Cosmic Ray Energetics and Mass Experiment

The purpose of the Cosmic Ray Energetics and Mass (CREAM) Experiment is to determine the composition of cosmic rays up to the 10¹⁵ eV "knee" in the cosmic ray spectrum. It is suspected that this knee in the cosmic ray spectrum can be explained by the theoretical maximum energy that a supernova can accelerate particles to through Fermi acceleration. This is accomplished with a timing-based charge detector and transition radiation detector at an altitude of at least 110,000 ft with the aid of a high-altitude balloon. After launching from McMurdo Station in Antarctica, the balloon will stay aloft for 60-100 days gathering data on charges and energies of the unimpeded cosmic rays that strike the detectors.

One of the advantages of this type of experiment is that it is possible to identify the original particle that would have caused the air shower detected by ground-based detectors. Maximum detectable energy level is determined by duration of the flight and size of the detector; a difficult barrier to get around for experiments of this type. An accurate measurement of the composition of cosmic rays is necessary in order to understand the origins of the cosmic rays found above the "knee" at 10¹⁵ eV. To date, the CREAM balloon experiments have accumulated a total of 161 days of exposure, longer than any other single balloon-borne experiment.^{[1] [2]}

CREAM III takes flight in Antarctica

Experimental goals

• Can the "knee" be explained by maximum acceleration due to supernovae?
• Have the composition of cosmic rays changed over time?
• Are multiple mechanisms responsible for the production of cosmic rays?

Construction

In order to answer these questions, it is of particular interest to investigate cosmic rays in the 10¹² to 10¹⁵ eV region due to several theories predicting a change in elemental composition just below the knee. To determine the elemental spectrum of cosmic rays, CREAM uses a silicon charge detector, timing charge detector, and scintillating fiber hodoscopes to detect the charge of incident particles up to that of iron (Z = 26). Energies are measured with a transition radiation detector (TRD), along with an ionization calorimeter. Because all detectors are in close proximity of each other, it is a prime concern to minimize the interaction between showers produced in the calorimeter, and the charge-measuring instruments. To dampen this effect, CREAM uses a larger number of pixels with a smaller area, along with a very fast readout time to differentiate between events caused by the primary particle and events caused by back-scattering from the calorimeter.

The relatively low density of the TRD allows for a larger detector geometry to detect particles with a lower flux. By measuring the Lorentz factor γ, combined with knowledge of the particle's charge, it is possible to calibrate the detector with various cosmic rays of charge ±1 (electrons, pions, muons, etc). Because of the relatively low geomagnetic cutoff energy for cosmic rays near the south pole, a cherenkov detector is placed between modules of the TRD to act as a veto for these low-energy particles.^[3]

Instrumentation of CREAM II

For power, the system includes batteries for energy storage, along with a solar array rated to sustain the mission for 100 days. Altogether, the instrument is expected to draw only 380 watts from a 28-volt supply, thanks to a very careful choice of energy-efficient electronics. In near-vacuum conditions, significant precautions must be taken against coronal discharges between unshielded electronics operating at as low as 100 volts. This is mitigated by encasing all relevant electronics in a lightweight dielectric compound, such as plaster.

The instrument must be able to operate in a wide range of temperatures, as the high albedo of Antarctica can cause very high temperatures, while periods of darkness will result in very low temperatures.

Excluding the ballast, total weight of the instrument must not exceed 5,500 pounds (2,500 kg) to reach the desired altitude. Retrieval is done by separating the instrument from the balloon after a sufficient amount of exposure, and a parachute opens to somewhat slow the descent of the instrument. Although the experiment is designed to meet the structural requirements of the Columbia Scientific Balloon Facility, it is inevitable that some damage will be incurred to replaceable parts of the instrument. The main priority is data retrieval; all other systems are considered secondary at this point.

ISS-CREAM

Pronounced "ice-cream", ISS-CREAM is the next generation version of the CREAM balloon experiments that is scheduled be placed on the International Space Station in 2016. Located at an altitude of 410 km, 10 times higher than previous balloon flights, ISS-CREAM will be able to take data almost non-stop during its three-year mission. Because of the extreme altitude, there is no atmosphere for incident particles to scatter off of before reaching the detector. It is expected that this ISS-based mission will gather an order of magnitude more data than the CREAM balloon experiments.^[4]

Funding

CREAM experiments are currently being funded by NASA.

Collaborators

The current CREAM collaboration team includes members from the University of Maryland, Pennsylvania State University, Sungkyunkwan University, National Autonomous University of Mexico, Laboratoire de Physique Subatomique et de Cosmologie of Grenoble, France, Kyungpook National University, Goddard Space Flight Center, and Northern Kentucky University.

References

1. E.S. Seo; et al. (25 April 2003). "Cosmic-ray energetics and mass (CREAM) balloon project" (PDF). Advances in Space Research.
2. "Cosmic Ray Energetics and Mass (CREAM)". 4 March 2015.
3. H.S. Ahn; et al. (10 May 2007). "Cosmic-ray energetics and mass (CREAM) instrument" (PDF). Nuclear Instruments and Methods in Physics Research: 1034–1053.
4. "Cosmic Ray Energetics and Mass for the International Space Station" (PDF).

External links

• Official website