SUPERCONDUCTING MAGNET SPECTROMETER

The objective of the balloon flight was to search for antiprotons in the cosmic rays using a superconducting magnet spectrometer developed by the Physical Science Laboratory in Las Cruces based on a previous apparatus developed by the same scientific group at the NASA's Johnson Space Center.

A basic scheme of the magnet spectrometer and the container gondola is shown in the figure at left (click to enlarge). The spectrometer has two main components: the SUPERCONDUCTING MAGNET and the MULTIWIRE PROPORTIONAL COUNTERS (MWPC) stack. The magnet was a scaled-up version of the first superconducting magnet to fly successfully on a balloon by the NASA JSC group back in 1969-1970. The new magnet was 61 cm in diameter and produced a magnetic field of ~40 kilogauss at the center of the coil when operating at a current of 120 Amperes. It weighed 150 kg and was maintained at a temperature a few degrees above the absolute zero inside a cryostat cooled by liquid helium. The purpose of the magnet was to deflect the course of heavy particles reaching the detector from outer space, so that the charge and momentum of each particle -its characteristic signature- can be measured.

The MWPC stack, consisted of eight identical 50 x 50 cm2 MWPCs modules staggered horizontally so that the top chambers are closer to the magnet face. This increased the effective maximum detectable rigidity of the spectrometer. The MWPCs position measurements were digitized using distributed inductance delay lines coupled to the chamber wires. The chambers were oriented with the anode wires perpendicular to the magnet axis so that most of the bending in the magnetic field occurs along the cathode coordinate axis. Position measurement, in each coordinate axis, was obtained by measuring the time of arrival of the signal at each end of the delay lines.

A gas Cherenkov counter, was located above the MWPC stack. The detector was filled with air or sulfur hexafluoride depending on the flight objectives. Its aperture was divided equally by four spherical mirrors, each of which was viewed by a 12.5 cm diameter RCA 4525 photomultiplier (PM) tube through a conical mirror that acted as a high transmission lens. The overall length of this detector was 1 meter, with an effective path length of 80 cm.

All scintillators, S1, S2, P1-P7, were 0.6 cm thick Pilot Y. Scintillators S1 and S2 were each viewed by two 5 cm diameter RCA 4523 PM tubes through two adiabatic light pipes, and all other scintillators were viewed by single RCA 4523 PM tubes through conventional light pipes. Except for P1, which was 45 x 45 cm2, all of the scintillators were 50 x 50 cm2. The scintillators P1 - P7 were each separated by 1.2 radiation length of lead thereby forming a shallow shower counter of 1.2 radiation lengths depth. This counter provided a rough energy determination (30%) of the electron events and was crucial in reducing the proton contamination of positron measurements.

The signals from the scintillators and the Gas Cerenkov system were pulse height analyzed and digitized with 12-bit resolution. These values, along with the outputs from the MWPC time digitizers, were telemetered and recorded on ground along with a flag to indicate the type of coincidence event. In addition, the time of flight between S1 and P1 was measured to determine the direction of motion of the incoming particle. The digitized data, together with 100 channels of sub-commutated engineering data (voltages, temperatures, pressures and logic state) were transmitted to the ground via a 48 kbit/s telemetry link. A 100-channel command link was used to control the payload on the ground and during flight.

The availability of the data in real time, and the possibility of actively controlling discriminators, detector voltages and logic circuitry pushed the development of a mini-computer based real-time data processing and experiment control system. A data van equipped with a Digital Equipment Corporation PDP-8E and PDP-11/10 computers was used for interactive payload control. Scientific data was presented to the experimenters in graphic and tabular form. Information was also available for examination in real-time on pulse height spectra, MWPC resolution, etc. Commands were issued to the payload to control the logic and detector operating conditions in order to optimize key parameters (e.g., chamber resolution and experiment dead-time). All commands were issued by the computers in response to keyboard mnemonics typed by the observing teams. In a typical flight about one hundred keyboard command sequence mnemonics were typed. These result in roughly one thousand actual two-digit commands being sent to the payload. Experience from first flights demonstrated that this interactive control technique was an invaluable aid in achieving high quality data from the payload.

The instrument and all its components, including electronics and batteries were encased in an insulated gondola 5 meters tall and 2.4 meters in diameter with a total mass of 2100 kg.

Balloon launched on: 6/22/1979 at 2:04 utc
Launch site: Columbia Scientific Balloon Facility, Palestine, Texas, US  
Balloon launched by: National Scientific Balloon Facility (NSBF)
Balloon manufacturer/size/composition: Zero Pressure Balloon Winzen 794.287 m3 (20.32 Microns - Stratofilm) - SF 415.29-080-NSCR-01
Balloon serial number: W 28.05-3-03
Flight identification number: 1151P
End of flight (L for landing time, W for last contact, otherwise termination time): 6/22/1979 at 13:53 utc
Balloon flight duration (F: time at float only, otherwise total flight time in d:days / h:hours or m:minutes - ): F 9 h
Landing site: 8 miles SE of Sierra Blanca, Texas, US
Payload weight: 2631 kgs

During this flight were detected for the first time antiprotons -the antimatter equivalent of ordinary protons.

• Antimatter detected in space by balloon Lakeland Ledger, 17 Oct 1979
• Cosmic ray proton & helium spectra from 5 - 200 GV measured with a magnetic spectrometer 20th International Cosmic Ray Conference, Vol. 1, p. 325 - 328
• Determination of the Energy Spectrum and Charge Composition of Muons at Sea-Level 20th International Cosmic Ray Conference Moscow, Volume 6, p.173
• Energy dependence of the P(bar)/P ratio in cosmic rays Astrophysical Letters, vol. 24, no. 2, 1984, p. 75-83
• Evidence for the existence of cosmic-ray antiprotons Physical Review Letters, vol. 43, Oct. 15, 1979, p. 1196-1199
• Evidence of Antimatter Found Washington Post, 17 Oct. 1979
• High-Level Balloon Detects Antimatter Flow From Space New York Times, 17 Oct. 1979
• National Scientific Balloon Facility Annual Report FY 1979 National Center for Atmospheric Research, September 1980
• Observation of cosmic ray positrons in the region from 5 to 50 GeV Astronomy and Astrophysics, vol. 188, no. 1, Dec. 1987, p. 145-154
• Results of a Recent Attempt to Observe Antiprotons in the Cosmic Rays 16th International Cosmic Ray Conference, Vol. 1. P.76
• Results of a search for deuterium at 25-50 GC/c using a magnetic spectrometer NASA. Goddard Space Flight Center 19th Intern. Cosmic Ray Conf., Vol. 2 p 68-71
• Scientific balloon finds theory-shattering antimatter Star-News, 18 Oct 1979
• Scientists confirm antimatter The Tuscaloosa News, 21 Oct 1979
• Scientists detect antimatter existing naturally in galaxy The Montreal Gazette, 17 Oct 1979
• Solar modulation of hydrogen and helium cosmic ray nuclei spectra above 400 MeV/Nucleon, from 1976 to 1993 24th International Cosmic Ray Conference, Italy, 1995
• Strange stuff found in space Lewiston Morning Tribune, 17 Oct 1979
• US scientists nab antimatter Ottawa Citizen, 18 Oct 1979