Development of a Thermal Isolation Structure for Aerospace Cryogenic Instruments
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Engineering topics
Publications and source records attributed to Nash, A..
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A proof of concept prototype cryostat has been developed to demonstrate the ability to accommodate low temperature science investigations within the constraints of the Hitchhiker siderail carrier on the space shuttle.
A proof of concept prototype cryostat has been developed to demonstrate the ability to accommodate low temperature science investigations within the constraints of the Hitchhiker siderail carrier on the Space Shuttle.
Subsystems for a proof of concept cryogenic payload have been developed to demonstrate the ability to accommodate low temperature science investigations within the constraints of the Hitchhiker siderail carrier on the Space Shuttle.
To address the gap in manifest opportunities for low temperature microgravity payloads that has accompanied the start of the build era for the International Space Station (ISS), development of a new facility compatible with one or more carriers in the baseline shuttle manifest has been undertaken.
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The end of regularly scheduled Microgravity Science Payload (MSP), shuttle mission(s), the severely limited ability to accommodate the existing low temperature flight hardware on other carriers, and the anticipated delays in the development schedule for the International Space Station (ISS) in combination have left low temperature microgravity investigations with few (if any) flight opportunities until several years into the next millennium.
The detection of methyl formate (HCOOCH3) in four transitions toward Orion KL, in two transitions toward Sagitarrius B2, and in one transition toward W51 is reported. The column densities of HCOOCH3 are found to be surprisingly large (2-5 x 10 to the 14th per sq cm) in all three clouds. Stimulated emission in the 18 cm K doublet of HCOOCH3 toward Sagittarius B2 is clearly demonstrated. The relatively large column densities of HCOOCH3 in clouds outside the galactic-center region probably imply that this molecule is widely distributed in the galaxy, but the negative results in other clouds require lower column densities than in Orion by a factor of 0.5 or less. Two unidentified lines were detected in Orion, at approx. 91 and 99 GHz.