Changeset 821
- Timestamp:
- 05/31/01 08:26:17 (23 years ago)
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trunk/ICRC_01/mccontrib.tex
r819 r821 374 374 the expected rates from proton showers and background light. 375 375 376 The estimated trigger rate due to proton showers is $143 \pm 11$ Hz. This 377 rate would increase due to other hadron showers (He, Li, ...) which 376 The numbers quoted in this section are calcuated for a zenith angle 377 $\Theta = 10^o$. Same studies have been done for $\Theta =0^o$ and 378 for $\Theta = 15^o$ and we got similar results. 379 We estimated the rate for the first level trigger 380 with the "standard" trigger conditions. 381 The first level trigger rate due to proton showers without any 382 background is $143 \pm 11~\mathrm{Hz}$. 383 This rate would increase due to other hadron showers (He, Li, ...) which 378 384 we have not simulated yet. About 25 \% larger rate is expected due mainly 379 to He. Moreover, to get a realistic rate one should assume a realistic 380 background, for instance 0.09 photo electrons per ns \citep{ml94} and 381 the Crab Nebula star field. Under this conditions the estimated rate is 382 $396 \pm 88$ Hz. 385 to He. 386 387 However, to get a more reliable rate one must take into account 388 a realistic background situation. We take for the diffuse part of the 389 night sky background a value of 0.09 photo electrons per ns 390 \citep{ml94} 391 and use the star field around the Crab nebula. 392 Under this more realistic conditions the first level trigger 393 background rate (protons and light of night sky) is $396 \pm 88$ Hz. 383 394 384 395 It has been also studied the effect on the trigger rate of the discriminator … … 396 407 \end{figure} 397 408 398 The numbers that appear in this section have been estimated for $10^\circ$399 zenith angle. But the same studies have been done for $0^\circ$ and $15^\circ$400 and401 we got similar results.402 409 403 410 \section{Conclusion} … … 420 427 MAGIC Collaboration, "The MAGIC Telescope, Design Study for 421 428 the Construction of a 17m Cherenkov Telescope for Gamma 422 Astronomy Above 10 GeV", Preprint MPI-PhE ?18-5, March 1998.429 Astronomy Above 10 GeV", Preprint MPI-PhE 18-5, March 1998. 423 430 424 431 \bibitem[Heck and Knapp(1995)]{hk95} … … 427 434 \bibitem[Mirzoyan and Lorenz(1997)]{ml97} 428 435 Mirzoyan R. and E. Lorenz, Proc. 25th ICRC, Durban, 7, p.356, 1997 429 430 431 \bibitem[Abramovitz and Stegun(1964)]{as64}432 Abramowitz, M. and Stegun, I. A., Handbook of Mathematical Functions,433 U. S. Govt. Printing Office, Washington D. C., 1964.434 435 \bibitem[Aref(1983)]{a83}436 Aref, H., Integrable, chaotic, and turbulent vortex motion in437 two-dimensional flows, Ann. Rev. Fluid Mech., 15, 345--389, 1983.438 436 439 437 \bibitem[Mirzoyan and Lorenz(1994)]{ml94} … … 444 442 445 443 \end{document} 444 445
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