By Rev. T.W.; Edited and Revised By Margaret W. Mayall Webb
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Additional resources for Celestial Objects for Common Telescopes. Edited and Rev. By Margaret W. Mayall
The pairings were required to be unique, so no jet is used twice. 3. The pairing that minimised x2 = (M$ - M,)* + (M$ - Ml)* was chosen. 4. The jj momenta were resealed to obtain the correct W mass, and the jjb mass was recomputed. 20 Supersymmetty 847 ATLAS defector and physics performance Volume II 25 May 7999 Technical Design Report _ SUSY .... SM tt (siddxmd subbacfed) Figure 20-38 Top signal (open), estimated Figure 20-39 torial background duction. Point 5. combina(shaded) at Point 5, and SM ti pro- Background-subtracted top - signal at Each step narrows the width of the Mjjb peak at the top mass.
This distribution is shown in Figure 20-40 for two different values of the slepton mass. A very precise measurement of the mass seems difficult. If the iL were slightly heavier, then it would also be possible to search for a four-lepton signal from one iL + ii:1 decay and one iL + X$1+ %pZlldecay, In principle the endpoint of the trilepton mass can be used to determine the slepton mass, although the rates are marginal. 10 below. 8 Exclusive SUGRA measurements for large tan p SUGRA phenomenology for tanp > 10 is more complicated because of the need to include additional Yukawa couplings and mixings in the b and ?
5. Presumably these branching ratios could also be used in a more quantitative way to improve the measurement of tan p at Point 2, but this has not been studied. 2 Point 3 Point 3 is a low-mass point with many well-measured quantities. The best-measured ones are summarised in Table 20-7. The measurements listed below the line in the table actually determine combinations of masses. 5M - 0 rather than M- . tan C(+,rn2 . Hence the distinction is less significant than for Points 1 and 2. While the fit is done including all the information simultaneously, m1,2 is mainly determined by Mx2 - Miry, which is accurately measured from the dilepton endpoint.