., Lowenthal, J. D., Mauskopf, P. D., McLure, R. J., Mortier, A. M. J., Negrello, M., Oliver, S., Peacock, J. A., Pope, A., Rawlings, S., Rieke, G., Roseboom, I., Rowan-Robinson, M., Scott, D., Serjeant, S., Smail, I., Swinbank, A. M., Stevens, J. A., Velazquez, M., Wagg, J., and Yun, M. S., 'AzTEC half square degree survey of the SHADES fields - I. Maps, catalogues and source counts', MNRAS 401, 160, 2010 28. Axiak, M., Kitching, T. D., and van Hemert, J. I., 'Evolution Strategies for Cosmology: A Comparison of Nested Sampling Methods', arXiv:1101.0717, 2011 29. Axon, D., Batcheldor, D., Buchanan, C., Capetti, A., Elitzur, M., Gallimore, J., Geballe, T., Horne, K., Kishimoto, M., Marconi, A., Mason, R., Maiolino, R., Netzer, H., Packham, C., Perez, E., Peterson, B., Tadhunter, C., Richmond, M., Robinson, A., Stirpe, G., and Storchi-Bergmann, T., 'Reverberation Mapping of the size of the Dusty Tori in Active Galactic Nuclei.', sptz.prop 80120, 2011 30. Bailin, J., Power, C., Norberg, P., Zaritsky, D., and Gibson, B. K., 'Anisotropic distribution of satellite galaxies (Bailin+, 2008)', yCat 739, 1133, 2010 31. Bain, H. and Fletcher, L., 'Radio Observations And Modeling Of A Post-flare Arcade', AAS 41, 321.05, 2010 32. Baker, D. E. A., Jameson, R. F., Casewell, S. L., Deacon, N., Lodieu, N., and Hambly, N., 'Low-mass stars and brown dwarfs in Praesepe', MNRAS 408, 2457, 2010 33. Balasubramaniam, K. S., Cliver, E. W., Pevtsov, A., Temmer, M., Henry, T. W., Hudson, H. S., Imada, S., Ling, A. G., Moore, R. L., Muhr, N., Neidig, D. F., Petrie, G. J. D., Veronig, A. M., Vrsnak, B., and White, S. M., 'On the Origin of the Solar Moreton Wave of 2006 December 6', ApJ 723, 587, 2010 34. Balcells, M., Benn, C. R., Carter, D., Dalton, G. B., Trager, S. C., Feltzing, S., Verheijen, M. A. W., Jarvis, M., Percival, W., Abrams, D. C., Agocs, T., Brown, A. G. A., Cano, D., Evans, C., Helmi, A., Lewis, I. J., McLure, R., Peletier, R. F., Perez-Fournon, I., Sharples, R. M., Tosh, I. A. J., Trujillo, I., Walton, N., and Westhall, K. B., 'Design drivers for a wide-field multi-object spectrograph for the William Herschel Telescope', SPIE 7735, 2010 35. Baldry, I. K., Robotham, A. S. G., Hill, D. T., Driver, S. P., Liske, J., Norberg, P., Bamford, S. P., Hopkins, A. M., Loveday, J., Peacock, J. A., Cameron, E., Croom, S. M., Cross, N. J. G., Doyle, I. F., Dye, S., Frenk, C. S., Jones, D. H., van Kampen, E., Kelvin, L. S., Nichol, R. C., Parkinson, H. R., Popescu, C. C., Prescott, M., Sharp, R. G., Sutherland, W. J., Thomas, D., and Tuffs, R. J., 'Galaxy And Mass Assembly (GAMA): the input catalogue and star-galaxy separation', MNRAS 404, 86, 2010 36. Barriga, P., Blair, D. G., Coward, D., Davidson, J., Dumas, J.-C., Howell, E., Ju, L., Wen, L., Zhao, C., McClelland, D. E., Scott, S. M., Slagmolen, B. J. J., Inta, R., Munch, J., Ottaway, D. J., Veitch, P., Hosken, D., Melatos, A., Chung, C., Sammut, L., Galloway, D. K., Marx, J., Whitcomb, S., Shoemaker, D., Hughes, S. A., Reitze, D. H., Iyer, B. R., Dhurandhar, S. V., Souradeep, T., Unnikrishnan, C. S., Rajalakshmi, G., Man, C. N., Heidmann, A., Cohadon, P.-F., Briant, T., Grote, H., Danzmann, K., Luck, H., Willke, B., Strain, K. A., Sathyaprakash, B. S., Cao, J., Cheung, Y.-K. E., and Zhang, Y., 'AIGO: a southern hemisphere detector for the worldwide array of ground- based interferometric gravitational wave detectors', CQG 27, 084005, 2010 37. Bassiri, R., Borisenko, K. B., Cockayne, D. J. H., Hough, J., MacLaren, I., and Rowan, S., 'Probing the atomic structure of amorphous Ta_2O_5 coatings', ApPhL 98, 031904, 2011 38. Bassiri, R., Borisenko, K. B., Cockayne, D. J. H., Hough, J., MacLaren, I., and Rowan, S., 'Probing the atomic structure of amorphous Ta_2O_5 mirror coatings for advanced gravitational wave detectors using transmission electron microscopy', JPhCS 241, 012070, 2010 39. Batista, V., and 139 colleagues, 'MOA-2009-BLG-387Lb: a massive planet orbiting an M dwarf', A&A 529, A102, 2011 40. Batista, V., and 132 colleagues, 'MOA-2007-BLG-387Lb light curve I band (Batista+, 2011)', yCat 352, 99102, 2011 41. Battaglia, M. and Kontar, E. P., 'Hard X-Ray Footpoint Sizes and Positions as Diagnostics of Flare Accelerated Energetic Electrons in the Low Solar Atmosphere', ApJ 735, 42, 2011 42.
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