Millimeter Interferometer Observations of the Magnetar 4U 0142+61

AIP Conference Proceedings AIP Publishing 1379:1 (2011) 152-155

Authors:

B Posselt, K Schreyer, Ü Ertan, S Trippe, K Menten, B Klein, Ersin Göğüş, Ünal Ertan, Tomaso Belloni

Testing the jet quenching paradigm with an ultradeep observation of a steadily soft state black hole

Astrophysical Journal Letters 739:1 (2011)

Authors:

DM Russell, JCA Miller-Jones, TJ MacCarone, YJ Yang, RP Fender, F Lewis

Abstract:

We present ultradeep radio observations with the Expanded Very Large Array of 4U 1957+11, a Galactic black hole (BH) candidate X-ray binary known to exist in a persistent soft X-ray state. We derive a stringent upper limit of 11.4 μJy beam-1 (3σ) at 5-7 GHz, which provides the most rigorous upper limit to date on the presence of jets in a soft state BH X-ray binary (BHXB). X-ray, UV, and optical fluxes obtained within a few weeks of the radio data can be explained by thermal emission from the disk. At this X-ray luminosity, a hard state BHXB that follows the established empirical radio-X-ray correlation would be at least 330-810 times brighter at radio frequencies, depending on the distance to 4U 1957+11. This jet quenching of >2.5 orders of magnitude is greater than some models predict and implies that the jets are prevented from being launched altogether in the soft state. 4U 1957+11 is also more than one order of magnitude fainter than the faintest of the "radio-quiet" population of hard state BHs. In addition, we show that, on average, soft state stellar-mass BHs probably have fainter jets than most active galactic nuclei in a state equivalent to the soft state. These results have implications for the conditions required for powerful, relativistic jets to form and provide a new empirical constraint for time- and accretion mode-dependent jet models, furthering our understanding of jet production and accretion onto BHs. © 2011. The American Astronomical Society. All rights reserved.

Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

(2011)

Authors:

The LIGO Scientific Collaboration, Virgo Collaboration, J Abadie, BP Abbott, R Abbott, TD Abbott, M Abernathy, T Accadia, F Acernese, C Adams, R Adhikari, C Affeldt, P Ajith, B Allen, GS Allen, E Amador Ceron, D Amariutei, RS Amin, SB Anderson, WG Anderson, K Arai, MA Arain, MC Araya, SM Aston, P Astone, D Atkinson, P Aufmuth, C Aulbert, BE Aylott, S Babak, P Baker, G Ballardin, S Ballmer, D Barker, F Barone, B Barr, P Barriga, L Barsotti, M Barsuglia, MA Barton, I Bartos, R Bassiri, M Bastarrika, A Basti, J Batch, J Bauchrowitz, Th S Bauer, M Bebronne, B Behnke, MG Beker, AS Bell, A Belletoile, I Belopolski, M Benacquista, JM Berliner, A Bertolini, J Betzwieser, N Beveridge, PT Beyersdorf, IA Bilenko, G Billingsley, J Birch, R Biswas, M Bitossi, MA Bizouard, E Black, JK Blackburn, L Blackburn, D Blair, B Bland, M Blom, O Bock, TP Bodiya, C Bogan, R Bondarescu, F Bondu, L Bonelli, R Bonnand, R Bork, M Born, V Boschi, S Bose, L Bosi, B Bouhou, S Braccini, C Bradaschia, PR Brady, VB Braginsky, M Branchesi, JE Brau, J Breyer, T Briant, DO Bridges, A Brillet, M Brinkmann, V Brisson, M Britzger, AF Brooks, DA Brown, A Brummit, T Bulik, HJ Bulten, A Buonanno, J Burguet--Castell, O Burmeister, D Buskulic, C Buy, RL Byer, L Cadonati, G Cagnoli, J Cain, E Calloni, JB Camp, P Campsie, J Cannizzo, K Cannon, B Canuel, J Cao, CD Capano, F Carbognani, S Caride, S Caudill, M Cavaglià, F Cavalier, R Cavalieri, G Cella, C Cepeda, E Cesarini, O Chaibi, T Chalermsongsak, E Chalkley, P Charlton, E Chassande-Mottin, S Chelkowski, Y Chen, A Chincarini, A Chiummo, H Cho, N Christensen, SSY Chua, CTY Chung, S Chung, G Ciani, F Clara, DE Clark, J Clark, JH Clayton, F Cleva, E Coccia, P-F Cohadon, CN Colacino, J Colas, A Colla, M Colombini, A Conte, R Conte, D Cook, TR Corbitt, M Cordier, N Cornish, A Corsi, CA Costa, M Coughlin, J-P Coulon, P Couvares, DM Coward, DC Coyne, JDE Creighton, TD Creighton, AM Cruise, A Cumming, L Cunningham, E Cuoco, RM Cutler, K Dahl, SL Danilishin, R Dannenberg, S D'Antonio, K Danzmann, V Dattilo, B Daudert, H Daveloza, M Davier, G Davies, EJ Daw, R Day, T Dayanga, R De Rosa, D DeBra, G Debreczeni, J Degallaix, W Del Pozzo, M del Prete, T Dent, V Dergachev, R DeRosa, R DeSalvo, V Dhillon, S Dhurandhar, L Di Fiore, A Di Lieto, I Di Palma, M Di Paolo Emilio, A Di Virgilio, M Díaz, A Dietz, F Donovan, KL Dooley, S Dorsher, M Drago, RWP Drever, JC Driggers, Z Du, J-C Dumas, S Dwyer, T Eberle, M Edgar, M Edwards, A Effler, P Ehrens, G Endrőczi, R Engel, T Etzel, K Evans, M Evans, T Evans, M Factourovich, V Fafone, S Fairhurst, Y Fan, BF Farr, W Farr, D Fazi, H Fehrmann, D Feldbaum, I Ferrante, F Fidecaro, LS Finn, I Fiori, RP Fisher, R Flaminio, M Flanigan, S Foley, E Forsi, LA Forte, N Fotopoulos, J-D Fournier, J Franc, S Frasca, F Frasconi, M Frede, M Frei, Z Frei, A Freise, R Frey, TT Fricke, JK Fridriksson, D Friedrich, P Fritschel, VV Frolov, PJ Fulda, M Fyffe, M Galimberti, L Gammaitoni, MR Ganija, J Garcia, JA Garofoli, F Garufi, ME Gáspár, G Gemme, R Geng, E Genin, A Gennai, LÁ Gergely, S Ghosh, JA Giaime, S Giampanis, KD Giardina, A Giazotto, C Gill, E Goetz, LM Goggin, G González, ML Gorodetsky, S Goßler, R Gouaty, C Graef, M Granata, A Grant, S Gras, C Gray, N Gray, RJS Greenhalgh, AM Gretarsson, C Greverie, R Grosso, H Grote, S Grunewald, GM Guidi, C Guido, R Gupta, EK Gustafson, R Gustafson, T Ha, B Hage, JM Hallam, D Hammer, G Hammond, J Hanks, C Hanna, J Hanson, J Harms, GM Harry, IW Harry, ED Harstad, MT Hartman, K Haughian, K Hayama, J-F Hayau, T Hayler, J Heefner, A Heidmann, MC Heintze, H Heitmann, P Hello, MA Hendry, IS Heng, AW Heptonstall, V Herrera, M Hewitson, S Hild, D Hoak, KA Hodge, K Holt, J Homan, T Hong, S Hooper, DJ Hosken, J Hough, EJ Howell, B Hughey, S Husa, SH Huttner, T Huynh-Dinh, DR Ingram, R Inta, T Isogai, A Ivanov, K Izumi, M Jacobson, H Jang, P Jaranowski, WW Johnson, DI Jones, G Jones, R Jones, L Ju, P Kalmus, V Kalogera, I Kamaretsos, S Kandhasamy, G Kang, JB Kanner, E Katsavounidis, W Katzman, H Kaufer, K Kawabe, S Kawamura, F Kawazoe, W Kells, DG Keppel, Z Keresztes, A Khalaidovski, FY Khalili, EA Khazanov, B Kim, C Kim, D Kim, H Kim, K Kim, N Kim, Y-M Kim, PJ King, M Kinsey, DL Kinzel, JS Kissel, S Klimenko, K Kokeyama, V Kondrashov, R Kopparapu, S Koranda, WZ Korth, I Kowalska, D Kozak, V Kringel, S Krishnamurthy, B Krishnan, A Królak, G Kuehn, R Kumar, P Kwee, M Laas-Bourez, PK Lam, M Landry, M Lang, B Lantz, N Lastzka, C Lawrie, A Lazzarini, P Leaci, CH Lee, HM Lee, N Leindecker, JR Leong, I Leonor, N Leroy, N Letendre, J Li, TGF Li, N Liguori, PE Lindquist, NA Lockerbie, D Lodhia, M Lorenzini, V Loriette, M Lormand, G Losurdo, J Luan, M Lubinski, H Lück, AP Lundgren, E Macdonald, B Machenschalk, M MacInnis, DM Macleod, M Mageswaran, K Mailand, E Majorana, I Maksimovic, N Man, I Mandel, V Mandic, M Mantovani, A Marandi, F Marchesoni, F Marion, S Márka, Z Márka, A Markosyan, E Maros, J Marque, F Martelli, IW Martin, RM Martin, JN Marx, K Mason, A Masserot, F Matichard, L Matone, RA Matzner, N Mavalvala, G Mazzolo, R McCarthy, DE McClelland, P McDaniel, SC McGuire, G McIntyre, DJA McKechan, GD Meadors, M Mehmet, T Meier, A Melatos, AC Melissinos, G Mendell, D Menendez, RA Mercer, L Merill, S Meshkov, C Messenger, MS Meyer, H Miao, C Michel, L Milano, J Miller, Y Minenkov, VP Mitrofanov, G Mitselmakher, R Mittleman, O Miyakawa, B Moe, P Moesta, M Mohan, SD Mohanty, SRP Mohapatra, D Moraru, G Moreno, N Morgado, A Morgia, T Mori, S Mosca, K Mossavi, B Mours, CM Mow--Lowry, CL Mueller, G Mueller, S Mukherjee, A Mullavey, H Müller-Ebhardt, J Munch, PG Murray, A Mytidis, T Nash, L Naticchioni, R Nawrodt, V Necula, J Nelson, G Newton, E Nishida, A Nishizawa, F Nocera, D Nolting, L Nuttall, E Ochsner, J O'Dell, E Oelker, GH Ogin, JJ Oh, SH Oh, RG Oldenburg, B O'Reilly, R O'Shaughnessy, C Osthelder, CD Ott, DJ Ottaway, RS Ottens, H Overmier, BJ Owen, A Page, G Pagliaroli, L Palladino, C Palomba, Y Pan, C Pankow, F Paoletti, MA Papa, M Parisi, A Pasqualetti, R Passaquieti, D Passuello, P Patel, D Pathak, M Pedraza, P Peiris, L Pekowsky, S Penn, C Peralta, A Perreca, G Persichetti, M Phelps, M Pickenpack, F Piergiovanni, M Pietka, L Pinard, IM Pinto, M Pitkin, HJ Pletsch, MV Plissi, R Poggiani, J Pöld, F Postiglione, M Prato, V Predoi, LR Price, M Prijatelj, M Principe, S Privitera, R Prix, GA Prodi, L Prokhorov, O Puncken, M Punturo, P Puppo, V Quetschke, FJ Raab, DS Rabeling, I Rácz, H Radkins, P Raffai, M Rakhmanov, CR Ramet, B Rankins, P Rapagnani, S Rapoport, V Raymond, V Re, K Redwine, CM Reed, T Reed, T Regimbau, S Reid, DH Reitze, F Ricci, R Riesen, K Riles, NA Robertson, F Robinet, C Robinson, EL Robinson, A Rocchi, S Roddy, C Rodriguez, M Rodruck, L Rolland, J Rollins, JD Romano, R Romano, JH Romie, D Rosińska, C Röver, S Rowan, A Rüdiger, P Ruggi, K Ryan, H Ryll, P Sainathan, M Sakosky, F Salemi, L Sammut, L Sancho de la Jordana, V Sandberg, S Sankar, V Sannibale, L Santamaría, I Santiago-Prieto, G Santostasi, B Sassolas, BS Sathyaprakash, S Sato, M Satterthwaite, PR Saulson, RL Savage, R Schilling, S Schlamminger, R Schnabel, RMS Schofield, B Schulz, BF Schutz, P Schwinberg, J Scott, SM Scott, AC Searle, F Seifert, D Sellers, AS Sengupta, D Sentenac, A Sergeev, DA Shaddock, M Shaltev, B Shapiro, P Shawhan, DH Shoemaker, A Sibley, X Siemens, D Sigg, A Singer, L Singer, AM Sintes, G Skelton, BJJ Slagmolen, J Slutsky, JR Smith, MR Smith, ND Smith, RJE Smith, K Somiya, B Sorazu, J Soto, FC Speirits, L Sperandio, M Stefszky, AJ Stein, E Steinert, J Steinlechner, S Steinlechner, S Steplewski, A Stochino, R Stone, KA Strain, S Strigin, AS Stroeer, R Sturani, AL Stuver, TZ Summerscales, M Sung, S Susmithan, PJ Sutton, B Swinkels, M Tacca, L Taffarello, D Talukder, DB Tanner, SP Tarabrin, JR Taylor, R Taylor, P Thomas, KA Thorne, KS Thorne, E Thrane, A Thüring, C Titsler, KV Tokmakov, A Toncelli, M Tonelli, O Torre, C Torres, CI Torrie, E Tournefier, F Travasso, G Traylor, M Trias, K Tseng, L Turner, D Ugolini, K Urbanek, H Vahlbruch, G Vajente, M Vallisneri, JFJ van den Brand, C Van Den Broeck, S van der Putten, AA van Veggel, S Vass, M Vasuth, R Vaulin, M Vavoulidis, A Vecchio, G Vedovato, J Veitch, PJ Veitch, C Veltkamp, D Verkindt, F Vetrano, A Viceré, AE Villar, J-Y Vinet, S Vitale, S Vitale, H Vocca, C Vorvick, SP Vyatchanin, A Wade, SJ Waldman, L Wallace, Y Wan, X Wang, Z Wang, A Wanner, RL Ward, M Was, P Wei, M Weinert, AJ We, R Weiss, L Wen, S Wen, P Wessels, M West, T Westphal, K Wette, JT Whelan, SE Whitcomb, D White, BF Whiting, C Wilkinson, PA Willems, HR Williams, L Williams, B Willke, L Winkelmann, W Winkler, CC Wipf, AG Wiseman, H Wittel, G Woan, R Wooley, J Worden, J Yablon, I Yakushin, H Yamamoto, K Yamamoto, H Yang, D Yeaton-Massey, S Yoshida, P Yu, M Yvert, A Zadroźny, M Zanolin, J-P Zendri, F Zhang, L Zhang, W Zhang, Z Zhang, C Zhao, N Zotov, ME Zucker, J Zweizig, C Akerlof, M Boer, R Fender, N Gehrels, A Klotz, EO Ofek, M Smith, M Sokolowski, BW Stappers, I Steele, J Swinbank, RAMJ Wijers, W Zheng

Modeling of the HERMES submillimeter source lensed by a dark matter dominated foreground group of galaxies

Astrophysical Journal 738:2 (2011)

Authors:

R Gavazzi, A Cooray, A Conley, JE Aguirre, A Amblard, R Auld, A Beelen, A Blain, R Blundell, J Bock, CM Bradford, C Bridge, D Brisbin, D Burgarella, P Chanial, E Chapin, N Christopher, DL Clements, P Cox, SG Djorgovski, CD Dowell, S Eales, L Earle, TP Ellsworth-Bowers, D Farrah, A Franceschini, H Fu, J Glenn, EA González Solares, M Griffin, MA Gurwell, M Halpern, E Ibar, RJ Ivison, M Jarvis, J Kamenetzky, S Kim, M Krips, L Levenson, R Lupu, A Mahabal, PD Maloney, C Maraston, L Marchetti, G Marsden, H Matsuhara, AMJ Mortier, E Murphy, BJ Naylor, R Neri, HT Nguyen, SJ Oliver, A Omont, MJ Page, A Papageorgiou, CP Pearson, I Pérez-Fournon, M Pohlen, N Rangwala, JI Rawlings, G Raymond, D Riechers, G Rodighiero, IG Roseboom, M Rowan-Robinson, B Schulz, D Scott, KS Scott, P Serra, N Seymour, DL Shupe, AJ Smith, M Symeonidis, KE Tugwell, M Vaccari, E Valiante, I Valtchanov, A Verma, JD Vieira, L Vigroux, L Wang, J Wardlow, D Wiebe, G Wright, CK Xu, G Zeimann, M Zemcov, J Zmuidzinas

Abstract:

We present the results of a gravitational lensing analysis of the bright z s = 2.957 submillimeter galaxy (SMG) HERMES found in the Herschel/SPIRE science demonstration phase data from the Herschel Multi-tiered Extragalactic Survey (HerMES) project. The high-resolution imaging available in optical and near-IR channels, along with CO emission obtained with the Plateau de Bure Interferometer, allows us to precisely estimate the intrinsic source extension and hence estimate the total lensing magnification to be μ = 10.9 ± 0.7. We measure the half-light radius R eff of the source in the rest-frame near-UV and V bands that characterize the unobscured light coming from stars and find R eff, * = [2.0 ± 0.1] kpc, in good agreement with recent studies on the SMG population. This lens model is also used to estimate the size of the gas distribution (Reff, gas = [1.1 ± 0.5] kpc) by mapping back in the source plane the CO (J = 5 → 4) transition line emission. The lens modeling yields a relatively large Einstein radius R Ein = 4.″10 ± 0″.02, corresponding to a deflector velocity dispersion of [483 ± 16] km s -1. This shows that HERMES is lensed by a galaxy group-size dark matter halo at redshift z l ∼ 0.6. The projected dark matter contribution largely dominates the mass budget within the Einstein radius with f dm(< R Ein) ∼ 80%. This fraction reduces to f dm(< R eff, G1 ≃ 4.5 kpc) ∼ 47% within the effective radius of the main deflecting galaxy of stellar mass M *, G1 = [8.5 ± 1.6] × 1011 M ⊙. At this smaller scale the dark matter fraction is consistent with results already found for massive lensing ellipticals at z ∼ 0.2 from the Sloan Lens ACS Survey. © 2011. The American Astronomical Society. All rights reserved.

A new model for the infrared emission of IRAS F10214+4724

Proceedings of the International Astronomical Union 7:S284 (2011) 205-209

Authors:

A Efstathiou, N Christopher, A Verma, R Siebenmorgen

Abstract:

We present a new model for the infrared emission of the high redshift hyperluminous infrared galaxy IRAS F10214+4724 which takes into account recent photometric data from Spitzer and Herschel that sample the peak of its spectral energy distribution. We first demonstrate that the combination of the AGN tapered disc and starburst models of Efstathiou and coworkers, while able to give an excellent fit to the average spectrum of type 2 AGN measured by Spitzer, fails to match the spectral energy distribution of IRAS F10214+4724. This is mainly due to the fact that the ν S ν distribution of the galaxy falls very steeply with increasing frequency (a characteristic of heavy absorption by dust) but shows a silicate feature in emission. We propose a model that assumes two components of emission: clouds that are associated with the narrow-line region and a highly obscured starburst. The emission from the clouds must suffer significantly stronger gravitational lensing compared to the emission from the torus to explain the observed spectral energy distribution. © 2012 International Astronomical Union.