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| = Quick Guide to the 30m observatory (DRAFT) = | = Quick Guide for Dummies - The novice 30m user = |
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| === PaKo: A typical observing session === | === A typical observing session: PaKo === |
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| === Network === === Computers and tasks === |
=== What are all the screens for ? Network topology or entering the unknown === === My machine is called mrt-lx18. Now what ? Software === == Details like telescope and instruments == |
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During observations, the backends take data and safe them in streams in FITS format. These streams are merged with streams from other parts of the system, e.g. antenna mount drive, and also with messages, to be included in IMBFits raw data files. These are then combined by mira/odp to create calibrated spectra, usually on the antenna temperature scale TA*, and safed as 30m files. These in turn can then be read offline with class by the observer. Mira, class, greg are part of the GILDAS software package. Astronomical data therefore is created in several levels: level-1 are the streams, level-2 are the IMBfits files, level-3 are the 30m files. In most cases, the observer and principal investigator is only interested in the 30m files. However, in case of calibration or other problems, it is possible to recalibrate data using MIRA, or even to recreate data from the streams. |
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| === How can I safe my data ? Use rsync, stupid ! === |
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| === CLASS: A typical session === === GREG: A typical session === |
=== Howto work with spectra: CLASS === === Howto work with data cubes: GREG === == Whom to complain to ? Help needed == Don't be afraid of "silly" questions, please! |
Contents
Quick Guide for Dummies - The novice 30m user
Howto observe ?
Getting started
A typical observing session: PaKo
Displays
Computer System
What are all the screens for ? Network topology or entering the unknown
My machine is called mrt-lx18. Now what ? Software
Details like telescope and instruments
Data
Online data processing (Odp)
During observations, the backends take data and safe them in streams in FITS format. These streams are merged with streams from other parts of the system, e.g. antenna mount drive, and also with messages, to be included in IMBFits raw data files. These are then combined by mira/odp to create calibrated spectra, usually on the antenna temperature scale TA*, and safed as 30m files. These in turn can then be read offline with class by the observer. Mira, class, greg are part of the GILDAS software package. Astronomical data therefore is created in several levels: level-1 are the streams, level-2 are the IMBfits files, level-3 are the 30m files. In most cases, the observer and principal investigator is only interested in the 30m files. However, in case of calibration or other problems, it is possible to recalibrate data using MIRA, or even to recreate data from the streams.
Where are my data ?
How can I safe my data ? Use rsync, stupid !
What happens to my data ? Backup, Storage
Next steps: user dp
Howto work with spectra: CLASS
Howto work with data cubes: GREG
Whom to complain to ? Help needed
Don't be afraid of "silly" questions, please!
This page is maintained by CK. Any comments are welcome.