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Microquasars: Hard X-ray/γ-ray emission

AIP Conference Proceedings AIP Publishing 558:1 (2001) 221-233
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Search for B → τv and B → Kvv̄

Physical Review Letters 86:14 (2001) 2950-2954

Authors:

TE Browder, Y Li, JL Rodriguez, H Yamamoto, T Bergfeld, BI Eisenstein, J Ernst, GE Gladding, GD Gollin, RM Hans, E Johnson, I Karliner, MA Marsh, M Palmer, C Plager, C Sedlack, M Selen, JJ Thaler, J Williams, KW Edwards, R Janicek, PM Patel, AJ Sadoff, R Ammar, A Bean, D Besson, R Davis, N Kwak, X Zhao, S Anderson, VV Frolov, Y Kubota, SJ Lee, R Mahapatra, JJ O'Neill, R Poling, T Riehle, A Smith, CJ Stepaniak, J Urheim, S Ahmed, MS Alam, SB Athar, L Jian, L Ling, M Saleem, S Timm, F Wappler, A Anastassov, JE Duboscq, E Eckhart, KK Gan, C Gwon, T Hart, K Honscheid, D Hufnagel, H Kagan, R Kass, TK Pedlar, H Schwarthoff, JB Thayer, E von Toerne, MM Zoeller, SJ Richichi, H Severini, P Skubic, A Undrus, S Chen, J Fast, JW Hinson, J Lee, DH Miller, EI Shibata, IPJ Shipsey, V Pavlunin, D Cronin-Hennessy, AL Lyon, EH Thorndike, CP Jessop, H Marsiske, ML Perl, V Savinov, D Ugolini, X Zhou, TE Coan, V Fadeyev, Y Maravin, I Narsky, R Stroynowski, J Ye, T Wlodek, M Artuso, R Ayad, C Boulahouache, K Bukin, E Dambasuren, S Karamov, G Majumder, GC Moneti, R Mountain

Abstract:

An analysis of 9.66 × 106 charged B meson decays which results in a conservative upper limit on the branching fraction B(B → τν) < 8.4 × 10-4. The analysis was slightly modified to establish B(B± → K± νν̄) < 2.4 × 10-4. The method used is optimized for conditions available at Y(4S) experiments, and some application of the method to other rare decay modes with large missing energy was aniticipated.
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Spectral evidence for a powerful compact jet from XTE J1118+480

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 322:2 (2001) l23-l27

Authors:

RP Fender, RM Hjellming, RPJ Tilanus, GG Pooley, JR Deane, RN Ogley, RE Spencer
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First observation of the decays B0 → D*- p̄π+ and B0 → D*-pn̄

Physical Review Letters 86:13 (2001) 2732-2736

Authors:

S Anderson, VV Frolov, Y Kubota, SJ Lee, R Mahapatra, JJ O'Neill, R Poling, T Riehle, A Smith, CJ Stepaniak, J Urheim, S Ahmed, MS Alam, SB Athar, L Jian, L Ling, M Saleem, S Timm, F Wappler, A Anastassov, JE Duboscq, E Eckhart, KK Gan, C Gwon, T Hart, K Honscheid, D Hufnagel, H Kagan, R Kass, TK Pedlar, H Schwarthoff, JB Thayer, E Von Toerne, MM Zoeller, SJ Richichi, H Severini, P Skubic, A Undrus, S Chen, J Fast, JW Hinson, J Lee, DH Miller, EI Shibata, IPJ Shipsey, V Pavlunin, D Cronin-Hennessy, AL Lyon, EH Thorndike, CP Jessop, H Marsiske, ML Perl, V Savinov, X Zhou, TE Coan, V Fadeyev, Y Maravin, I Narsky, R Stroynowski, J Ye, T Wlodek, M Artuso, R Ayad, C Boulahouache, K Bukin, E Dambasuren, S Karamov, G Majumder, GC Moneti, R Mountain, S Schuh, T Skwarnicki, S Stone, G Viehhauser, JC Wang, A Wolf, J Wu, S Kopp, AH Mahmood, SE Csorna, I Danko, KW McLean, S Márka, Z Xu, R Godang, K Kinoshita, IC Lai, S Schrenk, G Bonvicini, D Cinabro, S McGee, LP Perera, GJ Zhou, E Lipeles, SP Pappas, M Schmidtler, A Shapiro, WM Sun, AJ Weinstein, F Würthwein

Abstract:

Decay modes of the B0 of the type B → DNN̄X were observed. Measurements imply that DNN̄X final states may contribute substantially to the total observed B → barvon rate. Branching fractions were accurately measured.
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The radio galaxy K-z relation to z ~ 4.5

ArXiv astro-ph/0103364 (2001)

Authors:

Matt J Jarvis, Steve Rawlings, Steve Eales, Katherine M Blundell, Chris J Willott

Abstract:

Using a new radio sample, 6C* designed to find radio galaxies at z > 4 along with the complete 3CRR and 6CE sample we extend the radio galaxy K-z relation to z~4.5. The 6C* K-z data significantly improve delineation of the K-z relation for radio galaxies at high redshift (z > 2). Accounting for non-stellar contamination, and for correlations between radio luminosity and estimates of stellar mass, we find little support for previous claims that the underlying scatter in the stellar luminosity of radio galaxies increases significantly at z > 2. This indicates that we are not probing into the formation epoch until at least z > 3.
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