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information_for_astronomers:backends
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information_for_astronomers:backends [2013/10/16 15:53] akraus |
information_for_astronomers:backends [2024/08/01 07:50] (current) akraus |
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| ====== Available Backends ====== | ====== Available Backends ====== | ||
| - | (page under construction) | + | |
| + | The observatory offers a number of backends for various observing modes. Currently, | ||
| + | the electronic division of the MPIfR is deploying the new "Effelsberg Direct Digitization" (EDD) | ||
| + | system. | ||
| + | |||
| + | Within this, the RF signal is digitized directly in the receiver (without any mixing), and | ||
| + | transported to the backend via Ethernet with high data rate. The signal processing is realized | ||
| + | in software and allows to handle several observing modes (even simultaneously). Currently, | ||
| + | modes are available for continuum/polarimetry, spectroscopy, pulsar observations and VLBI. | ||
| + | |||
| + | For more details, please see [[https://www.ursi.org/proceedings/procGA23/papers/1703.pdf|the paper of Ewan Barr]]. | ||
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| + | |||
| + | Still, a number of hardware backends are available. If you are uncertain about | ||
| + | which receiver can be combined with the EDD or the conventional backends, please | ||
| + | do not hesitation to contact us at **eff-support[at]mpifr-bonn.mpg.de**.\\ | ||
| ===For Continuum Observations=== | ===For Continuum Observations=== | ||
| Line 11: | Line 26: | ||
| ===For Spectroscopy=== | ===For Spectroscopy=== | ||
| - | * [[xffts|XFFT spectrometer]] (2x 32768 channels, 2000, 500, 100 MHz Bandwidth) | + | * [[xffts|XFFT spectrometer]] (2x 65536 channels, 2500, 2000, 500, 300, 100, 50 MHz Bandwidth - not all modes are available with all receivers) |
| - | * Array FFT spectrometer (16x16384 channels) | + | * WFFTS - an Array spectrometer especially for the broad-band receivers (28x65536 channels) |
| //A description of the FFT spectrometer and how they work can be found in the paper of [[http://arxiv.org/abs/1203.3972|Klein et al.]]// | //A description of the FFT spectrometer and how they work can be found in the paper of [[http://arxiv.org/abs/1203.3972|Klein et al.]]// | ||
information_for_astronomers/backends.1381931604.txt.gz · Last modified: 2013/10/16 15:53 by akraus
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