Split-Pole Spectrograph: Difference between revisions
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[[File:SABER installing particle shield.png|thumb|right|Installing particle shield on SABER (photo taken on May 5, 2022)]] | [[File:SABER installing particle shield.png|thumb|right|Installing particle shield on SABER (photo taken on May 5, 2022)]] | ||
SABRE is a ''' | SABRE is a '''S'''ilicon '''A'''rray for '''B'''ranching '''R'''atio '''E'''xperiments | ||
<ref> E. C. Good ''et. al'', NIM A '''1003''', 165299 (2021) https://www.sciencedirect.com/science/article/pii/S0168900221002837</ref> | <ref> E. C. Good ''et. al'', NIM A '''1003''', 165299 (2021) https://www.sciencedirect.com/science/article/pii/S0168900221002837</ref> | ||
with the SPS. SABRE sits at | with the SPS. Its predecessor is the Yale Lamp Shade Array (YLSA). SABRE sits at backward angles from the target and covers roughly 30% of 4π. SABRE has both thick and thin dead-layer detectors, with the thin dead-layer detectors capable of reaching ~200 keV thresholds for protons and deuterons. | ||
= SPS Experiment Guide = | = SPS Experiment Guide = | ||
Revision as of 23:10, 27 May 2023
 Annotated picture of the SE-SPS, An plain picture is here : File:SPS Magnet.png |
 SE-SPS COSY simulation. An plain picture is here File:SPS Sketch With Cosy.png |
The Super Enge Split-Pole Spectrograph [1] [2] [3] was originally located at the Wright Nuclear Structure Laboratory (closed at 2013), at Yale University. It was moved to FSU in the fall of 2013. It consists of a reaction chamber, a split-pole magnetic spectrograph, a position-sensitive ionization drift chamber, and a plastic scintillator. It has an angular acceptance of 128 msr (vertical ±40 mrad, horizontal ±80 mrad). The maximum B-field is 1.63 T with a radius of curvature from 511 mm to 920 mm. The mean radius is 600 mm.
The Super Enge Split-Pole Spectrograph is an upgrade of the Yale Enge SPS. The major change is the redesign of the backward silicon detector array to the SABRE.
Magnet
The SPS contains 2 dipole magnets: pole-1 and pole-2. The magnet can be rotated from 0 to 55 degrees in the lab. The magnetic field has an upper limit of 1.63 T (or 16.3 kG).
COSY simulation and Transfer matrix
 Notice : | need to fill up. Any 1st few orders transfer matrixes? |
Focal plane detector
| Notice : | The drift ion chamber was repaired at summer 2018 |
The focal plane detector [4] [5] consists of an ion drift chamber with a set of delay lines to detect the position of a particle along the focal plane and a plastic scintillator to detect the energy of the incoming particle. Using the energy loss of the particle through the ion chamber with the energy deposited in the scintillator, particles of different charges and masses can be identified.
The typical pressure of the drift chamber is 70 to 300 Torr of isobutane gas [HC(CH3)3]. The pressure controls the density of the gas and affects the bias voltage, it further affects the drift velocity. Here is a table of pressure and bias voltages (data taken from the Ph.D. thesis of Erin Good).
| Gas pressure (Torr) | Anode bias (V) | Cathode plate bias (V) |
|---|---|---|
| 70 | +1050 to +1035 | -550 to -500 |
| 80 | +1150 | -550 |
| 100 | +1250 | -600 |
| 110 | +1200 to 1320 | -620 to -600 |
| 125 | +1425 | -650 |
| 130 | +1360 | -725 |
| 150 | +1500 | -700 |
From bottom to top, the cathode plate, drift region (contains four biased field-shaping wire grids), Frisch grid (grounded), three anode wires, and pickup pads (which are with the delay lines). Electrons induced by any radiation will drift upward, pass the Frisch grid, are accelerated by the anodes, and hit the pickup pads. The pickup pads are strips with 45° against the anode wires, almost parallel to the particle trajectories[5]. Each pickup strip is 0.09" (2.286 mm) wide and 1.4" (35.56 mm) long, and spaced 0.01" (0.245 mm). A total of 440 strips with a 5 ns delay per strip results in a nominal total delay of 2.2 μs. The position of the hit position can then be determined by the time difference at the end of the delay line.
There are two position-sensitive delay lines in the focal plane detector. By reconstructing the particle trajectory using the position information of both delay lines, the resolution can be enhanced by correcting for the kinematic shift of the reaction.
After passing the drift chamber, the particles will be stopped and detected in a plastic scintillator with a photomultiplier tube (PMT) at each end. Together with the energy loss, obtained by the cathode in the drift chamber, a ΔE-E particle identification can be done.
Outline of the algorithm
There are 7 readouts channels from the focal plane detector:
| readout | type of signal |
|---|---|
| cathode | energy loss |
| Front delay line Left | timing |
| Front delay line Right | timing |
| Rear delay line Left | timing |
| Rear delay line Right | timing |
| PMT Left | energy |
| PMT Right | energy |
Kinematic correction of the focal plane
|
 |
| Simulated rays near the focal plane. | An animation on the shift of the focal panel. An optimum is reached at FP = -42 mm. |
SABRE
SABRE is a Silicon Array for Branching Ratio Experiments [6] with the SPS. Its predecessor is the Yale Lamp Shade Array (YLSA). SABRE sits at backward angles from the target and covers roughly 30% of 4π. SABRE has both thick and thin dead-layer detectors, with the thin dead-layer detectors capable of reaching ~200 keV thresholds for protons and deuterons.
SPS Experiment Guide
Media:SPS_Experiment_Guide.pdf
SPS Operating Procedures
I created this section as a place to store procedures for the chamber swaps, however, I expect there are other things we might want to document here. -p
Repositories
Contact
- Jeff Blackmon mailto:blackmon@lsu.edu
- Ingo
- who should be contacted?
References
- ↑ H.A. Enge, NIM 162, 161 (1979) https://doi.org/10.1016/0029-554X(79)90711-0
- ↑ H. A. Enge, NIM 187, 1 (1981) https://doi.org/10.1016/0029-554X(81)90465-1
- ↑ J. E. Spencer and H. A. Enge, NIM 49, 181 (1967) https://doi.org/10.1016/0029-554X(67)90684-2
- ↑ C. Marshal et. al, IEEE Tran. Inst. and Meas. 68, 533 (2018) https://doi.org/10.1109/TIM.2018.2847938
- ↑ 5.0 5.1 R. G. Markham and R. G. H. Robertson, NIM 129, 131 (1975) https://doi.org/10.1016/0029-554X(75)90122-6
- ↑ E. C. Good et. al, NIM A 1003, 165299 (2021) https://www.sciencedirect.com/science/article/pii/S0168900221002837