C5 Detector and Background Monitoring System
The C5 detector consists of 2x2 scintillator layers interleaved with layers
of tungsten. It is positioned 1.2 m from the nominal interaction point
in the electron flight direction, in the central cutout of the RTD. It is
sensitive to the effluvia
from beam-gas interactions of the proton and electron beams.
The GFLT vetoes on C5 signals which exceed a threshold defined in the C5 NIM
logic located
on the third floor of the rucksack. C5 also provides rate information
which is used by the ZEUS and HERA shift crews to judge background conditions.
Its timing information provides accurate and detailed information on
the central position of the longitudinal ep interaction distribution and
on the proton-beam bunch length.
-
Shift Information
-
WHAT_TODO_WHEN
(contains information how to restart c5 system processes after the major failure like power lost, what to do in the case of RC problem,...)
-
gplotter
(contains information how to start c5 presenter "gplotter")
-
C5_EXPERTS
(contains information about c5 experts)
- General Documentation
-
The C5 DAQ
(see Chapter 4)
-
The C5 Upgrade
(ZEUS Note 01-002, J.A.Crittenden, W.Hain, U.Schneekloth, U.Wollmer and C.Youngman) summarizes the uses of the C5 detector 1992-2000 and describes in detail the
upgraded detector installed in 2001, its geometry and the plans for its
readout system.
-
The C5 Counter
(ZEUS Note 95-039, W.Schott)
-
Design of a New C5-Counter for ZEUS
(ZEUS Note 94-157, G.Poelz)
-
Stability of C5- and SRTD-TDC during 1994 runs
(ZEUS Note 95-151, Shun'ichi Mine, K. Tokushuku)
-
Analysis of C5 Detector Time Distributions for the
1993 Running Period
(ZEUS Note 94-041, J.A.Crittenden and T.Stange)
describes the investigations of proton satellite bunches which resulted
from the shortening of the proton bunch length beginning in 1993.
-
Results of Analysis of the C5 Detector Time
Distributions for the Fall 1992 Running Period
(ZEUS Note 93-041, J.A.Crittenden, M.Nakahata and K.Piotrzkowski)
describes the use of the C5 timing distributions in 1992 to make a correction
to the luminosity calculation necessitated by the presence of satellite
electron bunches.
Julia Fourletova
Last modified 28 Aug 2006